! File: 1065C.PROP ! Database: PEPDB ! Date: 16-FEB-1994:00:22:32 coverpage: title_1: ISOTOPIC ABUNDANCES OF CARBON AND OXYGEN AND FRACTIONATION IN title_2: INTERSTELLAR CARBON MONOXIDE sci_cat: INTERSTELLAR MEDIUM proposal_for: GTO/OS pi_title: PROF. pi_fname: DAVID pi_mi: L. pi_lname: LAMBERT pi_inst: TEXAS, UNIVERSITY OF pi_country: USA pi_phone: 512-471-4461 keywords_1: INTERSTELLAR MOLECULES-CO. ABUNDANCES AND keywords_2: NUCLEOSYNTHESIS-ISOTOPES OF C AND O - MOLECULAR PROCESSES - FRACTIONATION hours_pri: 4.00 num_pri: 1 hrs: X pi_position: PROFESSOR ! end of coverpage abstract: line_1: HRS observations of the CO A-X system between 1250 and 1550 A will be acquired line_2: and analyzed to obtain abundances of 12C16O, 13C16O, 12C17O, and 12C18O, and to line_3: study the rotational excitation of the CO molecule. Additional observations of line_4: the weak inter-combination line of C II at 2324 A have provided the C+ abundance line_5: which plays an important role in chemical fractionation. line_7: Diffuse interstellar gas towards local stars (e.g. Zeta Oph) will line_8: be observed lines of the less abundant isotopic species line_9: of CO. A check on the Galactic gradient in the 12C/13C ratio will be attempted line_10: by observing stars about 1 kpc towards and away from the Galactic center. ! ! end of abstract general_form_proposers: lname: LAMBERT fname: DAVID mi: L. inst: TEXAS, UNIVERSITY OF country: USA ! lname: FEDERMAN fname: STEVEN mi: R. inst: JET PROPULSION LABORATORY country: USA ! lname: GILLILAND fname: RONALD mi: L. inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: High S/N HRS echelle spectra of bright slightly reddened stars at line_2: several wavelengths between 1480 and 1230 A (G160M). Each exposure line_3: has been subdivided into several parts. Smaller intervals are assumed here in line_4: order to reduce fluctuations from photocathode granularity. ! question: 4 section: 1 line_1: For diffuse clouds, the ^12C/^13C ratio is just measurable from the ground via line_2: the CH^+ interstellar lines (see, in particular, Jura and BAAS, 1985). As line_3: discussed in 2., interpretation of isotopic ratios from dense clouds is line_4: confused by radiative transfer effects. The CO ultraviolet lines provide the line_5: only opportunity to measure ^12C/^13C and ^16O/^17O/^18O along several lines of line_6: sight. Copernicus and IUE lacked the necessary sensitivity. ! question: 6 section: 1 line_1: This program calls for high S/N spectra. Some observations should be scheduled line_2: in CYCLE1 to allow testing of techniques for high S/N, others to later cycles. line_3: Based on my experience with ground-based detectors, I suspect that a line_4: bright star will have to be observed in order to achieve an adequate line_5: calibration of the pixel-pixel variations: flat-fielding using a monochromatic line_6: lamp is unlikely to yield adequate accuracy. In the event that observation of line_7: a star is necessary, the observing time may be taken from that assigned to low line_8: priority stars. Note too that special techniques may be necessary to ensure line_9: high S/N: e.g., positioning the line on the optimum portion of the line_10: photocathode. ! question: 7 section: 1 line_1: The spectra as reduced by the standard STScI software will be analyzed at UT line_2: and JPL. Synthetic CO profiles will be fitted to the observations to extract line_3: the CO column density, rotational temperature, the radial velocity, and the line_4: isotopic abundance ratios. line_5: Software developed at STScI will be used to optimally separate the stellar line_6: spectra from fixed-pattern noise. ! question: 10 section: 1 line_1: Departmental, Institute and University computing facilities will be used. ! question: 13 section: 1 line_1: HRS observations of the CO A-X system between 1250 and 1550 A will be acquired line_2: and analyzed to obtain abundances of 12C160, 13C160, 12C170, and 12C180, and to line_3: study the rotational ecitation of the CO molecule. Additional observations of line_4: the weak inter-combination line of C II at 2324 A have provided the C+ abundance line_5: which plays an important role in chemical fractionation. line_7: Diffuse interstellar gas towards local stars (e.g. Zeta