ࡱ> +{ d f{|YG .bjbjَ  'H|]    RRR4!!!!h!v"!'S$@6(4j(j()3:$<JPLPLPLPZPQR$U WR-R= 23==RF..j()$FFF=.j(R)JP* ..=JPF6F;KORJP)j$a!!@6PSOFIA Concept of Operations (Preliminary) Document No. USRA-DAL-1004-05 Stratospheric Observatory For Infrared Astronomy (SOFIA) Prepared under Contract NAS2-97001 By: Universities Space Research Association (USRA) 7500 Maehr Road Waco, Texas 76705 Approved: Date: Tom F. Bonner, Jr. USRA SOFIA Project Manager Approved: Date: Christopher B. Wiltsee NASA SOFIA Project Manager REVISIONS Subsequent to release of Rev 5., vertical change bars in the left margin of each page indicate changes to this document. revdateDESCRIPTIONAPPROVAL55/20/98Completely revised. Added Revisions BlockSee front cover Table of Contents  TOC \o "1-4" 1.0 Scope  PAGEREF _Toc420822835 \h 1 1.1 System Overview  PAGEREF _Toc420822836 \h 1 1.2 Document Overview  PAGEREF _Toc420822837 \h 1 2.0 Referenced Documents  PAGEREF _Toc420822838 \h 3 3.0 Operations  PAGEREF _Toc420822839 \h 3 3.1 Operational Overview  PAGEREF _Toc420822840 \h 3 3.1.1 Mission  PAGEREF _Toc420822841 \h 3 3.1.2 Operational Policies  PAGEREF _Toc420822842 \h 6 3.1.3 Operational Constraints  PAGEREF _Toc420822843 \h 13 3.1.4 Operational Environment and Support  PAGEREF _Toc420822844 \h 15 3.3 Personnel profiles  PAGEREF _Toc420822845 \h 28 4.0 Operational Processes  PAGEREF _Toc420822846 \h 33 4.1 SRM&QA and Airworthiness Processes  PAGEREF _Toc420822847 \h 38 4.1.1 Safety for Flight Dispatch  PAGEREF _Toc420822848 \h 39 4.1.2 Mission Readiness for Flight Dispatch  PAGEREF _Toc420822849 \h 39 4.1.3 Mission Management and the Flight Dispatch Decision  PAGEREF _Toc420822850 \h 40 4.2 Call for Proposals/Peer Review for Science Instruments and Observing Time  PAGEREF _Toc420822851 \h 41 4.3 Yearly Scheduling  PAGEREF _Toc420822852 \h 43 4.3.1 Normal Scheduling Process  PAGEREF _Toc420822853 \h 43 4.3.2 Target of Opportunity Scheduling  PAGEREF _Toc420822854 \h 45 4.4 Flight Series Process  PAGEREF _Toc420822855 \h 45 4.5 Instrument Installation and Checkout  PAGEREF _Toc420822856 \h 46 4.5.1 Instrument installation at Moffett Field  PAGEREF _Toc420822857 \h 47 4.4.1.1 TA/MCCS Simulator Procedures  PAGEREF _Toc420822858 \h 47 4.6 Daily Operations Process  PAGEREF _Toc420822859 \h 53 4.6.1 Typical Flight Day (at Moffett Field)  PAGEREF _Toc420822860 \h 53 4.6.2 Non-Flight Weekday  PAGEREF _Toc420822861 \h 61 4.7 Research Flight Process  PAGEREF _Toc420822862 \h 62 4.7.1 Climbout (from takeoff until seatbelt sign is turned off ) :  PAGEREF _Toc420822863 \h 65 4.7.2 Ascent (from seatbelt sign turned off to opening of cavity door):  PAGEREF _Toc420822864 \h 66 4.7.3 Checkout ( from cavity door opening to first object leg):  PAGEREF _Toc420822865 \h 66 4.7.4 Transition between flight legs:  PAGEREF _Toc420822866 \h 67 4.7.5 First Observing Leg:  PAGEREF _Toc420822867 \h 68 4.7.5.1 Field & Object Acquisition  PAGEREF _Toc420822868 \h 68 4.7.5.9 Possible Automation  PAGEREF _Toc420822869 \h 75 4.7.8 Landing and Taxi:  PAGEREF _Toc420822870 \h 78 4.8 Maintenance Processes  PAGEREF _Toc420822871 \h 79 4.8.1 Scheduled Maintenance  PAGEREF _Toc420822872 \h 79 4.9 Continuous Improvement Process  PAGEREF _Toc420822873 \h 89 4.10 Deployment Process  PAGEREF _Toc420822874 \h 91 4.11 Data Center  PAGEREF _Toc420822875 \h 100 4.12 Education and Public Outreach Program  PAGEREF _Toc420822876 \h 110 4.13 SSMOC Configuration Management  PAGEREF _Toc420822877 \h 112 5.0 Definitions, Abbreviations, Acronyms  PAGEREF _Toc420822878 \h 114  1.0 Scope 1.1 System Overview The SOFIA System consists of the SOFIA Airborne Observatory, the suite of SOFIA Science Instruments and the SOFIA Science and Mission Operations Center (or SSMOC). The SOFIA Airborne Observatory consists of the integrated Aircraft System and the Mission System. For the purposes of this document, the Aircraft System consists of the basic Boeing 747 SP aircraft, all the Aircraft Modified Systems (AMS), including the power distribution system, the fuselage structural modification including aircraft control and system rerouting, the cavity door and cavity door mechanisms, and the personnel accommodations on the aircraft. The Mission System consists of the Telescope Assembly (TA) and TA subsystems, the Mission Controls and Communications System (MCCS), and the onboard cavity environmental conditioning system (CECS). The MCCS consists of the consoles and racks, and the electronic systems required to monitor and control the Mission System. A system that is not included in the Airborne Observatory, but is essential for the acquisition of science data, is the Science Instrument System. This system consists of the complement of Science Instruments (SI) (including the SI electronics) used on the Airborne Observatory. A Science Instrument, when in use, is mounted on the TA, and its associated SI Electronics are mounted on the Airborne Observatory in racks (see Figure 3.1.4.3-1). The SSMOC is the ground facility which houses the SOFIA Airborne Observatory and all the facilities required to manage, administer, operate and maintain the airborne observatory. This center also houses the science and education staff to coordinate and support the science and education communities in order to maximize the science and discovery output of SOFIA and its communication to the community at large. In addition, the SSMOC staff manages the suite of SOFIA Science Instruments, and supports the integration of these onto the Airborne Observatory. Although the management of the SI System is under SSMOC control, the development of the Science Instruments is by the science community (at universities, private research institutes, and government research centers) via a peer review process. A subset of the SIs are maintained at the SSMOC, the remainder are maintained at the universities or centers where they were developed. Figure 1.1-1 shows the breakdown of the SOFIA System into its subsystems. 1.2 Document Overview The purpose of this document is to describe the SOFIA System characteristics from an operational perspective. It will be used to facilitate understanding of SOFIA system goals EMBED Word.Picture.8 with the users and developers. Throughout this document, the term system "user" refers to all those who will be involved in use of the system during operations, including the following: scientists, aircraft and telescope operators and maintainers, engineers, education program staff and visitors, management and administrative staff. This document will form an overall basis for long-range operations planning and serves as a reference during the system requirements, analysis, and design phases to provide the necessary framework within which proposed system design and implementation alternatives can be evaluated. This document describes the operations-phase user organization and mission from an integrated user/system point of view. The Concept of Operations communicates to system developers and users, in the user's language, the desired operational characteristics of a system to be developed. It describes the SOFIA system context (Section 3.0), which consists of: - Mission Objectives - Operational philosophies and policies - Operational system characteristics - System constraints and limitations - User Organization (functions, responsibilities, capabilities, and interfaces of the science and operations staff) This document also describes all the major SOFIA System operation processes and procedures (Section 4.0), and provides the rationale behind the proposed procedures. Section 4 is written unevenly, covering in depth those processes which need definition for development of certain subsystems, and covering in less depth those processes which do not critically effect subsystems. (In reality, sections were written at the request of developers.) In summary, this is not an overview document which only covers the top level items of operations. This is a document primarily for the developers of SOFIA and as such has a mixture of detail and overview. This document will be revised throughout the development phase, primarily for internal by the USRA Team. 2.0 Referenced Documents ANSI/AIAA G-043-1992: Guide for the Preparation of Operational Concept Documents. SOF-1051: NASA/ARC Preliminary Operations Plan SOF-1009: SOFIA Science Objectives, Rationale, and Related Requirements NAS2-97001: SOFIA System Development and Operations Contract SOF-1001: SOFIA Operations Phase Summary Management Plan 3.0 Operations 3.1 Operational Overview 3.1.1 Mission The Universities Space Research Association (USRA), in partnership with United Airlines, University of California, the SASP Alliance (an alliance between the SETI Institute and Astronomical Society of the Pacific), Sterling Software, Raytheon Systems Company, and DLR designated German organizations, will operate the Stratospheric Observatory For Infrared Astronomy (SOFIA) as NASAs and DLRs premier observatory for infrared and submillimeter astronomy into the next century. SOFIA will operate for a total of twenty years starting in FY 2002. The above partnership will operate the observatory for the first five years, with an option for the second five years, after which the operations contract will be re-competed by NASA approximately every five years. The 747SP aircraft will carry a 2.5-meter telescope designed to make sensitive infrared measurements of a wide range of astronomical objects. It will fly at and above 41,000 feet for over 960 successful flight hours per year, to collect radiation in the wavelength range from 0.3 micrometers (m) to 1.6 millimeters region of the electromagnetic spectrum which is important for the following astrophysical reasons: 1. Most of the fundamental absorption and emission lines and bands of astrophysically, astrobiologically, and astrochemically significant molecules occur in this wavelength regime; 2. Most of the luminosity of our galaxy and in other galaxies emerges in this wavelength region; 3. Low dust extinction at these wavelengths permits unbiased and potentially complete observations of statistically large samples of objects; and 4. Formation of galaxies in the early universe and the crucial stages of formation of stars and planets can best be studied in this range of wavelengths. The SOFIA operations program will involve a number of agencies and organizations. NASA is the system owner, US funding source and managing agency. NASAs international partner, DLR, which provides the telescope for the observatory, will provide for 20% of the operations support, securing 20% of the observing time for the German science community. USRA will operate SOFIA for the US and German astronomical communities, which will provide science instrumentation for the observatory and use SOFIA for science observation. USRA, with the University of California, will provide a science-driven infrastructure for SOFIA that can respond effectively to the needs of the science user within a strictly cost-capped program. United Airlines will provide safe and effective flight and ground operations of the observatory on a world-wide scale. The SASP Alliance will work to make sure SOFIA is a prominent component of NASAs Education and Public Outreach Program, effectively communicating the excitement and importance of science to educational organizations and the general public. Raytheon Systems Company will provide engineering support and continuous improvement capabilities. The German contingent to the US operation will be fully integrated into the overall work force of the SOFIA Science and Mission Operations Center (see Section 3.3). All SOFIA operations will be under the direction of a USRA appointed Observatory Director, a senior astronomer of distinction with observatory management experience. The Observatory operations will be reviewed and approved by NASA. In 1995, the NASA SOFIA Science Working Group (SSWG) listed the following as the two principal goals of SOFIA: A: Maximize scientific productivity and discovery potential, and B: Promote educational opportunities and public outreach. From these goals the SSWG concluded that SOFIA operations should include the following provisions: (1) Scientific direction of the observatory by an astronomer who is responsible for all aspects of its operation, particularly its performance and productivity. This arrangement gives the best assurance that the observatory's resources will be allocated in a balance that achieves the goals of the observatory listed above. (2) Frequent independent peer review of proposed science and technology will assure not only the value of ongoing research, but also routine opportunities for the entire astronomical community to propose new research. It implies that the observatory will encourage guest investigators as well as principal investigators, and will enable straight-forward access by scientists from all nations. (3) An instrument complement that exploits the observatory's full potential must be assured by an operations plan which provides resources for continuous, innovative instrument and technology development over the projected twenty-plus year operational lifetime of SOFIA. The objective is to make available state-of-the-art focal plane instruments which achieve performance determined by the physical limitations of the observatory. Operations will allow the investigator to have continual access to the science instrument in flight (within appropriate safety constraints), because the instruments are state-of-the-art. (4) The need for full-sky observations and for rapid response to transient phenomena imply not only that operations must include routine deployments for extended southern hemisphere observations, but also that they must provide for self-contained expeditions to non- routine destinations to observe astronomical events such as occultations or eclipses. (5) A vigorous flight program and highly efficient operations will assure effective utilization of the observatory. These imply maximizing - within practical constraints - the number of science flight hours per year and the efficiency of operations, for example, in exchanging focal plane instruments on the telescope, in flight planning, and in observing. These also imply that observatory upgrades are implemented as needed to improve performance. (6) Stimuli for prompt publication and archiving of results will promote rapid access to observational results and their significance by the science community. (7) Flexibility in the program to include different types of investigations will permit, for example, approval of multiple-year proposals and key projects as appropriate to benefit from the continuity afforded by SOFIA's long lifetime. However, some speculative, high-risk investigations should also be included in the observing program, as should rapid adjustments of the schedule needed to accommodate observations of unexpected ephemeral events by qualified investigators. (8) A variety of educational activities, including development of stimulating programs for K-12 teachers, innovative science programs for undergraduates, graduate student doctoral research opportunities, research opportunities for young scientists, and exposure of infrared astronomy to the general public and the media. SOFIA's accessibility, mobility, and lifetime give it tremendous potential in this arena. The operational policies in Section 3.1.2 and the operational processes outlined in Section 4.0 are formulated with the above goals and provisions in mind, and with an emphasis on safety. As a minimum, Sections 3.1.2 and 4.0 will meet the contractual requirement on USRA by NASA (see NAS2-97001) of assuring that the SOFIA Airborne Observatory will fly 960 successful flight hours (SFH) per year for the contract duration. Policies for Successful Flight Hours are described in 3.1.2.6. 3.1.2 Operational Policies The SSMOC (SOFIA Science and Mission Operations Center) will be operated so the goals and provisions listed in Section 3.1.1 are met. These goals and provisions may be achieved using a number of operational scenarios. The numbers of scenarios are minimized if policies for the SSMOC are well defined. The Observatory Director, with inputs and concurrence from NASA and the SOFIA Science Council, defines these policies. 3.1.2.1 Science Instrument Policies: A. All science instrument development and upgrade supported by SOFIA shall be peer reviewed. B. Call for Proposals (CfPs) for science instrument development and upgrade is planned for every three years. The first was issued in FY 1997, the second will be issued in FY 2000, followed thereafter with CfPs approximately every three years. Grants may be provided for longer than three years, where appropriate. C. There will be three classes of science instruments on SOFIA: Facility-class Science Instrument (FSI): A general purpose, reliable and robust instrument that provides state-of-the-art science performance at commissioning, through the use of modern, but mature technologies. It is expected that this instrument will routinely be operated and maintained by a designated SSMOC FSI scientist in support of Guest Investigators (GIs) who will not be required to have extensive knowledge or experience in infrared instrumentation or observing techniques. The process of data acquisition, reduction, and calibration should be straightforward and transparent to the GI, with the assistance of the SSMOC FSI scientist. The GI should be able to perform data analysis of calibrated data using standard software routines, without requiring the assistance of the SSMOC FSI scientist. The FSIs will have standardized installation procedures, which will allow for quick installation and removal from the TA on the aircraft. This characteristic will be strived for in the other classes of science instruments given below, but will be a requirement for FSI. Standardization of installation is essential for achieving high flight rates (i.e., science productivity). Principal Investigator-class Science Instrument (PSI): A general purpose instrument that is developed and maintained at the state of the art throughout its useful operating life. It is expected that this instrument will be operated by the Principal Investigator (PI) team, both for its own research as well as for that of successful GIs. The interaction of the PI and GI teams is to be determined by mutual consensus for each GI proposal. Normally the instrument will reside at the PIs institution, where all maintenance and upgrades will be accomplished. The process of data acquisition, reduction, and calibration should be straightforward and transparent to the GI, requiring only a minimal level of assistance from the PI team. Special Purpose Principal Investigator-class Science Instrument (SSI): A special purpose instrument, specifically designed for a particular observation or set of observations not possible or practical with FSI or PSI instruments. This instrument may incorporate technologies at the edge-of-the-art that would be too risky to include in a general-purpose instrument. It is expected that the PI team will operate this instrument. Normally the instrument will reside at the PIs institution, where all maintenance and upgrades will be accomplished. D. Multiple Science Instrument installations shall be accommodated where science productivity will benefit from such an arrangement and where no observatory interface is violated (e.g., science instrument mass and envelope). E. Two separate readiness reviews for each PSI and SSI science instrument will be scheduled and carried out at regular intervals prior to each flight series served by that instrument. The first review will take place approximately ninety days before the flight series. If the science instrument is not demonstrated to be ready for flight, the PI must provide a plan within two weeks for approval by the Observatory Director for achieving readiness by 30 days prior to the flight series. The second review will be thirty days prior to the flight series. If the science instrument is not ready at this time, a backup flight series will be implemented using Facility Instruments. 3.1.2.2 Observing Allocation Policies: A. All U.S. science observing time on SOFIA, except the Director's Time (see G below), shall be allocated by peer review. B. Only single year observing programs will be awarded by the US and German allocation committees for the first three (TBC) years of operations (i.e., FY 2002 - FY 2004 inclusive). C. A study to outline and recommend productive SOFIA Deep Sky Surveys will be performed by a committee in the first year of operations (FY 2002, TBC). The data would be made available to the general science community as soon possible. D. Key Projects and Multi-year Projects will be considered after the first three years of operations (TBC). These will be allocated by peer review. E. Service observing (i.e., straightforward observations of short duration which do not require the presence of the Guest Investigator), using facility science instruments only, will be possible on SOFIA. These will be observations where whole flights are not required, but the observations are considered important enough that the data are taken when possible during flights (of normal duration) on other Guest Investigator programs, over a period of time, and possibly over a number of flight series. Facility scientists in charge of the FSI in use will be responsible for the acquisition of the service observing data. Service observing is awarded and allocated by the peer review committee allocating the science flights for that year. The possibility for service observations will commence in the first year within the engineering flights. F. Targets of Opportunity see Section 3.1.2.8 below. G. Up to five percent of the U.S. observing time can be designated as Director's Time. The Director's Time will not be peer reviewed by the annual allocation peer review committee and shall consist of the following allocation: a) Targets of opportunity not allocated by the annual peer review. These could be allocated by a special peer review set up by the director. b) Staff observing time for projects not granted time by the annual peer review, but deemed important by the director to enhance the science of the observatory staff. This time shall not be peer reviewed. c) Special projects that the director feels are important for the good of the observatory. Time that allows effective and efficient use of scheduling of the telescope. All Directors Time shall be clearly tracked and recorded. The use of Director's Time shall be reported annually to the science council. H. Observations with a particular science instrument will define a flight series: the installation of the science instrument on the telescope will mark the beginning of a flight series, with the end of the series being defined with that instruments removal. Once a science instrument is installed on the telescope it will not normally be removed until the end of the flight series. However, if a problem arises with the instrument during the flight series, the decision to remove or attempt to fix the instrument will be made by the Observatory Director in consultation with the SOFIA Project scientist and the PI. The duration of every flight series will be in units of a week. As a rule, science instrument changes will occur only once every other week. I. Science Instruments, and the SSMOC and science instrument operating procedures, will be designed to accommodate a flight rate of four flights per week. This policy drives: science instrument installation and removal requirements; science instrument maintenance and support requirements between flights; and SSMOC science instrument support (e.g., ground TA simulators). J. In certain cases, either because the PSI or SSI does not satisfy the readiness requirements or the instrument fails within the flight series, a backup observation plan with an FSI may be implemented. All such backup observation plans must have been peer-reviewed. This means that during a PSI or SSI flight series, a FSI is kept in ready mode in case of PSI/SSI failure. It also means that peer-reviewed science plans for FSIs can be executed on short notice (i.e., possibly without the presence of a Guest Investigator). 3.1.2.3 Flight Scheduling Policies: A. The schedule for all flights, including downtime and engineering flights, will be prepared at the beginning of the year. Changes to this flight schedule can only be made with the concurrence of the Observatory Director. As a rule, flight schedule changes must be made at least 30 days (TBC) in advance. An exception will be made for targets of opportunity. B. In order to achieve the required 960 SFH (in a normal flight year), a total of 1285 (TBC) research flight hours will be allocated by peer review and scheduled at the beginning of the year. This figure is based on achieving a system effectiveness (reliability, maintainability, and availability) of 0.80 (TBD). C. No make-up flights for lost science flight time will be allowed. D. There will be approximately five weeks of down-time every five years associated with Continuous Improvement of the Observatory. E. Approximately seven percent of all flights (about 10 flights per year) will be engineering flights. 3.1.2.4 Holiday (10 days of the year) Policies: A. Flights will not be scheduled around major holidays (i.e., Christmas, New Years). B. Flight weeks containing minor holidays (e.g. Labor Day, Memorial Day) will be able to support three flights. C. Three flights may be scheduled for Thanksgiving week (Monday, Tuesday, and Wednesday). 3.1.2.5 Weekend Policies: A. No Flights on Saturday and Sunday except: (a) on deployments (b) for Targets of Opportunity B. Limited (TBD) ground operations on weekends will be supported. C. The SSMOC will support weekend aircraft access for the PI/GI team, including electrical power and network connectivity. 3.1.2.6 Successful Flight Hours (SFH) Policies: Once the flight plan has been accepted by the Observatory, successful research flight hours (SFHs) are those for which: The Observatory is at the specified observing altitude, positioned in the appropriate location and at the appropriate time, as specified in the science team's flight plan, including any planned non-observing time; All Observatory systems critical to the ability of the science team to acquire quality data are operating satisfactorily; and, for flights originating and terminating at the home base, the zenith water vapor overburden does not exceed 10 microns and the cloud cover does not noticeably interfere with data taking. USRA will be held responsible for all aspects of the flight program which affect the ability of the science team to obtain high quality scientific data, except those elements that are under the control of DARA or the PI/GI science team (for example, the performance of the science instrument). For the purpose of estimating total flight time needed to achieve the required number of SFHs, USRA shall assume that TA performance will be the responsibility of DARA. For those research flights where part of the flight is deemed unsuccessful due to single or multiple equipment failure(s), NASA will determine SFH as follows: If the equipment failure is the responsibility of the PI/GI team and/or DARA, the remaining research hours in the flight plan shall be deemed successful, whether or not the Observatory continues to follow the flight plan; If the equipment failure is the responsibility of the Contractor, none of the remaining hours shall be deemed successful unless the failure is repaired in flight, in which case an appropriate reductions in SFH will be assessed; and If there are multiple equipment failures, involving both Contractor responsibility and PI/GI team or DARA responsibility, the NASA Contracting Officer shall determine the principal cause of the failure and assign SFH according to the above two rules. 3.1.2.7 Deployment Policies: A. There will be a main deployment site in the southern hemisphere (probably Christchurch, New Zealand). This will be maintained so it can efficiently support six weeks of operations with five flights a week on average (i.e., weekend flights are allowed). Since there will be multiple flight series within one southern hemisphere deployment, the facilities at this site must support SI preparation and integration procedures. As a rule, a two month deployment to the southern hemisphere will be scheduled each year. B. In the first two years of deployments, facility science instruments will be highly preferred over non-facility science instruments for the southern hemisphere deployments described in A. C. As a rule, all deployments to sites other than the main southern hemisphere deployment site will be single science instrument deployments only. D. Weekend flights will be supported on all deployments. 3.1.2.8 Targets of Opportunity Policies: A. Target of Opportunity requests will be reviewed by a special peer review committee that will be set up by the Observatory Director on an as-needed basis. [[OR]] PIs and GIs can submit Target of Opportunity proposals in response to the normal CFP. These proposals would be reviewed with all others and, if deemed of sufficiently high priority, would be activated if an event occurred. [TBC] B. In cases where Target of Opportunity observations would place an undue burden on the SSMOC (personnel and/or budgetary), the Observatory Director has veto authority in the allocation of time for targets of opportunity. C. Science flights displaced because of the Targets of Opportunity will be compensated in the following year: No make-ups within the same year. D. Special flight times may be considered for targets of opportunity (e.g., weekend flights or non-scheduled flight days) to lessen the impact to the existing schedule. E. If applicable, collaborations between the target of opportunity scientists and the scientists being displaced will be encouraged. 3.1.2.9 International Policies: A. The German science community shall have 20% of the science observing time allocation. This allocation will be selected through a German selection process, and incorporated into the SOFIA yearly flight schedule through a negotiation process between the US Observatory Director and a German selected representative. B. The time requested by a team led by a US GI to use a German science instrument will be charged to US observing time, and will be judged by the US peer review. C. Conversely, the time requested by a team led by a German GI to use a US science instruments will be charged to German observing time, and will be judged by the German peer review. D. Non-German and Non-US science flights will be supported by the SSMOC if successfully reviewed by either the US or German peer review committees. However, no US science grant money will be provided for non-US investigators. E. The Airborne Observatory and SSMOC will endeavor, where possible, to support special needs of the German science teams (e.g., 220 volt, single phase, power supply, TBD). 3.1.2.10 Education and Public Outreach (E/PO) Policies: A. All SSMOC personnel shall support the Education and Public Outreach at a level of 5% per person on average. The E/PO personnel will be nearly full-time on E/PO. B. The E/PO personnel shall devote approximately 5% of their time in support of the observatory and science effort (e.g. science web site development). C. The E/PO activities in the SSMOC and on the aircraft shall not interfere with the science productivity of SOFIA. D. The average E/PO passenger complement per science flight shall not exceed 3, including the E/PO facilitator. Under special circumstances, the Observatory can accommodate up to 10 E/PO passengers. 3.1.2.11 Data Center Policies (See also Paragraph 4.11: A. The data center will store all raw science data (for backup). The data center will archive all mission housekeeping data. The data center will update an investigator's comments about his/her flight series with a list of publications resulting from the SOFIA observations. These data center entries will be made available to future SOFIA peer review members and the science community on the WWW. 3.1.2.12 Safety Policies (See also Paragraph 4.1): A. The SOFIA Airborne Observatory will fly under NASA Safety Policies and under FAA FAR Part 121. If a conflict arises, the more stringent requirements will be implemented. B. The Observatory Director will have an independent SRM&QA staff to assure safety processes are in place and are correctly implemented. This SRM&QA staff will not be part of the day to day safety procedures. The SRM&QA manager has independent access to the USRA President, the USRA SOFIA Board of Directors and the ARC SEMA Office. C. Day to day operations, executed in accordance with USRAs approved safety plan shall be the responsibility of properly trained and qualified operations personnel. Personnel will follow standard UAL safety procedures modified as needed for SOFIA and approved by NASA and the FAA. D. FAA-certified UAL personnel will have the ultimate authority with respect to assessing the airworthiness of the Airborne Observatory after any maintenance work has been performed on it: No flight will be dispatched without formal clearance from the designated UAL dispatch officer for that flight. E. The Captain in Command, for a particular SOFIA flight, has the ultimate responsibility and authority for flight safety during that flight. The Captain also has the authority to cancel a flight even after a certified UAL person has authorized its dispatch. F. Neither the Observatory Director nor any SSMOC line manager will be able to overrule the decision of the certified UAL dispatch officer or the Captain in Command in regards to the dispatch of a flight. G. SOFIA will be tracked in United Airlines Aircraft Maintenance and Information Systems (AMIS). Both the aircraft and flight critical components will be tracked by this system. This record shall serve as the Record of Maintenance Work Accomplished. 3.1.3 Operational Constraints 3.1.3.1 Budget: Both the development and operations budgets for SOFIA place constraints on operations. Budget constraints during system development can result in a lower SOFIA Airborne Observatory System Effectiveness (see Section 3.1.3.3 below), thus requiring more efficient operation procedures to compensate. Budget constraints during operations can directly limit the overall efficiency of operations. If an Airborne Observatory System Effectiveness requires a very high flight rate to meet 960 Successful Flight Hours per year (due possibly to limited development funds), then this can only be met if the operations budget can support the staffing, equipment, and inventory required to meet such a flight rate. Refer to NAS2-97001 for the development and operations budgets. 3.1.3.2 Flight Profile of the Airborne Observatory: The zero fuel weight of the Airborne Observatory, as forecast at this stage of the development effort, will be about 366,000 lb. If this is achieved, then in order to maximize successful flight hours (as defined in NAS2-97001) within each flight, science research flight profiles will be either one of the following: Flat Flight Profile: - 0.5 hrs climb; 7.0 hrs at 41,000 ft; 0.75 hrs descent Step Flight Profile: - 0.5 hrs climb; 2.55 hrs at 41,000 ft; 0.1hrs climb; 2.6 hrs at 43,000ft; 0.1hrs climb; 1.65 hrs at 45,000 ft; 0.75 hrs descent. 3.1.3.3 SOFIA Airborne Observatory System Effectiveness and Science Effectiveness: The SOFIA Airborne Observatory Availability is assumed to be 0.91, which is the product of the availabilities of the Aircraft (0.97), MCCS & Aircraft Modified Systems (0.97) and the Telescope Assembly (0.97). The SOFIA Airborne Observatory Mission Reliability is assumed to be 0.88, that is a Mean Time Between Failures (MTBF) of 60 hours with an 80% confidence. This reliability is the product of the mission reliabilities of the Aircraft (0.985, MTBF=463 hrs), MCCS & Aircraft Modified Systems (0.947, MTBF= 129 hrs), and the Telescope Assembly (0.947, MTBF=129 hrs). Total SOFIA Airborne Observatory System Effectiveness is assumed to be 0.80, which is the product of the SOFIA Airborne Observatory Availability and SOFIA Airborne Observatory Mission Reliability . Total Science Effectiveness is assumed to be 0.78, which is the product of the SOFIA Airborne Observatory System Effectiveness (0.80) and the Science Instrument Effectiveness (0.97). 