! $Id: 5499,v 7.1 1994/07/27 18:40:19 pepsa Exp $ coverpage: title_1: SOFT X-RAY TRANSIENTS: OUTBURSTS IN BLACK HOLE ACCRETION DISKS title_2: CYCLE 4 - HIGH 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: 10.34 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 determine the relative strengths of the reprocessed X-ray flux emitted line_11: in the UV, and the 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. FOS work on Nova Muscae 1991 demonstrated the critical line_16: importance to this test of recording the UV and optical spectrum line_17: during the decline. An echo-mapping experiment during the bright phase of the line_18: outburst will measure the size of the reprocessing regions in the accretion disk line_19: and/or the radius of the companion star orbit using the FOS to obtain line_20: simultaneous 1100-2500A spectra and optical photometry with 2s time resolution. ! ! end of abstract general_form_proposers: lname: HORNE fname: KEITH title: PI inst: UNIVERSITY OF UTRECHT country: THE NETHERLANDS ! lname: LIVIO fname: MARIO inst: STSCI country: USA ! lname: HASWELL fname: CAROLE mi: A. 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: CHEN fname: WAN inst: NASA GODDARD SPACE FLIGHT CENTER country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We plan to line_2: observe the target SXT with the FOS in each of the following high resolution line_3: modes: line_4: Blue digicon / G130H line_5: Blue digicon / G190H line_6: Red digicon / G270H line_7: Red digicon / G400H line_8: to obtain spectral coverage from 1100A to 4800A. We line_9: will operate in RAPID mode, with READ-TIME=6.18s. This allows line_10: us to monitor short timescale variability. line_11: Additionally, on the first two visits we will spend 20 minutes with the line_12: FOS/BLUE/G160L configuration in order to record simultaneous white light line_13: photometry (with order 0) and low spectral resolution UV spectroscopy (with line_14: order 1). This will provide the data for the echo mapping experiment described line_15: in section 2. ! question: 4 section: 1 line_1: HST is needed for several reasons. By using the RAPID mode of the FOS, we will line_2: obtain higher time resolution than is possible with IUE, so we can monitor the line_3: expected rapid variations in emission from an accreting black hole. The echo- line_4: mapping observations we propose depend on this HST capability, as well as the line_5: unique ability to obtain simultaneous UV spectra and optical photometry. line_7: The IUE instruments have limited dynamic range and are incapable of obtaining line_8: measurements of sufficient signal-to-noise to address a number of important line_9: scientific issues. The emission lines in SXTs are rarely, if ever, resolved line_10: above the instrumental broadening of IUE's spectrograph in low resolution mode, line_11: so that no kinematic information is obtainable; in addition many lines are only line_12: marginally detected with IUE. HST/FOS with higher spectral resolution and light line_13: gathering power will easily resolve these features. line_15: Precise determination of the galactic reddening correction, based on removal of line_16: the 2200A decrement is of critical importance. Small uncertainties in E(B-V) can line_17: lead to substantial errors in the actual