! File: 3797C.PROP ! Database: PEPDB ! Date: 19-FEB-1994:19:49:48 coverpage: title_1: WFC IMAGING OF FAINT BLUE GALAXIES sci_cat: GALAXIES & CLUSTERS sci_subcat: GALAXY MORPHOLOGY proposal_for: GO pi_fname: DAVID pi_mi: C pi_lname: KOO pi_inst: LICK OBSERVATORY, UNIVERSITY OF CALIFORNIA, SANTA CRUZ pi_country: USA pi_phone: 408-459-2130 hours_pri: 5.61 num_pri: 7 wf_pc: Y funds_amount: 54914 funds_length: 12 ! end of coverpage abstract: line_1: We propose a pilot program of 5.6 hours of WFC imaging to study the line_2: structure of 7 faint (B=21 to 22) compact galaxies at redshifts z line_3: from 0.1 to 0.35. These galaxies are important as possible links to line_4: three puzzles that may be intimately related: the nature of very line_5: faint, very blue galaxies; the rate of close-encounter merging of line_6: field galaxies as a function of look-back time; and the connection line_7: between starbursts and "weak" AGN. The sub-arcsec morphology from HST line_8: will be correlated with existing ground-based spectroscopy, multi-band line_9: color photometry, long-term variability information, and similar data for line_10: neighboring galaxies. As a bonus, the structure of galaxy neighbors line_11: close enough to be within the WFC field will be measured. The line_12: feasibility of our proposal was verified in SAO 3121 (The Ability of HST line_13: to Do Morphology of Medium Redshift Galaxies). ! ! end of abstract general_form_proposers: lname: KOO fname: DAVID title: PI mi: C inst: LICK OBSERVATORY, UNIV OF CALIFORNIA, SANTA CRUZ country: USA ! lname: BERSHADY fname: MATTHEW mi: A inst: DEPT OF ASTRONOMY AND ASTROPHYSICS, UNIV OF CHICAGO country: USA ! lname: MAJEWSKI fname: STEVEN mi: R inst: OBSERVATORIES OF THE CARNEGIE INSTITUTION OF WASHINGTON country: USA ! lname: SMETANKA fname: JOHN mi: J inst: DEPT OF ASTRONOMY AND ASTROPHYSICS, UNIV OF CHICAGO country: USA ! lname: STANFORD fname: S ADAM inst: DEPT OF ASTRONOMY, UNIV OF CALIFORNIA, BERKELEY country: USA ! lname: WIRTH fname: GREGORY mi: D inst: DEPT ASTRON AND ASTROPHYSICS, UNIV OF CALIFORNIA, SANTA CRUZ country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We propose to take a pair of exposures with F555W of the WFC of 7 CNELG line_2: targets (Table 1.) These are among the brightest CNELG that are also at line_3: moderate redshifts where many blue galaxies have already been found in clusters line_4: and the field. The requested exposures (Table 1) have been adjusted by the line_5: integrated brightness, though the relevant parameter is surface brightness per line_6: pixel of the WFC. line_7: Though already observed in the UV with the FOC (see Figure 1), Lynx2.11378 line_8: is being reobserved with the WFC and the redder F555W filter to check its line_9: colors and check whether there is evidence for dust being the cause of the line_10: double component. line_11: Ideally, the two exposures are offset by half-pixels so that improved line_12: sampling can be achieved. The F555W filter is chosen because of its high line_13: throughput and because we expect that the corresponding PSF (and its variation line_14: with time and position) will be among the best determined. The stars in the line_15: WFC can be used as independent checks of the PSF library (see Table 1.) As line_16: mentioned below, we fully intend to extract the maximum information possible by line_17: using computer- intensive deconvolutions. These deconvolutions work best when line_18: the PSF is well defined. line_19: Our targets all lie within 3 widely-separated fields (each roughly 