! File: 3647C.PROP ! Database: PEPDB ! Date: 19-FEB-1994:14:59:17 coverpage: title_1: THE STAR-FORMING HISTORIES OF ELLIPTICAL GALAXIES sci_cat: GALAXIES & CLUSTERS sci_subcat: NEARBY GALAXIES proposal_for: GO pi_fname: HENRY pi_mi: C. pi_lname: FERGUSON pi_inst: UNIVERSITY OF CAMBRIDGE, INSTITUTE OF ASTRONOMY pi_country: ENGLAND pi_phone: 0223-337548 hours_pri: 15.00 num_pri: 2 fos: Y funds_length: 12 off_fname: DONALD off_lname: LYNDEN-BELL off_title: DIRECTOR off_inst: INSTITUTE OF ASTRONOMY off_addr_1: UNIVERSITY OF CAMBRIDGE, INSTITUTE OF ASTRONOMY off_addr_2: THE OBSERVATORIES, MADINGLEY ROAD off_city: CAMBRIDGE off_zip: CB3 0HA off_country: ENGLAND off_phone: (0223) 337548 ! end of coverpage abstract: line_1: We propose to obtain high S/N UV spectra to investigate the history of line_2: star formation in elliptical galaxies. These observations will provide line_3: an order of magnitude improvement in spectral signal-to-noise over that line_4: previously attainable with IUE. The data will also supplement and line_5: complement the limited set of elliptical-galaxy observations made in line_6: December 1990 with Astro-1. The HST spectra promise additional line_7: important constraints on the metallicity distribution and ages of the line_8: hot stellar component in these galaxies. ! ! end of abstract general_form_proposers: lname: FERGUSON fname: HENRY title: PI mi: C. inst: UNIVERSITY OF CAMBRIDGE, INSTITUTE OF ASTRONOMY country: ENGLAND esa: Y ! lname: WHITMORE fname: BRADLEY mi: C. inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! lname: BORNE fname: KIRK mi: D. inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! lname: BOHLIN fname: RALPH mi: C. inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! lname: DAVIDSEN fname: ARTHUR mi: F. inst: THE JOHNS HOPKINS UNIVERSITY country: USA ! lname: SPARKS fname: WILLIAM inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! lname: THOMSON fname: ROBERT mi: C. inst: UNIVERSITY OF CAMBRIDGE, INSTITUTE OF ASTRONOMY country: ENGLAND esa: Y ! lname: ZEPF fname: STEPHEN inst: PHYSICS DEPTARTMENT, UNIVERSITY OF DURHAM country: ENGLAND esa: Y ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: The FOS will be used with the G270H grating and 1" X 1" aperture to obtain line_2: spectra in the region 2200 - 3300 A (i.e., dominated by intermediate age line_3: stars). Absorption lines of interest lie at 2650, 2850, and 3050 A. The line_4: signal-to-noise ratios will range from 7 - 10 per A when possible. line_5: The FOS will also be used with the G190H grating to cover the region line_6: 1600 - 2300 A, where IUE spectra of ellipticals show considerable variety, line_7: and where the 2200 A interstellar absorption feature may be evident. line_8: Here is a summary of the proposed observations. The fluxes either line_9: estimated or measured in the IUE aperture are listed first, followed by line_10: exposure times computed to give S/N of 7-10 per A for spectra line_11: within a 3" diameter circle for imaging. line_12: NGC 1399 NGC 3610 line_13: F(1400) 11.0 e-15 1.7 e-15 line_14: F(2700) 4.4 e-15 5.6 e-15 line_15: FOS G130H 180M 180M line_16: FOS G190H 90M 120M line_17: FOS G270H 60M 60M line_19: NOTE: STScI HAS MODIFIED THIS PROPOSAL WITH THE ADDITION OF NEW ACQ/PEAKs line_20: BEFORE EACH FOS/BL SEGMENT DUE TO NEW SIDE-SWITCHING RULES. (THE SIDE SWITCH line_21: WAS ALLOWABLE AS ORIGINALLY SUBMITTED AT