! $Id: 5339,v 5.1 1994/07/27 16:50:25 pepsa Exp $ coverpage: title_1: CENTRAL STARS OF PLANETARY NEBULAE: A TEST OF THE title_2: RADIATIVELY DRIVEN WIND THEORY: CYCLE4 MEDIUM sci_cat: HOT STARS sci_subcat: SUBDWARFS proposal_for: GO pi_fname: ROBERTO pi_lname: MENDEZ pi_inst: 5588 pi_country: GERMANY pi_phone: +49-89-92209442 hours_pri: 0.63 num_pri: 1 fos: Y off_fname: ROLF-PETER off_lname: KUDRITZKI off_title: DIRECTOR off_inst: 5588 off_addr_1: INSTITUT F ASTRON U ASTROPHYS DER UNIVERSITAET MUENCHEN off_addr_2: SCHEINERSTRASSE 1 off_addr_3: 81679 MUENCHEN off_city: MUNICH off_country: GERMANY off_phone: +49-89-92209422 ! end of coverpage abstract: line_1: We propose to test the radiatively driven wind theory for central stars line_2: of planetary nebulae (CSPN). The test is interesting because CSPN differ line_3: substantially from the luminous and massive Pop.I stars. There is a clear line_4: discrepancy between spectroscopic+wind masses versus evolutionary masses line_5: of Pop.I OB stars. The result of the CSPN test would help to decide which line_6: masses need correction, with obvious impact on stellar atmosphere and line_7: stellar evolution theory. A well-tested and confirmed wind theory would line_8: become a powerful tool for stellar spectroscopic mass, radius, distance line_9: and luminosity determinations throughout the Local Group. In order to line_10: make this test with maximum efficiency we have selected a sample of line_11: CSPN with temperatures similar to those of Pop.I OB stars and showing line_12: a variety of wind strengths. We wish to obtain high S/N ultraviolet line_13: spectrograms with HST+FOS. Our list of CSPN necessarily includes faint line_14: and reddened objects which can only be observed with HST. FOS spectra line_15: in the range from 1150 to 2300 Angstroms, combined with existing high line_16: resolution optical data, will provide reliable values of Teff, log g, line_17: photospheric abundances and mass loss rates, using sophisticated NLTE line_18: "unified" models and NLTE metal line formation calculations including line_19: wind effects. This input will be used to predict, from wind models, the line_20: P Cygni profiles of UV resonance lines, to be compared with the observed ones. ! ! end of abstract general_form_proposers: lname: MENDEZ fname: ROBERTO inst: 5588 country: GERMANY esa: Y ! lname: KUDRITZKI fname: ROLF-PETER inst: 5588 country: GERMANY esa: Y ! lname: GABLER fname: RUDI inst: 5588 country: GERMANY esa: Y ! lname: BUTLER fname: KEITH inst: 5588 country: GERMANY esa: Y ! lname: BECKER fname: SYLVIA inst: 5588 country: GERMANY esa: Y ! lname: PAULDRACH fname: ADI inst: 5588 country: GERMANY esa: Y ! lname: PULS fname: JOACHIM inst: 5588 country: GERMANY esa: Y ! lname: LENNON fname: DANIEL inst: 5588 country: GERMANY esa: Y ! lname: HUSFELD fname: DIRK inst: 5588 country: GERMANY esa: Y ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We will observe the central star of the planetary nebula He 2-108. line_2: This star has a Teff of 33000 K and a strong wind, as indicated line_3: by the presence of emission at the wind-sensitive stellar line line_4: He II 4686. The V magnitude is 12.7, and E(B-V) = 0.4. We can take line_5: one spectrogram of this star, using the FOS and the blue detector line_6: with grating G130H. The S/N ratio must be at least 70. line_7: The spectral coverage will run from 1150A to 1600A and line_8: will contain all the important wind lines needed for our analysis: line_9: NV 1239,1243; CII 1334,1336; SiIV 1394,1403; CIV 1548,1551; line_10: plus a large number of photospheric lines due to Fe and Ni. line_11: The resolution of FOS (approximately 200 km/s) is not a problem line_12: for the analysis