! File: 4836C.PROP ! Database: PEPDB ! Date: 23-FEB-1994:05:32:51 coverpage: title_1: COMPOSITION OF GAS IN INDIVIDUAL INTERSTELLAR CLOUDS: title_2: CYCLE 3 MEDIUM PRIORITY OBSERVATIONS sci_cat: INTERSTELLAR MEDIUM sci_subcat: ABSORPTION LINES proposal_for: GO/DD 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: 7.06 num_pri: 2 hrs: Y pi_position: PROFESSOR EMERITUS ! end of coverpage abstract: line_1: Column densities of interstellar atoms of 17 atomic species of 10 line_2: elements will be measured in the line-of-sight to 2 early-type stars in line_3: the galactic disk, using the Goddard High Resolution Spectrograph to line_4: obtain precise measures in the ultraviolet with the highest available line_5: spectral resolution. These data will be analyzed to determine relative line_6: abundances in the several individual clouds present along each line of line_7: sight, and thus to determine how the composition of the gas in such line_8: clouds and the various physical processes occurring vary with cloud line_9: parameters such as H column density, velocity, ionization level, and line_10: distance z from the galactic plane. This information should help to line_11: clarify the many physical processes occurring in interstellar gas. line_12: The program should also increase our understanding of the balance line_13: 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. title: PROF. mi: R. inst: RICE UNIVERSITY country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: The observations of two stars planned during Cycle 3, supported line_2: with GO/DD time, will follow the pattern set in general for our line_3: ongoing GTO program (ID#1071), and more specifically the detailed line_4: observing program set for our one star observed in Cycle 1 (under line_5: ID#3215). A series of interstellar absorption lines longward line_6: of 1800 A will be observed with Echelle B of the GHRS, giving the line_7: highest resolution available (resolving power R about 85,000) for line_8: lines of S I, Si II, Mg I, Fe II, Co II, Cr II, Zn II, and Mn II. line_9: For photometric accuracy, the WSCAN mode will be used to give three line_10: adjacent exposures of each line. Another series of lines at shorter line_11: wavelengths, between 1120 and 1600 A, will be observed with the GHRS line_12: grating G160M, using the FP-SPLIT routine to obtain subexposures at line_13: four adjacent wavelengths. Of the many interstellar lines in this line_14: region the following species are of particular interest: C I, C II, line_15: C IV, N I, N V, O I, Mg II, S II, S III, Si II, Si III, Si IV, P II, line_16: P III, Fe II, and Mn II. While the resolving power with this grating line_17: is in the range from about 15,000 to 24,000, deconvolution of each line_18: spectrum may almost double the effective R. For accurate wavelength line_19: calibration, exposures of the calibration lamp spectrum will be taken line_20: at the beginning and end of each series. ! 