! File: 4058C.PROP ! Database: PEPDB ! Date: 20-FEB-1994:06:54:15 coverpage: title_1: MASS EXCHANGE BINARIES (FOS 34) AUGMENTATION: CYCLE 2 OBSERVATIONS sci_cat: STELLAR ASTROPHYSICS proposal_for: AUG/FOS cont_id: 3651 pi_title: PROF. pi_fname: BRUCE pi_lname: MARGON pi_inst: WASHINGTON, UNIVERSITY OF pi_country: USA pi_phone: 206-543-0089 hours_pri: 7.10 num_pri: 1 fos: Y ! end of coverpage abstract: line_1: The pre-launch FOS GTO program proposed a systematic study of degenerate stars line_2: in binary systems, both in the field and in globular clusters, plus a handful line_3: of related objects. For the isolated field systems, the emphasis is on spectro- line_4: photometry (in many cases time-resolved over a pulse or orbital period) and line_5: spectropolarimetry, to observe the effects of the intense ionizing flux emitted line_6: by the compact object on the nearby normal star and/or accretion disk. While line_7: some such effects are seen from the ground, they should be far more spectacular line_8: in the UV. The GTO program for the globular cluster systems typically proposes line_9: WF/PC or FOC images to locate candidates for cluster X-ray sources, followed by line_10: confirming FOS spectroscopy. Our published FOC observations of M14 show that line_11: even with the primary's spherical aberration, it is possible to reach flux line_12: levels relevant to these problems with angular resolution far better than line_13: achievable from the ground. Even one or two new close binaries identified line_14: through this program will be extremely important, as these systems are thought line_15: to dominate the kinetic energy budget of globular clusters, yet virtually none line_16: are currently known. Also proposed for augmentation are two related programs: line_17: FOS observations of the Crab pulsar and a study of UV-bright objects in line_18: globular cluster cores. The increased FOS integration times caused by the line_19: spherical aberration have drastically disrupted the original intended line_20: scientific program; augmentation proposed here partially restores these efforts. ! ! end of abstract general_form_proposers: lname: MARGON fname: BRUCE inst: UNIVERSITY OF WASHINGTON country: USA ! lname: HARMS fname: RICHARD title: PI mi: J. inst: APPLIED RESEARCH CORPORATION country: USA ! lname: BOHLIN fname: RALPH inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! lname: ANGEL fname: J. ROGER mi: P. inst: UNIVERSITY OF ARIZONA country: USA ! lname: BARTKO fname: FRANK inst: UNIVERSITY OF CALIFORNIA, SAN DIEGO country: USA ! lname: BEAVER fname: EDWARD inst: UNIVERSITY OF CALIFORNIA, SAN DIEGO country: USA ! lname: BURBIDGE fname: E. MARGARET inst: UNIVERSITY OF CALIFORNIA, SAN DIEGO country: USA ! lname: DAVIDSEN fname: ARTHUR mi: F. inst: JOHNS HOPKINS UNIVERSITY country: USA ! lname: FORD fname: HOLLAND mi: C. inst: JOHNS HOPKINS UNIVERSITY country: USA ! lname: HARTIG fname: GEORGE mi: F. inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! lname: ANDERSON fname: SCOTT mi: F. inst: UNIVERSITY OF WASHINGTON country: USA ! lname: DOWNES fname: RONALD mi: A. inst: STSCI country: USA ! lname: ALLEN fname: RICHARD mi: P. inst: UNIVERSITY OF ARIZONA country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: The intermediate polar DQ Her will be observed, including line_2: UV FOS spectrophotometry of modest spectral resolution at line_3: binary orbital phases of max light. Time-resolved line_4: FOS UV spectrophotometry through the 71S white dwarf line_5: rotation period will also be obtained. ! question: 4 