! File: 3706C.PROP ! Database: PEPDB ! Date: 19-FEB-1994:16:54:03 coverpage: title_1: THE NATURE OF GASEOUS LOOPS IN THE MILKY WAY HALO sci_cat: INTERSTELLAR MEDIUM sci_subcat: ABSORPTION LINES proposal_for: GO cont_id: 3706 pi_fname: LAURA pi_lname: DANLY pi_inst: SPACE TELESCOPE SCIENCE INSTITUTE pi_country: USA pi_phone: 301-338-4730 hours_pri: 6.79 num_pri: 3 hrs: Y funds_amount: 65412 funds_length: 12 off_fname: PETER off_lname: STOCKMAN off_title: ASSOCIATE DIRECTOR off_inst: SPACE TELESCOPE SCIENCE INSTITUTE off_addr_1: 3700 SAN MARTIN DRIVE off_city: BALTIMORE off_state: MD off_zip: 21218 off_country: USA off_phone: 301-338-4730 ! end of coverpage abstract: line_1: Recent evidence has shown that the nature of the gaseous halos of galaxies line_2: both depends upon and contributes to the nature of the underlying disk. line_3: "Galactic fountain" theories propose that hot gas produced in the disk rises to line_4: large scale height where it cools and flows back to the disk in a rain of cool line_5: clouds. Because of their anomolous negative velocities, the high latitude line_6: neutral hydrogen clouds are thought to be the returning gas in this halo line_7: circulation scheme. Most of the infalling gas is found in large, coherent line_8: loop-like structures toward the North Galactic Pole. We propose to study halo line_9: circulation by observing the kinematics and ionization balance the intermediate line_10: velocity clouds through absorption line observations of both high and low line_11: ionization species. By studying the ionization balance, we hope to determine line_12: the nature of the gas heating and cooling processes. Together with the line_13: kinematic information available through high spectral resolution GHRS data, line_14: we expect to be able to place severe constraints upon galactic circulation line_15: models. ! ! end of abstract general_form_proposers: lname: DANLY fname: LAURA title: PI inst: SPACE TELESCOPE SCIENCE INSTITUTE country: U.S.A. ! lname: BENJAMIN fname: ROBERT inst: UNIVERSITY OF TEXAS AT AUSTIN country: U.S.A. ! lname: KUNTZ fname: KIP mi: D. inst: SPACE TELESCOPE SCIENCE INSTITUTE country: U.S.A. ! lname: ALBERT fname: ELISE inst: UNITED STATES NAVAL ACADEMY country: U.S.A. ! lname: SHAPIRO fname: PAUL inst: UNIVERSITY OF TEXAS AT AUSTIN country: U.S.A. ! ! end of general_form_proposers block general_form_text: question: 2 section: 1 line_1: LEFT BLANK AS INSTRUCTED ! question: 3 section: 1 line_1: We propose to observe three lines of sight with the GHRS line_2: through the SSA each at three settings of grating G160M. The line_3: line of sights are toward the stars: line_5: HD 121800: l=113, b=49, V=9.1, B-V=+0.04, E(B-V)=0.06, line_6: Spectral type B2 V, D=2200 pc, Z=1650 pc line_8: BD+49 2137: l=134, b=66, V=10.7, line_9: Spectral type B7 V, Z=1600 pc line_11: BD+38 2182: l=182, b=62, V=11.2, B-V=-0.22, E(B-V)=0.02, line_12: Spectral type B2 V, D=4600 pc, Z=4100 pc \bigskip The three line_13: grating settings are centered as follows: 1. 1550 \AA. line_14: (Useable range 1534\AA - 1566\AA ) This setting will obtain line_15: the C IV $\lambda$$\lambda$1548-1550 lines. This setting line_16: will also obtain the weak C I line at $\lambda$1560, which line_17: will be used with the HI data to understand the neutral line_18: component. ! question: 3 section: 2 line_1: 2. 