! File: 2581C.PROP ! Database: PEPDB ! Date: 17-FEB-1994:08:39:47 coverpage: title_1: STELLAR WINDS OF MASSIVE STARS IN NEARBY GALAXIES sci_cat: STELLAR ASTROPHYSICS proposal_for: GO pi_title: DR. pi_fname: LUCIANA pi_lname: BIANCHI pi_inst: ASTRONOMICAL OBSERVATORY TORINO pi_country: ITALY pi_phone: ITALY-11-842040 keywords_1: EXTRAGALACTIC STARS, STELLAR WINDS, MASS LOSS, UV, keywords_2: SPECTROSCOPY. hours_pri: 8.00 num_pri: 5 hrs: X pi_position: ASTRONOMER off_fname: A. off_lname: FERRARI off_title: DIRECTOR, PROFESSOR off_inst: ASTRONOMICAL OBSERVATORY OF TORINO off_addr_1: OBSERVATORIO ASTRONOMICO off_addr_2: I-10025 PINO TORINESE (TO) off_phone: 11-842040 off_telex: 213236 TOASTR I ! end of coverpage abstract: line_1: We propose to study the stellar wind characteristics of hot massive stars in line_2: M31 and M33 by observing with the HST-FOS the profiles of UV resonance lines line_3: which are the main wind indicators. The immediate aim is to understand how line_4: mass loss rates, and other characteristics of the stellar winds, such as the line_5: velocity-laws (i.e. the acceleration) and the ionization, depend on line_6: metallicity. The final goal is to understand the evolution of massive stars in line_7: galaxies of different chemical composition. line_8: The dependence of hot star winds on metallicity is in fact predicted by the line_9: theory of radiation-pressure driven winds, but it could be observed so far only line_10: in the MCs stars (Hutchings, 1982; Garmany and Conti 1985; Kudritzski et al, line_11: 1987). In the past years we have pushed IUE to its limits to observe far UV line_12: spectra of the brightest/hottest stars in M31 and M33. In spite of the very low line_13: resolution (insufficent for quantitative line analysis) we observed for all the line_14: stars of our sample significantly lower terminal velocities and weaker P Cygni line_15: profiles than for galactic stars of similar type. line_16: The results of this pioneer study (that involved also an extensive ground based line_17: observing program) on one hand, and the recent significant improvements of the line_18: radiation driven wind theory and treatment of ionization equilibrium in the line_19: stellar atmospheres and envelopes on the other hand, show that a higher line_20: resolution study of the UV lines will be very interesting. ! ! end of abstract general_form_proposers: lname: LAMERS fname: HENNY inst: UTRECHT LABORATORY FOR SPACE RESEARCH country: NETHERLANDS esa: Y ! lname: MASSEY fname: PHILLIP inst: KPNO, NOAO country: USA ! lname: HUTCHINGS fname: JOHN mi: B. inst: DOMINION ASTROPHYSICAL OBSERVATORY country: CANADA ! lname: KUDRITZKI fname: ROLF-PETER inst: MUNICH UNIVERSITY country: FRG esa: Y ! lname: BIANCHI fname: LUCIANA title: P.I. inst: TURIN ASTRONOMICAL OBSERVATORY country: ITALY esa: Y ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We propose to observe some of the stars for which we have IUE spectra line_2: (and therefore we know UV fluxes and can assess line presence) at a line_3: resolution sufficient for quantitative analysis of the broad wind line_4: profiles - to determine mass loss rates- and accurate measurements of line_5: wind terminal velocities, by covering the whole range line_6: where the lines of interest are contained. The resolution is sufficient line_7: to analyze the broad wind lines but also to detect other weaker lines line_8: -that cannot be measured or even detected in IUE spectra. line_9: A S-to-N ratio higher than 20 is required for a good line_10: analysis of the broad profiles. We plan to cover with two line_11: spectra the range from the strong wind line of NV at 1240A line_12: to the photospheric NIII at 1750A. In the original proposal line_13: we asked to use GHRS, but the long exposure times would have line_14: forced us to rebin most spectra by a factor two, to achieve line_15: a S-to-N higher or equal 20 at the wavelenghts of the most line_16: important features. Using the most updated information on line_17: FOS sensitivity, we find that in the time granted to us we line_18: can achieve the S-to-N adequate for our purpose without line_19: rebinning, and the slight degradation of resolution for the line_20: change of instrument is therefore acceptable. ! question: 4 section: 1 line_1: Given the magnitude of the targets (around 17-18th) and the need of high line_2: resolution UV line profiles for the proposed scientific goals, it is evident line_3: that these observations can only be performed with the HST spectrographs. line_4: P.M. has obtained extensive optical observations of selected regions