THE TIME OF SUBMISSION.) ALSO, SEQ line_22: NO GAP SPECIAL REQUIREMENTS HAVE BEEN RELAXED TO SEQ WITHIN 36 HOURS BY STSCI line_23: SINCE THE SEQUENCES ARE TOO LONG TO FIT WITHIN NON-SAA IMPACTED ORBITS. ! question: 4 section: 1 line_1: The UV spectra will provide the ability to: 1) constrain the number of line_2: massive O and B stars from strengths of the CIV and Si absorption line_3: features 2) determine the number of intermediate-age stars, both from line_4: the level and shape of the continuum, and from various absorption lines line_5: 3) constrain the metallicity of the near-UV component from the line_6: strengths of absorption features such as the iron-line blends near 2400 line_7: A, 2600 A and 3000 A, the MgII doublet at 2800 A, and the MgI line at line_8: 2852 A, and 4) discriminate between the different theories for the line_9: origin of the far-UV flux (i.e., star formation, PAGB stars, hot line_10: horizontal branch stars, or accreting white dwarfs). line_11: Observations of NGC 1399 have also been made using the Hopkins line_12: Ultraviolet Telescope (Ferguson et al. 1991) and with IUE. ! question: 5 section: 1 line_1: S/N REQUIREMENTS: line_3: Spectra: line_4: S/N = 7 - 10 per Angstrom. This will be sufficient for detailed line_5: spectral synthesis. line_7: Minimum and maximum exposure times: line_8: 1200 s (20 m) is used as the minimum, even if the resulting S/N is line_9: greater than required; since the overhead begins to dominate anyway. line_10: For the maximum we have used 14400 s (4 hr). line_11: Assumptions: line_12: To ensure that we reach our desired S/N, we have made fairly line_13: conservative assumptions about the UV flux from the targets with the line_14: spectrograph apertures. Specifically, we have assumed that the UV line_15: profile follows the optical profile, and have used optical surface line_16: photometry (from the literature and from our own unpublished data) to line_17: compute the ratio of the flux in the FOS aperture to the flux in the line_18: IUE aperture. This is a conservative assumption because the optical line_19: profiles are affected by seeing, and because the UV is likely to be line_20: more centrally peaked. However, this is countered by the fact that some line_21: of the light is lost from the aperture due to the HST spherical line_22: abberation. For NGC3610 we have assumed a UV upturn similar to that in line_23: NGC3379. ! question: 5 section: 2 line_1: GENERAL DEFINITIONS: line_3: s = count rate per Angstrom (A) per second line_4: source through = fraction of the IUE flux expected in the smaller line_5: HST apertures line_6: F = flux in ergs / cm **2 / s / A line_7: eff = efficiency of grating (or filter) and detector line_8: wave = wavelength line_9: d = dark count line_10: t = exposure time line_12: EXAMPLE OF TYPICAL CALCULATION: line_13: FOS line_14: formula: (based on eq. 1, p. 56 of handbook, but per A instead of line_15: diode, and correcting for source throughput) line_17: s = 2.28 e12 X F X wave X eff X source through line_19: if> F = 1.0 e-15 line_20: wave = 2700 A line_21: eff = 0.052 (p. 10 of handbook) line_22: source through = 0.045 line_23: d = 0.0027 per diode, or .0013 per A ! question: 5 section: 3 line_1: s = 0.0144 ct/sec/A line_3: S/N = [ s * t * (s/d) / ((s/d) + 1) ] ** 1/2 line_4: = 7.9 per A (for exp. time =4800 s) ! question: 6 section: 1 line_1: Not applicable. ! question: 