Page 1 PROPOSAL FOR HUBBLE SPACE TELESCOPE OBSERVATIONS ST ScI Use Only ID 5499 Report Date: 18-Jul-95:17:32 Version: ********** Check-in Date: ********** 1.Proposal Title: SOFT X-RAY TRANSIENTS: OUTBURSTS IN BLACK HOLE ACCRETION DISKS CYCLE 4 - HIGH ------------------------------------------------------------------------------------ 2. Scientific Category 3. Proposal For 4. Proposal Type 5. Continuation ID HOT STARS GO Target of Oppt. Sub Category X-RAY BINARIES ------------------------------------------------------------------------------------ 6. Principal Investigator Institution Country Telephone Keith Horne STSCI USA ------------------------------------------------------------------------------------ 7. Abstract We will observe soft X-ray transients (SXTs) as targets of opportunity using the FOS at UV wavelengths. This is part of an extensive multiwavelength campaign to monitor newly discovered SXTs in outburst and throughout the subsequent decline. Recent work establishes that a high proportion of SXTs harbor black holes, so these observations provide an unrivalled opportunity to obtain high quality data from an accreting black hole. UV data is a keystone of the multiwavelength campaign because the disk regions of interest radiate predominantly in the UV. Emission lines will allow us to probe the kinematics of the inner disk region. We will determine the relative strengths of the reprocessed X-ray flux emitted in the UV, and the UV flux generated by viscous heating in the accretion flow. Multiwavelength observations will probe the changing morphology of the accretion flow throughout the outburst. The observations will yield a detailed quantitative test of the thermal disk instability model for SXT outbursts. FOS work on Nova Muscae 1991 demonstrated the critical importance to this test of recording the UV and optical spectrum during the decline. An echo-mapping experiment during the bright phase of the outburst will measure the size of the reprocessing regions in the accretion disk and/or the radius of the companion star orbit using the FOS to obtain simultaneous 1100-2500A spectra and optical photometry with 2s time resolution. ------------------------------------------------------------------------------------ ------------------------------------------------------------------------------------ 9. Est obs time (hours) pri: 10.34 par: 0 10. Num targs pri: 1 par: 0 ------------------------------------------------------------------------------------ 11. Instruments requested: FOS ------------------------------------------------------------------------------------ ------------------------------------------------------------------------------------ Page 2 I. GENERAL FORM Proposal 5499 PI: Keith Horne Proposal Title: SOFT X-RAY TRANSIENTS: OUTBURSTS IN BLACK HOLE ACCRETION DISKS CYCLE 4 - HIGH ------------------------------------------------------------------------------------ 1. Proposers: Proposers Institution Country ESA ------------------------------------------------------------------------------------ Pi Keith Horne UNIVERSITY OF UTRECHT THE NETHERL Mario Livio STSCI USA Carole A. Haswell STSCI USA Fuhua Cheng STSCI USA Chris R. Shrader NASA GODDARD SPACE FLIGHT CENTER USA Wan Chen NASA GODDARD SPACE FLIGHT CENTER USA ------------------------------------------------------------------------------------ 3. Description of proposed observations. We plan to observe the target SXT with the FOS in each of the following high resolution modes: Blue digicon / G130H Blue digicon / G190H Red digicon / G270H Red digicon / G400H to obtain spectral coverage from 1100A to 4800A. We will operate in RAPID mode, with READ-TIME=6.18s. This allows us to monitor short timescale variability. Additionally, on the first two visits we will spend 20 minutes with the FOS/BLUE/G160L configuration in order to record simultaneous white light photometry (with order 0) and low spectral resolution UV spectroscopy (with order 1). This will provide the data for the echo mapping experiment described in section 2. Page 3 ------------------------------------------------------------------------------------ 4. Justification of need for HST observations. HST is needed for several reasons. By using the RAPID mode of the FOS, we