section: 1 line_1: For this program, HST is needed primarily because of its line_2: high efficiency in the UV, as this wavelength regime is an line_3: essential key for understanding the intermediate polars. These line_4: systems should show especially strong spectral variations in the line_5: UV, modulated with the binary orbital period (and even with line_6: white dwarf rotational period). ! question: 5 section: 1 line_1: All observations in this program are time critical. The observations line_2: have been organized to allow lines 18-22 to be scheduled in line_3: consecutive orbits in one visit, and lines 23-27 in a second visit. ! question: 7 section: 1 line_1: Data reduction will be performed at the ST ScI, and the analysis will be line_2: performed using FOS IDT computer facilities. The DQ Her program involves line_3: analysis of FOS spectrophotometry (including time-resolved mode). The FOS line_4: IDT, of course, has extensive practical experience in the use of STSDAS line_5: (and other IRAF-related) software to reduce and analyze all the various line_6: types of FOS data. The analysis required for this program should be line_7: straightforward: e.g., looking for spectral variations as function of line_8: orbital or rotational phases. ! question: 8 section: 1 line_1: Although not essential to our scientific programs, we will try to obtain line_2: simultaneous (or contemporaneous) observations of DQ Her from the ground. line_3: Certain of these systems are known to have unstable periods, but require line_4: observations at certain specific phases. ! question: 9 section: 1 line_1: Partial data from about a dozen different FOS/GTO programs (and many line_2: OV and SV proposals) have been obtained to date. This proposal includes line_3: augmentation time related to the following FOS/GTO and SAO proposals line_4: 1051, 3202, and 3280 (Mass Exchange Binaries). ! question: 10 section: 1 line_1: Data analysis, research assistant support, and funding will be provided under line_2: NASA's FOS GTO contract(s). The FOS IDT support includes a total of roughly line_3: 30 Ph.D. astronomers and graduate students at 5 different institutions. At line_4: each institution one or more workstations (typically Sparc 2's or the line_5: equivalent), plus one or more Microvaxes (or equivalent) are essentially line_6: devoted to processing of HST data. ! question: 13 section: 1 line_1: Spectra and time-resolved spectra will be obtained as a function of line_2: orbital (and roation) period in DQ Her. ! !end of general form text general_form_address: lname: MARGON fname: BRUCE category: PI inst: UNIVERSITY OF WASHINGTON addr_1: ASTRONOMY DEPARTMENT, FM-20 city: SEATTLE state: WA zip: 98195 country: USA phone: 206 543-0089 telex: 4740096 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: DQ-HER descr_1: A,154 pos_1: RA= 18H 07M 30.35S +/-0.01S, pos_2: DEC = +45D 51' 31.7"+/-0.3", pos_3: PLATE-ID=00TB equinox: 2000 fluxnum_1: 1 fluxval_1: V = 14.2 +/- 0.3 fluxnum_2: 2 fluxval_2: V = 17.7 +/- 0.3 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 18.000 targname: DQ-HER config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: G400H num_exp: 1 time_per_exp: 1.0S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 18.1; req_2: ZERO-PHASE JD2434954.94425 +/- 0.00001D; req_3: PERIOD 0.19362087D +/- 0.001S; req_4: SPATIAL SCAN; req_5: CYCLE 2 /18-27; req_6: GROUP 18-27 WITHIN 6D; req_7: NON-INT /18-18.2 comment_1: THE PHASE IS TO AVOID THE comment_2: TA OCCURRING DURING ECLIPSE. comment_3: TA MUST OCCUR BETWEEN PHASES 0.5 AND comment_4: 