! Hubble Space Telescope Cycle 5 (1995) Phase II Proposal Template ! $Id: 5973,v 5.1 1995/04/11 15:10:50 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 09:56:30 EST 1994 ! Proposal_Information ! Section 4 Title: The Host Galaxies of Radio-Quiet High- Redshift Quasi-Stellar Objects Proposal_Category: GO Scientific_Category: Quasars Cycle: 5 Investigators PI_name: Matthew Lehnert PI_Institution: Institute of Geophysics and Planetary Physics CoI_Name: Timothy Heckman CoI_Institution: Dept of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218 Contact: ! Y or N (designate at most one contact) CoI_Name: James Lowenthal CoI_Institution: Lick Observatory, UC Santa Cruz, Santa Cruz, CA 95064 Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) Studying the environments of quasi-stellar objects (QSOs) at high redshift may help to answer the question: Why were powerful QSOs three orders of magnitude more common at z=2 to 3 than at present? Recent data have shown that high-z radio- loud quasars are immersed in spatially-resolved ``fuzz'' with properties suggestive of young, massive galaxies. Quasars as radio-loud as those studied to date represent <<1\ population of high-redshift radio galaxies are equally rare). To understand the applicability of these results to the much more numerous radio-quiet QSOs, and hence their implications for understanding the causes and effects of the ``quasar epoch'' at high-redshift, we propose to conduct a narrow-band (at LyAlpha) and broad-band (F555W) optical imaging investigation using WFPC2 on HST of a small sample of radio-quiet QSOs at similarly high redshifts as the radio-loud quasars studied previously. These data will allow us for the first time to compare at similar absolute spatial resolution the morphologies and luminosities of high-redshift radio-quiet QSOs to those of low-redshift QSOs studied from the ground, thus determining how the host galaxies of QSOs have evolved with time, and also to compare the hosts of high-redshift radio-quiet and radio-loud quasars. Questions ! Free format text (please update) Observing_Description: For this project, we selected 5 radio-quiet QSOs from the catalog of Hewitt and Burbidge (1994) with redshifts and optical magnitudes similar to those of the radio-loud quasars that will be observed as part of our Cycle 4 program (we also required the QSOs to have accurate coordinates listed in Hewitt and Burbidge). The radio-loud quasars that we will observe with HST in cycle 4 are the 5 quasars from Heckman Etal 1992a that had the brightest continuum and LyAlpha emitting fuzz of the entire sample of 18 and also happened (by happy coincidence!) to have recession velocities suitable to place redshifted LyAlpha into the band-passes of the OII Quad filters available with the WFPC2. Thus we have also selected radio-quiet QSOs with redshifts such that their LyAlpha emission falls into the bandpass of one of the four OII Quad filters. Continuum Imaging Our choice of continuum filter is dictated by three criteria. First, the bright LyAlpha line should be excluded from the bandpass. Second, the filter should be among the most efficient broad-band filters available on the WFPC2. Third, the central wavelength should be as near as possible to the redshifted wavelength of LyAlpha (3832, 3905, 3935, 4008, and 3838Angstrom \ for the 5 QSOs), to be suitable for continuum subtraction and still meet criteria one and two for all the QSOs in our sample. A reasonable compromise among these criteria is F555W. Since F555W can be used in either the WFC or the PC, we choose to image the QSOs in the PC to obtain the highest possible spatial resolution. LyAlpha Imaging The redshifted wavelengths of LyAlpha are 3832, 3905, 3935, 4008, and 3838Angstrom \ for QSOs 0050--280, 1045+060, 1207-- 107, 1313--156, and 2206--187, respectively. The three filters that are suitable for LyAlpha imaging are: FQUVN-B, which has a central wavelength of 