3.1.3.3 Number of Science Flight Weeks Available per Year: Total number of weeks available to fly science flights is about 44 per year (on average), since: (a) Total maintenance downtime required for the Airborne Observatory (including required maintenance) is assumed to be 4 weeks (on average) per year (see Section 4.8). However, for years with heavy aircraft maintenance (for HMV-Checks or higher, see Section 4.8), maintenance downtime could increase to about 10 weeks or more. It is important to note here that downtime is when the Airborne Observatory cannot support a flight series: Maintenance which can be performed during a flight series is NOT included in downtime, if it does not limit the flight rate of the Airborne Observatory. (b) Total time per year for engineering flights and deployment ferry flights (i.e., non-science flights) is assumed to be 2.5 weeks. (c) Downtime associated with holidays (summarized in 3.1.2.4.) is about 1.5 weeks (mostly around Christmas/New year). (d) No observatory time is assumed to be used for pilot proficiency training. This training will be carried out on ground flight simulators at the UAL facility in Denver, CO. 3.1.4 Operational Environment and Support 3.1.4.1 Moffett Airfield Figure 3.1.4.1 -1 shows the location of the SSMOC at Moffett Field, and the adjacent ramp and runway facilities. 3.1.4.2 SSMOC Facility: Hangar N211 & GSE Figures 3.1.4.2 -1 through 3.1.4.2-3 show the floor plan of the SSMOC. 3.1.4.3 Airborne Observatory System 3.1.4.3.1 MCCS The MCCS consists of the following components: lighting, power distribution, and intercom the console and rack arrangements (LOPA) computer services and equipment Mission Controls System (MCS) capabilities and human interface There will be general area lighting (dimmable on request) and lighting local to each work area (controlled individually). Intercom services will be provided and their use will be required at certain times during the flight (e.g., at takeoff); their use at other times is optional but recommended. 120V 60Hz power will be provided in standard connections (for the racks) and plugs (for individual items) at each general work area. Several seating and console arrangements on the aircraft will be available upon request, but the overall Layout of Personnel Accommodations (LOPA) will not change considerably from flight series to flight series. Seating and console arrangements will be as ergonomic and configurable as possible, given aircraft flight worthiness constraints. Standard consoles containing computers, work space, and power outlets will be available for use by investigators and other users (as defined in Section 1.2 above) as part of the LOPA. The LOPA will make provisions for required ground operations as well as flight operations (e.g., science instrument ground installation and servicing). Figure 3.1.4.3-1 shows the nominal SOFIA LOPA. At least one Unix computer will be available for investigator use for quick-look data reduction and as a remotely networked control station; additional computers can be provided if they are available. A color printer (letter-size paper) will be dedicated to investigator use and located near the investigators area. Standard networking interfaces (ATM and Ethernet) will be available. Standard Unix utilities and a variety of data analysis tools and libraries (IDL, iraf, AIPS, etc.) will be available at the investigator-dedicated computer, and remotely via the network. The MCS will provide a networked interface to all observatory functions. Custom off-line tools (e.g., flight planning) will be available over the network or for installation on investigator-provided computers. Auxiliary data logging capabilities will be provided to investigators, using Unix utilities and archival hardware. Real-time and near-real-time functions will be supported using a defined protocol (the SOFIA Command Language). Investigators will be able to control key observatory functionstelescope positioning and chopper settings being two principal examplesand display any observatory parameter using the SOFIA Command Language. Command responses will be available both immediately and when an operation is complete, and processing delays will be minimal, corresponding to the expected delay for the operation itself (typically less than 20ms for any command-acknowledgment sequence). This interface will be specified in some detail in the SOFIA Command Language specification. All system status parameters will be provided on universal displays for continuous monitoring by all users. The focus for MCCS will be on efficient, reliable science operations, with basic education and public outreach provisions. The MCCS will serve as the central hub of an integrated architecture, with the various observatory subsystems (including the TA) accessible through MCCS interfaces. MCCS will be designed around modular elements, with redundancy as appropriate to ensure mission success. For maximum commonality of hardware, GUI displays and controls will be used (rather than fixed hardware components) whenever possible. 3.1.4.4.2 TA and TA Cavity Figure 3.1.4.4.2 -1 shows a schematic of the telescope in the telescope cavity on the aircraft. Attached to the telescope is a large science instrument. This attachment is made at the science instrument mounting flange.       3.2 Organizational Structure Overview: The SOFIA Airborne Observatory, science and mission operations functions, and ground facilities and equipment will be integrated under the management of the SOFIA Science and Mission Operations Center (SSMOC). This center will be located in hangar N211 at Moffett Field in California. The SSMOC will be under the direction of an USRA appointed Observatory Director, who shall have authority over all SOFIA operations, excluding flight release, which will be controlled as described in Section 4.1. Figure 3.2-1 depicts the SSMOC organizational structure, which will consist of five functional groups below the Office of the Observatory Director: (1) Aircraft Operations and Support, (2) Mission Operations and Support, (3) Science Support, (4) Continuous Improvement, and (5) Education and Public Outreach. The first two functional groups in this list have tasks of considerable scope in the SSMOC and are headed by associate directors, the remainder of the groups are headed by the Project Scientist, Lead Engineer, and Project Educator, respectively. The Observatory Director together with the Assistant Director, Associate Directors, Project Scientist, Project Educator, Lead Engineer, and SRM&QA Manager will form the SSMOC management team, which will decide observatory priorities; the Observatory Director alone sets observatory policies within the policies and requirements set by NASA, DLR and FAA. The management team will attend weekly meetings, with members of the Observatory Director's staff (e.g., the Business Manager), to discuss safety, observatory performance and efficiency, progress in upgrades, science output, and public outreach. They will also address inputs from the science community and the sponsoring agencies. The science inputs will be gathered at annual NASA/DLR-designated SOFIA Science Council meetings, at semi-annual user group meetings, and in bi-annual user workshops. The users group will consist of nine selected SOFIA users with a diverse airborne astronomy background. The SRM&QA Manager oversees the SRM&QA activities within the SSMOC. Although the SRM&QA Manager is under the Observatory Director and will advise the Director on SRM&QA matters, he/she has the authority to bypass the Director and go to the USRA Board of Directors for SOFIA (which includes a UAL representative) if he/she feels the Observatory Director is violating proper SRM&QA practices. The authority flow for aircraft dispatch before each Airborne Observatory flight does not flow through the SRM&QA Manager, though the SRM&QA Manager has oversight over the process for such a dispatch. The Observatory Director may not overrule the decisions of the SRM&QA Manager, the dispatch mechanics or captain in command with regards to any matter relating to safety or readiness to conduct a mission. 3.2.1 Office of the Observatory Director The Office of the Observatory Director will manage all aspects of the SOFIA System, and will set policy and provide the overall management and administrative capabilities for the SSMOC. To this end, this office will organize and facilitate weekly management team meetings (see above). The Office of the Director will be responsible for SSMOC SRM&QA, business, contracts, personnel, and ground facility management; it will have the final authority on all SSMOC financial and contract matters, on all top level schedule decisions, and all personnel issues. The Office of the Director will handle the logistics and expenses for the advisory groups associated with SOFIA, and will be the SSMOC interface with USRA, NASA and DLR. It will be responsible for the preparation of the annual Call for Proposals for observing and the tri-annual Call for Proposals for the development of science instruments. This office will provide the logistics for the peer review processes and contract awards. The Office of the Director will contain a German Assistant Director to handle all German collaboration and support issues. 3.2.2 Aircraft Operations and Support (AOS) Group The Aircraft Operations and Support Group will be responsible for the operations and support of the Aircraft System (see Section 1.1). Maintenance for the Aircraft System will be designed and tailored for minimal impact to mission operations, and for maximum reliability and cost-effectiveness while meeting all requirements for safety and airworthiness. Scheduled line-maintenance, which includes routine pre/post flight checks, aircraft washes, "A" and lesser service checks (see Section 4.8), and small non-routine maintenance will be accomplished at Moffett Field. Heavy scheduled maintenance (e.g., "C" and heavier checks) will be accomplished at UAL's maintenance operations centers located at San Francisco or Oakland. For unscheduled maintenance, the AOS group will work with UALs line maintenance support system, headquartered in San Francisco Airport (SFO), which includes System Aircraft Maintenance and Control (SAMC), to quickly ascertain the repair requirements and plan to complete the unscheduled work as efficiently as possible. The AOS group will have the logistics support structure responsible for management of the Aircraft System inventory, including spares acquisition and purchased equipment repairs, as well as aircraft deployment kit management, support equipment maintenance, technical data, and aircraft support facilities at the SSMOC. UALs automated inventory control real-time system will be used to obtain and track SOFIA Aircraft System parts and inventory in real-time. The AOS group will also have the responsibility for training and configuration management for aircraft support and operations. The AOS group will have the functional responsibility and personnel to accomplish the planning and generation of every SOFIA flight in regards to the Aircraft System: it will directly prepare the Aircraft System and flight deck crew for each flight. In addition, the AOS group will monitor and coordinate any maintenance performed by other SSMOC groups on the Airborne Observatory (e.g., on the telescope or MCCS) and installed science instruments, and will assist where and when mutually agreed. The AOS Group will be responsible for the final Airborne Observatory maintenance release and flight dispatch as detailed in Section 4.1. FAA and NASA-approved UAL procedures will be followed for all maintenance performed on the Airborne Observatory and science instruments installed on the Airborne Observatory. The SFO-based UAL Maintenance Operations Center (MOC) will interface with the AOS group and the FAA to address any FAA concerns, and will conduct Quality Assurance audits periodically to demonstrate compliance to procedures and regulations. 3.2.3 Mission Operations and Support (MOS) Group The Mission Operations and Support (MOS) Group will be responsible for the operations and support of the Mission System (see Section 1.1). The MOS group will provide maintenance for the telescope assembly (TA) and subsystems, mission controls and communications systems (MCCS) and software, cavity environmental control system (CECS), unique support equipment, simulators, and mirror coating and cleaning. Maintenance of Mission System calibration and performance testing equipment will be supported in collaboration with scientists in the Science Support Group. Maintenance of the cavity will be carried out in coordination with the Aircraft Operations and Support Group and will include work on cavity bulkheads, door, shear layer control, cavity components, cavity surfaces (including paint) and cavity cleanliness. Personnel in the MOS group will also provide investigator lab and associated facilities, and data center support. The MOS group will have the logistics support structure responsible for management of the Mission System inventory, including spares acquisition and purchased equipment repairs, as well as mission deployment kit management, support equipment maintenance, technical data, and mission system support facilities at the SSMOC. The MOS group will set up and manage a closed inventory tracking system within the SSMOC that emulates the UAL inventory system. This system will keep track of FAA certified parts as well as parts not requiring this certification. The inventory storage will keep these parts separate, as in the UAL inventory. Inputs to the SSMOC inventory system will come from all SSMOC groups except the AOS group, which will use the UAL tracking system. The MOS group will also have the responsibility for training and configuration management for mission support and operations. AOS personnel from UAL will monitor this training, to assure compliance with the NASA and FAA approved procedures. The Mission Operations and Support Group will have the functional responsibility and personnel to accomplish planning and generation of every SOFIA flight in regards to the Mission System (i.e., the MCCS, TA, and TA cavity). The MOS group will prepare for flight the mission crew, the science investigators, and educators, with assistance from scientists and educators from the Science Support and E/PO groups. The MOS group will also help to ready the science instrument for flight with the assistance of the Science Support group and the science team (see Section 3.2.4 below). The Mission System will be maintained in compliance with NASA and FAA airworthiness requirements by MOS technicians and engineers following approved procedures, assured by the oversight of engineers and technicians in the MOS group who are qualified to verify that maintenance has been performed to these procedures. In addition, this oversight is monitored by the FAA certified UAL dispatch officer in the AOS group who has the final dispatch authority for the Airborne Observatory. 3.2.4 Science Support Group Interactions between the science community and SSMOC will be coordinated by scientists within the Science Support Group and the Observatory Director. Communication will be in the form of the SOFIA web-site, workshops, investigator handbooks, data center and user group meetings. The main task of the Science Support Group is the coordination of Principal Investigator (PI) and Guest Investigator (GI) support before, during, and after a SOFIA flight series. This support includes assisting the Office of the Observatory Director in the preparation and execution of the Call for Proposals/Peer review process for science instrument development and observing time. It also includes support for the science instrument developers in the areas of FAA Certification, interface compliance with the SOFIA Airborne Observatory, and science instrument installation and logistics (see Section 4.4). This group will also operate and support the facility science instruments with assistance from personnel in the MOS group. They will assist GI's with data reduction, and with the use of the SSMOC data center. Science Support Group personnel will be key in analyzing the performance of the telescope, and in maintaining some test equipment (e.g. the near-infrared test camera). These personnel will also help maintain those mission system instruments which are similar to science instruments (e.g., the water vapor monitors). The science instruments will be maintained either by MOS technicians or Science Support scientists, if it is a facility science instrument, or by an outside science team, if it is a PI or Special science instrument (see Section 3.1.2.1). In any of these cases, there will be at least one qualified technician or scientist to sign-off on a science instrument installed on the Airborne Observatory to verify that maintenance and installation was performed using NASA and FAA approved procedures. The Science Support group will assure that each external science team has such a qualified person, and that that person receives the correct training as specified by UAL in conformance with NASA and FAA requirements. This individual will assure proper configuration control of and airworthiness certification of changes to the SI when it is at the PIs home institution. All such SI changes will be documented for review by certified SSMOC personnel and for retention in the SSMOC data system. As with the Mission System, final airworthiness inspection and dispatch authority in regards to the science instrument belongs to the FAA certified UAL dispatch officer in the AOS group. The Science Support Group will support education and Public Outreach program activities to assure accuracy of E/PO products and materials; to support timely release of scientific discoveries; to review web content for accuracy and appropriateness; to present at workshops, meetings and symposia; and to support E/PO guests on flights in coordination with the E/PO flight facilitator. 3.2.5 Continuous Improvement Group The Continuous Improvement Group is charged with translating inputs from the science community, SSMOC staff, and performance metrics into design concepts with development plans, budgets, and schedules for potential facility upgrades. These will be discussed, authorized (or rejected), and prioritized within the SSMOC management team. (Note: NASA has approval authority on major upgrades or those with airworthiness implications see Section 4.9). This group will manage all approved upgrades and new designs. This group is small (see Section 3.3.5), but once an upgrade has been approved, this group will expand as necessary to fulfill the tasks of the upgrade using subcontracts, and personnel (if appropriate) from the other SSMOC groups. The Continuous Improvement group will: write the statement of work for the subcontract; approve final designs; coordinate the engineering and fabrication work with mission system and aircraft schedules through the Operations Control Center (see 3.2.7); make sure these are NASA and FAA approved and compliant; supervise integration and test of the upgrade; accept the new systems; manage the development and receipt of all new documentation associated with the upgrade; and supervise the training of SSMOC staff in regard to the upgrade. After the upgrade is complete and integrated, the Continuous Improvement group will resume its original number of personnel. 3.2.6 Education and Public Outreach Group The Education and Public Outreach group is responsible for the interactions between the SSMOC and the formal and informal educational community, including K-12 level, undergraduate and graduate students, and the general public. The E/PO team (see 3.3.6) will develop and conduct flight education programs as well as ground-based education programs. The group is also responsible for the public image of SOFIA through the conduct of public relations and services with the media (electronic, print, broadcast, internet, and science writers) in coordination with NASAs Office of Public Affairs. The group is responsible for prompt and accurate communication of the scientific and technological achievements of SOFIA to educators and the public. 3.2.7 Operations Control Center The Operations Control Center is not a separate functional group in the SSMOC, but a small group of SSMOC personnel, from a number of SSMOC functional groups, which is responsible for maintaining the master schedule and mission planning for the entire SSMOC: Its main task is to coordinate and integrate SSMOC activities. The Operations Control Center will take inputs from all SSMOC functional groups, and will integrate the maintenance schedule with the operations schedule of all SSMOC functions on yearly, monthly, weekly, and daily time scales. It will handle the logistics for deployments, especially in shipping equipment and setting up SOFIA support at deployment sites. The center will be headed by the AOS and MOS associate directors, but the day-to-day monitoring of the schedule and coordination of the Airborne Observatory operations and support will be the task of the AOS Controller and AOS Maintenance Team Leader, respectively, who are part of the Operations Control Center. 3.3 Personnel profiles The SSMOC will have 88 full-time staff members, who are described below. This number will increase temporarily (through temporary contracts) by about 10% in times of upgrades. Besides the full-time SSMOC staff, there will be visitors temporarily accommodated at the SSMOC (these do not include visitors on daytime tours). These visitors will include scientists, students, and education specialists such as teachers. Their stay at the SSMOC will range from a few days to a few months. It is expected that the SSMOC must accommodate at any given time a total of about 20 visiting scientists associated with a past, current, or future flight series. This number will grow if the data center becomes a place where scientists will come to reduce and analyze SOFIA data. The E/PO program is expected to have on average 4 visiting educators at any given time. In addition, up to 18 E/PO visitors could be at the SSMOC for a week or more to prepare for a flight or to participate in an E/PO workshop. (The SSMOC ground facility, hangar N211, is being modified to house 99 SSMOC staff, 20 visiting scientists, 4 visiting educators, and a classroom to seat 49.) The staffing level of the SSMOC will be sufficient for a 24 hour per day operation on the week days. However, the staffing level will be minimal on the weekend. This minimal level will enable continual access to the aircraft and assure availability of aircraft electrical power, aircraft connectivity to the computer network, and limited science instrument servicing (e.g., refilling cryogens), but will not normally be sufficient for removal or installation of science instruments or reconfiguration of the telescope (e.g., new tertiary mirror) or any substantial maintenance. 3.3.1 Office of the Observatory Director Personnel The Observatory Director is a USRA senior astronomer with observatory management experience. He/she is the official spokesperson for SOFIA to USRA, NASA, DLR, and the science community. The director is the final authority over all SOFIA activities (except flight release); is the single point-of-contact with the NASA SOFIA Program organization and interacts with the NASA/DLR designated SOFIA external Science Council; supports all NASA annual reviews for science policy and budget; and is responsible for the peer review process for science instruments and observing time. The Assistant Director is a USRA person with a technical management background. The assistant director is responsible for all technical and management aspects across the breadth of SOFIA operations; ensures that sound operations processes and engineering practices and methodology are applied in all activities; monitors the SSMOC schedule and plan maintained by the AOS group. German Assistant Director is a German support person with direct connections with the German scientific and technical communities. He/she is responsible for all German personnel and issues at the SSMOC. The German Assistant Director shall be the Observatory Directors spokesperson for the SSMOC to the DLR. The SRM&QA Manager is a USRA person responsible for the overall direction of Safety, Reliability, Maintainability & Quality Assurance activities across the SOFIA operations. He/she assures the existence and consistent implementation of sound processes and procedures for Safety, Reliability, Maintainability and Quality Assurance. The Business Manager is a USRA person responsible for all activities associated with finance and accounting, cost and schedule control and performance assessments, grants, contracting and acquisition, human resources, legal, mentor-protg plans and activities and Small Business/Small Disadvantaged Business goals and plans. The Administrative Staff consists of USRA personnel with the appropriate backgrounds for the following positions: contracts manager, personnel manager, facility manager, observatory director administrative assistant, accountant, accounting assistant, payroll technician, and two office managers. 3.3.2 Aircraft Operations and Support Group Personnel Associate Director for Aircraft Operations and Support is a UAL person with an aircraft operations management background. This person is responsible for the planning and implementation of all Aircraft System operations and maintenance, ground handling and aircraft support personnel and facilities to ensure success of SOFIA science missions; has the primary responsibility for all SOFIA operations decisions in the best interest of safety and schedule dependability consistent with UAL policies and procedures conforming to NASA and FAA requirements. Operations Controller is a UAL person who has the main responsibility of formulating (with inputs from other SSMOC groups) and communicating the SSMOC integrated master schedule and plan. The master schedule is formulated on a multiple number of time periods (yearly, monthly, weekly, and daily). The master schedule does not only incorporate aircraft schedules but those of all the other aspects of the SSMOC (mission system, science, education, administrative). Aircraft Engineer is a UAL person with an aircraft engineering background and the necessary certificates. This person has the prime responsibility to assure the airworthiness of flight and maintenance operations. UAL Business Analyst is a UAL person with a business management background. This person is responsible for all activities associated with UAL finance and accounting, cost and schedule control and performance assessments. Aircraft Support Staff consist of UAL personnel with the appropriate backgrounds and certificates for the following positions: team leader, chief mechanic, 6 aircraft mechanics/avionic technicians, and an inventory manager. These personnel execute all aspects of aircraft maintenance and ground support. All the SSMOC inventory will be integrated under the UAL inventory control system. Flight Crews are dedicated crews for SOFIA from Flight Crews International (FCI). There will be two such crews. Each crew will consist of three personnel covering the captain, first officer, and second officer positions. These crews will possess all qualifications and certificates required by NASA, the FAA and UAL, and will have undergone formal difference training for the SOFIA aircraft provided by specially-configured UAL training systems. When necessary, flight crew members will be augmented with UAL test pilots possessing proper SOFIA qualifications. 3.3.3 Mission Operations and Support Group Personnel Associate Director for Mission Operations and Support is a USRA person with a technical management background. This person is responsible for the planning and implementation of all Mission System operations and maintenance, ground handling and Mission System support personnel and facilities to ensure success of SOFIA science missions. Mission System Engineering Staff consists of one senior software engineer (Sterling Software), two senior mechanical engineers (1 German, 1 USRA/Raytheon), two senior electrical/electronic engineers (1 German, 1 USRA/Raytheon), and 3 junior mechanical/electrical engineers (1 German, 2 USRA). The engineering staff is responsible for configuration control of the Mission System design database, manuals, and other Mission System documentation. They are responsible for planning and directing Mission System maintenance efforts and formulating Mission System NASA and FAA approved support plans and procedures. In times of upgrades, they will work with the continuous improvement group. Mission System Technical Staff consists of 10 electrical/mechanical technicians (5 German, 5 USRA), two USRA software specialists, and one lab facility technician. These personnel execute the maintenance and ground support of the Mission System, which includes the TA, cavity, MCCS, and ground support equipment associated with the Mission System. Those technicians with Mission System dispatch sign-off authority will be appropriately qualified and certificated. Mission System Flight Staff consists of three German flight TA operators, two USRA flight computer specialists, and 3 USRA flight mission directors. These are technical positions and are optimally matrixed with the MOS technical staff. These are the members of the MOS staff who fly on science missions and provide observatory operation support (see also Section 4.7). The mission directors will be experienced flight operations personnel with appropriate backgrounds and demonstrated capabilities to perform in this important position. Data Center Librarian is a position requiring computer skills in high-level computer languages. This USRA person will maintain the science data center, and will help visiting scientists use the data-bases stored or accessible from the data center (including reference books and journals). SSMOC Web-Master will support the scientific and E/PO communities via the internet. The web master is responsible for development and maintenance of the SOFIA web-site. SSMOC Network Staff consists of three Sterling Software network specialists. The SSMOC computer network and general purpose software will be managed and maintained by these specialists. 3.3.4 Science Support Group Personnel Project Scientist is a USRA senior scientist. This person is responsible for all science community involvement with SOFIA; is responsible for science interfaces with SOFIA users and SOFIA operations; and is responsible for making sure the science instruments for SOFIA are operating, integrated into SOFIA, and available as required. The project scientist is expected to carry out his/her own research 50% of the time. Staff Scientists consists of three senior scientists (2 German, 1 USRA), four junior scientists (1 German, 3 USRA), and three half-time University of California Scientists. They are to provide science support to SOFIA users, and to help communicate the achievements and status of SOFIA to the science community. Science support includes support of outside scientists building science instruments for SOFIA and for those scientists observing with SOFIA. The scientists in the science staff are expected to carryout their own research 50% of the time. 3.3.5 Continuous Improvement Group Personnel Lead Engineer is a USRA senior engineer. This person is responsible for assessing the Airborne Observatory's performance; is responsible for assimilation of data and requirements and formulation of concepts, plans and budgets for Airborne Observatory improvements for consideration by the SSMOC management team. Once improvements are approved, the lead engineer is responsible for the development effort associated with the improvements. Engineering Staff consists of two USRA/Raytheon senior engineers. These engineers are matrixed with the engineering staff in the Mission Operations and Support group. They support the lead engineer in executing his/her responsibilities. The engineers in this group are a mix of software, mechanical, electrical, and electronic specialists. Temporary Upgrade Staff consists of contractor/subcontractor staff needed to supplement SSMOC staff for the approved upgrades to the airborne observatory. 3.3.6 Education and Public Outreach Group Personnel Project Educator is a S/ASP employee who will have overall management responsibility for all outreach programs not directed at the science community, including public affairs, K-14 education, and public outreach. This individual will directly manage the formal K-14 education programs and some outreach programs. Manager of Public Affairs reports to the Project Educator and will manage public affairs and media relations in close cooperation with NASA External Affairs. This individual will also manage some of the public outreach programs and will also be responsible for the overall architectural design and organization of the SOFIA website. Two Public Affairs Specialists will report to the Manager of Public Affairs. They will have day-to-day responsibility for press relations, press visitors, and other media relations activities. They will also have responsibility for some of the public outreach programs. They will be trained as E/PO flight facilitators and members of the mission crew. Two Education Specialists will report to the Project Educator. They will conduct ground-based and flight-based programs including development of educational programs and products, and hosting of educational visitors. Education specialists will be trained as E/PO flight facilitators and will be trained as members of the mission crew. One Administrative Specialist will support the E/PO team administrative needs and will report to the Project Educator. 4.0 Operational Processes Overview: SOFIA will operate over a 20-year period. Its main location of operation will be from Moffett Field in California, where the SSMOC (and airborne observatory) will be housed in hangar N211. A typical science flight will take-off from Moffett Field and land at Moffett Field. However, since a large fraction of the sky cannot be seen from the northern hemisphere, a long (about 2 months) deployment each year must be made to the southern hemisphere, to Christchurch, New Zealand (TBC), between May and August. At Christchurch, science flight series and flights will have similar characteristics to those from Moffett Field. Typically, about four flight series per Christchurch deployment will be executed, so the installation and deinstallation of science instruments must be possible in this deployment site. SOFIA will also have to spend about two to three weeks of the year being deployed to anywhere in the world because of occultation/eclipse studies. The location of the deployment depends on the track of the occultation/eclipse shadow across the Earth. These flight series will typically be short (about 10 days), and typically involve only one (or combined) science instrument and so installation and removal of instruments can usually occur at Moffett Field before deployment. Each year, a total of 960 successful flight hours at altitudes e" 41,000 ft must be achieved. Successful flight hours are achieved when all components of the SOFIA airborne observatory (i.e., the aircraft, MCCS, telescope, and cavity mechanisms) and the science instrument (TBD) are operating as specified. In order to achieve this number of flying hours per year a total of 137 successful science flights must be made per year with the flight profiles outlined in Sections 3.1.3 and 4.7. If we assume a total science effectiveness of 0.78 (see Section 3.1.3) then the total number of flights which must be planned for are 176, of which 16 will not actually takeoff, and another 23 are expected to be unsuccessful after takeoff. This translates to four science flights per week on average spread over 44 weeks, with the remainder of the year (8 weeks) used for airborne observatory maintenance requiring downtime (4 weeks), and downtime associated with engineering flights, deployment set-up and ferrying, and SSMOC holidays (a total of 4 weeks). Figure 4.0-1 (preliminary) summarizes the 20 year Level-1 Schedule for the SOFIA System. It shows the aircraft maintenance check schedules (see Section 4.8.1.1), the schedule for mission operations and planned upgrades, and the schedule for the peer review process which is used to select science investigators each year (see Section 4.2). On average there will be approximately 50 investigator teams awarded flights each year. Of these 50, some will be Principal Investigator (PI) teams and some will be Guest Investigator (GI) teams. PI's are scientists who will operate their own science instruments on SOFIA. GI's are scientists who will either use facility science instruments or PI science instruments (see Sections 4.2 and 4.3). On average there will be 20 installations/deinstallations of science instruments per year on the telescope. Some science instruments will be used more than once throughout the year. Each installation of a science instrument defines the beginning of a "flight series"; the termination of the flight series is defined by the science instrument's deinstallation. For operational convenience, a flight series will be a multiple of a week in length; on average a flight series will be two weeks in length (see Sections 4.4 and 4.5). This means that on average a flight series will support about 2 to 3 investigator teams, one of which could be a PI team (see Section 4.7). Figure 4.0-2 (preliminary) shows a top level schedule for a one week long flight series which follows a short deployment to Brazil. This schedule illustrates how a science instrument is being readied in the SSMOC for a flight series while another science instrument is being flown. It also shows how four flights are planned for one week of operations at Moffett Field, and how a science instrument is installed on the aircraft on a Monday, and removed on a Friday once the flight series is ended . Science flight take-off times range from 1600 to 2330 (PST), and landing times range from 0030 to 0800 (PST) (see Section 4.6.1) for night flights, although a few investigator teams a year (about 3) may need daylight science flights (e.g., solar eclipses or observations of Venus). The staffing level of the SSMOC will be sufficient for a 24 hour per day operation on the week days. However, the staffing level will be minimal on the weekend. This minimal level will enable continual access to the aircraft and to assure aircraft electrical power, aircraft connectivity to the computer network, limited science instrument servicing (e.g., refilling cryogens), but will not normally be sufficient for removal or installation of science instruments or reconfiguration of the telescope (e.g., new tertiary mirror) or any substantial maintenance. Figure 4.0-3 (preliminary) shows a top level schedule for a back-to-back flight day at Moffett Field (see Section 4.6.1). Sections 3.1.3 and 4.7 show the typical flight profiles to be used for science flights. These are about 8.25 hours long with 7 hours at altitude. Typically, the seven hours at altitude will be divided into about 6 flight legs (but can range from 2 to 16). Each flight leg allows the investigators to observe one location on the sky. Figure 4.0-4 (preliminary) shows the top level schedule for the first flight leg on a flight (see Section 4.7.5).    