! File: 4056C.PROP ! Database: PEPDB ! Date: 20-FEB-1994:06:49:49 coverpage: title_1: BINARIES IN GLOBULAR CLUSTERS 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: 2.68 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: NASA GODDARD SPACE FLIGHT CENTER country: USA ! lname: ALLEN fname: RICHARD mi: P. inst: UNIVERSITY OF ARIZONA country: USA ! ! end of general_form_proposers block general_form_text: question: 2 section: 1 line_1: ! question: 3 section: 1 line_1: WF/PC images of globular cluster interacting binaries will line_2: be obtained as acquistions for follow-up FOS spectra in line_3: cycle 3. If no interesting candidates are found, no line_4: followup spectra will be taken. If an interesting looking line_5: candidate is found, then follow-up spectra will be obtained line_6: in a later cycle, with the specific gratings to be used line_7: determined by the quality of the candidate. ! question: 4 section: 1 line_1: For this program, it is the high angular resolution of the line_2: HST which is most essential, although the UV capability is line_3: also exploited. The PC images will be used to search line_4: relatively crowded regions of Omega-Cen with the aim of line_5: optically selecting (via UV excess) a candidate for the line_6: globular cluster X-ray source. Follow-up FOS spectroscopy line_7: will be done in a later cycle if a suitable candidate is found. ! question: 5 section: 1 line_1: The images must be obtained NON-INT to avoid unecessary line_2: readout noise in these low S/N data ! 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. As a quick-look analysis, line_3: the PC multicolor images will simply be displayed and blinked to provide line_4: an initial search for candidates of unusual color. A more detailed line_5: examination of the images will come from DAOPHOT and DoPHOT (plus aperture) line_6: photometry of all of the stars. ! question: 8 section: 1 line_1: The PC images will be measured for precise target coordinates, so that the line_2: later FOS observations can be done as blind offsets from a nearby isolated line_3: star. ! 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: 1053, 3002, 3003, 3198, 3282 (Binaries in Globular Clusters); line_5: Among these related programs, data have been taken for SAO line_6: observations of M14 (proposals 3002 and 3003), and NGC6712 (proposal line_7: 1053). One relevant refereed paper has been published in ApJ Let. ! 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: Multicolor WF/PC images will be used to search for the optical counterparts of line_2: both central and noncentral X-ray sources. Objects identified through unusual line_3: colors will be observed with the FOS. ! !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: NGC5139 name_2: OMEGA-CEN descr_1: C,201,I,605 pos_1: RA =13H 26M 15.3S+/-0.1S, pos_2: DEC = -47D 06' 58" +/-1" equinox: 1950 fluxnum_1: 1 fluxval_1: SURF(V) = 16.7 +/-0.5 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 sequence_1: DEFINE sequence_2: PC targname: # config: PC opmode: IMAGE aperture: PC8-FIX sp_element: F336W wavelength: 3363 num_exp: 1 time_per_exp: 2000S fluxnum_1: 1 priority: 1 param_1: PRE-FLASH=YES, param_2: CR-SPLIT=NO req_1: SEQ 1-3 NO GAP; req_2: NON-INT / 1-3; req_3: POS TARG -5.4,+5.4 / 1-3; comment_1: PC PICTURES FOR SOURCE IDENTIFICATION. ! linenum: 2.000 sequence_1: DEFINE sequence_2: PC targname: # config: PC opmode: IMAGE aperture: PC8-FIX sp_element: F439W wavelength: 4385 num_exp: 1 time_per_exp: 2000S fluxnum_1: 1 priority: 1 param_1: PRE-FLASH=YES, param_2: CR-SPLIT=0.1 ! linenum: 3.000 sequence_1: DEFINE sequence_2: PC targname: # config: PC opmode: IMAGE aperture: PC8-FIX sp_element: F336W wavelength: 3363 num_exp: 1 time_per_exp: 2000S fluxnum_1: 1 priority: 1 param_1: PRE-FLASH=YES, param_2: CR-SPLIT=NO ! linenum: 4.000 sequence_1: USE sequence_2: PC targname: NGC5139 req_2: CYCLE 2/ 1-4; ! ! end of exposure logsheet ! No scan data records found