7 section: 1 line_1: Data will be reduced using the STSDAS standard packages in STSDAS. A line_2: spectral synthesis program being used for analysis of the HUT data will line_3: be used to analyze the HST spectra. This program uses the "isochrone line_4: synthesis" technique of Charlot and Bruzual (1990), and incorporates line_5: state-of-the art evolutionary tracks for massive stars from Maeder and line_6: Meynet (1988) and PAGB tracks from Schoenberner (1981, 1983). Model line_7: spectra are constructed using either real IUE stellar spectra or Kurucz line_8: model atmospheres. The program is entirely table driven, and several line_9: technical improvements in the input data are expected by the time the line_10: HST observations are available. In particular, evolutionary tracks line_11: using new opacities are likely to be available, as are tracks for line_12: metal-rich extreme HB stars (Pinsonneault, private communication). line_13: Kurucz (1991) models with a resolution of 10 A covering a wide range of line_14: gravities, temperatures, and abundances will also be available, line_15: allowing us to overcome the limitation of empirical stellar libraries line_16: for stars with near-solar abundances. In fitting model spectra to the line_17: data, we will make extensive use of the nonlinear least-squares fitting line_18: rogram 'specfit' now running under IRAF at Johns Hopkins and at line_19: Cambridge. line_21: A rough division of responsibilities is as follows: HF is responsible line_22: for coordinating the overall effort, performing standard reductions of line_23: ,spectra, and developing synthesis models for each galaxy; BW will ! question: 7 section: 2 line_1: perform spectral reconstructions based on latest STScI expertise and line_2: search HST archives for relevant ancillary information (e.g., UV line_3: spectra of stars in order to build up a library for spectral synthesis, line_4: UV spectra of other ellipticals for comparison sample, etc.); RB will line_5: provide expertise on optimizing the observations with the FOS, and will line_6: provide the IUE stellar spectral library and relevant FOS spectra; KB line_7: will modify his existing N-body code to include gasseous dissipation line_8: and star formation and will use the code to help interpret data, line_9: especially for the ellipticals that show evidence of recent line_10: interactions; SZ will provide ground-based data in support of the HST line_11: observations; AFD will provide expertise on FOS and HUT. ! question: 8 section: 1 line_1: The GASP system will be used to determine better target coordinates during line_2: phase II. ! question: 9 section: 1 line_1: Bohlin and Davidsen are on the FOS GTO team; Sparks is affiliated with line_2: the FOC GTO team. Observations for these teams are listed in documents line_3: readily available. Observations possibly relevant to this proposal line_4: include: line_6: 1034 - "M87'S JET, NUCLEUS, AND HOT CORONA (FOS NO. 12): CYCLE 0 line_7: OBSERVATIONS" line_8: 1038 - "IMAGING AND SPECTROPHOTOMETRY OF NUCLEAR ACTIVITY IN LINERS line_9: 1041 - "THE NUCLEUS OF NORMAL AND STARBURST GALAXIES (FOS 20): CYCLE 0 line_10: 1044 - "STELLAR AND GAS DYNAMICS IN NORMAL GALAXIES (FOS 24): CYCLE 0 line_11: 3105 - "UV IMAGING OF M31-GROUP GALAXIES " line_12: 2266 - "POST ASYMPTOTIC GIANT BRANCH EVOLUTION IN THE MAGELLANIC line_13: CLOUDS. " ! question: 10 section: 