! File: 4298C.PROP ! Database: PEPDB ! Date: 20-FEB-1994:20:51:52 coverpage: title_1: GALAXY POPULATIONS IN INTERMEDIATE REDSHIFT CLUSTERS title_2: CYCLE3 HIGH sci_cat: GALAXIES & CLUSTERS proposal_for: GO pi_title: DR. pi_fname: WARRICK pi_mi: J pi_lname: COUCH pi_inst: UNIVERSITY OF NEW SOUTH WALES pi_country: AUSTRALIA pi_phone: 61-2-697-4578 keywords_1: DISTANT GALAXY CLUSTERS, GALAXY EVOLUTION, GALAXY keywords_2: MORPHOLOGY hours_pri: 20.95 num_pri: 3 wf_pc: Y pi_position: LECTURER off_fname: JOHN off_mi: W off_lname: STOREY off_title: HEAD OF SCHOOL off_inst: SCHOOL OF PHYSICS, UNIVERSITY OF NEW SOUTH WALES off_addr_1: P.O. BOX 1 off_city: KENSINGTON, SYDNEY off_state: NSW off_zip: 2033 off_country: AUSTRALIA off_phone: 61-2-697-4566 off_telex: AA26054 ! end of coverpage abstract: line_1: We request WFC time to continue our program of high spatial line_2: resolution imagery of the members of southern rich galaxy line_3: clusters at intermediate redshifts (z ~ 0.3-0.4) which we have line_4: studied extensively at the AAT via fibre-optic spectroscopy and line_5: multi-colour photometry. Our comprehensive ground-based data have line_6: allowed us to measure precise line indices and colours for line_7: individual members in these clusters, thus allowing the line_8: construction of a unified picture for the various phenomena line_9: associated with the Butcher-Oemler effect whereby galaxies are line_10: seen at different stages of star-formation activity within a line_11: simple cycle. The WFC data will allow us to further our line_12: morphological classification of such galaxies, providing the line_13: information crucial to determining the physical phenomena which line_14: underlie the Butcher-Oemler effect. The superiority of our line_15: cluster samples in terms of the size and completeness of the line_16: spectroscopic and photometric coverage from theground makes them line_17: ideal targets for tackling this problem with HST. ! ! end of abstract general_form_proposers: lname: COUCH fname: WARRICK title: DR. mi: J inst: UNIVERSITY OF NEW SOUTH WALES country: AUSTRALIA esa: N ! lname: ELLIS fname: RICHARD title: PROF. mi: S inst: DURHAM UNIVERSITY country: UK esa: Y ! lname: SHARPLES fname: RAY title: DR. mi: M inst: DURHAM UNIVERSITY country: UK esa: Y ! lname: SMAIL fname: IAN title: MR. mi: R inst: DURHAM UNIVERSITY country: UK esa: Y ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We propose broad-band WFC imaging of the rich southern clusters line_2: AC118 and AC103 in F702W. The images will be exposed to depths line_3: required to provide morphological classifications of line_4: the bursting and post-starburst galaxies identified in our line_5: R < 20 spectroscopic and photometric ground-based samples. line_6: Morphological classification will proceed via quantitative line_7: surface photometry of the images obtained with the derivation line_8: of surface brightness profiles and disk/bulge ratios. Fourier line_9: deconvolution techniques will be employed to further enhance line_10: these processes. We propose additional F702W imaging of the line_11: cluster A2218. These observations will provide an important low line_12: redshift control sample to compare with the more distant Butcher-Oemler line_13: clusters. In addition we will obtain high resolution imaging line_14: of a wide variety of gravitationally lensed systems discovered line_15: in A2218. These include numerous