4.1 SRM&QA and Airworthiness Processes This section contains top-level descriptions of SRM&QA and airworthiness processes, particularly the process to be followed to dispatch the Observatory for flight. Detailed process descriptions will be developed by the USRA team and included in the SOFIA Operations Plan (Deliverable No PM17), which will require NASA SOFIA Project Office approval. The NASA SOFIA Project Office will obtain review and approval of the Plan from the Ames SEMA Office, the AFSRB, and the Office of the Ames Center Director, prior to its getting approval for the start of the SOFIA operations phase. During SOFIA operations, the SSMOC staff will be tasked with implementing all of the daily operations of the Airborne Observatory, including Safety, Reliability, Maintainability and Quality Assurance (SRM&QA), and airworthiness and flight safety processes. These will be implemented by following operation and maintenance plans and procedures developed specifically for SOFIA by the USRA team, which will be approved by NASA and the FAA, and continually reviewed through the monitoring of performance metrics, and by performing internal spot checks and audits. The Airborne Observatory operations will be conducted in accordance with FAA FAR Part 121. UAL standard maintenance and operations procedures will be followed, with necessary modifications for SOFIA, as documented in procedures and work instructions used by operations personnel. During system development, the USRA team will develop the necessary SOFIA-specific operating and maintenance procedures. Maintenance and operational check procedures for Aircraft System items and some Mission System items will be included with the standard UAL maintenance program. All other Mission System items will be maintained in accordance with approved procedures specific to SOFIA. During the SOFIA operations phase, the SSMOC staff will continue to examine ways to improve the observatory through its Continuous Improvement Program (see Section 4.9). For continuous improvement projects during operations (such as system upgrades or enhancements) SOFIA-specific maintenance and operating procedures will be developed as part of each project, and will be integrated with UAL processes as necessary. SOFIA upgrade designs and maintenance plans will be subject to approval by NASA and the FAA. The SOFIA airborne observatory will obtain airworthiness approval by NASA and certification by the FAA in all of its planned operating configurations before initiating the operations phase. That is, all of the initial suite of science instruments and their installations will have airworthiness approval. As new SIs are brought into operation at approximately 3-year intervals, they will also have pre-approved configurations and installations. SI configurations will be controlled between flight series such that any changes to their designs will require airworthiness review and approval, and certification update as needed. The SIs will be changed out on SOFIA at intervals of about every 2 weeks, and these are the only changes that are to be made to the Observatory configuration on a routine basis. The day-to-day airworthiness and flight dispatch process is thus amenable to a pre-developed, routine procedural and work-instruction-based activity, with inspection and signoff by qualified operations personnel. Two conditions must be met as a requirement to dispatch the Observatory on any flight: 1) The Observatory and its subsystems must meet all airworthiness and flight safety requirements, and 2) All requirements for science mission readiness must be satisfied. These conditions are evaluated by properly qualified and certified personnel using the process shown in figure 4.1-1. The critical characteristic of the process shown is that all requirements pertaining to airworthiness and flight safety are addressed on the left side of the chart, and all issues pertaining to science mission readiness or effectiveness are addressed on the right side of the chart. 4.1.1 Safety for Flight Dispatch The left side of figure 4.1-1 shows the major components of the Airborne Observatory - the aircraft, the mission systems, and the installed science instrument. Each of these components has a dispatch mechanic/technician who is properly trained and authorized to inspect and sign-off that component as ready and safe for flight. UALs approved sign-off procedures will be followed. In addition, the flight plan must be approved by the flight crew, from the standpoint of flight safety, e.g., proper fuel load for the flight, weather conditions, etc. The final safety sign-off for flight is performed by the fully qualified FAA certificated, UAL aircraft dispatch mechanic, with inputs from the other dispatch technicians. No one within USRA, the USRA team or NASA has the authority to overrule a dispatch mechanics decision that the Observatory is not safe or airworthy. 4.1.2 Mission Readiness for Flight Dispatch The right side of Figure 4.1-1 shows the elements of mission-readiness that must be evaluated for each flight. These elements are unrelated to airworthiness or safety but are associated with the determining the expected science return of a specific flight. The Mission Director will decide whether or not the Observatory is ready to perform its science mission and has the responsibility and authority to sign off for mission readiness. The Mission Director will rely on inputs from the: Lead scientist as to whether or not the science instrument and science team is ready, Mission System staff on whether the mission systems and staff are ready, Education and Public Outreach coordinator on whether the E/PO equipment and participants are ready for flight. Mission readiness will depend on the status of the science instrument installed, the science objectives for the flight, the status of the telescope and related systems, and other factors related to the specific mission to be conducted. The Mission Director will also review and approve the flight plan from the science and mission standpoint, and assure that any other mission-critical requirements are met. 4.1.3 Mission Management and the Flight Dispatch Decision Once the UAL aircraft dispatch mechanic has determined whether or not the Observatory is safe and airworthy and the Mission Director has evaluated the mission systems from a mission readiness perspective, a briefing is conducted with the USRA Mission Manager. The Mission Manager is where the left side (safety) and right side (mission readiness) of the flight dispatch process of figure 4.1-1 come together. The Observatory Director or an appropriately qualified designee will fill the position of Mission Manager. The function of the Mission Manager is to provide: USRA and the Observatory Director oversight and management control of the flight dispatch process with regard to safety and cost effectiveness in achievement of the annually required 960 SFH. Determination that every mission is not only safe, but also whether or not a mission is expected to be effective in terms of the science return. Briefing of the Mission Manager is conducted regardless of whether the Observatory is considered safe or ready so that the team, under the leadership of the Mission Manager, can determine: whether all outstanding safety or mission system performance issues can be resolved in accordance with approved procedures in order to support a late, rescheduled Observatory departure. whether flight plans or mission science criteria can be modified in order to accomplish the mission in spite of some loss of science. whether the mission will be cancelled. Even if the UAL dispatch mechanic has signed off that the Observatory is safe and airworthy, the Mission Manager is empowered to stop a mission if he/she has any safety concern. In no case does the Mission Manager have the authority to dispatch the Observatory if the authorized dispatch mechanic determines that the Observatory is not safe or airworthy. With safety and airworthiness concerns closed, the Mission Manager, with input from the Mission Director, will determine whether or not the mission will be effective in meeting the mission goals and the objectives of the Observatory Director. The Mission Manager does have the authority to overrule the decision of the Mission Director as to the effectiveness or readiness to conduct the mission. This entire process is overseen by the USRA teams SRM&QA organization, which is authorized to halt operations at any time if unsafe conditions are believed to exist. Once the Mission Manager has determined that all safety, airworthiness and mission readiness/effectiveness requirements have been met, the decision to fly is passed to the Captain in command. FAA regulations, as well as UALs established maintenance release process, place the ultimate responsibility and authority for safe operation of the Airborne Observatory in the hands of the Captain in command. The Captain in command has the final authority and responsibility for dispatch of the flight, based on the inspection of the aircraft by the flight crew and the dispatch material provided by the dispatch mechanic. No one has the authority to overturn a decision by the Captain in command not to fly. NASA will monitor the flight dispatch process and operations through audits and spot checks, and by reviewing the Airborne Observatory's performance metrics. In addition to NASA audits, which include those by the SOFIA Operations Office, the SEMA office and the AFSRB, the SSMOC will also be subject to UAL and FAA audits in regards to the airworthiness and flight safety aspects of operations.  4.2 Call for Proposals/Peer Review for Science Instruments and Observing Time Starting during SOFIA development, a peer review process will be set up to enable the science community to develop a complement of science instruments for the beginning of SOFIA operations in GFY (Government Fiscal Year) 2002: There will be one such call in GFY97 and another in GFY00. This peer review process will be extended in GFY01 to include proposals from investigators requesting observing time for GFY02. During development, the USRA Team will conduct the SOFIA peer review at USRAs Lunar and Planetary Institute (LPI) near the Johnson Space Center. During operations, the peer review process will be managed and conducted at the SSMOC at Moffett Field. Each year starting in GFY02, the Office of the Observatory Director and the Science Support Group will develop a Call for Proposals (CfP) for observing time on SOFIA for the following fiscal year period. The user community will be notified in December of each year (via post cards, an AAS announcement, e-mail, and WWW) that the CfP is available on the SOFIA website. Hardcopies will be sent to those who request them. The proposal deadline will be April 1 of each year. After receiving the proposals, the Office of the Observatory Director will distribute them to an expert review panel selected by the observatory director with the NASA program scientist's concurrence. The panel will meet in May to decide annual distribution of SOFIA flight time and grant money. Peer reviewers must assign weights to successful proposals which will be used by the SOFIA flight scheduling program. The NASA SOFIA program scientist will be an ex-officio member of each peer review panel and must concur in all funding and observing time allocation decisions. When results of the U.S. observing time allocation are final, the observatory director will meet with the corresponding German SOFIA science representative to orchestrate U.S. and German allocations. Letters of notification will be sent to all proposers, after selection, by July 1st of each year. With the combined list of U.S. weighted selections, the observatory director, with the SSMOC management team and the Operations Control Center, will produce the final observing time schedule (see Section 4.3). Awards and the yearly flight schedule will be posted on the SOFIA website by August 1st of each year. Funds to the winning proposals for observing will be distributed (pending NASA funding to USRA) as early as possible in the fiscal year of the awarded observations (nominally by November). In parallel with some of the CfP's for SOFIA observing time, there will be a CfP for SOFIA science instrument development. This CfP will solicit investigators for the development of facility class SI's (FSI), principal investigator class SI's (PSI), and special class SI's (SSI). Upgrades to existing SI's of all classes will also be funded through this CfP. The science instrument CfP will have a three year cycle instead of an annual cycle. The first CfP of this kind during operations will be issued in GFY03. The CfP and peer review process will exactly parallel in timing the CfP and peer review process for observing time, but with a different peer review panel. The funding will generally be for three years, but with the status of the science instrument being reviewed each year before subsequent funding is continued. Such reviews will be held by the Science Support Group to ensure that SI milestones are being met. Upon award for observing time or science instrument development funds, each investigator will be contacted by a SSMOC science coordinator; there will be one science coordinator per flight series (see below). This SSMOC scientist will be responsible for orchestrating the investigators interactions with the SSMOC. An investigator awarded observing time with no science instrument of his/her own will be called a Guest Investigator (GI), and an investigator awarded funds to develop a science instrument or awarded observing time with his/her own science instrument will be called a Principal Investigator (PI). The PI's and GI's will be instructed to review the Investigators Handbook on the SOFIA website (hardcopies will also be available upon request). The handbook will include: science instrument interface requirements for the telescope, aircraft (including EMI) and MCCS; the airworthiness certification process for science instruments; SSMOC procedures; and flight planning instructions. It will be possible to download the flight planning program from the SOFIA website. For developers of PSI's and SSI's, final design drawings must be sent to the SSMOC in the second year after award for NASA and FAA certification purposes and a review of telescope, MCCS and aircraft interfaces. For developers of FSI's, formal PDRs and CDRs (including FAA Design Approval) must be completed in the first and second years of development, respectively, followed by an acceptance review after the FSI's first flight series. 4.3 Yearly Scheduling 4.3.1 Normal Scheduling Process The SSMOC will be scheduled on a Government Fiscal Year (GFY) cycle (i.e., October 1 to September 30 of the following calendar year). The schedule for a year will be finalized by August 1st of the GFY prior to the GFY being planned. The schedule's determination will be based on the science flights awarded, the aircraft and observatory maintenance required for that given year, and the constraints of the operating budget for that year. A scheduling program will be used which will take as inputs: i) maintenance down times (see Section 4.8); ii) deployment constraints (or preferences); iii) any other SSMOC time constraints (e.g., holidays); iv) prioritized list of investigator teams with SI's to be used; v) each investigator team's set of preliminary flight plans (a requirement of the CFP) The scheduling program will assist the Operations Controller and the Project Scientist in scheduling the science flights for a year. The year will be divided into flight series, with each normally some multiple of a week in duration for ease of installation and removal of science instruments. Each flight series will have one installation of a science instrument (or a suite of science instruments mounted simultaneously) and one de-installation at its conclusion: The science instrument defines the flight series. The science instrument could be either a facility class instrument (FSI), a principal investigator class instrument (PSI), or a special class instrument (SSI). The FSI will be managed and supported by SSMOC personnel, the PSI and SSI by Principal Investigators (PI's) from the science community. Both the FSI's and PSI's could have a number of different investigators called Guest Investigators (GI's) using them within a single flight series, and all science instruments could have a number of flight series within one year. The final SOFIA science flight schedule will optimally group the observations, the investigators, and the science instruments into flight series which are scheduled so the highest priority astronomical objects of interest can be observed for the length of time required. The need for a deployment (or deployments) will be assessed and if necessary will be scheduled. The scheduling task for all the SSMOC activities resides in the Operations Control Center of the SSMOC (see 3.2.7), with inputs from the SSMOC management team and all the SSMOC functional groups. Once the annual schedule has been determined, it will be reviewed by the SSMOC management team and NASA, and once approved placed on the SOFIA website. This then is the master schedule - a 12 month plan with all the science flights, science instruments, investigators, deployments (including ferry flights), maintenance, and holidays blocked out. In addition to this, there will be intermediate and operating schedules for each flight series. The intermediate schedule for a flight series is prepared by the Operations Control Center 90 days before the start of a flight series, showing dates and approximate take-off times for the flights in the series. This schedule will also have an estimate of the number of investigators who will participate and their approximate arrival and departure times (this includes the members of the PI team). At this stage a contingency plan is developed as a back up in case the science instrument for the flight series is not found to be ready during its scheduled reviews. The operating schedule for the flight series is prepared by the Operations Control Center 30 days in advance of the series with details such as the flight plans (including flight take-off and landing times), the investigators (including their dates of arrival and departure), the logistics requirements (e.g., cryogens and shipping), and telescope configuration requirements (e.g., tertiary mirror). A readiness inspection of the PSI's and SSI's will be made either by a visit by a SSMOC scientist to the PI's institute or through a report by the PI showing the SI's performance characteristics. If the science instrument is not ready at 30 days prior to the flight series, and is considered not likely to be ready for the flight series, the back up plan for the flight series may be activated. (This may mean moving a facility class science instrument's flight series forward.) The coordination of the flight planning for a given flight series (i.e., the flight plans given to the Operations Control Center for scheduling purposes) will be the responsibility of the PI of the science instrument for the flight series flying PSI's and SSI's, but will be the responsibility of the SSMOC science coordinator for a FSI flight series. The first two years of operations will consist of a total of 1,200 SFH (Successful Flight Hours at or above 41,000 ft in altitude). In a normal year, after the second year of SOFIA operations, there will be a minimum of 960 SFH per year required, which translates to 137 successful science flights per year with each flight consisting of about 7 hours at altitude. If a total Science Effectiveness of 0.78 is used (see the Overview for this section), then to achieve 137 successful science flights about 4 flights per week must be planned and assigned to a science team over a 44 week period (the period remaining in a year after taking into account maintenance, weekends, and other down-times for the observatory). Hence, the peer review committee will assign a total of 176 flights to the science community each year, which will assure (with 80% confidence) 137 successful science flights per year. Typically, a year will contain about 20 flight series, with a total of about 50 investigator teams. This means, on average, each flight series will last two weeks and will support 2 to 3 investigator teams. 4.3.2 Target of Opportunity Scheduling (See Section 3.1.2.8) 4.4 Flight Series Process A flight series is normally a multiple of a week in length and is defined by the science instrument (or the suite of science instruments mounted simultaneously) to be used. The science instrument could be a FSI, PSI or SSI (see above). In the case of the FSI, SSMOC scientists and technicians will ready the science instrument for flight. In the case of the PSI and SSI, principal investigators (PI's) from the science community must arrive at the SSMOC between one and two weeks before the first flight to ready their instrument for the flight series. Guest investigators (GI's) who will use the science instruments (whether a FSI or PSI) will arrive at the SSMOC probably a few days before their first flight, to use the data center, familiarize themselves with the airborne observatory, and finalize their observing strategies. The near to final flight plans for the series would have been sent to the SSMOC, or generated by SSMOC scientists (see 4.3.1 above), 30 days prior to the first flight of the series. Below is the sequence of events an investigator will follow within a flight series (assuming a PSI flight series): a) Upon arrival at the SSMOC, the SSMOC science coordinator will show the PI/GI the facilities, especially the PI labs, PI/GI offices, telescope/MCCS simulator, data center and final flight planning facilities. The PI/GI will be introduced to the mission director for the flight series, who will help coordinate the PI/GI science team with SSMOC operations, education and public outreach, and mission operations and support, aircraft operations and support, and the continuous improvement programs during the flight series. (b) After the PSI has been assembled and readied for the flight series in a PI lab, the PI team will be assisted by flight mission crew (see 4.7) in integrating the science instrument into the airborne observatory via the telescope/MCCS simulators (see Section 4.5). This will occur a few days before their first flight. In this way, the SSMOC mission crew will be familiarized with the science instrument interfaces to the telescope and MCCS before the first flight. (c) On the first flight day of the series (normally a Monday), the science instrument will be attached to the telescope on the aircraft and integrated with the aircraft, MCCS, and TA systems with the help of telescope and computer operators, TA technicians, aircraft mechanics, and an airworthiness engineer. A high-fidelity simulation of the actual flight set-up sequence will be performed on the ground to test all aspects of the integrated system. (d) About 90 minutes before each flight of the series, the mission director will convene a pre-flight briefing with all flight personnel to summarize mission sequence and objectives for that flight. (e) In a morning meeting after each flight, the mission director will debrief (in person or in a mission report) aircraft, mission system, and science representatives on how the airborne observatory performed in flight. The meeting will be chaired by the aircraft schedule and planning controller. Where appropriate (possible), necessary corrections will be made prior to the next flight. A determination of the SFH achieved will be made jointly by the Mission Director and PI/GI, for Observatory Director review and NASA concurrence. (f) After the flight series, PIs and GIs will be asked to complete a questionnaire relating to science objectives of the flight series, how much was realized and the perceived reasons for any shortcomings. Science objective comments will go to the data center. The questionnaire will also relate to observatory performance, comments toward which will go to the observatory director. Figure 4.0-2 shows the timelines for a typical flight series. It shows a PI team arriving a week before their first flight in order to ready their SI at the SSMOC while another team is flying. Their SI will be mounted to the telescope on Monday morning, with the first flight that night. Normally, three flights will then follow back-to-back (Tuesday, Wednesday and Thursday), so Friday can be used to retrieve the last flight of the week and carry out a full day of maintenance, leaving the weekend relatively free of operations. If the flight series is longer than a week, the SI will be left mounted to the telescope over the weekend with electrical power available. Access to the aircraft over the weekend is possible, but SSMOC ground personnel will be very limited so aircraft activities will be very limited. The servicing of science instruments (e.g., filling with cryogens) will be possible on the weekend. Flights in the last week of the flight series will normally end on a Friday morning. De-installation of the SI will take place Friday morning. After the cavity has been warmed (see Section 4.6.1), and if the next flight series requires a different tertiary mirror or secondary button, the new mirror or button will be installed on Friday afternoon, so the cavity can be sealed over the weekend, and is ready for cooling on Monday. 4.5 Instrument Installation and Checkout 4.5.1 Instrument installation at Moffett Field Installation of a science instrument (SI) on the observatory will start with installation on the TA/MCCS simulator in the SSMOC laboratory. This procedure is required for all SIs and will occur one to a few days prior to each installation on the aircraft. An authorized and certified technician will inspect the completed simulator installation and describe any changes that will be required to obtain airworthiness approval for the subsequent installation aboard the aircraft. Transportation of the SI from the PI lab to the TA simulator lab, and subsequently onto the aircraft, will be facilitated by a SSMOC-provided cart designed especially for the purpose of transporting and mounting the SI on the TA and the TA simulator. It is assumed that no more than one or two SSMOC technicians will be required for this effort. This cart will be designed to correctly distribute loads to the aircraft floor for the heaviest allowable SI (600 kg) and will enable passage through the aircraft passenger door with the largest allowable SI. If the fully assembled SI is larger than the passenger door, then the reassembly of the SI inside the aircraft must not add more than 30 minutes (TBD) to the nominal SI installation time given in Section 4.5.1.2 below. 4.4.1.1 TA/MCCS Simulator Procedures The TA/MCCS Simulator will aid in determining or verifying: (a) the mechanical and vacuum interfaces between the TA and SI; (b) the optical alignment, focus, and boresight of the SI with the telescope; (c) the mechanical, electrical, communication, and protocol interfaces with the MCCS; and (d) the parameters for balancing the telescope with the SI (i.e., weight and c.g.). Mechanical Interface: The TA simulator will duplicate all mechanical, vacuum, and electrical connections required to fully operate the SI in flight on the SOFIA airborne observatory. Hence, the physical layout of the SI flange assembly, the vacuum manifold, the MCCS patch panel, and the cable drape and connector flanges will be identical to that on the aircraft. The TA simulator mounting flange area will be an exact duplicate of the SI mounting flange area on the TA. An instrument rotator identical to that used on the TA will be available for use with the TA simulator. Although the simulator will duplicate the TA and MCCS interfaces as accurately as possible, it will not duplicate the physical constraints associated with the ceiling or TA counterweight assembly, as these lie well outside the confines of the currently defined SI envelope. The simulator will have a floor clearance similar to that of the TA caged at 40 degrees elevation. The simulation of the floor clearance for other telescope orientations and SI rotations will be accomplished using several large plywood shims which can be inserted to approximate the location and orientation of the aircraft floor for extreme positions. This method is required because the simulator is stationary (i.e., it has no equivalent of the hydraulic bearing on the TA) and cannot reproduce the TA azimuth, elevation, and line-of-sight motions. Hence, final verification of all floor clearances will be done on the aircraft before the TA, with the SI attached, is uncaged. The TA simulator will duplicate the vacuum manifold and pumps that are on the actual TA and aircraft so that the investigator can pump on the SI cryogens as needed. There will be space reserved for a closed-cycle-cooler compressor and closed-cycle-cooler lines to be included in the simulator and TA cable drape. The relative placement of the compressor and its lines will be the same as on the aircraft. (b) Optical Alignment, Focus, and Boresighting: The TA simulator will be a single structure with a duplicate of the telescope mounting flange at one end and a tertiary mirror and alignment source fixture at the other end. The beam line from the alignment source fixture to the tertiary will form a 90 degree angle with the beam line from the tertiary to the SI flange and will reproduce the orientation of the telescope at 40 degrees elevation. However, the physical separations of the SI flange, tertiary, and alignment source fixture will be 1/3 to 1/2 the nominal TA separations, so that the simulator will have an overall length of only two to three meters. Three sources will be available for use in alignment on the simulator: a small laser or telescope; a broadcasting source (hot plate); and a focused source (portable collimated light source, PCLS). The first will be used primarily at the SI flange to verify the alignment of the simulator itself (this may be the same device that is used for TA alignment). The second will have an IR black surface which operates at approximately 100 degrees C. The third will use a small Cassegrain telescope and a quartz lamp to deliver both visible and IR radiation to the focal plane. Its focal range will accommodate all back focal distances allowed for the SI (-30 cm to +90 cm from the SI flange). Both the latter two sources will use circular chopper wheels and subtend a solid angle equivalent to that of the oscillating secondary mirror of the TA. They will be able to accept phase and frequency from the SI electronics (standard TTL) or synchronize with an internal clock and provide a reference output. The operational frequency range of the hot plate and PCLS choppers will be 5-10 and 5-30 Hz, respectively. Since access to the TA cavity during installation is highly restricted, all SI alignments will be done on the simulator. In order to transfer alignments from the simulator to the TA, several boresight boxes (BSB) will be provided for use by the investigators. A BSB will be mounted on the SI, in front of the SI window, before installation on the TA simulator. This BSB will remain attached to the SI throughout its flight series. Hence, at least two boresight boxes will be required: at any time one will be on the TA with the current flight experiment while the other is being used on the simulator by the next SI. The BSB will be mounted internal to (aft of) the SI flange and the SI will be mounted external to (forward of) the SI flange. The vacuum seal between the BSB and the SI will be made with an o-ring. The BSB will form a vacuum seal with the TA using either bellows couplers or a 41-inch diameter plate and o-ring seal. In the former case, access to the SI flange area is required for installation of the bellows coupler. In the latter case, the 41-inch flange plate will be transported from the simulator to the TA as part of the SI/BSB assembly. Each BSB will contain a flip mirror and an optical CCD camera. When the flip mirror is 'engaged', light is reflected into this optical CCD camera; when the flip mirror is removed from the beam line, light passes directly through the BSB and enters the SI through its window. The BSB will have a means of adjusting the CCD path length to accommodate the allowable range of back focal distances for SI. Alignment: This mechanical alignment orients the SI so that its field of view is centered on the secondary mirror of the telescope. For this procedure the chopped hot plate is mounted on the TA simulator (see above) and the flip mirror in the BSB is removed from the light path. The SI detects the signal from the hot plate, which is maximized by tilting/positioning either the SI or a mechanism which is an external or internal part of the SI. This alignment is the sole responsibility of the PI team; there will be no adjustment made to the nominal TA alignment to accomplish this task. Once the SI alignment is optimized, this tilt/position will be locked down and will remain unchanged for the duration of the flight series. (Note: Some investigators may develop SI with no provision for such an orientation adjustment. Such SI will still use the simulator to verify that their (fixed) orientation relative to the secondary is adequate for their experiment.) Focus: This adjustment ensures that the optical focus for the TA will coincide with the infrared focus for the SI. For this procedure, the PCLS is mounted on the TA simulator and the flip mirror in the BSB is initially removed from the light path. The focus on the collimator will be adjusted until a small (few arcsec) point-like source is minimized in spatial extent or gives maximum signal on a single pixel. Without changing the PCLS (so the image in the SI remains focused), the flip mirror in the BSB is engaged and its optical CCD camera is adjusted until its image is focused. This focus setting on the optical CCD camera is then locked and remains unaltered for the remainder of the flight series. Boresighting: The boresight procedure maps the IR focal plane onto the optical focal plane for use in pointing and guiding via visible (or near IR) stars. For this procedure, the PCLS is mounted on the TA simulator and the flip mirror in the BSB is initially removed from the light path. Once the SI is aligned and focused (in that order), the boresight or 'hot spot' of the SI is located by tilting the PCLS to illuminate a particular pixel on the detector array. This can be done directly in the case of two-dimensional imaging arrays (i.e., simply move the source to the desired location) or indirectly (i.e., maximize the signal on a particular pixel). Once the IR radiation from the PCLS is at the desired location in the focal plane, the BSB flip mirror is engaged so that the image falls on the optical CCD camera and the location of the optical image (which is coincident with the IR image) is recorded. This completes the optical alignment procedure on the TA simulator. Knowledge of the proper alignment, focus, and boresight for each SI are the responsibility of the PI team. Other Tasks: An instrument rotator plate can be used with the simulator to determine whether the boresight, wavelength, or other parameters of an SI depend on rotation angle. If a particular SI does not use the rotator plate, similar effects due to changes in TA elevation could be investigated by physically removing and reinstalling the SI in different orientations. If the boresight varies with rotation angle, it is the responsibility of the PI team to fully characterize or remove these effects so that the inflight focal plane imaging system can be operated in a simple and straightforward manner. The simulator will allow polarizing grids to be inserted in the optical path between the simulator sources and the SI. The acquisition, installation, and use of appropriate grids will be the sole responsibility of the individual PI teams. The simulator will have a bent optical path (90 degrees) with a single, reflective tertiary. Neither the dual tertiary nor the focal plane imager on the TA will be duplicated on the simulator (other than mechanical interferences). In conjunction with the facility rotator plate, the simulator could be used to measure the polarization of a beam splitter or mirror as a function of angle. MCCS Interface: The simulator will possess an interface patch panel and cable drape identical to that used in flight. All electrical connections between the SI and the MCCS will be physically present and the communication protocols between these two systems can be verified. The simulation of MCCS responses to SI commands will be as faithful as possible. For example, the MCCS indicator of TA stability and the transfers of housekeeping data will be fully operational, although the buffer contents for the latter will either be 'playbacks' of old flight data or 'dummy' data of some sort. On the other hand, the nod command for the TA will produce a status change in the MCCS, but will not be coupled to the alignment sources, so there will be no physical change in their output. Weight and Balance: Scenario 1: A device will be provided by the SSMOC for checking the SI weight and center of gravity for inputs into a software model, which will determine the required distribution of the removable weights on the back of the telescope to balance the telescope with the SI mounted. The c.g. of the SI (and total weight) could be determined by having three co-planar weight gauges on the SI cart (or another SI stand). These would give the c.g. in one plane. The SI would then be rotated by 90 degrees, and the procedure is repeated to get the c.g. of the SI within its volume. (The rotation of 90 degrees could be a problem for SIs with cryogens.) Scenario 2: (Yet to be approved by the MCCS IPT and the Aircraft Structure IPT.) Only the weight of the SI is measured on the ground. No determination of the SI c.g. is carried out in the TA simulator lab. The SI c.g. is determined in an automated fashion after SI installation on the TA. One of the above scenarios will be used (TBD). 