blue-UV source luminosity and spectral line_18: slope which is crucial to continuum modelling, and to source distance line_19: measurements. Figure 2 shows the dramatic advantage HST has over IUE in this; line_20: the FOS observations of Nova Muscae determined E(B-V) to within a few percent. ! question: 4 section: 2 line_1: line_2: We plan a total of 6 visits to the target throughout the decline from outburst. line_3: The table below gives details: line_5: exposure times (minutes) line_6: ------------------------------------------------ line_8: FOS blue blue red red blue line_9: visit t V g130h g190h g270h g400h G160L line_10: (days) mag exposure times (minutes) line_12: 1 0 13 6.72m 6.72m 6.72m 6.72m 20m line_13: 2 10 13.27 6.12m 6.12m 6.12m 6.12m 20m line_14: 3 20 13.54 6.12m 6.12m 6.12m 6.12m line_15: 4 30 13.18 6.12m 6.12m 6.12m 6.12m line_16: 5 60 14.63 6.12m 6.12m 6.12m 6.12m line_18: 6 90 15.44 9.00m 6.12m 6.12m 6.12m line_20: The exposure times, and estimated V magnitudes were calculated assuming line_21: the Nova Muscae light curve and aiming for 100 counts / Angstrom, with a line_22: minimum of 6.12 minutes exposure. Adjustments to increase efficiency line_23: were made. The time of visit is measured in days from the first visit. ! question: 4 section: 3 line_1: question 4, section 2 continued.... line_2: first observation of the target. line_4: The first four visits are separated by 10 days to allow us to monitor the line_5: changes in the spectrum near the outburst maximum, when the break in the line_6: slope of the spectrum should move through the UV to the optical part of line_7: the spectrum. The following visits are separated by 30 days line_8: to follow the accretion disk through the decline, and to catch the line_9: secondary maximum ~90 days after peak. ! question: 4 section: 4 line_1: Question 4, section 1 continued..... line_2: The greater sensitivity of HST will allow us to sample the ultraviolet emission line_3: over a much broader temporal baseline then has been possible with IUE (e.g. line_4: Nova Muscae 1991 became undetectable by IUE after about 4.5 months). ! question: 5 section: 1 line_1: The observations, although not strictly "time critical", should be made as soon line_2: as possible when an optical identification is made after the outburst. As we line_3: established in section 2, the earlier the source is observed, the more likely line_4: we are to make truly exciting discoveries. line_6: The echo-mapping observations will allow us to probe the geometry of the line_7: accretion flow on the first two visits. The success of this part of the line_8: program hinges on observing the source while the X-ray and UV flux is high, line_9: leading to substantial reprocessed flux in the optical. line_11: The test of the disk instability model, which is described in detail in line_12: section 2, also requires prompt observations to be fully successful. It is line_13: important to observe the disk from as early in the outburst as possible, to line_14: ensure we will see the predicted break in the spectral slope move through the line_15: UV. With the program of visits we describe in section 4b, we will be able line_16: to unequivocably determine if this occurs, and hence make a rigorous test line_17: of the model. line_19: In addition to these crucial