1 line_1: HF is funded by an SERC rolling grant for observational astronomy, line_2: through September 1992, with the possibility of extension to 1993. line_3: Computing facilities at Cambridge include four SUN-4 computers line_4: dedicated to HST projects, with a total of 4 Gigabytes of disk storage, line_5: and an exabyte cartridge tape system for off-line storage. Each SUN has line_6: at least 24 Mb of core memory and a i860 array processors have recently line_7: been installed to speed up image deconvolutions. An extensive line_8: suite of software is installed on the SUNs, including IRAF, STSDAS, line_9: FIGARO, VISTA, and MEMSYS5. These systems are maintained by an in-house line_10: support staff funded by STARLINK. line_11: Resources at STScI are, of course, designed to support reduction line_12: Analysis of HST data. The budget being submitted with this proposal line_13: will provide the additional support necessary. ! !end of general form text general_form_address: lname: FERGUSON fname: HENRY mi: C. category: PI inst: UNIVERSITY OF CAMBRIDGE, INSTITUTE OF ASTRONOMY addr_1: THE OBSERVATORIES, MADINGLEY ROAD city: CAMBRIDGE zip: CB3 0HA country: ENGLAND phone: (0223) 337548 telex: 817297 ASTRON G ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: NGC1399 name_2: ESO358-45 name_3: PGC13418 descr_1: E, 303, 309 pos_1: RA = 03H 38M 29.0S +/- 0.1S, pos_2: DEC = -35D 27' 00" +/- 2" equinox: 2000 rv_or_z: V = 1447 comment_1: FLUXES ARE ESTIMATED USING IUE AND comment_2: OPTICAL DATA APJS 64,601; AJ 98,538 comment_3: APJ 328, 440. FLUX1 = V TOTAL. comment_4: FLUXES 4-7 ARE ESTIMATES IN A 1" comment_5: SQUARE APERTURE, OBTAINED BY comment_6: SCALING IUE DATA BY OPTICAL comment_7: SURFACE BRIGHTNESS PROFILE. comment_8: 2700A FLUX IS FROM NGC4649. comment_9: UNCERTAINTIES ARE PROBABLY ~50%. fluxnum_1: 1 fluxval_1: V = 9.56 fluxnum_2: 2 fluxval_2: B-V = 0.99 fluxnum_3: 3 fluxval_3: E(B-V) = 0.0 fluxnum_4: 4 fluxval_4: V = 15.90 fluxnum_5: 5 fluxval_5: F-CONT(1500) = 3.0 E-15 fluxnum_6: 6 fluxval_6: F-CONT(1900) = 4.7 E-16 fluxnum_7: 7 fluxval_7: F-CONT(2700) = 1.1 E-16 ! targnum: 2 name_1: NGC3610 name_2: UGC6319 name_3: PGC34566 descr_1: E, 303, 320 pos_1: RA = 11H 18M 25.2S +/- 0.1S, pos_2: DEC = +58D 47' 10.4" +/- 1" equinox: 2000 rv_or_z: V = 1787 comment_1: FLUXES ARE ESTIMATED USING IUE AND comment_2: OPTICAL DATA APJS 64,601; R BAND comment_3: CCD IMAGE; APJ 328, 440; LONGO AND comment_4: DEVAUC. TEXAS MONOGRAPH. FLUX1 = V comment_5: TOTAL; FLUXES 4-7 ARE ESTIMATES IN comment_6: 1" SQ. APERTURE, FROM SCALING IUE comment_7: DATA BY OPTICAL SB PROF. 1500A AND comment_8: 1900A ARE FROM NGC4742; 2700A FROM comment_9: NGC2681 (X .787). UNCERTAIN BY comment_10: FACTORS OF 2 (2700A) TO 10 (1500A) fluxnum_1: 1 fluxval_1: V = 10.90 fluxnum_2: 2 fluxval_2: B-V = 0.82 fluxnum_3: 3 fluxval_3: E(B-V) = 0.0 fluxnum_4: 4 fluxval_4: V = 15.82 fluxnum_5: 5 fluxval_5: F-CONT(1500) = 1.3 E-16 fluxnum_6: 6 fluxval_6: F-CONT(1900) = 1.3 E-16 fluxnum_7: 7 fluxval_7: F-CONT(2700) = 2.3 E-16 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: NGC1399 config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 35S s_to_n: 20 fluxnum_1: 4 priority: 1 param_1: TYPE = UP, param_2: SCAN-STEP=0.7, param_3: SEARCH-SIZE=4 req_1: ONBOARD ACQ FOR 2-3; req_2: SEQ 1-4 WITHIN 36 H; req_3: CYCLE 2 / 1-8; comment_1: WANT TO MAXIMIZE S/N, SO DO A COARSE comment_2: PEAKUP TO GET WITHIN