4.5.1.2 SI Installation on the Aircraft After the SI has been checked out on the TA simulator, it will be installed on the aircraft, usually on the morning of the first flight day of the flight series (i.e., usually Monday morning). The de-installation of the previous SI will typically occur on the morning after its last flight (i.e., the morning of the previous Friday). The mechanical mounting of the SI on the TA will require the assistance of two TA technicians (with the aid of an SI cart), but will be primarily the responsibility of the PI team. Concurrently, two aircraft mechanics will load the science racks onboard the aircraft, secure them in the desired locations, and install the associated seating. After mechanical installation is complete, the SI will be connected to all of its cables, hoses, and electronics; cryogens will be filled as needed; and vacuum pumps will be turned on as appropriate. That is, the experiment will be placed in operational, flight-ready status. Although the TA technicians will assist with this activity, most of the interconnects (e.g., cable connections to the SI and the SI racks) and other details of this installation procedure will be carried out by the PI team, with review and signoff by certificated SSMOC technicians. This entire procedure should take no longer than 2 - 3 hours, since it would have been demonstrated in the TA/MCCS simulator. Once the installation is complete and the SI is operational, the (two) installation technicians will place the TA balancing weights required for three-dimensional, rotational balance of the TA/SI package. Scenario 1: This will be done by following the output of the balance computer program which used as inputs the weight and c.g. determined in the simulator lab. Scenario 2: (Yet to be approved by the MCCS IPT and Aircraft Structure IPT). This will be done by connecting strain gauges between the aircraft and telescope assemblies, rotating the telescope to several elevations, and using associated MCCS-based software to solve for a unique static solution. After the TA weights have been added (using either scenario), the RIS (Rotation Isolation System or TA bearing) will be activated and the telescope will be uncaged with the telescope at 40 degrees elevation. Then, as the telescope moves through all its angular degrees of freedom, the cable drape and floor clearances will be checked for interferences. The balance will be checked through the full elevation range of the telescope. For SIs using the instrument rotator plate, the balance of the telescope will be checked for all SI rotation positions with respect to the telescope. For SIs using the rotator plate, it is required that their center of gravity will be sufficiently close to their rotational axis that the TA fine balance system can compensate for SI rotation. The entire balancing procedure should take no longer than about 1 hour. After the telescope balance is complete, an observing sequence will be run to exercise all interfaces and subsystems, to test for electrical interferences, and to look for any other potential problems. As many systems as possible will be activated, including the secondary mirror assembly, the telescope gyros, the telescope torque motors, as well as the RIS. The TA VIS (Vibration Isolation System) need not be activated. Small forces will be applied to the telescope (by hand) to test EMI interference from the torque motors. A simulated tracking routine will be used to check that all the correct MCCS signals are being sent to the PI electronics, and that the MCCS and TA (i.e., the secondary mirror) are receiving all signals from the PI electronics. In general this test period should take no longer than 1 hour, but could be much longer if problems are uncovered. (If such problems are in the SI, then the Observatory Director will make a decision whether to substitute a contingency mission using a facility SI.) This stage of the SI checkout would often be run in parallel with the cavity cooldown sequence (see below). After installation is complete and all ancillary equipment is stowed, an airworthiness inspection of the set-up will be conducted by an aircraft mechanic. 4.5.2 Instrument installation on deployments An installation on deployment will be very similar to that described above, but will use a second, light-weight, less capable simulator. Unlike the permanent SSMOC simulator, this deployable simulator will not verify the mechanical installation of an SI (i.e., it will not provide a faithful reproduction of the SI mounting area on the TA and will have only limited vacuum and MCCS connectivity). For this reason, it is assumed that a new SI will not be installed on deployments without previous flight experience on the airborne observatory, or without having been first checked out at the TA simulator at the SSMOC. (Note: If a SSMOC approved TA simulator exists in Germany, then German SIs may use this to verify their new SIs before deployment.) The deployable simulator will provide a simplified flange for mounting/supporting the SI with or without the facility rotator plate and will facilitate the alignment, focus, and boresight procedures described above. It will consist of two separate parts, an abbreviated flange assembly for mounting the SI and an abbreviated spider assembly for mounting the alignment sources. There will be no tertiary. The light sources for the deployable simulator will be separate, but similar to those for the SSMOC simulator. The deployable simulator will have to be aligned each time it is used, but this should require less than 1 hour. While on deployment, the same safety and airworthiness inspections will be carried out by an aircraft mechanic after SI installation, as at the SSMOC. Note: While SOFIA is on deployment the TA simulator at the SSMOC is completely operational: No parts or equipment from that simulator are used by the deployment simulator. 4.5.3 Inflight focus and boresight procedures The focus and boresight procedures for SIs, initiated on the simulator, will be completed at the start of the first flight in the series. Focus: If a BSB has been employed, then the IR focus can be transferred to the focal plane imager (FPI) by placing any visible star near the center of the focal plane, engaging the BSB flip mirror, focusing the TA on the BSB CCD camera, and adjusting the FPI to put this same star simultaneously in focus. If a BSB is not being used, imaging SIs could focus pointing the telescope at an infrared source in the sky. Nonimaging SIs will, in this case, have to focus using dead-reckoning (i.e., measure the optical and IR path lengths and make them the same). Boresight: If a BSB has been employed, then the SI boresight can be transferred to the FPI by engaging the BSB flip mirror, moving the TA to place a bright visible star on the BSB CCD camera boresight, and recording the equivalent position on the FPI. Now the boresight of the SI, BSB CCD, and FPI should agree - it will be important not to forget to remove the BSB flip mirror before trying to observe with the SI! If a BSB is not used, the SI can be boresighted by pointing the telescope at an infrared source in the sky and either minimizing the source size (imaging SI) or maximizing the signal in a single pixel (nonimaging SI). 4.6 Daily Operations Process 4.6.1 Typical Flight Day (at Moffett Field) For the process described in this section, it is assumed that there was a research flight the night before, and another flight scheduled for the coming night using the same science instrument. Therefore, this process describes the "recovery" activities necessary after a research flight plus the activities necessary to prepare for a flight. Normal take-off times for science flights during winter will range from 1600 to 2330 (PST) with landings occurring about 8.5 hours later (0030 to 0800 PST) for night flights. During the summer months, the take-off times will nominally range from 1900 to 2230 (PDT) with landings occurring about 8.5 hours later (0330 to 0700 PDT) for night flights. Note: A few investigator teams (about 3 a year) may need daylight science flights (e.g., for solar eclipses or observations of Venus). The process outlined below begins as the aircraft taxis into the NASA ramp at Moffett Field. 4.6.1.1 Aircraft Retrieval, Refueling, and Docking ( ~ 4 hours total ) Scenario 1: After landing, the aircraft will taxi to a stop at the ramp entrance, will shut down engines, and will be towed to the fuel pit. An hour will be allowed for people to disembark with their carry-ons via portable airstairs to the one-left passenger door of the aircraft. During this hour, people will be allowed to work onboard the aircraft with power being supplied to the aircraft by a GPU (ground power unit). No direct link to the ground computer network will be available. However, the down-loading of mission data could be accomplished through storage disks and tapes very efficiently. This will be the mode on deployments (see Section 4.10). Large items required to be lifted onto the aircraft (e.g., liquid helium dewars to service the SI) will be supplied through the starboard number one door of the aircraft via an equipment lift. The fuel pit is located about 100 ft away from the hangar door. This scenario may be modified to accommodate circumstances as necessary. In its unmodified form, this scenario requires the least aircraft movement. Minimizing movement of the aircraft saves time, minimizes wear and tear on equipment, and minimizes risk. Scenario 2: After landing, the aircraft will taxi to a stop outside the N211 hangar, will shut down engines, and then will be towed into the hangar and docked into a nose-dock. An hour will be allowed for people to disembark and to unload equipment and carry-ons via the access ramp in the SSMOC which connects to the one-left passenger door of the aircraft via the nose-dock. During this hour (as in the first scenario) people will be allowed to work onboard the aircraft, but power will be supplied by the SSMOC power supply, the SSMOC computer network will be hooked up to the aircraft, as will aircraft airconditioning (if provided by the ground facility in N211), and SI service equipment (such as liquid helium dewars) can come through the port number one aircraft door via the SSMOC access ramp. After an hour, all people will disembark, and the aircraft will be closed and towed back to the fuel pit. In both the scenarios above, the standard process will be to re-fuel the aircraft as soon as possible (~1.5 hours) after landing. Refueling (~2 hours in duration) at this time will cut down on interruptions to the daily activities: At this time of day, the science team will leave to rest and recover from the flight, and there usually will not be educators or students desiring access to the plane. Access or additional activities on the aircraft will be coordinated with aircraft operations during this time. While the aircraft is fueling, power must be supplied by a GPU, since some SIs require power (although this power can be interrupted for periods on the order of one hour). During refueling only aircraft support and telescope cavity conditioning (see below) activities will be performed on the aircraft. In both scenarios above, during the hour after the engines have been shut off, scientists and mission crew may leave the aircraft as soon as the aircraft door is open or they may stay on the aircraft to finish up post-flight activities. Post-flight activities will include packing up their personal belongings and other items to be carried off the aircraft, removing and stowing their headsets and other equipment, backing-up data, finishing flight reports, servicing the science instrument, and procedural accomplishment of final shutdown and powering off of the telescope, MCCS and SI systems. For all flights, the mission director will summarize the flight in a report (including science team inputs) which will be sent to the SSMOC Operations Controller. This report will be used by the Operations Controller in the morning post-flight / pre-workday briefing to representatives of the mission system, science, educators, and aircraft staff. For a flight with a major problem, where immediate action and change to the schedule must take place upon landing, the Operations Controller will be contacted directly by the mission director. After refueling is completed, a power-down procedure will be performed prior to disconnecting power from the aircraft. If TA cavity conditioning ground equipment is hooked in place at this time (at times none may be required), this will be disconnected temporarily for the towing of the aircraft back to the hangar. The aircraft is towed into N211, up to the nose dock, and aircraft stabilization procedures will be accomplished if necessary. Power and computer network lines from the SSMOC ground facility are connected as well as other aircraft requirements (e.g., air-conditioning for the cabin, if provided). The TA cavity conditioning system is (re)connected (see below). Aircraft doors 1 (left and right) and 2 (left only) are opened by qualified personnel for use by SSMOC staff and investigators. 4.6.1.2 Day Shift Activities (0800 - 1600) 0800 Briefing: The SSMOC Controller will have a 30 minute briefing at the start of each weekday day-shift. The number of staff at this briefing will be small and will contain representatives from all aspects of the SSMOC (i.e., aircraft system, mission system, science, education, and management). The purpose of this briefing is to discuss the status of the airborne observatory, and any changes of plans required for the remainder of the day and week. The focus is on problems that may exist, and the solutions and plans for dealing with problems. If no major problems exist, then the existing detailed master schedule (formulated originally 30 days before hand by the Operations Control Center, but possibly with revisions) will be followed unchanged. Once every week there will be a longer than normal briefing to outline the overall schedule for the next week. The schedules and their changes are posted on an electronic bulletin board, which can be accessed by all SSMOC staff. If there is a major problem reported after the flight, some members of the SI team will have to attend the 0800 briefing. (Hence, the requirement for a small investigator rest area in the SSMOC if the flight landed at 0200, for example.) 4.6.1.2.1 Aircraft System Activities All required maintenance tasks and procedures will be performed per the NASA and FAA approved maintenance program. Additional activities required by the mission system support staff (from the MOS Group) will be coordinated and overseen by the AOS Group. Tasks that cannot be completed within the timeframe allocated will be reviewed by the Operations Control Center, which will coordinate any mission re-scheduling with the science team of the current flight series and with concurrence from the SSMOC management team. Note: Re-scheduling here means a later take-off time for a scheduled science flight, not a re-scheduling of a make-up flight. All maintenance tasks performed on any airborne observatory subsystem and the science instrument will have a final inspection and sign-off by an AOS, FAA-certified aircraft mechanic. This AOS mechanic, before signing off on mission system or science instrument work, will receive inputs from the oversight technicians in the MOS Group and science team who are qualified to determine if maintenance work being carried out on these subsystems has been performed per the NASA and FAA approved program. The aircraft system specific tasks listed below will be accomplished by the aircraft mechanics after all flights. Some will be carried out while the aircraft is being refueled, others when the aircraft has been docked in N211. Total time for tasks is estimated to be approximately 4 hours. Aircraft System Tasks 1. Walk-around inspection of A/C. 2. Review log book items, correct or defer as required. 3. Review any mission critical A/C non-routine write-ups. 4. Correct or defer all non-routine work discovered 5. Pre-service fuel, if required, and re-fuel aircraft. 6. Engine general visual inspection. 7. Service gases: e.g. oxygen, tire pressure. 8. Service fluids: e.g. engine oil, hydraulic fluid. 9. Perform an exterior light check. 10. Check brakes and tires for wear 11. Check fuel tanks for water and sump if present 12. Accomplish all additional SOFIA aircraft system tasks to support flight objectives. (Tasks will be identified and incorporated as appropriate.) 13. Check overwater emergency equipment. 14. Service lavatories, galleys, and set up cabin. 4.6.1.2.2 Mission System Activities Cavity Conditioning: (a) Initial cooldown of cavity (i.e., cavity is warm): Approximately six hours before take-off, the cavity cooling cart and a 650 gallon dewar of liquid nitrogen are positioned at the rear of the aircraft near the cooling ducts for the telescope cavity. In order to fill the cavity with dry, room temperature gas liquid nitrogen is supplied from the external dewar, through a heat exchanger, to the sealed cavity. This dry warm gas is required so water will not condense as the cavity is cooled. The warm purge will last about 30 minutes. The heat exchanger is then adjusted so cold dry gas flows into the cavity; after 30 minutes the cooling cart is brought into the cooling loop so gas is cycled through this cart to the cavity. The liquid nitrogen dewar at this stage is used only to replenish cold dry gas which has escaped the cavity through leaks (< 30 cfm). This closed cooling cycle is continued for 5 hours before a flight. The temperature of the return gas, the cavity and telescope components are monitored by the MCCS on the aircraft. (Cavity oxygen depletion sensors are wired to the cavity entrance to preclude inadvertent entry; the operation is also monitored by ground crew for safety.) (b) Conditioning cold cavity (i.e., after a flight with a short turn-around time): After the cavity door was closed on the previous flight, and as the plane was descending, the valve to the onboard liquid nitrogen dewars was opened so the cavity was pressurized with cold, dry nitrogen gas. It was kept pressurized with respect to the outside air throughout descent, landing, taxiing, and unloading. For most flight scenarios, the two 100 gallon tanks on board the aircraft will be sufficient to maintain the cavity in an over-pressurized state while the aircraft is being refueled. When this is not the case, an external liquid nitrogen dewar will be connected to the cavity airflow system to continue the cold pressurization of the cavity. This pressurization from an external liquid nitrogen tank will be continued until the cooling cart is required to start the closed-cycle procedure. (Note that the onboard dewars will be used during towing to the hangar, requiring retention of adequate supplies for this purpose.) (c) Cold cavity requiring a gentle warm-up (i.e., an early landing followed by a very late flight that night (e.g., 20 hours on ground), and cavity is to remain sealed): Same as for (b), but use heat exchanger. Temperature of gas is such that the cavity will warm up slowly (~ 5 hours). After the cavity is above the dew point, filtered hangar air can be used to pressurize the cavity. Cavity must remain pressurized for cleanliness and to keep it dry. Cavity cool down starts 6 hours before flight using procedure (a). (d) Cold cavity requiring a quick warm-up (i.e., must get into the cavity as quickly as possible): Same as for (c), but the heat exchanger is set at 30kW. The cavity will be warm and contain breathing air 1.5 hours after landing. The above scenarios for cavity conditioning require two technicians while hooking up the conditioning systems, but monitoring requires less than one fulltime technician. Telescope Assembly: (See also Section 4.5.1.2) After the airborne observatory has been refueled and is in its nose-dock, and before the science team returns from resting after the previous nights flight, certain telescope subsystem checks, maintenance, and upgrades can be performed. Some subsystems (e.g., the hydraulic system for the RIS) may need daily servicing. TA work requiring cavity access will be restricted, since priority will be given to preparing the cavity for the next flight, and so the cavity may be sealed and in its cooldown mode. If there is a time period after the cavity has warmed-up and before the cavity must be re-sealed for cooldown, then entry into the cavity will be allowed (after proper venting to safe oxygen levels) using cleanroom and FAA approved procedures. Before re-sealing the cavity for cooldown, an aircraft mechanic will inspect the cavity. Later in the day, after the science team has returned from resting, the telescope characteristics will normally be checked by running through a short observing sequence with the PI/GI team (see 4.6.1.2.3). Assistance will be provided in the TA simulator lab to incoming PI teams with checkout of SI for next flight series. MCCS: (See also section 4.5.1.2) After the airborne observatory has been refueled and is in its nose-dock, and before the science team returns from resting after the previous nights flight, certain MCCS subsystem maintenance, programming, and upgrades can be performed. Later in the day, after the science team has returned from resting, MCCS characteristics will normally be checked by running through an observing sequence with the PI/GI team (see 4.6.1.2.3). Assistance must be provided in the TA/MCCS simulator lab to incoming PI teams with checkout of SI for next flight series. Assistance must also be given to incoming GI/PI teams in setting up their MCCS science network. 4.6.1.2.3 Science Activities PI teams will service the SI if and when required (e.g., liquid helium and liquid nitrogen fills). If the SI is a facility instrument, then SSMOC scientists will service the SI. PI's and GI's will reduce and analyze data, and will prepare observing strategies for the next flights. Flight plans will be finalized. PI team for next flight series will be preparing their SI. (Or SSMOC scientists will be preparing a facility SI for next flight series.) After the current PI/GI team has rested and about 4 hours before a flight, an observing sequence will be simulated on the aircraft, with telescope (except VIS), MCCS, and SI systems operating (see 4.5.1.2). 4.6.1.2.4 Education Activities E/PO visitors will arrive no later than 1300 on the day of the flight (assumption: evening flight). E/PO visitors will be one or more of the following: formal educators (K-12 and undergraduate faculty), informal educators (museum and planetarium staff, broadcast staff), representatives of the media (print, electronic, broadcast, science writers), VIPs and students. E/PO visitors will participate in all pre-flight briefings including flight safety training provided for all mission participants. When possible, E/PO visitors will meet with the research team prior to flight to become acquainted and to better understand the purpose of the mission. E/PO visitors will be escorted by a flight facilitator (e.g. an education or public outreach specialist) at all times when in laboratories and on board SOFIA. No rest period will be required for E/PO visitors. 4.6.1.3 Pre-Flight Activities ( ~2 hours total within 1400 - 2130 period) The following pre-flight activities are required before flight: (1) Flight Plan finalized and filed (2) Weather Forecast (3) Passenger Manifest (4) Fuel Load (5) Weight & Balance These will be on the check list for the AOS group member who is assigned as the dispatch officer for that flight. About 2 hours before takeoff the flight and mission crew will arrive at the SSMOC to prepare for the flight after a mandatory 12 hour rest period. These crew are defined in Section 4.7 below. There will be no rest requirement for the science team or visitors in the E/PO program. A member of the flight crew will file the final flight plan with TBD (designated air traffic control authority) at this time. A preflight briefing (approx. 15 minutes in duration) will be held 90 minutes prior to take-off, requiring all flight participants to attend. The briefing will summarize the activities for that flight. Safety issues will not be briefed here, they will be summarized in an inflight safety video to be viewed on the aircraft while taxiing for takeoff. Prior to pushback (approx. 40 minutes), all cabin pre-flight and safety procedures will be completed: The maintenance release on all airborne observatory and science instrument maintenance performed since the last flight will be signed by the FAA-certified aircraft mechanic (after inputs from the MOS technicians and science team) and given to the dispatch officer (if not the same person), who will have the responsibility of the final airworthiness inspection of the airborne observatory by the ground crew. (The flight crew will also carryout an independent airworthiness inspection.) Also, at this time, all flight participants will identify their assigned seat for take-off and landing, check out intercom headsets, and check for life vests. The mission crew assigned to flight safety duties (see below) will perform those checks required by the FAA at this time. The flight deck crew will perform their checks as required by the FAA. Access to the ground is still allowed, and necessary, up until the aircraft doors are closed for the flight (approximately 5 minutes before push-back of the aircraft). Prior to the closure of the aircraft doors, the mission director (see below) will check and verify the passenger manifest. At this point no flight participants may leave the aircraft and all ground staff must disembark. The passenger manifest headcount is given to the flight crew, and then the signed paperwork from the flight deck is given to the dispatch crew prior to pushback. About 30 minutes before takeoff, the aircraft doors are closed, terminating ground airconditioning (if provided); flight participants are seated with seat belts fastened. The mission director uses the manifest to make sure everyone is on board and that they are seated and in communication over the intercom. The mission director also checks that all systems are configured for the pushback of the aircraft. If so, the mission director communicates readiness to the flight crew, who in-turn communicate to the ground crew. Then the cavity cooling cart is disconnected, and the computer network ground link is disconnected, but ground power is maintained. At this time the telescope operator opens the liquid nitrogen valve to the cavity. He/she regulates the heat exchanger depending on the telescope and cavity temperature (may be automated). When the flight crew is ready to push-back, they inform to the mission director. If the mission crew is ready, then the pushback begins. It is important that during pushback, engine start-up, taxi, and take-off that continuous power is maintained to run cabin lighting, computers, some TA/cavity systems, monitoring equipment, SI vacuum pumps and/or closed-cycle coolers, and air-conditioning (although the last can have interruptions up to 10 minutes). A possible scenario to maintain power is that the SSMOC power is maintained by transporting the SSMOC aircraft power cable during push-back from the nose-dock; push-back halts when the aircraft is out of the hangar far enough to start the aircraft's APU (or an engine). The flight crew will call back to the mission crew to inform them that they are ready for the power switchover. The switchover is not done until the mission director gives the go-ahead, because there may be safeguards that need to be initiated prior to the switchover. (Equipment sensitive to this power switch should be connected to an uninterruptible power source, UPS.) Once the go-ahead is given, power will be switched from ground power to the APU (or engine power), and the ground power cable from the hangar disconnected. Push-back will continue until the aircraft is on the Moffett Field taxiway adjacent to the NASA ramp. Then the engines will be started. Once all is ready for flight, ground communication and the tow truck will be disconnected, and the aircraft will taxi for takeoff. Taxi to takeoff takes about 5 minutes at Moffett Field on average. During push-back and taxi, an approved safety video will be shown, and the mission crew for the flight will perform the required safety duties at this time. 4.6.2 Non-Flight Weekday A non-flight weekday in a flight series will normally be a Friday. This will either be a day within the middle of a flight series or the last day of a flight series. If it is within the middle of a flight series, the science instrument will stay mounted to the telescope, and the days activities will in general follow those outlined in Section 4.6.1.2 until the end of the day (approximately 1800). On non-flight days, maintenance will be given priority over science observing sequence runs by the PI/GI teams; on these days maintenance can be performed in the TA cavity after it has been warmed (see Section 4.6.1.2.2 (c) or (d)). Care will be taken not to unintentionally reconfigure the airborne observatory in anyway during maintenance activities in the middle of a flight series. If the non-flight day is at the end of the flight series, the science instrument and science racks will be removed from the aircraft after the aircraft has been refueled and positioned in the nose-dock. This removal process will take about two hours. During this time the cavity will be warmed, and maintenance may be performed which can be performed concurrently. After the cavity has been warmed and vented, the telescope will be reconfigured for the next flight series (e.g., change of tertiary mirror or secondary button). After the telescope has been reconfigured and TA/cavity maintenance completed, the cavity will be inspected for airworthiness and sealed for the weekend, ready for cooldown on the following Monday. Normally this work should be completed by 1800. 4.6.3 Typical Weekend Day The level of SSMOC ground support on the weekends will be low. It will be enough to support: continual electrical power and computer connectivity to the airborne observatory; the servicing of science instruments on the airborne observatory; and science instrument preparation by science teams in the PI laboratories and TA simulator labs when required. 