! File: 4377C.PROP ! Database: PEPDB ! Date: 20-FEB-1994:23:50:50 coverpage: title_1: SOFT X-RAY TRANSIENTS: OUTBURSTS IN BLACK HOLE ACCRETION DISKS sci_cat: HOT STARS sci_subcat: X-RAY BINARIES proposal_for: GO targ_of_opp: Y pi_fname: KEITH pi_lname: HORNE pi_inst: STSCI pi_country: USA hours_pri: 9.33 num_pri: 1 fos: Y funds_length: 12 off_fname: HERVEY off_mi: P. off_lname: STOCKMAN off_title: DEPUTY DIRECTOR off_inst: 3470 off_addr_1: 3700 SAN MARTIN DRIVE off_city: BALTIMORE off_state: MD off_zip: 21218 off_country: USA off_phone: 410-338-4730 ! end of coverpage abstract: line_1: We will observe soft X-ray transients (SXTs) as targets of opportunity line_2: using the FOS at UV wavelengths. This is part of an extensive line_3: multiwavelength campaign to monitor newly discovered SXTs in outburst line_4: and throughout the subsequent decline. Recent work establishes that a line_5: high proportion of SXTs harbor black holes, so these observations provide line_6: an unrivalled opportunity to obtain high quality data from an accreting line_7: black hole. UV data is a keystone of the multiwavelength campaign because line_8: the disk regions of interest radiate predominantly in the UV. Emission line_9: lines will allow us to probe the kinematics of the inner disk region. line_10: We will examine the reprocessed X-ray flux emitted in the UV, and the line_11: UV flux generated by viscous heating in the accretion flow. line_12: Multiwavelength observations will probe the changing morphology of the line_13: accretion flow throughout the outburst. The observations will yield a line_14: detailed quantitative test of the thermal disk instability model for line_15: SXT outbursts. The interpretation of FOS observations of the SXT Nova line_16: Muscae 1991 demonstrated the critical importance to this test of line_17: recording the UV and optical spectrum during the decline. ! ! end of abstract general_form_proposers: lname: HORNE fname: KEITH title: PI inst: STSCI country: USA ! lname: CHENG fname: FUHUA inst: STSCI country: USA ! lname: SHRADER fname: CHRIS mi: R. inst: NASA GODDARD SPACE FLIGHT CENTER country: USA ! lname: HASWELL fname: CAROLE mi: A. inst: STSCI country: USA ! lname: CHEN fname: WAN inst: NASA GODDARD SPACE FLIGHT CENTER country: USA ! lname: LIVIO fname: MARIO inst: STSCI country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We plan 1 visit to the target in quiescence. Details of the line_2: timing of the visit and the exposure times are given in section 4b. line_3: We plan to observe the target SXT with the FOS in each of the line_4: following modes: line_5: Blue digicon / G160L, PRISM line_6: Red digicon / G270H, G400H, PRISM line_7: to obtain spectral coverage from 1100A to 6000A. These exposures line_8: will operate in RAPID mode, with READ-TIME=6.18s. This allows line_9: us to monitor short timescale variability, with good spectral line_10: resolution (SUB-STEP=4). The exposures are interleaved to allow line_11: coverage of variations around the binary orbit cycle. ! question: 4 section: 1 line_1: The HST/FOS observations will be wholly complementary to IUE observations line_2: in several important ways. The IUE instruments have limited dynamic range, line_3: and are incapable of obtaining measurements of sufficient signal-to-noise line_4: to address a number of important scientific issues. The broad, high excitation line_5: lines are rarely, if ever resolved above the instrumental broadening of IUE's line_6: spectrograph in low resolution mode, so that no