! File: 3759C.PROP ! Database: PEPDB ! Date: 19-FEB-1994:18:35:09 coverpage: title_1: DUST, MOLECULAR, ATOMIC COMPOSITION AND THE PHYSICAL CONDITIONS title_2: IN MOLECULAR CLOUDS sci_cat: INTERSTELLAR MEDIUM sci_subcat: DUST proposal_for: GO pi_fname: FRANCOIS pi_lname: BOULANGER pi_inst: RADIOASTRONOMIE - ECOLE NORMALE SUPERIEURE pi_country: FRANCE pi_phone: 33-44 32 33 47 hours_pri: 6.70 num_pri: 2 hrs: Y off_fname: PAUL off_lname: CRUVELLIER off_title: DIRECTOR off_inst: LABORATOIRE D'ASTRONOMIE SPATIALE off_addr_1: TRAVERSE DU SIPHON off_addr_2: LES TROIS LUCS off_city: 13012 MARSEILLE off_country: FRANCE off_phone: (33) 91 05 59 00 ! end of coverpage abstract: line_1: IRAS images of nearby molecular clouds show that the mid-IR (12 and 25um) line_2: emission, supposed to come from small particules, is distributed very line_3: differently from the 100 um emission from large grains. These variations line_4: in the IR colors probably result from variations in the abundance of the line_5: small particules. We have performed observations of clouds of different line_6: colors ("blue" and "red") in the Chamaeleon at sub-mm, visible and UV line_7: wavelengths. They show that the variations in the IR colors are accompa line_8: nied by variations in the extinction curve, in the abundance of molecules line_9: (CO, CH+), as well as in temperature and density. The observation with line_10: the GHRS of several atomic and molecular absorption lines in the spectra line_11: of stars located behind both red and blue clouds will give access to line_12: important information on the clouds : H column densities from the lines line_13: of SII, depletion processes from the Si abundance, density and line_14: temperature from lines of the different CO rotation levels, pressure line_15: independently from lines of different CI excitation levels, cooling line_16: rates and heating processes in cold and warm phases from respectively line_17: CII and OI excited levels... All these quantities compared with our line_18: models will in addition to the study of the color variations and their line_19: implications, constitute a valuable data base to understand the physics line_20: and chemistry of these molecular clouds. ! ! end of abstract general_form_proposers: lname: BOULANGER fname: FRANCOIS title: PI inst: RADIOASTRONOMIE - ECOLE NORMALE SUPERIEURE country: FRANCE esa: Y ! lname: GRY fname: CECILE inst: LABORATOIRE D'ASTRONOMIE SPATIALE country: FRANCE esa: Y ! lname: LEQUEUX fname: JAMES inst: OBSERVATOIRE DE PARIS-MEUDON country: FRANCE esa: Y ! lname: FALGARONE fname: EDITH inst: RADIOASTRONOMIE - ECOLE NORMALE SUPERIEURE country: FRANCE esa: Y ! ! end of general_form_proposers block general_form_text: question: 2 section: 1 line_1: ! question: 3 section: 1 line_1: We will record the spectrum of 2 stars at three spectral settings of line_2: the G160M grating. The three center wavelengths are 1265, 1338 and line_3: 1462 A. This should provide measurements of the following lines: line_4: CI (1216, 1280, and 1329 A) and CII (1355 A) line_5: OI (1355 A) line_6: CO (1447 and 1477 A) line_7: SII (1252 and 1258 A) line_8: To get the highest spectral resolution we will observe with the line_9: small aperture (SSA) and proceed by substepping the spectrum across line_10: the detector in 1/4-diode steps and then combining the four spectra line_11: into an oversampled spectrum, as it is described by R. Gilliland in line_12: the STScI Newsletter, June 1991. line_13: To correct for the photocathode granularity we will break down the line_14: exposure into 4 sub-exposures via the FP-split procedure. ! question: 4 section: 1 line_1: These observations (high resolution-spectroscopy in the Far-UV) can line_2: only be done with the GHRS on board the HST. Attempts for using IUE line_3: have been very disappointing for lack of resolution and signal to line_4: noise ratio. IUE spectra were used to plan these observations, showing line_5: us qualitatively which were the most interesting features in the spectra line_6: to characterize the two kinds of clouds. IUE low resolution spectra line_7: were used to derive the extinction curve for a larger sample of stars. line_8: We also high resolution optical spectra to measure the abundance of line_9: several molecular and atomic species. ! question: 5 section: 1 line_1: None ! question: 6 section: 1 line_1: None ! question: 7 section: 