! File: 4331C.PROP ! Database: PEPDB ! Date: 20-FEB-1994:22:09:26 coverpage: title_1: HOT GAS IN THE DISK AND HALO OF NGC4319 sci_cat: INTERSTELLAR MEDIUM sci_subcat: ABSORPTION LINES proposal_for: GO pi_fname: EDWARD pi_mi: B. pi_lname: JENKINS pi_inst: PRINCETON UNIVERSITY pi_country: U.S.A. hours_pri: 3.50 num_pri: 1 hrs: Y funds_length: 12 off_fname: ALAN off_mi: J. off_lname: SINISGALLI off_title: ASSOC. PROVOST ORPA off_inst: OFFICE OF RESEARCH AND PROJECT ADMINISTRATION off_addr_1: PRINCETON UNIVERSITY off_addr_2: 5 NEW SOUTH BUILDING off_city: PRINCETON off_state: NJ off_zip: 08544 off_country: U.S.A. off_phone: 609-258-3090 ! end of coverpage abstract: line_1: A bright (V = 15.2) Seyfert 1 galaxy, Mrk 205, will be observed line_2: with the G160M mode of GHRS at wavelengths centered on the N V line_3: resonance doublet, in an attempt to detect absorption features from line_4: hot gas in the disk and halo of a foreground spiral galaxy, NGC 4319. line_5: Our objective is to observe relative abundances and the kinematical line_6: behavior of this ion in an environment other than that of our own line_7: galaxy or the Magellanic Clouds, which have been well studied in the line_8: past. In addition to learning more about galactic coronae, our data will line_9: be useful in drawing parallels with unseen systems that produce the line_10: N V, C IV and Si IV features that appear at visible wavelengths in the line_11: spectra of high redshift quasars. ! ! end of abstract general_form_proposers: lname: JENKINS fname: EDWARD title: PI mi: B. inst: PRINCETON UNIVERSITY country: USA esa: N ! lname: JANNUZI fname: BUELL mi: T. inst: INSTITUTE FOR ADVANCED STUDY country: USA esa: N ! lname: SCHNEIDER fname: DONALD mi: P. inst: INSTITUTE FOR ADVANCED STUDY country: USA esa: N ! lname: BAHCALL fname: JOHN mi: N. inst: INSTITUTE FOR ADVANCED STUDY country: USA esa: N ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We will observe the Seyfert Galaxy Mrk 205 for absorption due to line_2: hot gas in either the disk or halo of NGC 4319 and our own line_3: Galaxy. The observation will be made using the GHRS with the line_4: G160M grating and the LSA, with the main objective being to cover line_5: the N V doublet that has features at 1239 and 1243 A. We will line_6: center the exposure at 1252 A, so that we can also observe 3 line_7: absorption lines of S II (1250, 1254 and 1259 A), as well as a line_8: blend of Si II and Fe II near 1260 A). This choice for a line_9: wavelength center will also allow for an adequate measurement of line_10: the continuum level below the N V doublet. line_12: Additional lines at random locations may be detected in the line_13: wavelength region we have chosen, since the Lyman-alpha forest line_14: for Mrk 205 extends from 1216 A to 1302 A. ! question: 4 section: 1 line_1: The absorption lines which serve as diagnostics of the presence line_2: and physical conditions of the hot gas (N V, Si IV, and C IV) are line_3: not observable with ground-based telescopes. IUE can not provide line_4: the sensitivity (at high resolution) to make the necessary line_5: observations. Our previous HST observations were required in line_6: order to be able to detect the absorption due to Mg II. ! question: 4 section: 2 line_1: We plan to use the G160M grating on GHRS, with the light entering line_2: through the LSA. All of our observing will be over a single line_3: wavelength interval, but exposures will be separated into small line_4: integrations to avoid smearing due to the GIMP. The flux of Mrk line_5: 205 at 1550 A has been measured by us and another group (Bowen line_6: and Blades) using HST. An average of the two determinations is line_7: 2e-14 erg cm^-2 s^-1 A^-1. On the assumption that the band from line_8: 1235 - 1269 A has the same value, we find from an application of line_9: eq. 4-6 of the GHRS Instrument Handbook that we can expect to line_10: obtain a SNR per diode of 9.5 for a total accumulation of 7872 line_11: seconds worth of integration on the target. (A dark count rate line_12: of 0.012 counts diode^-1 s^-1 was assumed.) This SNR translates line_13: to a 1-sigma error in the equivalent width of a line that is line_14: about 20 mA, assuming N V has the same width as that measured for line_15: C IV by Bowen and Blades. ! question: 5 section: 1 line_1: None, except for dark time acquisition discussed in Question 6 line_2: below. ! question: 6 section: 1 line_1: Our target Mrk 205 is faint enough to require us to perform line_2: acquisition during dark time, so that we avoid complications from line_3: the