of the wind features. The photospheric line line_13: spectrum suffers from such blending problems that spectral synthesis line_14: techniques are necessary to derive abundances in any case. line_15: A very high S/N ratio is essential for such studies. ! question: 4 section: 1 line_1: The UV spectrum is essential for our analysis, because it provides line_2: crucial information about the atmosphere and wind of our object. The UV line_3: stellar wind lines provide estimates of Vinfinity, and their profiles line_4: will be compared with the predicted ones in the last step of the line_5: analysis. The iron group elements do not show adequate optical lines for line_6: an abundance analysis, but have a rich UV spectrum. Several UV lines line_7: will be useful for ionization equilibrium studies which will provide line_8: additional constraints on the stellar Teff. Our object is too faint and line_9: reddened to be observed with IUE at the required signal-to-noise ratio. line_10: HST/FOS observations are therefore necessary for this project. line_11: In the last 5 years we have published a number of papers on the NLTE line_12: model atmosphere analysis of CSPN, based on high-resolution optical line_13: spectrograms obtained with the ESO 3.6m telescope and the INT line_14: telescope at La Palma, Canary Islands. In particular our target in line_15: this proposal has already been observed from a ground-based observatory line_16: at high spectral resolution, and the corresponding first-step line_17: (plane-parallel, hydrostatic) NLTE model atmosphere study has been line_18: made. We have estimated the HST/FOS exposure time using observed UV line_19: stellar fluxes (IUE low-resolution spectra). The requested signal to line_20: noise ratio (at least 70) is based upon previous experience gained line_21: with this instrumentation and is necessary to enable us to measure line_22: terminal velocities, by fitting the wind lines, to within 150 km/s line_23: and for the synthesis of line blends in the UV. ! question: 5 section: 1 line_1: No special scheduling requirements. ! question: 6 section: 1 line_1: No special calibrations required. ! ! ! question: 8 section: 1 line_1: No additional comments. ! question: 9 section: 1 line_1: GTO No. 1215 ULTRAVIOLET SPECTRAL ATLAS OF O-STARS IN THE MILKY WAY AND line_2: MAGELLANIC CLOUDS (RPK). line_3: GO No. 2233/4110 THE PHYSICS OF MASSIVE O-STARS IN DIFFERENT PARENT line_4: GALAXIES (RPK, KB, DH, AP, JP). line_5: GO No. 2581 STELLAR WINDS OF MASSIVE STARS IN NEARBY GALAXIES (RPK). line_6: GO No. 4550 MASSIVE STAR EVOLUTION FROM CARBON AND OXYGEN ABUNDANCES line_7: IN LMC WC STARS (RPK, KB, DJL). line_8: The present proposal is not directly related to any of the above line_9: proposals except in so far as it concerns the same general topic of line_10: quantitative spectroscopy of hot stars. The present proposal is line_11: specifically aimed at the analysis of central stars of planetary line_12: nebulae, a problem none of the above proposals deals with. line_13: GTO proposal 1215 and GO proposal 2581 are completed and results line_14: have been published in the literature (see below for examples). GO line_15: proposals 2233/4110 and 4550 are incomplete. The former still has line_16: observations of 4 early O-stars in the SMC outstanding which are line_17: crucial to interpretation of the metallicity dependence of mass loss line_18: rates in the galaxy, LMC and SMC. Nevertheless preliminary results line_19: for some stars have been published. To date no data for line_20: proposal 4550 have been obtained. ! question: 9 section: 2 line_1: (1) First Results from the GHRS: Spectroscopic determination of stellar line_2: parameters of an O3f star, Melnick 