! File: 5402P.PROP ! Database: PEPDB ! Date: 14-FEB-1994:14:56:57 coverpage: title_1: MULTIPLE ARC SYSTEMS IN X-RAY SELECTED title_2: CLUSTERS: CYCLE4MEDIUM sci_cat: GALAXIES & CLUSTERS sci_subcat: CLUSTERS/LENSES proposal_for: GO pi_fname: ISABELLA pi_mi: M. pi_lname: GIOIA pi_inst: 2192 pi_country: USA pi_phone: 808-956-9845 hours_pri: 15.00 wf_pc: Y off_fname: MOHEB off_lname: GHALI off_title: DIRECTOR OF RESEARCH off_inst: OFFICE OF RESEARCH ADMINISTRATION off_addr_1: 2540 MAILE WAY off_addr_2: SPALDING 253 off_city: HONOLULU off_state: HI off_zip: 96822 off_country: USA off_phone: 808-956-8612 ! end of coverpage abstract: line_1: We propose to observe two X-ray luminous clusters of galaxies line_2: MS0440.5+0204 and MS2137.3-2353 which contain multiple line_3: gravitationally lensed arc systems. The high resolution of line_4: WFPC-2 will allow us to accurately determine the masses line_5: for the lensing clusters and to do detailed reconstruction of the line_6: lensing sources through lensing models that we have developed. line_7: Since the magnification factor along the arcs is greater than 10, line_8: a 0.1 arcsec detail will represent a 0.01 arcsec detail in the line_9: source, which corresponds to 100 pc at redshift z = 1 line_10: (Ho=50 km/s/Mpc). This resolution cannot be obtained by any line_11: other means. The HST observations will be complemented line_12: by ROSAT HRI and Astro-D observations of the same clusters, line_13: and will allow us to compare the properties of the line_14: lensing mass as determined from the optical data with line_15: the mass of the cluster potential as derived from the line_16: X-ray observations. The two methods are independent ways line_17: of studying the mass distribution, each one providing strong line_18: constraints. ! ! end of abstract general_form_proposers: lname: GIOIA fname: ISABELLA mi: M. inst: 2192 country: USA ! lname: LUPPINO fname: GERARD mi: A. inst: 2192 country: USA ! lname: HAMMER fname: FRANCOIS inst: 1640 country: USA ! lname: LEFEVRE fname: OLIVIER inst: 1640 country: USA ! lname: SHAYA fname: EDWARD mi: J. inst: 2620 country: USA ! lname: ANNIS fname: JAMES mi: T. inst: 1990 country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: The Wide Field/Planetary Camera 2 will be used to observe the line_2: gravitationally lensed arcs in the clusters of galaxies MS0440.5+0204 line_3: and MS2137.3-2353. We have already detected the arcs using ground based line_4: telescopes. The WFPC-2 will allows us to reach the very high resolution line_5: needed for the modeling of the lensing sources. Consequently the data line_6: will be obtained in FULL mode. The best performance CCD has been chosen line_7: since at the redshift of the clusters they both fit very nicely inside line_8: the circa 1' x 1' FOV of WF3. We will use the additional time awarded to line_9: us during the phase I review to go deeper in each field rather than line_10: to observe through different filters. Since we already have colors from line_11: ground based observations we will use only the "Wide R" line_12: filter and try to detect the fainter arcs. The planned observations line_13: are quite straightforward, requiring blind acquisition at two single line_14: well determined positions. They will consist of 1 x 2200s exposure line_15: (splitted in half to identify cosmic ray events) per orbit for 20 line_16: orbits for a total observing time of 5.5 hours for MS0440.5+0204 and line_17: 6.2 hours for MS2137.3-2353. To ensure proper flux calibration, a line_18: red standard star needs to be observed. ! question: 3 section: 2 line_1: We plan to examine the data from