1 line_1: We will get from the ST ScI the calibrated science data which is line_2: provided as the output of the Routine Science Data Processing (RSDP) line_3: and Calibration Data Base Software (CDBS) at the Institut. line_4: The data reduction can be made at any of the proposing institutes line_5: which possess adequate facilities, with the help if necessary of the line_6: ESA ST/ECF in Garching. The data analysis will be done using an line_7: interactive program for line-profile fitting of which we have a line_8: considerable experience. ! question: 8 section: 1 line_1: None ! question: 9 section: 1 line_1: P 2078 "A search for primordial gas; is IZw18 a young galaxy?" line_2: PI J. Lequeux line_3: Not related to present project line_4: Observations not yet done line_5: no publication yet (see above) ! question: 10 section: 1 line_1: All resources to be provided by the proposer's institutes line_2: One student will be dedicated to the project. ! !end of general form text general_form_address: lname: BOULANGER fname: FRANCOIS category: PI inst: RADIOASTRONOMIE - ECOLE NORMALE SUPERIEURE addr_1: 24 RUE LHOMOND city: 75005 PARIS country: FRANCE phone: (33) 1 44 32 33 47 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: HD96675 descr_1: A,112,G,513 pos_1: RA=11H 05M 58.17S +/-.05S, pos_2: DEC=-76D 07' 49." +/-.5" equinox: 2000 pm_or_par: Y pos_epoch_bj: B pos_epoch_yr: 1950.00 ra_pm_val: -0.001533 dec_pm_val: -0.0060 rv_or_z: V = +0 fluxnum_1: 1 fluxval_1: V=7.65 +/-.01 fluxnum_2: 2 fluxval_2: B-V=+0.184 +/- .006 fluxnum_3: 3 fluxval_3: E(B-V)=0.31 +/- 0.03 fluxnum_4: 4 fluxval_4: F-CONT(1265)=5.0 +/-.5 E-11 fluxnum_5: 5 fluxval_5: F-CONT(1338)=6.0 +/-.5 E-11 fluxnum_6: 6 fluxval_6: F-CONT(1462)=7.0 +/-.5 E-11 ! targnum: 2 name_1: HD102065 descr_1: A,112,G,513 pos_1: RA=11H 43M 37.87S +/-.05S, pos_2: DEC=-80D 28' 59.4" +/-.5" equinox: 2000 pm_or_par: Y pos_epoch_bj: B pos_epoch_yr: 1950.00 ra_pm_val: -0.001733 dec_pm_val: -0.0030 rv_or_z: V = +0 fluxnum_1: 1 fluxval_1: V=6.567 +/-.008 fluxnum_2: 2 fluxval_2: B-V=+0.106 +/- .006 fluxnum_3: 3 fluxval_3: E(B-V)=0.17 +/- 0.04 fluxnum_4: 4 fluxval_4: F-CONT(1265)=1.0 +/-.1 E-11 fluxnum_5: 5 fluxval_5: F-CONT(1338)=1.3 +/-.13 E-11 fluxnum_6: 6 fluxval_6: F-CONT(1462)=1.6 +/-.16 E-11 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.100 targname: HD96675 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 time_per_exp: 1.8S priority: 1 param_1: SEARCH-SIZE=3 param_2: BRIGHT=RETURN param_3: LOCATE=DEF req_1: ONBOARD ACQ FOR 1.2-1.4; req_2: CYCLE 2 / 1.1-2.4; ! linenum: 1.200 targname: HD96675 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1265 num_exp: 4 time_per_exp: 17.5M s_to_n: 50 fluxnum_1: 4 priority: 1 param_1: STEP-PATT=5 param_2: FP-SPLIT=STD param_3: COMB=FOUR param_4: DOPPLER=ON req_5: CYCLE 2; ! linenum: 1.300 targname: HD96675 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1338 num_exp: 4 time_per_exp: 17.5M s_to_n: 60 fluxnum_1: 5 priority: 1 param_1: STEP-PATT=5 param_2: FP-SPLIT=STD param_3: COMB=FOUR param_4: DOPPLER=ON req_5: CYCLE 2; ! linenum: 1.400 targname: HD96675 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1462 num_exp: 8 time_per_exp: 17.5M s_to_n: 85 fluxnum_1: 6 priority: 1 param_1: STEP-PATT=5 param_2: FP-SPLIT=STD param_3: COMB=FOUR param_4: DOPPLER=ON req_5: CYCLE 2; ! linenum: 2.100 targname: HD102065 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-A2 time_per_exp: 3.6S priority: 1 param_1: SEARCH-SIZE=3 param_2: BRIGHT=RETURN param_3: LOCATE=DEF req_1: ONBOARD ACQ FOR 2.2-2.4; req_2: CYCLE 2 / 1.1-2.4; ! linenum: 2.200 targname: HD102065 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1265 num_exp: 3 time_per_exp: 11.7M s_to_n: 50 fluxnum_1: 4 priority: 1 param_1: STEP-PATT=5 param_2: FP-SPLIT=STD param_3: COMB=FOUR param_4: DOPPLER=ON req_5: CYCLE 2 ! linenum: 2.300 targname: HD102065 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1338 num_exp: 3 time_per_exp: 11.7M s_to_n: 60 fluxnum_1: 5 priority: 1 param_1: STEP-PATT=5 param_2: FP-SPLIT=STD param_3: COMB=FOUR param_4: DOPPLER=ON req_5: CYCLE 2 ! linenum: 2.400 targname: HD102065 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1462 num_exp: 4 time_per_exp: 17.5M s_to_n: 88 fluxnum_1: 6 priority: 1 param_1: STEP-PATT=5 param_2: FP-SPLIT=STD param_3: COMB=FOUR param_4: DOPPLER=ON req_5: CYCLE 2 ! ! end of exposure logsheet ! No scan data records found