! 6749f2.prop using the Non-Interrupt ! The Non-Interrupt part simply chop the first obs into sections, ! without optimize (regroup) the iterations. ! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6749,v 9.1 1996/12/13 15:35:34 pepsa Exp $ ! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6749,v 9.1 1996/12/13 15:35:34 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: Manning ! Phone: 410-338-4456 , E-mail: manning@stsci.edu ! ! This partially completed template was generated from a Phase I proposal. ! Name of Phase I Proposal: archive-0927.danly.prop ! Date generated: Fri Dec 22 16:56:51 EST 1995 ! Proposal_Information ! Section 4 Title: A Study of the Gaseous Halo of the Andromeda Galaxy Proposal_Category: GO Scientific_Category: GALAXIES & CLUSTERS Cycle: 6 Investigators PI_name: Dr. Laura Danly PI_Institution: Space Telescope Science Institute CoI_Name: Dr. J. Chris Blades CoI_Institution: Space Telescope Science Institute Contact: ! Y or N (designate at most one contact) CoI_Name: Dr. David Bowen CoI_Institution: Space Telescope Science Institute Contact: ! Y or N (designate at most one contact) CoI_Name: Dr. Elias Brinks CoI_Institution: NRAO Contact: ! Y or N (designate at most one contact) CoI_Name: Prof. Colin Norman CoI_Institution: Johns Hopkins University Contact: ! Y or N (designate at most one contact) CoI_Name: Prof. Rene Walterbos CoI_Institution: New Mexico State University Contact: ! Y or N (designate at most one contact) CoI_Name: Paul Lee CoI_Institution: Space Telescope Science Institute Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) We propose to study the gaseous environment of the Andromeda Galaxy (M31) by obtaining absorption line spectra of O I, Mg II, C II, Si II, C IV, and Si IV toward bright QSOs/AGN behind the galaxy. The lines of sight pass through a range of z- heights above the mid-plane (i.e. 3 - 16 kpc) and galactocentric distances (i.e. 20 - 40 kpc), permitting a study of different regions of this star forming galaxy. We will investigate the distribution, ionization, and kinematics of circum-galactic gas in M31 to gain insight into the physical mechanisms which govern its nature. We will compare results from M31 to the Milky Way, and will also use the data to provide information on the small scale structure on Milky Way halo gas. Learning about the physical mechanisms governing the origin and conditions in gas in the vicinity of galaxies provides a basis by which to interpret QSO absorption systems which are widely believed to originate in the vicinity of galaxies. An absorption line survey of the halo of our ``sister" spiral galaxy, Andromeda, has never before been conducted. The ultraviolet spectroscopic capability of HST provides the only means by which to accomplish this scientific goal. Questions ! Free format text (please update) Observing_Description: We propose observing 2 QSOs with the G140L grating of the GHRS and 2 QSOs with both the G140L and G270M gratings. The G140L will cover the wavelength range at which Si IV, C IV, Si II, C II, and O I absorption will be expected from M31, while the G270M will cover the wavalengths at which Mg II absorption is expected. For all exposures, we will obtain WAVECALs to ensure the best accuracy. Exposure times are shown in Table 1, and are estimated either from known UV fluxes (Q00339+4005), or from V magnitudes extrapolated to 1400 Angstrom\ and 2800 Angstrom\ assuming the QSO flux follows a power law of the form F_Nu \propto nu^-1. Exposure times are calculated to give a minimum S/N of 13 per pixel for half stepped data from the G140L grating, except for Q0034+3921 which is bright enought to give a S/N of 8 in a plausible exposure time. Exposure times were then adjusted to the nearest total exposure time corresponding