! $Id: 5399,v 59.1 1994/07/27 17:33:05 pepsa Exp $ coverpage: title_1: ULTRADEEP HST IMAGING OF THE HAWAII DEEP SURVEY FIELDS sci_cat: GALAXIES & CLUSTERS sci_subcat: SURVEYS proposal_for: GO pi_fname: LENNOX pi_lname: COWIE pi_inst: INSTITUTE FOR ASTRONOMY,UNIVERSITY OF HAWAII pi_country: USA pi_phone: 808-956-8134 hours_pri: 12.00 num_pri: 2 wf_pc: Y off_fname: PETER off_lname: GARROD off_title: DIRECTOR OF RESEARCH off_inst: UNIVERSITY OF HAWAII off_addr_1: OFFICE OF RESEARCH ADMINISTRATION off_addr_2: 2540 MAILE WAY off_addr_3: SPALDING 255 off_city: HONOLULU off_state: HI off_zip: 96822 off_country: USA off_phone: (808) 956-8612 ! end of coverpage abstract: line_1: Detailed morphological classification of galaxies at high line_2: redshifts requires angular resolution of around 0.1" FWHM line_3: and cannot be carried out from the ground. We propose to line_4: use the WFPC2 to observe the Hawaii deep survey fields SSA13 line_5: and SSA22 in the wide I band. These 2' x 2' fields have been line_6: observed at wavelengths 2200A (HST cycle 1),3400A,4500A,8400A line_7: and 2.1 micron to 5 sigma galaxy detection limits of a microJy line_8: or below (K=22, V=27). All galaxies with B<24 and K<19 now line_9: have determined redshifts and have been typed on the basis of line_10: their spectra as have 65 percent of the galaxies between line_11: K=19-20. SSA13 is a candidate field for the Japan-Hawaii ISO line_12: deep survey which will be the deepest 10 micron observation line_13: carried out with the ISO satellite. The proposed WFPC2 line_14: observations will be used to type the K<20 galaxy sample and line_15: to study the evolution of the galaxy type mix, surface line_16: brightness profiles, and merger rate as a function of absolute line_17: magnitude and redshift. line_18: The program was accepted in Cycle 1 for both wide band WFPC line_19: and 2200A FOC observations. After the discovery of the aberration line_20: the allocated time was concentrated into the 2200A FOC studies. ! ! end of abstract general_form_proposers: lname: COWIE fname: LENNOX inst: 2192 country: USA ! lname: HU fname: ESTHER inst: 2192 country: USA ! lname: SONGAILA fname: ANTOINETTE inst: 2192 country: USA ! lname: KORMENDY fname: JOHN inst: 2192 country: USA ! lname: CHAMBERS fname: KENNETH inst: 2192 country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: A total of six hours of on-target time through the wide I line_2: filter (F814W) is required for each of the two fields line_3: (SSA13 and SSA22). The fields should be centered on the line_4: geometric center of the four CCD chips and oriented so that line_5: the N-S direction lies parallel to the chip edges to optimise line_6: the field coverage. The preferred orientation is with the PC line_7: at the NE but this is not essential. The observations of SSA22 line_8: are broken into two groups of six 2400 second exposures each. line_9: The observations of SSA13 are broken into a single group of line_10: six 2600 second exposures each, with the individual exposure line_11: time being set by the read noise on the PC. Any significant line_12: reduction below these times would impact the noise on the PC line_13: portion of the field. Each of the six exposures should be line_14: spatially separated from the others to allow the use of median line_15: techniques, and we have specified a dithering pattern using line_16: 5 arcsec offsets to achieve this. In order to fully optimise line_17: this we also require that the exposures be obtained sequentially. line_18: Because of the multiple exposures we do not require CR-SPLIT. line_19: In order to optimise the scheduling, all exposures _must_ be line_20: identical and a minimum of _five_ individual exposures is required. ! question: 4 section: 1 line_1: (a) The resolution necessary to carry out this program line_2: cannot currently be achieved from the ground. The highest line_3: angular resolution images we have obtained from the ground line_4: (FWHM approx. 