! File: 3957C.PROP ! Database: PEPDB ! Date: 20-FEB-1994:01:37:34 coverpage: title_1: SEARCH FOR INTERSTELLAR MOLECULES IN SPECTRA OF TWO B STARS title_2: -- CYCLE 2 sci_cat: INTERSTELLAR MEDIUM proposal_for: GTO/HRS cont_id: 1200 pi_fname: ANDREW pi_mi: M. pi_lname: SMITH pi_inst: NASA, GODDARD SPACE FLIGHT CENTER pi_country: USA pi_phone: (301)286-3900 keywords_1: MOLECULAR CLOUD, INTERSTELLAR MOLECULES hours_pri: 9.00 num_pri: 2 pi_position: STAFF ASTRONOMER ! end of coverpage abstract: line_1: We will probe the chemical and physcial processes in diffuse line_2: interstellar clouds and look for evidence of line_3: molecule formation in gas heated by shocks or intense line_4: ultraviolet radiation. We will observe HD62542, a star in the line_5: Gum Nebula at seven carousel positions in the medium line_6: resolution modes. Optical studies indicate that one of line_7: the components of its interstellar spectrum is characterized line_8: by high density (approximately 10,000/cubic cm) and highest line_9: density per unit visual extinction of any star yet studied. line_10: We will also observe omicron Persei using the echelle, and line_11: combine the results with previous high quality results line_12: obtained by the "Copernicus" satellite. ! ! end of abstract general_form_proposers: lname: BRUHWEILER fname: FRED inst: CATHOLIC UNIVERSITY OF AMERICA country: USA ! lname: CARDELLI fname: JASON mi: D. inst: WISCONSIN, UNIVERSITY OF country: USA ! lname: SMITH fname: ANDREW mi: M. inst: NASA, GODDARD SPACE FLIGHT CENTER country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: The GHRS will be used. For both o Per and HD62542 we line_2: propose to look for six molecules, H2O, N2, HCl, CH2, SiO, line_3: and CS. For o Per, 88 carousel echelle settings are required, line_4: 14 at medium resolution and 2 at the low resolution. All line_5: require the FP-SPLIT option. A scheme is used that includes line_6: using multiple wavelength settings for each molecular line, line_7: thus sampling different parts of the detector windows line_8: and diode arrays to minimize fixed pattern noise. For line_9: HD62542, H2 and CO, will also be included. Medium and low line_10: resolution will be used, except for one echelle line_11: observation of the CO (7-0). 32 carousel settings are line_12: planned. The FP-SPLIT option is used, but varying the line_13: central wavelength for each molecular feature is not line_14: considered to be necessary since the anticipated equivalent line_15: widths should be several mA. When possible, lines of line_16: interest are placed on a region of the detector to avoid line_17: defective diodes and to minimize fixed pattern noise. line_18: For mostmolecules (CO and H2 excepted) the features are weak, line_19: long exposures and large S/N ratios are required. line_20: HD62542 line_21: exposures exposures exposures line_22: Cycle 2 line_23: 101.0,101.1,101.2,101.3,102.0,106.0 ! question: 3 section: 2 line_1: line_4: Star o Per line_5: exposures exposures exposures line_6: Cycle 3 line_7: 1.5, 1.6, 1.7, 6.1, 6.2, 6.3, 20.0, 20.1 line_8: 22.1, 22.2, 22.3, 24.0, 25.0, 26.0, 27.0 line_14: COMMENT CONTINUED FROM TF TARGET NUMBER 1: line_16: 21 F(2717)=2.7+/-0.3E-10, 22 F(2803)=2.5+/-0.3E-10, 23 F(1768)=6.8+/-2.0E-10, line_17: 24 F(2889)=2.5+/-0.3E-10, 25 F(1412)=8.6+/-2.0E-10, 26 F(1460)=9.2+/-2.0E-10 ! question: 4 section: 1 line_1: The spectra of few interstellar molecules exist in the optical line_2: whereas many are found in the HRS range. "Copernicus" line_3: demonstrated