<=== observer ===> "RGENZEL",\ "Genzel, R.",\ "",\ "Max-Planck-Institut fuer extraterrestrische Physik",\ "Giessenbachstrasse",\ "1603",\ "85740",\ "Garching b. Muenchen",\ "Germany",\ "49 89 32993614",\ "49 89 32993569",\ "lutz@mpe-garching.mpg.de",\ <=== proposal ===> "MPEXGAL1", 1, 4,\ {"active galactic nuclei",\ "compact galaxies",\ "normal galaxies",\ "quasars",\ "starburst galaxies"},\ {"D. Lutz",\ "A. Eckart",\ "H. Feuchtgruber",\ "A. Moorwood",\ "T. de Graauw",\ "E. Valentijn",\ "J. Koornneef",\ "M. Kessler",\ "A. Sternberg",\ "H. Netzer",\ "D. Hollenbach"} <=== title ===> Infrared Spectroscopy of Bright Galactic Nuclei and the Connection between Star Formation and AGNs. Part 1 of 3 <=== abstract ===> SCIENTIFIC ABSTRACT Exploration of the nature, physical conditions and evolution of the nuclear regions of luminous external galaxies is the main purpose of the SWS CP Proposal: GALACTIC NUCLEI. We propose to carry out multi-line spectroscopy for a detailed study of the circum-nuclear interstellar media and for a better determination of the properties of the central energy source(s). We will first explore the global character of the circum-nuclear gas by observing the brightest infrared lines in a sample of about 60 galaxies of all classes, including normal, starburst and distant luminous IRAS galaxies, as well as Seyferts, Liners and AGN/QSOs. In a next step we will then study physical properties and excitation of the circumnuclear regions of a selected group of galaxies in more detail by observing a wide range of ionic, atomic and molecular infrared lines. Due to the large gain in sensitivity and the full wavelength coverage, such a program will only become possible with the advent of ISO. With the help of theoretical modeling and comparison to nearby, prototypical `template' sources, these measurements will determine the physical processes in and constrain current evolutionary models of galactic nuclei. OBSERVATION SUMMARY We plan to take advantage of the spectroscopic capabilities of ISO over its full wavelength range, using the following AOTs: SWS: Medium resolution spectroscopy with the AOTs SWS01,SWS02,SWS06 LWS: Medium resolution spectroscopy with AOTs LWS01,LWS02 PHT: Low resolution spectra with AOT PHT40 For a small number of `template' sources, we will perform scans over the full ISO wavelength range. For all our program galaxies, we will obtain a survey of some of the brightest or most important lines: Species Lambda [Mg V] 5.608 [Ar III] 8.991 [Ne V] 14.320 (only in IR-luminous galaxies+N5253+N6764+IIZw40+IZw1+Mk463) [S III] 18.713 [O IV] 25.913 [S III] 33.480 [Si II] 34.814 [O III] 51.815 (Or LWS full scan) [O I] 63.184 '' [C II] 157.741 '' PHT-S Spectrum A subset of starburst galaxies will be studied in detail in a large number of lines characterizing various phases of the ISM: Species Lambda Br alpha 4.052 [MgV] 5.608 H2 S(5) 6.910 Pf alpha 7.460 [NeVI] 7.642 [ArIII] 8.991 [SIV] 10.511 H2 S(2) 12.279 [NeII] 12.814 [NeV] 14.320 [NeIII] 15.555 H2 S(1) 17.035 [SIII] 18.713 [ArIII] 21.842 [FeIII] 22.930 [FeI] 24.042 [NeV] 24.300 [SI] 25.249 [OIV] 25.913 [FeII] 25.988 H2 S(0) 28.219 [SIII] 33.480 [SiII] 34.814 [FeII] 35.349 [NeIII] 36.020 H2O 40.337 [O III] 51.815 (From LWS full scan) [N III] 57.317 '' [O I] 63.184 '' [O III] 88.356 '' [N II] 121.898 '' [O I] 145.526 '' [C II] 157.741 '' A search for molecular hydrogen emission (S(0) and S(2)) in galactic disks will be done for a number of mostly edge-on galaxies. The OH 34.6 line will be observed in the megamaser galaxies Arp 220, Mrk 231 and NGC3690A/BC, in coordination with LWS. H3+ emission from X-ray illuminated gas will be searched for in NGC 6240 and NGC 1068. A subset of active galactic nuclei will be observed in the following lines tracing the NLR, CLR, partially ionized and molecular zones: Species Lambda [SiIX] 2.585 [Mg VIII]3.028 [SiIX] 3.935 [MgIV] 4.488 [MgVII] 5.500 [MgV] 5.608 [SiVII] 6.515 S(5) 6.910 [NeVI] 7.642 [MgVII] 9.030 [SIV] 10.511 S(2) 12.279 [NeII] 12.814 [MgV] 13.540 [NeV] 14.320 [NeIII] 15.555 S(1) 17.035 [SIII] 18.713 [FeIII] 22.930 [FeI] 24.042 [NeV] 24.300 [OIV] 25.913 [FeII] 25.988 S(0) 28.219 [FeII] 35.349 [NeIII] 36.020 For the two Liners studied in detail, high excitation lines will be skipped We deviate from the philosophy to use both SWS and LWS by dropping LWS observations for those sources in which the LWS consortium will obtain equivalent data. Concatenation is asked for only in a limited number of cases where the same AOT is used at