! Proposal 6564, submission 2 ! PI: JAMES LOWENTHAL ! Received Fri Oct 11 00:44:46 EDT 1996 ! From: james@ucolick.org ! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6564,v 4.1 1996/11/12 17:15:34 pepsa Exp $ ! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6564,v 4.1 1996/11/12 17:15:34 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: Sleiman ! Phone: 410-338-4753 , E-mail: sleiman@stsci.edu ! ! This partially completed template was generated from a Phase I proposal. ! Name of Phase I Proposal: archive-0440.lowenthal.prop ! Date generated: Fri Dec 22 18:14:24 EST 1995 ! Proposal_Information ! Section 4 Title: DETAILED MORPHOLOGY OF A LYMAN-ALPHA GALAXY AT Z=2.3 Proposal_Category: GO Scientific_Category: COSMOLOGY Cycle: 6 Investigators PI_name: JAMES LOWENTHAL PI_Institution: LICK OBSERVATORY CoI_Name: BRUCE WOODGATE CoI_Institution: NASA/GSFC Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) The identification and detailed study of galaxies at high redshift remains the most direct path to understanding galaxy formation and evolution, yet there are only a handful of radio quiet galaxies known in emission at z>1.5. By using HST and WFPC2 to image the Coup Fourre Galaxy -- the first Lyman-alpha emission galaxy discovered near a high-redshift damped Ly- alpha\ absorption line cloud -- at z=2.3 in Ly-alpha\ and broad-band V and I, I will discriminate between star formation and nuclear activity as the source of Ly-alpha\ emission and will be able to test for evidence of galaxy mergers or interaction, and of the clumpy star formation sites thought to accompany young, coalescing galaxies. This source is a viable candidate for a primeval galaxy, the Rosetta Stone of cosmology, and detailed morphological study on kpc scales is crucial to compare the light profile to current-day disk or bulge systems, to relate the galaxy's characteristics directly to theories of galaxy formation, and to help clarify the relation between absorbing and emitting galaxies. Multi-band photometry will allow direct comparison to spectral synthesis models of galaxy evolution to estimate the galaxy's age and star formation history. We will also search the field for additional compact galaxies or protogalaxies physically associated with the absorber/emitter pair, using the Ly-alpha\ and broad-band filters to select candidates via their colors, sizes, and morphologies. Questions ! Free format text (please update) Observing_Description: There very fortunately happens to be on WFPC2 a 147A-wide filter, F410M, that includes Lyman-Alpha for z=2.3128 at 4027A. We request 16 orbits with this filter in order to reach an estimated signal-to-noise ratio S/N = 3 for a point source with emission line flux 1e-17 erg/s/cm^2, corresponding to the Lyman-Alpha flux from an unobscured galaxy at z=2.3 undergoing star formation at the rate of 1 Msun/yr. Such a source will provide an estimated signal of about 3e-3 e-/s, compared with an estimated background rate on the PC of 4e-4 e\s\pixel, which dominates the noise. We are assuming here a sky brightness of 22.3 mag/arcsec^2 based on an ecliptic latitude of 5 deg, and 2940 sec of usable integration time per orbit, after allowing for instrument overhead and Earth occulation. If our main target, the Coup Fourre galaxy, were a point source, it would appear at S/N~168, ensuring adequate signal-to-noise even if it were extended over 1 arcsec^2. CR-SPLITs should not be necessary for the F410M observations given the large number of exposures, although we will want to dither using one of the pre-programmed HST dither patterns, to reduce the effect of CCD cosmetic defects. We are also requesting 3 orbits of integration with the F555W = V and 2 orbits with the F814W = I filters. This will allow us to detect point sources of V=28.1 and I=27.5 with S/N=3, corresponding to two magnitudes fainter than an L* Sa galaxy at z=2.3 assuming passive evolution. These filters were chosen to provide a spectrally close comparison to the Lyman-Alpha images (V), to provide as long a spectral baseline as possible to aid in the identification of additional z=2.3 candidate sources via their broad-band colors (I), and to maintain consistency with the recommended WFPC2 filter selection policy. CR-SPLITs will be helpful for