0.5 arcsec) are not good enough to achieve line_5: the program goals even with the use of image restoration line_6: techniques. Ultradeep ground- and space-based imaging has line_7: been carried out at 2200 A (HST Cycle 1), 3400 A, 4500 A, line_8: 5500 A, 8400 A, and 21,000 A and in the soft x-rays (ROSAT line_9: 50,000 sec exposures). All K < 20 and B < 24 galaxies in line_10: the fields have been observed spectroscopically, and complete line_11: redshift samples and spectroscopic types have been obtained line_12: for all K < 19 nd B < 24 galaxies, and for 65 percent of the line_13: K = 19 - 20 sample. We will attempt to complete the K = 20 line_14: sample with allocated time on the Keck 10-meter telescope. line_16: (b) For a 'typical' I = 23 galaxy, the central surface line_17: brightness in a wide-field pixel is 27, and the measured line_18: typical value at 1 arcsec approximately I = 29 in a WFC line_19: pixel. The latter value produces a count rate of line_20: 1.0 x 10-2 e/s/pixel through the F814W filter. By comparison, line_21: the sky background at the field ecliptic latitudes is line_22: I = 27.2 per WFC pixel, giving 4 x 10-2 e/s/pixel. Assuming line_23: 1800s sub-exposures to provide clean cosmic-ray rejection and ! question: 4 section: 2 line_1: sky cleaning, and 7e/pixel read noise, the sky dominated line_2: noise/exposure/pixel becomes 11e and the S/N = 1.4 in 0.5 line_3: hrs. Requiring S/N = 5/pixel then implies a six-hour exposure. line_4: Simulations made using the ground-based observations of line_5: Figure 2, faded and shrunk as they would appear at the line_6: appropriate redshifts, show that this S/N should be adequate line_7: for classification. The proposed WFPC2 observations for the line_8: I < 23 galaxies should in fact be very similar in S/N and line_9: resolution to the galaxies shown in Figure 2. We request line_10: observations on two fields since each field is dominated by line_11: a small number of velocity groupings because of clustering line_12: effects. The WFC regions contain 34 galaxies at K < 20 in line_13: the two fields, 31 of which have I magnitudes less than 23 line_14: and should be classifiable. This sample size should be large line_15: enough to discern gross trends in the type mix and surface line_16: brightness profiles and to determine if there is enhanced line_17: merger activity in the high z population. ! question: 5 section: 1 line_1: Not applicable. ! question: 6 section: 1 line_1: Not applicable. ! ! question: 8 section: 1 line_1: Not applicable. ! question: 9 section: 1 line_1: (a) line_2: P2365 'HST Images of Ground-Based Deep Survey Fields', line_3: L. L. Cowie, S. J. Lilly line_4: P2403 'Hot Gas in the ISM', L. L. Cowie, E. B. Jenkins, line_5: A. Songaila line_6: P3543 'The Deep Ultraviolet Sky', S. J. Lilly, L. L. line_7: Cowie, E. M. Hu line_9: (b) The present program was originally approved in P2365 of line_10: Cycle 1. When the aberration was discovered, the deep high- line_11: resolution WFPC imaging was dropped and 2200 A imaging with line_12: the FOC was emphasised. P3543 provided 2200 A imaging of a line_13: further field, but because of the f/48 FOC problem, no data line_14: have been obtained. line_16: (c) Data were obtained only in the last year and are still line_17: being analyzed for P2365. Data are fully analyzed for P2403 line_18: and a paper is currently being prepared for publication line_19: describing the distribution and origin of high ionization line_20: species in the galactic disk (J. S. Huang, A. Songaila, L. L. line_21: Cowie and E. B. Jenkins). ! question: 10 section: 1 line_1: The analysis will be carried out using an existing Sparc 10 line_2: workstaion, including exabyte and CD ROM dirves, plus 2.1 line_3: Gbytes of disk and 96 Mbytes of RAM. Photographic images will line_4: be prepared using the Institute for Astronomy's (IFA) high line_5: resoltion Solitaire film writer. Additional spectrographic line_6: follow-up to complete redshift identification to K = 20 will line_7: be carried out using University of Hawaii time on the Keck line_8: 10-meter telescope. Extension line_9: of the bright-end K = 15 galaxy sample to 16 will be carried line_10: out by J. S. Huang as his Ph. D. thesis, using the University line_11: of Hawaii's 24-inch and 88-inch telescopes and NICMOS3 and line_12: Tek 2048 cameras. ! !end of general form text general_form_address: lname: Cowie fname: Lennox category: PI inst: 2192 addr_1: Institute for Astronomy addr_2: 2680 Woodlawn Dr. city: Honolulu state: HI zip: 96822 country: USA phone: 808-056-8134 telex: cowie@UHIFA.IFA.HAWAII.EDU ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: SSA22 descr_1: E, descr_2: 325 pos_1: RA = 22H 15M 1.00S +/- 0.15S, pos_2: DEC = 00D 00' 00.0" +/- 0.1", equinox: 1950.0 pm_or_par: N fluxnum_1: 1 fluxval_1: V=21.0 fluxnum_2: 2 fluxval_2: I=23.0 ! targnum: 2 name_1: SSA13 descr_1: E, descr_2: 325 pos_1: RA = 13H 10M 1.00S +/- 0.15S, pos_2: DEC = 43D 00' 31.0" +/- 0.1", equinox: 1950.0 pm_or_par: N fluxnum_1: 1 fluxval_1: V=21.0 fluxnum_2: 2 fluxval_2: I=23.0 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.100 targname: SSA22 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F814W num_exp: 1 time_per_exp: 2400S s_to_n: 5 fluxnum_1: 2 priority: 1 param_1: CR-SPLIT=NO req_1: CYCLE 4 / 1.1-2.6; req_3: SEQ 1.1-1.6 NO GAP comment_1: SIX EXPOSURES SHOULD comment_4: BE SEQUENTIAL WITH EACH EXPOSURE comment_5: SEPARATED BY 5 ARCSECONDS FROM comment_6: PRECEDING EXPOSURE ! linenum: 1.200 targname: SSA22 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F814W num_exp: 1 time_per_exp: 2400S s_to_n: 5 fluxnum_1: 2 priority: 1 param_1: CR-SPLIT=NO req_3: POS TARG +5.0,0.0; req_4: SAME ORIENT FOR 1.2-1.76 AS 1.1 ! linenum: 1.300 targname: SSA22 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F814W num_exp: 1 time_per_exp: 2400S s_to_n: 5 fluxnum_1: 2 priority: 1 param_1: CR-SPLIT=NO req_3: POS TARG +5.0,+5.0 ! linenum: 1.400 targname: SSA22 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F814W num_exp: 1 time_per_exp: 2400S s_to_n: 5 fluxnum_1: 2 priority: 1 param_1: CR-SPLIT=NO req_3: POS TARG +0.0,+5.0 ! linenum: 1.500 targname: SSA22 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F814W num_exp: 1 time_per_exp: 2400S s_to_n: 5 fluxnum_1: 2 priority: 1 param_1: CR-SPLIT=NO req_3: POS TARG -5.0,+5.0 ! linenum: 1.600 targname: SSA22 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F814W num_exp: 1 time_per_exp: 2400S s_to_n: 5 fluxnum_1: 2 priority: 1 param_1: CR-SPLIT=NO req_3: POS TARG -5.0,0.0 ! linenum: 1.710 targname: SSA22 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F814W num_exp: 1 time_per_exp: 2400S s_to_n: 5 fluxnum_1: 2 priority: 1 param_1: CR-SPLIT=NO req_3: SEQ 1.71-1.76 NO GAP comment_1: SIX EXPOSURES SHOULD comment_4: BE SEQUENTIAL WITH EACH EXPOSURE comment_5: SEPARATED BY 5 ARCSECONDS FROM comment_6: PRECEDING EXPOSURE ! linenum: 1.7200 targname: SSA22 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F814W num_exp: 1 time_per_exp: 2400S s_to_n: 5 fluxnum_1: 2 priority: 1 param_1: CR-SPLIT=NO req_3: POS TARG +5.0,0.0 ! linenum: 1.7300 targname: SSA22 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F814W num_exp: 1 time_per_exp: 2400S s_to_n: 5 fluxnum_1: 2 priority: 1 param_1: CR-SPLIT=NO req_3: POS TARG +5.0,+5.0 ! linenum: 1.7400 targname: SSA22 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F814W num_exp: 1 time_per_exp: 2400S s_to_n: 5 fluxnum_1: 2 priority: 1 param_1: CR-SPLIT=NO req_3: POS TARG +0.0,+5.0 ! linenum: 1.7500 targname: SSA22 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F814W num_exp: 1 time_per_exp: 2400S s_to_n: 5 fluxnum_1: 2 priority: 1 param_1: CR-SPLIT=NO req_3: POS TARG -5.0,+5.0 ! linenum: 1.7600 targname: SSA22 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F814W num_exp: 1 time_per_exp: 2400S s_to_n: 5 fluxnum_1: 2 priority: 1 param_1: CR-SPLIT=NO req_3: POS TARG -5.0,0.0 ! linenum: 2.100 targname: SSA13 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F814W num_exp: 1 time_per_exp: 2600S s_to_n: 5 fluxnum_1: 2 priority: 2 param_1: CR-SPLIT=NO req_3: SEQ 2.1-2.6 NO GAP comment_1: SIX EXPOSURES SHOULD comment_4: BE SEQUENTIAL WITH EACH EXPOSURE comment_5: SEPARATED BY 5 ARCSECONDS FROM comment_6: PRECEDING EXPOSURE ! linenum: 2.200 targname: SSA13 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F814W num_exp: 1 time_per_exp: 2600S s_to_n: 5 fluxnum_1: 2 priority: 2 param_1: CR-SPLIT=NO req_3: POS TARG +5.0,+0.0; req_4: SAME ORIENT FOR 2.2-2.6 AS 2.1 ! linenum: 2.300 targname: SSA13 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F814W num_exp: 1 time_per_exp: 2600S s_to_n: 5 fluxnum_1: 2 priority: 2 param_1: CR-SPLIT=NO req_3: POS TARG +5.0,+5.0 ! linenum: 2.400 targname: SSA13 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F814W num_exp: 1 time_per_exp: 2600S s_to_n: 5 fluxnum_1: 2 priority: 2 param_1: CR-SPLIT=NO req_3: POS TARG +0.0,+5.0 ! linenum: 2.500 targname: SSA13 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F814W num_exp: 1 time_per_exp: 2600S s_to_n: 5 fluxnum_1: 2 priority: 2 param_1: CR-SPLIT=NO req_3: POS TARG -5.0,+5.0 ! linenum: 2.600 targname: SSA13 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F814W num_exp: 1 time_per_exp: 2600S s_to_n: 5 fluxnum_1: 2 priority: 2 param_1: CR-SPLIT=NO req_3: POS TARG -5.0,0.0; ! ! end of exposure logsheet ! No scan data records found