several positions, e.g. of an interacting system. A number of very long observations with AOT SWS02 have been split. These are deliberately not concatenated to allow efficient scheduling. For details see the scientific justification below. In particular, the `quick overview of observations' indicates, for both positions of the hole, which sources are observed, to which level of detail, and the corresponding priority. The scientific justification contains also a list of requested S/N values for the various projects. In bright sources, these are often exceeded by large factors within the shortest possible integration times for the respective AOTs. For some faint lines in faint sources, the requested S/N cannot be met within the time limit of 1280s pure integration per line we have adopted for most sources. Details on integration time per line for each source by far exceed the size limits imposed for this file. They are available on request. Version March 7, 1994 <=== scientific_justification ===> Time distribution (for both launch windows) Team Total 1st 2nd 3rd priority SWS 435600 174240 130680 130680 AFM 115200 43200 36000 36000 SOT 32400 12960 9720 9720 ------------------------------------- 583200 230400 176400 176400 Our observing program can be separated into 4 sub-sections which differ in scientific goal, number of sources and number of lines. These sub-projects are described in turn in the following paragraphs. Whereas the proposal is structured into these subprojects for clarity, actual observations of individual sources will collect in one go all requirements that may originate from the subprojects, in order to avoid overheads. We aim at detecting most lines at a signal to noise ratio of 10 or better. For the adopted line-to-continuum ratios, this transforms into the minimum continuum S/N ratios listed below. Exceptions where this goal is not achieved are a few faint lines or faint sources where we have limited the integration time per source and per line to no more than 1280 secs. Upper limits e.g. for high excitation lines in ultraluminous IRAS galaxies may nevertheless be important constraints for the possible contribution of AGNs to the energy output of these objects. Similarly, we have limited the time for an LWS01 observation to not more than 0.5 hours including the separate background spectrum. Complete Spectral Scans of Template Sources: In this part of our program we plan to perform complete spectral scans (2.4 - 200 microns) on the prototypical `template' sources described above. The scientific goal here is to obtain unbiased, complete SWS and LWS spectra of sources that can be considered 'pure' or well studied cases and that can be used to refine the physical modelling described above. These spectra also serve to find unexpected, serendipitous spectral features. They will detect lines expected to be bright but not included in our line lists for detailed spectroscopy in order to keep them focussed to a subset best serving our diagnostic aims. This is e.g. the case for several fine-structure lines from star forming regions, planetary nebulae, and the NLR and CLR of active galaxies. The measurements will be carried out with the AOT SWS01, using the mode for full SWS resolution, and the Medium Resolution Spectrum (LWS01) AOT of LWS. Bright Line Survey: In this project we wish to explore the global characteristics of 8 of the brightest far-infrared emission lines in all program galaxies (plus the templates for calibration purposes). We have selected for study the 19 um and 34 um [S III] (SWS) and the 52 um [O III] lines (LWS) as probes of moderate density, photoionized gas, for which a first density estimate may be derived from the ratio of the [S III] lines. The 158 um [C II], 63 um [O I] (LWS) and 34 um [Si II] (SWS) lines have been selected as probes of moderate and high density neutral atomic gas in photodissociation regions and shocks. Measurements of [O IV] 26 um will probe for the presence of high excitation gas. For the ultraluminous IRAS galaxies, the discrimination between starburst and AGN energy sources will be strengthened by an additional search for the [NeV] 14.32um line (EP 97 eV). Due to the ability to simultaneously observe in the two sections of SWS, we will be able to supplement this list at no cost by a survey of another line from photoionized gas, [Ar III] 9.0 um, and a survey for the coronal line [Mg V] 5.6 um, which however will in most cases yield only upper limits. ISOPHOT-S spectra will relate these observations