! Proposal 6668, submission 1 ! PI: Megan Donahue ! Received Fri Feb 9 18:12:17 EST 1996 ! From: donahue@stsci.edu ! +====================+ ! | PED OUTPUT PRODUCT | ! +====================+ ! ! /diana/data1/megan/prop/hst_cycle6/6668.prop ! Generated by PREPROCESSOR, version 6.0e ! Date: Fri Feb 9 16:57:31 EST 1996 Proposal_Information Title: Star Formation and Galaxy Morphologies in Distant, X-ray Luminous Clusters of Galaxies Proposal_Category: GO Scientific_Category: COSMOLOGY Cycle: 6 Investigators PI_Name: Megan Donahue PI_Institution: Space Telescope Science Institute CoI_Name: John Stocke CoI_Institution: University of Colorado Contact: CoI_Name: Gerry Luppino CoI_Institution: Institute for Astronomy Contact: CoI_Name: Isabella Gioia CoI_Institution: Institute for Astronomy Contact: Abstract: Distant rich clusters of galaxies are natural laboratories for studying galaxy evolution because they provide large galaxy samples at fixed redshifts. Spectacular WFPC images of distant clusters of galaxies have revealed surprisingly complex galaxy morphologies and much higher interaction rates than in present -day clusters. We propose to obtain rest-frame U images of three distant (z=0.55-0.83) X-ray-selected, X-ray-luminous clusters of galaxies. With rest-frame B images from Cycle 5, we will be able to derive galaxy colors and color gradients. This data will distinguish young and old stellar populations, resolve galaxy ``train wrecks'', assess the colors of disk and bulges, and distinguish ram-pressure vs. merger induced star formation. We will compare the star formation in these galaxy clusters with that in low-z clusters of similar X-ray luminosity, distant optically-selected clusters, and field galaxies of similar redshift from the Hubble Deep Survey. Since intracluster medium (ICM) evolution plays at least a partial role in many models of galaxy evolution, these observations will test those models. Our ground-based and ROSAT and ASCA observations will supply cluster velocity dispersions, ICM morphology, temperatures and metallicities, as well as gas and cluster masses to characterize the intergalactic environment of these distant galaxies. Since at least two of these clusters are lensing background galaxies, these observations will provide morphology and color information for normal galaxies at even higher redshifts. Questions Observing_Description: We request 3 orbits to augment our Cycle 5 request to complete rest-frame B-band imaging of these clusters (see Duplications). The rest of our request, as limited by the Cycle 6 TAC, will be devoted to acquire rest- frame U-band images for only one cluster at redshifts 0.83. We will construct a single image of the cluster, at rest-wavelength U. We have chosen filters to enhance the contrast for photon wavelengths shorter than 4000Angstrom, while maximizing the number of counts. These filters will also be used by the Hubble Deep Field, thus facilitating direct comparison to the HDF galaxy sample. The orbit estimations were done assuming limiting magnitudes of m(U_rest) = 26.8 mag arcsec^-2 (z=0.8) in the F606W filter, and a required S/N=8-10 in 1 arcsec^2. This will produce observations similar to those acquired by Dressler et al. with the WF. We assumed sky ~ 27 mag pix^-1, dark counts 0.035 s^-1 pix^-1 and read noise of 5.2e^- pix^-1, and the handbook QT integral for the individual filters. Each orbit was assumed to have 45 minutes of visibility. Our results are tabulated below. Sky noise exceeds read noise in exposures exceeding 3-5 minutes, so the exposure during each orbit can be CR-SPLIT. Since we will have plenty of exposures, we have chosen not to CR-SPlIT the exposures so that we do not lose the overhead time. Filter& m_zero & Limit & Limit & Sky & Sky & SNR & Orbits , & & mag/pix & /s/pix & mag/pix & /s/pix (1"x1") F606W & 25.05 & 31.8 & 2.0(-3) & 27.0 & 0.166 & 8 & 10 We will dither the pointing between orbits 5 and 6 to remove hot pixels and improve spatial sampling. Real_Time_Justification: We will have Cycle 5 images of rest-frame B-band images of all 3 clusters. We have ASCA X-ray spectra for MS0451-03 (Donahue 1995, submitted) and MS1054-03 (Donahue et al. in prep.), as well as ROSAT PSPC images and spectra (Donahue & Stocke, 1995, ApJ, 449, 554), and a concurrent ASCA AO4 proposal for MS1137+66. X-ray spectra allow the determination of an overall gas temperature and iron abundance. We have deep ROSAT HRI (High Resolution Imager) observations for all clusters. (The most distant 2 are given priority A in AO6, MS0451-03 was observed in AO5). Xray HRI maps will allow the quanitification of structure in the cluster potential on scales of 30 h_50^-1 kpc. MS0451-03 now has 50 member redshifts, obtained by the CNOC collaboration, and MS1054-03 has 10 from our CFHT observations. We are planning to obtain stackrel>~ 30 redshifts for each of