arcs and arclets - several with line_16: spectroscopic redshifts and a unique optical Einstein ring. line_17: The F702W filter provides high throughput combined with rest wavelength line_18: coverage longward of the 4000A break in our two z=0.31 clusters. line_19: In A2218 because of the wide range of colours seen in the arcs line_20: F702W is a compromise choice to allow high signal to noise line_21: imaging of the widest range of gravitational arcs in the field. ! question: 4 section: 1 line_1: The largest 4-5m ground-based telescopes have been pushed line_2: to their observational limits in terms of detection, line_3: photometry and spectroscopy in investigations of the line_4: Butcher-Oemler effect. While there is now a much clearer line_5: understanding of the effect, the inability to spatially line_6: resolve the distant cluster galaxies from the ground remains line_7: the major barrier to resolving the key issues. None of the line_8: scientific objectives can be met from the ground because of line_9: atmospheric seeing limitations. Despite some progress with line_10: image enhancement techniques, such systems are not suitable for line_11: faint objects and do not reach the 0.1-0.2 arcsec resolution line_12: required for precise morphological work. ! question: 5 section: 1 line_1: Our main requirement is to obtain complete morphological line_2: information for the R<20 members in AC118 and AC103 identified line_3: and studied spectroscopically at the AAT. The R<20 limit line_4: corresponds to V < 21.0 and I < 19.3. Using our Cycle 1 GO line_5: observations of the z=0.3 cluster AC114 (the first target in line_6: this continuing project) we determine that a minimum of 5.8 line_9: hours (3 10**5 electrons in an R=20 source) in F702W on our line_10: AC118 and AC103 fields is required for us to pursue our line_11: morphological study of the galaxies in these clusters. line_12: A 5.7 hour exposure in F702W on A2218 will provide high signal line_13: to noise morphological information on the gravitational arcs line_14: and arclets to allow detailed modelling of their source galaxies. line_15: In order to correct for cosmic ray events, frame pairs are line_16: required, but to avoid charge defect problems associated with low line_17: background levels, ideally no individual sub-exposure should be line_18: less than 1 orbit. ! question: 7 section: 1 line_1: The WFC frames will be reduced on HST-funded SUN workstations line_2: using software proven for the analysis of extended galaxies line_3: (Couch and Newell 1984). All applicants have extensive line_4: experience in multicolour cluster photometry (Couch et al line_5: 1983) and in surface photometry of bright spheroidal line_6: and multi-component galaxies (Sharples, thesis). ! question: 10 section: 1 line_1: Durham University and the University of New South Wales line_2: both have excellent computing facilities. In particular the line_3: facilities at Durham consist of a network of 12 SUN workstations line_4: served by a multi-processor server partly funded from HST grants line_5: and a cluster of 9 microVAXs. There is one STARLINK programmer line_6: dedicated to image processing requirements. ! !end of general form text general_form_address: lname: COUCH fname: WARRICK mi: J title: DR. category: PI inst: UNIVERSITY OF NEW SOUTH WALES addr_1: SCHOOL OF PHYSICS addr_2: PO BOX 1 addr_3: KENSINGTON city: SYDNEY, NSW zip: 2033 country: AUSTRALIA