! $Id: 5422,v 6.1 1994/07/27 17:46:36 pepsa Exp $ coverpage: title_1: NEUTRAL GAS IN BLUE COMPACT GALAXIES: title_2: POPULATION III OR RECENT POLLUTION\? sci_cat: GALAXIES & CLUSTERS sci_subcat: GAS & DUST proposal_for: GO pi_fname: DANIEL pi_mi: R pi_lname: KUNTH pi_inst: 5436 pi_country: FRANCE pi_phone: 33-1-43201425 hours_pri: 14.93 num_pri: 3 hrs: Y off_fname: ALAIN off_lname: OMONT off_title: DIRECTOR off_inst: 5436 off_addr_1: 98BIS BOULEVARD ARAGO off_city: PARIS off_zip: 75014 off_country: FRANCE off_phone: 33-1-43201425 ! end of coverpage abstract: line_1: Using GHRS we have recently obtained the striking evidence that the line_2: neutral HI gas in the very metal-poor dwarf galaxy IZw 18 contains line_3: oxygen but with very low abundance (roughly 10(-3) times the solar line_4: value). Moreover this result shows that the HI is more metal deficient line_5: than the nebular gas by a factor of a least 20. If this oxygen had been line_6: formed by past star formation episodes, only one of such bursts would line_7: be required to form all the metals which would have been subsequently line_8: dispersed in the HI gas. Alternatively there is the possibility that line_9: metals observed in the HI gas were produced in a pre-galactic era via line_10: a population III generation. We propose to test this idea by observing line_11: a set of 3 blue compact galaxies with different metallicities line_12: (obtained from the HII regions) using the GHRS and the LSA around the line_13: Lyman-ALPHA and the OI lambda 1302 regions. We wish to investigate line_14: whether the metallicity of the neutral gas is correlated with that of line_15: the HII regions, hence giving constraints on the star formation history line_16: in these galaxies. The absence of correlation would favor the population line_17: III hypothesis. We also expect to catch Galactic high velocity clouds line_18: along the line of sight of one of our targets and thus constrain their line_19: origin from the derivation of their metal abundances. ! ! end of abstract general_form_proposers: lname: KUNTH fname: DANIEL mi: R inst: 5436 country: FRANCE esa: Y ! lname: LEQUEUX fname: JAMES inst: 5468 country: FRANCE esa: Y ! lname: MAS-HESSE fname: MIGUEL inst: LABORATORIO DE ASTROFISICA ESPACIAL Y FISICA FUNDAMENTAL country: SPAIN esa: Y ! lname: SARGENT fname: WALLACE mi: L inst: 1590 country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We propose to observe 3 Blue Compact Galaxies using the following line_2: instrumental configuration: GHRS + LSA + G160M centered at 1215 and line_3: 1300 A. Under this configuration the GHRS provides ~0.28 A resolution line_4: (assuming binning over 4 diodes) in a wavelength range of 34 A. We line_5: plan to take two exposures per target with the grating centered at line_6: around 1215 A and 1300 A, respectively, dividing each one in line_7: sub-exposures around 5 minutes long. In this way we will be able to line_8: measure the Lyman-ALPHA (1216 A), OI (1302 A) and SiII (1304 A) lines. line_9: By fitting theoretical profiles to the Lyman-ALPHA absorption line it line_10: will be possible to derive the neutral hydrogen column density along line_11: the line of sight. As a by-product we will have the opportunity to line_12: analyze in detail if Lyman-ALPHA appears in emission in these line_13: galaxies. By measuring the equivalent widths of the OI and SiII line_14: absorption lines we will derive their column densities and hence their line_15: abundance relative to hydrogen. The redshifts of the selected line_16: galaxies are high enough to disentangle between Galactic and line_17: intrinsic absorption lines. All the objects have already been observed line_18: with IUE through the 10"x20" aperture in low resolution. They are line_19: compact (UV emission extended over around 5"x5") and peaked at the line_20: center. We plan to use the flux coming from the star-forming regions line_21: to probe the neutral gas in front of