to an integral number of orbits. Table 1 lists the 2Sigma equivalent width detection limit, assuming a background count rate of 36 counts diode^-1 hr^-1, and a resolving power of 2150 with the G140L at Si IV and R=2400 at C IV. These limits are smaller or comparable to the equivalent widths of absorption lines through our own Galactic halo, ~ 0.2 Angstrom , ~ 0.3 Angstrom . Exposure times are calculated to give a S/N of 5 per pixel for half stepped data from the G270M grating for Q0039+4005 & Q0039+4003. A S/N of 5 gives a 2Sigma equivalent width limit of 0.03 Angstrom\ for a resolving power of 30,000 with the G270M. These limits will permit a search for the same low equivalent width absorption lines seen at higher redshift in QSO spectra. Real_Time_Justification: None. Groundbased optical observations of the background targets will be obtained at the William Herschel Telescope on La Palma in October 1995. Data will be obtained on Ca II and Na I absorption in the vicinity of M31. However, the ground based optical data is not capable of providing information on atomic species arising in highly ionized gas. Further, while the optical data should provide information on the kinematics of any high column density material near M31, the Ca II and Na I lines are up to a thousand times less sensitive than the ultraviolet lines such as Mg II and C II. The optical lines are not suited to studying the low column density gas in the outskirts of M31; the sensitive UV lines are required. Results from our ground based program may affect our HST program in the following ways. If for some reason, one of our targets is found to be unsuitable as a background source (i.e. highly variable, low flux compared to literature values, etc.), we will adjust our observing program to maximize the scientific productivity. Second, if the Ca II observations are found to be unusually strong, suggesting possible saturation, we will adjust our program to observe a Mg II line that will not be saturated. Results from the ground based program will be in hand before the TAC meets; we will alert the TAC to any changes as needed. Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: Fixed_Targets ! Section 5.1 Target_Number: 1 Target_Name: 0039+4005 Alternate_Names: CGPG 0039.2+4005, MRK 0957, 5C3.100 Description: Galaxy, Seyfert, Radio Galaxy Position: RA=0H 41M 53.37S +/- 0.01S, DEC=+40D 21' 17.5" +/- 0.1", PLATE-ID=01JV Equinox: J2000 RV_or_Z: Z=0.073 Flux: V = 15.14, B-V=0.80 ! Include at least V and B-V Comments: EMISSION LINES CONTAMINATE B-V COLORS; CONTINUUM IS ASSUMED FLAT. Target_Number: 2 Target_Name: 0039+4003 Alternate_Names: CGPG 0039.5+4003, IV Zw 029 Description: Galaxy, Seyfert Position: RA=0H 42M 16.09S +/- 0.01S, DEC=+40D 19' 35.9" +/- 0.1", PLATE-ID=01JV Equinox: J2000 RV_or_Z: Z=0.102 Flux: V = 16.3, B-V=0.75 ! Include at least V and B-V Comments: EMISSION LINES CONTAMINATE B-V COLORS; CONTINUUM IS ASSUMED FLAT. Target_Number: 3 Target_Name: 0035+4112 Alternate_Names: S 10721 Description: Galaxy, Seyfert Position: RA=0H 38M 33.12S +/- 0.01S, DEC=+41D 28' 50.3" +/- 0.1", PLATE-ID=01JV Equinox: J2000 RV_or_Z: Z=0.073 Flux: V = 17.0 ! Include at least V and B-V Comments: EMISSION LINES CONTAMINATE B-V COLORS; CONTINUUM IS ASSUMED FLAT. Target_Number: 4 Target_Name: 0035+4112a Alternate_Names: S 10721 Description: Galaxy, Seyfert Position: RA=0H 38M 33.12S +/- 0.01S, DEC=+41D 28' 50.3" +/- 0.1", PLATE-ID=01JV Equinox: J2000 RV_or_Z: Z=0.073 Flux: V = 17.0 ! Include at least V and B-V Comments: EMISSION LINES CONTAMINATE B-V COLORS; CONTINUUM IS ASSUMED FLAT. Visits ! Section 6 Visit_Number: 1 Visit_Requirements: ! Section 7.1 ! PCS MODE [Fine | Gyro] ! GUIDing TOLerance ! DROP TO GYRO IF NECESSARY [NO REACQuisition] ! SCHEDulability ! SEQ WITHIN