1 line_20: degree in diameter) that have been well studied for distant QSO's, radio line_21: sources, cluster galaxies, and field galaxies by ourselves and others over the line_22: last 17 years. We emphasize that an important bonus of this proposal is that line_23: our WFC images will also be used to study the morphology of neighbors to the ! question: 3 section: 2 line_1: primary CNELG targets. ! question: 4 section: 1 line_1: EXISTING GROUND BASED SUPPORT: We currently have UBVI photometry for all fields line_2: surrounding our targets, with a 24th mag limit for 4-m photographic data and line_3: 26th or fainter for certain fields with extremely deep CCD images from Palomar line_4: 5m and KPNO 4m. Near-IR imaging already exists for some of our targets and line_5: will continue to completion probably by the end of HST data receipt. The line_6: spectroscopy is obviously complete for the CNELG targets, though we may attempt line_7: higher resolution or wider spectral coverage of the same targets in the future. line_8: We also estimate that redshifts exist for 20 to 30 neighboring galaxies, line_9: depending on exact placement of our CNELG targets in the WFC frame, of line_10: magnitude typically between B = 19 and 22. If HST observations are successful, line_11: additional Redshifts of remaining neighbors will be acquired from the ARC 3.5m, line_12: KPNO 4m, or Keck 10m. All of the fields within which our targets lie have also line_13: been observed in the radio (Kron et al. 1985) to mJy levels and some to much line_14: fainter limits; only two CNELG have been found among 80 radio sources with line_15: redshifts in our samples. line_16: SPACE SUPPORT: Part of our Lynx fields have also received recent deep line_17: ROSAT exposures (R. Windhorst as PI.) line_18: WHY HST?: The SAO 3121 experiment (see Figure 1) says it all: we need high line_19: spatial resolution which only HST can provide in a practical way at this time. ! question: 5 section: 1 line_1: To improve spatial sampling, we request one half pixel offsets (0.05 line_2: arcsec) in both of the primary orthogonal directions of the edge of the WFC line_3: chips between our two exposures for each target. line_4: NOTE: STScI has recommended that PCS MODE FINE be used for line_5: these observations, and this has been agreed to by the PI. line_6: However, the PI also says that although PCS MODE FINE is line_7: preferred, PCS MODE COARSE may be used on an exposure-by- line_8: exposure basis if problems are encountered in trying to line_9: schedule in PCS MODE FINE. ! question: 7 section: 1 line_1: We anticipate that the bulk of the data analysis will be completed at UCSC line_2: with assistance by a graduate student RA under Koo's supervision. IRAF/STSDAS line_3: is currently operational at Lick and will be used both for the routine image line_4: processing and also for preliminary deconvolution. To take full advantage of line_5: the data we expect to send a member of the team or an RA to STScI to make use line_6: of the MEMSYS3 maximum entropy deconvolution package. Because our goal is line_7: morphology rather than accurate photometry of compact blue objects, the line_8: analysis will be relatively straightforward. We will then correlate the line_9: morphological data with our extensive database of photometry and spectroscopy line_10: of these objects to hopefully form a coherent picture of their nature. ! question: 9 section: 1 line_1: GTO 1282 Morphology of Faint Galaxies (King is PI) Related: no data collected line_2: and CNELG had to be eliminated from