4.7 Research Flight Process A science flight will be about 8.25 hours total in length. There will be two commonly used flight profiles: (a) Climb for 0.5 hours to 41,000 ft, maintain 41,000 ft for 7 hours, descend to land in about 0.75 hours; or (b) Climb for 0.5 hours to 41,000 ft, maintain 41,000 ft for 2.55 hours, then climb to 43,000 ft (0.1 hours) and maintain for 2.6 hours, then climb to 45,000 ft (0.1 hours) and maintain for 1.65 hours, descend to land in about 0.75 hours. (NOTE: These profiles assume an aircraft zero fuel weight of 367,000 lb.) Figure 4.7-1 shows a typical flight plan for a flight from Moffett Field. It shows seven observing legs, each about an hour long. Observing legs can vary in extent, from about 10 minutes to 4 hours each. Hence, the number of astronomical objects observed in one flight can range from about 2 to 16, but with an average of about seven. Normally, at least one object in a flight is called a calibrator. This is a well characterized object, so its measurement will calibrate the data for the whole flight. Without this calibration, observations will be relative, without absolute values, and so in most cases useless. Personnel on the flight will consist of the following: Flight Crew: Normally consists of three people, captain (left seat), first officer (right seat), and second officer. On long deployment flights there will be a fourth flight crew member. The captain is the ultimate authority in flight, and for final flight release. Mission Crew: Typically consists of two people, a "mission director" and a "telescope operator". However, on the first flight of a flight series with a PI or special science instrument an "observatory computer specialist" may also fly since there are many SI interfaces and computer requirements which may present problems on the first flight. If there are visitors in the E/PO program, the mission crew will be augmented by one "E/PO facilitator" for a group of eight or less. The mission director and E/PO facilitator will carry out all the flight safety duties required by NASA and the FAA in the main cabin. Flight crew will take care of the flight deck and upper deck. Mission Director has the primary responsibility of coordinating the activities in the cabin during the mission. This person will also be the sole person in communication with the flight deck. The mission director will take on the lead role in performing the safety duties required by NASA and the FAA, very much like the lead flight attendant on a commercial flight. During the flight the mission director will keep a log for the SSMOC operations controller. This log will outline the flight and highlight observatory performance and problems. The mission director will monitor the flight track of the aircraft, and verify that any flight plan alteration will maximize the observing time within the constraints. This person will be an experienced operations specialist from the SSMOC technical staff, and so will be able to perform technical tasks during the flight if required, and if his/her prime mission director responsibilities are already met. Telescope Operator has the technical responsibility for operating the telescope: have it pointed correctly; have it perform the observing routines required by the science team; have all systems being monitored and recorded; and can troubleshoot if telescope problems arise. This person will interact closely with the science team as they observe and shall have been briefed by the science team on the observing strategy to be followed during the flight. This person is also technically responsible for all the non-computer systems of the observatory, especially handling power requirements. Observatory Computer Specialist has the technical responsibility for running and monitoring the observatory computer systems and network, and troubleshooting problems relating to them both in hardware and software. When he is not on a flight, these tasks will be split between the telescope operator and the mission director. This person will work with the science team to make sure they are receiving required housekeeping data; are able to use their PI workstations and peripherals; and are able to communicate with and command the telescope through the MCCS system. As a lower priority, this person will help with the computer needs of the E/PO visitors if they are on board. If and when high bandwidth ground to air communications are established for SOFIA, this person will be responsible for its operations. E/PO Facilitator has the responsibility of coordinating the activities of the E/PO visitors with the rest of the mission. This person will work closely with the mission director, who in turn will make sure the E/PO visitors do not hinder science operations. The E/PO facilitator will direct the activities of the E/PO visitors, and will perform the inflight safety duties required by the FAA in regards to the E/PO visitors. Science Team: This will range in size, depending on the complexity of the science instrument and the number of guest investigators (GI's) involved in the flight series. For a PSI (a Principal Investigator SI), there will be a minimum of two in a science team (2 PIs), and as a maximum eight (4 PIs and 4 GIs). For a SSI (Special SI), there will be a minimum of two in a science team (2 PIs) and a maximum of six (6 PIs). If a FSI (facility SI) is being used, it will be supported by SSMOC scientists and technicians, who will be considered part of the "science team", not the "mission crew". In this latter case the minimum science team will be four (1 SSMOC scientist and 3 GIs), and as a maximum eight ( 2 SSMOC scientists and 6 GIs). In summary, the average number of scientists in a science team will be about six, but with a maximum of 8. E/PO Visitors: On some flights there will be no E/PO visitors, but on average there will be two. The maximum number of visitors will be ten. These visitors will be educators, media, VIP's, university students, and occasionally high school students. Others: On some flights (about 10%) there will be one trainee learning a crew position or one to two engineers working on some upgrade or performance problem of the observatory. These personnel will not be considered part of the mission crew, and trainees need not fly when engineers are required to fly. Figure 3.1.4.3-1 shows the layout of the floor plan in the SOFIA aircraft. The flight crew is on the flight deck for takeoff. The mission crew (except for the E/PO facilitators), the science team, the engineers and trainees are seated in Zone 2 of the main cabin for takeoff. The E/PO visitors are seated in Zone 1 of the main cabin. No one is seated in the upper deck cabin for take-off. The E/PO facilitator(s) are seated by the exit doors for Zone 1 for takeoff. Each flight participant can bring on the flight a maximum of 30 lb. of personal carry-on. This will include notebooks, portable computers, clothes, food and drink, etc. All carry-ons will be properly stowed for take-off and landing, and there may be (TBD) restrictions on the use of carry-on electronics for take-off and landing. All participants must provide their own meals. However, water (both cold and hot) and coffee will be made available. Provisions will be made on board for refrigeration and heating of food. There will be no set time for eating: People will eat when they are hungry and when they have a spare moment. There will be no cabin attendant services provided, except those relating to safety. 4.7.1 Climbout (from takeoff until seatbelt sign is turned off ) : [Note: In the flight described below it is assumed that the secondary mirror assembly (SMA) is required to "chop" (i.e., to oscillate between two tilt positions) while data is taken (i.e., continuously for 8 hours). This is the most common mode of data taking in the far-infrared, but some science instruments on SOFIA will not require the mirror to chop, and so for these instruments the secondary mirror will be held fixed.] Immediately after takeoff, there is the initial climbout phase of the flight. The initial climbout is defined by the seat belt sign, since operations are restricted without the freedom to move around in the cabin. This period could be very short (10 mins) or occasionally long (20 mins) depending on traffic control and the weather. The flight crew will inform the mission director as to the flight status; the flight crew has ultimate control of the seat belt indication to the passengers. The mission crew will adhere to all established operating procedures, which include required communication periods to the flight deck. During the climbout, systems on the aircraft are as they were for taxi and takeoff. Computers are on, so can be used by those sitting by them. Equipment which can interfere with aircraft avionics is off. The SI and telescope systems are monitored. The telescope is caged, both VIS (vibration isolation system) and RIS (rotation isolation system) are off, the telescope imagers are off, the secondary mirror assembly (SMA) is off and fixed, the gyros are off, the cavity door is closed, and the liquid nitrogen valve is still open to purge the cavity with cold nitrogen gas. The temperature of the cavity must be monitored, since it could get too cold, in which case the nitrogen gas must be warmed slightly or valved off. The flight path (planned vs actual) is also monitored. If deviations are made, because of vectoring by traffic control, calculations are made by a flight planning program to measure the overall effect to the observing plan and how best to correct the existing flight plan to gain back the observing objectives. E/PO visitors may be watching an orientation video at this time. 4.7.2 Ascent (from seatbelt sign turned off to opening of cavity door): After the seatbelt sign has been turned off, stowed equipment and carry-ons are unpacked and positioned for operation. The SI and its data acquisition system are fully activated. The telescope VIS and RIS are activated, the gyros, telescope imagers, and SMA are turned on. At an altitude of approximately 25,000 ft, the flow of nitrogen into the telescope cavity is turned off. The water vapor monitor is turned on and checked. This part of the ascent is a good opportunity to start up the telescope systems and do a full system checkout. By doing this, the system can be ready to begin observations the moment the aircraft reaches the first observing waypoint and turns onto heading. After the science team has confirmed that the SI is ready for observing, the telescope will be moved to the elevation of its first object. (It is usually stowed at 40 degrees in elevation.) The telescope will be uncaged (i.e., released and allowed to float so the aircraft moves freely around the telescope's large main bearing), and the telescopes balance checked. The telescope's blind pointing system can then be activated and tested, as well as the gyro stabilization system and the tracker loop minus a visual reference (i.e., will have gyro drift effects). The SMA can be tested at this time by sending a signal from the SI or MCCS (see below for displays). Ascent (and Checkout) is a busy time, so E/PO visitors will watch this setup action remotely, on their large video screen in Zone 1 with the E/PO facilitator explaining the procedures. 4.7.3 Checkout ( from cavity door opening to first object leg): Typically the cavity door will be opened at about 35,000 ft, about 20 minutes (?) after takeoff. The checkout phase is a continuation of the Ascent phase, except now the cavity door is open, positioned at the elevation of the telescope. The balance must be checked again, since now the wind loads from the cavity are present. The balance may have to be adjusted using the fine balance. After the balancing procedure is complete, any time left is a bonus. Usually the Checkout period is only 10 minutes long. If there is time, the telescope operator will fix and center the SMA, and point the telescope at the nearest star in the telescope's field of view. The complete tracker loop is now in operation so pointing stability can be checked. The telescope is then focused by moving the secondary until the star's image in the Focal Plane Imager (FPI) is the smallest. To check that the FPI and SI still have the same focus (based on the first flight, see 4.5.3), the flip mirror in the SI boresight box may be engaged and the image on the boresight box camera checked. The position of the SI boresight with respect to the FPI field of view can also be checked at this time using the camera in the boresight box (see Section 4.4.3). If there is more time available, the parameters for the SMA can be set and sent, and the resulting chopped image viewed to check the SMA performance (see displays below). Then the nodding routine can be tested if there is still time. 4.7.4 Transition between flight legs: The transition between flight legs begins when the telescope is caged at the end of the previous flight leg and ends about 5 minutes later after the aircraft has turned on to the new flight leg and is flying with wings level. The previous leg is ended when the investigator acknowledges that data taking is completed, or when the mission director overrides PI control and commands the telescope operator to the end the leg. At this command, the telescope operator will cage the telescope so it is no longer free floating, and will de-activate the tracking loop. All other systems are not altered. Once this has been done and has been communicated to the flight deck, the aircraft will start its turn. The pilots will have a "caged/uncaged" indicator on the flight deck, and they will also have a "time left on leg" value which they are monitoring (and which they will have seen turn to zero) so they're aware that a turn is imminent. They should see the indicator change from uncaged to "caged", so they know that it is OK to begin the turn. Some or all of this process could be automated, but there is a need for at least a pilot "acknowledge" for each turn. Settings for the next leg, for subsystems such as the aircraft (heading), telescope (elevation and line of sight positions), cavity door (elevation), secondary mirror (amplitude, rotation, offset, frequency, etc.), blind pointer (desired RA & Dec), and tracker (star field electronic overlays, AOIs, boresight, etc.) are sent to those systems, which are then configured for the next leg. Many of these parameters will have been given to the telescope operator in a computer file by the investigators before the flight. These parameter files will outline the observing strategy for each flight leg of the flight. Although the outline will be followed as much as possible, variations to it are very likely since the characteristics of the astronomical source or SI can differ from those assumed when planning the observing strategy. During the turn, the science team is readying for the commencement of observations: The SI team will configure the science instrument for the coming observations (set filters, apertures, grids, SI rotation, resolution etc.); and the guest investigators who are controlling the observing strategy for the leg are seated in the best positions to direct the observations and use the quick-look software. Much of the transition set-up could be automated, although manual override can be a common method of operations as well. An automated system during transition would be initiated when the investigator outputs a leg complete signal. The signal is received by the MCCS, which forwards appropriate messages to the systems requiring setup (described above): aircraft (heading turner), telescope, door, SMA, etc. These messages contain the necessary information to configure the systems for the next observing leg. As the aircraft is turning, the telescope is moving to the correct elevation, and virtually all systems have been configured before the turn is over, as specified by the investigators observing strategy. 4.7.5 First Observing Leg: The first observing leg commences once the aircraft is on heading with wings level. It ends when the telescope operator cages the telescope for the aircraft turn to the next leg. As stated before, an observing leg can vary a great deal in length, from 10 mins to 4 hours. The first leg will usually have a longer setup period than subsequent legs in the flight, especially if it is the first flight of the flight series (see 4.5.3). Most of the procedures outlined below are expected to ultimately be automated to some degree to be done efficiently and within the times stated. 4.7.5.1 Field & Object Acquisition Once aircraft is on heading and the telescope sends a correct elevation signal, the telescope operator will activate the blind pointing system which automatically moves the telescope to within 2 arcminutes of the desired sky position (entered during the turn). At this point, automatic field recognition analyzes a star field. Once the field has been identified, field acquisition is complete. Once the field has been identified, the MCCS knows the exact position of the telescope, because it knows the position of the identified field in the imager(s). The telescope operator (or the investigator) can now move the telescope to the first RA & Dec position on the investigators observing list. This sequence of acquisition should take no longer than 3 minutes. 4.7.5.2 Focus and Boresight For the first observing leg, the first object will be a star, so the telescope can be focused and boresighted (i.e., the FPI is focused and boresighted with respect to the boresight box CCD camera, see 4.5.3). This will not be necessary if these procedures were done in the checkout phase of the ascent. This sequence should not take longer than 2 minutes. 4.7.5.3 Chop Setup If the investigator is to use the chopping (i.e., oscillating) function of the secondary mirror, then (with the telescope tracking on the star) the SI team or the telescope operator will send a signal to the SMA, containing waveform, chop amplitude, frequency and phase information. The image of the star on the FPI will split into two if it is a two point chop, and three if it is a three point chop. Most observations employ a squarewave, two point chop, and this will be assumed for the following except where explicitly stated otherwise. The position angle of the chop direction with respect to the telescope coordinates (elevation and azimuth) and the chop amplitude can be measured and adjusted at this time if required. It is important to note that the chopper direction and position angle will change with respect to the sky, as the sky rotates with respect to the telescope coordinates during the observing leg. An update sequence can be programmed, so that after every integration set (see below) the chopper position angle can be reset, so the two images on the sky due to the chopper are in the same RA&Dec position even though the sky has rotated. This update should not be made while the SI is taking data, since changing the chopper angle can give infrared background changes, and the chopper performance may vary slightly with position angle. Once the chopper parameters have been set and measured, the telescope operator (or investigator) will move the telescope to one of the images (image A). The estimated duration of the chop setup process, once a star has been acquired, will be 1 minute. 4.7.5.4 Offset Tracking Many astronomical objects observed on SOFIA will be infrared sources with no optical image. Offset-tracking will be used for these sources. When offset tracking, a star near the infrared source will be placed on the FPI in such a manner as to place the infrared source on the boresight of the SI. The offset between the tracking star and the infrared object must be on the order of 5 arcmin or less, since the field-of-view of the FPI is 8 arcmin in diameter. The image of the star on the FPI will be used to close the tracking loop for the telescope. (If the SMA is chopping, the image in this procedure will refer to image A.) However, like the chopper position angle, the infrared source will rotate on the focal plane of the FPI with respect to the tracker star since the telescope can be in freeze-mode" (see below) for only 3 degrees in azimuth, and so updates must be made as required taking into account the sky rotation so the infrared source is still on the boresight of the SI with a stability as specified in SOF-1011 for offset tracking. Offset tracking requires accurate and continual measurements of the skys orientation with respect to the telescopes coordinate system (or that of the focal plane). The setup of offset tracking should take no longer than 1 minute. 4.7.5.5 Data Acquisition - Integration Sets Once the chop and the offset tracking have been setup, data taking can commence. An observing leg will be grouped into a number of integration sets. An integration set is a data acquisition period where an automatic sequence of SI and telescope procedures are followed for a length of time sufficient to complete these procedures and obtain sufficient signal-to-noise ratios in the data. If loss-of-track occurs within a set, then usually that set of data must be discarded. The period of an integration set varies greatly from one SI to another; the range is from a few seconds to several hours. For example: (1) Cameras, with CCDs which saturate quickly, must re-set (i.e., read-out) frequently, and hence have short integration periods (i.e., seconds). (2) High spectral resolution Fourier Transform Spectrometers (FTSs) must have long integrations by their nature (i.e., hours). (3) SIs, such as Fabry-Perot spectrometers or camera polarimeters, must scan or rotate optics internal to the SI during an integration set (i.e., interference grids for the Fairy-Perot and a polarizing grid or plate for the polarimeter). These sequences of internal scans and rotations typically last a few to 10 minutes. Convolved with the procedures internal to the SI, are telescope/SMA sequences. These sequences include telescope staring, nodding, scanning, and smooth slewing between predefined points on the sky. These telescope motions (or non-motions) are often performed while the SMA is chopping. The difference between scanning and slewing is that data is taken while scanning, but when the telescope is slewing, data is only taken at the end points. This means that a scan is a very controlled slew, with the telescope tracking throughout the scan (i.e., at all points of the scan you know exactly where you are pointed to 0.2 arcsec stability if the telescope is tracking on the source). A scanning routine is used for those cameras wanting to achieve super-resolution (i.e., to achieve better spatial resolution using deconvolution techniques). The staring mode for the telescope is the simplest, with the telescope not moving on the sky with a stability of 0.2 arcsec. Occultation studies use this set-up, since they stare at a star as it is occulted by a planet, moon or rings. 4.7.5.6 Chopping and Nodding The most commonly used telescope/SMA sequence in the far-infrared is the chopping-nodding routine. Infrared telescopes use chopping to cancel background emission due to the sky and telescope. This background emission usually dominates the emission coming from a desired infrared source when the telescope is warm (relative to temperatures in space) and located in the Earths atmosphere. A measurement taken using a chopping secondary mirror results in an ac-signal on the detectors in the SI with the same frequency as the chopping secondary, where the amplitude of the signal is ideally (source + sky + telescope) minus (sky + telescope) if one beam or image (e.g., image A) is on the source and one is off the source. Unfortunately, perfect cancellation of the telescope emission is hard to realize, since the beam resulting from the chopped secondary mirror moves on the primary mirror: A modulating offset signal, not due to the source, results if the primary mirror is not perfectly uniform (in both emissivity and temperature), or the beams to some extent see different parts of the cavity at the two different positions of SMA tilt. If this modulated offset is stable, then it in turn can be cancelled if the telescope is nodded (or beam-switched), so that for half of an integration set the source of interest is in the chopped beam (or chopped image) called left-beam (or image A) and for half of the integration set the source of interest is in the chopped beam (or chopped image) called right-beam (or image B). The movement of the source from one chopped beam to another is accomplished by moving (or nodding) the telescope, not the SMA. The separation of the chopped beams on the sky ranges from a few arcsecs to a few arcmins. This range is determined by the size of the infrared source; some sources are compact, others are very extended. The maximum chop amplitude on SOFIA will be 10 arcmins on the sky. (Both images of the chop do not have to be on the FPIs focal plane at the same time.) It can be calculated, and it has been proven experimentally, that the best cancellation of the chopping offset can be achieved with a nodding sequence of one left-beam, then two right-beams, followed by one left-beam (or LRRL nodding). An integration set is some multiple of this sequence. For example an integration set can contain 10 LRRL nods. The period of a chop cycle ranges from a few tens of milliseconds to a few seconds. The period of a LRRL nod cycle is on the order of a minute to a few, with equal integration time given to each nod position. At each nod position, there is an integral number of chop cycles. Data are not taken between nods, only at the end points, so quick telescope slewing and settling times are required for amplitudes of 10 arcmins or less. Tracking and offset-tracking must cater to such nod sequences, so the effective rms pointing stability at the endpoints of the nods over an integration set (if less than 1 hour) is as specified in SOF-1011. 4.7.5.7 Sky Rotation Corrections Sky rotation occurs because the SI focal plane is locked to the telescope's coordinate system, which is up-down in elevation and right-left in azimuth (or cross-elevation). The sky coordinate system, however, is set by celestial north-south (Declination or "Dec") and east-west (Right Ascension or "RA"). As the night progresses, astronomical sources circle the celestial north pole in the northern hemisphere (or south pole in the southern hemisphere), that is they rise and set. Because of this procession, the celestial north-south axis will rotate with respect to the telescope's elevation axis. The rate of this rotation depends on the location ( in R.A. and Dec) of the object in the sky and the position of the telescope on the earth (in latitude and longitude). For SOFIA flying close to Moffett Field, the fastest sky rotation rates (or changes to the "rotation of field", ROF) are for those objects close to the celestial North and high in telescope elevation, giving sky rotation rates of about 1 degree every minute; the slowest rotation rates, for this situation, are for those objects rising or setting with southern declinations (i.e., < 0 degrees in Dec) and low in telescope elevation, giving sky rotation rates of nearly zero. Two processes will be employed to counter sky rotation while observations are being made: (i) The first is a telescope process (the default process) called "ROF freeze-mode". Here the telescope is allowed to move, under gyro stabilization, in elevation and azimuth in such a way that the value of ROF stays constant. This can only be done for a range of 3 degrees, the unvignetted limits of the telescopes azimuth range of motion. Hence, for the fast rotators, the rotation of the sky can be kept constant for about 6 minutes. After this time, observations must stop while the telescope is moved towards the opposite telescope limit, and the ROF freeze-mode re-activated. This allows the ROF to remain constant within an integration set. The next integration set will have a new |ROF| < 6 degrees. (ii) The second is an SI process using an instrument rotator mounted between the SI and the telescope's mounting flange. In this case, the instrument rotator will remain stationary during an integration set, and the ROF will be kept constant using the ROF freeze-mode. After an integration set (or several depending on the rotation rate), the instrument rotator will be rotated (< 6 degrees) so the focal plane of the SI sees no change in ROF for its next integration set. Hence, while used as a counter to changes in ROF, an instrument rotator will be used discretely at a rate less than every 6 minutes, and for rotations of about 6 degrees or less per move. It is important to note that the SI rotator will not be moved while the telescope is tracking to the specifications given in the SOF-1011. The instrument rotator, however, will also be employed for polarimeters. For these SI's it is necessary to rotate the SI with respect to the telescope, so polarization due to the telescope can be removed from the analyzed data. Here the procedure will be to rotated the SI by 60 degrees once in every flight leg (on average) by using the instrument rotator. This rotation is rather severe, and can only be accomplished if such a rotation can be made without losing large quantities of cryogens from the SI, and the c.g. of the SI is close (TBD) to the rotation axis so the telescope balance can be maintained using the telescopes fine balance. Once the SI has been rotated, a number of integration sets will be taken in this position using the ROF freeze-mode/instrument rotator procedure to counter ROF changes. Then the SI will be returned to its original configuration with respect to the telescope before the 60 degree rotation. 4.7.5.8 Displays and Quick-Look Data Analysis During observations, the science investigator team will: setup and record integration sets; verify and/or change the boresight; tweak the telescope position to get a better signal; compensate for sky rotation angle changes; and alter integration parameters (e.g. use different filters in the SI, or change chop amplitude). The investigator team will also: monitor the incoming data from the SI; check the datas storage (with correct housekeeping headers); use quick-look software to carry-out preliminary data analysis; monitor displays showing the observatory housekeeping data; keep a logbook for data reduction and analysis purposes; and assist the telescope operator as needed to assure optimal telescope settings and commands are achieved and executed. Based on these outputs, analyses, and displays the team may decide to change the observing strategy to optimize science return. In many ways the SI will be the most sensitive and scrutinized monitor of the mission system. The investigators could be the first to notice that the observatory is not performing optimally. They will either see problems in the raw data outputs, or see it after analyzing the data using quick-look data analysis. Usually the PIs will concentrate on the raw data and the GIs will work on the data analysis. These two groups must be able to work closely together. If the science team has noticed a problem with the data, they, with the telescope operator, will look in a number of areas to diagnose the problem. Hence, the following must clearly be displayed at all times: (i) The raw and processed images of the WFI (Wide Field Imager), FFI (Fine Field Imager), and FPI (Focal Plane Imager) must be displayed. These cameras show if the telescope: is tracking with the correct accuracy and stability; is tracking on the correct star so the SI is boresighted correctly; has the correct rotation angle for the sky (using a rotation star pair in the WFI); and has the correct settling time, amplitude and position angle when the telescope is nodding and chopping. Integration wait times for the SI acquisition system may have to be changed if the telescope is taking longer than expected to settle at each end point. (ii) The waveform of the SMA must be displayed. This will show the stability of the chop and the chop settling time. This will show if a pointing image instability is due to the SMA or not. (iii) The water vapor monitor output must be displayed showing a time history. The level of water vapor directly affects the transmission of the astronomical source. It is important to see if sky transmission has changed. (iv) Telescope cavity and telescope temperatures must be displayed. Large background offsets will result, and seeing degrade, if there are large temperature differences within the cavity. The aircraft may fly into warmer air, which might cause such gradients to occur. (v) A graphical display of the telescope's position within the cavity, and within its limits, must be displayed. If the telescope is close to a limit, or a cavity element (e.g., the door in a line-of-sight sense), large background offsets and noise in the data may result. (vi) The flight track map of the aircraft compared with that in the flight plan must be displayed. Large deviations (caused by winds) could be the cause of the telescope's non-optimum position in the cavity. Also this display should clearly show time left on leg, so observing strategies can be formulated to fit into the time left. If the flight plan has been altered, this display should show the new calculated the flight plan to achieve the remaining observations. This may have to include a dead-leg, if the winds have moved the aircraft too far off course. Aircraft heading and attitude (pitch, roll, yaw) should be shown here also. (vii) A large video screen must be visible summarizing the observatory data that is being put on the science data file headers: For example, UT time, object name, telescope RA & Dec, water vapor, sky rotation, SI rotation, SI boresight, chopping parameters, telescope focus, etc. This header must be checked to see if it is correct; if values are incorrect, then quick-look data analyses will be incorrect since these use the headers in the data files. (vii) The telescope parameters that the telescope operator uses to diagnose the telescope performance must be clearly displayed: For example, torque motor currents, fine balance position, etc. If the telescope is not performing well, this will often be reflected in the SI data. For example, erratic torque motor currents may keep the telescope pointed, but may cause large EMI at the SI, and certainly imply that something is not right with the overall system. (viii) The status of the telescope should be clearly displayed: For example, elevation, azimuth, LOS, telescope focus, balance, caged or uncaged, tracking or not tracking, gyro stabilization or not, VIS activated or not, RIS activated or not, etc. This information clearly displayed helps a great deal during set-up periods, and will help E/PO programs. (ix) The status of the vacuum pumps should be clearly displayed: For example, on/off, pressures, flow rates, etc. Some SI's require their cryogens to be pumped, sensitivity of these SI's will decrease if the pumps are not working. (x) The status of communications should be displayed: For example, transmission power of all aircraft radios, intercom channel distribution, etc. Certain radio transmissions may affect the SI. During the observing leg, the telescope operator is working closely with the science team with the set-up of the telescope for their integrations, and is monitoring all telescope systems. The computer specialist (if on board) is monitoring and helping the science team with their computer network and systems, including observatory software packages. After the initial setup of the observing leg, the mission director will help coordinate the E/PO program with the science program. Within limits, E/PO visitors will be able to interface with the scientists and become familiar with the data acquisition process and the science questions being investigated. The E/PO program may also at this time start up their own experiment. The E/PO team will be able to capture images from the WFI, FFI, and the FPI at the E/PO console. A progressive program of optical imaging using these Non-IR sources will be developed which successive E/PO groups can contribute to. The mission director will monitor all aspects of the mission and the mission system with an emphasis on flight safety (e.g., power consumption levels, telescope motion). On SOFIA this monitoring to a large extent will be automated, where if a system parameter gets too close to or goes outside a limit, then a warning is given to the mission director (and telescope operator). The mission director will maintain the mission log: All problems or concerns must be reported to the mission director so they can be incorporated into the log. As an extension of this task, the mission director will make sure all mission housekeeping data are being recorded correctly. If flight path or aircraft attitude changes are required, it will be the mission director who will negotiate the change with the flight crew. If air turbulence occurs, all flight participants must be seated, this will be enforced by the mission director. 