real kinematic information line_7: is obtainable. The FOS with its higher spectral resolution will easily resolve line_8: such features. Also of importance is a precise determination of the galactic line_9: reddening correction. The 2000-2400A region is the least sensitive part of line_10: IUEs detectors, limiting the accuracy with which E(B-V) can be determined. line_11: FOS observations of Nova Muscae, determined E(B-V) to within a few percent. line_12: The combination of higher signal-to-noise continuum measurement over a broader line_13: band-pass than is possible with IUE can more significantly constrain the types line_14: of continuum model testing we discuss in section. By using the RAPID mode of line_15: the FOS we will also obtain higher time resolution than is possible with IUE. line_16: Finally, the greater sensitivity of HST will allow us to sample the UV emission line_17: over a much broader temporal baseline then has been possible with IUE (e.g. line_18: Nova Muscae 1991 became undetectable by IUE after about 4.5 months). ! question: 4 section: 2 line_1: We plan 1 visit to the target at quiescence. The following table line_2: gives details of the observing strategy, aiming to record the line_3: spectrum and light curve of GROJ0422+32. line_4: FOS/RD TA1, TA2, PRISM, G270H, PRISM, G400H line_5: 8 35 8 35 line_6: FOS/BL TA1, TA2, PRISM, G160L, PRISM, G160L, PRISM, G160L, PRISM line_7: 8 82 8 82 8 82 8 line_8: The numbers in the table above give exposure times in minutes. line_9: All observations are in RAPID mode with READ-TIME=6.18s. line_10: Interleaved prism exposures aid in combining spectra of variable line_11: target, and serve to monitor binary orbit variations. line_12: At Peg Stanley's request we've broken the proposal into 2 scheduling line_13: units to make it easier to schedule. This compromises science line_14: unless the two units are scheduled close together in time. ! question: 5 section: 1 line_1: The planned observations are now reduced to one visit because HST line_2: scheduling delays have allowed GROJ0422+32 to fade considerably, line_3: essentially back to its quiescent level. Cycle 1 HST observations line_4: of the SXT A0620-00, taken 14 years after its 1975 outburst, showed line_5: very low ultraviolet flux, indicating that accretion to the black line_6: hole had essentially halted. The present observations of GROJ0422+32 line_7: will test whether accretion is similarly halted, or whether it line_8: continues to occur in the early quiescent phase following line_9: its Aug 1992 outburst. The observations should therefore be made line_10: as soon as possible, subject to the Cycle 3 TAC requirement that line_11: this TOO proposal must not unduely disrupt the normal scheduling line_12: process. ! question: 7 section: 1 line_1: The data reduction will be done at the STScI where we have all line_2: the experience and the means necessary to guarantee a high quality line_3: outcome. ! question: 8 section: 1 line_1: There is a significant likelihood of a major SXT occurring during the line_2: duration of this line_3: proposal. Recurrence times of an individual sources vary greatly, but there line_4: has been line_5: over the last 4 years about one major event per year. line_6: These events are readily detectable by the Burst and Transient Source line_7: Experiment (BATSE) onboard Compton GRO. For example, several recent, line_8: much less dramatic events were discovered: a recurrent outbursts of 4U 1543-47 line_9: in April 1992 (Harmon, B.A. et al. 1992 