geocoronal Lyman-alpha background. The magnitudes V = 15.24 line_4: and (B - V) = 0.40 fall below the solid curve labeled N2 in Fig. line_5: 4-2 of the GHRS Instrument Handbook. ! question: 7 section: 1 line_1: The data will be reduced at the Institute for Advanced Study line_2: using STSDAS and software developed for the reduction and line_3: analysis of the Key Project Quasar Absorption Line Survey line_4: (Schneider et al. 1992). ! question: 8 section: 1 line_1: No special requests. ! question: 9 section: 1 line_1: Previous programs for which Jenkins is the PI: line_2: 2344 - High Velocity Lyman Alpha Absorption in the Vela SNR line_3: 2348 - Abundance Enhancements in Halo Gas line_5: Previous programs for which Jenkins is a Co-I: line_6: 2403 - Hot Gas in the Interstellar Medium (Related) line_7: 2347 - Close Spatial Sampling of Shocked Clouds in Vela SNR line_8: 2360 - R-Process Ejecta in the Vela SNR line_10: The Co-Is' (Bahcall, Jannuzi and Schneider) prevously approve line_11: programs are the following: line_12: 1018 - Spectroscopy of a Complete Sample of Bright Nearby Quasars line_13: 1022 - Do Galaxies Produce Quasar Absorption Lines? (related) line_14: 1024 - Do Rich Clusters of Galaxies Produce Quasar Absorption line_15: Lines line_16: 2424 - Quasar Abosrption Line Sujrvey (Key Project)(Related) line_17: 2775 - Non-Proprietary (Snapshot) Survey line_18: 3463 - High Ionized Nitrogen in the Galactic Halo line_19: 3519 - UV Imaging of Nearby Galaxies (Snapshot) line_20: 3648 - Imaging of BL Lac Host Galaxies and Environments line_21: 3981 - Gravitational Lens Candidate 1208+101: Photometry line_22: 3992 - Gravitational lens Candidate 1208+101: Spectroscopy ! question: 9 section: 2 line_1: Our previous HST observations of Mrk~205 (part of GTO1022) led to line_2: the first detection of absorption (Mg II) by the intervining gas line_3: of the galaxy NGC 4319 (Bahcall \etal 1992) and were a prime line_4: motivation for the current proposal. line_6: The initial scientific results of the Key Project Quasar line_7: Absorption Line Survey (GO2424) were reported in Bahcall \etal line_8: (1992). Observations obtained during the first six months of line_9: Cycle~1 determined the number densities at small redshifts of line_10: \Lya\ systems, of C~IV lines and extragalactic halos, of line_11: Lyman-limit systems, of associated absorption systems, and of line_12: damped \Lya\ systems. The number density of C~IV absorbers at line_13: small redshifts was found to be much less than at higher line_14: redshifts. The two-point correlation function of the \Lya\ lines line_15: was computed but the number of lines in the initial sample was line_16: too small to yield a definitive result. Approximately half of line_17: the absorption lines are identified with Galactic interstellar line_18: features. The survey shows that a large fraction of the sky is line_19: covered by high or very high velocity Galactic clouds and that line_20: C~IV is present in the Galactic halo (Savage \etal 1992). ! question: 10 section: 1 line_1: Princeton University provides extensive computing facilities, line_2: free of any capital costs. line_4: IAS will provide computing facilities, line_5: extensive software analysis programs, line_6: an experienced computing staff, and the line_7: salaries for the Co-Is. ! !end of general form text general_form_address: lname: Jenkins fname: Edward mi: B. category: PI inst: Princeton University addr_1: Princeton University Observatory city: Princeton state: NJ zip: 08544 country: USA phone: 609-258-3826 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: MARK205 descr_1: AGN BEHIND NGC4319 descr_2: E,312,H,517 pos_1: RA = 12H 21M 44.1S +/- 0.1S, pos_2: DEC = +75D 18' 38" +/- 1.0" equinox: 2000 pm_or_par: NO rv_or_z: Z=0.070 fluxnum_1: 1 fluxval_1: V = 15.24 +/- 0.2 fluxnum_2: 1 fluxval_2: B-V = 0.40 fluxnum_3: 1 fluxval_3: U-B = -0.94 fluxnum_4: 2 fluxval_4: F(1500) = 2.0 +/- 0.5 E-14 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: MARK205 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 9S fluxnum_1: 1 priority: 1 param_1: SEARCH-SIZE=3 param_2: BRIGHT=RETURN param_3: LOCATE=YES param_4: MAP=DEF req_1: ONBOARD ACQ FOR 2.000; req_2: CYCLE 3; req_3: DARK TIME comment_1: STEP-TIME=1S comment_2: RATE COMPUTED FROM 3C273/10 = 1374 C/S ! linenum: 2.000 targname: MARK205 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1252 num_exp: 24 time_per_exp: 328S s_to_n: 9 s_to_n_time: 7872S fluxnum_1: 2 priority: 1 param_1: STEP-PATT=5, param_2: CENSOR=YES req_1: CYCLE 3 ! ! end of exposure logsheet ! No scan data records found