target list line_4: GO 2684 Medium Deep Survey (Koo is co-I) Unrelated except for interest in line_5: morphology of distant galaxies (no data collected yet) line_7: SAO 3121 Morphology of Faint Galaxies (King was lone PI) Related ! question: 9 section: 2 line_1: SAO 3121: As seen in Figure 1, we easily resolved one of our CNELG. We also line_2: empirically checked that the morphology and structure of moderate redshift line_3: galaxies can be extracted from reasonable exposures using the FOC and WFC, i.e. line_4: HST can work on morphology of ordinary distant galaxies. ! question: 9 section: 3 line_1: SAO 3121: "The Current Ability of HST to Reveal Morphological Structure in line_2: Medium Redshift Galaxies," King, I.R., Stanford, S.A., Seitzer, P., Bershady, line_3: M.A., Keel, W.C., Koo, D.C., Weir, N., Djorgovski, S., and Windhorst, R.A. line_4: Astronomical Journal, 112, 1553, 1991. ! question: 10 section: 1 line_1: Lick Observatory and the Board of Astronomy and Astrophysics at the University line_2: of California, Santa Cruz now attract some of the top graduate students in the line_3: country. Our major competition remains Berkeley, CalTech, Chicago, Princeton, line_4: and the University of Arizona. Roughly 5 to 10 new students arrive each year. line_5: The PI will employ one graduate student at half a Research Assistantship to do line_6: the major initial data reductions and some of the deconvolutions. line_7: Lick has S. Faber (WF/PC GTO) and her group of WFPC experts; G. Illingworth line_8: is a co-I on working with the Medium Deep Survey (MDS) WF/PC data to study line_9: morphology of distant galaxies; and the PI was formerly the WF/PC Instrument line_10: Scientist at the STScI and is also a co-I on the MDS team with interest in line_11: distant galaxies. line_12: The theory group at UCSC is now very strong with the recent addition of L. line_13: Hernquist whose specialties include understanding the structure of colliding line_14: gas in the cores of galaxies. His gas-plus-star models are state-of-the-art and line_15: may be important to our understanding of the frequency and structures seen in line_16: our CNELG sample. line_17: The PI is building an near-IR imaging camera for the Lick 3m telescope. The line_18: camera is operational at this time and can reach K = 18 or fainter, which is line_19: sufficient to add near-IR data for any CNELG targets not already observed. line_20: Moreover, with the advent of the Keck 10m, additional high-spatial and line_21: high-spectral resolution work on our HST sample of CNELG can be secured if line_22: deemed important for the scientific interpretation. Our Chicago co-I's have line_23: access to the ARC 3.5m, due to begin operation within a year or so. ! !end of general form text general_form_address: lname: KOO fname: DAVID mi: C category: PI inst: LICK OBSERVATORY, UNIVERSITY OF CALIFORNIA, SANTA CRUZ addr_1: RM 461 NATURAL SCIENCES 2 addr_2: LICK OBSERVATORY addr_3: UNIVERSITY OF CALIFORNIA city: SANTA CRUZ state: CA zip: 95064 country: USA phone: (408) 459-2130 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: GAL-172116+500138 name_2: HERC1.13385 descr_1: E,307 pos_1: RA = 17H 20M 00.5S +/- 0.5", pos_2: DEC = +50D 04' 29" +/- 0.5" equinox: 1950 rv_or_z: Z = 0.10 fluxnum_1: 1 fluxval_1: V = 20.2 +/- .2 fluxnum_2: 2 fluxval_2: B-V = .3 +/- .2 ! targnum: 2 name_1: GAL-171908+494323 name_2: HERC1.3618 descr_1: E,307 pos_1: RA = 17H 17M 51.8S +/- 0.5", pos_2: DEC = +49D 46' 24" +/- 0.5" equinox: 1950 rv_or_z: Z = 0.13 fluxnum_1: 1 fluxval_1: V = 19.7 +/- .2 fluxnum_2: 2 fluxval_2: B-V = 1.0 +/- .2 ! targnum: 3 name_1: GAL-001723+160726 name_2: SA68.17255 descr_1: E,307 pos_1: RA = 00H 14M 47.8S +/- 0.5", pos_2: DEC = +15D 50' 46" +/- 0.5" equinox: 1950 rv_or_z: Z = 0.35 fluxnum_1: 1 fluxval_1: V = 19.8 +/- .2 fluxnum_2: 2 fluxval_2: B-V = 0.8 +/- .2 ! targnum: 4 name_1: GAL-001811+154754 name_2: SA68.6134 descr_1: E,307 pos_1: RA = 00H 15M 36.2S +/- 0.5", pos_2: DEC = +15D 31' 14" +/- 0.5" equinox: 1950 rv_or_z: Z = 0.29 fluxnum_1: 1 fluxval_1: V = 20.6 +/- .2 fluxnum_2: 2 fluxval_2: B-V = 0.6 +/- .2 ! targnum: 5 name_1: GAL-084519+444935 name_2: LYNX2.11378 descr_1: E,307 pos_1: RA = 08H 41M 54.1S +/- 0.5", pos_2: DEC = +45D 00' 31" +/- 0.5" equinox: 1950 rv_or_z: Z = 0.27 fluxnum_1: 1 fluxval_1: V = 20.2 +/- .2 fluxnum_2: 2 fluxval_2: B-V = 0.3 +/- .2 ! targnum: 6 name_1: GAL-084327+444009 name_2: LYNX2.8115 descr_1: E,307 pos_1: RA = 08H 40M 03.0S +/- 0.5", pos_2: DEC = +44D 50' 59" +/- 0.5" equinox: 1950 rv_or_z: Z = 0.20 fluxnum_1: 1 fluxval_1: V = 20.3 +/- .2 fluxnum_2: 2 fluxval_2: B-V = 0.3 +/- .2 ! targnum: 7 name_1: GAL-084426+444949 name_2: LYNX2.11500 descr_1: E,307 pos_1: RA = 08H 41M 02.1S +/- 0.5", pos_2: DEC = +45D 00' 42" +/- 0.5" equinox: 1950 rv_or_z: Z = 0.19 fluxnum_1: 1 fluxval_1: V = 20.4 +/- .2 fluxnum_2: 2 fluxval_2: B-V = 0.3 +/- .2 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.110 targname: GAL-172116+500138 config: WFC opmode: IMAGE aperture: WFALL sp_element: F555W num_exp: 1 time_per_exp: 20M fluxnum_1: 1 fluxnum_2: 2 priority: 1 param_1: CR-SPLIT=NO req_1: CYCLE 2 / 1.11; req_2: GROUP 1.11 , 1.12 NO GAP; req_3: PCS MODE F; comment_1: PCS MODE FINE PREFERRED, BUT comment_2: PCS MODE COARSE MAY BE USED comment_3: ON EXPOSURE-BY-EXPOSURE BASIS comment_4: IF NEEDED. ! linenum: 1.120 targname: GAL-172116+500138 config: WFC opmode: IMAGE aperture: WFALL sp_element: F555W num_exp: 1 time_per_exp: 20M fluxnum_1: 1 fluxnum_2: 2 priority: 1 param_1: CR-SPLIT=NO req_1: CYCLE 2 / 1.12; req_2: POS TARG .05 , .05; req_3: PCS MODE F; comment_1: PCS MODE FINE PREFERRED, BUT comment_2: PCS MODE COARSE MAY BE USED comment_3: ON EXPOSURE-BY-EXPOSURE BASIS comment_4: IF NEEDED. ! linenum: 1.210 targname: GAL-171908+494323 config: WFC opmode: IMAGE aperture: WFALL sp_element: F555W num_exp: 1 time_per_exp: 1600S fluxnum_1: 1 fluxnum_2: 2 priority: 1 param_1: CR-SPLIT=NO req_1: CYCLE 2 / 1.21 ; req_2: GROUP 1.21 , 1.22 NO GAP; req_3: PCS MODE F; comment_1: PCS MODE FINE PREFERRED, BUT comment_2: PCS MODE COARSE MAY BE USED comment_3: ON EXPOSURE-BY-EXPOSURE BASIS comment_4: IF NEEDED. ! linenum: 1.220 targname: GAL-171908+494323 config: WFC opmode: IMAGE aperture: WFALL sp_element: F555W num_exp: 1 time_per_exp: 1600S fluxnum_1: 1 fluxnum_2: 2 priority: 1 param_1: CR-SPLIT=NO req_1: CYCLE 2 / 1.22; req_2: POS TARG .05 , .05; req_3: PCS MODE F; comment_1: PCS MODE FINE PREFERRED, BUT comment_2: PCS MODE COARSE MAY BE USED comment_3: ON EXPOSURE-BY-EXPOSURE BASIS comment_4: IF NEEEDED. ! linenum: 2.110 targname: GAL-001723+160726 config: WFC opmode: IMAGE aperture: WFALL sp_element: F555W num_exp: 1 time_per_exp: 20M fluxnum_1: 1 fluxnum_2: 2 priority: 2 param_1: CR-SPLIT=NO req_1: CYCLE 2 / 2.11; req_2: GROUP 2.11 , 2.12 NO GAP; req_3: PCS MODE F; comment_1: PCS MODE FINE PREFERRED, BUT comment_2: PCS MODE COARSE MAY BE USED comment_3: ON EXPOSURE-BY-EXPOSURE BASIS comment_4: IF NEEDED. ! linenum: 2.120 targname: GAL-001723+160726 config: WFC opmode: IMAGE aperture: WFALL sp_element: F555W num_exp: 1 time_per_exp: 20M fluxnum_1: 1 fluxnum_2: 