4.7.5.9 Possible Automation During a leg, all of the operations noted in the general description above may be automated within the telescope operator's and investigators systems, using computer routines as appropriate for efficiency or simplification. Movements of the telescope to other positionsnods, scans, and smooth slewsmay be commanded automatically at any time, to be accomplished as rapidly as possible. Any changes in chopper performance can be automatically noted (assuming a trackable object in the focal plane image) and corrected. Changes to chopper configuration, offset positions, and observing locations can be all available directly to the investigator. Any commands will be acknowledged, and a function complete signal will be returned to the investigator when the command has been accomplished. The RA and Dec of the telescope may be automatically monitored at rates up to 10 Hz, and tracking system performance summaries made available at all times. Moving the Telescope to a New Position: To move a telescope to a new position, the investigator or operator executes a move the telescope command, providing the new coordinates. If absolute pointing of the telescope is in effect, the coordinates may be specified in RA and Dec. The coordinates may also be specified as offsets from the current position, or in offsets in focal plane coordinates (X,Y, and ROF), or by clicking a location on the user interface for the tracker subsystem. When the move command is received by the tracking subsystem, it turns the command into appropriate commands for the TA, which positions the telescope to the new location. When the telescope is within a predefined distance (typically the same as the loss of pointing distance limit) of the desired position, a position acquired signal is sent to the investigators system and is displayed on appropriate monitors. The system will be maintained at this position until a new command is received. Command/Display Coordinate Systems: Many coordinate systems will likely be available for commanding the telescope and seeing its position, but the most used one will probably be an absolute coordinate system based on RA, Dec, and ROF. Use of this coordinate system requires that the telescope be tracking on at least two identified targets, or that the TA gyro system provide pointing data to the necessary accuracy. This system is recommended for use whenever possible, because it unambiguously defines the precise intent of moves, scans, and the like, and supports readily understood integration of other subsystems such as the chopper. If a telescope-local coordinate system (such as X, Y, ROF offsets) are used to specify nods, moves, and other motions of the telescope, the effect of the requested move in sky coordinates is undefined. The telescope systems will attempt to maintain a fixed rotation reference as moves are performed, but only through an absolute pointing system can the actual position of the telescope be determined. ROF (Rotation of Field) Control Modes: The default ROF control mode can be set for each investigator. The most common is expected to be ROF freeze mode, in which ROF is locked to a particular value at the beginning of observations on a leg. (The value will be chosen to maximize the duration of observations before an ROF correction is needed.) The ROF will remain locked until, given current operating conditions, the facility is within several minutes of a possible loss of pointing condition due to telescope limits. The investigator will be notified of the impending change, and, unless a correction is prevented, the rotation of field will be adjusted during the next approved nod (or, at the investigators option, at the next investigator command to adjust ROF). The ROF will go to the optimal position for maximizing duration of observations before the next adjustment is required. Error Handling: Any error conditions during setup or normal operations are annunciated and automatically corrected if possible. Perhaps the most likely error, a condition where the telescope is no longer pointed at the ideal location (a loss of pointing condition, which may or may not result from a loss of lock on the tracking targets), results in enunciation of the error to the investigators computer system and mission crew, and automatic attempts to reposition the telescope. In a worst case scenario, this is essentially another execution of the acquisition process. 4.7.5.9 Manual Alternative Any of the above steps can be done manually. This section focuses on processes we might choose not to automate in the first operational release, and whether an alternate (non-automatic) approach exists. The Observatory should be automated for the initial set-up, but any individual activity could be a manual one: input of the object name, RA, and Dec setting the correct telescope and door elevations initial set-up of the chopper setting up the tracker parameters and modes (if different from nominal) A number of simple processes are also expected to be automatic, but could be enabled manually instead: uncaging and gyro-stabilizing the telescope blind pointing to the object (this could also be just a readout, with manual corrections) star overlay is displayed on the imager screens from the facility star database There does not appear to be much advantage to leaving these processes manual. Manual intervention is most likely to be desirable after the target is within 2 arcminutes of the boresight (i.e. after the blind pointing step is completed). At this point the operator, or the PI team might take control of the telescope. The steps would be as follows: Star Field Recognition: The star overlay is visually compared to the actual star field in the wide field imager. The track objects are manually identified in the field and on the overlay, and a link is established between two of the trackable objects and their overlaid counterparts Absolute Positioning: The telescope is repositioned to bring the science object onto the boresight. This might be accomplished by using the mouse to match up at least two stars with the corresponding overlay "stars" and then commanding the telescope to bring the two together. Integrated Tracker Setup: Once the telescope is boresighted on target, the operator selects the guide objects for tracking. (The system could still identify likely track objects with some kind of graphical marker, but it would be at the users description to use them, or choose another object.) The selection of the track objects would be as easy as clicking on the object with the mouse. Once all track objects have been identified, the system would be notified to start tracking. If chopping is enabled, the operator may want to adjust the chop by using the mouse to select where the chop should be, and letting the system adjust the chopper amplitude. Tracker Operations and Auto-Recovery: Finally, the user would use the mouse to mark the left and right beams. Losses of lock would be handled manually. 4.7.6 The Rest of the Flight: As the time on the first flight leg is close to running out, the mission director will inform everyone. This should not be a surprise, since the "time left on leg" is clearly displayed for all to see. Once the investigator has finished observing (or has been forced to), the telescope operator will cage the telescope to initiate the "transition between flight legs" phase as outlined in 4.7.4. The next leg is setup and executed as described in 4.7.5, excluding the focus and boresight procedures. The rest of the flight proceeds in this way (i.e., cycling through 4.7.4 and 4.7.5), until the end of the last observing leg. 4.7.7 End-off Last Observing Leg and Descent: Once observing is completed, what happens next depends on whether the descent will begin right away or whether more time will be spent at altitude, and other circumstances. If there is any time left at altitude, then the telescope may be uncaged after the turn, and used for whatever purpose necessary for whatever time is left. Examples of activities that might take place after observing is complete, and before descent begins are: checkout of any problems experienced in flight, planned telescope or SI system tests, and education activities. Descent: Once the descent begins there is not much time left in the flight, and final wrap-up activities must occur. These include: - center and cage (i.e., cage telescope at 40 degrees elevation) - Stop tracking - Stop gyro control - Close cavity door - Turn off RIS - Turn off VIS - Shutdown SI (PI discretion) - Entries into mission log - Finish up "paperwork" (flight statistics, squawks, other forms); this should all be computerized - Start nitrogen purge; other cavity environment controls as necessary - Shutdown E/PO experiments and observations - Shut down water vapor system It is extremely important to start the nitrogen purge of the cavity as soon as the cavity door is closed and the plane commences its descent, otherwise water will start to condense on the optics, and degrade the telescope's emissivity until the next recoating of the mirrors. 4.7.8 Landing and Taxi: During the taxi, although everyone on board must remain in their seats with seatbelts on, various activities are taking place, such as making the final entries into mission logs, completing notes and flight records. The scientists may be looking at data, or taking whatever actions are needed to shutdown the SI electronics systems. There may be discussion of the plan for post-flight activities, or the schedule for that day. In particular, if there have been problems on the flight, there may be discussion of the problems, the plan for addressing them, and possible impacts on the next day's schedule. The telescope operator may use the computers to look at telescope system data from the flight. Some more telescope system shutdown actions may be performed. The important comment here is that the computers are up and running, and everyone is on the intercom. The mission director is finishing the mission log with the conclusions of the discussion taking place. This log will be given to the SSMOC controller (see 4.5.1). 4.8 Maintenance Processes 4.8.1 Scheduled Maintenance Figure 4.0-1 gives a Level-1 Schedule of SOFIA operations and scheduled maintenance over the 20 year lifetime of the observatory. The current maintenance program schedule complies with all FAA and UAL requirements for a 747SP aircraft. During development, test, FAA certification of the modified aircraft and mission systems and subsequent receipt of the Supplemental Type Certificate (STC), additional maintenance and inspection requirements will be identified. These additional scheduled maintenance and inspection tasks, required under the STC, will address such Observatory elements including, but not limited to: New bulkheads Fuselage modifications Flight control system rerouting through the cavity Other aircraft and mission system modifications, rerouting or relocation - Mission subsystems including the cavity door, MCCS, Water Vapor Monitor and Telescope Assembly Science Instruments All of the maintenance and inspection items and their required intervals will be approved by the FAA as a part of the STC approval process, and by NASA. Once the STC has been received, UAL will update their existing maintenance program for SOFIA, by adding the additional SOFIA unique maintenance and inspection tasks and revising existing tasks in accordance with the terms of the STC. The result will be a maintenance program with characteristics and requirements different from UALs standard 747SP program, but one which will be implemented using the same planning, implementation and safety processes that are currently in use throughout UALs maintenance operations. 4.8.1.1 Aircraft System Aircraft System daily maintenance and A-checks will be performed for the most part at the SSMOC by AOS mechanics. The Aircraft will go to Oakland for heavy checks (C and higher, see below). Some Aircraft Subsystem maintenance/repair will be sent to outside vendors or UAL, if it is more cost effective than to perform the maintenance/repair at the SSMOC. Figure 4.0-1 shows the aircraft maintenance schedule over the 20 year lifetime of SOFIA. Below are the descriptions (including tasks) of each kind of aircraft maintenance check referred to in the schedule. Excluded from the tasks listed below are major engine overhauls which take between 60 to 90 days per engine. These overhauls are not to be confused with engine maintenance on the wing; these refer to overhauls where the engine is brought up to specifications, and are performed at an engine maintenance center such as UAL's maintenance center at SFO. The engine overhauls for SOFIA will be made in series, so only one engine need be leased to replace the engine removed for an overhaul. An overhaul of an engine will occur approximately every 5,000 flight hours, which translates to about every four years with the flight rate of SOFIA. It is planned to stagger the engine overhauls, by only overhauling two of the engines during development. Then approximately two years into operations the engines which were not overhauled will be overhauled in series (a total of 180 days); a spare engine will be leased for this 180 day period. The overhaul schedule of the engines will to some degree coincide with the C-checks for the aircraft. TABLE 4.8.1-1: RELATIONSHIP OF MAINTENANCE CHECKS CHECK MAXIMUM INTERVALCHECK INCLUDES:NOTES Preflight CheckSee note Accomplish prior to all flights.Post Flight CheckSee notePreflight Check Accomplish after all flightsStorage Check (ST)7 daysA-Check See notePreflight Check Postflight Check ST Check Accomplish every 460 hours, segmented into 4 segments. Accomplish each segment every 115 hours.C-Check2 YearsPreflight Check Postflight Check Next due A-Check Includes next V-Check due.V-Checks 2 Years Each V1,V3,V5, & V7 Corrosion Check has a 2 year interval. Each V2 & V6 Corrosion Check has a 4 year interval. The V4 Corrosion Check has a 6 year interval. The V8 Corrosion Chk has a 12 year interval. H-Check (HMV) 6 YearsPreflight Check Postflight Check Next due A-Check Next due C-Check V4-CheckIncludes next V-Check due.D-Check 12 YearsPreflight Check Postflight Check Next due A-Check Next due C-Check H-Check V4-CheckIncludes next V-Check due.* Pending FAA ACO and CMO approval. PRE FLIGHT CHECK Accomplish per check list prior to every flight Time required for tasks - 30 minutes TASKS 1. Walk-around inspection of A/C per standard procedures. 2. Power up A/C 3. Accomplish mission critical tasks. (Tasks will be identified and incorporated as appropriate). POST FLIGHT CHECK Accomplish after all flights. Time for tasks - 4 hours. TASKS 1. Walk-around inspection of A/C. 2. Review log book items, correct or defer as required. 3. Review any mission critical A/C non-routine write-ups. 4. Correct or defer all non-routine work discovered 5. Pre-service fuel, if required, and re-fuel aircraft. 6. Engine general visual inspection. 7. Service gases: e.g. oxygen, tire pressure. 8. Service fluids: e.g. engine oil, hydraulic fluid. 9. Perform an exterior light check. 10. Check brakes and tires for wear 11. Check fuel tanks for water and sump if present 12. Accomplish all additional SOFIA aircraft system tasks to support flight objectives. (Tasks will be identified and incorporated as appropriate.) 13. Check overwater emergency equipment. 14. Service lavatories, galleys, and set up cabin. ST-CHECK Accomplish every 7 days when A/C is in storage. Accomplish UAL short term or long term storage tasks. Tasks not requiring accomplishment every 7 days will be accomplished at multiple ST-Check intervals. Accomplish storage tasks only. All storage tasks will be accomplished in accordance with existing United Airlines procedures with modifications to support aircraft mission. Accomplishment of this check will zero the ST Check. A-CHECK Accomplish every 460 flight hours, accomplish in 4 segments not to exceed 115 hours. Tasks derived from UA 747 SP Maintenance Program as modified to support SOFIA modification and mission. Tasks to be segmented in conjunction with Service Checks. Every fourth segment will require 24 hours elapsed time and will include heavy maintenance on one engine. Time required for tasks - 16 Hours for each segment except for the 4th segment. TASKS 1. Includes all Post Flight and Preflight Check tasks. 2. Light routine maintenance on 3 engines and heavy routine maintenance on one engine. 3. General visual of modified area of fuselage, and operational check of modified telescope door and other appropriate systems and components. 4. Service fluid in batteries, starter units, generator automatic transmissions. 5. Replace heavy-use filters. 6. Inspect heavy wear areas of cockpit, cabin and lavatories. 7. Measure deterioration of specific components. 8. Check emergency equipment for condition and/or expiration date. 9. Perform SOFIA mission maintenance tasks to support mission capability. (As tasks are identified they will be incorporated as appropriate.) 10. Lube 11. Operationally check redundant systems to assure availability. (4A interval) 12. Functionally check systems where deterioration can be measured. (4A interval) 13. Weigh aircraft. (NASA request at 4A interval) C-CHECK Accomplished every 2 years. Tasks derived from UA 747 SP Maintenance Program as modified to support SOFIA modification and mission. Time required for tasks - 10 Days to 20 days TASKS 1. Includes next A check. 2. Detailed inspection of some structure including modified section. 3. Inspection of wiring for heat/vibration deterioration. 4. Lubricate flight control surfaces and mechanisms. 5. More extensive operational check of back-up systems. 6. Replace specific components with known deterioration profiles. 7. Perform cabin cleaning and maintenance. 8. Perform engine on-the-wing maintenance. 9. Functional checks of several entire aircraft systems (hydraulic system, parts of oxygen system) 10. Perform SOFIA mission maintenance tasks to support mission capability (As tasks are identified they will be incorporated as appropriate.) 11. Next due corrosion tasks as derived from Boeing CPCP Document D6-36022 as amended. Note: Interval revisions to the Boeing document requires FAA ACO approval prior to implementation. Heavy Maintenance Visit (HMV-Check) Accomplished every 6 years. Tasks derived from UA 747 SP Maintenance Program as modified to support SOFIA modification and mission. Time required for tasks - 56 Days TASKS 1. Includes next due C-Check. 2. Refurbish interiors, lavatories and galleys as required. 3. Perform corrosion repair/prevention treatment. 4. Conduct system operational checks. 5. Open fuel tanks for cleaning and structural inspection. 6. Perform flight control surface and actuator rework. 7. Perform detailed inspection of some structural items. 8. Accomplish A/C modification projects. 9. Perform SOFIA mission maintenance tasks to support mission capability (As tasks are identified, they will be incorporated as appropriate.) 10. Accomplish SOFIA mission modification projects as identified. 11. Next due corrosion tasks as derived from Boeing CPCP Document D6-36022 as amended. Note: Interval revisions to the Boeing document requires FAA ACO approval prior to implementation. D-Check Accomplished every 12 years. Tasks derived from UA 747 SP Maintenance Program as modified to support SOFIA modification and mission. Time required for tasks - 60 Days TASKS: 1. Includes HMV-Check and next due C-Check 2. Comprehensive inspection of aircraft structure. 3. Most complete operational/ functional test of aircraft systems. 4. Scheduled replacement of major A/C components (landing gear, flight control surfaces etc.). 5. Exterior repaint, if required. 6. Accomplish A/C modification projects. 7. Accomplish SOFIA mission modification projects as identified. 8. Perform major corrosion inspection/repair/ prevention treatment. 9. Accomplish detailed inspection of the modified structure area. 10. Overhaul landing gear. 11. Accomplish SOFIA mission maintenance tasks to support mission capability (As tasks are identified, they will be incorporated as appropriate.) 12. Next due corrosion tasks as derived from Boeing CPCP Document D6-36022 as amended. Note: Interval revisions to the Boeing document require FAA ACO approval prior to implementation. 4.8.1.2 Mission System Mission System maintenance will be performed for the most part at the SSMOC by MOS technicians and engineers. When the Aircraft goes to Oakland for heavy checks, some Mission System maintenance may be performed at Oakland, by MOS personnel, under the oversight of UAL mechanics, TBD. Some Mission Subsystem maintenance/repair will be sent to outside vendors/contractors if it is more cost effective than to perform the maintenance/repair at the SSMOC. 4.8.1.2.1 Mirror Re-coating Procedures: In order to maintain the telescope with an emissivity of < 0.13 (with an aluminum tertiary) the primary mirror will be recoated twice a year, and the tertiary and secondary mirrors more frequently as needed. The present plan is to recoat the primary mirror in a facility within the SSMOC, the tertiary and secondary mirrors will be recoated by external facilities under contract. There will be spare secondary and tertiary mirrors, so the time to recoat these will not subtract from observing time. There will be only one primary mirror, the recoating time for this element will subtract from observing time. The removal of the primary mirror assembly, the stripping of the primary mirror, the re-coating of the mirror, the installation back into the aircraft of the primary mirror assembly, and the realignment of the telescope optics should not take longer than a five day work week. As much as possible, the recoating of the primary mirror will coincide with other mission system and aircraft maintenance. Below is an outline describing how the primary mirror will be recoated: (1) For primary mirror assembly removal, the SOFIA telescope will be rotated within the telescope cavity to an elevation of 0 degrees, so the backend of the primary mirror cell is adjacent to the cavity door. (2) The primary mirror assembly will be removed from the aircraft by a leased, tall crane (i.e., it will not be a ceiling crane). (3) This crane will remove the primary mirror assembly from the telescope and will place it on a transport cart. The cart will have the ability to secure the primary mirror cell and will have pivots so the assembly can be turned to any angle. (4) The primary mirror assembly then will be rolled into a nearby cleaning and stripping room. This room will be kept at a clean-room level of 100,000. Here the primary mirror will be rotated to face upwards. (5) The mirror coating then will be stripped with the procedure approved by Schott for Zerodur. The primary mirror cell will be tilted so the acids and washing water can drain into a special hazard waste tank. Drainage cannot be through the central hole of the primary mirror, since this will be blocked. (6) Once the mirror has been stripped, the mirror assembly will be rotated to a down looking position and moved into the adjacent mirror coating room. This room will be kept at a clean-room level of 100,000. Although this room is at the same cleanliness level, it must be separate from the stripping room, since the chemicals in the stripping room will remain airborne to some degree. (7) A ceiling bridge crane (with proper fixtures) will lift the primary mirror assembly from the cart and will place it in a steel, evaporation chamber face down. (8) The chamber will be sealed and pumped down to 10-6 torr. Since the backside of the primary mirror cell will outgas, means must be provided to isolate this part of the primary mirror assembly from the vacuum chamber. There will be a final in situ cleaning of the mirror with an ion glow discharge using oxygen and argon gases. (9) There are three possible methods for coating the mirror at present: (a) evaporation from tungsten filaments, (b) evaporation by an electron-beam gun, and (c) sputtering using an anode bar. After evaporation or sputtering (20 minute procedures), time (approx. 30 minutes) will be given to cool the new aluminum coating. The chamber will then be vented using dry nitrogen then filtered air over a time period of 30 minutes. (10) The crane will then be employed to remove the mirror assembly and place it on the cart. The cart will then rotate the mirror to an up-ward looking position, and the mirror system reassembled (e.g., the tertiary pedestal should be reattached). (11) The cart will be wheeled back to the aircraft where the primary/tertiary mirror system will be installed into the aircraft by the tall crane. (12) Re-alignment of the optics (primary with the secondary) will then proceed (see Section 4.8.1.2.3). 4.8.1.2.2 Cavity and Mirror Cleaning Procedures: Cavity cleanliness and frequency of cleaning will be set to ensure a total emissivity for the telescope of <0.13 (with an aluminum tertiary). The cavity will be kept at a cleanroom level of class 100,000 (TBD). The mirror will be cleaned in-situ once every two weeks using CO2 snow cleaning method. After this method is used the cavity floor and walls will be vacuumed before the next flight. Experience on the Keck telescope in Hawaii shows that a static charge build-up on the front surface of the mirror occurs if this method of cleaning is used, and that resulting static discharges can damage electronics attached to the mirror support structure. To prevent this static build-up, the Keck mirrors have grounding strips from the front surface of the mirror. In addition, if water or water vapor should condense on the mirror surface, then a distilled water wash in situ will be required using lint free tissues. 4.8.1.2.3 Optics Alignment Procedures Whenever any TA optics (including the imagers) are disturbed in anyway, re-alignment of the optics to some degree must be performed. If a TA subsystem must be removed from the TA for maintenance (e.g., one of the TA imagers or the tertiary mirror assembly), then internal re-alignment of that subsystem will be performed in the TA Optical Lab after maintenance. The internally aligned subsystem will then be installed on the TA, where alignment of the subsystem to the TAs optical axis will be performed within the cavity with the cavity door closed. This alignment, and the alignment procedure after changing or removal of any of the telescope mirrors (i.e., primary, secondary, or dichroic tertiary) will be performed using lasers, theodolites, alignment cubes, and extensometers, mounted in various configurations within the cavity and at the TAs focal plane. Rarely, if ever, will there be the need to check the overall alignment of the telescope using a Ground Operation (i.e., when the aircraft is positioned outside the hangar with the cavity door open looking at a star). Details of the optical alignment procedures will be provided by the German TA Consortium in their Optical Assembly Alignment and Verification Plan. 4.8.1.2.4 Aircraft Mission Systems Maintenance Procedures [This paragraph still in work and will include the Water Vapor Monitor.] 4.8.1.2.5 Telescope Subsystems Maintenance Procedures [This paragraph still in work.] 4.8.1.3 Science Systems The Science Instruments and associated equipment, and the equipment at the SSMOC similar to science instruments (e.g., the water vapor monitor), will be maintained for the most part at the SSMOC by scientists from the Science Support Group and technicians from the MOS Group. Some Science Instrument maintenance/repair will be sent to outside vendors/contractors/universities/research institutes if it is more cost effective than to perform the maintenance/repair at the SSMOC. 4.8.1.3.1 Facility Science Instruments Maintenance Procedures For the most part, SSMOC personnel (from the MOS and Science Support groups) will maintain the facility science instruments at the SSMOC. Occasionally, if a major repair is required, it may be more cost effective to ask the original developers of the science instrument to perform the repair given appropriate funding for the task. (PI and Special Science Instruments are maintained by the PI at his/her home institution.) [The maintenance program for the facility SIs will be developed by the outside science team developing the facility SI. The USRA Team, NASA, and the FAA must approve all maintenance program plans.] 4.8.1.3.2 TA Simulator Equipment and TA Performance Test Equipment Maintenance Procedures MOS and Science Support personnel will maintain the TA Simulator Equipment and TA Performance Test Equipment at the SSMOC. [The maintenance program for these items will be developed by the USRA Team, and approved by NASA and the FAA (where applicable).] 4.8.1.4 SSMOC (Ground Facilities) Maintenance of the ground facilities at the SSMOC will be under the overall management of the facilities manager in the Office of the Director. This manager will see that the building and its facilities are maintained. However, each of the five SSMOC functional groups will be responsible for the maintenance of the equipment in their areas of the SSMOC. Ames Research Centers Facilities Management Division (Code JFP) will determine and provide all essential maintenance to the N211 structure and integral systems. 4.8.1.5 Inventory Control There will be two independent but similar inventory control systems at the SSMOC which will keep track of all spare parts and consumables required to run and maintain the SSMOC, the Airborne Observatory, and the Science Instruments. The first is the UAL inventory system, which is kept by United and has a worldwide tracking capability for aircraft parts. UAL will add, to this inventory system, parts which will be SOFIA Aircraft specific. The AOS Group in the SSMOC will use the UAL inventory system. The rest of the SSMOC will use a closed inventory control system which will imitate the UAL inventory system, but on a much smaller scale. This system will be kept by SSMOC personnel in the MOS Group and is for all SSMOC personnel. As in the UAL system, those parts and consumables that require FAA certification will be kept separate from the inventory that does not require certification. 4.8.2 Unscheduled Maintenance Unscheduled maintenance will be performed per NASA and FAA approved plans and procedures accordingly. All efforts will be made to minimize mission impact. 4.9 Continuous Improvement Process 4.9.1 Upgrade Planning and Scheduling As stated in Section 3.2.5, the Continuous Improvement Group is charged with translating inputs from the science community, SSMOC staff, and performance metrics into design concepts with development plans, budgets, and schedules for potential facility upgrades. These will be discussed, authorized (or rejected), and prioritized within the SSMOC management team. This group will manage all approved upgrades and new designs. This group is small, but once an upgrade has been approved, this group will expand as necessary to fulfill the tasks of the upgrade using subcontracts, and personnel (if appropriate) from the other SSMOC groups. The Continuous Improvement group will: write the statement of work for the subcontract; approve final designs; coordinate the engineering and fabrication work with mission system and aircraft schedules through the Operations Control Center; make sure these are NASA and FAA approved and compliant; supervise integration and test of the upgrade; accept the new systems; manage the development and receipt of all new documentation associated with the upgrade; and supervise the training of SSMOC staff in regard to the upgrade. After the upgrade is complete and integrated, the Continuous Improvement group will resume its original number of personnel. The NASA Ames Airworthiness and Flight Safety Review Board (AFSRB) will review and have final approval authority for major changes to the airborne observatory that may affect airworthiness. Minor changes with no airworthiness impact will not require AFSRB involvement; the AFSRB will make all such determinations. The planning, preparation, and development of Observatory upgrades will be carried out, as much as possible, without affecting the science research flight rate. Upgrades, which will require considerable down time of the Airborne Observatory, will occur as much as possible concurrently with heavy aircraft checks and during the periods designated for large Airborne Observatory upgrades. These periods are nominally about 2 months in duration, every 5 years (TBD). 4.9.2 Observatory Performance Testing Procedures Tracking of performance metrics will be one of the primary methods of monitoring the effectiveness and efficiency of the Airborne Observatory and SSMOC during SOFIA operations. This tracking will be the responsibility of the Continuous Improvement Group, but will be carried out in practice by a number of SSMOC Groups. For example, facility science instruments will be used to measure the telescope's performance in regards to emissivity, infrared background, and image quality at non-optical wavelengths. These measurements will be performed as much as possible while taking science data, and by personnel in the MOS and Science Support Groups. Their results will be given to the Continuous Improvement Group with recommendations. In addition, the Airborne Observatory is being designed to have self diagnostic capabilities. These will be observed by MOS and AOS personnel and passed on to the Continuous Improvement Group. Some results will not imply the necessity for an upgrade, but for early maintenance on a subsystem (e.g., mirror coating). This recommendation will be directed to the Operations Control Center for scheduling into the maintenance program. The total list of performance metrics is TBD at this time, but as a minimum the following performance metrics will be tracked during SOFIA operations: Description of metricNotesSuccessful Flight Hours (SFH)The definition of SOFIA SFH is given in the SOFIA contract. Performance incentive fee is based on SFH. Operational efficiency Number of successful flight hours divided by annual operations costObserving efficiencyRatio of successful observing time to total observatory time at altitude Customer SatisfactionMeasured by post-flight-series surveys of scientists, E&PO participantsProposals received/ funded per year + Flights granted per proposalSeparate tracking for University, government, German, otherScience quality and impactMeasured by number of science publications, number of journal citations, lead science articles in periodicals such as Science News and other TBD meansCostIncluding actual vs. planned cost, cost to complete, cost trendsAccident, incident, and hazard/ near-miss reportsTo be included in Contractors quarterly report.Work hours lost due to injuryTo be included in Contractors quarterly report.Trends in availability and reliability of the observatoryUnplanned downtime and causes 4.10 Deployment Process The deployment process will be a "turn-key" operation; whereby, a science mission will be planned 1 day after the airborne observatory arrives at the deployment location. Once a deployment has been identified by the Observatory Director/ Peer Review (see Sections 3.1.2.7 and 3.1.2.8) and scheduled by the Operations Control Center, a small cadre of SSMOC staff, called the Deployment Group, will be formed. This group, with representatives from all the SSMOC organizational groups relating to the deployment, will work closely with the Operations Control Center and will be responsible for the scheduling and planning of all activities relating to the specific geographic, science, and maintenance-ground handling mission requirements for a particular deployment. The deployment group is also responsible for developing procedures relating to specific deployment scenarios. The procedures will include: packing and shipping of deployment equipment and inventory (i.e., the deployment kits); the ordering and handling of special materials (which may be hazardous) at the site required for both science and maintenance tasks; the set-up of the mission facility site and accommodations for the deployment team; and emergency procedures. A deployment begins when the Airborne Observatory leaves Moffett Field for the deployment site, and ends when the Airborne Observatory returns to Moffett Field. 