will obtain higher time resolution than is possible with IUE, so we can monitor the expected rapid variations in emission from an accreting black hole. The echo- mapping observations we propose depend on this HST capability, as well as the unique ability to obtain simultaneous UV spectra and optical photometry. The IUE instruments have limited dynamic range and are incapable of obtaining measurements of sufficient signal-to-noise to address a number of important scientific issues. The emission lines in SXTs are rarely, if ever, resolved above the instrumental broadening of IUE's spectrograph in low resolution mode, so that no kinematic information is obtainable; in addition many lines are only marginally detected with IUE. HST/FOS with higher spectral resolution and light gathering power will easily resolve these features. Precise determination of the galactic reddening correction, based on removal of the 2200A decrement is of critical importance. Small uncertainties in E(B-V) can lead to substantial errors in the actual blue-UV source luminosity and spectral slope which is crucial to continuum modelling, and to source distance measurements. Figure 2 shows the dramatic advantage HST has over IUE in this; the FOS observations of Nova Muscae determined E(B-V) to within a few percent. We plan a total of 6 visits to the target throughout the decline from outburst. The table below gives details: exposure times (minutes) ------------------------------------------------ FOS blue blue red red blue visit t V g130h g190h g270h g400h G160L (days) mag exposure times (minutes) 1 0 13 6.72m 6.72m 6.72m 6.72m 20m 2 10 13.27 6.12m 6.12m 6.12m 6.12m 20m 3 20 13.54 6.12m 6.12m 6.12m 6.12m 4 30 13.18 6.12m 6.12m 6.12m 6.12m 5 60 14.63 6.12m 6.12m 6.12m 6.12m 6 90 15.44 9.00m 6.12m 6.12m 6.12m The exposure times, and estimated V magnitudes were calculated assuming the Nova Muscae light curve and aiming for 100 counts / Angstrom, with a minimum of 6.12 minutes exposure. Adjustments to increase efficiency were made. The time of visit is measured in days from the first visit. question 4, section 2 continued.... first observation of the target. The first four visits are separated by 10 days to allow us to monitor the changes in the spectrum near the outburst maximum, when the break in the slope of the spectrum should move through the UV to the optical part of the spectrum. The following visits are separated by 30 days to follow the accretion disk through the decline, and to catch the secondary maximum ~90 days after peak. Question 4, section 1 continued..... The greater sensitivity of HST will allow us to sample the ultraviolet emission over a much broader temporal baseline then has been possible with IUE (e.g. Nova Muscae 1991 became undetectable by IUE after about 4.5 months). ------------------------------------------------------------------------------------ 5. Description of special scheduling requirements. The observations, although not strictly "time critical", should be made as soon as possible when an optical identification is made after the outburst. As we established in section 2, the earlier the source is observed, the more likely we are to make truly exciting discoveries. The echo-mapping observations will allow us to probe the geometry of the accretion flow on the first two visits. The success of this part of the program hinges on observing the source while the X- ray and UV flux is high, leading to substantial reprocessed flux in the optical. The test of the disk instability model, which is described in detail in section 2, also requires prompt observations to be fully successful. It is important to observe the disk from as early in the outburst as possible, to ensure we will see the predicted break in the spectral slope move through the UV. With the program of visits we describe in section 4b, we will be able to unequivocably determine if this occurs, and hence make a rigorous test of the model. In addition to these crucial scientific motivations, we point out that the SXT flux decreases with time (e.g. at a rate of 0.6-1 magnitude per month for Nova Muscae), and any delay in scheduling will inevitably result in a loss of quality in the data obtained. Page 4 ------------------------------------------------------------------------------------ 