IAU Circular no. 5504) and EXO 1846-031 line_10: (Shrader,C.R. and Wagner,R.M. in preparation). At the time of this writing line_11: (phase I), a new transient event has been discovered, and localized to an line_12: accuracy of 0.2 degrees similarities (Harmon, et al. 1992 IAU circ. 5584). line_13: Since the distance, the intrinsic brightness,and the galactic line_14: extinction are all totally unknown prior to an outburst, we will need to line_15: update our detailed observation plan prior to activation of the program. As line_16: discussed in other sections of the proposal, our complementary target of line_17: opportunity programs on IUE and Compton GRO will supply us with the necessary line_18: information. As discussed in section 4, we will then use information obtained line_19: through our IUE target of opportunity program to assess the feasibility and line_20: scientific value of HST observations. ! question: 9 section: 1 line_1: CS: line_3: Cycle 1: line_4: GO-3232 "Observations of X-ray nova Muscae 1991" [CoI] line_6: KH: line_8: Cycle 1: line_9: GO-3232 "Observations of X-ray nova Muscae 1991" [CoI] line_10: GO-2380 "Instabilities in accretion disks and the outbursts line_11: of dwarf novae" [PI] line_12: GO-2334 "Ultraviolet spectroscopy of the black hole A0620-00"[CoI] line_13: Cycle 2: line_14: GO-3578 "Line Eclipse Mapping of an Accretion Disk Wind" [CoI] line_15: GO-3824 "A search for silicon and carbon in GP Com" [CoI] line_16: GO-3600 "Oscillations, flaring, and tomography of AE Aquarii"[PI] line_17: GO-3683 "Accretion disk mapping in eclipsing cataclysmic line_18: variables" [PI] line_19: GO-3836 "Spectroscopic Observations of the Exposed line_20: WDs in the Dwarf Novae U Gem, WZ Sag, and VW Hyi" [CoI] line_22: GO-3232, GO-2334 are related to present project. ! question: 9 section: 2 line_1: GO-2334: FOS spectra showed A0620-00 to be much fainter than line_2: expected, suggesting that the accretion disk viscosity shuts line_3: off completely in the quiescent periods between the outbursts of SXTs. line_4: GO-2380: FOS spectra of the eclipsing dwarf nova OY Car in line_5: quiescence (Dec 1991) and on the decline following a superoutburst line_6: (Apr-Jul 1992) are being used to discriminate between the disk line_7: instability and mass-transfer instability models of dwarf nova line_8: outbursts. A paper on the quiescent eclipse data has been accepted line_9: by the ApJ, while the data obtained following the superoutburst are line_10: under analysis. line_11: GO-3232: By combining HST/FOS, IUE, optical and x-ray spectra line_12: of Nova Muscae on the decline from outburst we place limits on the line_13: mass of the putative black hole in this system, and show that line_14: the cooling front predicted by disk instability model was not seen. line_15: a paper has been published in the ApJ 1992 October issue. line_16: GO-3578 will use HRS to investigate line profile changes during line_17: the eclipse of an accretion disk wind. line_18: GO-3600 will use FOS to investigate oscillations and flickering line_19: in an enigmatic CV with a magnetized and rapidly spinning accreting line_20: white dwarf. line_21: GO-3683 will obtain FOS observations of the eclipsing dwarf nova line_22: IP Peg in quiescence and on decline from an outburst to search for the line_23: cooling front in the disk as it cools and to study the disk structure. ! question: 9 section: 3 line_1: GO-3824 aims to determine metal abundances in the nearly pure line_2: helium disk in the ultra-short period