the remaining two clusters with Keck. A lens has been discovered in MS0451-03 (Luppino & Gioia 1995). Luppino & Kaiser (1995) have looked for weak gravitational lensing on a deep I-band image of MS1054-03, and have measured a clear shear signal at the 6Sigma level -- the first detection of lensing at such a high redshift. Similarly deep data does not yet exist for MS1137+66, but will be obtained this Spring with the Keck telescope. High resolution 20 cm radio continuum maps have been made of all three clusters with the VLA's B configuration deep enough to detect typical, low- luminosity cluster radio galaxies, and several head-tail radio galaxies have been discovered in each clusters. Several radio galaxies are detected in each cluster with morphologies and luminosities similar to those found in nearby rich clusters. Calibration_Justification: Additional_Comments: Fixed_Targets Target_Number: 1 Target_Name: MS1054-03 Alternate_Names: Description: CLUSTER OF GALAXIES,HIGH REDSHIFT CLUSTER (Z>0.5), Position: RA=10H 54M 26.9S +/- 5",DEC=-03D 21' 25.3" +/- 5" Equinox: B1950 RV_or_Z: Z = 0.83 RA_PM: Dec_PM: Epoch: Annual_Parallax: Flux: SURF(I) = 25 Comments: Solar_System_Targets Generic_Targets Scan_Data Visits Visit_Number: 01 Visit_Requirements: ORIENT 35D TO 55D On_Hold_Comments: Visit_Comments: I have selected an orientation and a position shift that would accomodate an extended cluster, about 2' e-w and 1' n-s in extent, centered on a cd galaxy. The target position is that of the cd galaxy. I believe that the pos targ command will NOT place the cd in the seam, but this should be checked. There are of course other orientation angles + position targets that can be accomodated: orient 125-145 pos targ -20.0,0.0 ; orient 215-235 pos targ 0.0,+20.0 ; orient 305-325 pos targ +20,0.0 Exposure_Number: 1 Target_Name: MS1054-03 Config: WFPC2 Opmode: IMAGE Aperture: WF3 Sp_Element: F606W Wavelength: Optional_Parameters: cr-split=no Number_of_Iterations: 1 Time_Per_Exposure: 2600S Special_Requirements: POS TARG 0.0,-20.0 Comments: Exposure_Number: 2 Target_Name: MS1054-03 Config: WFPC2 Opmode: IMAGE Aperture: WF3 Sp_Element: F606W Wavelength: Optional_Parameters: cr-split=no Number_of_Iterations: 1 Time_Per_Exposure: 2600S Special_Requirements: SAME POS AS 1 Comments: Exposure_Number: 3 Target_Name: MS1054-03 Config: WFPC2 Opmode: IMAGE Aperture: WF3 Sp_Element: F606W Wavelength: Optional_Parameters: cr-split=no Number_of_Iterations: 1 Time_Per_Exposure: 2600S Special_Requirements: SAME POS AS 2 Comments: Exposure_Number: 4 Target_Name: MS1054-03 Config: WFPC2 Opmode: IMAGE Aperture: WF3 Sp_Element: F606W Wavelength: Optional_Parameters: cr-split=no Number_of_Iterations: 1 Time_Per_Exposure: 2600S Special_Requirements: Comments: Exposure_Number: 5 Target_Name: MS1054-03 Config: WFPC2 Opmode: IMAGE Aperture: WF3 Sp_Element: F606W Wavelength: Optional_Parameters: cr-split=no Number_of_Iterations: 1 Time_Per_Exposure: 2600S Special_Requirements: SAME POS AS 4 Comments: Visit_Number: 02 Visit_Requirements: ORIENT 35D TO 55D On_Hold_Comments: Visit_Comments: I have selected an orientation and a position shift that would accomodate an extended cluster, about 2' e-w and 1' n-s in extent, centered on a cd galaxy. The target position is that of the cd galaxy. I believe that the pos targ command will NOT place the cd in the seam, but this should be checked. There are of course other orientation angles + position targets that can be accomodated: orient 125-145 pos targ -20.0,0.0 ; orient 215-235 pos targ 0.0,+20.0 ; orient 305-325 pos targ +20,0.0 Exposure_Number: 1 Target_Name: MS1054-03 Config: WFPC2 Opmode: IMAGE Aperture: WF3 Sp_Element: F606W Wavelength: Optional_Parameters: cr-split=no Number_of_Iterations: 1 Time_Per_Exposure: 2600S Special_Requirements: POS TARG 0.25,-19.75 Comments: Exposure_Number: 2 Target_Name: MS1054-03 Config: WFPC2 Opmode: IMAGE Aperture: WF3 Sp_Element: F606W Wavelength: Optional_Parameters: CR-SPLIT=No Number_of_Iterations: 1 Time_Per_Exposure: 2600S Special_Requirements: SAME POS AS 1 Comments: Exposure_Number: 3 Target_Name: MS1054-03 Config: WFPC2 Opmode: IMAGE Aperture: WF3 Sp_Element: F606W Wavelength: Optional_Parameters: cr-split=no Number_of_Iterations: 1 Time_Per_Exposure: 2600S Special_Requirements: SAME POS AS 2 Comments: Exposure_Number: 4 Target_Name: MS1054-03 Config: WFPC2 Opmode: IMAGE Aperture: WF3 Sp_Element: F606W Wavelength: Optional_Parameters: cr-split=no Number_of_Iterations: 1 Time_Per_Exposure: 2600S Special_Requirements: SAME POS AS 3 Comments: Exposure_Number: 5 Target_Name: MS1054-03 Config: WFPC2 Opmode: IMAGE Aperture: WF3 Sp_Element: F606W Wavelength: Optional_Parameters: cr-split=no Number_of_Iterations: 1 Time_Per_Exposure: 2600S Special_Requirements: SAME POS AS 4 Comments: Data_Distribution ! 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