! $Id: 5701,v 8.1 1994/07/27 20:30:02 pepsa Exp $ coverpage: title_1: GALAXY POPULATIONS IN INTERMEDIATE REDSHIFT CLUSTERS: title_2: CYCLE 4 CARRY-OVER sci_cat: GALAXIES & CLUSTERS proposal_for: GO/CAR cont_id: 4298 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. line_22: NOTE: The text ( above ) is from the original GF Q3 in Cycle 3 GO 4298. line_23: The remainder of GF Q3 pertains specifically to Cycle 4 Carry-Over. ! question: 3 section: 2 line_1: DESCRIPTION OF OBSERVATIONS: IMPLEMENTATION AND SCHEDULING NOTES line_2: FOR THE CYCLE 4 CARRY-OVER PROGRAM ( FORMERLY CYCLE 3 OBSERVATIONS ) line_3: The observations themselves should be performed as described here. line_4: line_5: All exposures are done with CR-SPLIT=NO to keep down read noise. line_6: For each target, there should be 3 exposures in F702W, all line_7: exposures per target being made together with NO GAPs, precluding line_8: intervention of any other activities. In each case, all three line_9: long exposures of a target should be made slightly shifted but line_10: at SAME ORIENTATION. The POS TARG positions are chosen to yield line_11: 3 pixel offsets in X and Y, thus POS TARG +10.0,+10.0, POS TARG line_12: +10.3,+10.0, and POS TARG +10.0,+10.3 are used. line_13: line_14: All exposures in this program should be made using the WFALL-FIX line_15: aperture in conjunction with the small shifts around POS TARG +10, line_16: +10 in order to place the Fixed Target List coords at ~ the apex of line_17: the pyramid. The Fixed Target List coords, POS TARGs, and ORIENT line_18: angles and tolerances have been chosen so as to avoid having objects line_19: of the greatest interest fall onto the apex of the pyramid or seams line_20: in between chips, etc., even though the FOV may be rotated slightly line_21: by STScI ( around the Fixed Target List coords at the apex, and line_22: within the tolerance range we have given for each specified ORIENT line_23: angle ) as needed for implementation and scheduling purposes. ! question: 3 section: 3 line_1: The details on a per-cluster basis are as follows: line_2: line_3: AC103 - IMPLEMENTATION AND SCHEDULING NOTES line_4: 3 exps in F702W, all done together at same time, with SAME ORIENT. line_5: NOTE: For purposes of overcoming hot pixels, do small shifts (3 pixels) line_6: around POS TARG +10,+10 ( i.e. at or near apex ) between each exposure. line_7: We will align the images post-observation to eliminate cosmic rays. line_8: Use ORIENT = 315D +/- 15D with field center ( FTL coords ): line_9: RA = 20h 52m 51.35s Dec = -64d 50' 26.5" Equinox: B1950 line_10: NOTE: Coords of the other two targets in this program are in line_11: J2000 Equinox, but this one is in B1950. line_12: line_13: AC118 - IMPLEMENTATION AND SCHEDULING NOTES line_14: 3 exps in F702W, all done together at same time, with SAME ORIENT. line_15: NOTE: For purposes of overcoming hot pixels, do small shifts (3 pixels) line_16: around POS TARG +10,+10 ( i.e. FTL coords at or near apex ) between line_17: each exposure. We will align images post-obs for cosmic ray removal. line_18: Use ORIENT = 37D +/- 5D ( preferred ) with field center coords: line_19: RA = 00h 14m 19.3s Dec = -30d 23' 18.2" Equinox: J2000 line_20: PLEASE INFORM US IF YOU NEED TO USE THE FOLLOWING OPTION: line_21: NOTE: If necessary for scheduling, may also use 217D +/- 5D with line_22: the SAME FTL coords at field center (FTL coords): line_23: RA = 00h 14m 19.3s Dec = -30d 23' 18.2" Equinox: J2000 ! question: 3 section: 4 line_1: A2218 - IMPLEMENTATION AND SCHEDULING NOTES line_2: 3 exps in F702W, all done together at same time, and at SAME ORIENT. line_3: NOTE: For purposes of overcoming hot pixels, do small shifts (3 pixels) line_4: around POS TARG +10,+10 (i.e. FTL coords at or near apex ) between line_5: exposures. We will align images post-obs for cosmic ray removal. line_6: Use ORIENT 95D +/- 5D (preferred) with field center ( FTL coords ): line_7: RA = 16h 35m 57.0s Dec = +66d 12' 38.0" Equinox: J2000 line_8: PLEASE INFORM US IF YOU NEED TO USE THE FOLLOWING OPTION: line_9: NOTE: May change ORIENT requirement to 45D +/- 5D or 225D +/- 