the galaxies. Therefore the exact line_22: pointing is not critical, and a tolerance of +/- 1" would be line_23: acceptable. ! question: 3 section: 2 line_1: The coordinates provided correspond to the brightest pixel measured on line_2: the digitized PSS scans with GASP. The intrinsic absorption is low, so line_3: that a good correlation between optical and UV flux is expected. We line_4: plan to acquire the targets by onboard acquisitions with the line_5: BRIGHT=RETURN option. We have selected a search size of 3 for the most line_6: compact objects, and 5 to avoid problems with UGC5720, which is a bit line_7: more extended. The corresponding STEP-TIMES have been estimated from line_8: the known optical-UV spectral energy distributions, temptatively line_9: scaled down to the LSA size. This observational strategy has been line_10: already used with success in IZw18. ! question: 4 section: 1 line_1: All the targets have been observed with IUE at low resolution. The line_2: resolution is too poor to even disentangle the galactic from the line_3: redshifted lines.This discrimination may also be difficult with the FOS, line_4: hence our choice of the GHRS. Only a depression in the continum is noted line_5: with IUE around lambda 1300 but the overall signal to noise is too small. line_6: The analysis of the Lyman-ALPHA region with IUE is hampered by the line_7: geocoronal line. In most of the cases the GHRS instrumental profiles line_8: will be wider than the intrinsic absorption lines, so that the dispersion line_9: velocity of the gas can not be measured directly. Since most of the lines line_10: will be located on the saturated range of the curve of groth, knowledge line_11: of the dispersion velocity is needed to properly derive the line_12: corresponding column densities. To circumvent this difficulty we will line_13: use VLA observations of the targets or apply for VLA time in order to line_14: derive the velocity dispersion in the HI cloud: we have already line_15: used successfully this method for IZW 18.In the infrared K line_16: imaging and spectroscopy will be performed at the CFHT and La Palma line_17: in order to have an independant study of the past star-formation on line_18: these objects. ! question: 5 section: 1 line_1: The proposed observations are neither real-time nor time critical and line_2: can be performed in any temporal order. The expected countrate during line_3: acquisition might be of the same order than the contribution due to line_4: geocoronal Lyman-ALPHA. Furthermore, strong geocoronal Lyman-ALPHA line_5: emission could hamper the detection of intrinsic Lyman-ALPHA emission, line_6: although this should appear 2-5 A redshifted. We have therefore line_7: requested DARK-TIME both for acquisition and for execution of the line_8: observations with the grid centered at 1215 A. ! question: 6 section: 1 line_1: the standard GHRS calibration would fulfill our requirements. ! ! question: 8 section: 1 line_1: The efficiency in using HST resources in the proposed way (78%) is very line_2: high, obtaining an important scientific return with low loss of line_3: spacecraft time. ! question: 9 section: 1 line_1: GO Program: 2078 line_2: Title: A Search for Primordial Gas: is I Zw 18 a Young Galaxy? line_3: PI,Co-Is: J. Lequeux,D. Kunth, W. Sargent and F. Viallefond line_4: GO Program: 2424 line_5: Title: Quasar Absorption Line Survey line_6: PI,Co-Is: J. Bahcall, W. Sargent (plus some other investigators) line_7: GO Program: 3810 line_8: Title: The Stellar Population of Wolf-Rayet Galaxies line_9: PI,Co-Is: P. Conti, W. Sargent (plus some other investigators) line_10: GO Program: 3507 line_11: Title: Ultra-violet Spect. and High-Resolution Imaging of 4395 line_12: PI,Co-Is: A. Filippenko, W. Sargent line_13: GO Program: 3746 line_14: Title: The cooling of the local diffuse interstellar matter line_15: PI,Co-Is: C. Gry, J. Lequeux (plus some other investigators) line_16: GO Program: 3759 line_17: Title: Dust, molecular, atomic composition etc... line_18: PI,Co-Is: F. Boulanger, J. Lequeux (plus some other investigators) line_19: GO Program: 3589 line_20: Title: Parallel high-resolution imaging of diff. obj. in the MCs line_21: PI,Co-Is: J. Walsh, J. Lequeux (plus some other investigators) ! question: 9 section: 2 line_1: Related: id=2078. Completed. Paper submitted to A&A. HI gas in IZw 18 line_2: contains a very small, but not null, abundance of heavy elements and may line_3: be either primeval with enrichment by Population III or enriched by line_4: previous star formation. line_5: "HST Observations of NGC 4395, the Least Luminous Seyfert 1 Nucleus: line_6: Evidence Against the Starburst Hypothesis for Broad-Lined Active line_7: Galactic Nuclei." A. V. Filippenko, L. C. Ho, and W. L. W. Sargent; line_8: Astrophysical Journal (Letters), in press (June 20, 1993 issue). line_9: "The HST Quasar Absorption Line Key Project I. First Observational line_10: results, Including Lyman-ALPHA and Lyman Limit Systems." J. Bahcall line_11: and 11 other authors; Ap. J.; 000; 000,; 1993 (in press) line_12: "The HST Quasar Absorption Line Key Project II. Data Calibration and line_13: Absorption Line Selection."; D. Schneider and 11 other authors; Ap. J line_14: .; 000; 000,; 1993 (in press). line_15: "The HST Quasar Absorption Line Key Project III. First Observational line_16: Results on the Milky way Gas." B. Savage and 13 other authors; Ap. J.; line_17: 000; 000,; 1993 (in press). ! question: 10 section: 1 line_1: All the participants have free access to the scientific infrastructure line_2: of their respective institutes, including data-analysis facilities line_3: already available, libraries, electronic networks and so on. They are line_4: also financially supported by the corresponding institutions and can line_5: dedicate all the time needed to the completion of this research line_6: programme. ! !end of general form text general_form_address: lname: KUNTH fname: DANIEL mi: R category: PI inst: 5436 addr_1: 98BIS BOULEVARD ARAGO city: PARIS zip: 75014 country: FRANCE phone: 33-1-43201425 telex: 205671 IAU F / KUNTH@IAP.FR ! lname: category: CON ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: UGC5720 name_2: HARO2 name_3: GSC03816-00902 descr_1: E, 307 pos_1: RA = 10H 32M 31.83S +/- 0.02S, pos_2: DEC = +54D 24' 3.5" +/- 0.2" equinox: J2000.0 rv_or_z: V = +1461 acqpr_1: EXT comment_1: CONTINUUM FLUXES THROUGH 2"X2" comment_2: APERTURE fluxnum_1: 1 fluxval_1: V = 13.0 +/- 0.2 fluxnum_2: 1 fluxval_2: B-V = 0.36 +/- 0.4 fluxnum_3: 2 fluxval_3: E(B-V) = 0.20 +/- 0.05 fluxnum_4: 3 fluxval_4: F-CONT(1300) = 60 +/- 6 E-15 fluxnum_5: 4 fluxval_5: F-CONT(1215) = 67 +/- 7 E-15 fluxnum_6: 5 fluxval_6: F-CONT(5500) = 34 +/- 4 E-16 ! targnum: 2 name_1: UGC9560 name_2: IIZW 70 name_3: GSC02561-00455 descr_1: E, 307 pos_1: RA = 14H 50M 56.50S +/- 0.02S, pos_2: DEC = +35D 34' 17.8" +/- 0.2" equinox: J2000.0 rv_or_z: V = +1218 acqpr_1: EXT comment_1: CONTINUUM FLUXES THROUGH 2"X2" comment_2: APERTURE fluxnum_1: 1 fluxval_1: V = 14.6 +/- 0.1 fluxnum_2: 1 fluxval_2: B-V = 0.26 +/- 0.6 fluxnum_3: 2 fluxval_3: E(B-V) = 0.05 +/- 0.05 fluxnum_4: 3 fluxval_4: F-CONT(1300) = 40 +/- 4 E-15 fluxnum_5: 4 fluxval_5: F-CONT(1215) = 36 +/- 4 E-15 fluxnum_6: 5 fluxval_6: F-CONT(5500) = 10 +/- 1 E-16 ! targnum: 3 name_1: MRK36 name_2: HARO4 descr_1: E, 307 pos_1: RA = 11H 4M 58.38S +/- 0.05S, pos_2: DEC = +29D 8' 15.2" +/- 0.5" equinox: J2000.0 rv_or_z: V = +646 acqpr_1: EXT comment_1: CONTINUUM FLUXES THROUGH 2"X2" comment_2: APERTURE fluxnum_1: 1 fluxval_1: V = 15.4 +/- 0.2 fluxnum_2: 1 fluxval_2: B-V = 0.28 +/- 0.4 fluxnum_3: 2 fluxval_3: E(B-V) = 0.05 +/- 0.05 fluxnum_4: 3 fluxval_4: F-CONT(1300) = 20 +/- 3 E-15 fluxnum_5: 4 fluxval_5: F-CONT(1215) = 26 +/- 3 E-15 fluxnum_6: 5 fluxval_6: F-CONT(5500) = 3.0 +/- 0.3 E-16 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: UGC5720 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 