! Proposal 6000, submission 3 ! PI: Marc Postman ! Received Fri Feb 10 16:32:13 EST 1995 ! From: postman@stsci.edu ! Hubble Space Telescope Cycle 5 (1995) Phase II Proposal Template ! $Id: 6000,v 4.1 1995/05/22 19:57:30 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: Giselle Sleiman ! Phone: 410 338-4753 , E-mail: sleiman@stsci.edu ! ! This partially completed template was generated from a Phase I proposal. ! Date generated: Sun Dec 18 10:33:04 EST 1994 ! Proposal_Information ! Section 4 Title: Morphology and Photometry of Galaxies in Optically Selected High Redshift Clusters Proposal_Category: GO Scientific_Category: Galaxies & Clusters Cycle: 5 Investigators PI_name: Marc Postman PI_Institution: Space Telescope Science Institute CoI_Name: James E. Gunn CoI_Institution: Princeton University Contact: N ! Y or N (designate at most one contact) CoI_Name: John G. Hoessel CoI_Institution: University of Wisconsin Contact: N ! Y or N (designate at most one contact) CoI_Name: Lori Lubin CoI_Institution: Princeton University Contact: N ! Y or N (designate at most one contact) CoI_Name: J. Beverley Oke CoI_Institution: Dominion Astrophysical Observatory Contact: N ! Y or N (designate at most one contact) CoI_Name: Donald Schneider CoI_Institution: Penn State University Contact: N ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) We are requesting deep, broad-band red WFPC2 images of six distant clusters (0.6 < z < 1.2) to analyze the morphological characteristics of the cluster members. The high angular resolution imagery of HST, combined with our extensive ground based u,v,g,r,i,z photometry, will allow the measurement of the morphological fractions in distant clusters as functions of redshift, color, galaxy density, and global cluster properties such as core radius and ellipticity. We will also study the rest frame UV properties of the cluster galaxies as a function of morphological type. Utilizing extensive data for clusters at lower redshifts, we will place new and fundamental constraints on the evolution of structural parameters of cluster galaxies, on the origin of the morphological segregation of galaxies, and on galaxy and cluster formation. The cluster sample has been selected objectively from large area optical/near IR ground based surveys. The proposal team has committed a significant amount of time on ground based telescopes for on--going spectroscopic data acquisition that will compliment the HST observations. We have also developed and tested algorithms for performing objective measurements of galaxy morphology that will be applied to the data. Questions ! Free format text (please update) Observing_Description: The F702W filter is the most efficient choice for imaging z > 0.6 clusters given the typical spectral energy distribution of the cluster galaxies combined with the relatively high QE and broad bandpass of this filter. The sole exception is for cluster CL023143+004844 where we choose to observe with the F606W filter because this cluster contains bluer galaxies. We opt against using F814W because the sky background is slightly higher, the QE is slightly lower, and one does not gain a significant signal-to-noise ratio (S/N) improvement given a passively evolving elliptical spectral energy distribution (with significant color evolution or a high spiral fraction, the drive to observe much redward of 8000 Angstrom is negated). We will rely on our ground based data for integrated color information. Our exposure time estimates are based