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 Echelle B, line_13: can answer detailed questions on the physical properties of individual line_14: 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 1 has been obtained. The STSDAS software (running as line_3: part of the IRAF system) and the IDL language have both been implemented line_4: on the SPARCstation. line_6: As part of the data processing, corrections will be made for a variety line_7: of effects, including scattered light, fixed pattern noise, and shift line_8: of wavelength calibration with temperature. Data analysis will line_9: determine for each line the function Nr(v), the apparent column density line_10: of species r per unit velocity interval, as a function of Doppler-shift line_11: velocity v. Comparison of Nr(v) between lines of different f-values line_12: but with the same lower state yields a correction of these values for line_13: saturation, if the corrections are not large. ! question: 8 section: 1 line_1: No additional comments or requests. ! question: 9 section: 1 line_1: PREVIOUS HST PROGRAMS: GTO 1071, 3215, and AUG 3444 "Composition line_2: of Gas in Individual Interstellar Clouds". These identification numbers, line_3: for observations in Cycles 0, 1, and 2, designate the ongoing GTO1071 line_4: project for which the present proposal represents observations on line_5: GO/DD time during Cycles 3. line_7: MAIN RESULTS OBTAINED FROM PREVIOUS RELATED PROGRAMS: Two stars, HD line_8: 68273 (Gamma-2 Velorum) and HD 93521, were observed for the program line_9: GTO 1071 during Cycle 0. Analysis of these data has yielded a line_10: new strategy for removing the effects of scattered light from GHRS line_11: echelle data and a very effective technique for correcting for fixed line_12: pattern noise in the data, an effect important for the brighter stars line_13: for which S/N can be about 100 or more. In the halo star HD93521, line_14: 1500 pc from the galactic plane, the observed widths of the line_15: C IV and Si IV absorption features are 50 km/sec (FWHM), as compared line_16: with 7 km/sec for a narrow S II component. Measures of the line_17: low-ionization lines (such as S II, Si II, Fe II) have given detailed line_18: information on the depletion of elements from the gas as a result line_19: of condensation on solid grains, and suggest that iron orthosilicate line_20: is a primary constituent of these grains. The temperature and density line_21: of the interstellar gas have also been determined. ! question: 9 section: 2 line_1: PUBLICATIONS RESULTING FROM THE ABOVE DATA: A brief description of line_2: these data and of their technical aspects has appeared in the STScI line_3: Newsletter, June 1991 (Vol. 8, No. 2). The observed profiles of the line_4: C IV and Si IV features in HD93521 are presented in Ap.J. Letters line_5: (May 10, 1992), and their possible interpretation discusssed. A full line_6: discussion of the HD 93521 results is scheduled to appear in the Ap.J. line_7: (May 20, 1993). ! 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 line_6: Department of Astrophysical Sciences contributed funds toward his line_7: salary during several years before full NASA funding (by subcontract line_8: with O'Dell's home institution, the Rice University of Technology) line_9: became available. Computer peripherals, including tape drives and a line_10: laser printer, are available at the Department for a small monthly line_11: 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: 19 name_1: HD118716 name_2: EPSILON-CEN descr_1: A,113,G,508,912 pos_1: RA=13H36M42.34S +/- .1S, pos_2: DEC=-53D12'46.6" +/- 1.0" equinox: 1950 pm_or_par: NO comment_1: SPECTRAL TYPE B1 III fluxnum_1: 1 fluxval_1: V=2.30,E(B-V)=0.04 fluxnum_2: 2 fluxval_2: F-CONT(1300)=2.1+/-0.2E-8 ! targnum: 24 name_1: HD151890 name_2: MU-1-SCO descr_1: A,110,G,508,912 pos_1: RA=16H48M28.69S +/- .1S, pos_2: DEC=-37D57'49.0" +/- 1.0" equinox: 1950 pm_or_par: NO acqpr_1: COMP comment_1: SPECTRAL TYPE B1.5 IV fluxnum_1: 1 fluxval_1: V=3.00,E(B-V)=0.05 fluxnum_2: 2 fluxval_2: F-CONT(1300)=8.9+/-0.9E-9 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 sequence_1: DEFINE sequence_2: D-1A targname: # config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1148.0 num_exp: 2 time_per_exp: 308S s_to_n: # fluxnum_1: 2 priority: # param_1: STEP-PATT=5, param_2: COMB=TWO, param_3: FP-SPLIT=DSFOUR req_1: SEQ 1-7 NO GAP comment_1: EXPOSURE TIME IN LINE 1 YIELDS S/N comment_2: =43 PER 3 KM/S BIN PER SUBEXPOSURE comment_3: FOR A STANDARD STAR WITH F-CONT(1300) comment_4: =1.0E-8 USING MEASURED HST SENSITIVITY ! linenum: 2.000 sequence_1: DEFINE sequence_2: D-1A targname: # config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1195.0 num_exp: 1 time_per_exp: 287S s_to_n: # fluxnum_1: 2 priority: # param_1: STEP-PATT=5, param_2: COMB=TWO, param_3: FP-SPLIT=DSFOUR comment_1: EXPOSURE TIMES IN LINES 2-7 YIELD S/N comment_2: =87 PER 3 KM/S BIN PER SUBEXPOSURE comment_3: FOR A STANDARD STAR WITH F-CONT(1300) comment_4: =1.0E-8 USING MEASURED HST SENSITIVITY ! linenum: 3.000 sequence_1: DEFINE sequence_2: D-1A targname: # config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1252.0 num_exp: 1 time_per_exp: 134S s_to_n: # fluxnum_1: 2 priority: # param_1: STEP-PATT=5, param_2: COMB=TWO, param_3: FP-SPLIT=DSFOUR ! linenum: 4.000 sequence_1: DEFINE sequence_2: D-1A targname: # config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1315.6 num_exp: 1 time_per_exp: 110S s_to_n: # fluxnum_1: 2 priority: # param_1: STEP-PATT=5, param_2: COMB=TWO, param_3: FP-SPLIT=DSFOUR ! linenum: 5.000 sequence_1: DEFINE sequence_2: D-1A targname: # config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1347.0 num_exp: 1 time_per_exp: 129S s_to_n: # fluxnum_1: 2 priority: # param_1: STEP-PATT=5, param_2: COMB=TWO, param_3: FP-SPLIT=DSFOUR ! linenum: 6.000 sequence_1: DEFINE sequence_2: D-1A targname: # config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1392.0 num_exp: 1 time_per_exp: 164S s_to_n: # fluxnum_1: 2 priority: # param_1: STEP-PATT=5, param_2: COMB=TWO, param_3: FP-SPLIT=DSFOUR ! linenum: 7.000 sequence_1: DEFINE sequence_2: D-1A targname: # config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1560.0 num_exp: 1 time_per_exp: 233S s_to_n: # fluxnum_1: 2 priority: # param_1: STEP-PATT=5, param_2: COMB=TWO, param_3: FP-SPLIT=DSFOUR ! linenum: 8.000 sequence_1: DEFINE sequence_2: BR-3B targname: # config: HRS opmode: WSCAN aperture: 0.25 sp_element: ECH-B wavelength: 1804.92-1807.08 num_exp: 1 time_per_exp: 186S s_to_n: # fluxnum_1: 2 priority: # param_1: STEP-PATT=7, param_2: COMB=TWO, param_3: WAVE-STEP=0.72 req_1: SEQ 8-14 NO GAP comment_1: "WAVE-STEP" IN COLUMN 9 OF LINE 8 IS comment_2: EQUIVALENT TO 8 CARROUSEL STEPS. comment_3: EXPOSURE TIMES IN LINES 8-14 YIELD S/N comment_4: =100 PER 3 KM/S BIN PER SUBEXPOSURE