! Proposal 6720, submission 1 ! PI: Matthew Lehnert ! Received Fri Feb 9 12:19:16 EST 1996 ! From: lehnert@strw.LeidenUniv.nl ! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6720,v 4.1 1996/12/04 19:42:51 pepsa Exp $ ! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6720,v 4.1 1996/12/04 19:42:51 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: van Orsow ! Phone: 410-338-4568 , E-mail: vanorsow@stsci.edu ! ! This partially completed template was generated from a Phase I proposal. ! Name of Phase I Proposal: archive-0857.lehnert.prop ! Date generated: Fri Dec 22 18:58:45 EST 1995 ! Proposal_Information ! Section 4 Title: The Evolution of Radio-Loud Quasars II Proposal_Category: GO Scientific_Category: AGN Cycle: 6 Investigators PI_name: Matthew Lehnert PI_Institution: Institute of Geophysics and Planetary Physics CoI_Name: Wil van Breugel CoI_Institution: Institute of Geophysics and Planetary Physics, LLNL, 7000 East Ave., L-413, Livermore, CA 94550 Contact: ! Y or N (designate at most one contact) CoI_Name: Vijay Kapahi CoI_Institution: National Center for Radio Astrophysics, TIFR, Pune 411 007, India Contact: ! Y or N (designate at most one contact) CoI_Name: Timothy Heckman CoI_Institution: Dept. of Physics & Astron, Johns Hopkins University, Baltimore, MD 21218 Contact: ! Y or N (designate at most one contact) CoI_Name: Patrick McCarthy CoI_Institution: Carnegie Observatories, 813 Santa Barbara St., Pasadena, CA 91101 Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) The first HST results from our cycle 5 mini-survey of a carefully selected sample of radio quasars show dramatic evolution in the morphologies and luminosities of their host galaxies between 0.3 < z < 2.7. Our complete sample is unique in that the quasars span a range of radio properties, are uniformly spread in look-back time, are imaged at the same (2000 Angstrom) restframe, and to approximately the same (observed) limiting surface brightness. We believe that our careful selection is crucial for investigating the properties and evolution of quasar host galaxies and our early results seem to bear this out. In view of the many unknown factors which may govern quasar and quasar-host evolution, and the already clear evidence for strong evolutionary effects (in short, 1 - 2 orbit exposures .), we propose to complete our original request to observe all 20 quasars from our sample. This will provide us with a sufficient number of quasars to allow some confidence in general conclusions and, in particular, to search for evolutionary differences/connections between the various radio source classes. When compared with the sofar much better studied radio galaxies in other HST programs, we will be able to address the important question of whether radio-loud quasars and radio galaxies are members of the same parent population as is fashionable in the AGN unification schemes, and investigate how the hosts of luminous AGN have evolved over the epochs where luminous quasars have become virtually extinct. Questions ! Free format text (please update) Observing_Description: Quasar Sample Our quasars all have redshifts of between 0.276 and 2.667 and are chosen from the Molonglo Reference Catalog of radio sources. We have split the sample into four redshift bins (z<0.7, 0.7 -0.5). The current request will complete our scheduled Cycle 5 program, which was reduced by 50\% from 20 to 10 targets. In view of the the already clear evidence for strong evolutionary effects (in short, 1 - 2 orbit exposures .), and the many unknown factors which may govern quasar and quasar-host evolution, we propose to complete our original request to observe all 20 quasars from our sample. 0.1in Continuum Imaging Our choice of continuum filter is dictated by three criteria. First, the filter bandpass should exclude bright emission lines. Second, the filter should be among the most efficient broad- band filters available on the WFPC2 and also correspond roughly to common ground-based filters to yield `real' magnitudes. Third, the central wavelength should correspond roughly to a uniform rest wavelength in all the quasars over the whole redshift range. The most suitable choices are F336W (~U, for quasars with z<0.7), F439W (~B, for quasars with 0.7 Sterrewacht Leiden ! PI Address from Phase I is: 2300 RA Leiden ! The Netherlands ! LLNL, L-413 ! 7000 East Ave. ! Livermore ! 94550 ! ! Ship_Via: UPS ! UPS (2-day) or OVERNIGHT ! Overnight shipping done at PI expense Recipient_Email: ! Needed if Ship_To: is not PI_Address ! ! Let us know what you think of this template and software! ! Please send a list of your likes and dislikes to your Program Coordinator