! Proposal 6608, submission 1 ! PI: Wil van Breugel ! Received Sun Feb 11 19:47:21 EST 1996 ! From: dey@noao.edu ! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6608,v 3.1 1996/02/12 15:58:05 pepsa Exp $ ! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6608,v 3.1 1996/02/12 15:58:05 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: Lucas ! Phone: 410-338-4716 , E-mail: lucas@stsci.edu ! ! This partially completed template was generated from a Phase I proposal. ! Name of Phase I Proposal: archive-0565.van_breugel.prop ! Date generated: Fri Dec 22 16:33:29 EST 1995 ! Proposal_Information ! Section 4 Title: DETAILED STUDIES OF TWO Z > 3.5 RADIO GALAXIES Proposal_Category: GO Scientific_Category: COSMOLOGY Cycle: 6 Investigators PI_name: Wil van Breugel PI_Institution: Lawrence Livermore National Laboratory CoI_Name: Huub Roettgering CoI_Institution: Leiden Observatory Contact: ! Y or N (designate at most one contact) CoI_Name: George Miley CoI_Institution: Leiden Observatory Contact: ! Y or N (designate at most one contact) CoI_Name: Hyron Spinrad CoI_Institution: University of California, Berkeley Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) A moderately deep image (6 hrs, F702W+WFPC2) of one of the highest redshift radio galaxies (4C41.17 at z = 3.80) has shown that the rest-frame UV continuum has 1) numerous bright knots along the inner radio source axis, and 2) a clumpy companion system. Both components appear embedded in a common halo of diffuse emission. These observations suggest that we may be witnessing, for the first time, the formation of a galaxy due to the merging of (star forming?) subclumps, as predicted in dissipative galaxy formation scenarios, and of the effects of a young (quasar like ?) AGN on this environment. We propose to obtain a deep HST rest-frame UV (F702W) image of one other z > 3.5 radio galaxy which we have discovered in our ongoing groundbased surveys: 4C 0512+60 at z = 3.790. Combined with extensive groundbased (Keck) observations and future HST NICMOS near-IR imaging and STIS longslit spectroscopy these data will provide crucial new information about key factors which shape young HZRGs (galaxy, AGN, environment, redshift), and will allow us to explore the possible connection between galaxy formation and the origin of AGN, and to test certain attributes of radio galaxy / quasar `unification' models. Questions ! Free format text (please update) Observing_Description: Our aims for the current proposal are to explore whether the rest-frame UV and Ly-alpha morphologies such as seen 4C41.17 (clumpy structure, aligned component, nearby companion, and diffuse halo) are a common property of very HZRGs. Our groundbased, 0.5 " seeing data of 4C 0512+60 (z = 3.790) shows good reason to suspect that this is the case, but the high spatial resolution of HST is essential for imaging their morphologies in detail. Perhaps the most surprising new result from the 4C41.17 observations has been the discovery of its clumpy, amorphous companion system. Its diffuse halo and morphological connection to 4C41.17 itself was not seen in the pre-Costar HST images (Miley Etal 1992, ApJ. 401 L69), nor could it have been detected in post-Costar images with the 4 times shorter exposure times used in the cycle 5 and the (proposed) cycle 6 'mini-survey' of HZRG structures. Indeed, even deeper observations of 4C41.17 itself would have been helpful since much of the diffuse F702W continuum emission is only visible at the 2 -- 3 Sigma, or 25.2 mag/(sq.arcsec) level. The faintest clumps in the 4C41.17 field are 26.7 mag. We will examine the usefulness of an ultradeep image, like the 32 orbit exposure of 3C324 by Dickinson Etal, of one of the z > 3.5 radio galaxies when we have high quality data on a number of them. 4C 0512+60 (m_R ~ 23.5) is 0.3 mag fainter than 4C41.17. It is unclear whether this means that the individual clumps will be also fainter, whether there will be fewer of them, or whether the low surface brightness emission will be lower. Since this target is at nearly the same redshift as 4C41.17 we choose to image this object to the same depth (10 orbits) allowing us to evaluate the morphological similarities/differences between these HZRGs at the same sensitivity levels. Real_Time_Justification: None. Calibration_Justification: ! Move appropriate text from Real_Time_Justification None. Additional_Comments: Since only 10 orbits (out of 25 requested) have been allocated we will image only one target, in one filter (F702W), and we will not use the LRF. Fixed_Targets ! Section 5.1 Target_Number: 1 Target_Name: GAL-0512+60 Alternate_Names: 4C0512+60 Description: GALAXY, RADIO GALAXY,HIGH Z GAL,PROTOGALAXY Position: RA=5H 12M 54.81S +/- 0.010S, DEC=60D 30' 51.9" +/- 0.1" Equinox: J2000 RV_or_Z: Z = 3.790 RA_PM: 0.0 Dec_PM: 0.0 Epoch: Annual_Parallax: 0.0 Flux: V = 24.5 B-V = 1.2 SURF(R)=29.0,SIZE=0.1 +/- 0.05 Comments: FAINT, EXTENDED GALAXY 15'' NWW OF DOUBLE STAR A. MUST BE SURE STAR A DOES NOT HAVE SPIKE THROUGH TARGET ON PC1; PA STAR - TARGET = 297 PC1 BLOOM PA=315; TRIED VARIOUS ORIENTS, BUT MOST OF THESE GIVE SCHED IN FEB 97. FOUND THAT BEST I CAN DO IS ORIENT OF 262 +/- 10. BUT CAN I TRUST THE PROGRAM .....? Solar_System_Targets Generic_Targets Scan_Data Visits ! Section 6 Visit_Number: 01 Visit_Requirements: ! Section 7.1 ORIENT 252.0D TO 272.0D ! Uncomment or copy visit level special requirements needed ! Most of these requirements (including ORIENT) will limit scheduling ! PCS MODE [Fine | Gyro] ! GUIDing TOLerance ! DROP TO GYRO IF NECESSARY [NO REACQuisition] ! ORIENTation TO ! ORIENTation TO FROM ! ORIENTation TO FROM NOMINAL ! SAME ORIENTation AS ! CVZ ! PARallel ! SCHEDulability ! AFTER [BY [TO ]] ! AFTER ! BEFORE ! BETWEEN AND ! GROUP WITHIN