comment_5: FOR A STANDARD STAR WITH F-CONT(1300) comment_6: =1.0E-8 USING MEASURED HST SENSITIVITY ! linenum: 9.000 sequence_1: DEFINE sequence_2: BR-3B targname: # config: HRS opmode: WSCAN aperture: 0.25 sp_element: ECH-B wavelength: 1825.95-1828.05 num_exp: 1 time_per_exp: 186S s_to_n: # fluxnum_1: 2 priority: # param_1: STEP-PATT=7, param_2: COMB=TWO, param_3: WAVE-STEP=0.70 comment_1: "WAVE-STEP" IN COLUMN 9 OF LINE 9 comment_2: IS EQUIVALENT TO 8 CARROUSEL STEPS. ! linenum: 10.000 sequence_1: DEFINE sequence_2: BR-3B targname: # config: HRS opmode: WSCAN aperture: 0.25 sp_element: ECH-B wavelength: 2024.51-2026.79 num_exp: 1 time_per_exp: 82S s_to_n: # fluxnum_1: 2 priority: # param_1: STEP-PATT=7, param_2: COMB=TWO, param_3: WAVE-STEP=0.76 comment_1: "WAVE-STEP" IN COLUMN 9 OF LINE 10 comment_2: IS EQUIVALENT TO 8 CARROUSEL STEPS. comment_3: VACUUM WAVELENGTHS USED IN LINE 10. ! linenum: 11.000 sequence_1: DEFINE sequence_2: BR-3B targname: # config: HRS opmode: WSCAN aperture: 0.25 sp_element: ECH-B wavelength: 2058.21-2060.79 num_exp: 1 time_per_exp: 90S s_to_n: # fluxnum_1: 2 priority: # param_1: STEP-PATT=7, param_2: COMB=TWO, param_3: WAVE-STEP=0.86 comment_1: "WAVE-STEP" IN COLUMN 9 OF LINE 11 comment_2: IS EQUIVALENT TO 8 CARROUSEL STEPS. comment_3: VACUUM WAVELENGTHS USED IN LINE 11. ! linenum: 12.000 sequence_1: DEFINE sequence_2: BR-3B targname: # config: HRS opmode: WSCAN aperture: 0.25 sp_element: ECH-B wavelength: 2259.49-2262.10 num_exp: 1 time_per_exp: 82S s_to_n: # fluxnum_1: 2 priority: # param_1: STEP-PATT=7, param_2: COMB=TWO, param_3: WAVE-STEP=0.87 comment_1: "WAVE-STEP" IN COLUMN 9 OF LINE 12 comment_2: IS EQUIVALENT TO 8 CARROUSEL STEPS. comment_3: VACUUM WAVELENGTHS USED IN LINE 12. ! linenum: 13.000 sequence_1: DEFINE sequence_2: BR-3B targname: # config: HRS opmode: WSCAN aperture: 0.25 sp_element: ECH-B wavelength: 2370.71-2373.35 num_exp: 1 time_per_exp: 82S s_to_n: # fluxnum_1: 2 priority: # param_1: STEP-PATT=7, param_2: COMB=TWO, param_3: WAVE-STEP=0.88 comment_1: "WAVE-STEP" IN COLUMN 9 OF LINE 13 comment_2: IS EQUIVALENT TO 8 CARROUSEL STEPS. comment_3: VACUUM WAVELENGTHS USED IN LINE 13. ! linenum: 14.000 sequence_1: DEFINE sequence_2: BR-3B targname: # config: HRS opmode: WSCAN aperture: 0.25 sp_element: ECH-B wavelength: 2601.88-2604.67 num_exp: 1 time_per_exp: 105S s_to_n: # fluxnum_1: 2 priority: # param_1: STEP-PATT=7, param_2: COMB=TWO, param_3: WAVE-STEP=0.93 comment_1: "WAVE-STEP" IN COLUMN 9 OF LINE 14 comment_2: IS EQUIVALENT TO 8 CARROUSEL STEPS. comment_3: VACUUM WAVELENGTHS USED IN LINE 14. ! linenum: 301.000 targname: HD151890 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-A2 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 302; req_2: CYCLE 3 / 301-316 comment_1: STEP-TIME=0.2 SEC. ! linenum: 302.000 targname: HD151890 config: HRS opmode: ACQ/PEAKUP aperture: 0.25 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 15.0S priority: 1 req_1: ONBOARD ACQUISITION FOR 303-308 comment_1: STEP-TIME=0.6 SEC. ! linenum: 303.