! Proposal 5892, submission 3 ! PI: Dr. Michael Shull ! Received Thu Aug 31 18:58:32 EDT 1995 ! From: spenton@casa.Colorado.EDU ! Proposal 5892, submission 2 ! PI: Dr. Michael Shull ! Received Fri Mar 24 14:21:28 EST 1995 ! From: spenton@casa.Colorado.EDU ! Proposal 5892, submission 1 ! PI: Dr. Michael Shull ! Received Fri Mar 10 16:50:03 EST 1995 ! From: spenton@casa.Colorado.EDU ! Hubble Space Telescope Cycle 5 (1995) Phase II Proposal Template ! $Id: 5892,v 5.1 1995/09/05 20:49:10 pepsa Exp $ ! MODIFIED BY A. BERMAN 3/16/95. DELETED END ORBITS, ADDED ONBOARD ACQ ! FOR AND ADJUSTED ACQ EXPOSURE TIMES TO 13.5S. ! ! 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: Alice Berman ! Phone: 410 338-4462 , E-mail: aberman@stsci.edu ! ! This partially completed template was generated from a Phase I proposal. ! Proposal_Information ! Section 4 Title: PHYSICAL CONDITIONS IN THE GALACTIC HALOS OF THE MILKY WAY AND NGC 3067 Proposal_Category: GO Scientific_Category: Interstellar Medium Cycle: 5 Investigators PI_name: Dr. Michael Shull PI_Institution: University of Colorado, Boulder CoI_Name: Dr. John Stocke CoI_Institution: University of Colorado, Boulder Contact: ! Y or N (designate at most one contact) CoI_Name: Mr. Steve Penton CoI_Institution: University of Colorado, Boulder Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) We propose to conduct a detailed GHRS spectroscopic study of the metal absorption lines in the halo gas of the Milky Way and NGC 3067, using the quasar 3C 232 as a background source. Because 3C 232 is the only QSO metal-line system imaged in H I emission for which we can study metal-line ratios in detail, it provides a rare opportunity to measure abundances, grain depletions, and photoionizing radiation fields in halo gas. Discovered in 21-cm and Ca II absorption, the NGC 3067 absorption system has now been studied in 21-cm emission and absorption (VLA, Westerbork) and in UV absorption (IUE, HST/FOS) with 3 components spread over 160 kms. The H I cloud is almost certainly a tidal tail, pulled out of NGC 3067 some (10 kpc)h_75^-1 into the halo. We will measure column densities of Fe I and II, Mg I and II, S II, Mn II, Si II, C IV, Si IV, and perhaps C II and O I. These abundances and the H I emission characteristics can be used to determine metallicities and grain depletions in the halos of NGC 3067 and the Milky Way. The Fe I/Fe II and Mg I/Mg II ionization equilibrium, coupled with H I columns, will be used to set the metagalactic photoionizing radiation field and to model the thermal equilibrium of halo gas. The C IV/Si IV absorption can be used to diagnose the relative effects of photoionization and hot gas in these halo absorption systems. The depletion factors of Si, Mn, and Fe will be used to estimate the amount of grain disruption during the tidal encounter. Questions ! Free format text (please update) Observing_Description: Our program requires us to measure a sufficient number of resonance absorption lines of key interstellar species (Mg, Fe, Si, S, Mg, Mn) to obtain abundances and depletion factors in the halos of the Galaxy and NGC 3067. In addition, we need to measure the ionization fractions, Fe I/Fe II and Mg I/Mg II, in order to determine the ionizing radiation field. Finally, to resolve the 3 known velocity components of the NGC 3067 absorption, spread over 160 kms, and to separate some Galactic lines from lines in NGC 3067, we need to make some of our measurements at resolution R = 20,000. The planned observing program consists of two parts. In Part I, we will use grating G270M (5 settings at R = 20,000 and S/N = 10) for the long-wavelength lines (2339 -- 2880 Angstrom) as shown in Figure 3. These observations require 20 orbits and will provide good measurements of Fe I, Fe II, Mg I, Mg II, and Mn II. In Part II, we will use grating G140L (2 settings at R = 2000) for the region 1150 -- 1716 Angstrom. These observations require 6 orbits and will measure Si II, S II, C IV, Si IV, and possibly C II and O I. The target, 3C 232, lies at 33^degrees declination and has a 54-min clear viewing zone per orbit. The GHRS observing times were computed for S/N = 10 (Part I) and S/N = 20 (Part II) breaking up the observing into 20-minute ``FP-split'' segments to handle pattern noise. The two tables below summarize the breakdown of these observations into ``orbits''. In Part I, we have optimized time by fitting the changes in G270M grating setting into some of the orbits (hence the fractional orbit