phone: 61-2-697-4578 telex: AA26054 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: AC103 descr_1: GALAXY CLUSTER ; descr_2: DISTANT GALAXY CLUSTER pos_1: RA = 20H 57M 09.4S +/- 0.2S, pos_2: DEC = -64D 39' 18.7" +/- 4.5" equinox: J2000 rv_or_z: Z = 0.31 fluxnum_1: 1 fluxval_1: V = 21.1 +/- 0.2 fluxnum_2: 2 fluxval_2: I = 20.2 +/- 0.2 ! targnum: 2 name_1: AC118 descr_1: GALAXY CLUSTER ; descr_2: DISTANT GALAXY CLUSTER pos_1: RA = 00H 14M 19.3S +/- 0.2S, pos_2: DEC = -30D 23' 18.2" +/- 4.5" equinox: J2000 rv_or_z: Z = 0.31 fluxnum_1: 1 fluxval_1: V = 21.1 +/- 0.2 fluxnum_2: 2 fluxval_2: I = 20.2 +/- 0.2 ! targnum: 3 name_1: A2218 descr_1: GALAXY CLUSTER ; descr_2: NEARBY GALAXY CLUSTER pos_1: RA = 16H 35M 52.9S +/- 0.2S, pos_2: DEC = +66D 12' 19.6" +/- 4.5" equinox: J2000 rv_or_z: Z = 0.17 fluxnum_1: 1 fluxval_1: V = 21.1 +/- 0.2 fluxnum_2: 2 fluxval_2: I = 20.2 +/- 0.2 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: AC103 config: WFC opmode: IMAGE aperture: WFALL sp_element: F702W num_exp: 1 time_per_exp: 1800S s_to_n: 110 s_to_n_time: 21000S fluxnum_1: 2 priority: 1 param_1: CR-SPLIT = NO param_2: PRE-FLASH = NO req_1: CYCLE 3; req_2: GROUP 1.0-1.1 NO GAP comment_1: MINIMUM USEFUL SUB-EXPOSURE comment_2: IS 2500S OR 1 ORBIT. comment_3: SUB-EXPOSURES POSITIONS SHOULD comment_4: BE RANDOMLY OFFSET FROM EACH comment_5: OTHER BY 0.5-1 ARCSEC TO ALLOW comment_6: HOTSPOT REMOVAL. ! linenum: 1.100 targname: AC103 config: WFC opmode: IMAGE aperture: WFALL sp_element: F702W num_exp: 4 time_per_exp: 2300S s_to_n: 110 s_to_n_time: 21000S fluxnum_1: 2 priority: 1 param_1: CR-SPLIT = NO param_2: PRE-FLASH = NO req_1: CYCLE 3 comment_1: MINIMUM USEFUL SUB-EXPOSURE comment_2: IS 2500S OR 1 ORBIT. comment_3: SUB-EXPOSURES POSITIONS SHOULD comment_4: BE RANDOMLY OFFSET FROM EACH comment_5: OTHER BY 0.5-1 ARCSEC TO ALLOW comment_6: HOTSPOT REMOVAL. ! linenum: 1.500 targname: AC103 config: WFC opmode: IMAGE aperture: WFALL sp_element: F702W num_exp: 1 time_per_exp: 1800S s_to_n: 110 s_to_n_time: 21000S fluxnum_1: 2 priority: 1 param_1: CR-SPLIT = NO param_2: PRE-FLASH = NO req_1: CYCLE 3; req_2: GROUP 1.5-1.6 NO GAP; req_3: POS TARG 0.7, 0.7 comment_1: MINIMUM USEFUL SUB-EXPOSURE comment_2: IS 2500S OR 1 ORBIT. comment_3: SUB-EXPOSURES POSITIONS SHOULD comment_4: BE RANDOMLY OFFSET FROM EACH comment_5: OTHER BY 0.5-1 ARCSEC TO ALLOW comment_6: HOTSPOT REMOVAL. ! linenum: 1.600 targname: AC103 config: WFC opmode: IMAGE aperture: WFALL sp_element: F702W num_exp: 4 time_per_exp: 2300S s_to_n: 110 s_to_n_time: 21000S fluxnum_1: 2 priority: 1 param_1: CR-SPLIT = NO param_2: PRE-FLASH = NO req_1: CYCLE 3; req_2: POS TARG 0.7, 0.7 comment_1: MINIMUM USEFUL SUB-EXPOSURE comment_2: IS 2500S OR 1 ORBIT. comment_3: SUB-EXPOSURES POSITIONS SHOULD comment_4: BE RANDOMLY OFFSET FROM EACH comment_5: OTHER BY 0.5-1 ARCSEC TO ALLOW comment_6: HOTSPOT REMOVAL. ! linenum: 2.000 targname: AC118 config: WFC opmode: IMAGE aperture: WFALL sp_element: F702W num_exp: 1 time_per_exp: 1800S s_to_n: 110 s_to_n_time: 21000S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO param_2: PRE-FLASH = NO req_1: CYCLE 3; req_2: SEQ 2.0-2.2 NO GAP comment_1: MINIMUM USEFUL SUB-EXPOSURE comment_2: IS 2500S OR 1 ORBIT. comment_3: SUB-EXPOSURES POSITIONS SHOULD comment_4: BE RANDOMLY OFFSET FROM EACH comment_5: OTHER BY 0.5-1 ARCSEC TO ALLOW comment_6: HOTSPOT REMOVAL. ! linenum: 2.200 targname: AC118 config: WFC opmode: IMAGE aperture: WFALL sp_element: F702W num_exp: 4 time_per_exp: 2300S s_to_n: 110 s_to_n_time: 21000S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO param_2: PRE-FLASH = NO req_1: CYCLE 3 comment_1: MINIMUM USEFUL SUB-EXPOSURE comment_2: IS 2500S OR 1 ORBIT. comment_3: SUB-EXPOSURES POSITIONS SHOULD comment_4: BE RANDOMLY OFFSET FROM EACH comment_5: OTHER BY 0.5-1 ARCSEC TO ALLOW comment_6: HOTSPOT REMOVAL. ! linenum: 2.500 targname: AC118 config: WFC opmode: IMAGE aperture: WFALL sp_element: F702W num_exp: 1 time_per_exp: 1800S s_to_n: 110 s_to_n_time: 21000S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO param_2: PRE-FLASH = NO req_1: CYCLE 3; req_2: POS TARG 0.7, 0.7; req_3: SEQ 2.5-2.6 NO GAP comment_1: MINIMUM USEFUL SUB-EXPOSURE comment_2: IS 2500S OR 1 ORBIT. comment_3: SUB-EXPOSURES POSITIONS SHOULD comment_4: BE RANDOMLY OFFSET FROM EACH comment_5: OTHER BY 0.5-1 ARCSEC TO ALLOW comment_6: HOTSPOT REMOVAL. ! linenum: 2.600 targname: AC118 config: WFC opmode: IMAGE aperture: WFALL sp_element: F702W num_exp: 4 time_per_exp: 2300S s_to_n: 110 s_to_n_time: 21000S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO param_2: PRE-FLASH = NO req_1: CYCLE 3; req_2: POS TARG 0.7, 0.7 comment_1: MINIMUM USEFUL SUB-EXPOSURE comment_2: IS 2500S OR 1 ORBIT. comment_3: SUB-EXPOSURES POSITIONS SHOULD comment_4: BE RANDOMLY OFFSET FROM EACH comment_5: OTHER BY 0.5-1 ARCSEC TO ALLOW comment_6: HOTSPOT REMOVAL. ! linenum: 3.000 targname: A2218 config: WFC opmode: IMAGE aperture: WFALL sp_element: F702W num_exp: 1 time_per_exp: 1800S s_to_n: 110 s_to_n_time: 20600S fluxnum_1: 1 priority: 2 param_1: CR-SPLIT = NO param_2: PRE-FLASH = NO req_1: CYCLE 3; req_2: SEQ 3.0-3.1 NO GAP comment_1: MINIMUM USEFUL SUB-EXPOSURE comment_2: IS 2500S OR 1 ORBIT. comment_3: SUB-EXPOSURES POSITIONS SHOULD comment_4: BE RANDOMLY OFFSET FROM EACH comment_5: OTHER BY 0.5-1 ARCSEC TO ALLOW comment_6: HOTSPOT REMOVAL. ! linenum: 3.100 targname: A2218 config: WFC opmode: IMAGE aperture: WFALL sp_element: F702W num_exp: 4 time_per_exp: 2300S s_to_n: 110 s_to_n_time: 20600S fluxnum_1: 1 priority: 2 param_1: CR-SPLIT = NO param_2: PRE-FLASH = NO req_1: CYCLE 3; comment_1: MINIMUM USEFUL SUB-EXPOSURE comment_2: IS 2500S OR 1 ORBIT. comment_3: SUB-EXPOSURES POSITIONS SHOULD comment_4: BE RANDOMLY OFFSET FROM EACH comment_5: OTHER BY 0.5-1 ARCSEC TO ALLOW comment_6: HOTSPOT REMOVAL. ! linenum: 3.500 targname: A2218 config: WFC opmode: IMAGE aperture: WFALL sp_element: F702W num_exp: 1 time_per_exp: 1800S s_to_n: 110 s_to_n_time: 20600S fluxnum_1: 1 priority: 2 param_1: CR-SPLIT = NO param_2: PRE-FLASH = NO req_1: CYCLE 3; req_2: SEQ 3.5-3.6 NO GAP; req_3: POS TARG 0.7, 0.7 comment_1: MINIMUM USEFUL SUB-EXPOSURE comment_2: IS 2500S OR 1 ORBIT. comment_3: SUB-EXPOSURES POSITIONS SHOULD comment_4: BE RANDOMLY OFFSET FROM EACH comment_5: OTHER BY 0.5-1 ARCSEC TO ALLOW comment_6: HOTSPOT REMOVAL. ! linenum: 3.600 targname: A2218 config: WFC opmode: IMAGE aperture: WFALL sp_element: F702W num_exp: 4 time_per_exp: 2300S s_to_n: 110 s_to_n_time: 20600S fluxnum_1: 1 priority: 2 param_1: CR-SPLIT = NO param_2: PRE-FLASH = NO req_1: CYCLE 3; req_2: POS TARG 0.7, 0.7 comment_1: MINIMUM USEFUL SUB-EXPOSURE comment_2: IS 2500S OR 1 ORBIT. comment_3: SUB-EXPOSURES POSITIONS SHOULD comment_4: BE RANDOMLY OFFSET FROM EACH comment_5: OTHER BY 0.5-1 ARCSEC TO ALLOW comment_6: HOTSPOT REMOVAL. ! ! end of exposure logsheet ! No scan data records found