! $Id: 5360,v 4.1 1994/07/27 17:04:46 pepsa Exp $ coverpage: title_1: MASS LOSS AND IRON CURTAIN IN SYMBIOTIC SYSTEMS sci_cat: INTERSTELLAR MEDIUM sci_subcat: NOVAE proposal_for: GO longterm: 1 pi_fname: HARRY pi_lname: NUSSBAUMER pi_inst: 7820 pi_country: SWITZERLAND pi_phone: 41-1-6323631 hours_pri: 5.87 num_pri: 3 hrs: Y off_fname: HARRY off_lname: NUSSBAUMER off_title: HEAD OF GROUP off_inst: INSTITUTE OF ASTRONOMY off_addr_1: ETH ZENTRUM off_city: 8092 ZUERICH off_country: SWITZERLAND off_phone: 41-1-6323631 ! end of coverpage abstract: line_1: We propose GHRS observations for studying mass loss of hot components in line_2: symbiotic novae and the close environment of the interacting binaries. We have line_3: indications that in some symbiotics the hot star loses mass by a fast wind. line_4: Mass loss by the cool giant has previously been investigated and is generally line_5: accepted. The detection of a second wind would imply that new physical line_6: processes need to be included in modelling symbiotic binaries, particularly the line_7: hydrodynamic treatment of the collision of two winds, with the related X-ray line_8: emission and other high energy phenomena. - It was recently suggested, that line_9: the interpretation of symbiotic spectra may be severely distorted by selective line_10: absorption by a forest of lines from neutral and lowly ionized atoms in the line_11: wind of the cool star. This `iron curtain' is mainly due to transitions from line_12: iron peak elements. Only HST has the required dynamic range and spectral line_13: resolution needed for a conclusive investigation of the wind and `iron curtain' line_14: problem. The present proposal addresses simultaneously three scientific goals: line_15: (1) A search for winds and mass losses from hot components in symbiotics stars. line_16: (2) Spectroscopic NLTE analyses of the wind features which will provide stellar line_17: parameters and wind characteristics of symbiotic novae. (3) An `iron curtain' line_18: analysis which allows an unambiguous interpretation of observed line profiles line_19: provides information about the physical state of the neutral and lowly ionized line_20: environment, in particular basic physical properties of the cool giant's wind. ! ! end of abstract general_form_proposers: lname: NUSSBAUMER fname: HARRY inst: 7820 country: SWITZERLAND esa: Y ! lname: SCHMUTZ fname: WERNER inst: 7820 country: SWITZERLAND esa: Y ! lname: VOGEL fname: MANFRED inst: 7820 country: SWITZERLAND esa: Y ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: For the spectroscopic analysis of the hot object and its wind we need medium line_2: resolution observations (R approx10'000). They are essential for separating line_3: the very strong (10 to 100 times continuum) but narrow (40 km/s) nebular line_4: lines from the rather weak (about twice continuum) but broad (500 km/s) line_5: lines from the hot wind. line_6: Practically the same set of lines is requested for PU Vul and AG Peg. line_7: For EG And only C IV 1550 and He II 1640 will be observed. line_8: (a) The following lines are needed for the wind analysis: line_9: Resonance multiplets: C IV 1549, N V 1240, Si IV 1397, (Al III 1857) line_10: Recombination lines: He II 1640, N IV 1718, O V 1371 line_11: Al III 1857 is only proposed for PU Vul line_12: (b) For modelling the nebula we need in addition: line_13: C III 1909, Si III 1891, N III 1750, N IV 1486. line_14: O IV 1400 is contained in the Si IV 1397 observation. line_15: The observations required under (a) also contain the necessary line_16: information for the `iron curtain' program. ! question: 4 section: 1 line_1: Further progress in the study of the hot wind and the characteristics of the line_2: hot object in the symbiotic system demands observations with a UV telescope of line_3: higher sensitivity and dynamic range than available