4.9.1 Extended Deployment (~ 15% - 20% of all research flights) 4.10.1.1 Background There will be one main deployment site in the Southern Hemisphere. This will probably be in Christchurch, New Zealand. This site is necessary since not all the sky is visible with flights from Moffett Field. Deployments to Christchurch are not "targets-of-opportunity" deployments, these will be discussed below. As a rule, a two month deployment to the Southern Hemisphere site will be scheduled each year; these two months will probably occur contiguously somewhere from May through to August of each year. The actual length and time of the deployment, the science instruments to be flown, and the types of observations to be made in the Southern Hemisphere will be selected by the normal Peer Review Process the year before (see section 4.2); the results of this process are known to the SSMOC at least 9 months before the start of the southern hemisphere deployment. The flight rate on a deployment may be higher than at Moffett Field, since weekend flights will be supported: On average five flights per week will be flown while on deployments (TBD). The Deployment Team is the SSMOC staff and outside scientists who are physically on deployment. Personnel on this team may rotate out with other SSMOC staff over the course of a two-month deployment. The deployment team at any given time on a Southern Hemisphere deployment will consist of: 11 (TBD) aircraft personnel (including 2 flight crew) 14 (TBD) mission system personnel (including ground and 2 mission crews) 8 (TBD) science investigators (including scientists from outside institutes) 1 (TBD) SSMOC manager/organizer 1 (TBD) E/PO facilitator A subset of this team will fly (commercially) to the deployment site approximately a week before the Airborne Observatory does. This subset will be called the Advance Team, and will consist of the flight and mission crew for the first flight of the deployment, and the ground crew required to: assemble the deployment ground support facility; meet the Airborne Observatory when it arrives; and ready the Airborne Observatory for its first science flight. Where possible, local UAL ground crew/facilities will be used. 4.10.1.2 Southern Hemisphere Deployment Site Requirements Requirements on a Southern Hemisphere long-term deployment site: (i) Airport must accommodate a B747SP, especially with aircraft access equipment and ground equipment such as power carts, air-conditioning cart, and tow vehicle. (ii) Airport with no night flight curfew (iii) Airport with available parking space for a B747SP for a period of up to 2 months. (iv) Make-shift lab space as close to the aircraft as possible with: - about 900 sq. ft. of lab/office space for science teams, with ceiling height capable of handling liquid nitrogen and helium transfers to science instruments; - Access to aircraft with heavy SI cart from the lab area; - Phone, electrical, and network access; - Accommodation for the deployable TA/MCCS simulator. (v) Work space (TBD) for rest of deployment team, with phone, electrical, and network access. (vi) Restroom facilities 4.10.1.3 Deployment Kit A deployment kit will be maintained at the SSMOC for Southern Hemisphere deployments. This kit will be configured to the requirements of a particular deployment by the deployment group, but much of the kit will be common to all deployments. The kit will be transported as much as possible in LD-3 containers, either in the SOFIA aircraft or by commercial freight carriers. The exception will be the cooling cart for the telescope cavity which will be the size and shape of an LD-26 container, and will fit in the Airborne Observatory's forward cargo hold. Where possible (and affordable), equipment will be stored at the Southern Hemisphere site permanently. Duplication of some support equipment will be necessary, since at times some equipment will need to be both at Moffett Field and on deployment. For example, there will need to be a deployment TA Simulator, since a TA Simulator must remain at the SSMOC to prepare the science instrument for the first local flight series after a deployment. 4.10.1.4 Pre- Deployment Schedule Immediately after peer review (9 months in advance): - Identify deployment countries and airfields to be used - Develop strawman flight plans to identify overflight and landing clearances required - Identify critical-path items (some countries require long lead-time for approval of clearances) - Determine routine maintenance to be carried out before and while on deployment. - Determine SI and SI team requirements on deployment. - Set up deployment schedule and milestones - Deployment budget to be finalized 6 months in advance: - The Observatory Director sends a letter to NASA HQ or NASA ARC to instigate state-department procedures for foreign country operations (TBD). - NASA or USRA (TBD) starts initial contact with foreign countries involved in the deployment - NASA or USRA (TBD) gets authorization for site visit (if required) - Identify any special requirements for deployment, and any associated engineering activities - If engineering or special needs exist, make plans - e.g. schedules/staffing/etc - for accomplishing them in time. - Determine what passport/visa/diplomatic clearance requirements are necessary. - Determine landing fees, ATC fees, weather service fees, etc at deployment airport. 4 months in advance: Establish requirements and begin identifying providers for the following: - Parking space - Hangar space if possible - Offices and lab space - Storage space - Phones/faxes/modem lines - Network interfaces and support, and computer equipment - Deployment team accommodation arrangements (including ground transportation) - Consumables: fuel, cryogens, oil, hydraulic fluids, crew and passenger oxygen, bottled water, office supplies - Tool kits and support equipment (e.g., tire changing kit) - Tug, towbar - Lavatory servicing - Ground power carts for the 747SP and for ground equipment (e.g. the ground-cooling cart). - Air start unit for 747SP if APU not installed on the aircraft. - 747SP capable air conditioning - Cargo loading equipment for a 747SP. Access equipment for a 747SP (e.g., airstairs). - SI transport and handling equipment - Cavity cooling cart (must be transported from the SSMOC for each deployment or have a second cart permanently located at the southern hemisphere site). - TA/MCCS simulator for deployments (must be transported from the SSMOC for each deployment or have a simulator permanently located at the southern hemisphere site). - Define the advance deployment team and their function. - Pick date/time/place(s) for advance site visits (if required). - Make initial contact with Freight Forwarders and Customs Brokers. 3 months in advance - Preliminary list of participants (including individual arrival & departure dates, modes of travel to/from deployment site, requirements for hotel, cars, etc) - Preliminary cargo lists including tool kits - Identify deployment items to be loaded in the cabin or cargo hold of the SOFIA aircraft, and which are to be sent by freight. - Identify cargo shipping requirements, arrangements, schedule, and costs with freight forwarders and customs agents. - Establish prearranged process to provide any spares that might be needed 2 - 1 month in advance: - Finalize deployment team membership, outlining responsibilities of each member. This includes the maintenance release procedures for aircraft dispatch before each flight while on deployment. Check that all the deployment team members have current passports and proper visas - Check that all the deployment team members have airport security/ badges if required - A check on the status of diplomatic clearances should be done at this time - Finalize accommodation arrangements for the deployment team. - If tours are planned on deployment (for public or invited guests), arrangements should be made at this time. - Finalize on need to have E/PO person from the SSMOC in the deployment team. - Finalize cargo list of boarded equipment. - Finalize list of equipment to be shipped and make shipping/customs arrangements. - Coordination with local officials, scientists, and educators in country of deployment to make arrangements and schedule for visitors who will fly as guests. 5 weeks in advance: - Set-up and test as required all deployment equipment for functionality and operation prior to packing. 4 - 2 weeks in advance - The deployment group with assistance from technicians and ground crew will begin packing for the deployment: At this point, spares for the aircraft and telescope should be ready for packing, and packing will begin. It is assumed that the aircraft is still on flight status, so ready access to the fly-away kits and boxes must be maintained during the packing process. The kits will be in LD-3 containers. A running inventory of all deployment LD-3 containers will be maintained to keep strict control of its contents whereabouts and serviceability until all are packed, boarded or shipped. All support equipment and inventory, which must be shipped, will be shipped about two weeks prior to deployment. Some equipment may need to be used in the SSMOC while the Airborne Observatory is on deployment, or it may be needed in the SSMOC during the two weeks prior to deployment. Sufficient quantity of such equipment items must exist so that a set can remain in the SSMOC while another set is shipped to the deployment location. If this equipment isnt needed at the SSMOC while the Observatory is on deployment, it may possibly be shipped aboard the Airborne Observatory to the deployment site. - Cargo boarded on the Airborne Observatory will include, but not be limited to: - Telescope spares (all to be carried if possible) - Aircraft spares (some to be shipped or supplied at deployment site) - Tool kits - Science instrument cargo (some to be shipped) - Expendables: e.g. printer paper, mag. tapes, bottled water - Equipment and Supplies: e.g. office supplies, portable copier - Manuals + other informational material - Baggage for crew traveling with the aircraft - TA/MCCS deployment simulator - Support equipment for the TA - Cavity cooling cart - Make sure routine maintenance required before deployment is/will be performed. Schedule for the week prior to departure: - Perform a deployment Operational Readiness Review which will demonstrate that all operation functions and procedures are in place. - Schedule U.S. customs visit to the SSMOC prior to departure. Usually, the airborne observatory is carrying out science flights out of Moffett Field just before a deployment. During the last flight series at Moffett Field before deployment, the first science instrument to be flown on deployment will be prepared for installation at the SSMOC. After the last flight of the flight series at Moffett Field, this science instrument will be installed (and balanced) on the telescope of the airborne observatory and will fly to the deployment site in a readied condition. Assuming that all cargo is packed and ready to go, it should be possible to carry out Moffett Field flights up until three days before departure. Two days should be reserved for instrument switchover and cargo loading, which will take place simultaneously during those two days. A likely schedule for a deployment-departure week would be: Monday - science flight from home base Tuesday - science flight from home base Wednesday - remove/install instrument and load cargo Thursday - secure cargo for deployment + final instrument checkout Friday - departure Saturday or Sunday (depending on if the dateline is crossed): arrive at deployment site 4.10.1.5 Deployment Schedule On arrival at deployment site: - Clearance through customs: The lead of the deployment team will take responsibility for the aircraft cargo manifests. Each individual on the aircraft will have filled out their own customs forms, which were available on board. Advance arrangements have been made at the point of arrival to facilitate passage through customs. - Depending on the location, the aircraft may have to be parked initially at the terminal. However, after the initial arrival (or, right away if feasible) the aircraft should be moved as soon as possible to its work location at the airport; this will allow the unloading and setting up of the deployment site to begin as soon as possible by the Advance Team. The people who flew out on the Airborne Observatory are resting at this time. - The advance deployment team will unpack and install equipment at designated site. - Operational checks are performed. - Aircraft, mission system, and SI are readied for next days planned science flight from the deployment site. If for any reason the schedule cannot be met, the lead of the deployment team will adjust the deployment schedule accordingly, with inputs from the deployment team and staff back at the SSMOC. As a rule, the flight schedule shall be maintained (just as it is at Moffett Field), and there will be no "make-up" flights (see Section 3.1.2.3). A flight series on deployment: As much as possible, a flight series at the main southern hemisphere deployment site will mimic a flight series at Moffett Field (see Section 4.6). The main difference will be that access to the aircraft will not be as convenient as at the SSMOC. Personnel will have to use flight stairs, and heavy equipment and cryogen dewars must be loaded onto the aircraft via lifts. Power will be provided to the aircraft by GPUs for durations matching those for SSMOC operations at Moffett Field (where power is supplied in the hangar from the ground facility), but since the aircraft is exposed (i.e., not in a hangar) an air-conditioning truck must also provide cooling into the cabin and cavity during the day. As at the SSMOC, the TA cavity cooldown will take place about 5 hours before take-off using the cavity cooling cart. As at the SSMOC, electrical power to the Airborne Observatory systems must not be interrupted from 2 hours before flight and during taxi and take-off. Therefore, the Airborne Observatory must be parked in such away that an APU or engine can be started before the GPU is disconnected before aircraft tow-back to its taxi position. It is planned that at New Zealand, the parked aircraft will be sufficiently close to the labs and offices, that a LAN line can be connected to the Airborne Observatory for computer connectivity. (This will probably not be the case for non-Christchurch deployments.) The science instruments for the flight series after the first flight series will be readied in the make-shift labs close to the Airborne Observatory. The TA/MCCS simulators which are deployed, may have limitations compared to those at the SSMOC, but SI installation at Christchurch must still only take on the order of 4 hours and will be similar to the procedures at the SSMOC (see Section 4.5.2). The last science instrument to fly will remain on the telescope for the ferry flight back to Moffett Field. Daily maintenance of the Airborne Observatory while on deployment will be performed in time slots similar to those outlined in Section 4.6 for a flight series at Moffett Field. These maintenance items would have been pre-planned before the deployment, and the required inventory/equipment would have been sent to Christchurch from the SSMOC or acquired at Christchurch (e.g., the leasing of aircraft equipment). After the last flight of a deployment: After all post science flight activity has ceased: - The deployment team will pack (including inventory) and make shipping and customs arrangements. They will also arrange for storage of SOFIA equipment to be left in place for the next deployment. - The cargo to be flown out by the Airborne Observatory will be readied and loaded for the flight back to the SSMOC. - Preparation and planning for Airborne Observatory departure from deployment site would have been finalized before the end of the last science flight by the deployment team. - After the Airborne Observatory has departed, part of the deployment team may have to remain behind for a few days to complete shipping and other formalities. 4.10.2 Short or Rapid Deployment (~ 5% of all research flights) On average a short deployment will be one to three weeks in total duration and the flight rate will be 4 to 5 flights per week. Short deployments to sites other than Christchurch will support only one flight series as a rule (i.e., one science instrument). The science instrument will be installed at the SSMOC and de-installed at the SSMOC after the deployment. This procedure circumvents the need for make-shift labs at the deployment site and the necessity for TA/MCCS simulators. In addition, ideally, office space for the deployment team would be close as possible to the parked aircraft, but this is no longer a strict requirement. The power and air-conditioning requirements for the aircraft would be the same as those stated for the Christchurch deployments. However, the LAN connectivity will not be a requirement on short deployments, since the office space for the deployment team may be some distance from the aircraft. Data (both housekeeping and science) will be downloaded onto tapes/discs and physically transported to and from the Airborne Observatory. The deployment teams for short deployments will be similar in size to those for the Christchurch deployments (in order to meet the flight rate) and an advance team will still be necessary (see Section 4.10.1). The planning and preparation for a short deployment will be similar to that outlined for the Christchurch deployment, the only difference being that some short deployments are targets-of-opportunity and so only have about a two month preparation time. This means that much of the 9 month preparation outlined in Section 4.10.1 must be condensed into a two month period. For some deployment sites this may not be possible for diplomatic and logistical reasons. If not, then the SSMOC cannot support that target-of-opportunity. 4.11 Data Center The Data Center will assist astronomers in all aspects of observing. These include: 1) Outreach to prospective investigators, 2) Observation preparation, 3) Conducting observations, 4) Data reduction, 5) Setting data archive format standards, and setting facility software standards, 6) Archiving the data of flights, 7) Validating the scientific measurement of Facility Instruments, 8) Maintaining an informative SOFIA WEB-Site with details below. Note: Numbers 4, 5, & 6, are at present under study, and may not be executed in operations. 4.11.1 Outreach to prospective investigators Outreach to prospective proposers to SOFIA (as well as seasoned airborne observers) is aimed at informing astronomers of the exciting opportunities available and attracting proposals from the broadest possible extent of the astronomical community, while attracting the highest quality proposals. To this end, the Data Center: - maintains an international email and postal mail address list of active IR astronomers. The WEB curator maintains the list and the Librarian is responsible for mailings. - posts SOFIA mailings and newsletters announcing proposal opportunities, support service offerings, conferences, workshops, instrument status, operational news, available jobs. All this information is also posted on the www. - through the www and in conjunction with NASA, provides science publicity. This includes an active science section on the www that points to salient papers in the different fields of astronomy, showing the possibilities and advantages of airborne observations in the IR window. (These activities also overlap with the Public Outreach and Educational goals of the Project; informing the community of the advances achieved and discoveries made.) - solicits guests to do archival research through the NASA ADP program (when and if approved and funded by NASA). 4.11.2 Observation preparation The Data Center helps both the prospective proposer and the prospective observer plan their project by: - Encouraging visits by prospective proposers and by approved observers to plan observations. - Supplying logistical and research support from the center. - Providing software tools for assessing experiments and planning observations: - Telescope Simulators - Instrument Simulators - Instrument Time Estimators - Atmospheric Absorption Modeling Code - Atmosphere monitoring data (e.g. O3 monitoring from TOMS facility) - Online atlases, such as the Infrared Sky Survey Atlas and related tools (IRSKY, SKYVIEW) - On-line spectral line data base, giving line strengths, energy states, wavelength uncertainties - Astronomical modeling codes: Blackbody Modeling, Radiative Transfer Codes such as HII region Modeling (Cloudy), PDR Region Modeling, etc., will be provided, albeit with little or no support or maintenance. - Access to imaging and processing tools such as IRAF, AIPS - SOFIA Archive searching Software - archives (wherein possible) from other IR Missions: KAO (if extant), ISO, SIRTF, IRAS, HST, 2MASS, etc.. - provides flight planning software and guidance in using it - provides flight Doppler shift computation tools - providing all of the above software tools through remote logins or via the www as well. - providing an Astronomy Library, in conjunction with NASA/Ames, which include The Palomar Sky Survey Prints, and Overlays, and other essential references and journals. - providing workstations and places to work for visitors - providing complete manuals on instruments, both on line and hard copy (as provided by the instrument teams and the facility) - providing expert guidance in the use of facility instrumentation - providing modern tools which may help both the observer prepare for the flight. These include: - digital star atlases and the software to rotate the fields for different LSTs. - catalog search tools (e.g. XCATSCAN) for discovering targets of opportunity, or significant additional targets present in a field. 4.11.3 Conducting observations The Data Center will provide the means for conducting observations in the most effective manner. In-flight software includes as much of the software list as in Section 4.10.2 as possible on-line during a flight. The minimal complement is: - quick look data reduction tools for Facility Instruments (and other instruments following the facility software standards) - detailed analysis tools for Facility Instruments (and other instruments following the facility software standards) - flight planning software - atmosphere modeling software - on-line Infrared Sky Survey Atlas (ISSA) - www access in-flight. If the www bandwidth is available, this would include and video output for educational outreach projects (see Education section). - quick access to a mirror of the SOFIA WEB Site . 4.11.4 Data reduction The Data Center will provide the observers with an environment suitable for data reduction by assuring: - the software environment outlined in section 4.11.1 will be constantly maintained, supported and regularly upgraded. - the Facility Instrument data reduction codes will be well developed and easy to use, with clear documentation. - important manuals will be available in multiple copies in all offices. - the PI team will have available sufficient computer resources such that there will be no equipment constraints to data reduction: there will be sufficient quantity and quality of high-speed processors, sufficient memories and associated peripherals (high speed laser printers and color laser printers) available to the observers so that availability of equipment will not be an obstacle. - staff astronomers and technical experts will be assigned to visiting groups and be cognizant to the experiment science goals and technical requirements - scheduling the use of the resources is done on an ongoing basis. 4.11.5 Data archive and facility software standards The Data Center will set software standards for the SOFIA Community. The standards will developed and used at the Data Center, and be the basis of the Facility Instrument data format, reduction software, and Mission Archive. Non-Facility Instrument groups are encouraged, but not required to adopt the Facility Standards in their software. The idea is that non-facility instrument teams who follow the facility standards would be able to use the facility software to reduce their data from their spectrometers and cameras. Likewise, these groups would find commonality in quick-look tools, in-flight reduction tools, and long term archive tools. As a very minimum, non-facility instrument groups will be required to follow minimum standards in their format for data archiving. The advantages of one standard for all facility software and as much as possible the PI software are: - gathering and using the best ideas from past missions for data formats and software selection - the Data Center will provide a service by explaining these and advocating these to the SOFIA community - standard programming language and routines will reduce duplication of software development (and costs) - guest observers will need to learn less when using multiple instruments - archiving and re-reducing data is facilitated A "Forum" will be held, and attended by software uses from major observatories, to select the model standard. Here is one possible standard: Data Format Example: A data set will include FITS files, representing calibration data, intermediate processing, and product data files. Primary headers of the FITS files contain standard identifiers as keywords: Observatory, telescope, instrument, observer, configuration, proposal number, proposal category, UT Date, Doppler Shift, RA, DEC, etc.. Data, (images, photometry, spectra, polarization measurements) are all stored in self-documented FITS files with a primary header as above and a FITS binary extension table. This is the format adopted by ISO and the HST. The binary extension tables format for storing data (as opposed to using "image" storage following the primary header) has proven a successful format standard for cameras (e.g. ISOCAM and NICMOS) and spectrometers alike. In the binary extension tables, multiple images and ancillary data may all be stored together and may be represented in diverse data types: bytes, integer, real, in arrays of appropriate dimensionality. Using TFORM, TUNIT and TTYPE, the extension files are self-documenting. Such ancillary data may include: time keys, raster position, detector identity, instrument configuration, apertures, tracking quality, field of view angle, integration time, wheel positions, wavelengths, beam switch flags, gain settings, temperatures, rms flux values. Likewise, multiple images that are taken together may be stored together in a single file. This format works very naturally for spectrometers where individual rms values may be stored in flat or array tables along with wavelengths, fluxes, scan numbers, time keys, quality flags, detector, aperture, order information, etc. Language Standard Example: Data reductions routines and useful analysis modules are written in IDL, with no linking to compiled codes (no C, no FORTRAN). Advantages to this standard are: - The Facility will encourage the PI teams to adopt the Facility software standards to their own advantage. The advantage the teams will derive is great: Facility camera and spectrometer packages will be written (provided the PI teams follow the data standard) such that the PI team can reduce their data with Facility software, in-flight, on the ground and from archived data. - If standards are adopted, users can use a variety of SOFIA instruments with minimal learning curves. - SOFIA can leverage off the software of other missions like ISO and HST - IDL is the most platform independent of data analysis packages. That the same code will run on PC's VMS, UNIX, and MACs provides incentive for its adoption by the instrument teams. - It is easy to learn (saving in programmer costs) - Graphic user interfaces (GUIs) can be written in this language as well as batch scripts - The language has good documentation - Public astronomy libraries of procedures exist - All code is pure ascii; there is no "compiler dependence" - IDL code may be developed that is callable from either a GUI or command line. In this way, data may be explored with a GUI, and a preferred data reduction methodology may be determined. Then batch scripts may be used to call the same routines to reduce bulk data in an automated process. 4.11.6 Data Archiving The SOFIA data archive can be considered on three levels, the first of which is mandated by NASA, and should be considered part of the baseline mission, while the third level, the most ambitious, exceeds current funding: I) data summaries, II) an archive of full backups of untreated data, and III) a user-friendly archive of well-organized, but unreduced data usable for archival research with well-supported software and staff assistance. A potential fourth level -- on which all data products are reduced and validated, and made publicly available (i.e., the IRAS model), is not currently being considered for SOFIA because of the wide variation expected for the observing procedures, observing conditions, and consequent reduction strategies. I. Data Summaries: A data summary for each flight will be compiled, and will be added to a continuously updated catalog of past SOFIA observations. Each summary would include basic information about the observation which would allow other investigators to later obtain a clear picture of what was tried and what was accomplished. It would not include the actual data or the supporting detailed observatory information needed to analyze the data. It would include the following entries from the observer log: the observers' identities, the sources observed and their coordinates, the instrument, the procedures used, the instrumental parameters (wavelength, bandwidth, integration times, chopper throw [where relevant], etc), and a few chosen highlights of the facility data, such as altitude, water vapor meter reading, and a cloud cover index. Finally, the catalog entries for each data summary will include the flight director logs, relevant observer comments, and a brief post-flight synopsis by the science PI or by a team member, giving commentary on the purpose of the mission, the degree of success and the value of the data, and problems which might not be evident from the routine data recorded. This latter PI contribution and accompanying flight director contributions will be facilitated by asking each PI team to fill out an on-line "debriefing" form subsequent to the observations but prior to landing. The PI and flight director logs will be similarly automated, not only for the purpose of producing coherent flight summaries, but also to assist all observers by having a standardized and systematic way of recording essential information. The observer logs would have a standard, but customizable design. Ideally, much of the information appearing in the observer log would be automatically entered by the Observatory software, and the observer would use it largely to check intention versus actuality. The data summaries will become part of the on-line Catalog of SOFIA Observations, which will be updated after each flight and maintained by SSMOC personnel. Search routines to ferret out entries based on source names, positions, frequencies, and/or investigators will be adapted from existing web-based routines (e.g., NASA's abstract service or the ISO archive search routines). The data summaries are not meant to convey the scientific results in any significant detail, but to indicate what was attempted, how successful the attempt seems to have been after the first look and therefore what data might subsequently be available. In the long term, it is desirable that the subsequent research publications be cross-referenced in the appropriate catalog entry, though this may require resources that are not yet identified. The Catalog will be a resource for investigators planning new observations (it should, for example, help avoid duplications), and for those who want to know what IR data may exist to complement their work done at other wavelengths or to shed light on their models. For data that remains long unpublished, it could stimulate collaborations with those who really need the final data product. II. Archive of Full Data Backups: The second level of archiving is a complete data archive, which goes beyond the data summaries by adding the actual quasi-raw data files, and a larger range of observatory and environmental data. Such an archive would be formed simply by independently recording all the data taken by the PI team onto a modern storage medium, and storing it in an organized fashion at the SSMOC data center. A no-frills data archive is relatively inexpensive, once the modest cost of the software to do the autonomous recording is amortized. This archive serves three purposes: - First, as a security backup for the PI team, who will record the same data independently on their own disks or tapes; - Second, as a means of providing community access to profoundly important results which warrant confirmation or deeper analysis, regardless of the inconvenience of accessing a database which is not necessarily supported on a user-friendly basis; and - Third, as a resource which can ultimately be made available for broad community access, if funding is made available for the necessary support personnel. This is the third level of archiving, and the Observatory will be seeking ways to eventually fund it. It is clear that NASA values data archives, so this may be more than a remote possibility. All data will be stored using a common format, such as FITS (see discussion under item 4.11.5). The data will be archived after as much processing as is reasonable to apply (i.e., all steps prior to those which may require investigator judgment or intervention). The facility archive will also store all potentially useful data describing observatory variables ("housekeeping" data) on a continuous basis. This data includes: 1) environmental variables such as cavity temperature, water vapor meter reading, and a cloud monitor index, 2) aircraft phase space coordinates such as altitude, heading, airspeed, geographical location, and UT and LST time, 3) telescope parameters such as rotation angle, elevation, azimuth, pointing offsets [nominal and additional], and information on the chopper, the rotator, and the guider. Another category of facility data is data relating specifically to the instrumental setup. The instrument teams will be responsible for supplying the instrument settings to the system, including all the observer-chosen parameters needed to be able to repeat an observation, the integration times, and the ID's of the observing procedures used. A subset of the facility and instrumental data will be written into the headers of the data files (the choices of which variables to be determined by the SSSC). Then, at the same time that the data files are written onto the investigator's disk or tape, they would also be funneled to the facility archive computer. All of the observatory data (housekeeping, environmental, instrumental, telescope and aircraft variables) will separately be stored as auxiliary files, and they will be recorded in the archive with a frequency to be determined, but possibly less often than the data files are stored. The observers would presumably also want to record these files. The archive channel will thereafter be separate and independent of the current investigators' channel. The format of observatory housekeeping data, and mechanisms for accessing that data, will be specified at least a year before operations begin. The electronic log files of the observers and mission director will be recorded in the archive at the end of each flight for subsequent use in both the data summaries and the long-term data archive. Because of the raw nature of data in the archive, it will be desirable to subject it to a validation period (on the order of a year, but TBD) before releasing it to anyone except the observing PI, whether the archive is openly supported for archival research or not. Here, "validation period" simply means allowing enough time to pass to allow discovery of problems with the instrument, the telescope or the MCCS that might not have been recognized during the observations. Finally, given that the data reduction software for Facility Instruments will be accessible, user-friendly, and facility supported, it may not be too much to expect that well-documented data in the archive, taken with instruments which employ the standardized interface software, can be widely accessed and profitably utilized by the community with minimal support from SSMOC personnel. III A User-friendly Archive: The third level data archive is one which is well-maintained and readily accessible, so that it can routinely be used for archival research (e.g., that of the STScI for the HST or of IPAC for IRAS and ISO). It differs from the second level archive by having staff support to provide software interfaces, to extract the unprocessed data from the tape library, and to advise and assist users in its reduction. Such an archive would require a substantial increment in funding for the SSMOC because it involves adding new personnel. However, as long as the second-level data archive is in place, the transition to a third-level archive can be made at any time if the requisite funds can be identified. Furthermore, for facility instruments, the software for reducing archival data will already be in place inasmuch as the SSMOC staff will be providing and maintaining widely accessible software packages for dealing with FI data (see Section 4.10.5), and these packages will be well documented. This capability extends to other instruments as well if they employ the standard data formats defined by the observatory for the FI instruments. For example, standards and software will probably be in place for both imaging and spectroscopic instruments. If the initial concept of a third-level data archive is simply to allow application of existing standard software to an existing database, then the only real needs are for a procedure by which investigators can gain access and a data librarian to facilitate that access. The design of the third-level archive would also facilitate remote access via a web interface. Finally, for any level of archiving, strong consideration should be given to the inclusion of two other media: continuous audio tapes of the essential communications on board, and continuous video tapes of the output from the focal plane camera. The incremental expense of creating these tapes and storing them in the archive alongside the data is small, and yet the information contained thereon can be important for archival researchers seeking to understand the sequence of events and motivations leading up to any particular observations. 