scientific motivations, we point out that the SXT line_20: flux decreases with time (e.g. at a rate of 0.6-1 magnitude per month for Nova line_21: Muscae), and any delay in scheduling will inevitably result in a loss of quality line_22: in the data obtained. ! ! question: 8 section: 1 line_1: There is a significant likelihood of a major transient event occurring line_2: during the approximately 1-year duration of this proposal. Although the line_3: recurrence times of an individual sources vary greatly, and are unpredictable, line_4: there have been over the last 5 years approximately one major event per year: line_5: GS2000+25 (April, 1988), GS2023+338 = V404 Cyg (May 1989) and GS1124-684 = line_6: Nova Muscae 1991 (January 1991), and GRO J0422+32 (August, 1992). The latter line_7: clearly demonstrates the capabilities of GRO/BATSE to discover and monitor line_8: the hard X-ray emission from events of this magnitude. Figure 1 (courtesy of line_9: the NASA/MSFC BATSE Consortium) is a 20-300 keV light curve of GRO J0422+32 line_10: derived from the BATSE occultation analysis of the BATSE discriminator-rate line_11: data. The peak intensity corresponds to approximately 3X that of the Crab. line_12: BATSE has also discovered one and possibly two SXT events of much lower line_13: peak intensity; a recurrent outbursts of 4U 1543-47 in April 1992 (Harmon, line_14: B.A. et al. 1992 IAU Circular no. 5504) and possibly EXO 1846-031 (peak line_15: intensities of < 1 Crab). line_17: We emphasize that a full feasibility assessment, based on prompt results line_18: from ground-based observatories and/or IUE will be made prior to requesting line_19: activation of this program. SXTs typically lie in the plane of the galaxy line_20: at > 1 kpc and can be heavily obscured in the blue-UV by dust extinction. line_21: For example, GS2000+25, whose peak brightness exceeded that of Nova Muscae line_22: 1991 by 50-60%, was so heavily reddened that it brightened to only 18 line_23: visual magnitudes and was undetecable by IUE (Shrader, C.R., 1988, IAU 4605). ! question: 8 section: 2 line_1: question 8, section 1 continued.... line_2: V404 Cyg, which was similarly dramatic in X-rays, brightened to a line_3: visual of magnitude about 12, but had a color excess perhaps as high as line_4: 1.6. It was marginally detected longward of 2600A by IUE, but it would line_5: not have been a suitable source for the work proposed here. line_7: As discussed in other sections of the proposal, our complementary target of line_8: opportunity programs will supply us with the necessary line_9: information for fully evaluating such feasibility considerations. line_11: We have no related Cycle 4 proposals, but we do have an accepted Cycle 3 line_12: TOO proposal. ! question: 9 section: 1 line_1: Cycle 1: line_2: GO-3232 "Observations of X-ray nova Muscae 1991" [CS,KH,CoIs] line_3: GO-2380 "Instabilities in accretion disks and the outbursts line_4: of dwarf novae" [KH,PI] line_5: GO-2334 "Ultraviolet spectroscopy of the black hole A0620-00" [KH,CoI] line_7: Cycle 2: line_8: GO-3578 "Line Eclipse Mapping of an Accretion Disk Wind" [KH,CoI] line_9: GO-3824 "A search for silicon and carbon in GP Com [KH,CoI] line_10: GO-3600 "Oscillations, flaring, and tomography of AE Aquarii [KH,PI] line_11: GO-3683 "Accretion disk