system GP Com. line_3: GO-3836 is a GHRS study of white dwarfs in three quiescent dwarf novae. ! question: 9 section: 4 line_1: "The HST observations of X-ray Nova Muscae 1991 and its spectral line_2: evolution" F. H. Cheng, K. Horne, N. Panagia, C. R., Shrader, line_3: R. Gilmozzi, F. Paresce and Lund, ApJ, 1992, 397, 664. line_5: "The Dim Inner Accretion Disk of the Quiescent Black Hole A0620-00" line_6: J. McClintock, K. Horne, R. Remillard submitted. line_8: "HST Eclipse Mapping of Dwarf Nova OY Car in Quiescence: An `FeII line_9: Curtain' with Mach ~ 6 Velocity Dispersion Veils the White Dwarf" line_10: K. Horne, T. Marsh, F. H. Cheng, I. Hubeny and T. Lanz, ApJ, 1993, line_11: accepted. ! question: 10 section: 1 line_1: Salary and basic computer facilities are being provided for the P.I. line_2: and most of the Co-Is. ! !end of general form text general_form_address: lname: Horne fname: Keith category: PI inst: STScI addr_1: 3700 San Martin Drive city: Baltimore state: MD zip: 21218 country: USA phone: 410-338-4955 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: GROJ0422+32 name_2: NOVA-PERSEI-1992 descr_1: A,161,162,164,165 pos_1: RA-OFF = +0.218S +/- 0.002S, pos_2: DEC-OFF = -22.27" +/- 0.2", pos_3: FROM 2 equinox: 2000 comment_1: OFFSET FROM 2 (MOVE E AND S) comment_2: AUG 13.17 1993 UT, RISE comment_3: AUG 25 1993 IUE SPECTRUM comment_4: APPROX FNU=NU**1/3 DE-REDDENED. comment_5: OBJECT NOT APPARENT ON GASP PLATES comment_6: POSN FROM MARK WAGNER ASTROMETRY comment_7: ASSUME FNU=NU**1/3, V=20.0, comment_8: E(B-V)=0.4 FOR EXP. CALCS. comment_9: RA = 04H 21M 42.787S +/- 0.2", comment_10: DEC = +32D 54' 27.09" +/- 0.2" fluxnum_1: 1 fluxval_1: V = 15.1 +/- 0.2 fluxnum_2: 2 fluxval_2: E(B-V) = 0.4 +/- 0.07 fluxnum_3: 3 fluxval_3: F-CONT(1500)= 1.0 +/- 0.25 E-14 ! targnum: 2 name_1: GROJ0422-OFFSET descr_1: I,603 pos_1: RA = 04H 21M 42.569S +/- 0.2", pos_2: DEC =+32D 54' 49.36" +/- 0.2" equinox: 2000 comment_1: OFFSET STAR comment_2: POSN FROM MARK WAGNER ASTROMETRY comment_3: OFFSET STAR IS NORTH AND SLIGHTLY comment_4: WEST OF GRO J0422. CLOSE ENOUGH comment_5: THAT NO ADDNL GUIDE STAR ACQS REQD. fluxnum_1: 1 fluxval_1: V = 16.69 +/- 0.2 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.100 targname: GROJ0422-OFFSET config: FOS/RD opmode: ACQ/PEAK aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 10S priority: 1 param_1: SEARCH-SIZE-X=1, param_2: SEARCH-SIZE-Y=4, param_3: SCAN-STEP-Y=1.4, req_1: ONBOARD ACQ FOR 1.2; req_2: SEQUENTIAL 1.1 - 3.2 NO GAP ; req_3: CYCLE 3 / 1.1 - 3.2 ; req_4: TARG OF OPP / 1.1 - 3.2 ; req_5: GROUP 1.1-11 WITHIN 2D; comment_1: OBSERVE ASAP. comment_2: B-V UNKNOWN. comment_3: OK TO RE-ORDER EXPOSURES, BUT comment_4: 2.1 AND 3.1 NOT IN SAME HST ORBIT. comment_5: TO PERMIT COORDINATED OBSERVATIONS, comment_6: PLEASE NOTIFY CO-I, CAROLE HASWELL. ! linenum: 1.200 targname: GROJ0422-OFFSET config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 15S priority: 1 param_1: SEARCH-SIZE-X=6, param_2: SEARCH-SIZE-Y=2, param_3: SCAN-STEP-X=0.7, param_4: SCAN-STEP-Y=0.7, req_1: ONBOARD ACQ FOR 1.3; comment_1: GASP PLATE EXTRACTIONS FOR THIS comment_2: FIELD HAVE ERRORS ~1". comment_3: USING PRECISE (0.2") ASTROMETRY comment_4: FROM MARK WAGNER FOR COORDS & comment_5: AND OFFSETS. SCAN PATTERN COVERS comment_6: DISCREPANCY BETWEEN GASP & WAGNER ! linenum: 1.300 targname: GROJ0422-OFFSET config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 15S priority: 1 param_1: SEARCH-SIZE-X=3, param_2: SEARCH-SIZE-Y=3, param_3: SCAN-STEP-X=0.35, param_4: