! Carryover Augmentation Observations ! Proposal ID 5720 coverpage: title_1: COMPOSITION OF GAS IN INDIVIDUAL INTERSTELLAR CLOUDS: title_2: CYCLE 4 CARRYOVER OBSERVATIONS sci_cat: INTERSTELLAR MEDIUM sci_subcat: ABSORPTION LINES proposal_for: AUG/OS cont_id: 3444 pi_title: PROF. pi_fname: LYMAN pi_lname: SPITZER pi_inst: PRINCETON UNIVERSITY pi_country: USA pi_phone: (609) 258-3809 keywords_1: INTERSTELLAR LINES hours_pri: 4.81 num_pri: 1 hrs: Y pi_position: PROFESSOR EMERITUS ! end of coverpage abstract: line_1: Column densities of some ten elements in various stages of ionization line_2: will be measured in the lines of sight to a number of stars, some in line_3: the Galactic disk and some in the halo. The Goddard High Resolution line_4: Spectrograph will be used with the highest available spectral line_5: resolution to make precise measurements on individual clouds. These line_6: data will be analyzed to determine relative abundances in the several line_7: clouds present along each line of sight, and thus to determine how the line_8: composition of the gas in such clouds and the various physical line_9: processes occurring vary with cloud parameters such as H column line_10: density, velocity, ionization level, and distance z from the Galactic line_11: plane. This information should help to clarify the many physical line_12: processes occurring in interstellar gas. In particular, measures of line_13: stars in the Galactic halo should help to identify the mechanisms line_14: responsible for the abundant C IV, Si IV, and N V known to be present line_15: in the interstellar gas at kiloparsec distances from the galactic line_16: plane. The program should also increase our understanding of the line_17: balance between formation and destruction of interstellar dust grains. ! end of abstract general_form_proposers: lname: SPITZER fname: LYMAN title: PROF. inst: PRINCETON UNIVERSITY country: USA ! lname: O'DELL fname: C. mi: R. title: PROF. inst: RICE UNIVERSITY country: USA ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: The Cycle 4 carry-over observations of this one halo star will line_2: supplement the data previously obtained for this star with GHRS Echelle line_3: B. Observations will be made with Echelle A at a number of wavelengths line_4: between 1190 and 1570 A, giving a resolving power of about 85,000 for line_5: lines of C I, II, and IV, N V, O I, Mg II, S II and III, Si II and IV, line_6: and P II and III. For photometric accuracy, the FP-SPLIT routine will line_7: be used to obtain four subexposures at adjacent wavelengths. Exposures line_8: of the wavelength calibration spectrum will be taken at the beginning line_9: and end of this series of exposures. ! question: 4 section: 1 line_1: Much pioneering work on individual interstellar clouds has been done line_2: from the ground. However, to obtain data on many elements, including line_3: the highly ionized species, requires observations from above the line_4: atmosphere. The Copernicus satellite made important contributions to line_5: this topic, but its resolving power of 20,000 was insufficient to line_6: resolve clearly many of the individual components in most lines of line_7: sight, although in favorable cases properties of individual clouds were line_8: successfully deduced. The IUE satellite has been enormously useful for line_9: broad surveys of interstellar absorption, especially for the fainter line_10: stars which could not be observed with Copernicus, but its resolving line_11: power of 10,000 is inadequate for resolving most components. The HST, line_12: with its resolving power of 85,000 for lines observed with the echelle line_13: gratings, can answer detailed questions on the physical properties