mapping in eclipsing cataclysmic line_12: variables" [KH,PI] line_13: GO-3836 "Spectroscopic Observations of the Exposed line_14: WDs in the Dwarf Novae U Gem, WZ Sag, and VW Hyi" [KH,CoI] line_16: Cycle 3: line_17: GO-3484 "Probing the Nuclear Regions of the Seyfert Galaxy line_18: NGC 5548" [KH,CoI] line_19: GO-4271 "Testing the Star-Disk Connection: CIV and MgII Maps line_20: of Disks" [KH,PI] line_21: GO-4377 "Soft X-Ray Transients: Outbursts in Black Hole line_22: Accretion disks." [KH,PI. ML,CH,FC,CS,WC,CoIs] line_23: GO-4589 "Energy Balance & Emission Lines in DQ Herculis Stars" [CH,CoI] ! question: 9 section: 2 line_1: Cycle 1: line_2: GO-2334: FOS spectra showed A0620-00 to be much fainter than expected, line_3: suggesting that the accretion disk viscosity shuts off completely line_4: in the quiescent periods between the outbursts of SXTs. line_5: GO-2380: FOS spectra of the eclipsing dwarf nova OY Car in quiescence line_6: (Dec 1991) and on the decline following a superoutburst (Apr-Jul 1992) line_7: are being used to discriminate between the disk instability and line_8: mass-transfer instability models of dwarf nova outbursts. line_9: A paper on the quiescent eclipse data is in draft form, while the data line_10: obtained following the superoutburst are under analysis. line_11: GO-3232: By combining HST/FOS, IUE, optical and x-ray spectra of Nova Muscae line_12: on the decline from outburst we place limits on the mass of the putative line_13: black hole in this system, and show that the cooling front predicted line_14: by disk instability model was not seen in this object. line_16: Cycle 2: line_17: GO-3578: HRS data has been taken to investigate line profile changes during line_18: the eclipse of an accretion disk wind. line_19: GO-3600: used FOS to investigate oscillations and flickering in an line_20: enigmatic CV with a magnetized and rapidly spinning accreting white dwarf. line_21: GO-3683: Some FOS observations of the eclipsing dwarf nova IP Peg have been line_22: taken. The remainder of the observations are pending. line_23: GO-3824: aims to determine metal abundances in the nearly pure helium disk ! question: 9 section: 3 line_1: line_2: ``The HST Observations of X-Ray Nova Muscae 1991 and its Spectral Evolution'' line_3: F.-H. Cheng, K. Horne, N. Panagia, C.R. Shrader, R. Gilmozzi, F. Paresce, line_4: N. Lund, (1992), ApJ, 397, 664. line_6: ``The Dim Inner Accretion Disk of the Quiescent Black Hole A0620-00'' line_7: J. McClintock, K. Horne, and R. Remillard, (199?), ApJL to be submitted. line_9: ``HST Eclipse Mapping of Dwarf Nova OY Car in Quiescence: An `FeII line_10: Curtain' with Mach ~ 6 Velocity Dispersion Veils the White Dwarf'' line_11: K. Horne, T. R. Marsh, F.-H. Cheng, I. Hubeny, and T. Lantz, (1993), ApJ, line_12: submitted. line_14: ``The Ultraviolet Pulsations of AE Aquarii as Observed With the Hubble Space line_15: Telescope'' K. Horne, M. Eracleous, E. L. Robinson, E. Zhang, T. R. Marsh, and line_16: J. Wood, Ap.J., (199?), to be submitted. ! question: 9 section: 4 line_1: question 9, section 2 continued.... line_2: in the ultra-short period system GP Com. Data is in hand; Carbon and line_3: Nitrogen were detected. line_4: GO-3836: Data aquisition is completed for this GHRS study of white dwarfs line_5: in three quiescent dwarf