on IUE. In particular, the line_4: wind line profiles from the hot star with their suspected P-Cygni absorption line_5: and the broad low contrast feet are only accessible with HST. For the symbiotic line_6: novae IUE does not reach the continuum level in high resolution in the line_7: neighbourhood of strong lines without overspilling through saturation from line_8: the strong nebular component. - The `iron curtain' program has the same line_9: requirements as the wind program, it needs sufficient continuum in the line_10: proximity of the strong absorption lines (see Figure). line_11: Closer inspection of IUE high resolution spectra show that emission lines like line_12: N V 1240, C IV 1550, or He II 1640 are blends of narrow strong nebular and line_13: broad wind lines. But the limited dynamic range of IUE does not allow to line_14: properly deconvolve the features. In addition the continuum is either absent or line_15: strongly distorted by overspilling from the peaks of the emission lines. line_16: We have accepted IUE proposals and shall submit for further observations line_17: to obtain absolute fluxes over the full IUE spectral range. IUE capabilities line_18: suffice to measure the general continuum longward of about 1300 Angstroem as line_19: well as fluxes of stronger nebular emission lines, in order to follow their line_20: evolution. IUE observations are insufficient for wind line profiles and line_21: their immediate neighbourhood. We have accepted ESO proposals, and we shall line_22: submit additional requests, in particular to obtain H and He line fluxes and line_23: their line profiles for wind diagnostics and abundance determinations. As ! question: 4 section: 2 line_1: PU Vul is the youngest symbiotic nova. We need HST for the nebular diagnostics line_2: as well as for the wind lines, where IUE cannot provide the necessary data. line_3: AG Peg is a symbiotic nova where the nebular lines now dominate the spectrum. line_4: With HST we shall be able to separate hot wind and nebular contributions. line_5: This is of prime importance for our model calculations. line_6: EG And is of particular interest for the `iron curtain' lines. IUE observations line_7: cannot provide the required signal/noise in the lines and underlying continua line_8: of the lines principally affected: C IV and He II. line_9: Symbiotic novae vary relatively slowly, neither of these observations are very line_10: time critical, except that EG And should not be observed during eclipse. ! question: 5 section: 1 line_1: EG And varies with a period of 482.days. It has its minimum at line_2: JD= 2'448'273 + E x 482.2. The length of the full eclipse lasts line_3: approximately 30 days. Therefore, line_4: avoid HST observations of EG And on the following dates: line_5: November 1994, line_6: December 1994, line_7: January 1995, line_8: February 1995 ! question: 6 section: 1 line_1: None ! ! ! 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, which line_4: will concentrate on the symbiotic star R Aqr (which is not a symbiotic nova), line_5: is not related to the purpose of this proposal. line_6: Nr. 3605 Extreme stellar winds and post-main-sequence evolution in the upper line_7: HR Diagramm (PI Leiterer, co-author Schmutz) line_8: Nr. 3663 UV spectropolarimatry of AG Car in its current outburst. line_9: (PI Leiterer, co-author Schmutz) line_10: Nr. 3882 UV spectropolarimatry of AG Car in its current outburst. (DD time) line_11: (PI Leiterer, co-author Schmutz) line_12: Nr. 4494 Symbiotic systems in the Magellanic Clouds. line_13: (Vogel, Nussbaumer, Shore) line_14: The observations are scheduled for December 1993. line_15: Nr. 4494 is indirectly related in that it should permit to put symbiotics on an line_16: absolute luminosity scale. ! question: 10 section: 1 line_1: From ETH and the Swiss Science Foundation we have received