! $Id: 16,v 4.1 1994/07/26 20:48:25 pepsa Exp $ coverpage: title_1: MORPHOLOGY OF GALAXIES IN CLUSTERS AT Z = 0.5: FUTURE- title_2: CYCLE OBSERVATIONS sci_cat: GALAXIES & CLUSTERS sci_subcat: EVOLUTION/COSMOLOGY proposal_for: GO longterm: 2 cont_id: 2373 pi_title: DR. pi_fname: ALAN pi_lname: DRESSLER pi_inst: THE OBSERVATORIES OF THE CARNEGIE INSTITUTION OF WASHINGTON pi_country: USA pi_phone: 818-304-0245 keywords_1: GALAXY MORPHOLOGY, EVOLUTION, GALAXY CLUSTER hours_pri: 28.50 num_pri: 5 wf_pc: Y funds_amount: 250064 funds_length: 24 funds_date: JAN-90 pi_position: ASTRONOMER off_fname: ALAN off_lname: DRESSLER off_title: STAFF MEMBER off_inst: THE OBSERVATORIES OF THE CARNEGIE INSTITUTION OF WASHINGTON off_addr_1: 813 SANTA BARBARA ST. off_city: PASADENA off_state: CA off_zip: 91101 off_country: USA off_phone: 818-304-0245 off_telex: 15613818 OCIW UT ! end of coverpage abstract: line_1: Our program is intended to study galaxy evolution through the line_2: investigation of galaxy morphology as a function of lookback time. line_3: The development of disks and bulges, the role of mergers, line_4: interactions, and other environmental influences, are expected to line_5: be visible over the range 0 < z < 1 as judged by the line_6: spectrophotometric evolution already observed over this redshift line_7: range. Over this first year of our two year program, we will line_8: image with the Wide Field Camera 5 fields in four line_9: rich clusters of galaxies at z = 0.35 - 0.55 for which extensive line_10: photometry and spectroscopy already exist. The fields include a line_11: wide range of environments from the dense cores of clusters to line_12: isolated field galaxies. These data will be used to classify line_13: images according to traditional morphological categories and line_14: will be used to determine quantitative measures of surface line_15: brightness distributions and bulge-to-disk ratios. The images line_16: will be obtained in two colors in order to map the distribution line_17: of star formation in comparison with low-z galaxies in line_18: similar clusters. The data are applicable to specific line_19: questions, like the cause of enhanced starburst activity line_20: found for high-z galaxies. ! ! end of abstract general_form_proposers: lname: BUTCHER fname: HARVEY title: PROF. inst: KAPTEYN OBSERVATORY country: NETHERLANDS esa: Y ! lname: GUNN fname: JAMES title: PROF. mi: E. inst: ASTROPHYSICAL SCIENCES, PRINCETON UNIVERSITY country: USA ! lname: OEMLER fname: AUGUSTUS, JR. title: PROF. inst: DEPARTMENT OF ASTRONOMY, YALE UNIVERSITY country: USA ! lname: DRESSLER fname: ALAN title: P.I. inst: THE OBSERVATORIES OF THE CARNEGIE INSTITUTION OF WASHINGTON country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 0 line_1: We will use the WFC to image 5 fields in 4 clusters line_2: 0.36 < z < 0.55 in the first year of our two-year line_3: program. Ground-based CCD images of these fields were used line_4: to select a WFC field which includes an area for which line_5: multicolor photometry for most objects and low resolution line_6: spectroscopy for some objects are already in hand. A line_7: typical field will contain 1 contaminating field galaxy for line_8: every 2 cluster galaxies, so the sample covers a wide range line_9: of environments. The spectra have been classified