8. Additional comments or special requests. There is a significant likelihood of a major transient event occurring during the approximately 1-year duration of this proposal. Although the recurrence times of an individual sources vary greatly, and are unpredictable, there have been over the last 5 years approximately one major event per year: GS2000+25 (April, 1988), GS2023+338 = V404 Cyg (May 1989) and GS1124-684 = Nova Muscae 1991 (January 1991), and GRO J0422+32 (August, 1992). The latter clearly demonstrates the capabilities of GRO/BATSE to discover and monitor the hard X-ray emission from events of this magnitude. Figure 1 (courtesy of the NASA/MSFC BATSE Consortium) is a 20-300 keV light curve of GRO J0422+32 derived from the BATSE occultation analysis of the BATSE discriminator-rate data. The peak intensity corresponds to approximately 3X that of the Crab. BATSE has also discovered one and possibly two SXT events of much lower peak intensity; a recurrent outbursts of 4U 1543-47 in April 1992 (Harmon, B.A. et al. 1992 IAU Circular no. 5504) and possibly EXO 1846-031 (peak intensities of < 1 Crab). We emphasize that a full feasibility assessment, based on prompt results from ground-based observatories and/or IUE will be made prior to requesting activation of this program. SXTs typically lie in the plane of the galaxy at > 1 kpc and can be heavily obscured in the blue-UV by dust extinction. For example, GS2000+25, whose peak brightness exceeded that of Nova Muscae 1991 by 50-60%, was so heavily reddened that it brightened to only 18 visual magnitudes and was undetecable by IUE (Shrader, C.R., 1988, IAU 4605). question 8, section 1 continued.... V404 Cyg, which was similarly dramatic in X-rays, brightened to a visual of magnitude about 12, but had a color excess perhaps as high as 1.6. It was marginally detected longward of 2600A by IUE, but it would not have been a suitable source for the work proposed here. As discussed in other sections of the proposal, our complementary target of opportunity programs will supply us with the necessary information for fully evaluating such feasibility considerations. We have no related Cycle 4 proposals, but we do have an accepted Cycle 3 TOO proposal. Page 5 ------------------------------------------------------------------------------------ 9. Description of previous HST work. Cycle 1: GO-3232 "Observations of X-ray nova Muscae 1991" [CS,KH,CoIs] GO-2380 "Instabilities in accretion disks and the outbursts of dwarf novae" [KH,PI] GO-2334 "Ultraviolet spectroscopy of the black hole A0620-00" [KH,CoI] Cycle 2: GO-3578 "Line Eclipse Mapping of an Accretion Disk Wind" [KH,CoI] GO-3824 "A search for silicon and carbon in GP Com [KH,CoI] GO-3600 "Oscillations, flaring, and tomography of AE Aquarii [KH,PI] GO-3683 "Accretion disk mapping in eclipsing cataclysmic variables" [KH,PI] GO-3836 "Spectroscopic Observations of the Exposed WDs in the Dwarf Novae U Gem, WZ Sag, and VW Hyi" [KH,CoI] Cycle 3: GO-3484 "Probing the Nuclear Regions of the Seyfert Galaxy NGC 5548" [KH,CoI] GO-4271 "Testing the Star-Disk Connection: CIV and MgII Maps of Disks" [KH,PI] GO-4377 "Soft X-Ray Transients: Outbursts in Black Hole Accretion disks." [KH,PI. ML,CH,FC,CS,WC,CoIs] GO-4589 "Energy Balance & Emission Lines in DQ Herculis Stars" [CH,CoI] Cycle 1: GO-2334: FOS spectra showed A0620-00 to be much fainter than expected, suggesting that the accretion disk viscosity shuts off completely in the quiescent periods between the outbursts of SXTs. GO-2380: FOS spectra of the eclipsing dwarf nova OY Car in quiescence (Dec 1991) and on the decline following a superoutburst (Apr-Jul 1992) are being used to discriminate between the disk instability and mass-transfer instability models of dwarf nova outbursts. A paper on the quiescent eclipse data is in draft form, while the data obtained following the superoutburst are under analysis. GO-3232: By combining HST/FOS, IUE, optical and x-ray spectra of Nova Muscae on the decline from outburst we place limits on the mass of the putative black hole in this system, and show that the cooling front predicted by disk instability model was not seen in this object. Cycle 2: GO-3578: HRS data has been taken to investigate line profile changes during the eclipse of an accretion disk wind. GO -3600: used FOS to investigate oscillations and flickering in an enigmatic CV with a magnetized and rapidly spinning accreting white dwarf. GO-3683: Some FOS observations of the eclipsing dwarf nova IP Peg have been taken. The remainder of the observations are pending. GO-3824: aims to determine metal abundances in the nearly pure helium disk ``The HST Observations of X-Ray Nova Muscae 1991 and its Spectral Evolution'' F.