1403 \AA. (Useable range 1387\AA - 1419\AA ) This setting line_2: will obtain the Si IV $\lambda$$\lambda$1393,1402 lines. line_3: Comparing these line strengths to the C IV line strengths is line_4: a principle diagnostic for hot gas. line_6: 3. 1249 \AA. (Useable range 1233\AA - 1265\AA ) This line_7: setting will obtain the N V $\lambda$1238-1242 lines. The line_8: high ionization potential of N V (77.5 eV) means that this line_9: line is a good diagnostic of hot gas. This setting will also line_10: obtain the strong low ionization lines S II $\lambda$1250, line_11: $\lambda$1253, $\lambda$1259, Si II $\lambda$1260. These low line_12: ionization lines are important diagnostics of the "warm" line_13: gas, as their spread of f-values allows a wide range of line_14: sensitivity. line_16: The exposure times were chosen to achieve S/N=50 and line_17: detection limits of about 4 mA for the HD 121800 line of line_18: sight, and S/N=30 and detection limits of about 7 mA for the line_19: BD+49 2137 and BD+38 2182 lines of sight. These signal to line_20: noise ratios will be appropriate for modeling, and will be ! question: 3 section: 3 line_1: adequate for the comparison with Space Telescope archive line_2: data for HD 93512. There are exposures of HD 121800 line_3: scheduled as part of GO program No.2257, however, the GO line_4: (Blair Savage) has not yet determined how to reshape his line_5: program in the light of the changest in the observatory line_6: capabilities. If there are exposures of HD 121800 taken as line_7: part of that program, we will utilize the archival spectra line_8: when they become available. ! question: 4 section: 1 line_1: High resolution, high S/N observations of a range of ions line_2: (including C IV, Si IV and N V) are necessary to study the line_3: nature of the ionization in the IV arch. Previous data line_4: taken with the IUE satellite are shown in Figure 3. While line_5: the data are tantalizing, they lack sufficient resolution line_6: and S/N to address the specific objectives of this proposal. line_7: In order to observe the highly ionized species at high line_8: resolution (about 13 km/s) and high S/N (S/N$\sim$30 for BD line_9: +38 2182 and BD +49 2137; S/N$\sim$50 for HD 121800) we line_10: require the capabilities of the GHRS on HST. line_12: Over the past decade, we have pursued studies of galactic line_13: halo gas using ground based optical, 21-cm H I, and IUE line_14: ultraviolet observations. Results from these extensive line_15: studies have laid the groundwork for the scientific line_16: objectives of this proposal. However, only the proposed HST line_17: observations will result in sufficiently high quality cloud line_18: column densities and velocites to compare with specific line_19: predictions of models for cooling gas. No ground based line_20: facilities or other space based facilities are capable of line_21: provided the data required to address the scientific issues line_22: outlined in this proposal. ! question: 5 section: 1 line_1: Wave calibrations are required for all nine GHRS spectra line_2: (3 spectra for each of 3 stars). see below. ! question: 6 section: 1 line_1: Wave calibrations are required for all nine GHRS spectra line_2: (3 spectra for each of 3 stars). This was not included line_3: in the Phase I proposal, but is now recognized as line_4: critical to the success of the program. Absolute velocity line_5: calibration to about 2-3 km/s is required. Each wave line_6: calibration must be performed with no gap immediately line_7: preceeding each spectral exposure. ! question: 