to the properties of dust features, and allow to deduce Lyman contiuum fluxes from Br alpha for some of the brighter sources. Because of the low spectral resolution and resulting low line-to-continuum ratio, only the very brightest lines can be seen in the PHT-S spectra. Summary of observations for the bright line survey: Species Lambda Minimum S/N on continuum [Mg V] 5.608 - [Ar III] 8.991 5 [Ne V] 14.320 50 (only in IR-luminous galaxies+N5253+N6764+IIZW40+IZw1+Mk463) [S III] 18.713 10 [O IV] 25.913 50 [S III] 33.480 20 [Si II] 34.814 20 [O III] 51.815 (LWS full scan, S/N>20 for the most difficult lambda~52um) [O I] 63.184 '' [C II] 157.741 '' PHT-S Spectrum Note: LWS01 fullscan replaced by LWS02 line spectra of 63.184 and 157.741 for sources with S(60um) < 5Jy. >From this data set we expect to be able to derive a first order impression on the global physical conditions and excitation (temperature, density) of the ionized and atomic interstellar media of galaxies of all types and get a census on the range of line luminosities in each type of galaxy. Due to the faintness of F10214+4724 (S_25um = 0.075 Jy) and its high redshift, it is not feasible to obtain comprehensive infrared spectroscopy as for the other sources in our sample. We will study 6 lines in the SWS range, ranging from relatively low excitation ([Ne II], [ArII]) to higher excitation ([ArIII],[OIV],[S IV]) and very high excitation ([NeVI],[SiIX]), in an attempt to classify the exciting radiation field as starburst-like or AGN like. [Ne II] emission with a line-to-continuum ratio as observed for the M82 starburst would be detected with high significance in the proposed integration time, whereas [S IV] emission scaled to the observed H alpha according to our Seyfert model could be detected in the case of AGN excitation. The SWS-AOT used for the Bright Line Survey is SWS02 with R~1000. For active galaxies known to exhibit very broad `narrow' lines (e.g. 19254-7245), we will instead use SWS06 to cover a broader range around the line center. LWS observations are done using the Grating Wavelength Range Spectrum (LWS01) AOT for sources brighter than 5 Jy at 60um. Even for a moderate number of lines, this maximises the scientific output with respect to the instrumental overheads. For the fainter sources, will will only observe the lines [O I] 63.2um and [C II] 157.7um, using AOT LWS02 to scan 5 resolution elements centered on each line. PHT-S spectra (AOT P40) for sources brighter than 4 Jy at 12um will be obtained with an integration time corresponding to a S/N ratio of at least 100-200 at 12um. For fainter sources, integration time will be limited to 512s (on-source), still allowing studies of dust features at reduced S/N. In most cases, we do not plan to take separate background spectra close to our sources, in order to avoid the additional time overhead of a factor of 2. The infrared background far from the galactic plane is typically ~0.2 Jy within a SWS beam and ~2 Jy within a LWS beam. For the SWS observations, the background signal is comparable to the source signal only for the fainter sources. The continuum fluxes of these sources are well known from IRAS observations, and possible line contamination by galactic emission can be separated kinematically. For LWS, background spectra will be taken for all except the template sources. PHT-S observations use a chopping AOT. Detailed Spectroscopy of Star-Forming Galaxies: In this section of our program we hope to determine the character of the radiation field (intensity and effective temperature of the UV field), constrain the range of excitation conditions in the ionized gas and explore the properties of the molecular interstellar medium in detail in a set of normal, star-forming and luminous IRAS galaxies, IR-bright AGN galaxies and the templates. The goal is that for these galaxies ~30 different ionic, atomic and molecular lines are then available that cover a wide range of excitation conditions. We expect that these galaxies will form the basic data set for a detailed comparison of observation and theoretical modeling of the different physical processes discussed throughout our proposal. For this purpose we have selected a larger number of atomic and molecular lines, and require measurements of higher accuracy for some of the survey lines. We will test the hypothesis that all galaxies that are characterized as star bursters on the basis of their far-infrared continuum properties can in fact be explained by photoionization of