SCAN-STEP-Y=0.35, req_1: ONBOARD ACQ FOR 2.1-3.2; comment_1: ACQUIRE WITH FOS/RD TO MINIMIZE TIME. ! linenum: 2.100 targname: GROJ0422+32 config: FOS/RD opmode: RAPID aperture: 4.3 sp_element: PRISM num_exp: 1 time_per_exp: 475.86S priority: 1 param_1: READ-TIME=6.18 comment_1: NOT IN SAME ORBIT AS 3.1 ! linenum: 2.200 targname: GROJ0422+32 config: FOS/RD opmode: RAPID aperture: 4.3 sp_element: G270H num_exp: 1 time_per_exp: 2095.02S priority: 1 param_1: READ-TIME=6.18 comment_1: PLEASE EXTEND EXPOSURE TO comment_2: FILL OUT SPACECRAFT ORBIT ! linenum: 3.100 targname: GROJ0422+32 config: FOS/RD opmode: RAPID aperture: 4.3 sp_element: PRISM num_exp: 1 time_per_exp: 475.86S priority: 1 param_1: READ-TIME=6.18 comment_1: NOT IN SAME ORBIT AS 2.1 ! linenum: 3.200 targname: GROJ0422+32 config: FOS/RD opmode: RAPID aperture: 4.3 sp_element: G400H num_exp: 1 time_per_exp: 2095.02S priority: 1 param_1: READ-TIME=6.18 comment_1: PLEASE EXTEND EXPOSURE TO comment_2: FILL OUT SPACECRAFT ORBIT ! linenum: 4.100 targname: GROJ0422-OFFSET config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 30S priority: 1 param_1: SEARCH-SIZE-X=1, param_2: SEARCH-SIZE-Y=4, param_3: SCAN-STEP-Y=1.4, req_1: ONBOARD ACQ FOR 4.2; req_2: SEQUENTIAL 4.1 - 11 NO GAP ; req_3: CYCLE 3 / 4.1 - 11 ; req_4: TARG OF OPP / 4.1 - 11 ; comment_1: OBSERVE ASAP. comment_2: B-V UNKNOWN. comment_3: TO PERMIT COORDINATED OBSERVATIONS, comment_4: PLEASE NOTIFY CO-I, CAROLE HASWELL. comment_5: DO FOS/RD ACQ IF 4.1 - 4.3 WILL NOT comment_6: SCHEDULE. ! linenum: 4.200 targname: GROJ0422-OFFSET config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 49S priority: 1 param_1: SEARCH-SIZE-X=6, param_2: SEARCH-SIZE-Y=2, param_3: SCAN-STEP-X=0.7, param_4: SCAN-STEP-Y=0.7, req_1: ONBOARD ACQ FOR 4.3; ! linenum: 4.300 targname: GROJ0422-OFFSET config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 49S priority: 1 param_1: SEARCH-SIZE-X=3, param_2: SEARCH-SIZE-Y=3, param_3: SCAN-STEP-X=0.35, param_4: SCAN-STEP-Y=0.35, req_1: ONBOARD ACQ FOR 5-11; ! linenum: 5.000 targname: GROJ0422+32 config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: PRISM num_exp: 1 time_per_exp: 475.86S priority: 1 param_1: READ-TIME=6.18 ! linenum: 6.000 targname: GROJ0422+32 config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G160L num_exp: 1 time_per_exp: 4919.28S priority: 1 param_1: READ-TIME=6.18 comment_1: SPLIT/EXTEND EXPOSURE TO comment_2: FILL OUT SPACECRAFT ORBITS ! linenum: 7.000 targname: GROJ0422+32 config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: PRISM num_exp: 1 time_per_exp: 475.86S priority: 1 param_1: READ-TIME=6.18 ! linenum: 8.000 targname: GROJ0422+32 config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G160L num_exp: 1 time_per_exp: 4919.28S priority: 1 param_1: READ-TIME=6.18 comment_1: SPLIT/EXTEND EXPOSURE TO comment_2: FILL OUT SPACECRAFT ORBITS ! linenum: 9.000 targname: GROJ0422+32 config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: PRISM num_exp: 1 time_per_exp: 475.86S priority: 1 param_1: READ-TIME=6.18 ! linenum: 10.000 targname: GROJ0422+32 config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G160L num_exp: 1 time_per_exp: 4919.28S priority: 1 param_1: READ-TIME=6.18 comment_1: SPLIT/EXTEND EXPOSURE TO comment_2: FILL OUT SPACECRAFT ORBITS ! linenum: 11.000 targname: GROJ0422+32 config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: PRISM num_exp: 1 time_per_exp: 475.86S priority: 1 param_1: READ-TIME=6.18 ! ! end of exposure logsheet ! No scan data records found