7 section: 1 line_1: The proposers have had extensive experience with reducing line_2: spectral data, both optical and ultraviolet. Initial line_3: reduction, and, if necessary, recalibration shall be line_4: accomplished at Space Telescope Science Institute using the line_5: STSDAS software. Detailed analysis to determine column line_6: densities, velocities, and velocity widths of the absorption line_7: line profiles will be accomplished with the existing KDAF line_8: software package (an IDL based IUE-RDAF derivative). This line_9: procedure will ensure a reduction that adheres to Space line_10: Telescope standards, yet will allow easy comparison with line_11: existing IUE and optical data. line_13: The data on both the high ionization species {\it and} the line_14: weakly ionized and neutral species will be analyzed in the line_15: context of models for the production of gas in the galactic line_16: fountain. Two of us (PS and RB) have developed and refined line_17: models for predicting the non-equilibrium radiative cooling, line_18: ionization, and recombination of halo gas (for descriptions, line_19: see Shapiro, P.R. and Benjamin, R. A. 1991, Publ. A.S.P., ! question: 7 section: 2 line_1: Vol. 103, in press; Shapiro, P. R. 1991, proc. from I.A.U. line_2: Symp. No. 144 on ``The Interstellar Disk-Halo Connection in line_3: Galaxies, p 417). We wish to determine if the observed line_4: column densities {\it and} kinematics give a self-consistent line_5: picture of both the heating and flow which are predicted line_6: according to the galactic fountain. Whatever results are line_7: obtained on the physical conditions of the gas will shed line_8: light as to its origin. ! question: 8 section: 1 line_1: This proposal is one of several programs (including an line_2: accepted GO program; see Question 8) designed to study gas line_3: in the environments of galaxies. These programs have been line_4: tailored specifically to meet the objectives outlined in the line_5: P.I.'s (accepted) Hubble Fellowship proposal. The goal of line_6: the Hubble Fellowship research is to study gas which is in line_7: the vicinity of a variety of galaxies, and is therefore line_8: subjected to a range of interstellar and intergalactic line_9: environments. Central to this research is a detailed study line_10: of the production and maintenance of Milky Way halo gas, line_11: where we can expect to obtain the highest quality data and line_12: develop the most detailed models. Accurate means to line_13: interpret quantitative spectroscopic data are critical to line_14: the interpretation of QSO absorption lines. line_16: Related Cycle 2 proposals include: line_18: $\bullet$ ``Spectroscopic Investigations of a Possible line_19: Galactic Chimney" (Danly, L, Albert, C. E., and Kuntz, K. line_20: D.) ! question: 8 section: 2 line_1: line_2: $\bullet$ ``A detailed Study of Nearby Ly$\alpha$ Systems" line_3: (Urry, C. M., Boggess, A., Maraschi, L., Danly, L., line_4: Bruhweiler, F. C., Falomo, R., Grady, C. A., Tanzi, E. G., line_5: and Treves, A.) line_7: $\bullet$ ``The Distance of High Velocity Clouds" (Wakker, line_8: B. P., Danly, L., Schwarz, U. J., and Van Woerden, H.) line_10: $\bullet$ ``Quasar Absorption Line Studies of Starburst line_11: Galaxy Enviornments" (Norman, C. N., Blades, J. C., Danly, line_12: L., and Heckman, T. J.) ! question: 9 section: 1 line_1: \ques{\phantom{8.} a. List HST program numbers and titles, line_2: and specify whether they are related to this project or line_3: not.