250S s_to_n: 30 s_to_n_time: 10S fluxnum_1: 1 fluxnum_2: 2 fluxnum_3: 3 fluxnum_4: 5 priority: 3 param_1: BRIGHT=RETURN, param_2: SEARCH-SIZE=5, param_3: LOCATE=YES, req_1: CYCLE 4; req_2: ONBOARD ACQ FOR 2-3; comment_1: 10000 CTS EXPECTED IN STEP-TIME=10S. ! linenum: 2.000 targname: UGC5720 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1210-1240 num_exp: 6 time_per_exp: 20M s_to_n: 11 s_to_n_time: 120M fluxnum_1: 4 priority: 3 param_1: STEP-PATT=DEF, param_2: FP-SPLIT=FOUR, param_3: DOPPLER=ON, req_1: CYCLE 4; req_2: DARK TIME; req_3: GROUP 2-3 NO GAP; comment_1: S/N FOR CONTINUUM PER DIODE. ! linenum: 3.000 targname: UGC5720 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1290-1320 num_exp: 4 time_per_exp: 22M s_to_n: 13 s_to_n_time: 88M fluxnum_1: 3 priority: 3 param_1: STEP-PATT=DEF, param_2: FP-SPLIT=FOUR, param_3: DOPPLER=ON, req_1: CYCLE 4; comment_1: S/N FOR CONTINUUM PER DIODE. ! linenum: 4.000 targname: UGC9560 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 500S s_to_n: 30 s_to_n_time: 20S fluxnum_1: 1 fluxnum_2: 2 fluxnum_3: 3 fluxnum_4: 5 priority: 1 param_1: BRIGHT=RETURN, param_2: SEARCH-SIZE=5, param_3: LOCATE=YES, req_1: CYCLE 4; req_2: ONBOARD ACQ FOR 5-6; comment_1: 10000 CTS EXPECTED IN STEP-TIME=20S. ! linenum: 5.000 targname: UGC9560 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1210-1240 num_exp: 4 time_per_exp: 20M s_to_n: 8 s_to_n_time: 140M fluxnum_1: 4 priority: 1 param_1: STEP-PATT=DEF, param_2: FP-SPLIT=DSFOUR, param_3: DOPPLER=ON, req_1: CYCLE 4; req_2: DARK TIME; req_3: GROUP 5-6 NO GAP; comment_1: S/N FOR CONTINUUM PER DIODE. ! linenum: 5.100 targname: UGC9560 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1210-1240 num_exp: 3 time_per_exp: 20M s_to_n: 8 s_to_n_time: 140M fluxnum_1: 4 priority: 1 param_1: STEP-PATT=DEF, param_2: FP-SPLIT=DSFOUR, param_3: DOPPLER=ON, req_1: CYCLE 4; req_2: DARK TIME; req_3: GROUP 5-6 NO GAP; comment_1: S/N FOR CONTINUUM PER DIODE. ! linenum: 6.000 targname: UGC9560 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1290-1320 num_exp: 6 time_per_exp: 21M s_to_n: 12 s_to_n_time: 126M fluxnum_1: 3 priority: 1 param_1: STEP-PATT=DEF, param_2: FP-SPLIT=FOUR, param_3: DOPPLER=ON, req_1: CYCLE 4; comment_1: S/N FOR CONTINUUM PER DIODE. ! linenum: 7.000 targname: MRK36 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 750S s_to_n: 30 s_to_n_time: 30S fluxnum_1: 1 fluxnum_2: 2 fluxnum_3: 3 fluxnum_4: 5 priority: 2 param_1: BRIGHT=RETURN, param_2: SEARCH-SIZE=5, param_3: LOCATE=YES, req_1: CYCLE 4; req_2: ONBOARD ACQ FOR 8-9.1; comment_1: 10000 CTS EXPECTED IN STEP-TIME=30S. ! linenum: 8.000 targname: MRK36 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1210-1240 num_exp: 5 time_per_exp: 21M s_to_n: 8 s_to_n_time: 210M fluxnum_1: 4 priority: 2 param_1: STEP-PATT=DEF, param_2: FP-SPLIT= FOUR, param_3: DOPPLER=ON, req_1: CYCLE 4; req_2: DARK TIME; req_3: GROUP 8-9.1 NO GAP; comment_1: S/N FOR CONTINUUM PER DIODE. ! linenum: 8.100 targname: MRK36 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1210-1240 num_exp: 5 time_per_exp: 21M s_to_n: 8 s_to_n_time: 210M fluxnum_1: 4 priority: 2 param_1: STEP-PATT=DEF, param_2: FP-SPLIT= FOUR, param_3: DOPPLER=ON, req_1: CYCLE 4; req_2: DARK TIME; req_3: GROUP 8-9 NO GAP; comment_1: S/N FOR CONTINUUM PER DIODE. ! linenum: 9.000 targname: MRK36 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1285-1315 num_exp: 5 time_per_exp: 20M s_to_n: 10 s_to_n_time: 200M fluxnum_1: 3 priority: 2 param_1: STEP-PATT=DEF, param_2: FP-SPLIT=FOUR, param_3: DOPPLER=ON, req_1: CYCLE 4; comment_1: S/N FOR CONTINUUM PER DIODE. ! linenum: 9.100 targname: MRK36 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1285-1315 num_exp: 5 time_per_exp: 20M s_to_n: 10 s_to_n_time: 200M fluxnum_1: 3 priority: 2 param_1: STEP-PATT=DEF, param_2: FP-SPLIT=FOUR, param_3: DOPPLER=ON, req_1: CYCLE 4; comment_1: S/N FOR CONTINUUM PER DIODE. ! ! end of exposure logsheet ! No scan data records found