Page 1 PROPOSAL FOR HUBBLE SPACE TELESCOPE OBSERVATIONS ST ScI Use Only ID 5431 Report Date: 18-Jul-95:17:22 Version: ********** Check-in Date: ********** 1.Proposal Title: FOS OBSERVATIONS OF LINER GALAXY NUCLEI: ULTRAVIOLET CLUES TO THE NATURE OF THE LINER PHENOMENON - CYCLE4MEDIUM ------------------------------------------------------------------------------------ 2. Scientific Category 3. Proposal For 4. Proposal Type 5. Continuation ID QUASARS & AGN GO Sub Category OTHER ACTIVE NUCLEI ------------------------------------------------------------------------------------ 6. Principal Investigator Institution Country Telephone Gail A. Reichert USRA USA ------------------------------------------------------------------------------------ 7. Abstract LINER galaxies potentially form a class of "dwarf" AGN, dominating the number densities of low luminosity AGN and their contribution to the diffuse X-ray background. LINERs also provide clues as to how star formation in galaxies might be triggered, and the relationship between star formation and nonthermal activity. Progress has been made at optical and radio wavelengths towards explaining the low- excitation, line-emitting gas observed in LINERs. However, the nature of this ubiquitous class of galaxies remains elusive primarily because the nuclear emission is swamped by galactic light at these wavelengths. Several models have been proposed -- shock heating, cooling flows, photoion- ization by "dwarf" AGN, and photoionization by hot stars or "Warmers". The direct spectral "signatures" of the nuclear emission can only be effectively studied in the UV where contamination from normal stars is much reduced. To understand the fundamental energetics of LINER galaxies, it is essential to characterize their UV continuum and determine the fluxes and profiles of the diagnostically important UV emission lines. The unique capabilities of HST offer us an unprecedented opportunity to isolate and study the nuclei of LINERs in the UV. We therefore propose FOS observations of a sample of LINERs, to 1) measure their UV continua accurately, 2) search for nonthermal (or stellar) photoionizing continua and also for UV absorption lines from hot young stars, and 3) measure the strengths and profiles of the UV emission lines. ------------------------------------------------------------------------------------ ------------------------------------------------------------------------------------ 9. Est obs time (hours) pri: 11.11 par: 0 10. Num targs pri: 4 par: 0 ------------------------------------------------------------------------------------ 11. Instruments requested: FOS ------------------------------------------------------------------------------------ ------------------------------------------------------------------------------------ Page 2 I. GENERAL FORM Proposal 5431 PI: Gail A. Reichert Proposal Title: FOS OBSERVATIONS OF LINER GALAXY NUCLEI: ULTRAVIOLET CLUES TO THE NATURE OF THE LINER PHENOMENON - CYCLE4MEDIUM ------------------------------------------------------------------------------------ 1. Proposers: Proposers Institution Country ESA ------------------------------------------------------------------------------------ Pi Gail A. Reichert USRA USA Alexei V. Filippenko UC-BERKELEY USA Joseph C. Shields STEWARD OBSERVATORY USA Steven N. Shore INDIANA UNIVERSITY AT SOUTH BEND USA Richard F. Mushotzky NASA GODDARD SPACE FLIGHT CENTER USA Elizabeth M. Puchnarewicz MULLARD SPACE SCIENCE LABORATORY UNITED KING X Graziella Branduardi-Raymont MULLARD SPACE SCIENCE LABORATORY UNITED KING X Keith O. Mason MULLARD SPACE SCIENCE LABORATORY UNITED KING X ------------------------------------------------------------------------------------ 3. Description of proposed observations. We propose HST FOS observations of four UV bright LINERs: NGC404, NGC4579, NGC4594, and NGC6500. Our goals are to detect faint lines, to search for absorption line signatures of hot young stars, to model the profiles of strong lines, and to determine the overall shape of the continuum. We therefore require spectra having good S/N ratio and modest resolution over the entire accessible UV wavelength range. Each