molecular clouds by a OB-star radiation field. Various lines of [S III], [S IV], [Ne II], [Ne III], [N II], [N III], [O III], [O IV], [Ar III] will sample ionized gas in ionization stages from 14 to 55 eV that can be reasonably expected from gas ionized by normal OB stars. The ratios of the [O III], [Ne III], [S III] and [Ar III] lines will give accurate electron densities. We have selected the 14 and 24 um [Ne V] and 7.6 um [Ne VI] lines to determine the excitation and density of a possible hot coronal medium generated by supernova explosions and investigate existence and physical conditions of hidden AGNs. In total, the lines of four different ionization states of neon will sample the ionizing radiation field over a wide range of energies without interference from abundance or depletion effects. We will also observe 4 um HI 5-4 and 7 um HI 6-5 for determining emission measures (Lyman continuum fluxes) and extinctions in the same beam as used for the fine structure lines. The combination of fine structure lines and recombination lines will also give a measure of abundances. 145 um [O I], 25 um [S I], transitions of [FeI], [FeII] and [FeIII], the H_2 pure rotational transitions S(0), S(1), S(2), S(5) and 40 um H_2O (6_43 - 5_32) are selected to probe dense, warm atomic and molecular material in photodissociation regions and shocks. The mid-IR [FeII] lines, together with well-known near-IR transitions, provide powerful constraints on the properties of partially ionized gas. [Fe III] observations will help to determine the Fe abundance / depletion. The 4.35um and 16.33um transitions in H3+ have been proposed as a unique spectral signature of X-ray excited gas (Draine and Woods 1990). This may however change in the light of re-evaluations of H3+ recombination rates. A limited attempt do detect these lines in N6240 and N1068 is made. Summary of observations for detailed spectroscopy of starforming galaxies: (including bright line survey lines) Species Lambda Minimum S/N on continuum Br alpha 4.052 10. [MgV] 5.608 - H2 S(5) 6.910 333. Pf alpha 7.460 50. [NeVI] 7.642 333. [ArIII] 8.991 50. [SIV] 10.511 50. H2 S(2) 12.279 100. [NeII] 12.814 50. [NeV] 14.320 100. [NeIII] 15.555 100. H2 S(1) 17.035 100. [SIII] 18.713 100. [ArIII] 21.842 333. [FeIII] 22.930 333. [FeI] 24.042 333. [NeV] 24.300 333. [SI] 25.249 333. [OIV] 25.913 333. [FeII] 25.988 333. H2 S(0) 28.219 333. [SIII] 33.480 100. [SiII] 34.814 100. [FeII] 35.349 333. [NeIII] 36.020 333. H2O 40.337 100. [O III] 51.815 (LWS full scan, S/N > 40 for the most difficult lambda~52um) [N III] 57.317 '' [O I] 63.184 '' [O III] 88.356 '' [N II] 121.898 '' [O I] 145.526 '' [C II] 157.741 '' The observations will be performed with AOT SWS02 at a resolution of 1000 and with LWS01 full scans. Time estimates for this section of our program have been derived using the line-to-continuum approach. SWS02 spectra of H3+ 4.35 and 16.33 have been added only for NGC6240 and NGC 1068. The OH 34.6 line will be observed in the megamaser galaxies Arp 220, Mrk 231 and NGC3690A/BC, in coordination with LWS. For NGC 4945, the 0-0 S(7) and 1-0 Q(3) lines of molecular hydrogen have been added, and the required S/N for the molcular hydrogen lines has been increased. For a number of edge-on systems covering a range of far-infrared luminosities, we will obtain off-nuclear SWS02 spectra in the lines of H_2 S(0) 28.219 and H_2 S(2) 12.279 offset by D25/2 from the nucleus. The SW section of SWS will simultaneously be aimed at the H_2 S(7) 5.5112 and H_2 1-0 Q(3) 2.432 lines. Detailed Spectroscopy of AGNs: In this section of our program we have selected bright Seyfert 1s, Seyfert 2s, NLXGs, Liners and two radio-selected AGNs. Detailed spectroscopy will be obtained probing gas in the NLR and CLR ([Ne II], [Ne III], [Ne V], [Ne VI], [S III], [S IV], [O IV], [Mg IV], [Mg V], [Mg VII], [Mg VIII], [SiVII], [Si IX]). The aim is to get a full description of the parameters of the infrared emission in the NLR/CLR, including densities from various line ratios at different levels of excitation. The H_2 S(0),S(1),S(2),S(5) lines, together with the [Si II] line (already observed in the bright line survey) will test the evidence for a warm, dense molecular/atomic zone near the nuclear emission region (Note that models for X-ray-illuminated molecular gas predict high intensities of the higher rotational transitions of H_2). Again, [Fe II] and [Fe III] will prove to be particularly useful in conjunction with NIR data. Including the lines that were