in M33 line_5: and M31, first to identify the most luminous/hottest stars that could be line_6: observed with IUE (grens plates at CFHT, UBV-CCD frames at KPNO 4m tel). line_7: Then spectra of several selected stars were secured at MMTO and low resolution line_8: (6A) spectra with IUE of the hottest ones, allowing line identification and line_9: determination of extinction, eff.Temp., Sp.type, Lbol. These results line_10: -described in Section 2- provided the basis for the proposed research. line_11: The study with low resolution spectra is continuing with IUE and ground-based line_12: telescopes, to extend the object sample, and fainter stars not accessible line_13: with IUE will be observed with the HST-FOS by J.H. (GTO). At high line_14: resolution we ask to observe only the brightest objects, for which we have line_15: analyzed already sufficient low dispersion data (see our references). line_16: High resolution H and He photospheric lines is planned from the ground line_17: (at MMTO or CFHT) though wery difficult, to determine Teff and Gravity line_18: with the improved model atmospheres of R.K. (see Mendez et al.1988), line_19: i.e. in a way independent from our previous results (comparison of UV line_20: continuum with model atmopsheres). This will be a complementary study to line_21: the wind analysis proposed with the HST, as it provides stellar parameters line_22: useful for the unified model. ! question: 5 section: 1 line_1: Most of the stars proposed for HST have already been observed by us with line_2: IUE. Therefore we know the flux level, in the range of interest, with an line_3: accuracy of 10%. From these UV fluxes (quoted in the Target list), the line_4: sensitivity tables in the handbooks and subsequent updates, we line_5: estimated the exposure times listed in the Exposure forms, for the needed line_6: resolution and S-to-N ratio as described in Section 3a. line_7: ( S-to-N better than 20). line_8: By switching to FOS (from the originally approved GHRS) the exposure line_9: times are longer at the shorter wls, and shorter at the longer wls, line_10: but we gain time and efficiency with the acquisitions. ! question: 7 section: 1 line_1: The preliminary data reduction will be done at the ST-ECF and at the line_2: ST ScI. Part of these data reduction packages is already available line_3: and more will be - also at our home institutes. line_4: The scientific analysis will be performed - besides the obvious steps line_5: of line identification, measurements of velocities and equivalent widths- line_6: as described in Section 2. A fit of the line profiles will be done with line_7: codes existing at the Observatory of Torino and SRL Hutrecht that compute line_8: theoretical P Cygni profiles with the SEI method. line_9: The ionization equilibrium will be computed with a detailed model developed line_10: at the Munich Astronomical Institute. A "unified model" fit will also line_11: be done to compute mass loss rate, wind dynamics, abundances and global line_12: stellar parameters for each star consistently (combining also the line_13: optical data). ! question: 8 section: 1 line_1: We have tried - for the Phase II proposal - to measure coordinates line_2: of the targets on GASP frames but most of them are rather faint so line_3: the results are not very accurate, or the gaussian centering fails. line_4: We obtained more precise results by measuring a good KPNO-4m tel. line_5: plate for M31, and a recent CCD frame for M33. The measurements were line_6: reduced using GSS stars as reference stars, and for these we quote line_7: the corresponding Plate-id. in the target list. ! question: 10 section: 1 line_1: We think that we have already available at our home Institutes line_2: the necessary S/W for data reduction, computing facilities and line_3: theoretical codes (on Vaxes and Cray) for the analysis described in line_4: this proposal. Computing capabilities and supporting man-power are line_5: planned to keep expanding in the future years. Students will also line_6: be available to collaborate to this project if needed. Travel funds, line_7: publication costs etc. are already granted to this project, by home line_8: Institutions and Research Foundations of each author's Country. ! !end of general form text general_form_address: lname: BIANCHI fname: LUCIANA title: DR. category: PI inst: ASTRONOMICAL OBSERVATORY OF TORINO addr_1: OSSERVATORIO ASTRONOMICO addr_2: I-10025 PINO TORINESE (TO) country: ITALY ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: M31-NGC206-231 descr_1: EXT-STAR; WN OF STAR pos_1: PLATE-ID=2801, pos_2: RA = 0H 37M 46.25S +/- 0.05S, pos_3: DEC = +40D 28' 2.6" +/- 0.3" equinox: 1950.0 pos_epoch_yr: 1980.00 comment_1: TARGET COORDINATES MEASURED ON comment_2: GOOD 4M-TEL PLATE USING GSS comment_3: REFERENCE STARS FROM QUOTED comment_4: GSS-FRAMES (PLATE-ID) comment_5: TARGET TOO FAINT ON GASP FRAME comment_6: CNTRTS=230 CALC'D W OLD TBLE 4.2 comment_7: AND OLD FORMULA (THE ONLY AVAIL) fluxnum_1: 1 fluxval_1: V = 18.6 , B-V = -0.03 fluxnum_2: 2 fluxval_2: F-CONT(1300) = 0.6 E-14 fluxnum_3: 3 fluxval_3: F-CONT(1550) = 0.4 E-14 fluxnum_4: 4 fluxval_4: TYPE = WN7 fluxnum_5: 5 fluxval_5: F-CONT(1240) = 0.7 E-14 ! targnum: 2 name_1: M31-OB78-277 descr_1: EXT-STAR; TYPE = B1 pos_1: PLATE-ID =2801, pos_2: RA = 0H 37M 46.83S +/- 0.05S, pos_3: DEC = +40D 26' 5.7" +/- 0.3" equinox: 1950.0 pos_epoch_yr: 1980.00 comment_1: TARGET COORDINATES MEASURED ON comment_2: GOOD 4M-TEL PLATE USING GSS comment_3: REFERENCE STARS FROM PLATE QUOTED comment_5: TARGET TOO WEAK ON GASP FRAME comment_6: CNTRTS=614 CALC'D W OLD TBLE 4.2 comment_7: AND OLD FORMULA (THE ONLY AVAIL) fluxnum_1: 1 fluxval_1: V = 17.4 , B-V = -0.06 fluxnum_2: 2 fluxval_2: F-CONT(1300) = 1.3 E-14 fluxnum_3: 3 fluxval_3: F-CONT(1550) = 1.0 E-14 fluxnum_4: 4 fluxval_4: TYPE = B1 fluxnum_5: 5 fluxval_5: F-CONT(1240) = 2.0 E-14 ! targnum: 3 name_1: M31-OB48-444 descr_1: EXT-STAR; TYPE = O8 pos_1: PLATE-ID=2805, pos_2: RA = 0H 42M 30.32S +/- 0.05S, pos_3: DEC = +41D 21' 23.9" +/- 0.3" equinox: 1950.0 pos_epoch_yr: 1980.00 comment_1: TARGET COORDINATES MEASURED ON comment_2: GOOD 4M-TEL PLATE USING GSS comment_3: REFERENCE STARS FROM PLATE QUOTED comment_5: TARGET TOO WEAK ON GASP FRAME comment_6: CNTRTS=77 CALC'D W OLD TBLE 4.2 comment_7: AND OLD FORMULA (THE ONLY AVAIL) fluxnum_1: 1 fluxval_1: V = 19.1 , B-V = -0.02 fluxnum_2: 2 fluxval_2: TYPE = O8 fluxnum_3: 3 fluxval_3: F-CONT(1300) = 0.4 E-14 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: M31-NGC206-231 config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G130H wavelength: 1150-1608 num_exp: 1 time_per_exp: 89.08M s_to_n: 25 fluxnum_1: 2,5 priority: 1 req_1: CYCLE1/1-12 ! linenum: 2.000 targname: M31-NGC206-231 config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G190H wavelength: 1595-2282 num_exp: 1 time_per_exp: 23M s_to_n: 22 fluxnum_1: 3 priority: 1 req_1: CYCLE1/1-12 ! linenum: 3.000 targname: M31-NGC206-231 config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G270H wavelength: 2227-3306 num_exp: 1 time_per_exp: 7M s_to_n: 25 priority: 1 req_1: CYCLE1/1-12 ! linenum: 4.000 targname: M31-OB78-277 config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G130H wavelength: 1150-1608 num_exp: 1 time_per_exp: 101M s_to_n: 25 fluxnum_1: 2,5 priority: 1 req_1: CYCLE1/1-12 ! linenum: 5.000 targname: M31-OB78-277 config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G190H wavelength: 1595-2282 num_exp: 1 time_per_exp: 13M s_to_n: 24 fluxnum_1: 3 priority: 1 req_1: CYCLE1/1-12 ! linenum: 6.000 targname: M31-OB78-277 config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G270H wavelength: 2227-3306 num_exp: 1 time_per_exp: 7M s_to_n: 24 priority: 1 req_1: CYCLE1/1-12 ! linenum: 7.000 targname: M31-OB48-444 config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G130H wavelength: 1150-1608 num_exp: 1 time_per_exp: 123M s_to_n: 25 fluxnum_1: 1,2 priority: 1 req_1: CYCLE1/1-12 ! linenum: 8.000 targname: M31-OB48-444 config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G190H wavelength: 1595-2282 num_exp: 1 time_per_exp: 22M s_to_n: 24 fluxnum_1: 1,2 priority: 1 req_1: CYCLE1/1-12 ! linenum: 9.000 targname: M31-OB48-444 config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G270H wavelength: 2227-3306 num_exp: 1 time_per_exp: 7M s_to_n: 25 priority: 1 req_1: CYCLE1/1-12 ! linenum: 10.000 targname: M31-NGC206-231 config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 60.0S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 1-3; req_2: CYCLE1/1-12 comment_1: TEN TIMES THE EXP TIME FROM comment_2: TABLE 2 PAGE 10 OF HANDBOOK; ! linenum: 11.000 targname: M31-OB78-277 config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 20.0S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 4-6; req_2: CYCLE1/1-12 comment_1: TEN TIMES THE EXP TIME FROM comment_2: TABLE 2 PAGE 10 OF HANDBOOK; ! linenum: 12.000 targname: M31-OB48-444 config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 96.0S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 7-9; req_2: CYCLE1/1-12 comment_1: TEN TIMES THE EXP TIME FROM comment_2: TABLE 2 PAGE 10 OF HANDBOOK; ! ! end of exposure logsheet ! No scan data records found