grants for two line_2: Ph.D. students to work on these projects. In addition three post-doctoral line_3: positions have been granted to work on HST related projects. There line_4: are always a number of students who work in our institute to fulfill part of line_5: their obligation for their physics degree. Travel money needed is included line_6: in the budget of our institute. At ETH (Swiss Federal Institute of Technology) line_7: we have excellent computer facilities which we can access directly from our line_8: institute, e.g. Cray Y-MP, VAX 9000. Allocation of requested computer access line_9: and time has never been a problem. In addition we have several computer line_10: work stations as part of the infrastructure of our institute. ! !end of general form text general_form_address: lname: NUSSBAUMER fname: HARRY category: PI inst: 7820 addr_1: ETH ZENTRUM city: 8092 ZURICH country: SWITZERLAND phone: 41-1-632 3631 telex: nussbaum@astro.phys.ethz.ch ! lname: category: CON ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: PU-VUL descr_1: A,155 pos_1: RA = 20H 21M 13.30S +/- 0.15S, pos_2: DEC = +21D 34' 18.0" +/- 2.0" equinox: 2000 pos_epoch_bj: J pos_epoch_yr: 2000.00 fluxnum_1: 1 fluxval_1: V = 8.8 fluxnum_2: 1 fluxval_2: B-V= 0.0 ! targnum: 2 name_1: AG-PEG descr_1: A,155 pos_1: RA = 21H 51M 02.00S +/- 0.15S, pos_2: DEC = +12D 37' 31.9" +/- 2.0" equinox: 2000 pos_epoch_bj: J pos_epoch_yr: 2000.00 fluxnum_1: 1 fluxval_1: V = 8.7 fluxnum_2: 1 fluxval_2: B-V= 1.3 ! targnum: 3 name_1: EG-AND descr_1: A,155 pos_1: RA = 00H 44M 37.17S +/- 0.2S, pos_2: DEC = +40D 40' 45.9" +/- 2.0" equinox: 2000 pos_epoch_bj: J pos_epoch_yr: 2000.00 comment_1: AVOID EG AND DURING THE comment_2: DATES GIVEN TO QUESTION 5 fluxnum_1: 1 fluxval_1: V = 7.3 fluxnum_2: 1 fluxval_2: B-V= 1.7 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.010 targname: PU-VUL config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 3.6S fluxnum_1: 1 priority: 1 param_1: SEARCH-SIZE=3, param_2: BRIGHT=RETURN, param_3: LOCATE=YES req_1: CYCLE 4; req_2: ONBOARD ACQ FOR 1.02 comment_1: STEP-TIME=0.4 SEC ! linenum: 1.020 targname: PU-VUL config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 40.8S fluxnum_1: 1 priority: 1 req_1: CYCLE 4; req_2: ONBOARD ACQ FOR 1.03-1.11; comment_1: STEP-TIME=0.4 SEC ! linenum: 1.030 targname: PU-VUL config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1240 num_exp: 1 time_per_exp: 1650.0S s_to_n: 20 fluxnum_1: 1 priority: 1 param_1: FP-SPLIT=STD req_1: CYCLE 4; comment_1: SIGNAL-NOISE IN THE CONTINUUM ! linenum: 1.040 targname: PU-VUL config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1400 num_exp: 1 time_per_exp: 1400.0S s_to_n: 20 fluxnum_1: 1 priority: 1 param_1: FP-SPLIT=STD req_1: CYCLE 4; comment_1: SIGNAL-NOISE IN THE CONTINUUM ! linenum: 1.050 targname: PU-VUL config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1485 num_exp: 1 time_per_exp: 1200.0S s_to_n: 20 fluxnum_1: 1 priority: 1 param_1: FP-SPLIT=STD req_1: CYCLE 4; comment_1: SIGNAL-NOISE IN THE CONTINUUM ! linenum: 1.060 targname: PU-VUL config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1550 num_exp: 1 time_per_exp: 1500.0S s_to_n: 20 fluxnum_1: 1 priority: 1 param_1: FP-SPLIT=STD req_1: CYCLE 4; comment_1: SIGNAL-NOISE IN THE CONTINUUM ! linenum: 1.070 targname: PU-VUL config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1640 num_exp: 1 time_per_exp: 1600.0S s_to_n: 20 fluxnum_1: 1 priority: 1 param_1: FP-SPLIT=STD req_1: CYCLE 4; comment_1: SIGNAL-NOISE IN THE CONTINUUM ! linenum: 1.080 targname: PU-VUL config: HRS opmode: ACCUM aperture: 2.0 sp_element: G200M wavelength: 1718 num_exp: 1 time_per_exp: 1200.0S s_to_n: 20 fluxnum_1: 1 priority: 1 param_1: FP-SPLIT=STD req_1: CYCLE 4; comment_1: SIGNAL-NOISE IN THE CONTINUUM ! linenum: 1.090 targname: PU-VUL config: HRS opmode: ACCUM aperture: 2.0 sp_element: G200M