novae. There is preliminary evidence that the line_6: white dwarf rotation rates are small. line_8: Cycle 3: line_9: GO-3484: The 39 day FOS campaign is underway. Spectral variability suitable line_10: to the goals of the echo-mapping analysis has been detected. line_11: GO-4377: is a TOO program to obtain FOS spectra of the late stages of decline line_12: of an as yet unidentified SXT target. line_13: GO-4589: will use FOS to examine the pulsations and line profile modulations line_14: due to the rotation of the magnetically accreting white dwarf YY Dra. line_15: GO-4271: will measure the surface brightness of MgII and CIV emission as a line_16: function of orbital angular velocity in the disks. ! question: 10 section: 1 line_1: Salary and basic computer facilities are being provided for the P.I. and most line_2: of the Co-Is. ! !end of general form text general_form_address: lname: Horne fname: Keith category: PI inst: University of Utrecht addr_1: Sterrekundig Instituut addr_2: P.O. Box 80000 city: Utrecht, NL-3508 TA country: The Netherlands phone: 410-338-4955 ! ! end of general_form_address records ! No fixed target records found ! No solar system records found generic_targets: targnum_1: 1 targnum_2: 1 name_1: SXT descr_1: A,161,162,164.165 criteria_1: OBJECT WILL BE SELECTED BY criteria_2: PROPOSERS AFTER DISCOVERY WITH criteria_3: BATSE. comment_1: NEWLY OURBURSTING SXT WILL BE comment_2: FOLLOWED THROUGH DECLINE. comment_3: UNTIL OUTBURST OCCURS, DETAILS comment_4: OF LUMINOSITY, E(B-V), ETC comment_5: ARE UNKNOWN. OPTICAL/IUE DATA comment_6: WILL ENABLE EFFICIENCT USAGE comment_7: OF HST TIME ALLOCATION. comment_8: ASSUME FNU=NU**1/3 SPECTRUM comment_9: V=13+(TIME/36.8DAYS), E(B-V)=0.3 comment_10: FOR EXPOSURE LOGSHEET CALCS. ! ! end of generic targets exposure_logsheet: linenum: 1.100 targname: SXT config: FOS/RD opmode: ACQ/PEAK aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 0.34S priority: 1 param_1: SEARCH-SIZE-X=1 param_2: SEARCH-SIZE-Y=3 param_3: SCAN-STEP-Y=1.204 req_1: ONBOARD ACQ FOR 1.2 ; req_2: CYCLE 4 / 1.1-6.6; req_3: TARG OF OPP / 1.1-6.6 comment_1: FOS/BL ACQ/PEAK/MIRROR EXP=0.55S comment_2: ORDER OF EXP 1.3-1.8 UNIMPORTANT comment_3: OBSERVE ASAP AFTER TARGET ID'D comment_4: ACQ/PEAK EXP TIME FOR 10000 COUNTS comment_5: PLEASE NOTIFY P.I. WHEN DATES ARE comment_6: SCHEDULED OR CHANGED ! linenum: 1.200 targname: SXT config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 0.34S priority: 1 param_1: SEARCH-SIZE-X=6 param_2: SEARCH-SIZE-Y=2 param_3: SCAN-STEP-X=.602 param_4: SCAN-STEP-Y=.602 req_1: ONBOARD ACQ FOR 1.3-1.8 comment_1: FOS/BL ACQ/PEAK/MIRROR EXP=0.55S comment_2: ORDER OF EXP 1.3-1.8 UNIMPORTANT comment_3: IF FOS/BL FIRST comment_4: DO ACQ/PEAK comment_5: FOR FOS/BL/MIRROR comment_6: CLOSE TO (OVER?) BRIGHTNESS LIMIT ! linenum: 1.300 targname: SXT config: FOS/RD opmode: RAPID aperture: 4.3 sp_element: G270H num_exp: 1 time_per_exp: 401.7S priority: 1 param_1: READ-TIME=6.18 comment_1: DETAILED OBSERVING PLAN IS comment_2: LIKELY TO CHANGE WHEN comment_3: ACTUAL TARGET IS ID'D comment_4: THESE EXPOSURES ARE GUIDELINES comment_5: ONLY ! linenum: 1.400 targname: SXT config: FOS/RD opmode: RAPID aperture: 4.3 sp_element: G400H num_exp: 1 time_per_exp: 401.7S priority: 1 param_1: READ-TIME=6.18 comment_1: PLEASE CONSULT PI