coverpage: title_1: BLACK HOLE BINARIES IN THE LMC sci_cat: STELLAR ASTROPHYSICS sci_subcat: X-RAY BINARIES proposal_for: GO/CAR cont_id: 3489 pi_fname: JOHN pi_mi: B pi_lname: HUTCHINGS pi_inst: DOMINION ASTROPHYSICAL OBSERVATORY pi_country: CANADA pi_phone: 604-363-0018 hours_pri: 13.30 hours_par: 0.70 num_pri: 2 num_par: 2 wf_pc: Y fos: Y hrs: Y time_crit: Y funds_amount: 28767 funds_length: 12 off_fname: JAMES off_mi: E off_lname: HESSER off_title: DIRECTOR off_inst: DOMINION ASTROPHYSICAL OBSERVATORY off_addr_1: 5071 W. SAANICH RD off_city: VICTORIA off_state: BC off_zip: V8X 4M6 off_country: CANADA off_phone: 604-363-0007 ! end of coverpage abstract: line_1: The endpoints of stellar evolution - white dwarfs, neutron stars and line_2: black holes - can be most directly studied when they occur in binary line_3: systems such as cataclysmic variables and X-ray binaries. However, only line_4: a handful of black-hole candidates have been found, and thus very little line_5: is known about their physical properties and associated accretion disks. line_6: Two black-hole X-ray binaries, LMC X-3 and CAL 87, are particularly line_7: suitable for investigation in the UV, where important diagnostic line_8: emission lines are present and where the disk structure can be modelled line_9: from the continuum. LMC X-3 has recently been found to have a line_10: precessing accretion disk (P = 200 days) allowing different parts of the line_11: disk to be observed over a timescale of months. CAL 87 (P orb 10.6hr) is line_12: the only known eclipsing black hole, so that observation throughout the line_13: eclipse will yield detailed information about the disk structure, line_14: particularly very near the collapsed star itself. ! ! end of abstract general_form_proposers: lname: HUTCHINGS fname: JOHN title: PI mi: B inst: DOMINION ASTROPHYSICAL OBSERVATORY country: CANADA ! lname: COWLEY fname: ANNE mi: P inst: ARIZONA STATE UNIVERSITY country: USA ! lname: CRAMPTON fname: DAVID inst: DOMINION ASTROPHYSICAL OBSERVATORY country: CANADA ! lname: SCHMIDKE fname: PAUL mi: C inst: ARIZONA STATE UNIVERSITY country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: For LMC X-3 we propose to obtain low dispersion GHRS spectra at two line_2: wavelength settings, to cover 1160-1750A at each observation. As the star line_3: is faint (17.5m), we will need to acquire by blind offset from a nearby line_4: brighter star, unless HST pointing improves. The observation will be repeated line_5: at five 200-day (disk precession) phases, at a fixed (1.7-day) line_6: orbital phase. line_8: If GHRS low dispersion observations are not possible, we would use the line_9: FOS with G130H and G190H gratings to cover the same spectral range. For line_10: FOS use, the target acquisition will be direct. line_12: For CAL 87, we propose to obtain FOS low dispersion (G160L) spectra line_13: at 6 binary phases, to model the continuum changes through the 10 hour line_14: orbit. We also propose to obtain FOS high dispersion (G130H) spectra line_15: of the C IV line at 3 binary phases, to measure the profile changes, and line_16: model the eclipse of the line-emitting region. line_18: We request parallel exposures with the PC to study the stellar line_19: population of the LMC in the neighbourhood of these binaries. ! question: 4 section: 2 line_1: line_2: For LMC X-3, we require minimum S/N of 20 per 2A (LSA resolution) with GHRS, line_3: and this leads to exposure estimates of 2 hours for the combined 2 grating line_4: settings, for each visit to the star. (This is true for observation line_5: with either GHRS or FOS, as throughput and