! File: 1071C.PROP ! Database: PEPDB ! Date: 16-FEB-1994:00:37:08 coverpage: title_1: COMPOSITION OF GAS IN INDIVIDUAL INTERSTELLAR CLOUDS -- CYCLE 0 sci_cat: INTERSTELLAR MEDIUM sci_subcat: ABSORPTION LINES proposal_for: GTO/OS pi_title: PROF. pi_fname: C. pi_mi: R. pi_lname: O'DELL pi_inst: RICE UNIVERSITY pi_country: USA pi_phone: 713-527-8101 EX3633 keywords_1: INTERSTELLAR LINES hours_pri: 20.00 num_pri: 27 hrs: X pi_position: PROF. SP.PHYS.ASTR. ! end of coverpage abstract: line_1: Column densities of interstellar atoms of some ten atomic species will be line_2: measured in the line of sight to 27 early-type stars, using the High-Resolution line_3: Spectrograph to obtain precise measures in the ultraviolet with highest line_4: spectral resolution. These data will be analyzed to determine relative line_5: abundances in the several individual clouds present along each line of sight, line_6: and thus to determine how the composition of the gas in such clouds varies with line_7: cloud parameters such as H column density, velocity, ionization level and line_8: distance z from the galactic plane. This information should help to clarify the line_9: equilibrium between gas and grains,--i.e., how the gas condenses on the grains line_10: and how the grains are destroyed by a variety of phenomena occurring in line_11: interstellar clouds. ! ! end of abstract general_form_proposers: lname: O'DELL fname: C. mi: R. inst: RICE UNIVERSITY country: USA ! lname: SPITZER JR. fname: LYMAN inst: PRINCETON UNIVERSITY country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: For each of 27 stars a series of interstellar absorption lines will be line_2: observed, using the Echelle mode of the High Resolution spectrograph in the line_3: Accumulation mode. For the brighter stars measures will be made for each line line_4: with the spectrum moved parallel to the dispersion to two different positions line_5: on the photocathode, to help correct for cathode non-uniformities. In line_6: addition, the scattered light will be measured on each side of the spectrum, line_7: again in order to achieve the maximum photometric precision. A substep line_8: routine, with offsets of 1/2 diode, will be used to achieve full line_9: spectrophotometric accuracy. line_11: The sequence of lines observed will differ somewhat in the different stars, line_12: depending on the anticipated strength of the various lines and the photometric line_13: accuracy achievable with practical exposure times on stars of different line_14: magnitudes. Among the atomic species whose lines will be observed are CII, NI line_15: and V, OI, SII, SIII, SiII and IV, MgII, PII and III, FeII. line_17: When data on HRS performance are available in orbit, some modifications of the line_18: observing sequence for each star may be desirable. line_20: About half the time will be devoted to 5 relatively faint stars (V ~ 7 mag) at line_21: distances from the galactic plane exceeding 1 kpc. The other half will be used line_22: for observing a much larger number of brighter stars at low galactic latitudes line_23: (13 with V < 4.0 mag, 7 with V between 4 and 5 mag, and 2 w/V between 5 & 6 mag. ! question: 3 section: 2 line_1: The exposure listed on lines 27 through 32 of the exposure log sheet should, line_2: insofar as practicable, be included in cycle 0; those on lines 33-49, in cycle line_3: 1; those on lines 50-58, in cycle 2. line_5: (cont'd from EL line 3.000) line_6: 2 samples per diode in substep pattern. line_8: (cont'd from PROBLEM LOG/item # 5) line_9: particularly Alpha-1-Cru, with a component 5.6" away and a brightness dimmer by line_10: 0.5 mag than that of the primary. ! question: 4 section: 1 line_1: This program requires measures of interstellar absorption lines produced by line_2: atoms in their dominant stage of ionization, so that the relative abundances of line_3: several chemical abundances can be intercompared, without any necessity for line_4: ionization corrections. Only one such element has such lines (TiII) accessible line_5: from the ground. Moreover, none of the highly ionized species, such as SIII line_6: and PIII, which have low abundances in H I regions can be observed from the line_7: ground; observations of such ions are needed to ascertain which components of line_8: interstellar lines are produced by H II regions. ! question: 7 section: 