<=== observer ===> "CLEINERT",\ "Leinert, Ch.",\ "",\ "Max-Planck-Institut f\"ur Astronomie",\ "K\"onigstuhl 17",\ "",\ "D-69117",\ "Heidelberg",\ "Germany",\ "49 6221 528264",\ "49 6221 528246",\ "leinert@mpia-hd.mpg.de" <=== proposal ===> "GLOBAL3B",1,1,\ {"interplanetary medium"},\ {"Salama,A.", "Gr\"un,E.", "Staude,J.", "Lemke,D.",\ "Abraham,P."} <=== title ===> Global mapping, seasonal variation and search for arcminute structure of zodiacal light, Section 3B <=== abstract ===> SCIENTIFIC ABSTRACT The purpose of this proposal is twofold. First, to provide a global picture of the zodiacal light as seen by ISOPHOT. This skeleton allows us to make consistent use of the large amount of serendipity background measurements to be expected; it allows us to adopt the results obtained with the infrared satellite COBE for use or comparison with ISO; it helps to determine reliable backgrounds, which is important in particular for studies of galactic and extragalactic background, but also for the study of faint objects. Second, it allows us to study aspects of the spatial distribution of interplanetary dust which have not been treated sufficiently so far: the search for arcminute structure in the zodiacal light, the out-of-ecliptic distribution, the variation of absorption cross section per unit volume with heliocentric distance, and the location of the plane of symmetry as a function of heliocentric distance, where distance is measured by the temperature of the dust. For these measurements the ability of ISO to avoid stars and bright infrared cirrus and therefore to measure "pure" zodiacal light, is an important advantage. This proposal is part of the ISOPHOT effort to measure diffuse sky brightness. It is coordinated in some detail with the ISOPHOT proposals "Measurement of the extragalactic background radiation", "Properties of interplanetary dust" and "Diffuse infrared emission of the galaxy". PERFORMANCE TIME OVERVIEW Observations priority 1 priority 2 priority 3 sum ---------------------------------------------------------------------------- global mapping - 13590 s 9060 s 22650 s (6.3 h) seasonal variation 21066 s - - 21066 s (5.9 h) arcminute structure 4614 s 4614 s 4614 s 13842 s (3.9 h) --------------------------------------------------------------------------- total 25680 s 18204 s 13674 s 57558 s (7.1 h) (5.1 h) (3.8 h) (16.0 h) 45 % 32% 24% OBSERVATION SUMMARY The distribution and absolute brightness of zodiacal light is studied by means of multiband photometry. There are three parts to this proposal: 1. To determine the global distribution of zodiacal light 2. To measure the seasonal variations of the zodiacal light 3. To search for arcminute structure in the zodiacal light The first two parts will be performed in sufficient extent to allow an intercomparison with COBE and use of the COBE results for inter- polation. The choice of filters has been coordinated with the proposal on "extragalactic backgound light", to which the zodiacal light constitutes an important foreground. The filter at 180 micron is most sensistive to cirrus emission and is always included to improve the correction for this emission. We aim at relative photometric accuracies of a few percent or better, which is needed to separate extragalactic background light from the much brighter zodiacal light and which is highly wanted for modelling of the interplanetary dust distribution. Object lists and breakdown of observations by AOT's will be given in the three separate parts. The common observing plan for photometry will be given in this summary. For all measurements the largest available aperture (180 arcsec) will be used. For a detailed observing plan, special requirements and a detailed description of the target positions see section scientific justification <=== scientific_justification ===> -------- spring launch --------------- Team top 40% middle 30% remaining 30% total performance time --------------------------------------------------------------------- PHOT 21900 s 15369 s 10839 s 48108 s (13.4 h) SOT 3780 s 2835 s 2835 s 9450 s ( 2.6 h) --------------------------------------------------------------------- Sum 25680 s 18204 s 13674 s 57488 s (7.1 h) (5.1 h) (3.8 h) (16.0 h) 45 % 32 % 24 % -------- autumn launch ------------- Team top 40% middle 30% remaining 30% total performance time --------------------------------------------------------------------- PHOT 21900 s 15369 s 10839 s 48108 s (13.4 h) SOT 3780 s 2835 s 2835 s 9450 s ( 2.6 h) --------------------------------------------------------------------- Sum 25680 s 18204 s 13674 s 57488 s (7.1 h) (5.1 h) (3.8 h) (16.0 h) 45 % 32 % 24 % === Detailed observing plan === 1. Wideband photometry Filter t(on object) t(performance) ------------------------------------------------- P_3.6 256 s 562 s P_7.3 32 s 114 s P_11.5 32 s 98 s P_25 32 s 198 s P_60 32 s 200 s C_160 32 s 76 s C_180 32 s 82 s Acquisition 180 s ------------------------------------------------- Performance time 1510 s (0.42 h) 2. Mid-IR photometry Filter t(on object) t(performance) ------------------------------------------------- P_12.8 32 s 106 s P_25 32 s 198 s P_60 32 s 200 s C_180 32 s 82 s Acquisition 180 s ------------------------------------------------- Performance time 766 s (0.21 h) 3. "Slew" photometry filter " slew " performance time ----------------------------------------------------------- P_11.5 start beta = -5.0 2408 s four sparse maps, each about 2.5 deg. end of beta = +5.0 P_25 same 2788 s P_60 same 2796 s ----------------------------------------------------------- total 7992 s (2.22 h) === Special requirements === 1. It is the nature of the objects studied here that they are moving with the annual motion of the sun. This leads to the following consequences: a. FIXED TIME OBSERVATIONS are needed in most cases, because visibility and aspect conditions are only fulfilled around certain dates (defined by a value of lambda(sun), but also depending on launch date). These observations will be clearly indicated in the object lists of the three parts of this proposal. Typically, the time window for execution of these observations is one or a few weeks. FIXED TIME OBSERVATIONS are also required for the "slews" across the ecliptic plane, since it is essential that these measurements be performed in one continuous stream. Also, the "slews" in different colour have to be performed close in time (on the same orbit or within a few orbits). b. COORDINATES in alpha, delta can and will be provided for these moving objects, but only after more is known about lauch date and final visibilities. Therefore they will not be given now but after the required information is available. c. Observations have to be performed at low background positions and at correct angles with respect to the sun. Therefore, even for non-fixed-time-observations strong constraints result, and we give PREFERRED TIME WINDOWS for these observations. 2. In contrast to most other observing programmes, the measurements of this proposal require absolute measurements. This needs both calibration and a knowledge of the dark current of the detectors for the integration times used. We assume, that - as part of the general calibration effort - DARK CURRENT MEASUREMENTS of sufficient quality will be available for the proposed measurements. === Part 2: Seasonal variations of zodiacal light - continuation and end === The seasonal variations are measured both at high and at low ecliptic latitude. At high latitude they mainly result in brightness changes, at low latitudes they mainly result in a shift of the brightness maximum. These are FIXED TIME OBSERVATIONS to be performed at particular heliocentric positions of the earth (including ISO) and with time windows dictated by the visibilities.. They consist of pointed observations to be repeated a few times during the mission, and of raster scans, also in part to be repeated. === Object list === The list is given both for an autumn launch (30.11.95) and a spring launch (31.5.96). HIGH LATITUDE object (autumn) object (spring) Observations,repetitions Priority ---------------------------------------------------------------------------- ECL90,-90 ECL90,+90 mid-IR photometry, 2x 1 ECL50,-45 ECL50,+45 mid-IR photometry, 2x 1 ECL130,-45 ECL130,+45 mid-IR photometry, 2x 1 ECL90,+45 ECL90,-45 mid-IR photometry, 2x 1 ECL90,+90 ECL90,-90 mid-IR photometry, 4x 1 ---------------------------------------------------------------------------- LOW LATITUDE object (autumn) object (spring) Observations Priority ---------------------------------------------------------------- ECLSLEW ECLSLEW "slew photometry" 1 by sparse maps repetition 25 micron only 1 ------------------------------------------------------------------ POSITIONS: ECLSLEW is a strip in a low background region around lambda = 0 deg for one of the observations, around lambda = 150 deg for the other observation, and extending from beta = -5 deg to beta = +5 deg. The observations have to be performed at |lambda - lambda(sun)| approx.= 95 deg. ECL a,b means a position on the sky with|lamba - lambda(sun)| = a, beta = b. The actual measurement has to be performed at a nearby low background position. The actual value of beta is realised by a list of such low background positions. The actual value of |lambda - lambda>(sun)| is realised by the choice of observing period. VISIBILITIES AND REPETITIONS: According to presently available visibilities the following approximate time windows result (to be updated after launch). object(autumn/spring) autumn spring ---------------------------------------------------------------------------- ECL90,-90 / ECL90,+90 45,135 deg. 180,270 deg. lambda(sun) ECL**,-45 / ECL**,+45 160-200 200-260 orbits 240-400 400-440 orbits ECL**,+45 / ECL**,-45 180-240 160-200 orbits 400-420 340-400 orbits ECL90,+90 / ECL90,-90 0,90,180,270 deg. 180,270,0,90 deg. lambda(sun) ------ ECLSLEW 160-180 220-230 orbits ECLSLEW (repetition) 360-400 370-380 orbits ----------------------------------------------------------------------------- PERFORMANCE TIME: Priority 1 21066 s (5.9 h) Priority 2 - - Priority 3 - - -------------------------------------- Sum 21066 s (5.9 h) <=== autumn_launch_targets ===> 1, "PHT17", 1.0, "N", "Q ", 0.00000, 0.00000, 2000, 0.000, 0.000, 326, 2 2, "PHT18", 1.0, "N", "Q ", 0.00000, 0.00000, 2000, 0.000, 0.000, 44, 3 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