} line_5: Proposal No. 2644, ``The Environments of Starburst Galaxies: line_6: Absorption-Line Studies of Galactic Outflows line_8: This GO program is related to the objectives of this line_9: proposal as described in Question 7. line_11: \ques{\phantom{8.} b. Summarize the main results obtained line_12: from previous related programs.} line_14: The data have not yet been obtained line_16: \ques{\phantom{8.} c. List publications resulting from the line_17: above data (Format: Title, Authors, Journal, Volume, Page, line_18: and Year.)} line_20: N/A (see 8b) ! question: 10 section: 1 line_1: The Space Telescope Science Institute has a wide variety of line_2: hardware and software systems to support the research line_3: proposed here. These include STSDAS, IDL, and KDAF which line_4: are supported on both the VAX cluster and the Sun line_5: Workstations. ! !end of general form text general_form_address: lname: DANLY fname: LAURA category: PI inst: SPACE TELESCOPE SCIENCE INSTITUTE addr_1: 3700 SAN MARTIN DRIVE city: BALTIMORE state: MD zip: 21218 country: USA phone: 301-338-4422 telex: 684-9101-STSCI-411 ! ! end of general_form_address records fixed_targets: targnum: 10 name_1: HD121800 name_2: GSC04177-00880 descr_1: A,110; G,508,510; pos_1: PLATE-ID=01BR, pos_2: RA= 13H 55M 15.4S +/- 0.2S, pos_3: DEC= +66D 7' 0.7" +/- 1" equinox: J2000 rv_or_z: V=13 fluxnum_1: 1 fluxval_1: V=9.1, TYPE=B2V, E(B-V)=0.06 fluxnum_2: 2 fluxval_2: B-V=-0.17 fluxnum_3: 3 fluxval_3: F-CONT(1240) = 16 E-11 fluxnum_4: 4 fluxval_4: F-CONT(1400) = 1 E-10 fluxnum_5: 5 fluxval_5: F-CONT(1550) = 9 E-11 ! targnum: 20 name_1: BD+49D2137 name_2: GSC03458-00650 descr_1: G,508,510; descr_2: A,110; pos_1: PLATE-ID=024D, pos_2: RA= 12H 25M 0.4S +/- 0.1S, pos_3: DEC= +49D 8' 30.4" +/- 1" equinox: J2000 rv_or_z: V=115 fluxnum_1: 1 fluxval_1: V=10.7, TYPE=B7V, E(B-V)=0.02 fluxnum_2: 2 fluxval_2: B-V=-0.14 fluxnum_3: 3 fluxval_3: F-CONT(1240) = 2 E-12 fluxnum_4: 4 fluxval_4: F-CONT(1400) = 18 E-13 fluxnum_5: 5 fluxval_5: F-CONT(1550) = 17 E-13 ! targnum: 30 name_1: BD+38D2182 name_2: GSC03009-02485 descr_1: G,508,510; descr_2: A,110; pos_1: PLATE-ID=01R8, pos_2: RA= 10H 49M 12.9S +/- 0.1S, pos_3: DEC= +38D 0' 14.5" +/- 1" equinox: J2000 rv_or_z: V=79 fluxnum_1: 1 fluxval_1: V=11.2, TYPE=B2V, E(B-V)=0.02 fluxnum_2: 2 fluxval_2: B-V=-0.22 fluxnum_3: 3 fluxval_3: F-CONT(1240) = 36 E-13 fluxnum_4: 4 fluxval_4: F-CONT(1400) = 22 E-13 fluxnum_5: 5 fluxval_5: F-CONT(1550) = 17 E-13 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: HD121800 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 1.8S fluxnum_1: 1 priority: 1 param_1: BRIGHT=RETURN req_1: ONBOARD ACQ FOR 1.10 - 1.60; req_2: CYCLE 2 / 1.0 - 3.60 ! linenum: 1.100 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1249 num_exp: 1 time_per_exp: DEF priority: 1 param_1: STEP-PATT=5 req_1: CALIB FOR 1.2; req_2: SEQ 1.1-1.2 NO GAP ! linenum: 1.200 targname: HD121800 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1249 num_exp: 1 time_per_exp: 490S s_to_n: 50 fluxnum_1: 3 priority: 1 param_1: FP-SPLIT=STD param_2: STEP-PATT=5 comment_1: EXPOSURE TIME IS NEAREST INTEGER comment_2: LARGER THAN INTEGER MULTIPLE OF 27.2 S ! linenum: 1.300 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1403 num_exp: 1 time_per_exp: DEF priority: 1 param_1: STEP-PATT=5 req_1: CALIB FOR 1.4; req_2: SEQ 1.3-1.4 NO GAP ! linenum: 1.400 targname: HD121800 