already observed in these sources during the survey these AGNs will then be observed in lines that trace the active nucleus as well as lines that are expected to be bright for star formation. This project will thus provide a basic data set for testing models of the NLR/CLR of AGNs, and test whether these prototype AGNs are also currently forming stars. For the AGNs that are also template sources, this data set will be complemented by line detections expected from the full scans. Time estimates for this section have been derived using the approach to scale the expected line emission with the dereddened Hbeta flux, adopting predictions from photoionization models and a certain margin for bright lines. Lines included in the survey (L/C-based) and in this project ([S III], [O IV]) will be observed according to the method predicting the fainter line flux. Again, a limit of not more than 1280s pure integration time per line has been enforced. Summary of observations for detailed spectroscopy of AGNs: Species Lambda I/Ihbeta_limit (to be detected with 10 sigma) Seyferts Liners [SiIX] 2.585 0.02 - [MgVIII] 3.028 0.10 - [SiIX] 3.935 0.05 - [MgIV] 4.488 0.10 - [MgVII] 5.500 0.20 - [MgV] 5.608 0.10 - [SiVII] 6.515 0.05 - S(5) 6.910 0.02 - [NeVI] 7.642 0.02 - [MgVII] 9.030 0.20 - [SIV] 10.511 0.50 - S(2) 12.279 0.02 - [NeII] 12.814 0.02 0.31 [MgV] 13.54 0.02 - [NeV] 14.320 0.19 - [NeIII] 15.555 0.50 1.60 S(1) 17.035 0.02 0.02 [SIII] 18.713 0.35 0.60 [FeIII] 22.93 0.10 - [FeI] 24.042 0.10 - [NeV] 24.300 0.07 - [OIV] 25.913 0.50 0.01 [FeII] 25.988 0.10 - S(0) 28.219 0.02 - [FeII] 35.349 0.10 - [NeIII] 36.020 0.15 0.11 Note: Not all coronal lines will be observed in N1275, CenA Quick overview of observations ============================== Note: This list is a merger of the two lists for different `hole' positions. If a source shows up in several projects, observations with the same AOT are merged to avoid overheads. Priorities are given for autumn/spring launch, i.e. 1/2 means priority 1 for autumn launch and 2 for spring launch Source Full scan Survey Detailed(SB) Detailed(AGN) H2 off-nuc SWS SWS LWS PHT SWS LWS SWS SWS ------------------------------------------------------------------------ Templates: GC SgrA 1/1 2/ 3/ 2/ * GC Ring NE 1/ 2/ 3/ 2/ GC Ring SW 1/ 2/ 3/ 2/ RCW103 1/ 3/ IC443 /1 /3 30 Dor 1/1 2/2 3/3 3/3 2/2 3/3 W 51 1/ 2/ 3/ 2/ * DR 21 /1 /2 /3 /3 /3 /3 M82 1/1 1/1 3/3 1/1 NGC 253 2/2 2/2 3/3 2/2 2/2 NGC 1068 1/1 1/1 3/3 1/1* 1/1 Circinus 1/ 1/ 1/ 3/ 1/ 1/ 1/ NGC 4151 1/1 1/1 3/3 1/1 Normal Galaxies/Dwarfs NGC 891 1/1 3/ 3/3 1/1*3/ 2/2 NGC 4567 3/3 3/3 3/3 NGC 4568 3/3 3/3 3/3 NGC 5194 M51 3/3 3/3 IIZw40 /3* He2-10 /3 /3 /3 NGC 6052 3/ HII Galaxies / Starbursts IC 342 /2 /3 /2 NGC 1808 /1 /1 /3 /1 /1 NGC 3256 /1 1/1 1/1 3/3 1/1 1/1 NGC 3690/IC 694 A 2/2 3/3 2/2* NGC 3690/IC 694 BC 2/2 3/3 2/2* NGC 4945 1/ 3/ 1/ * NGC 5236 M83 3/ 3/ 3/ NGC 1614 /3 /3 /3 NGC 2903 /3 /3 /3 NGC 3079 /2 /2 /3 /2 NGC 4038 3/3 3/3 NGC 4039 3/3 3/3 NGC 4038/39 overl. 3/3 3/3 NGC 5253 3/ *3/ 3/ F15564+6359 3/ 3/ 3/ NGC 6764 3/3 3/3 NGC 6946 3/3 3/3 3/3 NGC 7552 3/3 3/3 3/3 /3 /3 IR luminous / Mergers Mrk 231 1/1 3/3 1/1* Arp 220 1/ 3/ 1/1* NGC 6240 1/ 3/ 1/1* 20551-4250 1/1 2/1 3/3 2/1 2/1 05189-2524 /1 /3 /1 06035-7102 /1 /2 /3 06206-6315 /2 /2 /3 08572+3915 /1 /3 09320+6134 UGC5101 1/1 3/3 F10214+4724 1/1* 12112+0305 1/1 3/3 13428+5608 Mrk273 1/1 3/3 3/3 14348-1447 1/ 3/ 15250+3609 3/ 3/ 17208-0014 1/ 2/ 3/ 19254-7245 1/1 2/2 3/3 20100-4156 3/3 3/3 3/3 22491-1808 1/1 3/3 23128-5919 1/1 2/1 3/3 /2 /1 Seyfert 1s NGC 1365 2/1 2/2 3/3 2/1 NGC 7469 2/2 2/2 3/3 2/2 NGC 3783 3/3 3/3 13224-3809 3/ *3/ 3/ Seyfert 2s Mrk 6 /1 /3 /3 /1 Mrk 1 3/3 3/3 3/3 Mrk 573 /3 /3 NGC 1672 /3 /3 /3 Mrk 3 /3 /3 Mrk 34 3/ 3/ 3/ NGC 5643 3/ 3/ 3/ PKS 2048-57 3/3 3/3 3/3 NLXGs NGC 7582 2/1 1/1 1/1 3/3 1/1 NGC 5506 2/ 3/ 2/ NGC 2992 /2 /2 /3 /3 /2 Liners M 81 2/2 3/3 2/2 NGC 4569 3/3 3/3 3/3 3/3 NGC 4826 3/ 3/ 3/ AGNs/QSOs CenA 1/ 3/ 1/ 1/ * 3C273 2/2* 3/3 IZw1 2/2 3/3 3/3 Mrk 1014 3/3 3/3 3/3 NGC 1275 2/2 2/ 3/3 2/2* 3C120 /3 /3 /3 M87 2/2 3/3 3/3 Mrk 463 3/ 3/ 3/ Mrk 876 1613+658 /3 /3 /3 3C48 2/2*2/2*3/3 Edge-on IC 2389 /2 UGC 5965 /3 UGC 9665 2/ UGC 11859 2/2 ESO12-1050 3/3 ESO480-0090 2/2 ESO157-0490 /3 * means line list modified for this source/instrument with respect to that outlined for the various projects. For individual sources, these modifications are: SgrA* : 3.61HeH+, 3.953H3+, 4.695H2, 9.665H2, 16.331H3+, 39.399H2O added in coordination with Drapatz et al. proposal W51 IRS2: 3.235H2, 