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1190.5 num_exp: 1 time_per_exp: 60S priority: 1 param_1: STEP-PATT=5, param_2: COMB=TWO req_1: SEQ 303-305 NO GAP; req_2: CALIB FOR 304 ! linenum: 304.000 sequence_1: USE sequence_2: D-1A targname: HD151890 time_per_exp: X1.12 s_to_n: 87 priority: 1 comment_1: THE MULTIPLICATIVE FACTOR 1.12 FOR ALL comment_2: D-1A EXPOSURES FOR THIS STAR HAS BEEN comment_3: CALCULATED TO GIVE S/N=87 PER 3 KM/S comment_4: BIN PER SUBEXPOSURE FOR MOST SPECTRAL comment_5: FEATURES, USING THE HRS SENSITIVITY AS comment_6: MEASURED IN CYCLE 0. ! linenum: 305.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1560.0 num_exp: 1 time_per_exp: 60S priority: 1 param_1: STEP-PATT=5, param_2: COMB=TWO req_1: CALIB FOR 304 ! linenum: 306.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B wavelength: 1805.28 num_exp: 1 time_per_exp: 13.6S priority: 1 param_1: STEP-PATT=7, param_2: COMB=TWO req_1: SEQ 306-308 NO GAP; req_2: CALIB FOR 307 ! linenum: 307.000 sequence_1: USE sequence_2: BR-3B targname: HD151890 time_per_exp: X1.12 s_to_n: 100 priority: 1 comment_1: THE MULTIPLICATIVE FACTOR 1.12 FOR ALL comment_2: BR-3B EXPOSURES FOR THIS STAR HAS BEEN comment_3: CALCULATED TO GIVE S/N=100 PER 3 KM/S comment_4: BIN PER SUBEXPOSURE, USING THE HRS comment_5: SENSITIVITY AS MEASURED IN CYCLE 0. ! linenum: 308.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B wavelength: 2604.81 num_exp: 1 time_per_exp: 13.6S priority: 1 param_1: STEP-PATT=7, param_2: COMB=TWO req_1: CALIB FOR 307 ! linenum: 309.000 targname: HD118716 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-A2 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 310 comment_1: STEP-TIME=0.2 SEC. ! linenum: 310.000 targname: HD118716 config: HRS opmode: ACQ/PEAKUP aperture: 0.25 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 15.0S priority: 1 req_1: ONBOARD ACQUISITION FOR 311-316 comment_1: STEP-TIME=0.6 SEC ! linenum: 311.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1190.5 num_exp: 1 time_per_exp: 60S priority: 1 param_1: STEP-PATT=5, param_2: COMB=TWO req_1: SEQ 311-313 NO GAP; req_2: CALIB FOR 312 ! linenum: 312.000 sequence_1: USE sequence_2: D-1A targname: HD118716 time_per_exp: X0.50 s_to_n: 87 priority: 1 comment_1: THE MULTIPLICATIVE FACTOR 0.50 FOR ALL comment_2: D-1A EXPOSURES FOR THIS STAR HAS BEEN comment_3: CALCULATED TO GIVE S/N=87 PER 3 KM/S comment_4: BIN PER SUBEXPOSURE FOR MOST SPECTRAL comment_5: FEATURES, USING THE HRS SENSITIVITY AS comment_6: MEASURED IN CYCLE 0. ! linenum: 313.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1560.0 num_exp: 1 time_per_exp: 60S priority: 1 param_1: STEP-PATT=5, param_2: COMB=TWO req_1: CALIB FOR 312 ! linenum: 314.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B wavelength: 1805.28 num_exp: 1 time_per_exp: 13.6S priority: 1 param_1: STEP-PATT=7, param_2: COMB=TWO req_1: SEQ 314-316 NO GAP; req_2: CALIB FOR 315 ! linenum: 315.000 sequence_1: USE sequence_2: BR-3B targname: HD118716 time_per_exp: X0.50 s_to_n: 100 priority: 1 comment_1: THE MULTIPLICATIVE FACTOR 0.50 FOR ALL comment_2: BR-3B EXPOSURES FOR THIS STAR HAS BEEN comment_3: CALCULATED TO GIVE S/N=100 PER 3 KM/S comment_4: BIN PER SUBEXPOSURE USING THE HRS comment_5: SENSITIVITY AS MEASURED IN CYCLE 0. ! linenum: 316.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B wavelength: 2604.81 num_exp: 1 time_per_exp: 13.6S priority: 1 param_1: STEP-PATT=7, param_2: COMB=TWO req_1: CALIB FOR 315 ! ! end of exposure logsheet ! No scan data records found