the first 3 orbits for each cluster line_2: and have a waiting period of about 50 days before the rest of the data line_3: is taken. This will allow us to make small changes and to optimize line_4: exposure times, CR-SPLITting, etc. Consequently we have chosen the line_5: NO GAP mode for the first 3 orbits and no restriction for the line_6: remaining exposures to be taken about 7 weeks after the 1st orbit. line_7: We also require the same orientation for each cluster and offsets line_8: of 1 to 3 arcsec in X and Y to remove possible effects of bad pixels, line_9: bad columns, undersampling, etc. To reach our scientific goals involving line_10: detection of very thin and very faint arcs down to mu(R)~/=24-25, we line_11: have to remove all the possible instrumental and cosmic ray effects. ! question: 4 section: 1 line_1: We have used the Tektronix 2048x2048 CCD at the f/10 focus of the line_2: University of Hawaii 2.2 meter telescope on Mauna Kea (0.22"/pix) and line_3: the High Resolution Camera on the CFHT equipped with SAIC-2 1024x1024 line_4: CCD with 0.13 arcsec pixel for MS0440.5+0204. MS2137.3-2353 has been line_5: observed at CFHT with FOCam (scale=0.206"/pix), and at ESO NTT and 3.6m line_6: telescopes by 2 Co-I's of this proposal (FH and OL) in collaboration line_7: with the Toulouse group. Exposures have been taken in BVRI filters. line_8: Even with seeing as good as 0.5" (FWHM), some arc images are unresolved. line_9: HST is clearly the only telescope capable of carrying out the proposed line_10: observations. The high resolution of HST/WFPC-2 is critical for this line_11: experiment. Besides the already known arcs, HST may reveal yet line_12: undetected arclets since we expect them to be thin and short. ! question: 6 section: 1 line_1: We need flat fields with the WFPC-2 for the F702W filter. As well as line_2: a PSF observation made by a short exposure of a single bright star line_3: in the F702W filter. It is our understanding that these will be made line_4: available by the HST team. A red standard star needs also to be line_5: observed through the same filter to ensure proper flux calibration. ! question: 7 section: 1 line_1: The data obtained with HST will be reduced on a SUN workstation at the line_2: Institute for Astronomy, University of Hawaii, using IRAF and/or VISTA. line_3: Each one of the investigators has a considerable experience reducing line_4: astronomical images with one or both of these packages. A key line_5: measurement parameter will be the elongation ratio of gravitaional lens line_6: arclets where the short axis dimension will be near the HST resolution line_7: limit. A major part of the interpretation rests with the gravitational line_8: lens modeling. The modeling software has been developed and is being line_9: improved in collaboration with astronomers at the Observatoire de line_10: Meudon. It will be tested and run at the Institute for Astronomy, the line_11: home institution of the PI and one of the Co-I's. ! question: 9 section: 1 line_1: Only one of the proposers (E. Shaya) has been previously working with line_2: HST data. He is a member of the WFPC-1 GTO team and has been heavily line_3: involved in the data reductions. His work has contributed to the line_4: publication of nine papers in either the Astron. J. or the Astrophys. line_5: J. The science relationship of his previous work with this proposal has line_6: been with the paper "Imaging of the Gravitation Lens System PG1115+080 line_7: with the Hubble Space Telescope" submitted to the Astron. Journal. This line_8: study involved the measurement of accurate positions and relative line_9: intensities of lensed images of quasars and fits to gravitational line_10: lens models. ! question: 10 section: 1 line_1: A key resource at the Institute for Astronomy is access to ground-based line_2: telescopes for complementary studies. In particular, multi-band imaging line_3: and spectroscopy will be pursued - two vital ingredients along with line_4: the high resolution HST images for the modeling. A network line_5: of public and private SUN workstations are connected by ethernet line_6: at the Institute for Astronomy. However, the public disk capacity and line_7: the public workstations are heavily subscribed. To reduce and analyze line_8: the HST data in a timely and efficient manner, funding is requested line_9: through this proposal for the purchase of a workstation and a 2 Gbyte line_10: SCSI disk. The Institute provides support for all publication line_11: requirements including graphics capabilities. ! !end of general form text general_form_address: lname: Gioia fname: Isabella mi: M. category: PI inst: 2192 addr_1: Institute for Astronomy addr_2: University of Hawaii addr_3: 2680 Woodlawn Drive city: Honolulu state: HI zip: 96822 country: USA phone: 808-956-9845 telex: gioia@galileo.ifa.hawaii.edu FAX 808-988-2790 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: MS0440.5+0204 name_2: GAL-CLUS-044033+020447 descr_1: F,404,411,409,920 pos_1: RA = 04H 40M 33.8S +/- 0.1S, pos_2: DEC = 02D 04' 47.5" +/- 1.0" equinox: 1950 rv_or_z: Z=0.19 fluxnum_1: 1 fluxval_1: SURF(R) = 23.9 +/- 0.2 fluxnum_2: 2 fluxval_2: V = 22.1 +/- 0.2 fluxnum_3: 2 fluxval_3: SURF(V) = 24.2 +/- 0.2 fluxnum_4: 2 fluxval_4: B-V = 0.8 +/- 0.2 fluxnum_5: 2 fluxval_5: E(B-V) = 0.09 +/- 0.2 ! targnum: 2 name_1: MS2137.3-2353 name_2: GAL-CLUS-213723-235319 descr_1: F,404,411,409,911 pos_1: RA = 21H 37M 23.7S +/- 0.1S, pos_2: DEC = -23D 53' 19.3" +/- 1.0" equinox: 1950 rv_or_z: Z=0.313 fluxnum_1: 1 fluxval_1: SURF(R) = 24.4 +/- 0.25 fluxnum_2: 2 fluxval_2: V = 22 +/- 0.25 fluxnum_3: 2 fluxval_3: SURF(V) = 24.9 +/- 0.25 fluxnum_4: 2 fluxval_4: B-V = 0.04 +/- 0.25 fluxnum_5: 2 fluxval_5: E(B-V) = 0.03 +/- 0.25 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: MS0440.5+0204 config: WFPC2 opmode: IMAGE aperture: WF3-FIX sp_element: F702W wavelength: 6895 num_exp: 1 time_per_exp: 1900S s_to_n: 2.1 s_to_n_time: 1100S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO req_1: CYCLE 4/1-10; req_2: SAME ORIENT FOR 2-10 AS 1; req_3: SEQ 1.0-5.0 NO GAP comment_1: THE CALCULATED S/N IS PER PIXEL comment_2: PER 1100S AT SURF(R)=23.5 MAG/"SQ. ! linenum: 2.000 targname: MS0440.5+0204 config: WFPC2 opmode: IMAGE aperture: WF3-FIX sp_element: F702W wavelength: 6895 num_exp: 1 time_per_exp: 2300S s_to_n: 2.1 s_to_n_time: 1100S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO req_1: POS TARG +0.5, +0.5 comment_1: THE CALCULATED S/N IS PER PIXEL comment_2: PER 1100S AT SURF(R)=23.5 MAG/"SQ. comment_3: OFFSET IN X AND Y TO REMOVE comment_4: POSSIBLE EFFECTS OF BAD PIXELS, ETC. ! linenum: 3.000 targname: MS0440.5+0204 config: WFPC2 opmode: IMAGE aperture: WF3-FIX sp_element: F702W wavelength: 6895 num_exp: 1 time_per_exp: 2300S s_to_n: 2.1 s_to_n_time: 1100S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO req_1: POS TARG +1, -1 comment_1: THE CALCULATED S/N IS PER PIXEL comment_2: PER 1100S AT SURF(R)=23.5 MAG/"SQ. comment_3: OFFSET IN X AND Y TO REMOVE comment_4: POSSIBLE EFFECTS OF BAD PIXELS, ETC. ! linenum: 4.000 targname: MS0440.5+0204 config: WFPC2 opmode: IMAGE aperture: WF3-FIX sp_element: F702W wavelength: 6895 num_exp: 1 time_per_exp: 2300S s_to_n: 2.1 s_to_n_time: 1100S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO