! From: loki@nately.UCSD.EDU (Lance Cottrell) ! ! Hubble Space Telescope Cycle 5 (1995) Phase II Proposal Template ! Id: 6115 ! ! For help call your Program Coordinator: Max Mutchler ! Phone: 410 338-1321 , E-mail: mutchler@stsci.edu Proposal_Information Title: Imaging a Low Redshift Damped LyAlpha Absorption Galaxy Proposal_Category: GO Scientific_Category: Quasars Cycle: 5 Investigators PI_name: Lin Zuo PI_Institution: University of California, San Diego CoI_Name: David Tytler CoI_Institution: University of California, San Diego Contact: Abstract: ! Free format text (please update) The HST Quasar Absorption Snapshot Survey (Tytler et al. 1994) has discovered a low redshift (z_abs=0.576) damped LyAlpha absorption (DLA) trough in the spectrum of quasar 0117+2118. Only one other low redshift damped LyAlpha system has been published. Many people believe that the QSO damped LyAlpha systems are produced by discs of spiral galaxies. The best way to test this proposal is to image the quasar field to find the galaxy responsible. For the high reshift absorbers this is almost impossible because distant galaxies are too faint. Our discovery of a low redshift damped system enables us to actually carry out this essential test. We propose to use WFPC2 with its high spatial resolution capability to image the quasar 0117+2118 field to search for the absorbing galaxy at z=0.576. We will also observe with FOS/G190H to get a better determination of the HI column density and the absorption redshift. We need the HST because (1) DLA absorbers are expected to be very close to the line of sight to the QSO -- few arcsec. (2) We want to determine the type of galaxy which is responsible for the DLA system. (3) We want to measure the distance from the QSO to the center of the galaxy. (4) The far UV spectrum is needed. Questions ! Free format text (please update) Observing_Description: We will use WFPC2 to obtain images in the quasar 0117+2118 field. The F702W (Wide R) filter is chosen because its broad wavelength band and the corresponding maximum system throughput will enable us go deep to see the morphology of faint galaxies. The filter is to the red of the redshifted 4000Angstrom break (the Balmer jump). Since the quasar is relatively bright with a V magnitude 16.05, we expect it to produce charge overflow. This is unfortunate but acceptable since the expected galaxies are extended sources. Dividing the total exposure time into many segments would introduce large readout noise and increase the overhead time tremendously. The observing format proposed here has been demonstrated to be very successful in a similar HST/WFPC2 program: ID number 5176, PI Ed Beaver (Ross Cohen, private communication). 0.5truecm We will also observe with FOS/RD G190H in ACCUM mode. We will use the Binary Search acquisition and the 1.0^'' aperture. The flux level at 1900Angstrom\ is about 1* 10^-15ergs s^-1cm^-2AA^-1 (Fig. 1). With the proposed two orbits observation, we expect to achieve a S/N~eq 15 per diode. We will use Keck Telescope to try to get spectra of the detected galaxies to measure the galaxy emission redshifts. Ground based echelle spectra of the QSO absorption lines will be used to get velocity dispersions and column densities. Combined with our HST/FOS N_HI determination, and lines in the proposed G190H spectrum, we will estimate the metal abundance in the absorbing galaxy. Real_Time_Justification: None. Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: Fixed_Targets Target_Number: 1 Target_Name: PG0117+213 Alternate_Names: Description: GALAXY, Quasar, Lyman Alpha Cloud Position: RA = 01H 20M 17.25S +/- 0.75", DEC = 21D 33' 46.3" +/- 0.75", PLATE-ID=021K Equinox: J2000 RV_or_Z: RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: V=16.05 +/- 0.02 ! Include at least V and B-V Comments: !6504 08 48 50.20 12 02 28.4 10.940 0.22 08 51 34.34 11 51 10.63 Target_Number: 2 Target_Name: MMJ6504 Alternate_Names: Description: STAR Position: RA=08H 51M 34.33S +/- 0.100S, DEC= 11D 51' 10.4" +/- 1.00", PLATE-ID=028I Equinox: J2000 Epoch: 1983.12 Rv_or_z: RA_PM: 0.0 Dec_PM: 0.0 Annual_Parallax: 0.0 Flux: V = 10.94 +/- 0.1 Comments: B-V=0.22 M67 PSF standard star Scan_Data Scan_Number: 1 FGS_scan: Cont_or_Dwell: D Dwell_points: 2 !Dwell_points: 3 Dwell_Secs: 1.0 ! Dummy value Scan_Width: .5 Scan_Length: .5 Sides_Angle: 90.0 Number_Lines: 2 Scan_Rate: First_line_PA: 90. Scan_Frame: S/C Length_Offset: Width_Offset: !VVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVV Visits ! Section 6 Visit_Number: 1 Visit_Requirements: PCS MODE F SEQ 1-2 WITHIN 2H GROUP 1-3 WITHIN 4H ORIENT 99D TO 100D Visit_Comments: This is the first of two orientations. We want these done consecutively. Exposure_Number: 1 Target_Name: PG0117+213 Config: WFPC2 Opmode: IMAGE Aperture: WF3 Sp_Element: F702W Wavelength: 6906.0 Optional_Parameters: ATD-GAIN=7, CR-SPLIT=NO Number_of_Iterations: 1 Time_Per_Exposure: 8S ! this should give about 20,000 counts. Special_Requirements: Comments: Exposure_Number: 2 Target_Name: PG0117+213 Config: WFPC2 Opmode: IMAGE Aperture: WF3 Sp_Element: F702W Wavelength: 6906.0 Optional_Parameters: ATD-GAIN=7, CR-SPLIT=DEF Number_of_Iterations: 2 Time_Per_Exposure: 800S ! with CR-SPLIT this is two 400S Special_Requirements: EXPAND Comments: !VVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVV Visits Visit_Number: 2 Visit_Requirements: PCS MODE F ORIENT -28D TO -30D FROM 1 Visit_Comments: This is the second of two orientations. We want these done consecutively. Exposure_Number: 1 Target_Name: PG0117+213 Config: WFPC2 Opmode: IMAGE Aperture: WF3 Sp_Element: F702W Wavelength: 6906.0 Optional_Parameters: ATD-GAIN=7, CR-SPLIT=NO Number_of_Iterations: 1 Time_Per_Exposure: 8S ! this should give about 20,000 counts. Special_Requirements: Comments: Exposure_Number: 2 Target_Name: PG0117+213 Config: WFPC2 Opmode: IMAGE Aperture: WF3 Sp_Element: F702W Wavelength: 6906.0 Optional_Parameters: ATD-GAIN=7, CR-SPLIT=DEF Number_of_Iterations: 2 Time_Per_Exposure: 800S ! with CR-SPLIT this is two 400S Special_Requirements: EXPAND Comments: !VVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVVV Visit_Number: 3 Visit_Requirements: PCS MODE F Visit_Comments: This is the PSF observation. Exposure_Number: 1 ! Section 6.5 Target_Name: MMJ6504 Config: WFPC2 Opmode: IMAGE Aperture: WF3 Sp_Element: F702W Wavelength: 6906.0 Optional_Parameters: ATD-GAIN=15, CR-SPLIT=NO, SCAN-READ=ALL, READ=3 Number_of_Iterations: 1 Time_Per_Exposure: 0.11S Special_Requirements: SPATIAL SCAN 1 1-4 Comments: Exposure_Number: 2 ! Section 6.5 Target_Name: MMJ6504 Config: WFPC2 Opmode: IMAGE Aperture: WF3 Sp_Element: F702W Wavelength: 6906.0 Optional_Parameters: ATD-GAIN=7, CR-SPLIT=NO, SCAN-READ=ALL, READ=3 Number_of_Iterations: 1 Time_Per_Exposure: 1.0S Special_Requirements: Comments: Exposure_Number: 3 ! Section 6.5 Target_Name: MMJ6504 Config: WFPC2 Opmode: IMAGE Aperture: WF3 Sp_Element: F702W Wavelength: 6906.0 Optional_Parameters: ATD-GAIN=7, CR-SPLIT=NO, SCAN-READ=ALL, READ=3 Number_of_Iterations: 1 Time_Per_Exposure: 10S Special_Requirements: Comments: Exposure_Number: 4 ! Section 6.5 Target_Name: MMJ6504 Config: WFPC2 Opmode: IMAGE Aperture: WF3 Sp_Element: F702W Wavelength: 6906.0 Optional_Parameters: ATD-GAIN=7, CR-SPLIT=NO, SCAN-READ=ALL, READ=3 Number_of_Iterations: 1 Time_Per_Exposure: 38S Special_Requirements: 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: ! ! Center for Astrophysics and Space ! Sciences, Mail Code 0111, ! La Jolla, CA 92093-0111 ! ! 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! ! 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