1 line_1: While the numerical analysis required for this program is straightforward and line_2: not very complex, the amount of data to be measured and analyzed is rather line_3: large. A full-time research associate will be engaged for a period of two line_4: years to undertake the systematic analysis of this material, with close line_5: collaboration by L. Spitzer. ! question: 13 section: 1 line_1: Spectra of interstellar lines will be observed with the HRS-Echelle in the line_2: spectra of 27 stars, some at large distances from the galactic plane, others in line_3: the galactic disc. The lines of elements such as C, N, O, Mg, Si, P, S and Fe line_4: will be resolved into components and the composition determined. Dependence of line_5: depletion on the physical properties of the components should help to clarify line_6: the equilibrium between dust grains and the gas. ! !end of general form text general_form_address: lname: SPITZER JR. fname: LYMAN category: CON inst: PRINCETON UNIV. OBSERVATORY addr_1: PEYTON HALL city: PRINCETON state: NJ zip: 08544 country: USA phone: 609-452-3809 telex: 322409 ! lname: O'DELL fname: C. mi: R. title: PROF. category: PI 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: 1 name_1: HD93521 descr_1: O9.5V pos_1: RA=10H45M33.60S +/- .1S, pos_2: DEC=37D50'4.5" +/- 1.0" equinox: 1950 pm_or_par: NO fluxnum_1: 1 fluxval_1: V=7.04,E(B-V)=0.02 fluxnum_2: 2 fluxval_2: F-CONT(1300)=3.2+/-0.9E-10 ! targnum: 17 name_1: HD68273 name_2: GAMMA2VEL descr_1: O9I+WC8 pos_1: RA=8H7M59.47S +/- .1S, pos_2: DEC=-47D11'18.4" +/- 1.0" equinox: 1950 pm_or_par: NO acqpr_1: COMP fluxnum_1: 1 fluxval_1: V=1.83,E(B-V)=0.05 fluxnum_2: 2 fluxval_2: F-CONT(1300)=4.8+/-0.5E-8 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 sequence_1: DEFINE sequence_2: BR-1 targname: # config: HRS opmode: WSCAN aperture: 0.25 sp_element: ECH-A wavelength: 1191.20-1192.61 num_exp: 1 time_per_exp: 18S s_to_n: # fluxnum_1: 2 priority: # param_1: STEP-PATT=DEF, param_2: COMB=TWO, param_3: WAVE-STEP=0.47 req_1: CYCLE 0 / 001-020 comment_1: EXPOSURE TIMES IN LINES 1-12 YIELD comment_2: S/N=100 FOR EACH OF 3 SUBEXPOSURES comment_3: FOR A STANDARD STAR WITH F-CONT(1300)= comment_4: 1.0E-8, ASSUMING ORIGINAL HST FLUXES. comment_5: "WAVE-STEP" IN COLUMN 9 OF LINE 1 IS comment_6: EQUIVALENT TO 8 CARROUSEL STEPS. ! linenum: 2.000 sequence_1: ^ sequence_2: ^ targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: ^ wavelength: 1240.05-1241.55 num_exp: ^ time_per_exp: 33S s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: STEP-PATT=DEF, param_2: COMB=TWO, param_3: WAVE-STEP=0.50 comment_1: "WAVE-STEP" IN COLUMN 9 OF LINE 2 IS comment_2: EQUIVALENT TO 8 CARROUSEL STEPS. ! linenum: 3.000 sequence_1: ^ sequence_2: ^ targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: ^ wavelength: 1252.18-1253.62 num_exp: ^ time_per_exp: 27S s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: STEP-PATT=DEF, param_2: COMB=TWO, param_3: WAVE-STEP=0.48 comment_1: "WAVE-STEP" IN COLUMN 9 OF LINE 3 IS comment_2: EQUIVALENT TO 8 CARROUSEL STEPS. ! linenum: 4.000 sequence_1: ^ sequence_2: ^ targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: ^ wavelength: 1302.44-1304.00 num_exp: ^ time_per_exp: 24S s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: STEP-PATT=DEF, param_2: COMB=TWO, param_3: WAVE-STEP=0.52 comment_1: "WAVE-STEP" IN COLUMN 9 OF LINE 4 IS comment_2: EQUIVALENT TO 8 CARROUSEL STEPS. ! linenum: 5.000 sequence_1: ^ sequence_2: ^ targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: ^ wavelength: 1333.46-1335.02 num_exp: ^ time_per_exp: 33S s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: STEP-PATT=DEF, param_2: COMB=TWO, param_3: WAVE-STEP=0.52 comment_1: "WAVE-STEP" IN COLUMN 9 OF LINE 5 IS comment_2: EQUIVALENT TO 8 CARROUSEL STEPS. ! linenum: 6.000 sequence_1: ^ sequence_2: ^ targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: ^ wavelength: 1356.16-1356.97 num_exp: ^ time_per_exp: 57S s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: STEP-PATT=DEF, param_2: COMB=TWO, param_3: WAVE-STEP=0.27 comment_1: "WAVE-STEP" IN COLUMN 9 OF LINE 6 IS comment_2: EQUIVALENT TO 4 CARROUSEL STEPS. ! linenum: 7.000 sequence_1: ^ sequence_2: ^ targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: ^ wavelength: 1391.69-1393.37 num_exp: ^ time_per_exp: 66S s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: STEP-PATT=DEF, param_2: COMB=TWO, param_3: WAVE-STEP=0.56 comment_1: "WAVE-STEP" IN COLUMN 9 OF LINE 7 IS comment_2: EQUIVALENT TO 8 CARROUSEL STEPS. ! linenum: 8.000 sequence_1: ^ sequence_2: ^ targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: ^ wavelength: 1529.68-1530.52 num_exp: ^ time_per_exp: 60S s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: STEP-PATT=DEF, param_2: COMB=TWO, param_3: WAVE-STEP=0.28 comment_1: "WAVE-STEP" IN COLUMN 9 OF LINE 8 IS comment_2: EQUIVALENT TO 4 CARROUSEL STEPS. ! linenum: 9.000 sequence_1: ^ sequence_2: ^ targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: ^ wavelength: 1546.32-1548.18 num_exp: ^ time_per_exp: 69S s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: STEP-PATT=DEF, param_2: COMB=TWO, param_3: WAVE-STEP=0.62 comment_1: "WAVE-STEP" IN COLUMN 9 OF LINE 9 IS comment_2: EQUIVALENT TO 8 CARROUSEL STEPS. ! linenum: 10.000 sequence_1: DEFINE sequence_2: BR-1 targname: # config: HRS opmode: WSCAN aperture: 0.25 sp_element: ECH-B wavelength: 1804.92-1807.08 num_exp: 1 time_per_exp: 27S s_to_n: # fluxnum_1: 2 priority: # param_1: STEP-PATT=DEF, param_2: COMB=TWO, param_3: WAVE-STEP=0.72 comment_1: "WAVE-STEP" IN COLUMN 9 OF LINE 10 IS comment_2: EQUIVALENT TO 8 CARROUSEL STEPS. ! linenum: 11.000 sequence_1: ^ sequence_2: ^ targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: ^ wavelength: 2368.98-2371.62 num_exp: ^ time_per_exp: 15S s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: STEP-PATT=DEF, param_2: COMB=TWO, param_3: WAVE-STEP=0.88 comment_1: "WAVE-STEP" IN COLUMN 9 OF LINE 11 IS comment_2: EQUIVALENT TO 8 CARROUSEL STEPS. ! linenum: 12.000 sequence_1: ^ sequence_2: ^ targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: ^ wavelength: 2600.71-2603.50 num_exp: ^ time_per_exp: 24S s_to_n: ^ fluxnum_1: ^ priority: ^ param_1: STEP-PATT=DEF, param_2: COMB=TWO, param_3: WAVE-STEP=0.93 comment_1: "WAVE-STEP" IN COLUMN 9 OF LINE 12 IS comment_2: EQUIVALENT TO 8 CARROUSEL STEPS. ! linenum: 13.000 targname: HD68273 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-A1 num_exp: 1 time_per_exp: 57.8S priority: 2 param_1: FAINT=700, param_2: LOCATE=YES, param_3: MAP=END-POINT, SEARCH-SIZE=5 req_1: ONBOARD ACQUISITION FOR 13.1; req_2: SEQ 13-16 NO GAP; ! linenum: 13.100 targname: HD68273 config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-A1 num_exp: 1 time_per_exp: 9.2S priority: 2 req_1: ONBOARD ACQ FOR 14-16; comment_1: STEP-TIME=0.2 SEC ! linenum: 14.000 targname: WAVE config: ^ opmode: ACCUM aperture: SC1 sp_element: ECH-A wavelength: 1191.43 num_exp: 1 time_per_exp: 40S priority: 2 param_1: STEP-PATT=DEF, param_2: COMB=TWO ! linenum: 15.000 sequence_1: USE sequence_2: BR-1 targname: HD68273 time_per_exp: X3.2 s_to_n: 180 priority: 2 comment_1: THE MULTIPLICATIVE FACTOR 3.2 FOR ALL comment_2: BR-1 EXPOSURES FOR THIS STAR HAS BEEN comment_3: CALCULATED TO GIVE S/N=180 FOR THE HST comment_4: FLUX AS REDUCED BY SPHERICAL comment_5: ABERRATION. ! linenum: 16.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC1 sp_element: ECH-B wavelength: 2603.03 num_exp: 1 time_per_exp: 10S priority: 2 param_1: STEP-PATT=DEF, param_2: COMB=TWO ! linenum: 17.000 targname: HD93521 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 57.8S priority: 2 param_1: FAINT=1200, param_2: LOCATE=YES, param_3: MAP=END-POINT, SEARCH-SIZE=5 req_1: ONBOARD ACQUISITION FOR 17.1; req_2: SEQ 17-20 NO GAP; ! linenum: 17.100 targname: HD93521 config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 9.2S priority: 2 req_1: ONBOARD ACQ FOR 18-20; comment_1: STEP-TIME=0.2 SEC. ! linenum: 18.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC1 sp_element: ECH-A wavelength: 1191.43 num_exp: 1 time_per_exp: 40S priority: 2 param_1: STEP-PATT=DEF, param_2: COMB=TWO ! linenum: 19.000 sequence_1: USE sequence_2: BR-1 targname: HD93521 time_per_exp: X16.0 s_to_n: 32 priority: 2 comment_1: THE MULTIPLICATIVE FACTOR 16 FOR ALL comment_2: BR-1 EXPOSURES FOR THIS STAR HAS BEEN comment_3: CALCULATED TO GIVE S/N=32 FOR THE HST comment_4: FLUX AS REDUCED BY SPHERICAL comment_5: ABERRATION. ! linenum: 20.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC1 sp_element: ECH-B wavelength: 2603.03 num_exp: 1 time_per_exp: 10S priority: 2 param_1: STEP-PATT=DEF, param_2: COMB=TWO ! ! end of exposure logsheet ! No scan data records found