req_1: POS TARG -0.5, -0.5 comment_1: THE CALCULATED S/N IS PER PIXEL comment_2: PER 1100S AT SURF(R)=23.5 MAG/"SQ. comment_3: OFFSET IN X AND Y TO REMOVE comment_4: POSSIBLE EFFECTS OF BAD PIXELS, ETC. ! linenum: 5.000 targname: MS0440.5+0204 config: WFPC2 opmode: IMAGE aperture: WF3-FIX sp_element: F702W wavelength: 6895 num_exp: 1 time_per_exp: 2300S s_to_n: 2.1 s_to_n_time: 1100S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO req_1: POS TARG -1, +1 comment_1: THE CALCULATED S/N IS PER PIXEL comment_2: PER 1100S AT SURF(R)=23.5 MAG/"SQ. comment_3: OFFSET IN X AND Y TO REMOVE comment_4: POSSIBLE EFFECTS OF BAD PIXELS, ETC. ! linenum: 6.000 targname: MS0440.5+0204 config: WFPC2 opmode: IMAGE aperture: WF3-FIX sp_element: F702W wavelength: 6895 num_exp: 1 time_per_exp: 1900S s_to_n: 2.1 s_to_n_time: 1100S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO req_1: POS TARG +1.5, +1.5; req_2: SEQ 6.0-10.0 NO GAP comment_1: THE CALCULATED S/N IS PER PIXEL comment_2: PER 1100S AT SURF(R)=23.5 MAG/"SQ. comment_3: OFFSET IN X AND Y TO REMOVE comment_4: POSSIBLE EFFECTS OF BAD PIXELS, ETC. ! linenum: 7.000 targname: MS0440.5+0204 config: WFPC2 opmode: IMAGE aperture: WF3-FIX sp_element: F702W wavelength: 6895 num_exp: 1 time_per_exp: 2300S s_to_n: 2.1 s_to_n_time: 1100S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO req_1: POS TARG +2, -1.5 comment_1: THE CALCULATED S/N IS PER PIXEL comment_2: PER 1100S AT SURF(R)=23.5 MAG/"SQ. comment_3: OFFSET IN X AND Y TO REMOVE comment_4: POSSIBLE EFFECTS OF BAD PIXELS, ETC. ! linenum: 8.000 targname: MS0440.5+0204 config: WFPC2 opmode: IMAGE aperture: WF3-FIX sp_element: F702W wavelength: 6895 num_exp: 1 time_per_exp: 2300S s_to_n: 2.1 s_to_n_time: 1100S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO req_1: POS TARG -1.5, -2 comment_1: THE CALCULATED S/N IS PER PIXEL comment_2: PER 1100S AT SURF(R)=23.5 MAG/"SQ. comment_3: OFFSET IN X AND Y TO REMOVE comment_4: POSSIBLE EFFECTS OF BAD PIXELS, ETC. ! linenum: 9.000 targname: MS0440.5+0204 config: WFPC2 opmode: IMAGE aperture: WF3-FIX sp_element: F702W wavelength: 6895 num_exp: 1 time_per_exp: 2300S s_to_n: 2.1 s_to_n_time: 1100S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO req_1: POS TARG -2, +2 comment_1: THE CALCULATED S/N IS PER PIXEL comment_2: PER 1100S AT SURF(R)=23.5 MAG/"SQ. comment_3: OFFSET IN X AND Y TO REMOVE comment_4: POSSIBLE EFFECTS OF BAD PIXELS, ETC. ! linenum: 10.000 targname: MS0440.5+0204 config: WFPC2 opmode: IMAGE aperture: WF3-FIX sp_element: F702W wavelength: 6895 num_exp: 1 time_per_exp: 2300S s_to_n: 2.1 s_to_n_time: 1100S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO req_1: POS TARG +2.5, +2.5 comment_1: THE CALCULATED S/N IS PER PIXEL comment_2: PER 1100S AT SURF(R)=23.5 MAG/"SQ. comment_3: OFFSET IN X AND Y TO REMOVE comment_4: POSSIBLE EFFECTS OF BAD PIXELS, ETC. ! linenum: 11.000 targname: MS2137.3-2353 config: WFPC2 opmode: IMAGE aperture: WF3-FIX sp_element: F702W wavelength: 6895 num_exp: 1 time_per_exp: 1900S s_to_n: 1.4 s_to_n_time: 1100S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO req_1: CYCLE 4 / 11-20; req_2: SAME ORIENT FOR 12-20 AS 11; req_3: SEQ 11-15 NO GAP comment_1: THE CALCULATED S/N IS PER PIXEL comment_2: PER 1100S AT SURF(R)=24 MAG/"SQ. ! linenum: 12.000 targname: MS2137.3-2353 config: WFPC2 opmode: IMAGE aperture: WF3-FIX sp_element: F702W wavelength: 6895 num_exp: 1 time_per_exp: 2300S s_to_n: 1.4 s_to_n_time: 1100S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO req_1: POS TARG +0.5, +0.5 comment_1: THE CALCULATED S/N IS PER PIXEL comment_2: PER 1100S AT SURF(R)=24 MAG/"SQ. comment_3: OFFSET