42, in the Large Magellanic Cloud: line_3: Heap, S.R., Altner, B., Ebbets, D., Hubeny, I., Hutchings, J.S., line_4: Kudritzki, R.P. Voels, S.A., Haser, S., Pauldrach, A., Puls, J., line_5: Butler, K., 1991., Ap. J. Let., 377, L29. line_6: (2) Hot stars and the Hubble Space Telescope: line_7: Kudritzki, R.P., Lennon, D.J. Becker, S.R., Butler, K., Gabler, R., line_8: Haser, S., Husfeld, D., Pauldrach, A., Puls, J., Voels, S., 1993, line_9: in: Science with the Hubble Space Telescope, line_10: ESO Wokshop and Conference Series No 44, p279. line_11: (3) The stellar wind of an O8.5Ia(f) stars in M31 - no evidence for line_12: abnormally low mass loss: Haser, S.M., Lennon, D.J., Kudritzki, R.P., line_13: Puls, J., Astron. Astrophys., submitted, 1993. line_14: (4) Radiation driven winds of hot stars. XII. A first step towards line_15: detailed UV line diagnostics of O-stars: Pauldrach, A.W.A., Kudritzki, line_16: R.P., Puls, J., Butler, K., Hunsinger, J., Astron. Astrophys., line_17: in press, 1993. line_18: (5) Quantitative spectroscopy of O-stars in the Magellanic Clouds. II. line_19: The O3 stars Sk-67 211 and Sk-68 137 in the LMC: Husfeld, D., Lennon, line_20: D.J., Kudritzki, R.-P., Gabler, R., Pauldrach, A.W.A., Puls, J., Voels, line_21: S., Conti, P.S., Wachter, S., Astron. Astrophys. in press. 1993. ! question: 10 section: 1 line_1: Munich University: data reduction and analysis facilities and personnel line_2: are described under section 7. There are no problems with the funding line_3: of the necessary computer calculations required for this project. line_4: Funds for travel, preparation of observations, reduction, etc will also line_5: be available. ! !end of general form text general_form_address: lname: MENDEZ fname: ROBERTO category: PI inst: 5588 addr_1: INSTITUT F ASTRON U ASTROPHYS DER UNIVERSITAET MUENCHEN addr_2: SCHEINERSTRASSE 1 addr_3: 81679 MUENCHEN city: MUNICH country: GERMANY phone: +49-89-92209442 telex: MENDEZ@USM.UNI-MUENCHEN.DE ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: PK316+8D1 name_2: HE2-108 name_3: GSC8289-00125 descr_1: A,184 pos_1: PLATE-ID=039T, pos_2: RA = 14H 18M 8.79S +/- 0.1S, pos_3: DEC = -52D 10' 39.7" +/- 0.2" equinox: 2000 rv_or_z: V = -8 fluxnum_1: 1 fluxval_1: V=12.7,B-V=0.1,E(B-V)=0.4 fluxnum_2: 2 fluxval_2: F-CONT(1400) = 15 +/- 3 E-14 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: PK316+8D1 config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: G190H num_exp: 1 time_per_exp: 5S fluxnum_1: 2 priority: 1 param_1: SCAN-STEP-Y=1.204, param_2: SEARCH-SIZE-X=1, param_3: SEARCH-SIZE-Y=3, req_1: ONBOARD ACQ FOR 2; req_2: CYCLE 4 / 1-5; ! linenum: 2.000 targname: PK316+8D1 config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: G190H num_exp: 1 time_per_exp: 6S fluxnum_1: 2 priority: 1 param_1: SCAN-STEP-X=0.602, param_2: SCAN-STEP-Y=0.602, param_3: SEARCH-SIZE-X=6, param_4: SEARCH-SIZE-Y=2, req_1: ONBOARD ACQ FOR 3; ! linenum: 3.000 targname: PK316+8D1 config: FOS/BL opmode: ACQ/PEAK aperture: 0.3 sp_element: G190H num_exp: 1 time_per_exp: 7S fluxnum_1: 2 priority: 1 param_1: SCAN-STEP-X=0.172, param_2: SCAN-STEP-Y=0.172, param_3: SEARCH-SIZE-X=5, param_4: SEARCH-SIZE-Y=5, req_1: ONBOARD ACQ FOR 4; ! linenum: 4.000 targname: PK316+8D1 config: FOS/BL opmode: ACQ/PEAK aperture: 0.3 sp_element: G190H num_exp: 1 time_per_exp: 7.0S fluxnum_1: 2 priority: 1 param_1: SCAN-STEP-X=0.052, param_2: SCAN-STEP-Y=0.052, param_3: SEARCH-SIZE-X=5, param_4: SEARCH-SIZE-Y=5, req_1: ONBOARD ACQ FOR 5; ! linenum: 5.000 targname: PK316+8D1 config: FOS/BL opmode: ACCUM aperture: 0.3 sp_element: G130H num_exp: 1 time_per_exp: 2280.0S s_to_n: 70 fluxnum_1: 2 priority: 1 ! ! end of exposure logsheet ! No scan data records found