ABOUT 0.35" OF comment_3: BRIGHTEST SPOT. ALTHOUGH NUCLEUS PER comment_4: SE IS NOT THE TARGET, WE WISH ALL OBS comment_5: FOR BOTH SIDES TO BE TAKEN WITH SAME comment_6: POINTING. STSCI SAYS NOT POSSIBLE. ! linenum: 2.000 targname: NGC1399 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G190H num_exp: 1 time_per_exp: 5284.2S s_to_n: 11 fluxnum_1: 6 priority: 1 comment_1: S/N IS MEAN PER ANGSTROM. comment_2: IT MIGHT MAKE SENSE TO SCHEDULE comment_3: THE NGC1399 OBSERVATIONS comment_4: AFTER THOSE FOR PROPOSAL 3728 comment_5: (FOC IMAGING OBSERVATIONS.) comment_6: THIS IS NOT A REQUIREMENT, THOUGH. ! linenum: 3.000 targname: NGC1399 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G270H num_exp: 1 time_per_exp: 3542.4S s_to_n: 15 fluxnum_1: 7 priority: 1 comment_1: S/N IS MEAN PER ANGSTROM. ! linenum: 3.500 targname: NGC1399 config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 70S fluxnum_1: 4 priority: 1 param_1: TYPE = UP, param_2: SCAN-STEP=0.7, param_3: SEARCH-SIZE=4 req_1: ONBOARD ACQ FOR 4; comment_1: FOS/BL ACQ/PEAK ADDED BY STSCI DUE TO comment_2: NEW OPERATING RULES FOR SINGLE-SIDE comment_3: ACQS. POINTING WILL BE SPLIT FROM RED comment_4: SIDE POINTING BY SAA PASSAGE, SO THE comment_5: POINTING FOR THE FOS/BL OBS CANNOT BE comment_6: GUARANTEED TO BE SAME AS FOR FOS/RD. ! linenum: 4.000 targname: NGC1399 config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G130H num_exp: 1 time_per_exp: 10453.2S s_to_n: 8 fluxnum_1: 5 priority: 1 comment_1: S/N IS MEAN PER ANGSTROM. comment_2: ESPECIALLY PREFER DARK TIME comment_3: FOR THIS OBSERVATION. THIS comment_4: IS NOT A REQUIREMENT BUT A comment_5: PREFERENCE. ! linenum: 5.000 targname: NGC3610 config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 30S s_to_n: 20 fluxnum_1: 4 priority: 1 param_1: TYPE = UP, param_2: SCAN-STEP=0.7, param_3: SEARCH-SIZE=4 req_1: ONBOARD ACQ FOR 6-7; req_2: SEQ 5-8 WITHIN 36 H; comment_1: WANT TO MAXIMIZE S/N, SO DO A COARSE comment_2: PEAKUP TO GET WITHIN ABOUT 0.35" OF comment_3: BRIGHTEST SPOT. ALTHOUGH NUCLEUS PER comment_4: SE IS NOT THE TARGET, WE WISH ALL OBS comment_5: FOR BOTH SIDES TO BE TAKEN WITH SAME comment_6: POINTING. STSCI SAYS NOT POSSIBLE. ! linenum: 6.000 targname: NGC3610 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G190H num_exp: 1 time_per_exp: 5835.6S s_to_n: 10 fluxnum_1: 6 priority: 1 comment_1: S/N IS MEAN PER ANGSTROM. ! linenum: 7.000 targname: NGC3610 config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G270H num_exp: 1 time_per_exp: 3531.6S s_to_n: 20 fluxnum_1: 7 priority: 1 comment_1: S/N IS MEAN PER ANGSTROM. ! linenum: 7.500 targname: NGC3610 config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 60S fluxnum_1: 4 priority: 1 param_1: TYPE=UP, param_2: SCAN-STEP=0.7, param_3: SEARCH-SIZE=4 req_1: ONBOARD ACQ FOR 8; comment_1: FOS/BL ACQ/PEAK ADDED BY STSCI DUE TO comment_2: NEW OPERATING RULES FOR SINGLE-SIDE comment_3: ACQS. POINTING WILL BE SPLIT FROM RED comment_4: SIDE POINTING BY SAA PASSAGE, SO THE comment_5: POINTING FOR THE FOS/BL OBS CANNOT BE comment_6: GUARANTEED TO BE SAME AS FOR FOS/RD. ! linenum: 8.000 targname: NGC3610 config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G130H num_exp: 1 time_per_exp: 10453.2S s_to_n: 4 fluxnum_1: 5 priority: 1 comment_1: S/N IS MEAN PER ANGSTROM. comment_2: FLUX IS VERY UNCERTAIN ! ! end of exposure logsheet ! No scan data records found