! Hubble Space Telescope Cycle 5 (1995) Phase II Proposal Template ! $Id: 5791,v 1.1 1994/12/14 19:05:22 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: ellingson-683.prop ! Date generated: Wed Dec 14 14:05:13 EST 1994 ! Proposal_Information ! Section 4 Title: Quasar Environments and Associated C IV Absorption Proposal_Category: AR Scientific_Category: Quasars Cycle: 5 Investigators PI_name: Erica Ellingson PI_Institution: Dept. of Astronomy, New Mexico State University CoI_Name: John Stocke CoI_Institution: Center for Astrophysics and Space Astronomy, U. Colorado Contact: ! Y or N (designate at most one contact) CoI_Name: Howard Yee CoI_Institution: Dept. of Astronomy, U. Toronto Contact: ! Y or N (designate at most one contact) CoI_Name: Jill Bechtold CoI_Institution: Steward Obs., U. Arizona Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) We propose to use HST FOS UV spectra of quasars with z < 1.0 to investigate the nature of associated (z_abs ~ z_em) C IV absorption line systems. These systems, which are often seen in the optical spectra of radio-loud quasars at z ~ 1.5, may be caused by the halos of galaxies in a cluster around the quasars, or may be intrinsic to the quasar itself. We will test these scenarios by comparing the incidence of associated absorption with our extensive imaging and spectroscopic observations of galaxies associated with quasars. Previous results suggest that if the galaxy halo scenario is true, then cluster galaxy halos may have undergone significant evolution since z ~ 1.5. Analysis of these new archival data will allow us to determine whether this is the case, and if so, study the evolution of galaxy halos in different environments for the first time. 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