on a direct analysis of the WFPC2+F702W HST data of the z = 1.2 3C324 cluster observed by Dickinson (who kindly provided us access to these data). Our desire is to reach a S/N ratio of at least ~5 within the half-light radius of 0.50 L^* galaxies at z ~ 1.0. This requirement is based jointly on the desire to have quality data for a significant number of cluster members and on our estimates of the minimum signal needed to perform reliable measurement of basic morphological characteristics such as the effective radius, compactness parameter, asymmetry, and radial profile. After 16,800 seconds of exposure time, the relationship between S/N ratio and AB magnitude within the half-light radius of galaxies in the 3C324 WFC data is log_10(S/N) = -0.413 AB + 10.827. Thus, galaxies with AB <= 24.52 will typically have S/N >= 5 over their central 80 WFC pixels. This corresponds to the flux a passively evolving 0.50 L^* elliptical galaxy at z = 1.0 would have within its half-light radius (assuming an effective radius of 3h^-1 kpc). Color evolution aids S/N considerations but we want to be conservative to avoid biasing our results. We will, thus, require 7 orbits to perform our analysis on our most distant clusters; 6 orbits for the clusters at 0.7 <= z <= 0.83; and 7 orbits for CL023143+004844 because of its especially blue galaxy population. These S/N computations are relatively independent of the assumed Hubble constant. The individual exposures will be CR-split. We will request offsets of a few WFC-pixels after every 2 orbits to improve rejection of residual hot pixels and other CCD defects. Real_Time_Justification: No special requirements needed. We have acquired and reduced multiband photometry for the clusters in our HST target list (see table). Spectroscopic observations for galaxies in 4 of our 6 cluster already exist and were obtained by us at the Hale 5m telescope. Lubin, Gunn, and Postman have a dedicated observing program with the Apache Point ARC 3.5m telescope to continue our spectroscopic observations. We have up to 20 hrs guaranteed time on the ARC 3.5m per month, beginning with 16 hrs in October 1994. Oke will have several nights on the Keck 10m telescope in the spring and fall of 1995 to carry out spectroscopic slit--mask observations of additional galaxies in these clusters. Schneider and Hoessel will also commit significant blocks of their GTO time on the Hobby-Eberly 8m telescope (formally the SST) and on the WIYN telescope, respectively, for spectroscopic data acquisition. All members of the proposal team have expertise in the fields of galaxy and cluster formation and evolution. Postman and Gunn have developed and tested software for measuring structural parameters and performing morphological classification of galaxies. Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: Fixed_Targets ! Section 5.1 Target_Number: 1 Target_Name: GAL-CLUS-002352+042307 Alternate_Names: GHO-KP-CHI-EPSILON Description: CLUSTER OF GALAXIES, RICH CLUSTER Position: RA = 00H 23M 53.76S +/- 0.5S, DEC = +04D 23' 11.1" +/- 2.0" Equinox: J2000 RV_or_Z: Z = 0.832 Flux: V = 23.7 Comments: Gunn, Hoessel, Oke Cluster KP Chi Epsilon Target_Number: 2 Target_Name: GAL-CLUS-023143+004844 Alternate_Names: GHO-KP-EPSILON Description: CLUSTER OF GALAXIES, RICH CLUSTER Position: RA = 02H 31M 43.82S +/- 0.5S, DEC = +00D 48' 47.3" +/- 2.0" Equinox: J2000 RV_or_Z: Z = 0.607 Flux: V = 22.0 Comments: Gunn, Hoessel, Oke Cluster KP Epsilon Target_Number: 3 Target_Name: GAL-CLUS-160733+411013 Alternate_Names: PAL-SUPPL-CLUSTER-019 Description: CLUSTER OF GALAXIES, RICH CLUSTER Position: RA = 16H 07M 31.63S +/- 0.5S, DEC = +41D 10' 11.7" +/- 2.0" Equinox: J2000 RV_or_Z: Z = 0.900 Flux: V = 23.5 Comments: Gunn, Hoessel, Oke Cluster C-37 = PDC Suppl. 