45.114H2O added in coordination with Drapatz et al. proposal NGC 1068: 4.35H3+, 16.33H3+ added NGC 891: only 4.052, 5.608, 8.991, 10.511, 12.279, 12.814, 14.320, 18.713, 25.913, 25.988, 28.219, 33.480, 34.814 will be observed II Zw 40: 4.052H, 12.279H2, 25.988[FeII] added NGC3690/IC694: 34.615 OH added NGC 4945: 2.424H2, 5.511H2 added NGC 5253: 4.052H, 12.279H2, 25.988[FeII] added Mrk 231 : 34.615 OH added Arp 220 : 34.615 OH added NGC 6240: 4.35H3+, 16.33H3+ added F10214+4724: See text above 13224-3809: 14.32NeV, 25.988[FeII] added Cen A : no Mg, Si coronals except 3.935 and 5.608 3C273 : Only survey lines + 17.035H2, but deep integration NGC 1275: no Mg, Si coronals except 3.935 and 5.608 3C48 : Modified due to redshift. Observed with SWS: 2.165H, 4.052H, 5.608[MgV], 6.985[ArII], 8.911[ArIII], 18.713[SIII], 25.913[OIV]. Observed with LWS: 33.480[SIII], 34.814[SiII], 63.184[OI] <=== autumn_launch_targets ===> 1,"SWS01",1.,"N", "GC SgrA* ", 17.76112, -29.00794, 2000, 0., 0., 6498,0 2,"SWS02",2.,"N", "GC SgrA* ", 17.76112, -29.00794, 2000, 0., 0., 2694,0 3,"SWS01",1.,"N", "GC Ring NE ", 17.76161, -28.99725, 2000, 0., 0., 6498,0 4,"SWS02",2.,"N", "GC Ring NE ", 17.76161, -28.99725, 2000, 0., 0., 3346,0 5,"SWS01",1.,"N", "GC Ring SW ", 17.76073, -29.01825, 2000, 0., 0., 6498,0 6,"SWS02",2.,"N", "GC Ring SW ", 17.76073, -29.01825, 2000, 0., 0., 3346,0 7,"PHT40",3.,"N", "GC SgrA* ", 17.76112, -29.00794, 2000, 0., 0., 493,8 8,"PHT40",3.,"N", "GC Ring NE ", 17.76161, -28.99725, 2000, 0., 0., 333,9 9,"PHT40",3.,"N", "GC Ring SW ", 17.76073, -29.01825, 2000, 0., 0., 333,0 10,"SWS01",1.,"N", "RCW103 ion ", 16.29214, -51.10136, 2000, 0., 0., 6498,0 11,"PHT40",3.,"N", "RCW103 ion ", 16.29214, -51.10136, 2000, 0., 0., 493,0 12,"SWS01",1.,"N", "30 Dor ", 5.64612, -69.08553, 2000, 0., 0., 6498,0 13,"SWS02",2.,"N", "30 Dor ", 5.64612, -69.08553, 2000, 0., 0., 4402,0 14,"LWS01",2.,"N", "30 Dor ", 5.64612, -69.08553, 2000, 0., 0., 570,0 15,"PHT40",3.,"N", "30 Dor ", 5.64612, -69.08553, 2000, 0., 0., 493,0 16,"SWS01",1.,"N", "W 51 IRS2 ", 19.39443, +14.51835, 2000, 0., 0., 6498,0 17,"SWS02",2.,"N", "W 51 IRS2 ", 19.39443, +14.51835, 2000, 0., 0., 2580,0 18,"PHT40",3.,"N", "W 51 IRS2 ", 19.39443, +14.51835, 2000, 0., 0., 493,0 19,"SWS01",1.,"N", "M82 ", 9.93076, +69.67899, 2000, 0., 0., 6498,0 20,"SWS02",1.,"N", "M82 ", 9.93076, +69.67899, 2000, 0., 0., 2818,0 21,"PHT40",3.,"N", "M82 ", 9.93076, +69.67899, 2000, 0., 0., 493,0 22,"SWS01",2.,"N", "NGC 253 ", 0.79255, -25.28811, 2000, 0., 0., 6498,0 23,"SWS02",2.,"N", "NGC 253 ", 0.79255, -25.28811, 2000, 0., 0., 3258,0 24,"SWS02",2.,"N", "NGC 253 off ", 0.80013, -25.20350, 2000, 0., 0., 2112,0 25,"PHT40",3.,"N", "NGC 253 ", 0.79255, -25.28811, 2000, 0., 0., 493,0 26,"SWS01",1.,"N", "NGC 1068 ", 2.71132, -00.01314, 2000, 0., 0., 6498,0 27,"SWS06",1.,"N", "NGC 1068 ", 2.71132, -00.01314, 2000, 0., 0., 3985,0 28,"SWS06",1.,"N", "NGC 1068 ", 2.71132, -00.01314, 2000, 0., 0., 6667,0 29,"SWS02",1.,"N", "NGC 1068 ", 2.71132, -00.01314, 2000, 0., 0., 2112,0 30,"PHT40",3.,"N", "NGC 1068 ", 2.71132, -00.01314, 2000, 0., 0., 493,0 31,"SWS01",1.,"N", "Circinus ", 14.21936, -65.33930, 2000, 0., 0., 6498,0 32,"SWS02",1.,"N", "Circinus ", 14.21936, -65.33930, 2000, 0., 0., 9180,0 33,"LWS01",1.,"N", "Circinus ", 14.21936, -65.33930, 2000, 0., 0., 570,0 34,"PHT40",3.,"N", "Circinus ", 14.21936, -65.33930, 2000, 0., 0., 493,0 35,"SWS01",1.,"N", "NGC 4151 ", 12.17573, +39.40584, 2000, 0., 0., 6498,0 36,"SWS02",1.,"N", "NGC 4151 ", 12.17573, +39.40584, 2000, 0., 0., 5902,0 37,"SWS02",1.,"N", "NGC 4151 ", 12.17573, +39.40584, 2000, 0., 0., 8340,0 38,"PHT40",3.,"N", "NGC 4151 ", 12.17573, +39.40584, 2000, 0., 0., 1261,0 39,"SWS02",1.,"N", "NGC 891 ", 2.37590, +42.34949, 2000, 0., 0., 7470,0 40,"SWS02",1.,"N", "NGC 891 ", 2.37590, +42.34949, 2000, 0., 0., 6036,0 41,"SWS02",2.,"N", "NGC 891 off ", 2.37652, +42.36697, 2000, 0., 0., 2112,0 42,"SWS02",2.,"N", "NGC 891 off1 ", 2.37706, +42.38028, 2000, 0., 0., 2112,0 43,"SWS02",2.,"N", "NGC 891 off2 ", 2.37759, +42.39581, 2000, 0., 0., 2112,0 44,"LWS01",2.,"N", "NGC 891 ", 2.37590, +42.34949, 2000, 0., 0., 960,0 45,"PHT40",3.,"N", "NGC 891 ", 2.37590, +42.34949, 2000, 0., 0., 1261,0 46,"SWS02",3.,"N", "NGC 4567 ", 12.60908, +11.25803, 2000, 0., 0., 2164,47 47,"SWS02",3.,"N", "NGC 4568 ", 12.60950, +11.24026, 2000, 0., 0., 948,0 48,"LWS01",3.,"N", "NGC 4567 ", 12.60908, +11.25803, 2000, 0., 0., 1740,49 49,"LWS01",3.,"N", "NGC 4568 ", 12.60950, +11.24026, 2000, 0., 0., 1580,0 50,"PHT40",3.,"N", "NGC 