! Proposal 5970, submission 1 ! PI: Mauro Giavalisco ! Received Wed Feb 15 10:12:04 EST 1995 ! From: giaval@stsci.edu ! Hubble Space Telescope Cycle 5 (1995) Phase II Proposal Template ! $Id: 5970,v 8.1 1995/08/03 23:06:46 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: Doug Van Orsow ! Phone: 410 338-4568 , E-mail: vanorsow@stsci.edu ! ! This partially completed template was generated from a Phase I proposal. ! Date generated: Sun Dec 18 09:50:22 EST 1994 ! Proposal_Information ! Section 4 Title: Exploring the Morphology of Cluster Galaxies at Redshift z=3.4 Proposal_Category: GO Scientific_Category: Galaxies & Clusters Cycle: 5 Investigators PI_name: Mauro Giavalisco PI_Institution: Space Telescope Science Institute CoI_Name: Duccio Macchetto CoI_Institution: Space Telescope Science Institute Contact: ! Y or N (designate at most one contact) CoI_Name: Piero Madau CoI_Institution: Space Telescope Science Institute Contact: ! Y or N (designate at most one contact) CoI_Name: William Sparks CoI_Institution: Space Telescope Science Institute Contact: ! Y or N (designate at most one contact) CoI_Name: Charles Steidel CoI_Institution: Massachussets Insitute of Technology Contact: ! Y or N (designate at most one contact) CoI_Name: Alexander Szalay CoI_Institution: The Johns Hopkins University Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) Primeval galaxies are systems in the process of forming their first stellar populations. Despite intensive searches over more than a decade, the population of primeval galaxies has not been found and we remain essentially ignorant, from an empirical point of view, as to the early phases of galaxy formation and evolution. In view of this, we propose to obtain images with the WFPC2 of two radio-quiet, star-forming galaxies at z=3.4 that we have identified in the field around Q0000-263, and of another 14 z=3.4 galaxy candidates. The two galaxies with confirmed redshifts are very likely a nascent spheroidal system with relatively intense Ly-alpha\ emission, and a disc galaxy producing the damped Ly-alpha\ absorption in the spectrum of the QSO, respectively. The latter 14 galaxies have identical SEDs to the two with known redshift, and are also spatially clustered with them at the 98.8\ be the most distant group or cluster of galaxies thus far identified. We propose the F702W filter to study the rest-frame UV light of the 16 galaxies in a spectral region that at z=3.4 corresponds to ~ 1600 Angstrom. This study is aimed at elucidating the morphology of the star-forming regions of two confirmed z=3.4 galaxies, probing the existence of the structural components such as disk and bulge, and at establishing the general morphological properties of the cluster candidates in comparison with other similarly faint (but foreground) galaxies in the field. Questions ! Free format text (please update) Observing_Description: The proposed observations consist of WFPC2 imaging of the field around Q0000-263 through the F702W passband with a total integration time of 15 hours or 24 orbits. Targets of the program are 16 galaxies with magnitudes in the interval 24<\cal R<25.5 (our customized \cal R filter, intermediate between the Johnson R and I, is quite similar to the F702W). These galaxies are distributed within an area of about 2.5x2.5 arcmin^2 and, with the exception of two of them, they can all be accomodated in the WFPC2 field with a proper orientation of the telescope. One of these galasies cause a damped Lyman-alpha/Lyman-limit absorption system in the spectrum of QSO 0000-263, which has V~18.6 and it is placed at about 2.5 arcsec from it. We will put the QSO with the absorbing galaxy in the PC chip. We want each exposure about 20 minute long, which avoids strong saturation of the QSO. After each exposure the telescope will be stepped by a few pixels both in RA and DEC (integer pixel shift). Due to uncertainty in the magnitude of the QSO in the F702W filter, we set CLOCKS=YES we minimize the effects of saturation. Also, we do not need CRSPLIT because we will have enough exposures to allow a proper subtraction of cosmic rays. Real_Time_Justification: None. Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: Fixed_Targets ! Section 5.1 Target_Number: 1 Target_Name: GAL-000328-260354 Alternate_Names: GAL-CLUS-000328-260354 Description: CLUSTER OF GALAXIES, HIGH REDSHIFT CLUSTER (z>0.5), GALAXY, STARBURST, LYMAN ALPHA CLOUD, PROTOGALAXY Position: RA=00H 03M 23.23S +/- 0.01S, ! Most common specification format is DEC=-26D 03' 06.7" +/- 0.1" ! RA=0H 0M 0.00S +/- 0S, ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 Equinox: J2000 RV_or_Z: Z = 3.4 RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: U-V = 36.0 E-1, V-R = 30.0 E-2, ! Include at least V and B-V U = 27.5, V = 23.9, R = 24.2, U-V = 25.0 E-1, V-R = 5.0 E-1, U = 27.5, V = 25.0, R = 24.5 Comments: Very high galactic latitude field with b~-79. With the exception of a QSO with V~18.6, there are no bright stars in this field. The brightest galaxy has V~20. The QSO is at z=4.11. The galaxy causing the damped system of the QSO is at z=3.390, and the Lyman-alpha galaxy is at z=3.428. !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: 01 Visit_Requirements: ORIENT 295.26D to 295.26D ! Section 7.1 GROUP 1-2 WITHIN 21D ! 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