target will be observed using three HST grating settings, as follows: (1) FOS, G130H grating, 1150-1608 A, 1.0 A/diode, blue digicon. (2) FOS, G190H grating, 1573-2323 A, 1.5 A/diode, red digicon. (3) FOS, G270H grating, 2227-3306 A, 2.1 A/diode, red digicon. Each target will be observed using all three gratings. Spectra will be obtained through the 1.0" circular aperture for all targets except NGC 4579. This yields the best throughput, and the resulting resolution will be adequate for our purposes. NGC 4579 will be observed using the 0.5" circular aperture, to avoid contamination with a nearby bright component of emission. At UV wavelengths, the starlight contamination through either 1.0" or 0.5" aperture will be small compared with light from the core component for all four targets. The FOS spectra will be combined with optical spectra obtained at ground-based observatories. This will give reliable continuum shapes over the range 1150-10000 A, and it will allow us to obtain accurate emission-line intensity ratios between UV and optical lines. Page 3 ------------------------------------------------------------------------------------ 4. Justification of need for HST observations. Despite intensive study since the identification of LINERs as a class (Heckman 1980), our understanding of the LINER phenomenon remains confused. Studies of LINERs at optical wavelengths are critically limited by the strength of the background radiation of the normal stellar component, which completely overwhelms the nuclear emission. Groundbased observations can give us no information concerning the fluxes in the ultraviolet emission lines, several of which (e.g., CIV, HeII, SiIII], OIII], SiIV, NIII]) are extremely important diagnostics of the state of the line emitting gas, and are also insensitive to the presence of main sequence (and supergiant) O-type stars. The situation is better with IUE, as the stellar continuum at UV wavelengths is much decreased. However, due to the large aperture, IUE spectra are also dominated by the extended stellar background. Moreover, only a very few LINERs are bright enough to study with IUE in exposures of < 16 hours, and the resulting spectra are also of too low S/N to allow us to detect the weaker UV lines or absorption lines from hot young stars. Camera artifacts in the IUE spectra also complicate measurements of emission line fluxes and profiles. Radio observations have been useful in showing that many LINERs contain compact, flat spectrum, nuclear radio sources similar to those seen in AGN. However, this is not conclusive evidence since the emission from collections of supernova remnants could also mimic a (relatively) flat spectrum. X-ray observations of LINERs hold promise, but provide little information on the fluxes at photon energies near those which would excite the line emitting gas. For these reasons, we propose HST FOS observations of selected LINERs. Our goals are to detect faint lines, to search for absorption line signatures of hot young stars, to model the profiles of broad lines, and to determine the overall shape of the continuum. HST, with its ultraviolet sensitivity, its higher spectral resolution, the linear responses of its spectral instruments over wide dynamic ranges, and its ability to use smaller apertures in the ultraviolet, is uniquely suited for studying LINER galaxies at UV wavelengths. Ultraviolet observations with HST are the only means by which we can significantly advance our understanding of the fundamental energetics of LINER galaxies, and the means by which the line emitting gas is excited. The exposure times for each target should be as follows: (1) NGC404: 109 min G130H, 30 min G190H, 9 min G270H. (2) NGC4579: 114 min G130H, 55 min G190H, 13 min G270H. (3) NGC4594: 62 min G130H, 30 min G190H, 8 min G270H. (4) NGC6500: 171 min G130H, 47 min G190H, 17 min G270H. The exposure times were calculated to give us signal-to-noise ratios (S/N) of at least 8 (after rebinning to 512 diodes) in the continuum over almost the entire ultraviolet range from 1400 A to 3200 A. For the brighter three targets, we expect to obtain S/N of 20 in the continuum at C III] 