these less-numerous integrations. We intend to place the Lyman-Alpha galaxy on the WF3 chip, with the V=16.6 image of the QSO PHL 957, 47 arcsec away, ideally falling on PC1, (but possibly on WF1-3, if orientation constraints so dictate). This will ensure high S/N for our main target and maximum sensitivity to faint sources within 250 h^-1 kpc of the damped Lyman-Alpha cloud, while helping to alleviate saturation and providing maximum resolution for the QSO PSF region, which may show faint Lyman-Alpha emission from the Damped Lyman-Alpha Clouds itself. ! Real_Time_Justification: !Calibration_Justification: ! Move appropriate text from Real_Time_Justification ! Additional_Comments: Fixed_Targets ! Section 5.1 Target_Number: 1 Target_Name: PHL957-GAL Alternate_Names: QSO0100+130-GAL,COUP-FOURRE Description: GALAXY, HIGH Z GAL, LYMAN ALPHA CLOUD, QSO Position: RA=01H 03M 08.44S +/- 0.06S,DEC=+13D 16' 40.92" +/- 1.0" ! RA=0H 0M 0.00S +/- 0S, ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 Equinox: 2000.0 RV_or_Z: Z=2.313 RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: V=23.6 +/-0.5, B-V=0.6 +/- 0.5 ! Include at least V and B-V Comments: Main object of interest is "Coup Fourre Galaxy" at z=2.313, a Lyman-alpha galaxy 47 arcsec to the northwest of the QSO PHL 957 line of sight. QSO is V=16.5. With galaxy on WF3, desire QSO on PC1 (ORIENT=120), but QSO on WF1, WF2, or WF3 is acceptable, so we specify no ORIENT constraint. Scan_Data ! Appendix B ! 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: ! Section 7.1 ! Uncomment or copy visit level special requirements needed ! Most of these requirements (including ORIENT) will limit scheduling On_Hold_Comments: Visit_Comments: It is crucial to image BOTH the Galaxy and the QSO. Original ORIENT = 120.0D +/- 70D has been abandoned. Instead we specify location of galaxy on WF3, so that any ORIENT will image QSO somewhere on PC, WF1, WF2, or WF3. Exposure_Number: 1 ! Section 6.5 Target_Name: PHL957-GAL Config: WFPC2 Opmode: IMAGE Aperture: WF3-FIX Sp_Element: F410M Wavelength: Optional_Parameters: DITHER-TYPE=BOX,CR-SPLIT=NO Number_of_Iterations: 1 Time_Per_Exposure: 2600S Special_Requirements: POS TARG +21.5,+21.5 ! Section 7.2 Exposure_Number: 2 ! Section 6.5 Target_Name: PHL957-GAL Config: WFPC2 Opmode: IMAGE Aperture: WF3-FIX Sp_Element: F410M Wavelength: Optional_Parameters: DITHER-TYPE=BOX,CR-SPLIT=NO Number_of_Iterations: 1 Time_Per_Exposure: 2600S Special_Requirements: SAME POS AS 1 ! Section 7.2 Visit_Number: 2 Visit_Requirements: ! Section 7.1 ! Uncomment or copy visit level special requirements needed ! Most of these requirements (including ORIENT) will limit scheduling ORIENT -10D TO 10D FROM 1 Exposure_Number: 1 ! Section 6.5 Target_Name: PHL957-GAL Config: WFPC2 Opmode: IMAGE Aperture: WF3-FIX Sp_Element: F410M Wavelength: Optional_Parameters: DITHER-TYPE=BOX,CR-SPLIT=NO Number_of_Iterations: 1 Time_Per_Exposure: 2600S Special_Requirements: POS TARG +21.5,+21.5 ! Section 7.2 Exposure_Number: 2 ! Section 6.5 Target_Name: PHL957-GAL Config: WFPC2 Opmode: IMAGE Aperture: WF3-FIX Sp_Element: F410M Wavelength: Optional_Parameters: DITHER-TYPE=BOX,CR-SPLIT=NO Number_of_Iterations: 1 Time_Per_Exposure: 2600S Special_Requirements: SAME POS AS 1 ! Section 7.2 Visit_Number: 3 Visit_Requirements: ! Section 7.1 ! Uncomment or copy visit level special requirements needed ! Most of these requirements (including ORIENT) will limit scheduling ORIENT -10D TO 10D FROM 1 Exposure_Number: 1 ! Section 6.5 Target_Name: PHL957-GAL Config: WFPC2 Opmode: IMAGE Aperture: WF3-FIX Sp_Element: F555W Wavelength: Optional_Parameters: Number_of_Iterations: 3 Time_Per_Exposure: 2500S Special_Requirements: POS TARG +21.5,+21.5 ! Section 7.2 Exposure_Number: 2 ! Section 6.5 Target_Name: PHL957-GAL Config: WFPC2 Opmode: IMAGE Aperture: WF3-FIX Sp_Element: F814W Wavelength: Optional_Parameters: Number_of_Iterations: 2 Time_Per_Exposure: 2600S Special_Requirements: SAME POS AS 1 ! Section 7.2 ! Uncomment or copy exposure level special requirements needed Comments: 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: ! ! KERR HALL ! UNIVERSITY OF CALIFORNIA ! SANTA CRUZ ! 95064 ! ! Ship_Via: UPS ! UPS (2-day) or OVERNIGHT ! 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