listings). , begincenter TABLE 1: Part I: Wavelength Settings for G 270M , endcenter begincenter begintabularccrrl Setting & Wavelengths & Expo & Orbits & Ions , & (Angstrom) & (min) & & , 1 & 2835 - 2880 & 160 & 4.5 & Mg I , 2 & 2782 - 2828 & 144 & 3.5 & Mg II , 3 & 2577 - 2624 & 140 & 3.5 & Mn II, Fe II , 4 & 2488 - 2535 & 140 & 4.0 & Fe I , 5 & 2339 - 2387 & 180 & 4.5 & Fe II , endtabular endcenter vspace1cm begincenter TABLE 2: Part II: Wavelength Settings for G 140L , endcenter begincenter begintabularccrrl Setting & Wavelengths & Expo & Orbits & Ions , & (Angstrom) & (min) & & , 1 & 1150 - 1436 & 81 & 2 & S II, C II, Si II, O I, Si IV , 2 & 1430 - 1716 & 153 & 4 & Si IV, C IV, Si II, Fe II , endtabular endcenter Real_Time_Justification: None A key question about the extended H I emission and metal-line absorption cloud in the NGC 3067 halo is its tidal origin. We will conduct a ground-based (optical) deep spectroscopic survey searching for galaxies in the field down to B = 19 over a 1^degrees field of view. These observations will be proposed at the WIYN telescope using the HYDRA spectrograph. Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: Fixed_Targets ! Section 5.1 ! Target Data updated 8/28/95 - AFB Target_Number: 1 Target_Name: 3C232 Alternate_Names: 0955+326 Description: GALAXY,QSO Position: RA = 9H 58M 21.00S +/- 0.04S, DEC = 32D 24' 2.3" +/- 0.5", PLATE-ID = 01RS Equinox: J2000 RV_or_Z: Z=0.533 RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: 1983.132 Annual_Parallax: Flux: V=15.78, B-V=0.1 ! Include at least V and B-V Comments: Coordinates are from an inventory GASP measurement by ABerman ! Original values: ! Position: RA=09H 58M 21.0S +/-0.05S, ! DEC=32D 24' 01.9" +/-0.05" ! Equinox: 2000. ! 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 On_Hold_Comments: Visit_Comments: 3C232-G270M-2 Wavelength settings Exposure_Number: 1 ! Section 6.5 Target_Name: 3C232 Config: HRS Opmode: ACQ Aperture: 2.0 Sp_Element: MIRROR-N2 Wavelength: Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 13.5S Special_Requirements: ONBOARD ACQ FOR 2-3 ! Section 7.2 Comments: STEP-TIME=1.5S Exposure_Number: 2 ! Section 6.5 Target_Name: 3C232 Config: HRS Opmode: ACCUM Aperture: 2.0 Sp_Element: G270M Wavelength: 2835-2880 Optional_Parameters: FP-SPLIT=NO,STEP-PATT=DEF,DOPPLER=ON Number_of_Iterations: 6 Time_Per_Exposure: 1849.6S Special_Requirements: ! Section 7.2 Exposure_Number: 3 ! Section 6.5 Target_Name: 3C232 Config: HRS Opmode: ACCUM Aperture: 2.0 Sp_Element: G270M Wavelength: 2782-2828 Optional_Parameters: FP-SPLIT=NO,STEP-PATT=DEF,DOPPLER=ON Number_of_Iterations: 5 Time_Per_Exposure: 2148.8S Special_Requirements: Visit_Number:2 Visit_Requirements: ! Section 7.1 On_Hold_Comments: Visit_Comments: 3C232-G270M-2 Wavelength settings Exposure_Number: 4 ! Section 6.5 Target_Name: 3C232 Config: HRS Opmode: ACQ Aperture: 2.0 Sp_Element: MIRROR-N2 Wavelength: Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 13.5S Special_Requirements: ONBOARD ACQ FOR 5-6 ! Section 7.2 Comments: STEP-TIME=1.5S Exposure_Number: 5 ! Section 6.5 Target_Name: 3C232 Config: HRS Opmode: ACCUM Aperture: 2.0 Sp_Element: G270M Wavelength: 2577-2624 Optional_Parameters: FP-SPLIT=NO,STEP-PATT=DEF,DOPPLER=ON Number_of_Iterations: 5 ! 7.7 m subexp Time_Per_Exposure: 1795.2S Special_Requirements: ! Section 7.2 Exposure_Number: 6 ! Section 6.5 Target_Name: 3C232 Config: HRS Opmode: ACCUM Aperture: 2.0 Sp_Element: G270M Wavelength: 2339-2387 Optional_Parameters: FP-SPLIT=NO,STEP-PATT=DEF,DOPPLER=ON Number_of_Iterations: 6 ! 8.14766 m sub exp Time_Per_Exposure: 2148.8S ! 195.54m total Special_Requirements: ! Section 7.2 Visit_Number:3 Visit_Requirements: ! Section 7.1 On_Hold_Comments: Visit_Comments: 3C232-G270M-1 Wavelength Settings Exposure_Number: 7 ! Section 6.5 Target_Name: 3C232 Config: HRS Opmode: ACQ Aperture: 2.0 Sp_Element: MIRROR-N2 Wavelength: Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 13.5S Special_Requirements: ONBOARD ACQ FOR 8 ! Section 7.2 Comments: STEP-TIME=1.5S Exposure_Number: 8 ! Section 6.5 Target_Name: 3C232 Config: HRS Opmode: ACCUM Aperture: 2.0 Sp_Element: G270M Wavelength: 2488-2535 Optional_Parameters: FP-SPLIT=NO,STEP-PATT=DEF,DOPPLER=ON Number_of_Iterations: 5 Time_Per_Exposure: 2094.4S Special_Requirements: ! Uncomment or copy exposure level special requirements needed ! INTeractive ACQuisition FOR ! ONBOARD ACQuisition FOR 1 ! POSition TARGet , ! SAME POSition AS ! DO FOR TARGets ! FGS only ! PARallel WITH ! GROUP-FGS WITHIN