according line_10: to "activity", related to star formation or an active line_11: nucleus. The fields centers are chosen to maximize the line_12: number of "active" galaxies. line_14: Observations will be coadded single-orbit exposures line_15: of 7,500 s or 10,000 s in each of two broad-band colors. line_16: roughly corresponding to rest-frame V and a band line_17: between U and B. Color maps will be constructed to study line_18: the distribution of star formation. The two colors will line_19: be coadded for the morphological classification, producing line_20: an effective wavelength near the center of the B band. This line_21: will be directly comparable to morphological classification line_22: at low redshift which is traditionally done in this color. ! question: 4 section: 0 line_1: Morphology is the missing component in our attempts to line_2: study galaxy evolution for 0 < z < 1. At the distance line_3: of our intended targets, 1 arcsecond = 7 1/h kpc, so line_4: morphological classification is extremely crude with line_5: ground-based seeing of FWHM = 0.5-1.0 arcseconds. No line_6: meaningful comparisons can be made with low-z classification line_7: systems. The HST with the WFC, with its field of 2.7 x 2.7 line_8: arcminutes and 0.1 arcsecond pixels, affords us the only line_9: opportunity to fundamentally correct this deficiency. line_11: In his study of 55 rich clusters, Dressler (1980 Ap. J. line_12: Suppl. 42) assigned Revised Hubble types to about 6000 line_13: galaxies. The more distant clusters in his sample have an line_14: average redshift z = 0.05, for which the 1 arcsecond FWHM line_15: seeing obtained by Dressler gave a resolution of line_16: approximately 0.7 1/h kpc. Though not as detailed as the line_17: classification of galaxies within the Local Supercluster, line_18: where resolutions of order 100 pc can be obtained, such line_19: imaging has thus been shown to be sufficient to distinguish line_20: between the major classes in the Hubble or de Vaucouleurs line_21: schemes. With HST imaging, nearly the same resolution of 0.7 line_22: 1/h kpc can be obtained for galaxies in clusters at z = 0.5. ! question: 5 section: 0 line_1: From CCD images of low-z cluster spirals we have line_2: simulated HST observations and concluded that, for clusters line_3: at z = 0.4, exposures of 15,000 s (6 x 2500 s single-orbit) line_4: exposures are required for a S/N = 20, necessary for even line_5: rudimentary classification. The more distant clusters at z line_6: = 0.55 in our sample will require at least 20,000 seconds (8 line_7: x 2500 s single-orbit) exposures. We have arrived at these line_8: numbers by obtaining CCD images of spiral galaxies in line_9: low-redshift clusters and using them to simulate exposures line_10: with the HST WFC, taking into account telescope and detector line_11: efficiency, dark current, readout noise, resolution, and line_12: sampling. We have found that at z = 0.5 the fine detail of line_13: spiral structure, particularly for early-type spirals, is line_14: only marginally discernible in the 10,000 s exposures line_15: obtained in each color. By coadding the two colors we line_16: should achieve a S/N and resolution comparable to that of line_17: Dressler's 1980 morphological classification of 6000 line_18: galaxies in 55 low-redshift