2 priority: 2 param_1: CR-SPLIT=NO req_1: CYCLE 2 / 2.12; req_2: POS TARG .05 , .05; req_3: PCS MODE F; comment_1: PCS MODE FINE PREFERRED, BUT comment_2: PCS MODE COARSE MAY BE USED comment_3: ON EXPOSURE-BY-EXPOSURE BASIS comment_4: IF NEEDED. ! linenum: 2.210 targname: GAL-001811+154754 config: WFC opmode: IMAGE aperture: WFALL sp_element: F555W num_exp: 1 time_per_exp: 1700S fluxnum_1: 1 fluxnum_2: 2 priority: 2 param_1: CR-SPLIT=NO req_1: CYCLE 2 / 2.21; req_2: GROUP 2.21 , 2.22 NO GAP; req_3: PCS MODE F; comment_1: PCS MODE FINE PREFERRED, BUT comment_2: PCS MODE COARSE MAY BE USED comment_3: ON EXPOSURE-BY-EXPOSURE BASIS comment_4: IF NEEDED. ! linenum: 2.220 targname: GAL-001811+154754 config: WFC opmode: IMAGE aperture: WFALL sp_element: F555W num_exp: 1 time_per_exp: 1700S fluxnum_1: 1 fluxnum_2: 2 priority: 2 param_1: CR-SPLIT=NO req_1: CYCLE 2 / 2.22; req_2: POS TARG .05 , .05; req_3: PCS MODE F; comment_1: PCS MODE FINE PREFERRED, BUT comment_2: PCS MODE COARSE MAY BE USED comment_3: ON EXPOSURE-BY-EXPOSURE BASIS comment_4: IF NEEDED. ! linenum: 3.110 targname: GAL-084519+444935 config: WFC opmode: IMAGE aperture: WFALL sp_element: F555W num_exp: 1 time_per_exp: 1600S fluxnum_1: 1 fluxnum_2: 2 priority: 3 param_1: CR-SPLIT=NO req_1: CYCLE 2 / 3.11; req_2: GROUP 3.11 , 3.12 NO GAP; req_3: PCS MODE F; comment_1: PCS MODE FINE PREFERRED, BUT comment_2: PCS MODE COARSE MAY BE USED comment_3: ON EXPOSURE-BY-EXPOSURE BASIS comment_4: IF NEEDED. ! linenum: 3.120 targname: GAL-084519+444935 config: WFC opmode: IMAGE aperture: WFALL sp_element: F555W num_exp: 1 time_per_exp: 1600S fluxnum_1: 1 fluxnum_2: 2 priority: 3 param_1: CR-SPLIT=NO req_1: CYCLE 2 / 3.12; req_2: POS TARG .05 , .05; req_3: PCS MODE F; comment_1: PCS MODE FINE PREFERRED, BUT comment_2: PCS MODE COARSE MAY BE USED comment_3: ON EXPOSURE-BY-EXPOSURE BASIS comment_4: IF NEEDED. ! linenum: 3.210 targname: GAL-084327+444009 config: WFC opmode: IMAGE aperture: WFALL sp_element: F555W num_exp: 1 time_per_exp: 20M fluxnum_1: 1 fluxnum_2: 2 priority: 3 param_1: CR-SPLIT=NO req_1: CYCLE 2 / 3.21; req_2: GROUP 3.21 , 3.22 NO GAP; req_3: PCS MODE F; comment_1: PCS MODE FINE PREFERRED, BUT comment_2: PCS MODE COARSE MAY BE USED comment_3: ON EXPOSURE-BY-EXPOSURE BASIS comment_4: IF NEEDED. ! linenum: 3.220 targname: GAL-084327+444009 config: WFC opmode: IMAGE aperture: WFALL sp_element: F555W num_exp: 1 time_per_exp: 20M fluxnum_1: 1 fluxnum_2: 2 priority: 3 param_1: CR-SPLIT=NO req_1: CYCLE 2 / 3.22; req_2: POS TARG .05 , .05; req_3: PCS MODE F; comment_1: PCS MODE FINE PREFERRED, BUT comment_2: PCS MODE COARSE MAY BE USED comment_3: ON EXPOSURE-BY-EXPOSURE BASIS comment_4: IF NEEDED. ! linenum: 3.310 targname: GAL-084426+444949 config: WFC opmode: IMAGE aperture: WFALL sp_element: F555W num_exp: 1 time_per_exp: 1600S fluxnum_1: 1 fluxnum_2: 2 priority: 3 param_1: CR-SPLIT=NO req_1: CYCLE 2 / 3.31; req_2: GROUP 3.31 , 3.32 NO GAP; req_3: PCS MODE F; comment_1: PCS MODE FINE PREFERRED, BUT comment_2: PCS MODE COARSE MAY BE USED comment_3: ON EXPOSURE-BY-EXPOSURE BASIS comment_4: IF NEEDED. ! linenum: 3.320 targname: GAL-084426+444949 config: WFC opmode: IMAGE aperture: WFALL sp_element: F555W num_exp: 1 time_per_exp: 1600S fluxnum_1: 1 fluxnum_2: 2 priority: 3 param_1: CR-SPLIT=NO req_1: CYCLE 2 / 3.32; req_2: POS TARG .05 , .05; req_3: PCS MODE F; comment_1: PCS MODE FINE PREFERRED, BUT comment_2: PCS MODE COARSE MAY BE USED comment_3: ON EXPOSURE-BY-EXPOSURE BASIS comment_4: IF NEEDED. ! ! end of exposure logsheet ! No scan data records found