3831Angstrom, suitable for observing both 0050--280 and 2206--187; FQUVN-C, which has a central wavelength of 3915Angstrom, suitable for observing both 1045+060 and 1207--107; and FQUVN-D, which has a central wavelength of 3992Angstrom, suitable for observing 1313--156. The redshifted OII quad filters (FQUVN) can be used only in the WFC. Note that the equivalent width of the LyAlpha line is likely to be large and thus the narrow-band images will be dominated by LyAlpha emission. The observing strategy described above is almost exactly the same as for our radio- loud quasar HST Cycle 4 program. Exposure times will be 2 * 42 minutes (using CR-split for both of the exposures, 21 minutes per exposure) through the narrow-band filters (this fills exactly two orbits per QSO) and 3 * 11 minutes (no CR- split; using the first orbit for a QSO to do the continuum imaging; fills exactly one orbit per QSO) through the continuum filter F555W. These exposure times will allow us to detect structures down to 8times10^-17 ergs cm^-2 s^-1 HST PSF^-1 at LyAlpha and to ~28 V mag HST PSF^-1 at F555W, sufficiently sensitive to detect extended near-nuclear emission and any clumpy structure on sub-galaxy scales if it is similar to the light of present-day L(star) galaxies. Real_Time_Justification: We have no special requirements. Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: Fixed_Targets ! Section 5.1 Target_Number: 1 Target_Name: 0050-280 Alternate_Names: Description: Galaxy, QSO Position: RA=00H 52M 31.8S +/- 0.5S, DEC=-27D 48' 07.3" +/- 0.9" Equinox: J2000.0 RV_or_Z: Z=2.152 RA_PM: 0.0000 ! Units are seconds of time per year Dec_PM: 0.0000 ! Units are seconds of arc per year Epoch: J2000.0 Annual_Parallax: 0.0000 Flux: V=20.25, U-B=-0.69 Comments: Target_Number: 2 Target_Name: 1045+060 Alternate_Names: Description: Galaxy, QSO Position: RA=10H 47M 42.76S +/- 0.3S, DEC=05D 49' 59.2" +/- 0.5" Equinox: J2000.0 RV_or_Z: Z=2.212 RA_PM: 0.0000 ! Units are seconds of time per year Dec_PM: 0.0000 ! Units are seconds of arc per year Epoch: J2000.0 Annual_Parallax: 0.0000 Flux: V=19.48 Comments: Target_Number: 3 Target_Name: 1207-107 Alternate_Names: Description: Galaxy, QSO Position: RA=12H 09M 51.92S +/- 0.3S, DEC=-10D 59' 58.1" +/- 0.5" Equinox: J2000.0 RV_or_Z: Z=2.237 RA_PM: 0.0000 ! Units are seconds of time per year Dec_PM: 0.0000 ! Units are seconds of arc per year Epoch: J2000.0 Annual_Parallax: 0.0000 Flux: V=19.03 Comments: Target_Number: 4 Target_Name: 1313-156 Alternate_Names: Description: Galaxy, QSO Position: RA=13H 15M 44.41S +/- 0.3S, DEC=-15D 56' 46.6" +/- 0.5" Equinox: J2000.0 RV_or_Z: Z=2.297 RA_PM: 0.0000 ! Units are seconds of time per year Dec_PM: 0.0000 ! Units are seconds of arc per year Epoch: J2000.0 Annual_Parallax: 0.0000 Flux: V=20.59 Comments: Target_Number: 5 Target_Name: 2206-187 Alternate_Names: MD5:79 Description: Galaxy, QSO Position: RA=22H 09M 28.40S +/- 0.3S, DEC=-18D 32' 57.9" +/- 0.5" Equinox: J2000.0 RV_or_Z: Z=2.157 RA_PM: 0.0000 ! Units are seconds of time per year Dec_PM: 0.0000 ! Units are seconds of arc per year Epoch: J2000.0 Annual_Parallax: 0.0000 Flux: V=19.60 Comments: ! This is a template for a single visit containing a single exposure ! Repeat exposure and visit blocks as needed Visits Visit_Number: 1 Visit_Requirements: On_Hold_Comments: Visit_Comments: Exposure_Number: 1 Target_Name: 0050-280 Config: WFPC2 Opmode: IMAGE Aperture: PC1 Sp_Element: F555W Wavelength: 5407 Optional_Parameters: CR-SPLIT=NO Number_of_Iterations: 3 Time_Per_Exposure: 700S Special_Requirements: Exposure_Number: 2 Target_Name: 0050-280 Config: WFPC2 Opmode: IMAGE Aperture: WF4 Sp_Element: FQUVN Wavelength: 3839 Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 2500S Special_Requirements: Exposure_Number: 3 Target_Name: 0050-280 Config: WFPC2 Opmode: IMAGE Aperture: WF4 Sp_Element: FQUVN Wavelength: 3839 Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 2500S Special_Requirements: POS TARG 0.5, 0.5 Visit_Number: 2 Visit_Requirements: On_Hold_Comments: Visit_Comments: Exposure_Number: 1 Target_Name: 1045+060 Config: WFPC2 Opmode: IMAGE Aperture: PC1 Sp_Element: F555W Wavelength: 5407 Optional_Parameters: CR-SPLIT=NO Number_of_Iterations: 1 Time_Per_Exposure: 600S Special_Requirements: Exposure_Number: 2 Target_Name: 1045+060 Config: WFPC2 Opmode: IMAGE Aperture: PC1 Sp_Element: F555W Wavelength: 5407 Optional_Parameters: CR-SPLIT=NO Number_of_Iterations: 2 Time_Per_Exposure: 700S Special_Requirements: Exposure_Number: 3 Target_Name: 1045+060 Config: WFPC2 Opmode: IMAGE Aperture: WF3 Sp_Element: FQUVN Wavelength: 3916 Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 2400S Special_Requirements: Exposure_Number: 4 Target_Name: 1045+060 Config: WFPC2 Opmode: IMAGE Aperture: WF3 Sp_Element: FQUVN Wavelength: 3916 Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 2400S Special_Requirements: POS TARG 0.5, 0.5 Visit_Number: 3 Visit_Requirements: On_Hold_Comments: Visit_Comments: Exposure_Number: 1 Target_Name: 1207-107 Config: WFPC2 Opmode: IMAGE Aperture: PC1 Sp_Element: F555W Wavelength: 5407 Optional_Parameters: CR-SPLIT = NO Number_of_Iterations: 1 Time_Per_Exposure: 600S Special_Requirements: Exposure_Number: 2 Target_Name: 1207-107 Config: WFPC2 Opmode: IMAGE Aperture: PC1 Sp_Element: F555W Wavelength: 5407 Optional_Parameters: CR-SPLIT = NO Number_of_Iterations: 2 Time_Per_Exposure: 700S Special_Requirements: Exposure_Number: 3 Target_Name: 1207-107 Config: WFPC2 Opmode: IMAGE Aperture: WF3 Sp_Element: FQUVN Wavelength: 3916 Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 2400S Special_Requirements: Exposure_Number: 4 Target_Name: 1207-107 Config: WFPC2 Opmode: IMAGE Aperture: WF3 Sp_Element: FQUVN Wavelength: 3916 Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 2400S Special_Requirements: POS TARG 0.5, 0.5 Visit_Number: 4 Visit_Requirements: On_Hold_Comments: Visit_Comments: Exposure_Number: 1 Target_Name: 1313-156 Config: WFPC2 Opmode: IMAGE Aperture: PC1 Sp_Element: F555W Wavelength: 5407 Optional_Parameters: CR-SPLIT = NO Number_of_Iterations: 1 Time_Per_Exposure: 600S Special_Requirements: Exposure_Number: 2 Target_Name: 1313-156 Config: WFPC2 Opmode: IMAGE Aperture: PC1 Sp_Element: F555W Wavelength: 5407 Optional_Parameters: CR-SPLIT = NO Number_of_Iterations: 2 Time_Per_Exposure: 700S Special_Requirements: Exposure_Number: 3 Target_Name: 1313-156 Config: WFPC2 Opmode: IMAGE Aperture: WF2 Sp_Element: FQUVN Wavelength: 3986 Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 2400S Special_Requirements: Exposure_Number: 4 Target_Name: 1313-156 Config: WFPC2 Opmode: IMAGE Aperture: WF2 Sp_Element: FQUVN Wavelength: 3986 Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 2400S Special_Requirements: POS TARG 0.5, 0.5 Visit_Number: 5 Visit_Requirements: On_Hold_Comments: Visit_Comments: Exposure_Number: 1 Target_Name: 2206-187 Config: WFPC2 Opmode: IMAGE Aperture: PC1 Sp_Element: F555W Wavelength: 5407 Optional_Parameters: CR-SPLIT = NO Number_of_Iterations: 1 Time_Per_Exposure: 600S Special_Requirements: Exposure_Number: 2 Target_Name: 2206-187 Config: WFPC2 Opmode: IMAGE Aperture: PC1 Sp_Element: F555W Wavelength: 5407 Optional_Parameters: CR-SPLIT = NO Number_of_Iterations: 2 Time_Per_Exposure: 700S Special_Requirements: Exposure_Number: 3 Target_Name: 2206-187 Config: WFPC2 Opmode: IMAGE Aperture: WF4 Sp_Element: FQUVN Wavelength: 3839 Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 2400S Special_Requirements: Exposure_Number: 4 Target_Name: 2206-187 Config: WFPC2 Opmode: IMAGE Aperture: WF4 Sp_Element: FQUVN Wavelength: 3839 Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 2400S Special_Requirements: POS TARG 0.5, 0.5 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: ! ! Lawrence Livermore National Lab ! oratory ,7000 East Ave., L-413, ! Livermore, CA 94550 ! ! 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