clusters (z = 0.05). Should line_19: this still be insufficient, we have the option of repeating line_20: the first year's 5 fields in the second year. We have not line_21: included the possibility that evolution may make such line_22: features easier to detect. ! question: 7 section: 0 line_1: In order to accomplish our scientific objectives line_2: we must develop methods of moving from images to line_3: parametrized data. Traditionally this has been accomplished line_4: by using the image processing capabilities of the human eye line_5: plus brain, in order to assign morphological classes, line_6: estimate bulge-to-disk ratios, and describe distributions of line_7: color, dust, non-axisymmetric structures, etc. These line_8: classifications are semi-quantitative at best, and useful line_9: results regarding the evolution of galaxy morphology will line_10: depend on having an equivalent sample of observations at low line_11: redshift for which the same subjective criteria can be line_12: applied. With this in mind, Dressler and Gunn have begun to line_13: obtain CCD images of low redshift clusters 0.02 < z < 0.04 line_14: in seeing of FWHM < 1 arcsecond. With suitable processing, line_15: such data can be used to simulate the HST observations line_16: (similar sampling, S/N, and resolution) in order to provide line_17: calibration images. Thus, although the criteria will be line_18: remain subjective in this initial step, it can be applied so line_19: that redshift is the only significant variable, and a good line_20: assessment of differential morphology can be made. This line_21: procedure will be useful in applying traditional line_22: classification schemes like the Hubble or de Vaucouleurs line_23: systems. ! question: 10 section: 0 line_1: Dressler, Oemler, and Gunn each have access to a MicroVAX line_2: computer with image display capability. Each MicroVAX is line_3: part of a VAX system, supplied and maintained individually line_4: by MWLCO, Yale, and Princeton, which includes a variety of line_5: I/O devices and access to BITNET and other communication line_6: networks. line_8: Partial support for students will be provided Yale line_9: University and Princeton University. ! !end of general form text general_form_address: lname: DRESSLER fname: ALAN category: PI inst: THE OBSERVATORIES OF THE CARNEGIE INSTITUTION OF WASHINGTON ! lname: DRESSLER fname: ALAN title: DR. category: PI inst: THE OBSERVATORIES OF THE CARNEGIE INSTITUTION OF WASHINGTON addr_1: 813 SANTA BARBARA ST. city: PASADENA state: CA zip: 91101 country: USA phone: 818-304-0245 telex: 1561318 OCIW UT from_date: 01-OCT-89 to_date: 31-DEC-91 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: GAL-CLUS-001558+1609-FLD1 descr_1: Z = 0.54 CLUSTER OF GALAXIES pos_1: RA= 00H15M58.4S +/-0.1S, pos_2: DEC= +16D09'07" +/-1" equinox: 1950.0 pm_or_par: N rv_or_z: Z=0.54 ! targnum: 2 name_1: GAL-CLUS-001558+1609-FLD2 descr_1: Z = 0.54 CLUSTER OF GALAXIES pos_1: RA= 00H16M00.0S +/-0.1S, pos_2: DEC= +16D10'42" +/-1" equinox: 1950.0 pm_or_par: N rv_or_z: Z=0.54 ! targnum: 3 name_1: GAL-CLUS-002400+165300-FLD1 descr_1: Z = 0.39 CLUSTER OF GALAXIES pos_1: RA= 00H23M56.9S +/-0.1S, pos_2: DEC= +16D53'10" +/-1" equinox: 1950.0 pm_or_par: N rv_or_z: Z=0.39 ! targnum: 4 name_1: GAL-CLUS-002400+165300-FLD2 descr_1: Z = 0.39 CLUSTER