4567 ", 12.60908, +11.25803, 2000, 0., 0., 1261,51 51,"PHT40",3.,"N", "NGC 4568 ", 12.60950, +11.24026, 2000, 0., 0., 1101,0 52,"SWS02",3.,"N", "NGC 5194 M 51 ", 13.49797, +47.19515, 2000, 0., 0., 1108,0 53,"PHT40",3.,"N", "NGC 5194 M 51 ", 13.49797, +47.19515, 2000, 0., 0., 1261,0 54,"SWS02",3.,"N", "NGC 6052 ", 16.08692, +20.54215, 2000, 0., 0., 932,0 55,"SWS02",1.,"N", "NGC 3256 ", 10.46423, -43.90374, 2000, 0., 0., 5898,0 56,"LWS01",1.,"N", "NGC 3256 ", 10.46423, -43.90374, 2000, 0., 0., 960,0 57,"PHT40",3.,"N", "NGC 3256 ", 10.46423, -43.90374, 2000, 0., 0., 1261,0 58,"SWS02",2.,"N", "NGC 3690 A ", 11.47601, +58.56293, 2000, 0., 0., 5576,0 59,"SWS02",2.,"N", "NGC 3690 A ", 11.47601, +58.56293, 2000, 0., 0., 4344,0 60,"SWS02",2.,"N", "NGC 3690 B/C ", 11.47524, +58.56266, 2000, 0., 0., 6364,0 61,"PHT40",3.,"N", "NGC 3690 A ", 11.47601, +58.56293, 2000, 0., 0., 1261,62 62,"PHT40",3.,"N", "NGC 3690 B/C ", 11.47524, +58.56266, 2000, 0., 0., 1101,0 63,"SWS02",1.,"N", "NGC 4945 ", 13.09095, -49.46819, 2000, 0., 0., 8186,0 64,"PHT40",3.,"N", "NGC 4945 ", 13.09095, -49.46819, 2000, 0., 0., 1261,0 65,"SWS02",3.,"N", "NGC 5236 M83 ", 13.61682, -29.86535, 2000, 0., 0., 8718,0 66,"SWS02",3.,"N", "NGC 5236 M83 ", 13.61682, -29.86535, 2000, 0., 0., 3904,0 67,"PHT40",3.,"N", "NGC 5236 M83 ", 13.61682, -29.86535, 2000, 0., 0., 1261,0 68,"SWS02",3.,"N", "NGC 4038 ", 12.03142, -18.86809, 2000, 0., 0., 756,69 69,"SWS02",3.,"N", "NGC 4039 ", 12.03148, -18.88614, 2000, 0., 0., 596,70 70,"SWS02",3.,"N", "NGC 4038/39 ov", 12.03192, -18.88448, 2000, 0., 0., 596,0 71,"PHT40",3.,"N", "NGC 4038 ", 12.03142, -18.86809, 2000, 0., 0., 1261,72 72,"PHT40",3.,"N", "NGC 4039 ", 12.03148, -18.88614, 2000, 0., 0., 1101,73 73,"PHT40",3.,"N", "NGC 4038/39 ov", 12.03192, -18.88448, 2000, 0., 0., 1101,0 74,"SWS02",3.,"N", "NGC 5253 ", 13.66548, -31.64140, 2000, 0., 0., 1978,0 75,"LWS01",3.,"N", "NGC 5253 ", 13.66548, -31.64140, 2000, 0., 0., 960,0 76,"PHT40",3.,"N", "NGC 5253 ", 13.66548, -31.64140, 2000, 0., 0., 1261,0 77,"SWS02",3.,"N", "F15564+6359 ", 15.95056, +63.84190, 2000, 0., 0., 6766,0 78,"LWS02",3.,"N", "F15564+6359 ", 15.95056, +63.84190, 2000, 0., 0., 640,0 79,"PHT40",3.,"N", "F15564+6359 ", 15.95056, +63.84190, 2000, 0., 0., 1261,0 80,"SWS02",3.,"N", "NGC 6764 ", 19.13788, +50.93319, 2000, 0., 0., 1222,0 81,"PHT40",3.,"N", "NGC 6764 ", 19.13788, +50.93319, 2000, 0., 0., 1261,0 82,"SWS02",3.,"N", "NGC 6946 ", 20.58120, +60.15385, 2000, 0., 0., 1512,0 83,"SWS02",3.,"N", "NGC 6946 off ", 20.58114, +60.21496, 2000, 0., 0., 2112,0 84,"SWS02",3.,"N", "NGC 6946 sky ", 20.58120, +60.35385, 2000, 0., 0., 1512,0 85,"PHT40",3.,"N", "NGC 6946 ", 20.58120, +60.15385, 2000, 0., 0., 1261,0 86,"SWS02",3.,"N", "NGC 7552 ", 23.26966, -42.58421, 2000, 0., 0., 756,0 87,"LWS01",3.,"N", "NGC 7552 ", 23.26966, -42.58421, 2000, 0., 0., 960,0 88,"PHT40",3.,"N", "NGC 7552 ", 23.26966, -42.58421, 2000, 0., 0., 1261,0 <=== spring_launch_targets ===> 1,"SWS01",1.,"N", "GC SgrA* ", 17.76112, -29.00794, 2000, 0., 0., 3498,0 2,"SWS01",1.,"N", "IC443 ion ", 6.29288, +22.88191, 2000, 0., 0., 6498,0 3,"PHT40",3.,"N", "IC443 ion ", 6.29288, +22.88191, 2000, 0., 0., 493,0 4,"SWS01",1.,"N", "30 Dor ", 5.64612, -69.08553, 2000, 0., 0., 6498,0 5,"SWS02",2.,"N", "30 Dor ", 5.64612, -69.08553, 2000, 0., 0., 4402,0 6,"LWS01",2.,"N", "30 Dor ", 5.64612, -69.08553, 2000, 0., 0., 570,0 7,"PHT40",3.,"N", "30 Dor ", 5.64612, -69.08553, 2000, 0., 0., 493,0 8,"SWS01",1.,"N", "DR 21 ", 20.65009, +42.32797, 2000, 0., 0., 6498,0 9,"SWS02",2.,"N", "DR 21 ", 20.65009, +42.32797, 2000, 0., 0., 5546,0 10,"LWS01",3.,"N", "DR 21 ", 20.65009, +42.32797, 2000, 0., 0., 570,0 11,"PHT40",3.,"N", "DR 21 ", 20.65009, +42.32797, 2000, 0., 0., 493,0 12,"SWS01",1.,"N", "M82 ", 9.93076, +69.67899, 2000, 0., 0., 6498,0 13,"SWS02",1.,"N", "M82 ", 9.93076, +69.67899, 2000, 0., 0., 2818,0 14,"PHT40",3.,"N", "M82 ", 9.93076, +69.67899, 2000, 0., 0., 493,0 15,"SWS01",2.,"N", "NGC 253 ", 0.79255, -25.28811, 2000, 0., 0., 6498,0 16,"SWS02",2.,"N", "NGC 253 ", 0.79255, -25.28811, 2000, 0., 0., 3258,0 17,"SWS02",2.,"N", "NGC 253 off ", 0.80013, -25.20350, 2000, 0., 0., 2112,0 18,"PHT40",3.,"N", "NGC 253 ", 0.79255, -25.28811, 2000, 0., 0., 493,0 19,"SWS01",1.,"N", "NGC 1068 ", 2.71132, -00.01314, 2000, 0., 0., 6498,0 20,"SWS06",1.,"N", "NGC 1068 ", 2.71132, -00.01314, 2000, 0., 0.,10352,0 21,"SWS02",1.,"N", "NGC 1068 ", 2.71132, -00.01314, 2000, 0., 0., 2112,0 22,"PHT40",3.,"N", "NGC 1068 ", 2.71132, -00.01314, 2000, 0., 0., 493,0 