IF TIMING comment_2: CONSTRAINTS PRECLUDE SCHEDULING ! linenum: 1.500 targname: SXT config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 401.7S priority: 1 param_1: READ-TIME=6.18 ! linenum: 1.600 targname: SXT config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G190H num_exp: 1 time_per_exp: 401.7S priority: 1 param_1: READ-TIME=6.18 ! linenum: 1.800 targname: SXT config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G160L num_exp: 1 time_per_exp: 1198.92S priority: 1 param_1: READ-TIME=6.18 ! linenum: 2.100 targname: SXT config: FOS/RD opmode: ACQ/PEAK aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 0.44S priority: 1 param_1: SEARCH-SIZE-X=1 param_2: SEARCH-SIZE-Y=3 param_3: SCAN-STEP-Y=1.204 req_1: ONBOARD ACQ FOR 2.2 ; req_2: AFTER 1.1 BY 10D +/- 2D comment_1: FOS/BL ACQ/PEAK/MIRROR EXP=0.71S comment_2: ORDER OF EXP 2.3-2.8 UNIMPORTANT comment_4: ACQ/PEAK EXP TIME FOR 10000 COUNTS comment_5: PLEASE NOTIFY P.I. WHEN DATES ARE comment_6: SCHEDULED OR CHANGED ! linenum: 2.200 targname: SXT config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 0.44S priority: 1 param_1: SEARCH-SIZE-X=6 param_2: SEARCH-SIZE-Y=2 param_3: SCAN-STEP-X=.602 param_4: SCAN-STEP-Y=.602 req_1: ONBOARD ACQ FOR 2.3-2.8 comment_1: FOS/BL ACQ/PEAK/MIRROR EXP=0.71S comment_2: ORDER OF EXP 2.3-2.8 UNIMPORTANT comment_3: IF FOS/BL FIRST comment_4: DO ACQ/PEAK comment_5: FOR FOS/BL/MIRROR comment_6: CLOSE TO (OVER?) BRIGHTNESS LIMIT ! linenum: 2.300 targname: SXT config: FOS/RD opmode: RAPID aperture: 4.3 sp_element: G270H num_exp: 1 time_per_exp: 364.62S priority: 1 param_1: READ-TIME=6.18 comment_1: DETAILED OBSERVING PLAN IS comment_2: LIKELY TO CHANGE WHEN comment_3: ACTUAL TARGET IS ID'D comment_4: THESE EXPOSURES ARE GUIDELINES comment_5: ONLY ! linenum: 2.400 targname: SXT config: FOS/RD opmode: RAPID aperture: 4.3 sp_element: G400H num_exp: 1 time_per_exp: 364.62S priority: 1 param_1: READ-TIME=6.18 comment_1: PLEASE CONSULT PI IF TIMING comment_2: CONSTRAINTS PRECLUDE SCHEDULING ! linenum: 2.500 targname: SXT config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 364.62S priority: 1 param_1: READ-TIME=6.18 ! linenum: 2.600 targname: SXT config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G190H num_exp: 1 time_per_exp: 364.62S priority: 1 param_1: READ-TIME=6.18 ! linenum: 2.800 targname: SXT config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G160L num_exp: 1 time_per_exp: 1198.92S priority: 1 param_1: READ-TIME=6.18 ! linenum: 3.100 targname: SXT config: FOS/RD opmode: ACQ/PEAK aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 0.55S priority: 1 param_1: SEARCH-SIZE-X=1 param_2: SEARCH-SIZE-Y=3 param_3: SCAN-STEP-Y=1.204 req_1: ONBOARD ACQ FOR 3.2 ; req_2: AFTER 1.1 BY 20D +/- 2D comment_1: FOS/BL ACQ/PEAK/MIRROR EXP=0.91S comment_2: ORDER OF EXP 3.3-3.6 UNIMPORTANT comment_3: OBSERVE ASAP AFTER TARGET ID'D comment_4: ACQ/PEAK EXP TIME FOR 10000 COUNTS comment_5: PLEASE NOTIFY P.I. WHEN DATES ARE comment_6: SCHEDULED OR CHANGED ! linenum: 3.200 targname: SXT config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 0.55S priority: 1 param_1: SEARCH-SIZE-X=6 param_2: SEARCH-SIZE-Y=2 param_3: SCAN-STEP-X=.602 param_4: SCAN-STEP-Y=.602 req_1: ONBOARD ACQ FOR 3.3-3.6 comment_1: FOS/BL ACQ/PEAK/MIRROR EXP=0.91S comment_2: ORDER OF EXP 3.3-3.6 