1909 and longward of 2400 A, and S/N of 12 in the range 1400 to 1600 A. For NGC6500 (which is 1/3 as bright), we expect to obtain S/N of 13, 13, and 10 over the same ranges. The expected count rates in the various gratings were calculated based on the observed IUE fluxes, and our separations of the IUE emission into core and (extended) background components. We used the curves given in Figure 1.2.3 in the FOS Instrument Handbook (Kinney 1993), and made the following assumptions: (1) that the nuclear emission is spatially distributed as a point source. (2) that the nuclear emission in NGC6500 comprises the same fraction of the total emission as in NGC3998. (3) that the extinctions to all objects are the foreground reddenings as estimated by Burstein and Heiles (1984). (4) that the fluxes for NGC6500 at wavelengths < 2000 A can be scaled according to the observed IUE LWP fluxes and the average spectrum of the brighter objects. We did not include the fluxes from the extended components of emission seen by IUE, as we estimate that these will be negligible in the 1.0" aperture for all wavelengths < 3200 A. The estimated count rates are all high enough that background subtraction should be unnecessary. Sample calculations for NGC~4579 show that for nuclear fluxes of 2.0, 1.4, and 1.1 e-15 ergs/square cm/sec/A at 1400, 1800, and 2400 A, we can expect count rates of 0.028, 0.15, and 0.57 counts/s/diode with the G130H (blue), G190H (red), and G270H (red) gratings, respectively. Estimated nuclear fluxes for our other targets are as follows: NGC404: 1.9, 2.4, and 1.5 e-15 ergs/square cm/sec/A at 1400, 1800, and 2400 A. NGC4594: 3.3, 2.0, and 1.6 e-15 ergs/square cm/sec/A at 1400, 1800, and 2400 A. NGC6500: 3.3e-16 erg/square cm/sec/A at 2400 A. Exposure times for G130H and G190H estimated by scaling observed 2400 A flux to average spectrum of our other targets. Our program requires a total on-target observing time of 667 minutes (11.11 hours), and about 1071 minutes (17.85 hours) total spacecraft time. Page 4 ------------------------------------------------------------------------------------ 5. Description of special scheduling requirements. Because our targets are galaxies, and the emission is likely to be extended on subarcsec scales, our strategy will be to acquire the targets using three acquisition peakups; the first using a 3 by 1 spatial scan with the 4.3" aperture, the second using a 6 by 2 spatial scan with the 1" circular aperture, and the third using a 3 by 3 spatial scan with the 0.5" circular aperture. For NGC 4579, we will do a fourth acquisition peakup, using a 3 by 3 spatial scan in the 0.3" aperture. Our plan is to acquire each target using the red side of the FOS. The aquisitions should be done using the G270H grating for NGC 404 and NGC 4579 and the G400H grating for NGC 4594 and NGC 6500. The dwell times for the first ACQ/PEAK should be 4 sec, 5 sec, 0.9 sec, and 5 sec for NGC404, NGC4579, NGC4594, and NGC 6500 respectively. The dwell times for the second ACQ/PEAK should be 4 sec, 5 sec, 2 sec, and 11 sec, and the dwell times for the third ACQ/PEAK should be 5 sec, 5 sec, 8.5 sec, and 30 sec. Finally the dwell time for the fourth for NGC 4579 should be 16 sec. FOC images (at 2300 A) of NGC 404 and NGC 4579 show that the nuclei in these galaxies are point sources, and the dwell times were calculated based on the estimated 2300 A fluxes. For NGC 4594 and NGC 6500, the dwell times were calculated based on the estimated magnitudes within the 4.3", 1", or 0.5" apertures, assuming a K5V spectrum. In all cases the dwell times should yield about 1000 counts for each dwell point. Since the visit to each target will require less than 6 hours of spacecraft time, we do not need separate acqusitions for the blue side (G130H). At visual wavelengths, the light from these galaxies are dominated by fairly late type (late G - K) stars. We would much prefer that target acquisition be performed with the red side of the FOS, to ensure that enough counts are obtained for each dwell point in the scan, without having to decrease our science exposures. However, if it becomes necessary to use the blue side for