IN X AND Y TO REMOVE comment_4: POSSIBLE EFFECTS OF BAD PIXELS, ETC. ! linenum: 13.000 targname: MS2137.3-2353 config: WFPC2 opmode: IMAGE aperture: WF3-FIX sp_element: F702W wavelength: 6895 num_exp: 1 time_per_exp: 2300S s_to_n: 1.4 s_to_n_time: 1100S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO req_1: POS TARG +1, -1 comment_1: THE CALCULATED S/N IS PER PIXEL comment_2: PER 1100S AT SURF(R)=24 MAG/"SQ. comment_3: OFFSET IN X AND Y TO REMOVE comment_4: POSSIBLE EFFECTS OF BAD PIXELS, ETC. ! linenum: 14.000 targname: MS2137.3-2353 config: WFPC2 opmode: IMAGE aperture: WF3-FIX sp_element: F702W wavelength: 6895 num_exp: 1 time_per_exp: 2300S s_to_n: 1.4 s_to_n_time: 1100S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO req_1: POS TARG -0.5, -0.5 comment_1: THE CALCULATED S/N IS PER PIXEL comment_2: PER 1100S AT SURF(R)=24 MAG/"SQ. comment_3: OFFSET IN X AND Y TO REMOVE comment_4: POSSIBLE EFFECTS OF BAD PIXELS, ETC. ! linenum: 15.000 targname: MS2137.3-2353 config: WFPC2 opmode: IMAGE aperture: WF3-FIX sp_element: F702W wavelength: 6895 num_exp: 1 time_per_exp: 2300S s_to_n: 1.4 s_to_n_time: 1100S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO req_1: POS TARG -1, +1 comment_1: THE CALCULATED S/N IS PER PIXEL comment_2: PER 1100S AT SURF(R)=24 MAG/"SQ. comment_3: OFFSET IN X AND Y TO REMOVE comment_4: POSSIBLE EFFECTS OF BAD PIXELS, ETC. ! linenum: 16.000 targname: MS2137.3-2353 config: WFPC2 opmode: IMAGE aperture: WF3-FIX sp_element: F702W wavelength: 6895 num_exp: 1 time_per_exp: 1900S s_to_n: 1.4 s_to_n_time: 1100S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO req_1: POS TARG +1.5, +1.5; req_2: SEQ 16.0-20.0 NO GAP comment_1: THE CALCULATED S/N IS PER PIXEL comment_2: PER 1100S AT SURF(R)=24 MAG/"SQ. comment_3: OFFSET IN X AND Y TO REMOVE comment_4: POSSIBLE EFFECTS OF BAD PIXELS, ETC. ! linenum: 17.000 targname: MS2137.3-2353 config: WFPC2 opmode: IMAGE aperture: WF3-FIX sp_element: F702W wavelength: 6895 num_exp: 1 time_per_exp: 2300S s_to_n: 1.4 s_to_n_time: 1100S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO req_1: POS TARG +2, -1.5 comment_1: THE CALCULATED S/N IS PER PIXEL comment_2: PER 1100S AT SURF(R)=24 MAG/"SQ. comment_3: OFFSET IN X AND Y TO REMOVE comment_4: POSSIBLE EFFECTS OF BAD PIXELS, ETC. ! linenum: 18.000 targname: MS2137.3-2353 config: WFPC2 opmode: IMAGE aperture: WF3-FIX sp_element: F702W wavelength: 6895 num_exp: 1 time_per_exp: 2300S s_to_n: 1.4 s_to_n_time: 1100S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO req_1: POS TARG -1.5, -2 comment_1: THE CALCULATED S/N IS PER PIXEL comment_2: PER 1100S AT SURF(R)=24 MAG/"SQ. comment_3: OFFSET IN X AND Y TO REMOVE comment_4: POSSIBLE EFFECTS OF BAD PIXELS, ETC. ! linenum: 19.000 targname: MS2137.3-2353 config: WFPC2 opmode: IMAGE aperture: WF3-FIX sp_element: F702W wavelength: 6895 num_exp: 1 time_per_exp: 2300S s_to_n: 1.4 s_to_n_time: 1100S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO req_1: POS TARG -2, +2 comment_1: THE CALCULATED S/N IS PER PIXEL comment_2: PER 1100S AT SURF(R)=24 MAG/"SQ. comment_3: OFFSET IN X AND Y TO REMOVE comment_4: POSSIBLE EFFECTS OF BAD PIXELS, ETC. ! linenum: 20.000 targname: MS2137.3-2353 config: WFPC2 opmode: IMAGE aperture: WF3-FIX sp_element: F702W wavelength: 6895 num_exp: 1 time_per_exp: 2300S s_to_n: 1.4 s_to_n_time: 1100S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO req_1: POS TARG +2.5, +2.5 comment_1: THE CALCULATED S/N IS PER PIXEL comment_2: PER 1100S AT SURF(R)=24 MAG/"SQ. comment_3: OFFSET IN X AND Y TO REMOVE comment_4: POSSIBLE EFFECTS OF BAD PIXELS, ETC. ! ! end of exposure logsheet ! No scan data records found