Oph) will line_8: be observed for the lines of the less abundant isotopic species line_9: of CO. A check on the Galactic gradient in the 12C/13C ratio will be attempted line_10: by observing stars about 1 kpc towards and away from the Galactic center. ! !end of general form text general_form_address: lname: FEDERMAN fname: STEVEN mi: R. category: CON inst: JET PROPULSION LABORATORY addr_1: 4800 OAK GROVE AVENUE city: PASADENA state: CA zip: 91109 country: USA phone: 818-354-2274 telex: 910-588-3294 ! lname: GILLILAND fname: RONALD mi: L. inst: SPACE TELESCOPE SCIENCE INSTITUTE addr_1: 3700 SAN MARTIN DRIVE city: BALTIMORE state: MD zip: 21218 country: USA phone: 301-338-4454 ! lname: LAMBERT fname: DAVID mi: L. title: PROF. category: PI inst: UNIVERSITY OF TEXAS addr_1: ASTRONOMY DEPARTMENT addr_2: RLM 15.308 city: AUSTIN state: TX zip: 78712 country: USA phone: 512-471-4461 telex: 910-874-1351 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: HD149757 name_2: ZETA-OPH descr_1: OB STAR BEHIND INTERSTELLAR CLOUD pos_1: RA = 16H 37M 09.53S +/- 0.01S, pos_2: DEC = -10D 34' 02.1" +/- 0.04", pos_3: PLATE-ID=006P equinox: 2000 pm_or_par: Y pos_epoch_yr: 1950.00 ra_pm_val: 0.000800 ra_pm_unct: 0.000067 dec_pm_val: 0.0230 dec_pm_unct: 0.0010 fluxnum_1: 1 fluxval_1: V=2.56, TYPE = 09.5 V, E(B-V)=0.32 fluxnum_2: 2 fluxval_2: F-CONT(2320)=1.2 +/- .2 E-9 fluxnum_3: 3 fluxval_3: F-CONT(1400)=4.0 +/- .4 E-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: STOBSG targname: # config: HRS opmode: ACCUM aperture: 0.25 sp_element: # wavelength: 1.0 num_exp: # time_per_exp: 108.8S s_to_n: 100 s_to_n_time: 20M fluxnum_1: 2 priority: # param_1: FP-SPLIT=STD param_2: STEP-PATT=5 ! linenum: 2.000 targname: HD149757 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 5.0S s_to_n: 10 fluxnum_1: 1 priority: 1 param_1: SEARCH-SIZE=5, param_2: FAINT=15000 req_1: CYCLE 1 / 2.0 ; req_2: ONBOARD ACQ FOR 2.1 comment_1: CENTER IN LSA AND TAKE IMAGE ! linenum: 2.100 targname: HD149757 config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 9.2S s_to_n: 10 fluxnum_1: 1 priority: 1 req_1: CYCLE 1 / 2.1 ; req_2: ONBOARD ACQ FOR 2.2-9.2 ! linenum: 2.200 targname: HD149757 config: HRS opmode: IMAGE aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 96.8S s_to_n: 10 fluxnum_1: 1 priority: 1 req_1: CYCLE 1 / 2.2 ! linenum: 5.000 sequence_1: USE sequence_2: STOBSG targname: HD149757 sp_element: G160M wavelength: X1463.7 num_exp: 3 time_per_exp: X4 priority: 1 req_1: CYCLE 1 / 5.0, 5.1, 5.2, 5.3, 5.4, 5.5 comment_1: MULTIPLEXS 1448 AND 1478 REGIONS ! linenum: 5.100 sequence_1: USE sequence_2: STOBSG targname: HD149757 sp_element: G160M wavelength: X1464.8 num_exp: 3 time_per_exp: X4 priority: 1 ! linenum: 5.200 sequence_1: USE sequence_2: STOBSG targname: HD149757 sp_element: G160M wavelength: X1462.6 num_exp: 3 time_per_exp: X4 priority: 1 ! linenum: 5.300 sequence_1: USE sequence_2: STOBSG targname: HD149757 sp_element: G160M wavelength: X1466.8 num_exp: 3 time_per_exp: X4 priority: 1 ! linenum: 5.400 sequence_1: USE sequence_2: STOBSG targname: HD149757 sp_element: G160M wavelength: X1461.0 num_exp: 3 time_per_exp: X4 priority: 1 ! linenum: 5.500 sequence_1: USE sequence_2: STOBSG targname: HD149757 sp_element: G160M wavelength: X1471.0 num_exp: 3 time_per_exp: X4 priority: 1 ! linenum: 7.000 sequence_1: USE sequence_2: STOBSG targname: HD149757 sp_element: G160M wavelength: X1353.1 time_per_exp: X3 priority: 1 req_1: CYCLE 1 / 7.0, 7.1, 7.2 ! linenum: 7.100 sequence_1: USE sequence_2: STOBSG targname: HD149757 sp_element: G160M wavelength: X1355.0 time_per_exp: X3 priority: 1 ! linenum: 7.200 sequence_1: USE sequence_2: STOBSG targname: HD149757 sp_element: G160M wavelength: X1357.9 time_per_exp: X3 priority: 1 ! linenum: 9.000 sequence_1: USE sequence_2: STOBSG targname: HD149757 sp_element: G160M wavelength: X1271.1 time_per_exp: X3 priority: 1 req_1: CYCLE 1 / 9.0, 9.1, 9.2 ! linenum: 9.100 sequence_1: USE sequence_2: STOBSG targname: HD149757 sp_element: G160M wavelength: X1273.0 time_per_exp: X3 priority: 1 ! linenum: 9.200 sequence_1: USE sequence_2: STOBSG targname: HD149757 sp_element: G160M wavelength: X1275.9 time_per_exp: X3 priority: 1 ! ! end of exposure logsheet ! No scan data records found