acquisition, then we calculate that we would require an additional 0.6, 1.65, 2.68, and 11.02 minutes for the acquisition peakups for NGC404, NGC4579, NGC4594, and NGC6500, respectively. If the blue side is used for all of the target acquisitions, then a total additional time of 15.95 minutes would be required. Please take the additional time required from the G130H exposure for NGC6500. ------------------------------------------------------------------------------------ 6. Description of special calibration exposures. None. ------------------------------------------------------------------------------------ 8. Additional comments or special requests. When our HST observing dates become known, we will request nearly simultaneous time at Lick and Keck Observatories to obtain spectra and images at optical and infrared wavelengths. We will also apply for VLA and/or VLBI time to map the radio emission, and continue to apply for Rosat time to look for X-ray emission. (We have already been awarded Rosat time to observe one of our targets, NGC4579; NGC4594 will be observed by Dr. W. Forman.) These data will be combined with the UV spectra to construct an overall continuum spanning a large wavelength range. A complete analysis of the data will subsequently be done. Note that no funds are being requested to support the ground-based observations. The aims of this proposal may overlap somewhat with the aims of other GTO and GO cycle 1 spectroscopic programs to investigate other LINERs (notably those involving M81), but it appears from the GTO program handbook and supplement that the observing strategies will differ substantially and that ours will be a more effective and thorough approach to investigate their ultraviolet properties. We will request these and other related data when these are released, in order to increase our sample and allow more definitive comparisons between LINERs of various types. Page 5 ------------------------------------------------------------------------------------ 9. Description of previous HST work. Filippenko, Reichert, and Shields, Co-Is: GO 3484, "Probing the Nuclear Regions of the Seyfert Galaxy NGC 5548". (PI: B. M. Peterson). Not related to this project. Filippenko, PI: GO 3507, "UV Spectroscopy and High-Resolution Imaging of NGC 4395, the Least Luminous and Nearest Known Seyfert 1 Nucleus" . Not related to this project. Filippenko, PI: GO 4340, "Origin of Blue Featureless Continuum in Seyfert 2 Nuclei". Not related to this project. Filippenko, PI: GO 4635, "Accretion Disk Line-Profile Hypothesis in Arp 102B". Not related to this project. Mushotzky, Reichert, Co-Is: GTO 1160, "Absorption Cloud Physics in Seyfert Galaxy Nuclei" (PI: S. Maran). Not related to this project. Reichert, PI: GO 4350, "FOS Observations of LINER Galaxy Nuclei". Related to this project. With involvement by Filippenko as PI in 3 additional programs (GO 2590, GO 4302, GO 4312) and as co-I in 3 additional programs (GO 3519, PI: D. Maoz; GO 3810, PI: P. Conti; QSO Snapshot Survey, PI: J. N. Bahcall), and by Shore as PI in 5 additional programs (GO 3412, GO 3812, GO 3825, 4053, 4806) and as co-I in one additional program (GO 4494, PI: Vogel). None are related to this project. The only program related to this proposal is our Cycle 3 GO program 4350. As yet, none of the observations for this program have been done. We are resubmitting the proposal for Cycle 4 in the event that not all of the observations are successfully carried out during Cycle 3. "A Gravitational Lens Candidate Discovered with the Hubble Space Telescope." D. Maoz et al., Ap. J (Lett.) 386:L1 (1992). "HST Observations of NGC 4395,the Least Luminous Seyfert 1 Nucleus: Evidence Against the Starburst Hypothesis for Broad-Lined Active Galactic Nuclei." A. V. Filippenko, L. C. Ho, and W. L. W. Sargent, Ap J. (Lett.), in press. "NGC 4395: Evidence Against the Starburst Hypothesis for Seyfert 1 Nuclei and QSOs." A. V. Filippenko, L. C. Ho, and W. L. W. Sargent, in {\it 16th Texas Symposium/3rd Symposium on Particles, Strings, and Cosmology}, ed. C. Akerlof and M. Srednicki (New York: New York Academy of Sciences), 1993, in press. Plus 11 additional publications