of line_14: individual clouds towards many stars. ! question: 5 section: 1 line_1: There are no Realtime Data or Special Scheduling Requests required. ! question: 6 section: 1 line_1: There are no Special Calibrations required. ! question: 7 section: 1 line_1: To analyze the HST/GHRS data for this ongoing project, a dedicated Sun line_2: SPARCstation 10 has been obtained. This facility should be entirely line_3: adequate for the processing and analysis of all the data. The STSDAS line_4: software (running as part of the IRAF system) and the GHRSDAF software line_5: (written in the IDL language) have both been implemented on the line_6: SPARCstation. line_7: line_8: As part of the data processing, corrections will be made for a variety line_9: of effects, including scattered light, fixed pattern noise, and shift line_10: of wavelength calibration with temperature. Data analysis for this star line_11: will determine the minimum number of components required to fit the line_12: observed absorption profiles. Each component will be assumed to have a line_13: Gaussian intrinsic absorption profile, with some mean radial velocity line_14: and velocity dispersion, the same for all atomic species, and a column line_15: density different for each species; these quantities will be found line_16: from least squares solutions. ! question: 8 section: 1 line_1: No additional comments or requests. ! question: 9 section: 1 line_1: PREVIOUS HST PROGRAMS line_2: GTO 1071, 3215, 3444, and 4835 for cycles 0-3. line_3: line_4: MAIN RESULTS OBTAINED FROM PREVIOUS RELATED PROGRAMS line_5: Three stars have been fully analyzed in this program. The column line_6: densities obtained for some two dozen components have shown line_7: approximately how the amount of gas ``locked up'' in small particles, line_8: or grains, varies from one interstellar cloud to another, depending on line_9: the temperature, density, and mean velocity of the cloud. Ratios of line_10: certain column densities yield values of the electron density, which line_11: are unexpectedly high, suggesting that some unexpected physical process line_12: ionizes interstellar hydrogen. The column density ratios between the line_13: highly ionized atoms suggest that different processes in the disk and line_14: halo ionize these atoms. question: 9 section: 2 line_1: PUBLICATIONS RESULTING FROM THE ABOVE DATA line_2: line_3: Ap.J., 391, L41, 1992 on highly ionized atoms towards HD 93521 (halo) line_4: Ap.J., 409, 299, 1993 on composition of clouds towards HD 93521 (halo) line_5: Ap.J., 427, 232, 1994 on interstellar clouds towards HD 68273 (disk) line_6: line_7: In addition, a similar paper on HD 149881 (halo) will be submitted line_8: shortly. ! question: 10 section: 1 line_1: The participation of L. Spitzer, now Senior Research Astronomer at line_2: Princeton University, is without charge to the Project; he expects to line_3: devote nearly all his research time to this work. The chief annual line_4: cost to the Project is the full-time salary of E.L. Fitzpatrick, line_5: now Research Astronomer with Continuing Appointment. The Department line_6: of Astrophysical Sciences contributed funds toward his salary during line_7: several years before full NASA funding (by subcontract with O'Dell's line_8: home institution, the Rice University of Technology) became available. line_9: Computer peripherals, including tape drives and a laser printer, are line_10: available at the Department for a small monthly charge. ! end of general form text general_form_address: lname: SPITZER fname: LYMAN title: PROF. category: PI inst: PRINCETON UNIV. OBSERVATORY addr_1: PEYTON HALL city: PRINCETON state: NJ zip: 08544 country: USA phone: 609-258-3809 ! lname: O'DELL