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1403 num_exp: 1 time_per_exp: 688S s_to_n: 50 fluxnum_1: 4 priority: 1 param_1: FP-SPLIT=STD param_2: STEP-PATT=5 comment_1: EXPOSURE TIME IS NEAREST INTEGER comment_2: LARGER THAN INTEGER MULTIPLE OF 27.2 S ! linenum: 1.500 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1550 num_exp: 1 time_per_exp: DEF priority: 1 param_1: STEP-PATT=5 req_1: CALIB FOR 1.6; req_2: SEQ 1.5-1.6 NO GAP ! linenum: 1.600 targname: HD121800 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1550 num_exp: 1 time_per_exp: 980S s_to_n: 50 fluxnum_1: 5 priority: 1 param_1: FP-SPLIT=STD param_2: STEP-PATT=5 comment_1: EXPOSURE TIME IS NEAREST INTEGER comment_2: LARGER THAN INTEGER MULTIPLE OF 27.2 S ! linenum: 2.000 targname: BD+49D2137 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 1.8S fluxnum_1: 1 priority: 1 param_1: BRIGHT=RETURN req_1: ONBOARD ACQ FOR 2.10 - 2.60; ! linenum: 2.100 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1249 num_exp: 1 time_per_exp: DEF priority: 1 param_1: STEP-PATT=5 req_1: CALIB FOR 2.2; req_2: SEQ 2.1-2.2 NO GAP ! linenum: 2.200 targname: BD+49D2137 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1249 num_exp: 3 time_per_exp: 20M s_to_n: 30 fluxnum_1: 3 priority: 1 param_1: FP-SPLIT=STD param_2: STEP-PATT=5 ! linenum: 2.300 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1403 num_exp: 1 time_per_exp: DEF priority: 1 param_1: STEP-PATT=5 req_1: CALIB FOR 2.4; req_2: SEQ 2.3-2.4 NO GAP ! linenum: 2.400 targname: BD+49D2137 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1403 num_exp: 3 time_per_exp: 20M s_to_n: 30 fluxnum_1: 4 priority: 1 param_1: FP-SPLIT=STD param_2: STEP-PATT=5 ! linenum: 2.500 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1550 num_exp: 1 time_per_exp: DEF priority: 1 param_1: STEP-PATT=5 req_1: CALIB FOR 2.6; req_2: SEQ 2.5-2.6 NO GAP ! linenum: 2.600 targname: BD+49D2137 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1550 num_exp: 4 time_per_exp: 20M s_to_n: 30 fluxnum_1: 5 priority: 1 param_1: FP-SPLIT=STD param_2: STEP-PATT=5 ! linenum: 3.000 targname: BD+38D2182 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 1.8S fluxnum_1: 1 priority: 1 param_1: BRIGHT=RETURN req_1: ONBOARD ACQ FOR 3.10 - 3.60; ! linenum: 3.100 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1249 num_exp: 1 time_per_exp: DEF priority: 1 param_1: STEP-PATT=5 req_1: CALIB FOR 3.2; req_2: SEQ 3.1-3.2 NO GAP ! linenum: 3.200 targname: BD+38D2182 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1249 num_exp: 2 time_per_exp: 24M s_to_n: 30 fluxnum_1: 3 priority: 1 param_1: FP-SPLIT=STD param_2: STEP-PATT=5 ! linenum: 3.300 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1403 num_exp: 1 time_per_exp: DEF priority: 1 param_1: STEP-PATT=5 req_1: CALIB FOR 3.4; req_2: SEQ 3.3-3.4 NO GAP ! linenum: 3.400 targname: BD+38D2182 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1403 num_exp: 3 time_per_exp: 20M s_to_n: 30 fluxnum_1: 4 priority: 1 param_1: FP-SPLIT=STD param_2: STEP-PATT=5 ! linenum: 3.500 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1550 num_exp: 1 time_per_exp: DEF priority: 1 param_1: STEP-PATT=5 req_1: CALIB FOR 3.6; req_2: SEQ 3.5-3.6 NO GAP ! linenum: 3.600 targname: BD+38D2182 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1550 num_exp: 4 time_per_exp: 30M s_to_n: 30 fluxnum_1: 5 priority: 1 param_1: FP-SPLIT=STD param_2: STEP-PATT=5 ! ! end of exposure logsheet ! No scan data records found