on stellar topics (Shore as principal author or co- author). ------------------------------------------------------------------------------------ 10. Resources to be supplied by investigator's institution(s). All members of the consortium routinely have access to DEC Vax computers and/or Vax workstations and/or Sun workstations dedicated to astronomical data reduction and running IRAF or equivalent data analysis environments. Many computer programs exist for analysis of data. All members are linked by computer networks and have considerable experience of working closely together "at a distance". Of course, we will want the entire group to meet at least once for a comprehensive discussion of the data and their interpretation. (Note that no funds for travel for non-US investigators are being requested.) A number of us supervise excellent graduate student research assistants, some of whom may participate in various aspects of this project. Ground-based complementary observations can readily be obtained (with short notice) at Lick Observatory; proposals for Keck time will also be submitted by co-I Filippenko. The usual secretarial and technical support is available at UC Berkeley, GSFC, MSSL, Steward Observatory, and Indiana State University. ------------------------------------------------------------------------------------ 11. Address Information Name: GAIL A. REICHERT Category: PI Institution: USRA Address: CODE 668 NASA/GODDARD SPACE FLIGHT CENTER City: GREENBELT State: MD Zip Code: 20771 Country: USA Telephone: (301) 286 5307 Telex (or e-mail): ------------------------------------------------------------------------------------ TARGET LIST a) Fixed Targets ID = 5431 [ 6] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 ------------------------------------------------------------------------------------------------------------------------------------ Tar| Target | Target | Target |Coord | Radial |Acqui|FLX| Flux data No | Name | Description | Position |Eqnx | Vel. |Prblm|REF| | | | | | | | | ------------------------------------------------------------------------------------------------------------------------------------ 1 NGC404 E,303,304,317,910 RA = 01H 09M 26.98 S +/- 2000.0 V = -39 1 V = 15.5 +/- 0.3 0.06S, 2 B-V = 0.86 DEC = +35D 43' 04.52" +/- 3 F-CONT(1400) = 1.9 +/- 0.4 E-15 0.3" 4 F-CONT(1700) = 2.3 +/- 0.5 E-15 5 F-CONT(2400) = 1.5 +/- 0.4 E-15 Comments: FLUXES ARE FOR NUCLEUS ONLY, FROM OUR IUE OBSERVATIONS. V MAG IS FOR 4.3 X 1.4 SEC APERTURE, BASED ON SURFACE PHOTOMETRY OF BARBON ET AL 1982 A&A 115:388. COORDINATES HAVE BEEN MEASURED USING OUR OWN OPTICAL PLATE ------------------------------------------------------------------------------------------------------------------------------------ 2 NGC4579 M58 E,301,315,317,910 RA = 12H 35M 11.99S +/- 1950.0 V = 1 V = 15.2 +/- 0.3 0.02S, +1519 2 B-V = 0.9 DEC = +12D 05' 35.6" +/- 3 F-CONT(1400) = 2.0 +/- 0.5 E-15 0.3" 4 F-CONT(1700) = 1.4 +/- 0.3 E-15 5 F-CONT(2400) = 1.1 +/- 0.3 E-15 Comments: FLUXES ARE FOR NUCLEUS ONLY, FROM OUR IUE OBSERVATIONS. V MAG IS FOR 4.3 X 1.4 SEC APERTURE, BASED ON SURFACE PHOTOMETRY OF WHITMORE AND 1982 AJ 87:500. COORDINATES ARE VLA RADIO POSITION OF NUCLEUS FROM VAN DER HULST ET AL. 1981 AJ 86:1175. ------------------------------------------------------------------------------------------------------------------------------------ 3 NGC4594 M104 E,301,315,317,910 RA = 12H 37M 23.38S +/- 1950.0 V = 1 V = 14.0 +/- 0.3 SOMBRERO- 0.02S, +1091 2 B-V = 1.1 GALAXY DEC = -11D 20' 55.0" +/- 3 F-CONT(1400) = 3.3 +/- 0.8 E-15 0.3" 4 F-CONT(1700) = 2.0 +/- 0.5 E-15 5 F-CONT(2400) = 1.6 +/- 0.4 E-15 Comments: FLUXES ARE FOR NUCLEUS ONLY, FROM OUR IUE OBSERVATIONS. V MAG IS FOR 4.3 X 1.4 SEC APERTURE, BASED ON SURFACE PHOTOMETRY OF KORMENDY 1988 APJ 335:50. ESTIMATED V MAG FOR 1 SEC APERTURE IS 15.5. COORDINATES ARE VLBI RADIO POSITION OF NUCLEUS FROM JAUNCEY ET AL 1989 AJ 98:54. ------------------------------------------------------------------------------------------------------------------------------------ 4 NGC6500 E,301,315,317,320,910 RA = 17H 53M 48.14S +/- 1950.0 V = 1 V = 15.9 +/- 0.2 0.01S, +3003 2 F-CONT(1500) = 7.0 E-16 DEC = +18D 20' 40.2" +/- 3 F-CONT(1800) = 5.0 E-16 0.1" 4 F-CONT(2300) = 3.3 +/- 1.1 E-16 Comments: ESTIMATED NUCLEAR FLUXES (SEE QUESTION 5). V MAG IS FOR 4.3 X 1.4 4 SEC APERTURE, ASSUMING SAME PROFILE AS NGC4579. ESTIMATED V MAG FOR 1 SEC APERTURE IS 17.3. COORDINATES ARE VLA RADIO POSITION OF NUCLEUS FROM HUMMEL ET AL. 1984 A&A 134:207. ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 5431 [ 7] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 | 9 |10 | 11 | 12 |13 |14| 15 ------------------------------------------------------------------------------------------------------------------------------------ Line | Seq | Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | S/N |Flx|Pr| Special Number | Name | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| |Rel. Time|Ref| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 1 NGC404 FOS/RD ACQ/ 4.3 G270H SCAN-STEP- 1 4S 4 1 ONBOARD ACQ FOR 2 PEAK Y=1.204 CYCLE 4 / 1-6 SEARCH-SIZE-X=1 GROUP 1-6 NO GAP SEARCH-SIZE-Y=3 Comments: BLUE SIDE ACQ/PEAK- SPECTRAL ELEMENT=G270H; EXP=5S ------------------------------------------------------------------------------------------------------------------------------------ 2 NGC404 FOS/RD ACQ/ 1.0 G270H SCAN-STEP- 1 4S 4 1 ONBOARD ACQ FOR 3 PEAK X=.602 SCAN-STEP- Y=.602 SEARCH-SIZE-X=6 SEARCH-SIZE-Y=2 Comments: BLUE SIDE ACQ/PEAK- SPECTRAL ELEMENT=G270H; EXP=6S ------------------------------------------------------------------------------------------------------------------------------------ 3 NGC404 FOS/RD ACQ/ 0.3 G270H SCAN-STEP- 1 15S 4 1 ONBOARD ACQ FOR 4- PEAK X=.172 6 SCAN-STEP- Y=.172 SEARCH-SIZE-X=5 SEARCH-SIZE-Y=5 Comments: BLUE SIDE ACQ/PEAK- SPECTRAL ELEMENT=G270H; EXP=6S ------------------------------------------------------------------------------------------------------------------------------------ 4 NGC404 FOS/RD ACCUM 1.0 G270H 2760 1 9M 20 5 2 Comments: IF THERE IS EXTRA TIME BEFORE EARTH OCCULTATION NEAR END OF EXPOSURE, CAN INCREASE EXPOSURE TIME TO INCREASE S/N RATIO. ------------------------------------------------------------------------------------------------------------------------------------ 5 NGC404 FOS/RD ACCUM 1.0 G190H 1950 1 30M 20 4 1 Comments: IF THERE IS EXTRA TIME BEFORE EARTH OCCULTATION NEAR END OF EXPOSURE, CAN INCREASE EXPOSURE TIME TO INCREASE S/N RATIO. ------------------------------------------------------------------------------------------------------------------------------------ 6 NGC404 FOS/BL ACCUM 4.3 G130H 1380 1 109M 12 3 1 Comments: IF THERE IS EXTRA TIME BEFORE EARTH OCCULTATION NEAR END OF EXPOSURE, CAN INCREASE EXPOSURE TIME TO INCREASE S/N RATIO. ------------------------------------------------------------------------------------------------------------------------------------ 11 NGC4579 FOS/RD ACQ/ 4.3 G270H SCAN-STEP- 1 5S 4 1 ONBOARD ACQ FOR 12 PEAK Y=1.204 CYCLE 4 / 11-17 SEARCH-SIZE-X=1 GROUP 11-17 NO GAP SEARCH-SIZE-Y=3 Comments: BLUE SIDE ACQ/PEAK- SPECTRAL ELEMENT=G270H; EXP=6S ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 5431 [ 8] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 | 9 |10 | 11 | 12 |13 |14| 15 ------------------------------------------------------------------------------------------------------------------------------------ Line | Seq | Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | S/N |Flx|Pr| Special Number | Name | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| |Rel. Time|Ref| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 12 NGC4579 FOS/RD ACQ/ 1.0 G270H SCAN-STEP- 1 5S 4 1 ONBOARD ACQ FOR 14 PEAK X=.602 SCAN-STEP- Y=.602 SEARCH-SIZE-X=6 SEARCH-SIZE-Y=2 Comments: BLUE SIDE ACQ/PEAK- SPECTRAL ELEMENT=G270H; EXP=7S ------------------------------------------------------------------------------------------------------------------------------------ 14 NGC4579 FOS/RD ACQ/ 0.3 G270H SCAN-STEP- 1 16S 4 1 ONBOARD ACQ FOR 15 PEAK X=.172 -17 SCAN-STEP- Y=.172 SEARCH-SIZE-X=5 SEARCH-SIZE-Y=5 Comments: BLUE SIDE ACQ/PEAK- SPECTRAL ELEMENT=G270H; EXP=22S ------------------------------------------------------------------------------------------------------------------------------------ 15 