! File: 4494C.PROP ! Database: PEPDB ! Date: 22-FEB-1994:14:42:57 coverpage: title_1: SYMBIOTIC SYSTEMS IN THE MAGELLANIC CLOUDS title_2: CYC3 MEDIUM sci_cat: HOT STARS sci_subcat: ERUPTIVE BINARIES proposal_for: GO pi_fname: MANFRED pi_lname: VOGEL pi_inst: ETH ZURICH pi_country: SWITZERLAND hours_pri: 10.20 num_pri: 6 fos: Y off_fname: JAN off_lname: STENFLO off_title: HEAD OF INSTITUTE off_inst: 7820 off_addr_1: ETH ZENTRUM off_city: 8092 ZURICH off_country: SWITZERLAND off_phone: 41-1-256 3804 ! end of coverpage abstract: line_1: We propose FOS observations of line_2: symbiotic systems in the Magellanic Clouds. The goal of this line_3: proposal is twofold : (1) The main goal is an accurate line_4: determination of the luminosity and radiation temperature of the line_5: hot component in symbiotic systems. That knowledge is of prime line_6: importance when trying to situate symbiotics in an evolutionary line_7: scenario. Since distances to galactic symbiotics are very badly line_8: known, observations in the Magellanic Clouds can be the basis for line_9: a breakthrough. (2) From the nebular spectrum we can fairly easily line_10: determine relative CNO abundances of symbiotic nebulae. As the line_11: nebula has its origin in the red giant, this provides a line_12: straightforward method for determining relative C/N/O abundances line_13: of the Magellanic red giants without the uncertainties of a line_14: stellar atmosphere analysis. Up to now almost all information line_15: about the chemistry of the Clouds has been derived from H II line_16: regions and planetary nebulae. The proposed observations present line_17: therefore also a new possibility for studying abundances in the line_18: Magellanic Clouds. ! ! end of abstract general_form_proposers: lname: VOGEL fname: MANFRED title: PI inst: ETH ZURICH country: SWITZERLAND esa: Y ! lname: NUSSBAUMER fname: HARRY inst: ETH ZURICH country: SWITZERLAND esa: Y ! lname: SHORE fname: STEVEN mi: N. inst: COMPUTER SCIENCES CORPORATION country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: For determining the radiation temperature and luminosity of the line_2: hot component we need to observe the He II 1640 line and the line_3: continuum to wavelengths as short as possible. As these observations line_4: do not require high resolution, we plan for each target one exposure line_5: with the G130H grating, observed in the 4.3 arcsec aperture. line_6: As a side benefit we obtain at the shortest HST wavelengths some of line_7: the most interesting nebular emission lines like N V 1240, line_8: the dielectronic recombination line O V 1371 and the multiplet line_9: Si IV 1401. They give additional information on the ionization state line_10: of these objects. line_11: For abundance determinations we need absolute fluxes of the line_12: CNO lines in the UV: C III] 1908, C IV 1550, N III] 1750, N IV] line_13: 1486, and O III] 1664. In addition to the G130H observation for the line_14: temperature and luminosity determination, one complementary exposure line_15: with the G190H grating will provide the C III] 1908 line. Thus, two line_16: exposures for every target would then cover the range from line_17: 1150 to 2300 A, and contain all the crucial emission lines line_18: as well as a sufficiently broad fraction of the stellar and line_19: nebular continuum to determine the shape of the continuous energy line_20: distribution. ! question: 3 section: 2 line_1: We restrict our target list to 5 objects, 3 in the LMC and 2 in the line_2: SMC :i) S 63-LMC was observed with IUE, and it will be line_3: our standard for estimating exposure times for the targets with line_4: unknown UV flux. Its primary seems to be rich in carbon. line_5: ii) Sanduleak's star was also observed with IUE. However, the line_6: continuum is underexposed and only detectable on the IUE photowrites. line_7: The UV emission line spectrum is very similar to that of the S line_8: condensation in Eta Carinae. In both objects nitrogen seems to be line_10: overabundant, indicating processing through the CNO cycle. This line_11: seems like planetary nebulae in the Magellanic Clouds, which are all line_12: overabundant in nitrogen as compared with H II regions. ! question: 3 section: 3 line_1: iii) S 147-LMC was recently discovered by Morgan and Allen. They line_2: find that the primary is an oxygen-rich giant on the asymptotic branch. line_3: In the LMC two distinct asymptotic giant branches exist, one of which is 1.5 line_4: magnitudes brighter than the other, possble evidence for two line_5: distinct star-forming episodes about 100 million years and a few line_6: Gyr ago. The chemistry of cool giants is expected to be different line_7: for these two classes, and we believe that our observations line_8: provide valuable information about the composition of cool stars. line_9: iv) N 73 and Ln 358 are members of the SMC. The line_10: available optical spectra do not allow a classification of the line_11: primaries involved. Very little is known about the CNO abundances line_12: of cool giants in the SMC. Spite et al. (1989) analyzed 3 F line_13: supergiant and found a carbon and oxygen deficiency of [C/H] = line_14: -0.9 dex and [O/H] = -0.6 dex relative to galactic H II regions. line_15: Again, our proposed observations would provide a unique extension line_16: of the knowledge about the chemical composition to cooler stars. ! question: 4 section: 1 line_1: By their very nature symbiotics demand observations in the far UV. The line_2: hot components have radiation temperatures of at least 50000 K, but line_3: mostly of 100000 K and higher. Contrary to other classes of double line_4: star systems, the hot components are only directly observable at the line_5: shortest wavelengths accessible with HST. On the other hand, the line_6: luminous M giant which dominates the visual and the infrared, makes line_7: essentially no contribution in the far UV. line_8: IUE provided a tremendous boost to research of galactic symbiotics. line_9: However, the limited sensitivity and the low dynamic range of IUE line_10: prevented anything beyond an exploratory study of symbiotic systems in line_11: the Magellanic Clouds in the UV. The FOS on HST is very well suited line_12: for an extension of research to extragalactic symbiotics. There is at line_13: present no substitute for the dynamic range required by our proposal line_14: and provided by HST. In addition, since the hot components in line_15: symbiotic systems are only directly observable at wavelengths shorter line_16: than 1600 A, the FOS is the most suited instrument for the line_17: proposed scientific goal, and there is obviously no ground-based line_18: substitute. ! question: 5 section: 1 line_1: S 63-LMC is reasonably well observed with IUE to estimate line_2: absolute fluxes in the UV. We use this star as a reference and line_3: scale the exposure times for the targets with unknown UV fluxes line_4: according to their blue or visual magnitudes. The visual line_5: magnitude of S 63 is V = 15.6, and the ultraviolet flux is line_6: approximately 1E-14 erg/cm/cm/sec/Ang at 1500 A. The strength of line_7: the three emission lines C III] 1908, N III] 1750, and O III] line_8: 1664 which are in the G190H range is between 3E-14 and 4E-14 line_9: erg/cm/cm/sec, and the line width we estimate to be approximately 2 A. ! question: 5 section: 2 line_1: The exposure times for S 63 are calculated as follows : the line_2: calibration curve of the FOS/BL (Gilliland and Hartig 1991) yield line_3: for G130H at 1500 A about 1E+13 cts/diode/sec per line_4: erg/cm/cm/sec/A, and the sensitivity of G190H is about 2E+13 line_5: cts/diode/sec per erg/cm/cm/sec/A at 1640 A, and higher for line_6: longer wavelengths. For a S/N = 10 in the continuum this requires line_7: an integration time of 1000 sec using the G130H grating in order line_8: to obtain the energy distribution of the hot object. For the He line_9: II 1640 equivalent width and the emission lines of C III] 1908, N III] line_10: 1750, and O III] 1664 an integration time of 300 sec will line_11: provide a S/N of about 10 in the emission lines and in the He II line_12: 1640 equivalent width. All exposures will be taken through the line_13: 4.3 arcsec aperture. The total exposure time for S 63 line_14: would therefore be approx. 