the usefulness of the UV to interstellar studies line_4: but it possessed neither the resolving power not the line_5: sensitivity required to measure the column densities of line_6: molecules other than CO and molecular hydrogen. I.U.E. has line_7: been successful in observations of faint stars, but line_8: its resolving power is about a factor of 2 less than that of line_9: "Copernicus" and its limiting S/N ratio is much too large line_10: to detect any interstellar molecules other than CO. ! question: 5 section: 1 line_1: No real-time observations are required. ! question: 6 section: 1 line_1: A single wavelength scale calibration is required for each line_2: target in order to relate line velocities measured with the line_3: GHRS to measurements of other instruments. Accuracies on line_4: the order to +/- 0.5 km/s an d +/- 2.2 km/s for the high line_5: and medium resolving power modes can be realized. Determining line_6: cloud component radial velocities relative to measured background line_7: star velocities is unreliable because the stellar lines are line_8: are broadened by rotation and blending. The wavelength scale line_9: calibration should be performed immediately following a science line_10: observation for the same carousel position to avoid any time line_11: dependent variations of the wavelength scale due, for example, line_12: to temperature fluctuations or positional variations of the line_13: stellar image in the science apertures. Otherwise, there is line_14: no requirement for ambiguous observations or uninterrupted line_15: exposures. ! question: 7 section: 1 line_1: These will be designed to determine column densities of both molecular and line_2: atomic species with a view toward finding abundances. Both curve-of-growth and line_3: profile fitting techniques will be employed. In some cases it is line_4: possible using comparatively few reaction channels to draw line_5: conclusions regarding the details of relevant gas phase line_6: chemistry, and to a limited extent, the physical conditions of line_7: the cloud)s) in which the molecules are embedded. Such species line_8: include HCl, SiO, and CS. Other species such as H2O, N2 and line_9: CH2 will require analyses involving large arrays of chemical line_10: reactions since the chemistry of Hydro-carbons and oxygen- line_11: bearing molecules is complex. Cloud models will be constructed line_12: in which chemical equililbrium is established and in which the line_13: chemistry is time dependent as during the passage of an MHD shock. line_14: The success of this analysis will depend on the line_15: quality and quantity of our measurements as well as on the availability of line_16: reasonably accurate rate constants. ! question: 10 section: 1 line_1: Both computer hardware and software will be available at NASA/GSFC for data line_2: analysis. ! question: 13 section: 1 line_1: This program constitutes a search for molecules in diffuse interstellar clouds. line_2: The High Resolution Spectrograph will be used to observe portions line_3: of the spectrum of HD62542 at medium resolving power and line_4: portions of the spectrum of o Per at both high and medium line_5: resolving power. The scientific goal is to study molecule line_6: formation mechanisms in diffuse interstellar clouds. ! !end of general form text general_form_address: lname: SMITH fname: ANDREW mi: M. category: PI inst: NASA, GODDARD SPACE FLIGHT CENTER city: GREENBELT state: MD zip: 20771 country: USA phone: 301-344-8648 telex: 89675 