OF GALAXIES pos_1: RA= 00H23M53.8S +/-0.1S, pos_2: DEC= +16D54'50" +/-1" equinox: 1950.0 pm_or_par: N rv_or_z: Z=0.39 ! targnum: 5 name_1: GAL-CLUS-ABELL370-FLD1 descr_1: Z = 0.37 CLUSTER OF GALAXIES pos_1: RA= 02H37M21.1S +/-0.1S, pos_2: DEC= -01D47'12" +/-1" equinox: 1950.0 pm_or_par: N rv_or_z: Z=0.37 ! targnum: 6 name_1: GAL-CLUS-ABELL370-FLD2 descr_1: Z = 0.37 CLUSTER OF GALAXIES pos_1: RA= 02H37M31.2S +/-0.1S, pos_2: DEC= -01D45'27" +/-1" equinox: 1950.0 pm_or_par: N rv_or_z: Z=0.37 ! targnum: 7 name_1: GAL-CLUS-030330+1706-FLD1 descr_1: Z = 0.43 CLUSTER OF GALAXIES pos_1: RA= 03H03M27.0S +/-0.1S, pos_2: DEC= +17D07'07" +/-1" equinox: 1950.0 pm_or_par: N rv_or_z: Z=0.43 ! targnum: 8 name_1: GAL-CLUS-030330+1706-FLD2 descr_1: Z = 0.43 CLUSTER OF GALAXIES pos_1: RA= 03H03M16.1S +/-0.1S, pos_2: DEC= +17D07'07" +/-1" equinox: 1950.0 pm_or_par: N rv_or_z: Z=0.43 ! targnum: 9 name_1: GAL-CLUS-093942+4713-FLD1 descr_1: Z = 0.40 CLUSTER OF GALAXIES pos_1: RA= 09H39M42.0S +/-0.1S, pos_2: DEC= +47D12'34" +/-1" equinox: 1950.0 pm_or_par: N rv_or_z: Z=0.40 ! targnum: 10 name_1: GAL-CLUS-093942+4713-FLD2 descr_1: Z = 0.40 CLUSTER OF GALAXIES pos_1: RA= 09H39M56.5S +/-0.1S, pos_2: DEC= +47D12'34" +/-1" equinox: 1950.0 pm_or_par: N rv_or_z: Z=0.40 ! targnum: 11 name_1: GAL-CLUS-3C295-FLD1 descr_1: Z = 0.46 CLUSTER OF GALAXIES pos_1: RA = 14H09M33.3S +/-0.1S, pos_2: DEC= +52D26'12" +/-1" equinox: 1950.0 pm_or_par: N rv_or_z: Z=0.46 ! targnum: 12 name_1: GAL-CLUS-3C295-FLD2 descr_1: Z = 0.46 CLUSTER OF GALAXIES pos_1: RA = 14H09M49.7S +/-0.1S, pos_2: DEC= +52D28'42" +/-1" equinox: 1950.0 pm_or_par: N rv_or_z: Z=0.46 ! targnum: 13 name_1: GAL-CLUS-144642+2621-FLD1 descr_1: Z = 0.37 CLUSTER OF GALAXIES pos_1: RA= 14H47M16.5S +/-0.1S, pos_2: DEC= +26D20'20" +/-1" equinox: 1950.0 pm_or_par: N rv_or_z: Z=0.37 comment_1: THESE POSITIONS MAY BE SLIGHTLY IN comment_2: ERROR; UPDATES WILL BE PROVIDED. ! targnum: 14 name_1: GAL-CLUS-144642+2621-FLD2 descr_1: Z = 0.37 CLUSTER OF GALAXIES pos_1: RA= 14H47M33.1S +/-0.1S, pos_2: DEC= +26D22'50" +/-1" equinox: 1950.0 pm_or_par: N rv_or_z: Z=0.37 comment_1: THESE POSITIONS MAY BE SLIGHTLY IN comment_2: ERROR; UPDATES WILL BE PROVIDED. ! targnum: 15 name_1: GAL-CLUS-160134+4254-FLD1 descr_1: Z = 0.53 CLUSTER OF GALAXIES pos_1: RA= 16H01M27.7S +/-0.1S, pos_2: DEC= +42D53'50" +/-1" equinox: 1950.0 pm_or_par: N rv_or_z: Z=0.53 ! targnum: 16 name_1: GAL-CLUS-160134+4254-FLD2 descr_1: Z = 0.53 CLUSTER OF GALAXIES pos_1: RA= 16H01M38.7S +/-0.1S, pos_2: DEC= +42D54'50" +/-1" equinox: 1950.0 pm_or_par: N rv_or_z: Z=0.53 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 sequence_1: DEFINE sequence_2: MEXP targname: # config: WFC opmode: IMAGE aperture: ALL sp_element: # num_exp: # time_per_exp: 2100S priority: # param_1: CR-SPLIT=NO, param_2: PRE-FLASH=NO comment_1: THIS SEQUENCE IS INTENDED TO FIT comment_2: EACH EXPOSURE INTO 1 ORBIT. comment_3: ADJUST EXPOSURE TIME +/- 20 PERCENT comment_4: TO ACCOMPLISH. comment_5: THIS IS THE CYCLE 2 VERSION OF THIS comment_6: PROPOSAL: AD/RAL 91/04/16 ! linenum: 2.000 sequence_1: USE sequence_2: MEXP targname: GAL-CLUS-001558+1609-FLD1 sp_element: F622W num_exp: 3 priority: 1 req_1: CYCLE 2 / 2-3; req_2: GROUP 2-3 WITHIN 1D; req_3: SAME POS FOR 3 AS 2; req_4: SAME ORIENT FOR 3 AS 2; req_5: POS TARG 0,0 / 2-11; req_6: COND