22 min. Exposure times for the other line_15: targets are calculated assuming that the spectrum of S 63 is typical line_16: of all five objects, and that the exposure times will simply scale as line_17: their V magnitudes. The indivudual exposure times are chosen to tune the line_18: the total spacecraft to the allocated 10.2 hours. The total number of line_19: targets is 5, the total number of visits is also 5, and the total number line_20: of exposures is 10. ! question: 6 section: 1 line_1: None ! question: 7 section: 1 line_1: At the institutes of the investigators the following expertise line_2: and plans exist. (a) At NASA-GSFC data analysis software exists line_3: for analyzing HRS observations, including wavelength line_4: determination and absolute line and continuum intensity line_5: calibration. (b) At the Institute of Astronomy of the ETH Zurich line_6: we have systematically developed physical models and numerical line_7: methods for calculating synthetic spectra of symbiotic systems line_8: for various chemical compositions. These methods have already line_9: been applied to symbiotic systems in the Galaxy. Nussbaumer et line_10: al. (1988) determined relative CNO abundances for 24 galactic line_11: systems observed with IUE, and Muerset et al. (1991) derived line_12: luminosities and radiation temperatures for 21 symbiotic stars line_14: included in the IUE archive. We have chosen five targets, 3 line_15: objects in the LMC and 2 in the SMC. Although this numbers will not line_16: provide a statistically significant data set, we are confident to line_17: add new information about the star formation history in the line_18: Clouds and the production mechanism for the CNO elements. ! question: 8 section: 1 line_1: None. ! question: 9 section: 1 line_1: Nr. 2342 - The symbiotic phenomenon. line_2: (Michalitsianos, Fahey, Kafatos, Nussbaumer, Paresce) line_3: The observations have not yet been done. The goal of that project, line_4: which will concentrate on the symbiotic star R Aqr (which is not a line_5: symbiotic nova), is not related to the purpose of this proposal. ! question: 10 section: 1 line_1: At ETH (Swiss Federal Institute of Technology) we have excellent line_2: computer facilities which we can access directly from our line_3: institute, e.g. Cray YMP, VAX 9000. Allocation of requested line_4: computer access and time has never been a problem. In addition we line_5: have several computer work stations as part of the infrastructure line_6: of our institute. From ETH and the Swiss Science Foundation we line_7: have always received grants for two to three Ph.D. students to line_8: work on these projects, in addition two post-doctoral positions line_9: have been granted to work on HST related projects. Travel money line_10: needed is included in the budget of our institute. Cray YMP time line_11: will also be available at GSFC. SPAN links between institutions line_12: will permit rapid exchange of, and analysis of, the HST data. ! !end of general form text general_form_address: lname: VOGEL fname: MANFRED category: PI inst: ETH Zurich addr_1: ETH ZENTRUM city: 8092 ZURICH country: SWITZERLAND phone: 41-1-256 3806 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: S63 descr_1: A,155 pos_1: RA = 05H 48M 43.2S +/- 0.1S, pos_2: DEC = -67D 36' 09.1" +/- 1" equinox: 2000 fluxnum_1: 1 fluxval_1: V = 14.7 ! targnum: 2 name_1: SANDULEAK descr_1: A,155 pos_1: RA = 05H 45M 19.5S +/- 0.1S, pos_2: DEC = -71D 16' 05.7" +/- 1" equinox: 2000 fluxnum_1: 1 fluxval_1: V = 15.0 ! targnum: 3 name_1: S147 descr_1: A,155 pos_1: RA = 04H 54M 03.5S +/- 0.1S, pos_2: DEC = -70D 59' 32.3" +/- 1" equinox: 2000 fluxnum_1: 1 fluxval_1: V = 15.8 ! targnum: 5 name_1: LN358 descr_1: A,155 pos_1: RA = 00H 59M 12.4S +/- 0.1S, pos_2: DEC = -75D 05' 17.2" +/- 1" equinox: 2000 fluxnum_1: 1 fluxval_1: V = 15.0 ! targnum: 6 name_1: N73 descr_1: A,155 pos_1: RA = 01H 04M 39.3S +/- 0.1S, pos_2: DEC = -75D 48' 24.3" +/- 1" equinox: 2000 fluxnum_1: 1 fluxval_1: V = 15.5 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 3.000 targname: S63 config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 10S fluxnum_1: 1 priority: 3 req_1: ONBOARD ACQ FOR 4; req_2: SPATIAL SCAN; req_3: CYCLE 3 / 3-6 comment_1: COARSE PEAK-UP IN 4.3 ! linenum: 4.000 targname: S63 config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 10S fluxnum_1: 1 priority: 3 req_1: ONBOARD ACQ FOR 5-6; req_2: SPATIAL SCAN; req_3: CYCLE 3 / 4-6 comment_1: FINE PEAK-UP IN 1.0 ! linenum: 5.000 targname: S63 config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 30M s_to_n: 10 fluxnum_1: 1 priority: 3 ! linenum: 6.000 targname: S63 config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G190H num_exp: 1 time_per_exp: 20M s_to_n: 10 fluxnum_1: 1 priority: 3 ! linenum: 7.000 targname: SANDULEAK config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 10S fluxnum_1: 1 priority: 4 req_1: ONBOARD ACQ FOR 8; req_2: SPATIAL SCAN; req_3: CYCLE 3 / 7-10 comment_1: COARSE PEAK-UP IN 4.3 ! linenum: 8.000 targname: SANDULEAK config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 10S fluxnum_1: 1 priority: 4 req_1: ONBOARD ACQ FOR 9-10; req_2: SPATIAL SCAN; req_3: CYCLE 3 / 8-10 comment_1: FINE PEAK-UP IN 1.0 ! linenum: 9.000 targname: SANDULEAK config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 38M s_to_n: 10 fluxnum_1: 1 priority: 4 ! linenum: 10.000 targname: SANDULEAK config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G190H num_exp: 1 time_per_exp: 25M s_to_n: 10 fluxnum_1: 1 priority: 4 ! linenum: 11.000 targname: S147 config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 15S fluxnum_1: 1 priority: 2 req_1: ONBOARD ACQ FOR 12; req_2: SPATIAL SCAN; req_3: CYCLE 3 / 11-14 comment_1: COARSE PEAK-UP IN 4.3 ! linenum: 12.000 targname: S147 config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 15S fluxnum_1: 1 priority: 2 req_1: ONBOARD ACQ FOR 13-14; req_2: SPATIAL SCAN; req_3: CYCLE 3 / 12-14 comment_1: FINE PEAK-UP IN 1.0 ! linenum: 13.000 targname: S147 config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 46M s_to_n: 10 fluxnum_1: 1 priority: 2 ! linenum: 14.000 targname: S147 config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G190H num_exp: 1 time_per_exp: 32M s_to_n: 10 fluxnum_1: 1 priority: 2 ! linenum: 15.000 targname: LN358 config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 10S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 16; req_2: SPATIAL SCAN; req_3: CYCLE 3 / 15-18 comment_1: COARSE PEAK-UP IN 4.3 ! linenum: 16.000 targname: LN358 config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 10S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 17-18; req_2: SPATIAL SCAN; req_3: CYCLE 3 / 16-18 comment_1: FINE PEAK-UP IN 1.0 ! linenum: 17.000 targname: LN358 config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 38M s_to_n: 10 fluxnum_1: 1 priority: 1 ! linenum: 18.000 targname: LN358 config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G190H num_exp: 1 time_per_exp: 25M s_to_n: 10 fluxnum_1: 1 priority: 1 ! linenum: 19.000 targname: N73 config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 12S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 20; req_2: SPATIAL SCAN; req_3: CYCLE 3 / 19-22 comment_1: COARSE PEAK-UP IN 4.3 ! linenum: 20.000 targname: N73 config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 12S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 21-22; req_2: SPATIAL SCAN; req_3: CYCLE 3 / 20-22 comment_1: FINE PEAK-UP IN 1.0 ! linenum: 21.000 targname: N73 config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 42M s_to_n: 10 fluxnum_1: 1 priority: 1 ! linenum: 22.000 targname: N73 config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G190H num_exp: 1 time_per_exp: 30M s_to_n: 10 fluxnum_1: 1 priority: 1 ! ! end of exposure logsheet scan_data: line_list: 3,7,11,15,19 fgs_scan: cont_dwell: D dwell_pnts: 3 dwell_secs: 1.00 scan_width: 0.0000 scan_length: 2.8000 sides_angle: 90.0000 number_lines: 1 scan_rate: 0.0000 first_line_pa: 0.0000 scan_frame: S/C len_offset: 1.4 wid_offset: 0.0 ! line_list: 4,8,12,16,20 fgs_scan: cont_dwell: D dwell_pnts: 6 dwell_secs: 1.00 scan_width: 0.7000 scan_length: 3.5000 sides_angle: 90.0000 number_lines: 2 scan_rate: 0.0000 first_line_pa: 90.0000 scan_frame: S/C len_offset: 1.75 wid_offset: 0.35 ! ! end of scan data