4.11.7 Validating the Scientific Measurement of Facility Instruments The validation of the scientific measurements of facility instruments will be accomplished by: - Developing a calibration database from previous and concurrent missions (e.g. SIRTF) - Preparing a set of requirements on the instrument calibration - Obtaining accurate cross-calibration results - Monitoring the instrument performance with trend analysis 4.11.8 SOFIA Science Web-Site for Science, Education and Public Outreach A good observatory WEB-site contains a whole picture of an observatory; a view of its operations, sensitivity, success and future. It attracts users and informs them. It shows how well the Observatory plan is working. The following functions of the WEB have been discussed already above. This list of WEB responsibilities brings together and summarizes the important role of the SOFIA WEB, as a Coordinator. The SOFIA WWW pages will have a diverse audience which will be reached by two objectives: Science Support, and Education and Public Outreach. Development of these WWW pages will be an ongoing task as much of the information contained in them is dynamic and expanding. As the observatory reaches each development milestone on its way toward operational status, the need to inform and prepare the science and education communities increases. The WWW pages will provide SOFIA with an immediate and wide reaching medium for fulfilling this need. Science Support activities will include: - Keeping the science community abreast of SOFIA progress - Schedule - Instruments - Telescope - Aircraft modifications - Publicizing expected observatory capabilities including facility instruments publishing science meeting agendas and minutes developing and maintaining observatory electronic library - SOFIA technical reports - SOFIA PI handbook - Announcing call for proposals; both instrument and observation time - Maintaining science mailing/subscription list - Providing a forum for questions and answers among astronomers - Documenting procedures - Working relationships between PI's and GI's - Application process for observations (yearly call for proposals) Education and Public Outreach activities will include: - Publishing education and public outreach plan - Printing/posting press releases and photos - Publishing meeting agendas and minutes - Providing educational lessons and teacher training - Interactive software - Handouts - Maintaining educator mailing/subscription list - Answering frequently asked questions Maintenance of SOFIA WWW pages consists of the day to day tasks required of every WWW site. These activities will include: - Ensuring all information is correct and current - Monitoring logs Maintaining and updating web server hardware and software Answering questions and comments addressed to web curator 4.12 Education and Public Outreach Program The Education and Public Outreach program is described more fully in PM09, Education and Public Outreach Plan. As a science-rich and technologically intensive observatory, SOFIA offers unique opportunities to enhance scientific literacy both for the general public and for pre-college, undergraduate, and graduate education. SOFIAs Education and Public Outreach (E/PO) program will bring the excitement, hardships, challenges, discoveries, teamwork and educational value of SOFIA to American students, teachers and the public on a national scale. E/PO includes programs and activities, which engage the scientific research and contractor communities, employ state-of-the-art educational technologies, partner with the larger formal and informal educational community, and serve the general public through the media. The E/PO program goals will be met through activities, which support: - Representatives of the media: print, electronic, and broadcast journalists, and science writers; - K-14 students and teachers; - Informal educators through planetaria, science and technology museums; - Faculty and students in schools of education; - Professional societies in science and education; - Groups that are historically underrepresented in the space science program. SOFIA will promote excellence in science, mathematics and technology education through direct involvement of non-scientists in partnerships, workshops, internships, and as participants/observers on research flights. In addition, people will be able to participate remotely in SOFIA operations and flights through the telecommunications media. Finally, the SOFIA E/PO team will provide up-to-date information on the scientific accomplishments of SOFIA to the public through the media. The E/PO team will develop formal and complimentary educational programs which combine in-class/on-the-ground and in-flight activities. All programs will have nationwide participation with special emphasis on serving groups historically underrepresented in space sciences. The E/PO team will work closely with Office of Space Sciences (OSS) to develop appropriate relationships with NASAs Education Division, Minority University Research and Education Division, Educational Program Offices at NASA Centers, Regional Teacher Resource Centers, and the Space Grant Consortium. Existing partnerships will be extended with civic organizations such as Rotary International which supported FOSTER teacher participants on the Kuiper Airborne Observatory (KAO). SOFIA E/PO will work closely with science, mathematics and technology education organizations to recruit teacher participants, present at meetings, and effectively communicate with the education community. Support from businesses, industries, corporations and civic organizations will be sought to leverage E/PO funds. SOFIA will be an accessible, mobile and highly visible research facility wherever it flies in the USA and abroad. It will be a flagship for NASA, DLR and the USRA team. On board, there will be sufficient space to host up to 10 visitors from the educational communities, print and broadcast media, science writers, government, and public to observe science in action during research missions. Public outreach activities will include SOFIA as a fly-in classroom at NASA Ames Research Center (ARC) and on deployment. SOFIA is a unique facility and can be the focus of educational television programs with the prospect of wide public and school dissemination. Public Outreach staff will work closely with the USRA team and others to support timely communication of SOFIA discoveries and accomplishments. The E/PO program will be developed to reflect the national goals and standards for science, mathematics and technology education described in the leading national policy documents and appropriate local and regional frameworks for education. In order to measure the impact and significance of the E/PO activities, formative (during the process) and summative (long-term or ending) evaluation will be conducted by external, professional evaluators. Program evaluation and the advice of the SOFIA Education and Public Outreach Working Group will be important criteria for the renewal of programs, initiation of new programs, and other changes to improve services, minimize cost and maximize the impact of NASAs investment in education and public outreach. Through these activities, SOFIAs Education and Public Outreach program will meet the goals and objectives of OSSs Partners in Education: A Strategy for Integrating Education and Public Outreach into NASAs Space Science Programs and NASAs Strategic Plan. 4.13 SSMOC Configuration Management Configuration Management (CM) is a management discipline that applies technical and administrative direction to the development, production, and support life cycle of a configuration item. This discipline is applicable to hardware, software, processed materials, services, and related technical documentation. CM is an integral part of life-cycle management. The main objective of CM is to document and provide full visibility of the products required design configuration and on the status of achievement of the products physical and functional requirements as-built. A second objective is that everyone working on the project at any time in its life cycle uses correct and accurate documentation. The Office of the Observatory Director will set policy and provide the overall management and administrative capabilities for Configuration Management during SOFIA operations. This office will also be the interface with NASA and DLR concerning CM matters. The Configuration Management Plan (CMP), being developed by the USRA Team, will provide direct communication of configuration management policy and directives to all SSMOC personnel. The CMP also thereby ensures the timely identification, evaluation, and resolution of CM issues as they arise and provides a description of responsibilities and interfaces. USRA has charged all SOFIA team members, and their sub-contractors, with the responsibility to prepare, coordinate, deliver and to make changes to all engineering data per the guidance set forth in the CMP. This means that, during operations, each subcontractor in the SSMOC will control all configurations under their direct responsibility in the SSMOC (e.g., UAL will be responsible for the configuration of the Aircraft System), and will support USRA in the Office of the Director with the integration of the Configuration Management Process. Figure 4.13-1 illustrates the primary and supporting roles of the USRA Team for SOFIA configuration management during the operation phase.  4.13.1 Configuration Management Process: The CM process comprises the following integrated activities; configuration identification, configuration control, configuration status accounting, and configuration auditing. The configuration Identification includes the following: (A) Product Structure and Selection of Configuration Items- The product structure should describe the relationship and the position of configuration items in the breakdown of the product. Configuration items should be selected by applying a decomposition (i.e. breakdown) process to the product using guidance criteria for the selection of configuration items. (B) Documentation of Configuration Items- All the necessary functional and physical characteristics of a configuration item including interfaces, changes, deviations, and waivers should be contained in clearly identified documents. These are normally categorized as configuration documents. (C) Numbering- Numbering conventions should be established and applied to the identification of configuration items, their parts and assemblies, documents, interfaces, changes, deviations, and waivers. (D) Establishment of Configuration Baselines- Configuration baselines are established at Functional Configuration Audits and Physical Configuraiton Audits during CLIN 1. Configuration baselines plus approved controlled changes to those baselines constitute the current approved configuration. Configuration Control involves the following activities, which shall be documented in detail, in a change control procedures: (A) Documenting and justify the change(s) (B) Evaluating consequences of the change(s) (C) Approving or disapproving the change(s) (D) Implementing and verify the change(s) (E) Processing deviations and waivers Configuration Status Accounting shall commence as and when configuration data are first generated. CSA should provide information about configuration identifications and identify all departures from the specified configuration baselines. It thus enables changes to configuration baselines to be traceable. CSA records and reports should be a by-product of the identification and control activities. Configuration Audits shall be performed to assure the product is accurately reflected by its configuration documents. 5.0 Definitions, Abbreviations, Acronyms The definitions, abbreviations, and acronyms used in this document are referenced in the SOFIA lexicon, PD-2009 or listed below. AFSRBAirworthiness and Flight Safety Review BoardSEMASafety, Environmental and Mission AssuranceTBCTo be confirmed  Only true for Scenario 1 under the Weight and Balance Section below. 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!! !cec! !101έコ޽ﭪceccecޜΜέコνέΌsusﭪތsus101sussussusέΜsussusRURRURνένsusBEBννέsusRURέsusBEBRURέsussussuscecceccecsuscecsusRURsus101101101sus101101101susBEBsussussussusBEBέέ޽RURcecceccecRURRURΜceccecsuscecsuscecsussusΌsussussussusBEBcec! !RURBEBRURsussusRURRURBEBcecsuscecsussussusBEBsusRURBEBsus101101susBEB101BEBRUR101sussuscecRURRURRURBEBBEBRURBEBRUR101cecceccecRUR! !RURRURRURRURRURRURRURBEBRURBEBcecBEBBEBRURRURBEBRURcecsussussussussus101cecsussuscecceccecceccecceccecsuscecsuscecceccecsussussussuscecsuscecceccecsussuscecceccecceccecBEBcecceccecsuscecceccecsusceccecceccecceccecsuscecRURcecceccecsussusceccecceccecsussusRURޜﭪν޽susRURsusﭪޭΌννコcecνcecsussuscecﭪsusRURﭪ޽ΌΌﭪޭތﭪΌΜコޭRUR! !νsusΜތέRURsussusΌﭪތνΜ޽cecRURRURBEBRURsussusνコBEBΜcecコ޽έsusތRURcecΜsus޽ޭνRUR޽sussusΜsussusޭcecsusΌޭﭪcecsussusΜcecsusνBEBRURBEBsusތsussuscecΜsus޽コsusޭsusέsusΜcecsusΜޭcecsusRURޭﭪsusRURRURsussussusތsusRURBEBsussussusޭcecέsussussusBEBBEBsusRURRURޭsus޽ﭪέ޽ޭޭRURνsussusޭsusέﭪνsusޭcecBEBcecsusRURBEBBEBsuscec޽susέ޽ﭪsusRURRURBEBsusRURcecsus޽έΜcecΌRURcecsusceccecsusBEBsusRUR! !ΜތsuscecsussusΜsuscecsusΌsusތ޽ceccecceccecsussussussussusceccecBEBޭޭﭪsuscecRURRURceccecRURRURcecRURRURceccecsussus޽Μsuscecsussussuscecޜcec! !BEBέ101BEBcecRUR! !sussusRURRURޜsussus101cecBEBRUR101cecνޭ101ޭ101cecﭪcecRUR! !! !BEBޭsus101! !! !! !! !! !! !ﭪBEBBEB101BEBBEB101cecsussuscecﭪﭪΜﭪޭﭪνޜﭪޜތΌΜﭪsus101RURceccecBEBBEB101BEB101RURBEBRUR101RURRURRURBEBνννΌsussuscecsusceccec޽RURcecBEB101RURcecsussusceccecﭪޭޭ޽ޭޭޜﭪޭﭪޭνﭪένコޜޭﭪޭޜέΜ޽έΜcecsusΜޭννέޭﭪコޭޭΜέޜޭέ޽コޜޭέΜޭΜέΜΜΜޜέﭪΜﭪ޽susﭪcecΌޜތsusޜsusޭsus޽ޜsusννέsusޭΌ޽ޜΌﭪsusޭコsussus޽susޭsusRURceccecsusޜsus޽susﭪcecﭪﭪνcecޭﭪﭪcecRURcecޜνcecsusέ޽sussussusRURRURsussusBEB101RURBEBRUR101RURBEBBEBBEB101101BEBsusޭsussussuscecRURRUR101cecコ޽ﭪﭪ޽޽ﭪޭޜޭޭޜﭪ޽ޜﭪޜコννέコ޽ޭﭪޭﭪコέsussussusνΜsus޽sussusέέޭޭﭪコޭέコﭪޭﭪތތތνﭪޜコޜ޽ޜﭪﭪޜsus޽ޜνޭέΜέΜޜνコsussusέceccecceccecceccecBEBsusޜνޭޭέΜΜsussusνΜ޽έΌ޽νsusνsuscecceccecceccecceccecsussussusceccecceccecceccecBEBsusΌﭪsus޽RURsusRURΜcec޽޽cecέΌsusνޭތνޭcecέޭΌνޭΌέޜコޜ޽޽ﭪνέﭪΌνννΜ޽޽ΌޭޭsusΜsusޭέﭪΜތΌコޭΌέތΜތννﭪﭪνΌތνsussusννέRURν޽޽ޭνﭪﭪތRUR101101susRURRURceccecceccecBEBsusRURRURRURRURRURBEBsusޭceccecsussuscecsus! !! !susBEB! !! !! !BEBsusޭsussuscecsuscecsussusννcecﭪޭsusﭪsussusΌsusޭﭪޜﭪ޽ﭪޭޭsusコޭ޽cecέތsusޭsussusﭪέޜތޜcecέέޭޜsussussussusތΜsusνΜcecέޭsusތνέsussusνΜsussusﭪΌsussusތsusέﭪcecέsussusތΜcecέsussusΜcecޭcecsusޭΜBEBcecRURΜsusΜRURΜέsusνsusRURΌsussus޽ﭪޭsusΜέΌΜތޭޜΜﭪΜޭcecsusﭪΌޜΜΜΜΜsussusޜΜΜޭތޭΜΌsusޜﭪΜޜcecﭪΜέΌΜsusBEBcecceccecΜޜcecsusコ޽ΜέcecceccecコΜޭsussusRURνތޭsusέ! !cecceccecsussusތﭪsussusέޜsussussusέΌRURRURޭޭ޽sussussusΜsusBEBコ޽޽susRURﭪΜΌޭέΜﭪRURsussuscecceccecsussussusceccecRURέތRURΌΌޭνﭪޭﭪﭪRURRURsusޭޜ޽ޭνコ޽ﭪνΜRURޜέޜέsusRURBEBBEBBEBcecRURRURRURcecRURsusceccecsussussusތνέsus101RURRUR101101101BEBsusRURRUR101RUR101101RURﭪsusRURΜΌ޽ޭﭪνέsusޭRURsussusνέsussusޭﭪΜޭνޜﭪޜsussusﭪsusޜsussus޽ΜﭪsusΜsusΜsussusﭪΌsusΜsusޭΜνέޜsusν޽susޭﭪﭪννコޭsusέコތsusΜsusﭪコތޜcecsusޭ޽ތޭέΜ޽޽ޭΜέsusﭪέތޜsusﭪνコέsusνsusΜޜνΜﭪέΜνsusΜsuscecコsusέޭΜ޽νﭪﭪΜ޽コΌνޭココΌﭪέ޽޽コΜコޭνν޽ΜޭޭΜޜsussusνコΜޜޭココΜΜν޽޽コΜέޭﭪΜޭΌコΜޜコΜコνココνΜコνコΜένcecsusνތﭪνﭪνένBEBνﭪޭﭪޭコcecέΜRURコﭪνν޽suscecBEBRUR101101BEB101101101101RURsusBEBsus101susRURBEBBEBsus޽susޭ޽RURRURέBEBsussusRUR101BEBRURRURsuscecsusRURRURsusތコΌsusέޜ޽ΜRURέέޜsusνέέﭪΜΌコsussusコννﭪ޽Μ޽޽ﭪތޭννΜέތコﭪΜコޭޭコޭޭޜﭪΜﭪνޜΜコﭪコsusޭsusﭪココޭココBEBέsusコޭsusޭνޭcecsusޭﭪތέコޭﭪޜﭪ޽ﭪsusΜޜνޭΜﭪޜsusޜﭪﭪsusέΜﭪνﭪsusέココ޽ΜsussusココﭪsusέΌsus޽susޭsuscecޭRURsus޽sussusޜsussussusޜνsus޽޽susέcec޽ތΜsusコޜコcecコ޽޽コ޽ޭޭコﭪsusﭪコν޽ﭪνν޽susνέޜRURceccecceccecsussussussusceccecceccecsusコsuscecννコceccecコcecνޜތένννޭޭ޽ν޽ννコέﭪﭪέ޽susνRURcecsuscecsusRURRURRURsusBEBsussuscecsussusBEBRURコ޽ޜ޽޽コsusνsusﭪޭ޽Μޭﭪέコ޽ޭﭪコέ޽ﭪ޽ﭪޭコޜޭﭪތ޽ޭ޽コΜ޽έޜޭ޽ޭޭΌޭޭコsusέν޽ﭪコceccecέέコ޽コέﭪﭪνコ޽޽ޭコννޜ޽޽ޭνBEB޽コννコ޽޽BEBνޭRURޭޜRURcecsusココޜﭪޭތ޽コތコޭ޽νcecν޽RURRUR! 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!BEB޽Μ101BEBsussusBEBcecsusコcecsusBEBsus101! !RURcecތΜ101susRURΌ! !BEBRURέ޽νRURcecΜΜRURceccecceccecceccecceccecRUR! !cecέceccecsuscecsussussusRURsuscec޽susRURRUR! !101101RURBEB101! !RURcecceccecceccecceccecceccecceccecRURRUR101BEBBEBcecRURcecBEBBEBcecΜcecRURcecޭsussuscecRURRURRURcecceccecceccecRURcecRURcecceccecceccecceccecceccecRURcecceccecceccecceccecceccecRURRURcecceccecRUR޽RURcec101コsusBEBcecRUR101101BEBBEB޽RUR޽101έΜsusRURRURRURRURBEBsussusέ101RURΜ޽suscec޽101νコΜRURcecޭέsus101! !101BEBRUR! !Μcecﭪﭪ޽susέ101コ޽ޜέένΌコνޜνތνﭪνޜコﭪ޽νコޭ101ΌRUR! !susΌsusﭪsusceccecココsuscecsusコﭪννsussusνތΌΜޭ101RURceccecRURRURRURcecRURsusRUR101101BEBRURRURRURBEBBEBRURBEBsussusﭪRURsussus! !RURRURsus! !RUR101101cecRURޭ101޽ޭνsusΜRURcecν޽101! !! !RUR101! !! !101susΜRURΜRURcecsussussuscecέ101޽sussussussusνέRURsussusRURsusBEBsusRURcecRURέﭪコޜRURRURέsusRURceccec! !νBEB101BEBBEBcecRURޜRURsussusRURBEBRURBEBΜέΜޭ޽BEBsussusRURBEBsussussusBEBRURRURcecsusBEBRURRURsus! !susRURcecRURBEBRURsuscec101! !! !ޭRURcec޽Ό޽コνBEBBEB101101BEBBEBRURcecceccecBEB101cecRURRURcecRURRURRURRURBEBBEBBEB101101101101RURcecコޭBEBsussussussusRURRUR101101RURsusBEB101cec101cecRUR! !susBEB! !cec! !޽RURsussuscecRURsusΜޭBEBޭޭ޽ޭνν޽έޭޭν޽ޜέsuscec޽sussussusBEBsussusBEB! !sus! !޽RURBEBsussusRURRURέﭪﭪRURsusRURέRUR޽ﭪ޽νέコνコcecsus101޽RURRUR! !RURRURRUR101BEBBEB! !Μsuscecsus޽コ޽ޭνΜ޽έޭsusRUR޽101ތsusνέコޜ޽BEBsus101BEBcecBEBBEBcecBEBBEBRUR101101101RURRURRURRURRURcecRURRURRURceccecRURcecBEBRURΌceccecBEBΌέέތﭪsusνRURέ101ތέޭέsusBEBsus޽101ΌsusコsussusRURcecέsussus101ﭪέ޽sus101101susRURRURsuscec޽101コsussussusceccecsuscecsusRURޭ޽cecﭪsuscecέsus! !BEBBEBsus! !susތcecBEBΜコένsussussus101έ! !101RUR101! !sus101BEBBEBsussus! !BEBRURRUR101ΜRURRURceccecsussusRURBEBBEB101cecsuscecBEBΜsusRUR޽BEBޭRURBEBRURRURޭBEB101ތsusέsussussuscecsussussusBEBsus101BEBRURέέ޽ν޽BEBcecνޭ101ޭコέΌBEBRURBEBsussussus! !cecsus101BEBRURBEBBEBsusBEBέ޽RURέ101101RURceccecRURRUR! !RURRURBEBBEBRURέBEBBEBcecsussusΌνsussusޭ101޽έsussussusνRURcecBEBRUR101! !sus101susRURcecRUR101! !sus! !BEB! !ΜތνコΜBEBνsusέceccecsusRURﭪ101sussusRURcecsusRUR! !RUR! !cecRUR! !BEBcecsussus! !BEBsussusν101コsusﭪsusޭޭν101BEB101RURRURBEBsus101BEBcecBEBceccecsussus101sussusBEBތsusRURBEBsuscecsuscecﭪﭪceccecceccecceccecceccecceccecBEBcecceccecceccecceccecRURRURcecsusceccecRURcecceccecsussusRURsussussussusceccecBEBcecsusBEBsussussusﭪνsussussussussusνcec101BEB101cecBEBBEBceccecsusRURRURsussussuscecsuscecsussuscecBEBνcecsussuscecRURRUR101RURBEBތココ޽޽ν޽コν޽コ޽コ޽ννコνΌΌココcecﭪﭪν޽޽ν޽νέ! !ޭsusތΌsusRURコΜﭪsussusBEBνέޭέέcecsuscecΌ101޽susޭﭪέΌRURBEB101sussusRURコﭪޭsusBEBޭsusRURΌRURsusBEBコ޽susRURBEBBEBcecΜsusέ! !sussus101ޭcec޽RURsusΜRURνsusBEBέcecޭBEBcecBEBcecsusBEBRURcecBEBBEBsusέRUR101BEBޜ޽޽RURތBEBsussusRURcecRURsuscec101BEBsusBEBsusBEBsusνcecΌRURsusRURBEB101ceccecޜsussusRURsusBEBsusνRURRURcecތコceccecޭBEBsusRURcecέBEBRURBEBέޭΜcecޭsussusέBEBcecsuscec101sussusRURsusBEBcec101BEBBEBޭRURέsusνέcecsusRURcecsussussussusΜsusBEBޜޭRURsussussussussussussuscecsussusceccecsussus! !! !101101101101101101RUR101101101101101101101101101BEBcecBEBsussusBEBέRURέsussusRURBEBRURRURsussussusΜ101BEB101RURsussusRURsussusBEBBEBcec! !RURsus! !101susﭪΜ101suscecsussusRURRURcecsussusceccecέsusRURνޭ101RURcecΌνRURΜsusRURsus޽cecΜ101sussussus޽101cecޭ޽sussusޜcecΜBEBsusRUR! !! !! !BEBRURBEB! !sussusRURcecココsusRURﭪcecsusέν! !sussuscecνceccecޜsussussussuscecsusBEBBEBތsusνΌBEBRURBEBBEB101BEB101101101101101101101101101101101101101101RUR101101101RURceccecceccecceccecsussuscecceccecceccecceccecέRURBEBRURΜcecsusRUR޽έRURsussussussusέsuscecsusBEBBEBRURsus101susέcecBEB޽cecsuscecsussusﭪcecBEBceccecsuscecޭsusコsuscecsusBEBRURΜsusޭsussusBEBsussussuscecsusコ޽sussusﭪﭪsussusRURsusRUR101susコ޽ﭪRURsusތﭪcecΜsusceccecBEBsussus101101RURRURRURsusν101ޜsusココsussussuscec101cecsusコBEBsusΌތcecBEBsusRUR! !コsussussusBEBޜsusコsusΜΌcecRURcecsus! !޽susννRURޭコޭsussusRURsus101cecRURsusRUR101sussus! !RURRUR101RURsus޽コsusRURέcecﭪﭪέΌcecέﭪsusBEB! !susRURceccec! !! !RUR! !! !! !cecBEBޜsus! !ﭪޜέRURέsusޭsussuscec޽ޜνsusBEBsusBEBsussussus101101cecRURsusRURsusBEBsussusBEBΌޜRUR޽ޭRURcec101101BEBBEBBEBsuscec! !101sussuscec޽susコBEBﭪBEBRURcecココέΌRUR޽Μ101susRURsussussusޜΌRUR޽޽BEB101cecﭪsusRURRURBEBsussusν޽suscecBEBBEBcec101susΌsusRURRURsusޭsussusRURcec101ceccecΜcecsuscecޜsusBEBsus101cecνΜcec޽ΌRURBEBsussusތcec! !cecΌތތέ޽ΌsuscecRURsuscecsussusޜένsusceccecsusceccecνコν޽ﭪένコcecέ޽޽ﭪ޽޽コνsusBEBRURsusRURcecΌޭBEBcecBEBcec101BEBRURsusRURsusRURBEBsusコένޭ޽ΜΜcecsuscecBEBcecsussusΜތ޽susޜsussusΜsuscecsuscecsusRURcecsussussuscecRURcecRURceccecceccecceccecceccecceccecceccecceccecceccecceccecceccecceccecceccecceccecceccecceccecsuscec101RURsus101RURRURBEBsussusΜsusBEBcec101RURsussusコﭪΌޜέRURcecsus101susΜsusBEBRURcecBEBcecRURRURRURRURRURޭ޽cecコΜ޽Όcecsussus101cec! !! !101! !BEBBEBcecBEB! !BEB! !susBEB޽ΜΌBEBsussus101susέコޜsusνsus޽ΌRURcecsus101susRURRURBEBBEBsussusνsusνΜޭsusRURsus101sussusRURsusRURBEBsusRURsusRURsusέsusコΌޜRURsus101susνsusνsusceccec101susBEBsuscecsusνRURޭΌsuscecBEBsuscec޽ΌRURceccecsussus޽ννsussusΌcecsusBEBsusν޽νsusコΌΌsuscecΜsusΌ޽ΜsuscecRURBEBsus! !! !RUR޽cecBEBBEBνsusコsusﭪތRURcecΜceccecsusޜsusRURﭪޜRURsuscecRURޜ޽susΌcecΜceccec101! !susRUR! !! !BEB! !BEB101cec101! !BEBRURέޜコsus! !RURsus101BEBsusRURceccec޽コέΌcecsusコέsussusΌsusޭsusceccecsusRURsus! !BEBsussusBEBsus޽RURBEB101BEBRURBEBޭsusRURsusBEBBEB! !BEBRURsus101RUR! !! !RURRURBEBcec101ﭪコνRURcec޽νsussussusޜﭪ101ޜ! !RUR101! !BEBsussusRUR101ތsus101! !susceccecέBEBsusRURBEBsusﭪޭޭνRUR! !BEB! !sussusBEBsusRURsuscecsussussussusΜsusޭsusコνRURcecﭪޜޭΜﭪcecsusRURcecsuscecsusceccecsusceccecsuscecsussussussussussussusBEBsussusRURceccecތޭsussusޭceccecsus! !RURRURsus! !Όsus޽ތceccecޜsussusﭪcecsusޭsussussussuscecRURޭތ101コcecsus! !! !RUR! !BEBBEBBEB101BEBRURcecޜRURsusέコsusRURcecޭޭνRURsusﭪ! !suscec޽RUR! !BEBsussussus101ޭceccecBEBsusΜ101101sus! !ތ! !BEBRUR! !RURcecBEBέννRURsuscecﭪcecRURޜsusRURRURsussusνέ޽νcecsussussusΜνsussuscec! !101RURcecsusRURcec޽νcecsusﭪsussusνsuscecޜBEB! !sus޽έsussusέ޽sussusތBEBコsussusޭRURcecBEBsussusέRURΜBEBέRURBEB101cecsusRURsusﭪޭコ޽޽޽ένコ޽ތΜBEBcecν޽ތ޽ﭪコޜsusέcec޽ννν101RURνޭνBEBBEBコ101BEBBEBBEBBEBBEBBEBRURsuscecBEBceccecRURRURΌコνﭪέޭBEB101101! !susﭪﭪ101ceccecRURތsussussussuscecsussussusceccecRURsusコceccecﭪsusコޭ101RUR! !susBEBRURޜsusBEBﭪﭪBEB101susコsusRURsusΌRURcecコsusRUR101޽cecޭ101cecﭪBEBBEBcec޽BEBcec! !BEBsus101ތcec޽ޜBEB101sus101cecsus! !RUR101cecޭBEBBEBsus101susνBEBRURRURsussusޭ101ޜcec޽έRUR101cecsus! !cec! !cecBEBBEBsusޜέ101RURBEBBEBceccecコνコޭRURsus101sus101RUR! !RURcecέΌBEB101susRURcecsuscec101ތέsusBEBBEB101cecsusceccecRUR101BEBRURsuscecコޜcecRUR101cec޽ޭ101RURceccecRURcec101޽νέコ101ޭ޽ﭪ޽ﭪRURBEBBEB޽ν޽sus101BEBRURν޽コRUR101cec޽コ101sussus޽ޭνޭ޽ޭνRURRUR101sus޽susBEBcecsus101susコޜ101sus101cecޭsuscecRURBEB101! !101101101101101101101BEBBEB! !RURνΜޭޭޭBEBRURBEBcec޽޽έέޜέέޭﭪέcecތsus101susޭBEBsussuscecsussuscecsussusΌέތ޽νRURBEBsusコޭޜコceccecέsus޽έޭ޽ﭪﭪcecBEBRURsusﭪcecޜ101cecޜsus޽susBEBceccecsusBEBBEBコν޽RURcecsussussusコRURcecRURBEBcecέBEBsus101BEBsuscecέsusνRURννννέέ޽ޜBEBコBEBコέcecRUR޽޽Μコ޽susΜ޽޽コέsusBEBsusBEBsusBEB101BEBBEBBEBsussus! !RURBEBsusRUR! !BEBBEB! !! !susތﭪνﭪコﭪﭪތνޭcecRURcecBEBތsusRURcecRURRUR޽޽ޭsusέ޽޽ﭪޜ޽Μ101RURRURsussusBEBsussussussussussusޭέコνΜココνBEBsusRURޭ޽޽ννcecRURBEBsuscecsus101RURcecceccecsusBEB! !101έέΌBEBsusコ101コνsuscecコޜΜBEBRURޭ޽޽έﭪコέcecBEBcecRUR! !cecRUR! !ތ޽ココcecBEBcecޭΌsussusBEBBEBRURRURBEBΌޭコέコﭪRURcec101cecﭪ! !101RURBEBsussus޽ޭﭪ޽RURsuscecsus101コsusBEBﭪﭪRUR޽cecコRURBEBRURceccecRURRURsusΜ޽ޭsusέέޭﭪceccecRURcecRURRURsussuscecRURޭޜsusνsuscecsusνޭsusޜ101ceccecRURRURBEBsusBEBsussuscecέέέޜννceccecsuscecsusRUR101޽susコޭcecsusコΜsusޭέコRURRUR! !cecέޭコcecRUR! !susコﭪνﭪޭޜRURRURRURތsuscec޽ν޽コޭν޽コޭέコココﭪコsusRURRURνRURޜBEB! !! !ތRURcecRURRURcecBEBRURsusceccecRURRURRURsusBEBcecΌsusޭコνޭﭪsuscecコRURﭪRURRURcecRURRURsusޭ޽コνέﭪﭪﭪޭsuscecRURBEBcecތsussus޽޽BEBޜsusνsusRURBEBcecsussus! !ﭪΜﭪコRURsuscec޽ޭތ޽コココޭコBEB101BEBRURRURBEBRUR101suscecceccecsus! !suscecceccecsussuscecBEBcecsussussus101BEBcecsussussus101cecﭪRURRURBEBBEBRURsusΜコޭコcecsusRURRURsus! !RURsusΜΌﭪsussus޽sussuscec޽101cecνέﭪコcecΌsussusRURBEBBEBceccecsus! !cecέޭޭsusތsuscecsusޭޭ޽ޜέsusν޽޽νコBEBsussusޜﭪRUR޽޽Όsusﭪsussussus! !BEBRURsusΜsusތ101sus101BEBRURsusνέΜΜ޽susέޜ޽! !susΜέέΜsusΌRURsusBEBcecRURcecsusRURBEBceccecέﭪコέコRURΜcecsusRURsusRURcecRUR! !ΌsusﭪνココRURΜ޽޽νBEBތΜތένBEBΜΜBEBBEBBEBBEB101BEBsusBEBcecBEBBEBcecތsuscecRURsusRURRURsussusތsusνコέޭsusέ޽sus޽コﭪsusコsusޭޜέコsusコsusތνﭪコΜΌﭪコνRURコΜνコsusBEBޜޜコޭΜコsusތ޽cecsusΜsus101susRURcecsussussusコRURコRURBEBsusRURBEBޭRURコsusΜsusコsus޽޽! !ތceccecΌBEBsusΜνsussusRURsus! !ޭν޽έsussusΜέRURコBEBsusBEB101BEBcec! !ﭪcecコΌνcecΜsusRURcecޭRURέsussusޜ! !BEBsuscecsusΜsusRURsusRURsusRURsusRURcecsussusέέޜsusﭪέέsussussusRURRURތBEBsus101BEB! !BEBsussusޜコﭪsusޭsussussusRURsusRURBEB! !cec! !RUR! !BEBΌRUR! !! !RURތΌޭέcecΌRURsusޭsuscecsussusRURﭪ! !έﭪ޽Μコ޽ΌsusޭޜRURν޽޽BEBRURRURΌコBEBένέコ޽ޭ޽νceccecRURﭪΌννsusRURRURsusތRURννcec! !BEBコΌν޽޽コޜޭsusceccecޭﭪޜﭪRURޭcec޽sussusceccecRURsussussussusޜޭﭪﭪޜRURcecﭪcecΌޭތsussusﭪޭBEBޜBEBsusέsusΜﭪΜέRURsusέΜBEB޽! !susνޜcecﭪﭪコ޽! !έΌΜνsusRURRURsuscecތsusޭνތsus! !BEBRURcecコﭪﭪޭ޽޽RURsussusRURRURsussusέsusﭪΜコ޽RURޜΜέsussusRURޭέތcecޭέތBEBsusތcec101RURޜRURBEBsuscecޭsusΜBEBޭﭪ޽susBEBBEBνޜνBEBޜޭココ޽ތcecތcecޭ101101sussusBEBcecBEBBEBBEBsusﭪコRURޜコsuscec! !susBEB101BEBRURsussusޭRURBEBsussusBEBRURRURBEBRUR! !Ό޽susコνRURޜέコ޽ޜνRURsus޽޽޽ΌBEBΌコνޭέコRURcecsuscecޭέココέ޽sussussusތޜﭪέ޽RURsusBEBBEBsusRURsusޭコΜέ޽޽susέRURΜsussussussusココޭsussusコνތsussusBEB! !sussusޭBEBBEBsus޽έޭνcecΜ޽ﭪέコέRURコνBEB! !suscecsussusޭsussussussusRUR޽susRURޭ! !! !BEBceccecsusﭪνތcecコޭ޽޽ޭތsus! !101cec101susνコν޽޽ޭ޽ތ޽޽cec101RURBEBBEBRUR101sussus101susRURsuscec101ޭέRURcecsuscecsussusBEBνコޭ޽RURsusceccecsus101BEBRUR101BEBcecRURBEBcecsus޽コﭪsusνRURBEBRURcecBEB! !101! !suscec޽޽έココcecsus޽νέsussussusΜνcecένsusRURsussusココﭪコRURコﭪޜޭsussusέRURコέޭތsussusコsuscecBEBﭪcecޜν޽ތﭪRURΌތsusޭBEB101! !RURsusﭪRURcecRURRURBEBRURsusRURsus101! !ޭsussuscecsuscecﭪsusΌsussusBEBsussussusνΌsusRURRURsus101ν޽cecceccecsusBEB101! !susތΜﭪνRURsusBEBBEBcecRURsussus޽ΌsusΌRURsusRURsuscecRURコ޽cecsusΌsus! !! !susBEBsussuscecRURBEBRURcecsusέޭsusBEBBEB! !101cecsuscecέΜcecﭪcecﭪ޽νsusޭﭪBEBsus޽ν޽sussussussuscecέΜν޽޽RURΜΌޜコޭﭪޭνޭコﭪޭ޽コέ޽νޭޭ޽޽ޭコﭪΌ޽ﭪ޽cec޽sus޽ޜ޽コޜsusέコﭪޜsusνココ޽ޭRURRURcecRURsussusޭޭRURcecsusέޭコ޽ﭪコ޽ޜޭﭪsusコRURsussusνcecsusﭪﭪRURRURRURRURsusﭪsussusέsussusBEBceccecޭココ101ﭪココ޽޽޽ﭪ޽ν޽cecceccecceccecceccecceccecceccecceccecceccecceccecceccecceccecceccecceccecceccecsussusνΜν101101101101101101101101! 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!! !BEBRURsusνRUR101BEB! !RURsusRURέRURsussusέcec101101101RURcecBEBBEBBEBsussuscecsusRURBEBRURﭪcecsusRURBEBBEB! !! !cecsussusRUR101cecRURBEBcecBEBRURΌcecBEBcecceccecBEBBEBBEBBEBBEB101BEBBEBRURsus޽νένﭪsusRURsusޭBEB101101101101BEBRURBEBcec101BEB101101101RURcecRURΜsussusコ޽νsussussus޽コޭﭪﭪsusRURsussus޽suscecޭBEBRURcec޽ތΌコ޽޽ތsusޭsussus޽Μތν޽ﭪsusތޜsusﭪ޽コBEBcecޭΜsusέޭ޽コ޽コcec޽コޜコcec޽コRURRURﭪ޽Όޭsussus޽޽ޭΜޭsussusνcecΜΜsusﭪΜνsusޜޭ޽コތތΌcecsussusένコ޽ޭsusνココνޭέ޽έތ޽ޭνޭތsuscecBEBBEBތ޽έsussusޭ޽コέ޽ޭޭνΌέ޽έ޽νsusΌޜRURceccecΜBEB޽޽! !! !RURޜsussusΜコBEBRURcecνsusΜRURコޭRURsusceccecsussusBEBBEBBEBRUR101BEBΜcecコ޽sussusBEBBEBコcecコέBEBνコތココέﭪΜތޜsussussusΌRURsus޽sus޽νέRUR޽sussussusceccecRURνBEB޽ޭRURceccecνコޭέsus޽! !BEBΌsusέcecsussuscecsusέΌsusBEBޜsus޽suscecsuscecνέޭ޽ޭBEB޽susέޭsus޽ޜsussuscecBEBRURsusRURsusRURceccecceccecsussussusceccecޜޭsusΌcecRURcecsussusνsusޭsusΜsuscecsussusﭪΌsuscecコΜޜcecﭪRUR! !BEB! !RURcecsussus! !! !! !ΜތcecsusBEB޽޽ココcecRURRURsusceccecceccecceccecceccecceccecsuscecRURceccecBEBBEBν޽έޭRURsussussusRURsuscec! !! !101101! !! !101BEB101BEBcecRURcecޭ! !RURsusBEBsussussusBEBsusRUR! !BEBBEB101! !! !susRURcecνέcecތBEBsussussussusﭪνέν޽ένΜޭΜ! !! !νBEBRURsusRURΜνcecRURcec! !ceccec101νsussussus! !RURsus! !suscecRURBEBBEBRURBEBޜsusΜﭪ101コcecνέコﭪsusޜsusRUR! !RURBEBcecRURコsusέ! !! !sussussusRURﭪceccecBEBBEBBEBsuscec! !! !cecsusBEBBEB101! !suscecBEB101101101BEBcecRURcecRURBEBRURsussusνﭪ޽ޜތcec޽ޭcecceccecceccecRURRURcecsussusBEBsuscecﭪBEBތﭪﭪ޽޽Όsussussus! !101! !susBEBsuscecsusޜRURcecsusν! !޽suscecޜέ޽sussusΜ101suscec! !101RURcecsusRURBEBRURceccecΌコRURένތsussusRURsussuscecceccecsusBEBcecsusޭsusコsusޜcecBEBceccecsuscec! !susBEBsussusνRURΌ! !! !! !sus! !susRUR101101! !susνコ޽έΌﭪ޽ΜΌ101RURBEBRURsus101cecRURsusBEBcecsussusRURceccecνsussussussussusﭪ޽ﭪννΌsusRURsussussusRURRURsusRURތ101RURBEBRURέRURޭsusΜﭪνތsussusRUR! !Όsussuscec101cecBEBRURRURBEBRURRURceccecRURRURBEBRURcecsussusRUR! !ΜέέﭪcecνココνޜBEBsusRURsusRURcecΜsus޽έcecBEBBEBRURBEBBEBsuscecsusRURsuscec! !101RURΜsussus޽ޭﭪ! !suscecBEB޽Όέ޽RURsusRURsussussusޜޭsusޭ޽νコ! !cecsussuscec101RURcecRURcecsus101susRURBEBBEBRURceccecRURcecsussusコsusRUR101RURRUR! !sus! !101101101BEBsusBEBsusν! !RURsus! !RURBEBRURcec! !Μ101sussussuscecRURRURsuscecRUR! !101RURΌνsusޜΌcecsusΜ101susRURBEB101101101! !101101101101101! !101101101101101101101101101101sussusRURBEB! !sussusތcecRURsusBEBRURsussusBEBceccecsusRURBEBRURBEBBEBceccecRURBEBRURsusRURRURBEBsussusBEBsussusBEBcec101suscecΜsuscec! !susΜsus޽101BEBΌRURΜέsussusތ! !101susΌcecΜsus޽susRURΌΌsus101suscecޭ! !BEBBEBBEBBEBBEB101BEBBEB101101101! !! !cecsus101BEBcecRURޭsusޭΜ101BEBcecRURέ101RURcecRURΜsusBEBRURsuscecν101コceccecΜcecRUR޽޽RURBEB! !sussuscecBEBsuscec101ceccecBEB101susRURsussussussussuscecsuscecsus101RURsusceccecΌBEBcecνތ! !RURsusceccec101BEBceccec101RURRUR޽sussuscecޭBEBsus! !cecRURcecތΜތsussussusν޽ν޽ν101101BEBBEBsussussusBEBsuscecBEBRUR! !! !cec101susRURΜsuscecsus101޽cec101101susRURΜsussus޽cec101cecRURBEBBEBBEBsuscec101susRUR! !susΜRUR޽susBEBBEBBEBcecsussusBEBRURcec101cecsussus! !BEBsusRURένceccecBEBένﭪέތココ޽ޜsussuscecBEB101101! !RUR101sus! !ν޽νޭsussussussus! !cecsusBEBsuscecsuscecRUR! !sus! !BEBcecceccec޽έsusΜRUR! !RURRURsusޜcecRURνcecsusceccecsusέcecRURRUR! !cec101cecBEB޽޽޽έcecBEB101101BEBcecBEB101! !! !BEBceccecνsusRURBEB! !έ! !RUR! !ΜޭsussussussuscecΌcec101! !sussussussusRURRURBEBcecceccecceccec! !sus! !! !susRURRUR! !RURRURcecsusRURνέBEB101! !sussus! !BEB101101RURcec101޽ceccecޜsussusBEBsussus101cecBEBRURBEBBEBceccecsussuscec101101BEBRUR! !RUR! !RURceccec101RURRURέތcec101コsuscec! !susceccecsus101cec101BEBsusRURޭέRURコcec101susRUR101޽޽޽RURޜﭪΌcecΜέέν޽susν޽101susRURBEBRURsussuscecέΌένBEBcecBEBRURsussussussussussuscecsussussussus޽έRURsuscecsussusBEBBEBcecRURBEBBEBsusBEBޭ޽ένﭪcecコ޽ν޽ޭコ޽コνένޜޭﭪνsusRURΌRURceccecRURsuscecsussusceccecceccecﭪννsusνsusRURsusRURέcecތތ޽޽susBEBΜΌޭcec! !cecﭪBEBcec101έޭcecコ޽޽コRURΜνޜ101έRURcecRURBEBΜ޽Ό101suscecsuscecsusceccecsuscecceccec! !suscecBEBsusBEB! !sus! !έcecsusΌν޽cecέRURBEBέコﭪνΌνsussussusRURsuscec101! !suscecBEBΜRURތsussusBEB! !ceccec޽sus޽cecBEBޜRURBEBcecRURΌRURRURsussuscecޜsusコΌsussussusRURޜコνRURRURceccecsusRURceccec101sus! !RURRURBEBBEBRURRUR101sussusRURsusBEB101BEB101cecBEBRURBEB! !ﭪRURsusRURΜBEBcecBEBRURΌceccec101cec! !ΌsussussussusコsusޜsusコΌΌRURΜRURRURέޭsuscecΌsusޭsusBEBRUR101cecBEB101BEB! !RURRUR޽cecsusBEBcecέcecRURcec101101RUR! !! !cecコsusBEB101BEB! !RUR! !! !RURcecνsuscecBEB! !BEBRUR101RURRURBEBsussusννsus޽έ޽susﭪ޽cecBEBRURcecﭪΜsussusRURRURsussusRURsusέޭsus޽RURcecέﭪsusBEBsusތޭRURﭪﭪﭪコ޽cecRURΜRURRUR101! !BEBsusRUR! !cecRURέsusޭތBEBsusRURsusޭRURBEBBEBsussusﭪsusތsusRURcec101BEB! !RURBEB! !BEBcecsuscecBEBコsusコޭsusΜcecRURcec101ν101RURcecsuscecceccecRURcecceccecceccecceccecRURRURRURcecceccecceccecceccecsussussussusRURceccecsuscecRURRURޭRURBEBsusRURcecέsus! !RURRUR! !sus! !! !101susΌsus! !޽susコ޽ތRURceccecέﭪsussusBEBsus޽޽RURRURΌcecRUR! !RURsusBEBsusνsussussusޭコޜ޽susBEBsusceccecsusννέ޽cecsussus! !コBEBRURνޭ޽RURcecRURsussuscecRURsussussusRURcecBEBceccecέέcecsusRURޜ! !ޜcecコ޽BEBcecRURcecsuscecRURRURcecRUR101RURRURsusBEBRURνcec! !コνコcecBEBcecRURcec޽ﭪνννコνތ101ﭪコ޽コνsuscecRURsusRURcecέcecsusﭪsusRURνέsus޽ﭪsusコsusޭsus޽ޭޭνRURBEBcecRUR101101cecsussussussusޭތcecBEB! !ޜνޭコRURcecsusRURコ޽RUR޽޽susRURコνﭪޭsussuscec! !RURBEBsussusRURBEBRURsusΌRUR101sussusBEBsusΌ! !RURBEBBEBsusޭ޽νsusﭪΜcecΜsusޭޭޭRURBEBcecRURsusceccecBEBsuscecsusέRUR101susRURsuscecsussus101sus! !ﭪRURޜBEBsusRURέέBEBΜcec޽έRURBEBRURέΜsusΌsussusνcecsusBEBRURcec޽ﭪsusΜcecsus! !! !101BEBBEBsus101RURRURRURέΜBEBコcecsuscec101cecRURBEB޽RUR! !susコcec޽Ό! !RURޭ޽RUR101101! !! !! !101101susRUR޽ޭsussusﭪcecsusコcecsussusBEBνsusޜέޭ޽ﭪRURsuscecέRURRURコνRURﭪ޽ތcec޽cecνΌνsusココRURέcecΌコΜsussussusޜ޽ﭪޭ޽νコﭪννBEBsusBEBޜތsussussuscecsuscecsusޜޜsus! !BEB! !BEBBEBRURBEBコBEBBEBBEB101BEBsussusﭪsusRURコcecޜννέޜ޽ޜﭪBEBތRURRURRURcecΜBEB101101! !޽ޜsussusRURsusコsussus101cec! !cec101! !cec! !! !! !! !! !101RURΜRURsusνcecsusﭪBEBsusRURRURcecέέsus! !susRURRURsuscecΜcecBEBέΜ! !νsusBEBceccecένsussusRURBEBceccecsusΌέsus101susﭪRURέceccec! !ޜ޽sussussusޭތBEBΜBEBcecBEBέΌsuscecsussusコRURcecޜsus޽コcecsusceccecceccecRURRURcecRURޭsussus޽RURcecBEBﭪ޽ν޽ޭsusceccec޽sussus! !BEBBEBsuscecRURsuscecޜBEBsusBEBsusceccecRUR101sus޽sus޽ޭsussussuscecRURcecsusRURcecތνΜcecsusνRURcecޭﭪ! !BEBsuscec101BEB! !susνsusέBEBcecsuscecRURsusνޭޭތsussusﭪﭪceccecBEBsussusBEBcec޽RUR! !ceccecsussusޭsus101101έcecBEBcecceccecsusνRURceccecBEBcecޭތcecsussusΜsusBEBcecsusRURRURΜcecތ޽cecsusコΌޭsusRURコ޽ޭRURνRURνsussusΜޜޜRURsusRURBEBsusBEB! !BEBceccecsusコ޽νRURޭcec101νsusBEBΌceccecsusRURBEBコRURRURBEB101sussussuscecRURcecRURsuscecBEBﭪココ! !suscecsusRURBEBRURsusRUR! !! !BEBcec! !BEBcecsusBEB޽RURcecBEBBEBRURココRURcec! !cecsussus޽RURcec101cec޽νsussusBEBsus޽! !RURRURBEBRURRURceccec޽cecRURBEBRURﭪsus! !RUR޽cecRURsusޜ! !101BEBsus101νsusޭﭪޜsuscecޭsuscecέ! !BEBsuscecsusޭRURコsuscecﭪޭRURRURceccecBEBέ! !susΜceccecsussusceccecBEBRURRURBEBRURsus޽susﭪΌ101ޭBEBsusBEBRURsuscecsuscecsusRURコsus޽έ޽޽νΜcecBEBsussusέﭪsusޭޜsusΌRUR! !έBEBRURRURcecRURRURRUR101BEBBEBRURRURRURRURRURRURRURceccecRURBEBRURBEBRURBEBcecRURRURcecsusRURRURsusBEBsussussus! !susRURceccecBEBsussusRURέﭪέΌsusννcecRURcecsusceccecsusceccecsusceccecsusRURceccecBEBRURceccecsusRURέΌRURceccecένέBEBޭsussussussusBEBBEBsussussusBEBsusRURRURsussus޽cecﭪsusRURsusέBEBΌsusコ޽susﭪﭪsussusޜRURތsussusBEBތsuscecsussussussuscecsussussussussusΌέsussusRURsusBEBRURΜsusޭ޽コceccecsusﭪνν޽޽susޭνΜν޽έコ޽ﭪﭪ޽ތsus! !susコ޽sussussusRURBEBBEBRURBEBBEBRURsus101BEBBEBBEBBEBcecޭνޭコsussussussusތsusΌsusBEBޜ޽susﭪsusコsusﭪέννννΜcec! !Μﭪsus! !BEBcecRUR! !! !ﭪޭcecﭪޭcecsusΜsussussus޽ތ޽cecsusRUR! !BEB! !RURޭRURcecޭcecsussuscec޽ceccecRURޜ! !RURsuscecBEBcecRUR101RURcecޭcecsuscecsusBEB101RURsuscec޽sussussusޭsusޭޭcecsusRURsus101RURcecsus! !101sus! !RURތsussusﭪޭޜνsusBEBΌνRURBEBBEB101BEBcecRURcecRURceccec101RURBEB101BEBRURBEBBEBcecﭪέﭪsusRUR101101101101101! !101101101101101! !101101101101101101101BEB101101101101101101RURcecέcecRURޭΜcecBEBsusΌcecsusRURsus޽ceccecRURRURcecsusコޭﭪsusコceccecRURﭪsussusコΜΌﭪέޭν޽޽޽ޭޭΜsusνcecsus! !RURcec! !! !sus! !BEB101cecΜ޽Μsusޭތsussus޽ﭪνΜέsusﭪsussussuscecﭪ޽ޜέコޭsusνsusコޜsusRUR! !RURcecRURBEB޽έέέsusΌ! !BEB޽޽޽ﭪ101ν޽ޭ101RURsus101ﭪέޜBEBﭪﭪΜコޭsus101susΜέέsussuscecޭﭪΌέﭪޜ101ޜcecRURsus! !BEB101Μコ޽ޭBEBsusνέ! !ﭪ޽コﭪ101sus101susRURsusΜﭪތތココέޭ޽ﭪޭsusν101sussussus101susRUR101101νέコΌsusRURsuscecsussusﭪRURcecsussusコέ޽コ101sus޽Όsussussus101έBEBsuscecコޭޜRURsussus101ޭcecRURRUR޽έsus101コBEBBEBsuscecコޭRURRURޭ101コޭceccecsussussusコcecޭコﭪތޜﭪﭪ101ޜsusΌΌތココ101susΌﭪcecBEB101Μcecコ޽コέ޽޽RUR101! !101! !! !! !! !! !! !101101101101101! !! !! !! !! !susBEBcecޭﭪsussus! !101cecΜコココ101cecޭコsus޽コcecRURceccecsusBEB! !RURRURތcec101cecsusコޭﭪތcecsus101sus޽ceccecέ101BEBRUR! !sussusνBEBRURコ! !ޭν101コsusޭ޽cecRURΌ޽ޜRURޭココ! !101susBEBsuscecΌsusBEBBEBBEB! !susBEBέRURsus! !RURsuscecRURコΜコﭪRURΌ! !susތcec޽Μコέ޽ޜsussusΜコ! !susceccecsus101sussus! !RURsussusRURέޭﭪコﭪΌﭪΜRURsusBEBsussusRURsussusRURﭪ101BEBRURBEBsus101! !RURBEBcecsus! !コﭪ޽ΜΜ޽޽ﭪBEBRURsus! !! !susﭪޭέ޽susΜνένcecޜsussussuscecsusBEBsussusコcecνﭪsusコsus޽έRURsusコΌcecRURココ! !RURRURcecsussussuscecsussusRURcecޜBEBRURcecRURcec! !101101101! !101! !コέﭪﭪﭪココﭪcecﭪRURތέΜsussuscecRUR101cecsussussussussussussussus101BEBέBEBRURcecコ޽ﭪ޽Μޭsusέコތceccecsusceccecsus101ﭪsusޭޭコsusコcecΜέceccecsus101ޜRURsusέ޽101έRURsusコޭ101101101! !! !101101101! !! !BEBcecceccecceccecRURcecRURcecRURceccecRURsus޽susνRUR޽ޭBEBcec޽ﭪsus! !101! !101! !RURBEBsussusコcecsusRURRURBEBcecsusRURޜޜコsus101sus޽ﭪcec! !! !cecコ101BEBﭪﭪﭪ101cec101! !suscecޜRURcecBEB޽! !cecBEB101޽ﭪ101cecνcecsussusRURRURRURRURέ101νsusRURcecތޭcec! !RUR101101101101! !޽BEBέΜέ101sussussuscecRURcecRURνcecBEB101ΌsusνBEBコޭ101! !ޭcecsusΜcecތΌsusν101! !susBEBޭsusBEBRURsuscecRUR101ޭRURΜcecﭪコέsusceccecRUR101RURRURsussussuscecsusRURsusRURsuscec޽cec! !RURBEBޭﭪ101޽ތ101101! !susﭪBEBsus޽cecRURΜ! !޽νコsusBEB޽101sussussus޽susޭcec101Μ! !susޭΜޜﭪcec101RURRURcecsusﭪRURcecν101cecsuscecޜﭪcecBEBcecceccecBEBBEBBEBcecRURsussuscec101101RURsussussusﭪsusBEBsusRUR101101BEBsusޭޭRURBEB101RURcecΜsusBEBsusﭪޭコννޭޭsus101BEBRURコsusﭪsus101suscecsusν޽޽RURέޭsus101sussussusRURRURcecޭsusﭪRUR101BEBsusBEBsusޜsusコﭪΌceccec101ΌsusΜsusέcec101RURsusRURsussusތコRURޜsusRURνcecΌsusﭪޭcecsusRURRURRURνsuscecsusޜsuscecνcecέsusBEBsus! !! !cecsusceccecsuscecsussusﭪ޽޽ޭコν޽޽コΜޜcec! !sus101RURsusRUR! !sussusBEB! !RURRUR! !101101BEBRURΜコsus101sussusޭsuscecsussussussussussussusތコsusBEBνޭޭνRURcecsussussusﭪsus101RUR101BEBRUR! !cecsuscec! !! !RURcecsusコν޽ﭪﭪsusﭪ޽޽sussusޭコﭪsusﭪέcecコޭsusޭνﭪ޽ﭪΌ޽susνsusνތޜcecsussus޽νΌBEBBEBsussussussusRURsusBEBcecRURތRURBEBﭪένsusΌνcec޽cecνޭޜέsusέΌ! !RURsussusコBEB޽susﭪsusέέ! 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