0.25 DUE TO ECLIPSING NATURE OF OBJECT ! linenum: 18.100 targname: DQ-HER config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: G400H num_exp: 1 time_per_exp: 1.0S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 18.2; req_2: SPATIAL SCAN; ! linenum: 18.200 targname: DQ-HER config: FOS/BL opmode: ACQ/PEAK aperture: 0.5 sp_element: G400H num_exp: 1 time_per_exp: 1.0S fluxnum_1: 1 priority: 1 param_1: SCAN-STEP=0.35, param_2: SEARCH-SIZE=3 req_1: ONBOARD ACQ FOR 19-22; ! linenum: 19.000 targname: DQ-HER config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G160L wavelength: 1150-2510 num_exp: 1 time_per_exp: 2397.60S fluxnum_1: 1 priority: 1 param_1: READ-TIME=4.44 req_1: PHASE 0.61 +/- 0.04 OF REF18; req_2: NON-INT /19-22; req_3: SEQ 19-22 WITHIN 7.5H; comment_1: DQ HER TIME-RESOLVED DATA comment_2: (ASYNCHRONOUS). ! linenum: 20.000 targname: DQ-HER config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G160L wavelength: 1150-2510 num_exp: 1 time_per_exp: 2397.60S fluxnum_1: 2 priority: 1 param_1: READ-TIME=4.44 comment_1: DQ HER TIME-RESOLVED AT MIN comment_2: (ASYNCHRONOUS). ! linenum: 21.000 targname: DQ-HER config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G160L wavelength: 1150-2510 num_exp: 1 time_per_exp: 2397.60S fluxnum_1: 1 priority: 1 param_1: READ-TIME=4.44 comment_1: DQ HER TIME-RESOLVED comment_2: (ASYNCHRONOUS). ! linenum: 22.000 targname: DQ-HER config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G130H num_exp: 1 time_per_exp: 2400S fluxnum_1: 1 priority: 1 comment_1: DQ HER AT MAX ! linenum: 23.000 targname: DQ-HER config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: G570H num_exp: 1 time_per_exp: 1.0S fluxnum_1: 1 priority: 2 req_1: ONBOARD ACQ FOR 23.1; req_2: SPATIAL SCAN; req_3: NON-INT /23-23.2 comment_1: TA MUST OCCUR BETWEEN PHASES 0.5 AND comment_2: 0.25 DUE TO ECLIPSING NATURE OF OBJECT ! linenum: 23.100 targname: DQ-HER config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: G570H num_exp: 1 time_per_exp: 1.0S fluxnum_1: 1 priority: 2 req_1: ONBOARD ACQ FOR 23.2; req_2: SPATIAL SCAN; ! linenum: 23.200 targname: DQ-HER config: FOS/BL opmode: ACQ/PEAK aperture: 0.5 sp_element: G570H num_exp: 1 time_per_exp: 1.0S fluxnum_1: 1 priority: 2 param_1: SCAN-STEP=0.35, param_2: SEARCH-SIZE=3 req_1: ONBOARD ACQ FOR 24-27; ! linenum: 24.000 targname: DQ-HER config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G160L wavelength: 1150-2510 num_exp: 1 time_per_exp: 2397.60S fluxnum_1: 1 priority: 2 param_1: READ-TIME=4.44 req_1: PHASE 0.61 +/- 0.04 OF REF18; req_2: NON-INT /24-27; req_3: SEQ 24-27 WITHIN 7.5H; comment_1: DQ HER TIME-RESOLVED DATA comment_2: (ASYNCHRONOUS). ! linenum: 25.000 targname: DQ-HER config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G160L wavelength: 1150-2510 num_exp: 1 time_per_exp: 2397.60S fluxnum_1: 2 priority: 2 param_1: READ-TIME=4.44 comment_1: DQ HER TIME-RESOLVED AT MIN comment_2: (ASYNCHRONOUS). ! linenum: 26.000 targname: DQ-HER config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G160L wavelength: 1150-2510 num_exp: 1 time_per_exp: 2397.60S fluxnum_1: 1 priority: 2 param_1: READ-TIME=4.44 comment_1: DQ HER TIME-RESOLVED comment_2: (ASYNCHRONOUS). ! linenum: 27.000 targname: DQ-HER config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G190H num_exp: 1 time_per_exp: 2400S fluxnum_1: 1 priority: 2 comment_1: DQ HER AT MAX ! ! end of exposure logsheet scan_data: line_list: 18.0, 23.0 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: 18.1, 23.1 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