NGC4579 FOS/RD ACCUM 0.5 G270H 2760 1 13M 20 5 2 Comments: IF THERE IS EXTRA TIME BEFORE EARTH OCCULTATION NEAR END OF EXPOSURE, CAN INCREASE EXPOSURE TIME TO INCREASE S/N RATIO. ------------------------------------------------------------------------------------------------------------------------------------ 16 NGC4579 FOS/RD ACCUM 0.5 G190H 1950 1 55M 20 4 1 Comments: IF THERE IS EXTRA TIME BEFORE EARTH OCCULTATION NEAR END OF EXPOSURE, CAN INCREASE EXPOSURE TIME TO INCREASE S/N RATIO. ------------------------------------------------------------------------------------------------------------------------------------ 16.5 NGC4579 FOS/BL ACQ/ 0.3 G130H SCAN-STEP- 1 16S 4 1 ONBOARD ACQ FOR 17 PEAK X=.172 SCAN-STEP- Y=.172 SEARCH-SIZE-X=5 SEARCH-SIZE-Y=5 Comments: BLUE SIDE ACQ/PEAK- FOR FOS SIDE SWITCH ------------------------------------------------------------------------------------------------------------------------------------ 17 NGC4579 FOS/BL ACCUM 0.5 G130H 1380 1 114M 12 3 1 Comments: IF THERE IS EXTRA TIME BEFORE EARTH OCCULTATION NEAR END OF EXPOSURE, CAN INCREASE EXPOSURE TIME TO INCREASE S/N RATIO. ------------------------------------------------------------------------------------------------------------------------------------ 21 NGC4594 FOS/RD ACQ/ 4.3 G400H SCAN-STEP- 1 2.0S 1 1 ONBOARD ACQ FOR 22 PEAK Y=1.204 CYCLE 4 / 21-26 SEARCH-SIZE-X=1 GROUP 21-26 NO GAP SEARCH-SIZE-Y=3 Comments: BLUE SIDE ACQ/PEAK- SPECTRAL ELEMENT=G400H; EXP=2.1S ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 5431 [ 9] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 | 9 |10 | 11 | 12 |13 |14| 15 ------------------------------------------------------------------------------------------------------------------------------------ Line | Seq | Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | S/N |Flx|Pr| Special Number | Name | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| |Rel. Time|Ref| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 22 NGC4594 FOS/RD ACQ/ 1.0 G400H SCAN-STEP- 1 2S 1 1 ONBOARD ACQ FOR 23 PEAK X=.602 SCAN-STEP- Y=.602 SEARCH-SIZE-X=6 SEARCH-SIZE-Y=2 Comments: BLUE SIDE ACQ/PEAK- SPECTRAL ELEMENT=G400H; EXP=5S ------------------------------------------------------------------------------------------------------------------------------------ 23 NGC4594 FOS/RD ACQ/ 0.3 G400H SCAN-STEP- 1 20.0S 1 1 ONBOARD ACQ FOR 24 PEAK X=.172 -26 SCAN-STEP- Y=.172 SEARCH-SIZE-X=5 SEARCH-SIZE-Y=5 Comments: BLUE SIDE ACQ/PEAK- SPECTRAL ELEMENT=G400H; EXP=22S ------------------------------------------------------------------------------------------------------------------------------------ 24 NGC4594 FOS/RD ACCUM 1.0 G270H 2760 1 8M 20 5 2 Comments: IF THERE IS EXTRA TIME BEFORE EARTH OCCULTATION NEAR END OF EXPOSURE, CAN INCREASE EXPOSURE TIME TO INCREASE S/N RATIO. ------------------------------------------------------------------------------------------------------------------------------------ 25 NGC4594 FOS/RD ACCUM 1.0 G190H 1950 1 30M 20 4 1 Comments: IF THERE IS EXTRA TIME BEFORE EARTH OCCULTATION NEAR END OF EXPOSURE, CAN INCREASE EXPOSURE TIME TO INCREASE S/N RATIO. ------------------------------------------------------------------------------------------------------------------------------------ 26 NGC4594 FOS/BL ACCUM 1.0 G130H 1380 1 62M 12 3 1 Comments: IF THERE IS EXTRA TIME BEFORE EARTH OCCULTATION NEAR END OF EXPOSURE, CAN INCREASE EXPOSURE TIME TO INCREASE S/N RATIO. ------------------------------------------------------------------------------------------------------------------------------------ 31 NGC6500 FOS/RD ACQ/ 4.3 G400H SCAN-STEP- 1 5S 1 1 ONBOARD ACQ FOR 32 PEAK Y=1.204 CYCLE 4 / 31-36 SEARCH-SIZE-X=1 GROUP 31-36 NO GAP SEARCH-SIZE-Y=3 Comments: BLUE SIDE ACQ/PEAK- SPECTRAL ELEMENT=G400H; EXP=12.4S ------------------------------------------------------------------------------------------------------------------------------------ 32 NGC6500 FOS/RD ACQ/ 1.0 G400H SCAN-STEP- 1 11S 1 1 ONBOARD ACQ FOR 33 PEAK X=.602 SCAN-STEP- Y=.602 SEARCH-SIZE-X=6 SEARCH-SIZE-Y=2 Comments: BLUE SIDE ACQ/PEAK- SPECTRAL ELEMENT=G400H; EXP=29S ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 