UNIMPORTANT comment_3: IF FOS/BL FIRST comment_4: DO ACQ/PEAK comment_5: FOR FOS/BL/MIRROR comment_6: CLOSE TO (OVER?) BRIGHTNESS LIMIT ! linenum: 3.300 targname: SXT config: FOS/RD opmode: RAPID aperture: 4.3 sp_element: G270H num_exp: 1 time_per_exp: 364.62S priority: 1 param_1: READ-TIME=6.18 comment_1: DETAILED OBSERVING PLAN IS comment_2: LIKELY TO CHANGE WHEN comment_3: ACTUAL TARGET IS ID'D comment_4: THESE EXPOSURES ARE GUIDELINES comment_5: ONLY ! linenum: 3.400 targname: SXT config: FOS/RD opmode: RAPID aperture: 4.3 sp_element: G400H num_exp: 1 time_per_exp: 364.62S priority: 1 param_1: READ-TIME=6.18 comment_1: PLEASE CONSULT PI IF TIMING comment_2: CONSTRAINTS PRECLUDE SCHEDULING ! linenum: 3.500 targname: SXT config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 364.62S priority: 1 param_1: READ-TIME=6.18 req_1: CYCLE 4; ! linenum: 3.600 targname: SXT config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G190H num_exp: 1 time_per_exp: 364.62S priority: 1 param_1: READ-TIME=6.18 ! linenum: 4.100 targname: SXT config: FOS/RD opmode: ACQ/PEAK aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 0.71S priority: 1 param_1: SEARCH-SIZE-X=1 param_2: SEARCH-SIZE-Y=3 param_3: SCAN-STEP-Y=1.204 req_1: ONBOARD ACQ FOR 4.2 ; req_2: AFTER 1.1 BY 30D +/- 2D comment_1: FOS/BL ACQ/PEAK/MIRROR EXP=1.17S comment_2: ORDER OF EXP 4.3-4.6 UNIMPORTANT comment_3: OBSERVE ASAP AFTER TARGET ID'D comment_4: ACQ/PEAK EXP TIME FOR 10000 COUNTS comment_5: PLEASE NOTIFY P.I. WHEN DATES ARE comment_6: SCHEDULED OR CHANGED ! linenum: 4.200 targname: SXT config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 0.71S priority: 1 param_1: SEARCH-SIZE-X=6 param_2: SEARCH-SIZE-Y=2 param_3: SCAN-STEP-X=.602 param_4: SCAN-STEP-Y=.602 req_1: ONBOARD ACQ FOR 4.3-4.6 comment_1: FOS/BL ACQ/PEAK/MIRROR EXP=1.17S comment_2: ORDER OF EXP 4.3-4.6 UNIMPORTANT comment_3: IF FOS/BL FIRST comment_4: DO ACQ/PEAK comment_5: FOR FOS/BL/MIRROR comment_6: 30 +/- 2 DAYS AFTER VISIT 1 (1.1-1.8) ! linenum: 4.300 targname: SXT config: FOS/RD opmode: RAPID aperture: 4.3 sp_element: G270H num_exp: 1 time_per_exp: 364.62S priority: 1 param_1: READ-TIME=6.18 comment_1: DETAILED OBSERVING PLAN IS comment_2: LIKELY TO CHANGE WHEN comment_3: ACTUAL TARGET IS ID'D comment_4: THESE EXPOSURES ARE GUIDELINES comment_5: ONLY ! linenum: 4.400 targname: SXT config: FOS/RD opmode: RAPID aperture: 4.3 sp_element: G400H num_exp: 1 time_per_exp: 364.62S priority: 1 param_1: READ-TIME=6.18 comment_1: PLEASE CONSULT PI IF TIMING comment_2: CONSTRAINTS PRECLUDE SCHEDULING ! linenum: 4.500 targname: SXT config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 364.62S priority: 1 param_1: READ-TIME=6.18 ! linenum: 4.600 targname: SXT config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G190H num_exp: 1 time_per_exp: 364.62S priority: 1 param_1: READ-TIME=6.18 ! linenum: 5.100 targname: SXT config: FOS/RD opmode: ACQ/PEAK aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 1.55S priority: 1 param_1: SEARCH-SIZE-X=1 param_2: SEARCH-SIZE-Y=3 param_3: SCAN-STEP-Y=1.204 req_1: ONBOARD ACQ FOR 5.2 ; req_2: AFTER 1.1 BY 60D +/- 5D comment_1: FOS/BL ACQ/PEAK/MIRROR EXP=2.50S comment_2: ORDER OF EXP 5.3-5.6 UNIMPORTANT comment_3: OBSERVE ASAP AFTER TARGET ID'D comment_4: ACQ/PEAK EXP TIME FOR 10000 COUNTS comment_5: PLEASE NOTIFY P.I. WHEN DATES ARE comment_6: SCHEDULED OR CHANGED ! linenum: 5.200 targname: SXT config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 1.55S priority: 1 param_1: SEARCH-SIZE-X=6 param_2: SEARCH-SIZE-Y=2 param_3: SCAN-STEP-X=.602 param_4: SCAN-STEP-Y=.602 req_1: ONBOARD ACQ FOR 5.3-5.6 comment_1: FOS/BL ACQ/PEAK/MIRROR EXP=2.50S comment_2: ORDER OF EXP 5.3-5.6 UNIMPORTANT comment_3: IF FOS/BL FIRST comment_4: DO ACQ/PEAK comment_5: FOR FOS/BL/MIRROR comment_6: 60 +/- 5 DAYS AFTER VISIT 1 (1.1-1.8) ! linenum: 5.300 targname: SXT config: FOS/RD opmode: RAPID aperture: 4.3 sp_element: G270H num_exp: 1 time_per_exp: 364.62S priority: 1 param_1: READ-TIME=6.18 comment_1: DETAILED OBSERVING PLAN IS comment_2: LIKELY TO CHANGE WHEN comment_3: ACTUAL TARGET IS ID'D comment_4: THESE EXPOSURES ARE GUIDELINES comment_5: ONLY ! linenum: 5.400 targname: SXT config: FOS/RD opmode: RAPID aperture: 4.3 sp_element: G400H num_exp: 1 time_per_exp: 364.62S priority: 1 param_1: READ-TIME=6.18 comment_1: PLEASE CONSULT PI IF TIMING comment_2: CONSTRAINTS PRECLUDE SCHEDULING ! linenum: 5.500 targname: SXT config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 364.62S priority: 1 param_1: READ-TIME=6.18 ! linenum: 5.600 targname: SXT config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G190H num_exp: 1 time_per_exp: 364.62S priority: 1 param_1: READ-TIME=6.18 ! linenum: 6.100 targname: SXT config: FOS/RD opmode: ACQ/PEAK aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 3.3S priority: 1 param_1: SEARCH-SIZE-X=1 param_2: SEARCH-SIZE-Y=3 param_3: SCAN-STEP-Y=1.204 req_1: ONBOARD ACQ FOR 6.2 ; req_2: AFTER 1.1 BY 90D +/- 5D comment_1: FOS/BL ACQ/PEAK/MIRROR EXP=5.2S comment_2: ORDER OF EXP 6.3-6.6 UNIMPORTANT comment_3: OBSERVE ASAP AFTER TARGET ID'D comment_4: ACQ/PEAK EXP TIME FOR 10000 COUNTS comment_5: PLEASE NOTIFY P.I. WHEN DATES ARE comment_6: SCHEDULED OR CHANGED ! linenum: 6.200 targname: SXT config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: MIRROR num_exp: 1 time_per_exp: 3.3S priority: 1 param_1: SEARCH-SIZE-X=6 param_2: SEARCH-SIZE-Y=2 param_3: SCAN-STEP-X=.602 param_4: SCAN-STEP-Y=.602 req_1: ONBOARD ACQ FOR 6.3-6.6 comment_1: FOS/BL ACQ/PEAK/MIRROR EXP=5.2S comment_2: ORDER OF EXP 6.3-6.6 UNIMPORTANT comment_3: IF FOS/BL FIRST comment_4: DO ACQ/PEAK comment_5: FOR FOS/BL/MIRROR comment_6: 90 +/- 5 DAYS AFTER VISIT 1 (1.1-1.8) ! linenum: 6.300 targname: SXT config: FOS/RD opmode: RAPID aperture: 4.3 sp_element: G270H num_exp: 1 time_per_exp: 364.62S priority: 1 param_1: READ-TIME=6.18 comment_1: DETAILED OBSERVING PLAN IS comment_2: LIKELY TO CHANGE WHEN comment_3: ACTUAL TARGET IS ID'D comment_4: THESE EXPOSURES ARE GUIDELINES comment_5: ONLY ! linenum: 6.400 targname: SXT config: FOS/RD opmode: RAPID aperture: 4.3 sp_element: G400H num_exp: 1 time_per_exp: 364.62S priority: 1 param_1: READ-TIME=6.18 comment_1: PLEASE CONSULT PI IF TIMING comment_2: CONSTRAINTS PRECLUDE SCHEDULING ! linenum: 6.500 targname: SXT config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 537.66S priority: 1 param_1: READ-TIME=6.18 ! linenum: 6.600 targname: SXT config: FOS/BL opmode: RAPID aperture: 4.3 sp_element: G190H num_exp: 1 time_per_exp: 364.62S priority: 1 param_1: READ-TIME=6.18 ! ! end of exposure logsheet ! No scan data records found