! Hubble Space Telescope Cycle 5 (1995) Phase II Proposal Template ! $Id: 5790,v 1.1 1994/12/14 19:03:30 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: n/a ! Phone: n/a , E-mail: n/a ! ! This partially completed template was generated from a Phase I proposal. ! Name of Phase I Proposal: eisenhardt-908.prop ! Date generated: Wed Dec 14 14:03:23 EST 1994 ! Proposal_Information ! Section 4 Title: Tracking the Red Envelope: Elliptical Galaxy Evolution in High Redshift Galaxy Clusters Proposal_Category: AR Scientific_Category: Galaxies & Clusters Cycle: 5 Investigators PI_name: Peter Eisenhardt PI_Institution: Jet Propulsion Laboratory/California Institute of Technology CoI_Name: Adam Stanford CoI_Institution: Jet Propulsion Laboratory/California Institute of Technology Contact: ! Y or N (designate at most one contact) CoI_Name: Mark Dickinson CoI_Institution: Space Telescope Science Institute Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) We propose to obtain images of 12 high redshift galaxy clusters from the HST Archive. We have obtained deep, wide- field near-IR imaging of these clusters as part of our survey of ~30 rich clusters up to z=1.0. The primary goal of our near -IR imaging survey is to study the evolution of the elliptical galaxy population as a function of redshift in galaxy clusters. The high spatial resolution of HST imaging enables us to determine morphological types for high redshift galaxies. We will use WFPC2 images of our clusters from the Archive to extract elliptical subsamples from our near-IR selected galaxy catalogs on the basis of their HST morphology rather than on the basis of an assumed red color. The resulting elliptical samples, unbiased by optical color selection effects, will allow us to study the color evolution of ellipticals to z=1 and test the passive evolution scenario. By comparing the change in the mean colors of the ellipticals with spectral synthesis models over a lookback time of ~10 Gyr we hope to be able to synchronize the cosmological and stellar evolutionary clocks. Questions ! Free format text (please update) Observing_Description: Real_Time_Justification: Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: Fixed_Targets ! Section 5.1 Target_Number: Target_Name: Alternate_Names: Description: Position: ! Most common specification format is ! RA=0H 0M 0.00S +/- 0S, ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 Equinox: RV_or_Z: RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: ! Include at least V and B-V Comments: 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: Visit_Requirements: ! 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