wavelength: 1750 num_exp: 1 time_per_exp: 1000.0S s_to_n: 20 fluxnum_1: 1 priority: 1 param_1: FP-SPLIT=STD req_1: CYCLE 4; comment_1: SIGNAL-NOISE IN THE CONTINUUM ! linenum: 1.100 targname: PU-VUL config: HRS opmode: ACCUM aperture: 2.0 sp_element: G200M wavelength: 1860 num_exp: 1 time_per_exp: 900.0S s_to_n: 20 fluxnum_1: 1 priority: 1 param_1: FP-SPLIT=STD req_1: CYCLE 4; comment_1: SIGNAL-NOISE IN THE CONTINUUM ! linenum: 1.110 targname: PU-VUL config: HRS opmode: ACCUM aperture: 2.0 sp_element: G200M wavelength: 1900 num_exp: 1 time_per_exp: 900.0S s_to_n: 20 fluxnum_1: 1 priority: 1 param_1: FP-SPLIT=STD req_1: CYCLE 4; comment_1: SIGNAL-NOISE IN THE CONTINUUM ! linenum: 2.010 targname: AG-PEG config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 1.8S fluxnum_1: 1 priority: 1 param_1: SEARCH-SIZE=3, param_2: BRIGHT=RETURN, param_3: LOCATE=YES req_1: CYCLE 4; req_2: ONBOARD ACQ FOR 2.02; comment_1: STEP-TIME=0.2 SEC ! linenum: 2.020 targname: AG-PEG config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 20.4S fluxnum_1: 1 priority: 1 req_1: CYCLE 4; req_2: ONBOARD ACQ FOR 2.03-2.09; comment_1: STEP-TIME=0.2 SEC ! linenum: 2.030 targname: AG-PEG config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1240 num_exp: 1 time_per_exp: 600.0S s_to_n: 25 fluxnum_1: 1 priority: 1 param_1: FP-SPLIT=STD req_1: CYCLE 4; comment_1: SIGNAL-NOISE IN THE CONTINUUM ! linenum: 2.040 targname: AG-PEG config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1371 num_exp: 1 time_per_exp: 600.0S s_to_n: 25 fluxnum_1: 1 priority: 1 param_1: FP-SPLIT=STD req_1: CYCLE 4; comment_1: SIGNAL-NOISE IN THE CONTINUUM ! linenum: 2.050 targname: AG-PEG config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1400 num_exp: 1 time_per_exp: 600.0S s_to_n: 25 fluxnum_1: 1 priority: 1 param_1: FP-SPLIT=STD req_1: CYCLE 4; comment_1: SIGNAL-NOISE IN THE CONTINUUM ! linenum: 2.060 targname: AG-PEG config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1485 num_exp: 1 time_per_exp: 600.0S s_to_n: 25 fluxnum_1: 1 priority: 1 param_1: FP-SPLIT=STD req_1: CYCLE 4; comment_1: SIGNAL-NOISE IN THE CONTINUUM ! linenum: 2.070 targname: AG-PEG config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1550 num_exp: 1 time_per_exp: 600.0S s_to_n: 25 fluxnum_1: 1 priority: 1 param_1: FP-SPLIT=STD req_1: CYCLE 4; comment_1: SIGNAL-NOISE IN THE CONTINUUM ! linenum: 2.080 targname: AG-PEG config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1640 num_exp: 1 time_per_exp: 600.0S s_to_n: 25 fluxnum_1: 1 priority: 1 param_1: FP-SPLIT=STD req_1: CYCLE 4; comment_1: SIGNAL-NOISE IN THE CONTINUUM ! linenum: 2.090 targname: AG-PEG config: HRS opmode: ACCUM aperture: 2.0 sp_element: G200M wavelength: 1718 num_exp: 1 time_per_exp: 600.0S s_to_n: 25 fluxnum_1: 1 priority: 1 param_1: FP-SPLIT=STD req_1: CYCLE 4; comment_1: SIGNAL-NOISE IN THE CONTINUUM ! linenum: 3.010 targname: EG-AND config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 9.0S fluxnum_1: 1 priority: 1 param_1: SEARCH-SIZE=3, param_2: BRIGHT=RETURN, param_3: LOCATE=YES req_1: CYCLE 4; req_2: ONBOARD ACQ FOR 3.02; comment_1: STEP-TIME=1.0 SEC ! linenum: 3.020 targname: EG-AND config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 102.0S fluxnum_1: 1 priority: 1 req_1: CYCLE 4; req_2: ONBOARD ACQ FOR 3.03-3.04; comment_1: STEP-TIME=1.0 SEC ! linenum: 3.030 targname: EG-AND config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1550 num_exp: 1 time_per_exp: 45.0M s_to_n: 20 fluxnum_1: 1 priority: 1 param_1: FP-SPLIT=STD req_1: CYCLE 4; comment_1: SIGNAL-NOISE IN THE CONTINUUM ! linenum: 3.040 targname: EG-AND config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1640 num_exp: 1 time_per_exp: 45.0M s_to_n: 20 fluxnum_1: 1 priority: 1 param_1: FP-SPLIT=STD req_1: CYCLE 4; comment_1: SIGNAL-NOISE IN THE CONTINUUM ! ! end of exposure logsheet ! No scan data records found