5431 [ 10] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 | 9 |10 | 11 | 12 |13 |14| 15 ------------------------------------------------------------------------------------------------------------------------------------ Line | Seq | Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | S/N |Flx|Pr| Special Number | Name | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| |Rel. Time|Ref| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 33 NGC6500 FOS/RD ACQ/ 0.3 G400H SCAN-STEP- 1 30S 1 1 ONBOARD ACQ FOR 34 PEAK X=.172 -36 SCAN-STEP- Y=.172 SEARCH-SIZE-X=5 SEARCH-SIZE-Y=5 Comments: BLUE SIDE ACQ/PEAK- SPECTRAL ELEMENT=G400H; EXP=77S ------------------------------------------------------------------------------------------------------------------------------------ 34 NGC6500 FOS/RD ACCUM 1.0 G270H 2760 1 17M 13 4 2 Comments: IF THERE IS EXTRA TIME BEFORE EARTH OCCULTATION NEAR END OF EXPOSURE, CAN INCREASE EXPOSURE TIME TO INCREASE S/N RATIO. ------------------------------------------------------------------------------------------------------------------------------------ 35 NGC6500 FOS/RD ACCUM 1.0 G190H 1950 1 47M 13 3 1 Comments: IF THERE IS EXTRA TIME BEFORE EARTH OCCULTATION NEAR END OF EXPOSURE, CAN INCREASE EXPOSURE TIME TO INCREASE S/N RATIO. ------------------------------------------------------------------------------------------------------------------------------------ 36 NGC6500 FOS/BL ACCUM 1.0 G130H 1380 1 171M 9 2 1 Comments: IF THERE IS EXTRA TIME BEFORE EARTH OCCULTATION NEAR END OF EXPOSURE, CAN INCREASE EXPOSURE TIME TO INCREASE S/N RATIO. ------------------------------------------------------------------------------------------------------------------------------------ Summary Form for Proposal 5431 [ 11] Item Used in this proposal ------------------------------------------------------------------------------------------------------------------------------------ Configurations FOS/RD FOS/BL ------------------------------------------------------------------------------------------------------------------------------------ Opmodes ACQ/PEAK ACCUM ------------------------------------------------------------------------------------------------------------------------------------ Optional Parameters SCAN-STEP-Y=1.204 SEARCH-SIZE-X=1 SEARCH-SIZE-Y=3 SCAN-STEP-X=.602 SCAN-STEP-Y=.602 SEARCH-SIZE-X=6 SEARCH-SIZE-Y=2 SCAN-STEP-X=.172 SCAN-STEP-Y=.172 SEARCH-SIZE-X=5 SEARCH-SIZE-Y=5 ------------------------------------------------------------------------------------------------------------------------------------ Proposal for GO ------------------------------------------------------------------------------------------------------------------------------------ S/C Hours 11.11 ------------------------------------------------------------------------------------------------------------------------------------ Scientific Category QUASARS & AGN ------------------------------------------------------------------------------------------------------------------------------------ Scientific Sub-category OTHER ACTIVE NUCLEI ------------------------------------------------------------------------------------------------------------------------------------ Special Requirements ONBOARD ACQ FOR 2; CYCLE 4 / 1-6; GROUP 1-6 NO GAP; ONBOARD ACQ FOR 3; ONBOARD ACQ FOR 4-6; ONBOARD ACQ FOR 12; CYCLE 4 / 11-17; GROUP 11-17 NO GAP; ONBOARD ACQ FOR 14; ONBOARD ACQ FOR 15-17; ONBOARD ACQ FOR 17; ONBOARD ACQ FOR 22; CYCLE 4 / 21-26; GROUP 21-26 NO GAP; ONBOARD ACQ FOR 23; ONBOARD ACQ FOR 24-26; ONBOARD ACQ FOR 32; CYCLE 4 / 31-36; GROUP 31-36 NO GAP; ONBOARD ACQ FOR 33; ONBOARD ACQ FOR 34-36; ------------------------------------------------------------------------------------------------------------------------------------ Spectral Elements G270H G190H G130H G400H ------------------------------------------------------------------------------------------------------------------------------------ Target Names NGC404 NGC4579 M58 NGC4594 M104 SOMBRERO-GALAXY NGC6500 ------------------------------------------------------------------------------------------------------------------------------------