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: HD23180 name_2: OMICRON-PER descr_1: B1 III STAR SHOWING descr_2: INTERSTELLAR descr_3: MOLECULAR SPECTRUM pos_1: RA=3H44M19.1S+/-0.1S, pos_2: DEC=+32D17'18"+/-1.0" equinox: 2000 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 2000.00 ra_pm_val: 0.000533 ra_pm_unct: 0.000133 dec_pm_val: -0.0090 dec_pm_unct: 0.0020 an_prlx_val: 0.0230 rv_or_z: V=+18.5 comment_1: 11 F(1335)=8.7+/-2.0E-10 comment_2: 12 F(1341)=8.7+/-2.0E-10 comment_3: 13 F(1657)=8.2+/-2.0E-10 comment_4: 14 F(1914)=4.0+/-0.6E-10 comment_5: 15 F(2190)=2.7+/-0.3E-10 comment_6: 16 F(2242)=2.4+/-0.3E-10 comment_7: 17 F(2266)=2.8+/-0.3E-10 comment_8: 18 F(2313)=2.8+/-0.3E-10 comment_9: 19 F(2344)=2.9+/-0.3E-10 comment_10: 20 F(2576)=3.2+/-0.3E-10 fluxnum_1: 1 fluxval_1: V=3.83+/-0.02,TYPE=B1III,E(B-V)=0.31 fluxnum_2: 2 fluxval_2: F(1216)=1.0+/-0.3E-10 fluxnum_3: 3 fluxval_3: F(1222)=2.0+/-0.5E-10 fluxnum_4: 4 fluxval_4: F(1227)=2.5+/-0.6E-10 fluxnum_5: 5 fluxval_5: F(1241)=7.9+/-2.0E-10 fluxnum_6: 6 fluxval_6: F(1257)=7.9+/-2.0E-10 fluxnum_7: 7 fluxval_7: F(1273)=7.9+/-2.0E-10 fluxnum_8: 8 fluxval_8: F(1290)=9.0+/-2.0E-10 fluxnum_9: 9 fluxval_9: F(1302)=7.0+/-2.0E-10 fluxnum_10: 10 fluxval_10: F(1310)=1.0+/-0.2E-9 ! targnum: 3 name_1: HD62542 name_2: SAO218917 descr_1: B5 V STAR IN THE descr_2: GUM NEBULA pos_1: RA=7H 40M 58.073S+/-0.05", pos_2: DEC=-42D 06' 36.16"+/-0.7" equinox: 1950 pm_or_par: Y pos_epoch_bj: B pos_epoch_yr: 1950.00 ra_pm_val: -0.001000 ra_pm_unct: 0.000080 dec_pm_val: 0.0170 dec_pm_unct: 0.0012 fluxnum_1: 1 fluxval_1: V=8.04, TYPE=B5V, B-V=0.17 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 101.000 targname: HD62542 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 5S fluxnum_1: 1 priority: 1 param_2: BRIGHT=RETURN, param_3: SEARCH-SIZE=5 req_1: ONBOARD ACQ FOR 101.1-117; req_2: CYCLE 2/101-117 ! linenum: 101.100 targname: HD62542 config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 20.4S s_to_n: 10 fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 106-117; req_2: CYCLE 2 ! linenum: 106.000 targname: HD62542 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1234.86 num_exp: 33 time_per_exp: 5.8M s_to_n: 30 priority: 1 param_1: STEP-PATT=4, param_2: FP-SPLIT=STD req_1: CYCLE 2 comment_1: MOLECULAR H2O ! linenum: 108.000 targname: HD62542 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1284.20 num_exp: 20 time_per_exp: 5.8M s_to_n: 42 priority: 1 param_1: STEP-PATT=4, param_2: FP-SPLIT=STD req_1: CYCLE 2 comment_1: MOLECULAR HCL,N2 ! linenum: 109.000 targname: WAVE config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1344.27 num_exp: 1 time_per_exp: 30S priority: 1 param_1: STEP-PATT=4 req_1: CALIB FOR 109.1; CYCLE 2; req_2: SEQ 109.0-109.1 NO GAP ! linenum: 109.100 targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: ^ wavelength: 1344.27 num_exp: 10 time_per_exp: 5.8M s_to_n: 22 priority: 1 param_1: STEP-PATT=4, param_2: FP-SPLIT=STD req_1: CYCLE 2 comment_1: MOLECULAR C2,CLI,OI,CII ! linenum: 110.000 targname: HD62542 config: ^ opmode: ^ aperture: ^ sp_element: ^ wavelength: 1400.42 num_exp: 20 time_per_exp: 5.8M s_to_n: 42 priority: 1 param_1: STEP-PATT=4, param_2: FP-SPLIT=STD req_1: CYCLE 2 comment_1: MOLECULAR CH2 ! linenum: 117.000 targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: G270M wavelength: 2586.76 num_exp: 10 time_per_exp: 5.8M s_to_n: 42 priority: 1 param_1: STEP-PATT=4, param_2: FP-SPLIT=STD req_1: CYCLE 2 comment_1: MOLECULAR CS ! ! end of exposure logsheet ! No scan data records found