efficiencies trade off roughly.) line_6: The UV flux of CAL 87 is not known (but will be after the cycle 1 GTO data line_7: are obtained). Best estimates require 10 minutes for the FOS low dispersion line_8: spectra to achieve a mean S/N of 10 over the UV continuum. The Si IV and line_9: C IV line data require a S/N of 20 per ~2A (1 arcsec aperture resolution) line_10: and we estimate exposures for this grating setting of 30 mins per visit. line_12: To sample the periods sufficiently, we require 5 or more visits to line_13: each system, making a total of ~14 hours integration time. ! question: 5 section: 3 line_1: The proposal requires observations at specific binary and precession line_2: phases to accomplish its science goals. We will specify windows of these line_3: phases as widely as possible, to facilitate scheduling, but the timing is line_4: an essential requirement. ! !end of general form text general_form_address: lname: HUTCHINGS fname: JOHN mi: B category: PI inst: DOMINION ASTROPHYSICAL OBSERVATORY addr_1: 5071 W. SAANICH RD city: VICTORIA state: BC zip: V8X 4M6 country: CANADA phone: 604-363-0018 telex: 049-7295 NRC DAO VIC ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: CAL87STAR descr_1: A, 139 pos_1: PLATE-ID=05ZW, pos_2: RA=5H 46M 50.3S+/-1", pos_3: DEC=-71D 10' 17.70"+/-1" equinox: 2000 fluxnum_1: 1 fluxval_1: V=12.3,TYPE=K0 ! targnum: 2 name_1: OFFSET-CAL87 descr_1: A, 133 pos_1: RA-OFF=-3.47S+/- 0.1S, pos_2: DEC-OFF=82.6" +/- 0.3", pos_3: FROM 1, pos_4: PLATE-ID=05ZW equinox: 2000 comment_1: UV FLUXES KNOWN FROM IUE. fluxnum_1: 1 fluxval_1: V=19.0 +/- 0.4,TYPE=F ! ! end of fixed targets ! No solar system records found generic_targets: targnum_1: 3 name_1: FIELD-NEAR-CAL87 descr_1: LMC FIELD criteria_1: WFPC2 PARALLEL OBSERVATION ! ! end of generic targets exposure_logsheet: linenum: 30.000 targname: CAL87STAR config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 3S priority: 1 req_1: ONBOARD ACQ FOR 30.1; req_2: CYCLE 4 / 30-34; req_3: SEQ 30-32.1 NO GAP; ! linenum: 30.100 targname: CAL87STAR config: FOS/BL opmode: ACQ/PEAK aperture: 0.3 sp_element: MIRROR num_exp: 1 time_per_exp: 3S priority: 1 param_1: SCAN-STEP-X=0.1, param_2: SCAN-STEP-Y=0.1, param_3: SEARCH-SIZE-X=4, param_4: SEARCH-SIZE-Y=4 req_1: ONBOARD ACQ FOR 30.5; ! linenum: 30.500 targname: OFFSET-CAL87 config: FOS/BL opmode: ACQ/PEAK aperture: 0.5 sp_element: MIRROR num_exp: 1 time_per_exp: 30S priority: 1 param_1: SCAN-STEP-X=0.3, param_2: SCAN-STEP-Y=0.3, param_3: SEARCH-SIZE-X=3, param_4: SEARCH-SIZE-Y=3, req_1: ONBOARD ACQ FOR 31-32.1; ! linenum: 31.000 targname: OFFSET-CAL87 config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G160L wavelength: 1150-2510 num_exp: 1 time_per_exp: 30M priority: 1 req_1: ZERO-PHASE JD2447506.80 +/- 0.02D; req_2: PERIOD 0.44268D +/- 0.00001D; req_3: PHASE 0.6 +/- 0.06 ! linenum: 32.000 targname: OFFSET-CAL87 config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G160L wavelength: 1150-2510 num_exp: 6 time_per_exp: 38M priority: 1 ! linenum: 32.100 targname: OFFSET-CAL87 config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G160L wavelength: 1150-2510 num_exp: 1 time_per_exp: 30M priority: 1 ! linenum: 33.000 targname: FIELD-NEAR-CAL87 config: WFPC2 opmode: IMAGE aperture: WFALL sp_element: F469N num_exp: 1 time_per_exp: 9320S priority: 1 req_1: PAR comment_1: INTENDED TO BE PARALLEL WITH 32 ! linenum: 34.000 targname: FIELD-NEAR-CAL87 config: WFPC2 opmode: IMAGE aperture: WFALL sp_element: F467M num_exp: 1 time_per_exp: 1700S priority: 1 param_1: CR-SPLIT=NO req_1: PAR comment_1: INTENDED TO BE PARALLEL WITH 31 ! ! end of exposure logsheet