5D line_10: if necessary for scheduling, provided you use this alternate field line_11: center ( FTL coords ): line_12: RA = 16h 35m 52.4s Dec = +66d 12' 38.0" Equinox: J2000 line_13: line_14: GENERAL NOTES ON THE PROGRAM STRUCTURE line_15: In this version of the program, each individual exposure of a line_16: given cluster has its own individual exposure log line, with line_17: special requirements SEQ NO GAP and SAME ORIENT tying the individual line_18: exposures together, and small offsets of 3 WF pixels in X and Y near line_19: POS TARG +10,+10 being applied to each line individually, while the line_20: ORIENT on one line is tied to all in a group by the aforementioned line_21: SAME ORIENT. It is also understood that in some cases the initial line_22: exposure may need to be slightly shorter, but hopefully not more than line_23: a few hundred seconds shorter at most, in order to accomodate the ! question: 3 section: 5 line_1: time for full guide star acquisition, etc. line_2: line_3: Please inform the observers and the STScI staff contact Ray Lucas line_4: if the program structure is changed, including any changes needed line_5: to ORIENT angles, target positions, exposure times, and special line_6: requirements, etc., so that they might have some input into the line_7: final structure if any decisions are required. line_8: line_9: In this WFPC2 carry-over program, we are using less time and line_10: therefore fewer exposures per target to achieve the same science. line_11: Both hot pixels and cosmic rays are a bigger problem with WFPC2, line_12: but the optimum solutions for each are in opposition. Since hot line_13: pixels are best identified and overcome by small shifts between line_14: exposures, but cosmic ray removal is facilitated and made more line_15: effective by having all the exposures of a given target aligned, line_16: we have decided to try and align the 3 exposures per target in line_17: the post-observation phase ( pointing accuracy is supposed to be line_18: good to 2-3 milliarcsec ) in order to remove cosmic rays and keep line_19: down the read noise, and the small offsets from +10,+10 in the 2nd line_20: and 3rd exposures will be used to provide a small shift of an line_21: integral number of pixels ( for detecting and overcoming the line_22: effects of hot pixels, etc. ) ! question: 3 section: 6 line_1: NOTE: Exposure time has been shortened to 1900s for the first line_2: orbit in the sequence of observations for each target. This line_3: was done in order to allow time for a full GS acquisition on the line_4: first orbit, and keeps the data set consistent for each object. line_5: This was done as a result of consultations between the PI and line_6: Ray Lucas at STScI. The observers wish the second and third orbits line_7: of each target to retain a full 2300s exposure time if possible. line_8: If this is never possible during the intended scheduling windows, line_9: please advise both the PI and Ray Lucas. - RAL 7/25/94 ! 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. ( NOTE: The previous text in GF Q5 is from the line_19: original GO 4298. See GF Q3 for updated text on implementation line_20: of this carry-over program. ) ! ! 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: F, descr_2: 404 pos_1: RA = 20H 52M 51.35S +/- 0.2S, pos_2: DEC = -64D 50' 26.5" +/- 4.5" equinox: B1950 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 comment_1: NOTE: THE EQUINOX IS B1950 IN comment_2: THIS CASE, UNLIKE THE OTHER 2 comment_3: TARGETS, WHICH ARE J2000. ! targnum: 2 name_1: AC118 descr_1: F, descr_2: 404 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: F, descr_2: 404,411,412 pos_1: RA = 16H 35M 57.0S +/- 0.2S, pos_2: DEC = +66D 12' 38.0" +/- 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: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F702W num_exp: 1 time_per_exp: 1900S s_to_n: 110 s_to_n_time: 21000S fluxnum_1: 2 priority: 1 param_1: CR-SPLIT=NO req_1: CYCLE 4; req_2: POS TARG +10.0,+10.0; req_3: ORIENT 315D +/- 15D; req_4: SAME ORIENT FOR 1.1-1.2 AS 1.0; req_5: SEQ 1.0-1.2 NO GAP; comment_1: ALL EXPOSURES OF THIS