! Proposal 5995, submission 2 ! PI: Olivier Le Fevre ! Received Tue Jun 6 03:55:21 EDT 1995 ! From: lefevre@DAEC.ObsPM.Fr ! Hubble Space Telescope Cycle 5 (1995) Phase II Proposal Template ! $Id: 5995,v 3.1 1995/06/21 19:41:47 pepsa Exp $ ! ! Refer to the HST Phase II Proposal Instructions to fill this out ! ! Anything after a "!" is ignored, and may be deleted ! ! All keywords with multiple entries are comma delimited except the ! Visit_Requirements and Special_Requirements keywords which can be ! delimited with carriage returns or semi-colons, but not commas ! ! For help call your Program Coordinator: Giselle Sleiman ! Phone: 410 338-4753 , E-mail: sleiman@stsci.edu ! ! This partially completed template was generated from a Phase I proposal. ! Date generated: Sun Dec 18 10:26:32 EST 1994 ! Proposal_Information ! Section 4 Title: Morphology of galaxies in very high redshift clusters: 3C265 (z=0.811), and 3C184 (z=0.996) Proposal_Category: GO Scientific_Category: Galaxies & Clusters Cycle: 5 Investigators PI_name: Olivier Le Fevre PI_Institution: Observatoire de Paris-Meudon Abstract: ! Free format text (please update) We are proposing to obtain morphological information on galaxies in two of the highest redshift clusters known at present. The environments of 3C265 (z=0.811) and 3C184 (z=0.996) have been shown by us to contain rich clusters: deep imaging and spectroscopy from the ground show an excess of galaxies, several of them subsequently identified at the same redshift as the radio-galaxy in spectroscopy. The morphological state of galaxies in high redshift clusters should give us important clues about the formation and evolution of galaxies in dense environments and the formation of clusters. The role played by mergers into the observed raise in the blue active fraction of galaxies with redshift (the Butcher-Oemler effect), the location of star forming regions, and the shape of "normal" elliptical and spiral galaxies, and their differences with galaxies in present day clusters, can be ideally assessed from HST imaging with WFPC2. Only a handful of clusters are known at z>0.8, these observations are expected to bring unique clues on the evolution of galaxies in clusters when the universe was 40% of its present age. Questions ! Free format text (please update) Observing_Description: Observations will be performed in the F606W and F814W filters, in the WF. For typical cluster galaxies at z=0.8 and z=1, A S/N>1 for mu_V=26.5 will probe I=19-22 galaxies at least 3 magnitudes fainter than the central surface brightness of "disc" galaxies (a disc has mu_I=21+10log(1+z) at z=0.8). 8 consecutive orbits will be needed on 3C184 to obtain a total integration time of 9510 sec. in F606W, and 12690 sec. in F814W, which will yield a S/N=3 for mu_V=25.3 mag/arcsec^2 and mu_I=24.6 mag/arcsec^2 respectively. The calcultations are as follows:, beginitemize item F606W: From the WFPC2 handbook pp.56-58 the sky brightness with mu_V=23.3 mag/arcsec^2, and an efficiency of 0.04485, will give 0.0485 e^-/sec/pixel; a galaxy at mu_V=25.3 mag/arcsec^2 will give 0.00851 e^-/sec/pixel, and the dark current at -77^degreesC is 0.016 e^-/sec/pixel. The S/N in 9510 sec will then be, fracSN=\frac0.00851*9510SQRT(5.2^2+(0.00851+0.0485+0.016)*951 0) = 3 item F814W: for AB_Nu=-0.5 and an efficiency of 0.01822, the sky will give 0.03618 e^-/sec/pixel; a galaxy at mu_I=24.6 will give 0.0104 e^-/sec/pixel. The S/N in 12690 sec. will be, fracSN=\frac0.0104*12690SQRT(5.2^2+(0.0104+0.0485+0.016)*1269 0)= 3 enditemize Seven consecutive orbits will be necessary on 3C265 to obtain exposure times of 7020 sec and 9720 sec in F606W and F814W respectively. Similar calculations as shown above indicate that a S/N=3 will be reached for mu_V=25.1 and mu_I=24.4 in F606W and F814W respectively. Small shifts between each exposure (on order 20 min) and a minimum of 6 exposures per filter will be obtained to best remove cosmic rays and low level flat field defects. A total of 15 orbits is then requested for this program. Real_Time_Justification: Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: The TAC has recommended to observe 3C184 only, for 4 orbits. Fixed_Targets ! Section 5.1 Target_Number:1 Target_Name:GAL-CLUS-073924+702311 Alternate_Names: Description:CLUSTER OF GALAXIES, HIGH REDSHIFT CLUSTER (Z>0.5) Position:RA = 07H33M59.01S +/-0.19S, DEC = +70D30' 1.1" +/-1.0" ! Most common specification format is ! RA=0H 0M 0.00S +/- 0S, ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 Equinox:1950 RV_or_Z:Z=0.994 RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux:V=21.5 B-V=0.52 V-R=0.11 ! Include at least V and B-V Comments:Flux is for radio-galaxy, cluster galaxies have fluxes from V=22.0 down to the computed HST plate limit. !Solar_System_Targets ! Section 5.2 ! Target_Number: ! Target_Name: ! Description: ! Level_1: ! Satellite of Sun ! Level_2: ! Satellite of Level_1 ! Level_3: ! Satellite of Level_2 ! Window: ! Flux: ! Include at least V and B-V ! Comments: !Generic_Targets ! Section 5.3 ! Target_Number: ! Target_Name: ! Description: ! Criteria: ! Flux: ! Comments: !Scan_Data ! Appendix B ! Scan_Number: ! FGS_Scan: ! Cont_or_Dwell: ! Dwell_Points: ! Dwell_Secs: ! Scan_Width: ! Scan_Length: ! Sides_Angle: ! Number_Lines: ! Scan_Rate: ! First_Line_PA: ! Scan_Frame: ! Length_Offset: ! Width_Offset: ! This is a template for a single visit containing a single exposure ! Repeat exposure and visit blocks as needed Visits ! Section 6 Visit_Number:1 Visit_Requirements:PCS MODE F ! Section 7.1 ! Uncomment or copy visit level special requirements needed ! Most of these requirements (including ORIENT) will limit scheduling ! PCS MODE [Fine | Gyro] ! GUIDing TOLerance ! ORIENTation TO ! ORIENTation TO FROM ! ORIENTation TO FROM NOMINAL ! SAME ORIENTation AS CVZ ! PARallel ! AFTER [BY [TO ]] ! AFTER ! BEFORE ! BETWEEN AND ! GROUP WITHIN