IF TAC OK; ! linenum: 3.000 sequence_1: ^ targname: ^ sp_element: F725LP num_exp: 3 priority: ^ req_1: COND IF TAC OK; ! linenum: 4.000 sequence_1: USE sequence_2: MEXP targname: GAL-CLUS-093942+4713-FLD1 sp_element: F555W num_exp: 2 priority: 1 req_1: CYCLE 2 / 4-5; req_2: GROUP 4-5 WITHIN 1D; req_3: SAME POS FOR 5 AS 4; req_4: SAME ORIENT FOR 5 AS 4; req_5: COND IF TAC OK; ! linenum: 5.000 sequence_1: ^ targname: ^ sp_element: F814W num_exp: 2 priority: ^ req_1: COND IF TAC OK; ! linenum: 6.000 targname: GAL-CLUS-ABELL370-FLD2 config: WFC opmode: IMAGE aperture: ALL sp_element: F555W num_exp: 2 time_per_exp: 2100S priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=NO req_1: CYCLE 2 / 6-7; req_2: GROUP 6-7 WITHIN 1D; req_3: SAME POS FOR 7 AS 6; req_4: SAME ORIENT FOR 7 AS 6; req_5: COND IF TAC OK; ! linenum: 7.000 targname: GAL-CLUS-ABELL370-FLD2 config: WFC opmode: IMAGE aperture: ALL sp_element: F814W num_exp: 2 time_per_exp: 2100S priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=NO req_1: COND IF TAC OK; ! linenum: 8.000 sequence_1: USE sequence_2: MEXP targname: GAL-CLUS-144642+2621-FLD1 sp_element: F555W num_exp: 2 priority: 1 req_1: CYCLE 2 / 8-9; req_2: GROUP 8-9 WITHIN 1D; req_3: SAME POS FOR 9 AS 8; req_4: SAME ORIENT FOR 9 AS 8; req_5: COND IF TAC OK; ! linenum: 9.000 sequence_1: ^ targname: ^ sp_element: F814W num_exp: 2 priority: ^ req_1: COND IF TAC OK; ! linenum: 10.000 sequence_1: USE sequence_2: MEXP targname: GAL-CLUS-160134+4254-FLD1 sp_element: F622W num_exp: 3 priority: 1 req_1: CYCLE 2 / 10-11; req_2: GROUP 10-11 WITHIN 1D; req_3: SAME POS FOR 10 AS 11; req_4: SAME ORIENT FOR 10 AS 11; req_5: COND IF TAC OK; ! linenum: 11.000 sequence_1: ^ targname: ^ sp_element: F725LP num_exp: 3 priority: ^ req_1: COND IF TAC OK; ! linenum: 12.000 sequence_1: USE sequence_2: MEXP targname: GAL-CLUS-001558+1609-FLD2 sp_element: F622W num_exp: 3 priority: 1 req_1: CYCLE 2 / 12-13; req_2: GROUP 12-13 WITHIN 1D; req_3: SAME POS FOR 13 AS 12; req_4: SAME ORIENT FOR 13 AS 12; req_5: COND IF TAC OK; ! linenum: 13.000 sequence_1: ^ targname: ^ sp_element: F725LP num_exp: 3 priority: 1 req_1: COND IF TAC OK; ! linenum: 16.000 sequence_1: USE sequence_2: MEXP targname: GAL-CLUS-ABELL370-FLD1 sp_element: F555W num_exp: 2 priority: 1 req_1: CYCLE 2 / 16-17; req_2: GROUP 16-17 WITHIN 1D; req_3: SAME POS FOR 17 AS 16; req_4: SAME ORIENT FOR 17 AS 16; req_5: COND IF TAC OK; ! linenum: 17.000 sequence_1: ^ targname: ^ sp_element: F814W num_exp: 2 priority: ^ req_1: COND IF TAC OK; ! linenum: 18.000 sequence_1: USE sequence_2: MEXP targname: GAL-CLUS-030330+1706-FLD1 sp_element: F555W num_exp: 3 priority: 1 req_1: CYCLE 2 / 18-19; req_2: GROUP 18-19 WITHIN 1D; req_3: SAME POS FOR 19 AS 18; req_4: SAME ORIENT FOR 19 AS 18; req_5: COND IF TAC OK; ! linenum: 19.000 sequence_1: ^ targname: ^ sp_element: F814W num_exp: 2 priority: ^ req_1: COND IF TAC OK; ! linenum: 20.000 sequence_1: USE sequence_2: MEXP targname: GAL-CLUS-093942+4713-FLD2 sp_element: F555W num_exp: 2 priority: 1 req_1: CYCLE 2 / 20-21; req_2: GROUP 20-21 WITHIN 1D; req_3: SAME POS FOR 21 AS 20; req_4: SAME ORIENT FOR 21 AS 20; req_5: COND IF TAC OK; ! linenum: 21.000 sequence_1: ^ targname: ^ sp_element: F814W num_exp: 2 priority: ^ req_1: COND IF TAC OK; ! ! end of exposure logsheet ! No scan data records found