fname: C. mi: R. title: PROF. inst: RICE UNIVERSITY addr_1: DEPT. OF SPACE PHYSICS & ASTRONOMY addr_2: P.O. BOX 1892 city: HOUSTON state: TX zip: 77251 country: USA phone: 713-527-8101 X3633 telex: 556457 ! end of general_form_address records fixed_targets: targnum: 4 name_1: HD215733 name_2: BD16D4814 name_3: GSC00768 descr_1: A,113,G,508,911 pos_1: PLATE-ID=00GO, pos_2: RA = 22H 47M 02.5S +/- 0.1", pos_3: DEC = 17D 13' 59.1" +/- 0.1", equinox: J2000 pm_or_par: NO fluxnum_1: 1 fluxval_1: V=7.32,E(B-V)=0.10 fluxnum_2: 2 fluxval_2: F-CONT(1300)=1.2+/-0.2E-10 comment_1: SPECTRAL TYPE B1 II ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: ! linenum: 1.000 sequence_1: DEFINE sequence_2: EC-A4 targname: # config: HRS opmode: ACCUM aperture: 0.25 sp_element: ECH-A wavelength: 1192.53 num_exp: 2 time_per_exp: 103S s_to_n: # fluxnum_1: 2 priority: # param_1: STEP-PATT=6, param_2: COMB=TWO, param_3: FP-SPLIT=DSFOUR req_1: SEQ 1-9 NO GAP comment_1: EXPOSURE TIME IN LINE 1 GIVES S/N=71 comment_2: PER DIODE FOR EACH OF 8 SUBEXPOSURES comment_3: FOR A STANDARD STAR WITH F-CONT(1300) comment_4: =1.0E-8 AND POST-COSTAR SENSITIVITY ! linenum: 2.000 sequence_1: DEFINE sequence_2: EC-A4 targname: # config: HRS opmode: ACCUM aperture: 0.25 sp_element: ECH-A wavelength: 1241.00 num_exp: 1 time_per_exp: 131S s_to_n: # fluxnum_1: 2 priority: # param_1: STEP-PATT=6, param_2: COMB=TWO, param_3: FP-SPLIT=DSFOUR comment_1: EXPOSURE TIME IN LINE 2 GIVES S/N=100 comment_2: PER DIODE FOR EACH OF 4 SUBEXPOSURES comment_3: FOR A STANDARD STAR WITH F-CONT(1300) comment_4: =1.0E-8 AND POST-COSTAR SENSITIVITY ! linenum: 3.000 sequence_1: DEFINE sequence_2: EC-A4 targname: # config: HRS opmode: ACCUM aperture: 0.25 sp_element: ECH-A wavelength: 1252.39 num_exp: 1 time_per_exp: 95S s_to_n: # fluxnum_1: 2 priority: # param_1: STEP-PATT=6, param_2: COMB=TWO, param_3: FP-SPLIT=DSFOUR comment_1: EXPOSURE TIME IN LINE 3 GIVES S/N=100 comment_2: PER DIODE FOR EACH OF 4 SUBEXPOSURES comment_3: FOR A STANDARD STAR WITH F-CONT(1300) comment_4: =1.0E-8 AND POST-COSTAR SENSITIVITY ! linenum: 4.000 sequence_1: DEFINE sequence_2: EC-A4 targname: # config: HRS opmode: ACCUM aperture: 0.25 sp_element: ECH-A wavelength: 1262.22 num_exp: 1 time_per_exp: 131S s_to_n: # fluxnum_1: 2 priority: # param_1: STEP-PATT=6, param_2: COMB=TWO, param_3: FP-SPLIT=DSFOUR comment_1: EXPOSURE TIME IN LINE 4 GIVES S/N=100 comment_2: PER DIODE FOR EACH OF 4 SUBEXPOSURES comment_3: FOR A STANDARD STAR WITH F-CONT(1300) comment_4: =1.0E-8 AND POST-COSTAR SENSITIVITY. comment_5: (ORDER 45 HAS HIGHEST SENSITIVITY) ! linenum: 5.000 sequence_1: DEFINE sequence_2: EC-A4 targname: # config: HRS opmode: ACCUM aperture: 0.25 sp_element: ECH-A wavelength: 1304.15 num_exp: 1 time_per_exp: 75S s_to_n: # fluxnum_1: 2 priority: # param_1: STEP-PATT=6, param_2: COMB=TWO, param_3: FP-SPLIT=DSFOUR comment_1: EXPOSURE TIME IN LINE 5 GIVES S/N=100 comment_2: PER DIODE FOR EACH OF 4 SUBEXPOSURES comment_3: FOR A STANDARD STAR WITH F-CONT(1300) comment_4: =1.0E-8 AND POST-COSTAR SENSITIVITY ! linenum: 6.000 sequence_1: DEFINE sequence_2: EC-A4 targname: # config: HRS opmode: ACCUM aperture: 0.25 sp_element: ECH-A wavelength: 1335.32 num_exp: 1 time_per_exp: 76S s_to_n: # fluxnum_1: 2 priority: # param_1: STEP-PATT=6, param_2: COMB=TWO, param_3: FP-SPLIT=DSFOUR comment_1: EXPOSURE TIME IN LINE 6 GIVES S/N=100 comment_2: PER DIODE FOR EACH OF 4 SUBEXPOSURES comment_3: FOR A STANDARD STAR WITH F-CONT(1300) comment_4: =1.0E-8 AND POST-COSTAR SENSITIVITY ! linenum: 7.000 sequence_1: DEFINE sequence_2: EC-A4 targname: # config: HRS opmode: ACCUM aperture: 0.25 sp_element: ECH-A wavelength: 1393.96 num_exp: 1 time_per_exp: 124S s_to_n: # fluxnum_1: 2 priority: # param_1: STEP-PATT=6, param_2: COMB=TWO, param_3: FP-SPLIT=DSFOUR comment_1: EXPOSURE TIME IN LINE 7 GIVES S/N=100 comment_2: PER DIODE FOR EACH OF 4 SUBEXPOSURES comment_3: FOR A STANDARD STAR WITH F-CONT(1300) comment_4: =1.0E-8 AND POST-COSTAR SENSITIVITY ! linenum: 8.000 sequence_1: DEFINE sequence_2: EC-A4 targname: # config: HRS opmode: ACCUM aperture: 0.25 sp_element: ECH-A wavelength: 1549.72 num_exp: 2 time_per_exp: 127S s_to_n: # fluxnum_1: 2 priority: # param_1: STEP-PATT=6, param_2: COMB=TWO, param_3: FP-SPLIT=DSFOUR comment_1: EXPOSURE TIME IN LINE 8 GIVES S/N=71 comment_2: PER DIODE FOR EACH OF 8 SUBEXPOSURES comment_3: FOR A STANDARD STAR WITH F-CONT(1300) comment_4: =1.0E-8 AND POST-COSTAR SENSITIVITY ! linenum: 9.000 sequence_1: DEFINE sequence_2: EC-A4 targname: # config: HRS opmode: ACCUM aperture: 0.25 sp_element: ECH-A wavelength: 1561.11 num_exp: 2 time_per_exp: 114S s_to_n: # fluxnum_1: 2 priority: # param_1: STEP-PATT=6, param_2: COMB=TWO, param_3: FP-SPLIT=DSFOUR comment_1: EXPOSURE TIME IN LINE 9 GIVES S/N=71 comment_2: PER DIODE FOR EACH OF 8 SUBEXPOSURES comment_3: FOR A STANDARD STAR WITH F-CONT(1300) comment_4: =1.0E-8 AND POST-COSTAR SENSITIVITY ! linenum: 201.000 targname: HD215733 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N1 num_exp: 1 time_per_exp: 1.8S priority: 1 param_1: BRIGHT=RETURN param_2: SEARCH-SIZE=3, param_3: LOCATE=YES, req_1: ONBOARD ACQUISITION FOR 202; req_2: CYCLE 4 / 201-204 comment_1: STEP-TIME = 0.2 SEC ! linenum: 202.000 targname: HD215733 config: HRS opmode: ACQ/PEAKUP aperture: 0.25 sp_element: MIRROR-N1 num_exp: 1 time_per_exp: 5.0S priority: 1 param_1: SEARCH-SIZE=5, req_1: ONBOARD ACQUISITION FOR 203-204 ! linenum: 203.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-A wavelength: 1192.35 num_exp: 1 time_per_exp: 60S priority: 1 param_1: STEP-PATT=DEF, param_2: COMB=TWO req_1: SEQ 203-204 NO GAP; req_2: CALIB FOR 204 ! linenum: 204.000 sequence_1: USE sequence_2: EC-A4 targname: HD215733 time_per_exp: X6.6 s_to_n: 26 priority: 1 comment_1: THE MULTIPLICATIVE FACTOR 6.6 FOR ALL comment_2: EC-A4 EXPOSURES FOR THIS STAR HAS BEEN comment_3: CALCULATED TO GIVE S/N=26 PER DIODE comment_4: PER SUBEXPOSURE FOR MOST SPECTRAL comment_5: FEATURES, USING ESTIMATED POST-COSTAR comment_6: HRS SENSITIVITY linenum: 206.000 targname: HD215733 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N1 num_exp: 1 time_per_exp: 1.8S priority: 1 param_1: BRIGHT=RETURN param_2: SEARCH-SIZE=3, param_3: LOCATE=YES, req_1: ONBOARD ACQUISITION FOR 207; req_2: CYCLE 4 / 206-209 comment_1: STEP-TIME = 0.2 SEC ! linenum: 207.000 targname: HD215733 config: HRS opmode: ACQ/PEAKUP aperture: 0.25 sp_element: MIRROR-N1 num_exp: 1 time_per_exp: 5.0S priority: 1 param_1: SEARCH-SIZE=5, req_1: ONBOARD ACQUISITION FOR 208-209 linenum: 208.000 targname: HD215733 config: HRS opmode: ACCUM aperture: 0.25 sp_element: ECH-A wavelength: 1241.00 num_exp: 1 time_per_exp: 864.6S s_to_n: 26 fluxnum_1: 2 priority: 1 param_1: STEP-PATT=6, param_2: COMB=TWO, param_3: FP-SPLIT=DSFOUR comment_1: EXPOSURE TIME IN 208 GIVES S/N=100 comment_2: PER DIODE FOR EACH OF 4 SUBEXPOSURES comment_3: FOR A STANDARD STAR WITH F-CONT(1300) comment_4: =1.0E-8 AND POST-COSTAR SENSITIVITY linenum: 209.000 targname: HD215733 config: HRS opmode: ACCUM aperture: 0.25 sp_element: ECH-A wavelength: 1561.11 num_exp: 2 time_per_exp: 752.4S s_to_n: 26 fluxnum_1: 2 priority: 1 param_1: STEP-PATT=6, param_2: COMB=TWO, param_3: FP-SPLIT=DSFOUR comment_1: EXPOSURE TIME IN LINE 9 GIVES S/N=71 comment_2: PER DIODE FOR EACH OF 8 SUBEXPOSURES comment_3: FOR A STANDARD STAR WITH F-CONT(1300) comment_4: =1.0E-8 AND POST-COSTAR SENSITIVITY ! end of exposure logsheet ! No scan data records found