23,"SWS01",1.,"N", "NGC 4151 ", 12.17573, +39.40584, 2000, 0., 0., 6498,0 24,"SWS02",1.,"N", "NGC 4151 ", 12.17573, +39.40584, 2000, 0., 0., 5902,0 25,"SWS02",1.,"N", "NGC 4151 ", 12.17573, +39.40584, 2000, 0., 0., 8340,0 26,"PHT40",3.,"N", "NGC 4151 ", 12.17573, +39.40584, 2000, 0., 0., 1261,0 27,"SWS02",1.,"N", "NGC 891 ", 2.37590, +42.34949, 2000, 0., 0., 7470,0 28,"SWS02",1.,"N", "NGC 891 ", 2.37590, +42.34949, 2000, 0., 0., 6036,0 29,"SWS02",2.,"N", "NGC 891 off ", 2.37652, +42.36697, 2000, 0., 0., 2112,0 30,"SWS02",2.,"N", "NGC 891 off1 ", 2.37706, +42.38028, 2000, 0., 0., 2112,0 31,"SWS02",2.,"N", "NGC 891 off2 ", 2.37759, +42.39581, 2000, 0., 0., 2112,0 32,"PHT40",3.,"N", "NGC 891 ", 2.37590, +42.34949, 2000, 0., 0., 1261,0 33,"SWS02",3.,"N", "NGC 4567 ", 12.60908, +11.25803, 2000, 0., 0., 2164,34 34,"SWS02",3.,"N", "NGC 4568 ", 12.60950, +11.24026, 2000, 0., 0., 948,0 35,"LWS01",3.,"N", "NGC 4567 ", 12.60908, +11.25803, 2000, 0., 0., 1740,36 36,"LWS01",3.,"N", "NGC 4568 ", 12.60950, +11.24026, 2000, 0., 0., 1580,0 37,"PHT40",3.,"N", "NGC 4567 ", 12.60908, +11.25803, 2000, 0., 0., 1261,38 38,"PHT40",3.,"N", "NGC 4568 ", 12.60950, +11.24026, 2000, 0., 0., 1101,0 39,"SWS02",3.,"N", "NGC 5194 M 51 ", 13.49797, +47.19515, 2000, 0., 0., 1108,0 40,"PHT40",3.,"N", "NGC 5194 M 51 ", 13.49797, +47.19515, 2000, 0., 0., 1261,0 41,"SWS02",3.,"N", "II Zw 40 ", 5.92850, +03.39209, 2000, 0., 0., 4002,0 42,"SWS02",3.,"N", "He 2-10 ", 8.60416, -26.40941, 2000, 0., 0., 9330,0 43,"PHT40",3.,"N", "He 2-10 ", 8.60416, -26.40941, 2000, 0., 0., 1261,0 44,"SWS02",3.,"N", "IC 342 ", 3.78002, +68.09632, 2000, 0., 0., 5634,0 45,"SWS02",3.,"N", "IC 342 sky ", 3.78002, +68.19632, 2000, 0., 0., 5634,0 46,"PHT40",3.,"N", "IC 342 ", 3.78002, +68.09632, 2000, 0., 0., 1261,0 47,"SWS02",1.,"N", "NGC 1808 ", 5.12841, -37.51265, 2000, 0., 0., 5370,0 48,"LWS01",1.,"N", "NGC 1808 ", 5.12841, -37.51265, 2000, 0., 0., 960,0 49,"PHT40",3.,"N", "NGC 1808 ", 5.12841, -37.51265, 2000, 0., 0., 1261,0 50,"SWS01",1.,"N", "NGC 3256 ", 10.46423, -43.90374, 2000, 0., 0., 6498,0 51,"SWS02",1.,"N", "NGC 3256 ", 10.46423, -43.90374, 2000, 0., 0., 5898,0 52,"LWS01",1.,"N", "NGC 3256 ", 10.46423, -43.90374, 2000, 0., 0., 960,0 53,"PHT40",3.,"N", "NGC 3256 ", 10.46423, -43.90374, 2000, 0., 0., 1261,0 54,"SWS02",2.,"N", "NGC 3690 A ", 11.47601, +58.56293, 2000, 0., 0., 9740,0 55,"SWS02",2.,"N", "NGC 3690 B/C ", 11.47524, +58.56266, 2000, 0., 0., 6364,0 56,"PHT40",3.,"N", "NGC 3690 A ", 11.47601, +58.56293, 2000, 0., 0., 1261,57 57,"PHT40",3.,"N", "NGC 3690 B/C ", 11.47524, +58.56266, 2000, 0., 0., 1101,0 58,"SWS02",3.,"N", "NGC 1614 ", 4.56668, -08.57911, 2000, 0., 0., 756,0 59,"LWS01",3.,"N", "NGC 1614 ", 4.56668, -08.57911, 2000, 0., 0., 960,0 60,"PHT40",3.,"N", "NGC 1614 ", 4.56668, -08.57911, 2000, 0., 0., 1261,0 61,"SWS02",3.,"N", "NGC 2903 ", 9.53614, +21.50170, 2000, 0., 0., 756,0 62,"LWS01",3.,"N", "NGC 2903 ", 9.53614, +21.50170, 2000, 0., 0., 960,0 63,"PHT40",3.,"N", "NGC 2903 ", 9.53614, +21.50170, 2000, 0., 0., 1261,0 64,"SWS02",2.,"N", "NGC 3079 ", 10.03272, +55.67995, 2000, 0., 0., 1864,0 65,"SWS02",2.,"N", "NGC 3079 off ", 10.03409, +55.65462, 2000, 0., 0., 2112,0 66,"LWS01",2.,"N", "NGC 3079 ", 10.03272, +55.67995, 2000, 0., 0., 960,0 67,"PHT40",3.,"N", "NGC 3079 ", 10.03272, +55.67995, 2000, 0., 0., 1261,0 68,"SWS02",3.,"N", "NGC 4038 ", 12.03142, -18.86809, 2000, 0., 0., 756,69 69,"SWS02",3.,"N", "NGC 4039 ", 12.03148, -18.88614, 2000, 0., 0., 596,70 70,"SWS02",3.,"N", "NGC 4038/39 ov", 12.03192, -18.88448, 2000, 0., 0., 596,0 71,"PHT40",3.,"N", "NGC 4038 ", 12.03142, -18.86809, 2000, 0., 0., 1261,72 72,"PHT40",3.,"N", "NGC 4039 ", 12.03148, -18.88614, 2000, 0., 0., 1101,73 73,"PHT40",3.,"N", "NGC 4038/39 ov", 12.03192, -18.88448, 2000, 0., 0., 1101,0 74,"SWS02",3.,"N", "NGC 6764 ", 19.13788, +50.93319, 2000, 0., 0., 1222,0 75,"PHT40",3.,"N", "NGC 6764 ", 19.13788, +50.93319, 2000, 0., 0., 1261,0 76,"SWS02",3.,"N", "NGC 6946 ", 20.58120, +60.15385, 2000, 0., 0., 1512,0 77,"SWS02",3.,"N", "NGC 6946 off ", 20.58114, +60.21496, 2000, 0., 0., 2112,0 78,"SWS02",3.,"N", "NGC 6946 sky ", 20.58120, +60.35385, 2000, 0., 0., 1512,0 79,"LWS01",3.,"N", "NGC 6946 ", 20.58120, +60.15385, 2000, 0., 0., 960,0 80,"PHT40",3.,"N", "NGC 6946 ", 20.58120, +60.15385, 2000, 0., 0., 1261,0 81,"SWS02",3.,"N", "NGC 7552 ", 23.26966, -42.58421, 2000, 0., 0., 5898,0 82,"LWS01",3.,"N", "NGC 7552 ", 23.26966, -42.58421, 2000, 0., 0., 960,0 83,"PHT40",3.,"N", "NGC 7552 ", 23.26966, -42.58421, 2000, 0., 0., 1261,0