19. ! This is a template for a single visit containing a single exposure ! Repeat exposure and visit blocks as needed Visits ! Section 6 Visit_Number: 1 Visit_Requirements: ORIENT 315D TO 55D Visit_Comments: Rotate U3 axis between 315D and 55D east of north Exposure_Number: 101 ! Section 6.5 Target_Name: GAL-CLUS-002352+042307 Config: WFPC2 Opmode: IMAGE Aperture: WFALL-FIX Sp_Element: F702W Optional_Parameters: CR-SPLIT=NO Number_of_Iterations: 1 Time_Per_Exposure: 2300S Special_Requirements: POS TARG 10.00, 10.00 Exposure_Number: 102 ! Section 6.5 Target_Name: GAL-CLUS-002352+042307 Config: WFPC2 Opmode: IMAGE Aperture: WFALL-FIX Sp_Element: F702W Optional_Parameters: CR-SPLIT=NO Number_of_Iterations: 3 Time_Per_Exposure: 2600S Special_Requirements: POS TARG 10.00, 10.00 Exposure_Number: 103 ! Section 6.5 Target_Name: GAL-CLUS-002352+042307 Config: WFPC2 Opmode: IMAGE Aperture: WFALL-FIX Sp_Element: F702W Optional_Parameters: CR-SPLIT=NO Number_of_Iterations: 3 Time_Per_Exposure: 2600S Special_Requirements: POS TARG 10.50, 10.50 Visit_Number: 2 Visit_Requirements: ORIENT 315D TO 75D Visit_Comments: Rotate U3 axis between 315D and 75D east of north Exposure_Number: 201 ! Section 6.5 Target_Name: GAL-CLUS-023143+004844 Config: WFPC2 Opmode: IMAGE Aperture: WFALL-FIX Sp_Element: F606W Optional_Parameters: CR-SPLIT=NO Number_of_Iterations: 1 Time_Per_Exposure: 2300S Special_Requirements: POS TARG 10.00, 10.00 Exposure_Number: 202 ! Section 6.5 Target_Name: GAL-CLUS-023143+004844 Config: WFPC2 Opmode: IMAGE Aperture: WFALL-FIX Sp_Element: F606W Optional_Parameters: CR-SPLIT=NO Number_of_Iterations: 2 Time_Per_Exposure: 2600S Special_Requirements: POS TARG 10.00, 10.00 Exposure_Number: 203 ! Section 6.5 Target_Name: GAL-CLUS-023143+004844 Config: WFPC2 Opmode: IMAGE Aperture: WFALL-FIX Sp_Element: F606W Optional_Parameters: CR-SPLIT=NO Number_of_Iterations: 3 Time_Per_Exposure: 2600S Special_Requirements: POS TARG 10.50, 10.50 Visit_Number: 3 Visit_Requirements: ORIENT 115D TO 175D Visit_Comments: Rotate U3 axis between 115D and 175D east of north Exposure_Number: 301 ! Section 6.5 Target_Name: GAL-CLUS-160733+411013 Config: WFPC2 Opmode: IMAGE Aperture: WFALL-FIX Sp_Element: F702W Optional_Parameters: CR-SPLIT=NO Number_of_Iterations: 1 Time_Per_Exposure: 2400S Special_Requirements: POS TARG 10.00, 10.00 Exposure_Number: 302 ! Section 6.5 Target_Name: GAL-CLUS-160733+411013 Config: WFPC2 Opmode: IMAGE Aperture: WFALL-FIX Sp_Element: F702W Optional_Parameters: CR-SPLIT=NO Number_of_Iterations: 3 Time_Per_Exposure: 2700S Special_Requirements: POS TARG 10.00, 10.00 Exposure_Number: 303 ! Section 6.5 Target_Name: GAL-CLUS-160733+411013 Config: WFPC2 Opmode: IMAGE Aperture: WFALL-FIX Sp_Element: F702W Optional_Parameters: CR-SPLIT=NO Number_of_Iterations: 3 Time_Per_Exposure: 2700S Special_Requirements: POS TARG 10.50, 10.50 Data_Distribution ! Defaults indicated; change if desired Medium: 8MM ! 8MM or 6250BPI or 1600BPI Blocking_Factor: 10 ! 10 or 1 ! Only astronomers with very old 9- ! track tape drives should consider ! a blocking factor of 1 Ship_To: PI_Address ! STSCI or PI_Address or ! PI Address from Phase I is: ! ! 3700 San Martin Drive ! ! 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