TARGET comment_2: SHOULD BE TAKEN TOGETHER WITH comment_3: NO GAPS IN BETWEEN, AND WITH comment_4: THE EXACT SAME ORIENT. POS TARG comment_5: +10,+10 PLACES FTL COORDS AT comment_6: APEX. ! linenum: 1.100 targname: AC103 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F702W num_exp: 1 time_per_exp: 2300S s_to_n: 110 s_to_n_time: 21000S fluxnum_1: 2 priority: 1 param_1: CR-SPLIT=NO req_1: CYCLE 4; req_2: POS TARG +10.3,+10.0; comment_1: EXPOSURE TIME IN FIRST ORBIT comment_2: HAS BEEN CUT SLIGHTLY TO comment_3: ALLOW TIME FOR FULL GS ACQ. comment_4: SECOND AND THIRD EXPOSURES comment_5: 2300s EACH. ! linenum: 1.200 targname: AC103 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F702W num_exp: 1 time_per_exp: 2300S s_to_n: 110 s_to_n_time: 21000S fluxnum_1: 2 priority: 1 param_1: CR-SPLIT=NO req_1: CYCLE 4; req_2: POS TARG +10.0,+10.3; comment_1: NOTE: ALL S_TO_N_TIME comment_2: VALUES FOR ALL TARGETS comment_3: ARE FROM ORIGINAL PROGRAM comment_4: AND ARE NOT VALID VALUES comment_5: FOR THIS CARRY-OVER comment_6: PROGRAM. ! linenum: 2.000 targname: AC118 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F702W num_exp: 1 time_per_exp: 1900S s_to_n: 110 s_to_n_time: 21000S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO req_1: CYCLE 4; req_2: POS TARG +10.0,+10.0; req_3: ORIENT 37D +/- 5D; req_4: SAME ORIENT FOR 2.1-2.2 AS 2.0; req_5: SEQ 2.0-2.2 NO GAP; comment_1: ALL 3 EXPOSURES OF THIS TARGET comment_2: SHOULD BE TAKEN TOGETHER WITH comment_3: NO GAPS IN BETWEEN, AND WITH comment_4: THE EXACT SAME ORIENT FOR ALL. comment_5: POS TARG +10,+10 PLACES FTL comment_6: COORDS AT APEX. ! linenum: 2.100 targname: AC118 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F702W num_exp: 1 time_per_exp: 2300S s_to_n: 110 s_to_n_time: 21000S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO req_1: CYCLE 4; req_2: POS TARG +10.3,+10.0; comment_1: ORIENT 217D +/-5D ALSO OK FOR FTL comment_2: COORDS LISTED, IF NECESSARY FOR comment_3: FOR SCHEDULING, BUT ORIENT=37D comment_4: +/-5D IS PREFERRED. EXP TIME IS comment_5: SLIGHTLY LESS IN FIRST ORBIT FOR comment_6: GS ACQ, BUT 2300S IN 2ND & 3RD. ! linenum: 2.200 targname: AC118 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F702W num_exp: 1 time_per_exp: 2300S s_to_n: 110 s_to_n_time: 21000S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO req_1: CYCLE 4; req_2: POS TARG +10.0,+10.3; comment_1: NOTE: ALL S_TO_N_TIME comment_2: VALUES FOR ALL TARGETS comment_3: ARE FROM ORIGINAL PROGRAM comment_4: AND ARE NOT VALID VALUES comment_5: FOR THIS CARRY-OVER comment_6: PROGRAM. ! linenum: 3.000 targname: A2218 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F702W num_exp: 1 time_per_exp: 1900S s_to_n: 110 s_to_n_time: 20600S fluxnum_1: 1 priority: 2 param_1: CR-SPLIT=NO req_1: CYCLE 4; req_2: POS TARG +10.0,+10.0; req_3: ORIENT 95D +/- 10D; req_4: SAME ORIENT FOR 3.1-3.2 AS 3.0; req_5: SEQ 3.0-3.2 NO GAP; comment_1: ALL 3 EXPOSURES OF THIS TARGET comment_2: SHOULD BE TAKEN TOGETHER WITH comment_3: NO GAPS IN BETWEEN, AND WITH comment_4: THE EXACT SAME ORIENT. POS TARG comment_5: +10,+10 PLACES FTL COORDS AT comment_6: APEX. ! linenum: 3.100 targname: A2218 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F702W num_exp: 1 time_per_exp: 2300S s_to_n: 110 s_to_n_time: 20600S fluxnum_1: 1 priority: 2 param_1: CR-SPLIT=NO req_1: CYCLE 4; req_2: POS TARG +10.3,+10.0; comment_1: EXPOSURE TIME FOR FIRST comment_2: ORBIT WAS CUT SLIGHTLY comment_3: TO ALLOW FOR FULL GS ACQ. comment_4: EXPOSURE TIME FOR 2ND & 3RD comment_5: ORBITS SHOULD REMAIN AT comment_6: 2300S FOR EACH, THOUGH. ! linenum: 3.200 targname: A2218 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F702W num_exp: 1 time_per_exp: 2300S s_to_n: 110 s_to_n_time: 20600S fluxnum_1: 1 priority: 2 param_1: CR-SPLIT=NO req_1: CYCLE 4; req_2: POS TARG +10.0,+10.3; comment_1: ALTERNATE ORIENTS 45D +/- 10D comment_2: OR 225D +/- 10D MAY BE USED comment_3: IF NECESSARY, PROVIDED THAT comment_4: THESE COORDS ARE USED INSTEAD: comment_5: RA=16H 35M 52.4S, DEC=+66D 12' comment_6: 38.0", EQUINOX = J2000 ! ! end of exposure logsheet ! No scan data records found