-H. Cheng, K. Horne, N. Panagia, C.R. Shrader, R. Gilmozzi, F. Paresce, N. Lund, (1992), ApJ, 397, 664. ``The Dim Inner Accretion Disk of the Quiescent Black Hole A0620-00'' J. McClintock, K. Horne, and R. Remillard, (199?), ApJL to be submitted. ``HST Eclipse Mapping of Dwarf Nova OY Car in Quiescence: An `FeII Curtain' with Mach ~ 6 Velocity Dispersion Veils the White Dwarf'' K. Horne, T. R. Marsh, F.-H. Cheng, I. Hubeny, and T. Lantz, (1993), ApJ, submitted. ``The Ultraviolet Pulsations of AE Aquarii as Observed With the Hubble Space Telescope'' K. Horne, M. Eracleous, E. L. Robinson, E. Zhang, T. R. Marsh, and J. Wood, Ap.J., (199?), to be submitted. question 9, section 2 continued.... in the ultra-short period system GP Com. Data is in hand; Carbon and Nitrogen were detected. GO-3836: Data aquisition is completed for this GHRS study of white dwarfs in three quiescent dwarf novae. There is preliminary evidence that the white dwarf rotation rates are small. Cycle 3: GO-3484: The 39 day FOS campaign is underway. Spectral variability suitable to the goals of the echo-mapping analysis has been detected. GO-4377: is a TOO program to obtain FOS spectra of the late stages of decline of an as yet unidentified SXT target. GO- 4589: will use FOS to examine the pulsations and line profile modulations due to the rotation of the magnetically accreting white dwarf YY Dra. GO-4271: will measure the surface brightness of MgII and CIV emission as a function of orbital angular velocity in the disks. ------------------------------------------------------------------------------------ 10. Resources to be supplied by investigator's institution(s). Salary and basic computer facilities are being provided for the P.I. and most of the Co-Is. ------------------------------------------------------------------------------------ 11. Address Information Page 6 Name: Keith Horne Category: PI Institution: University of Utrecht Address: Sterrekundig Instituut P.O. Box 80000 City: Utrecht, NL-3508 TA State: Zip Code: Country: The Netherlands Telephone: 410-338-4955 Telex (or e-mail): ------------------------------------------------------------------------------------ TARGET LIST c)Generic Targets ID = 5499 [ 7] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 7 ------------------------------------------------------------------------------------------------------------------------------------ Tar| Target | Target | Selection Criteria |Acqui|FLX| Flux data No | Name | Description | |Prblm|REF| | | | | | | ------------------------------------------------------------------------------------------------------------------------------------ 1 SXT A,161,162,164.165 OBJECT WILL BE SELECTED BY 1 PROPOSERS AFTER DISCOVERY WITH BATSE. Comments: NEWLY OURBURSTING SXT WILL BE FOLLOWED THROUGH DECLINE. UNTIL OUTBURST OCCURS, DETAILS OF LUMINOSITY, E(B-V), ETC ARE UNKNOWN. OPTICAL/IUE DATA WILL ENABLE EFFICIENCT USAGE OF HST TIME ALLOCATION. ASSUME FNU=NU**1/3 SPECTRUM V=13+(TIME/36.8DAYS), E(B-V)=0.3 FOR EXPOSURE LOGSHEET CALCS. ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 5499 [ 8] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 | 9 |10 | 11 | 12 |13 |14| 15 ------------------------------------------------------------------------------------------------------------------------------------ Line | Seq | Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | S/N |Flx|Pr| Special Number | Name | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| |Rel. Time|Ref| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 1.1 SXT FOS/RD ACQ/ 4.3 MIRROR SEARCH-SIZE-X=1 1 0.34S 1 ONBOARD ACQ FOR PEAK SEARCH-SIZE-Y=3 1.2 SCAN-STEP- CYCLE 4 / 1.1-6.6 Y=1.204 TARG OF OPP / 1.1- 6.6 Comments: FOS/BL ACQ/PEAK/MIRROR EXP=0.55S ORDER OF EXP 1.3-1.8 UNIMPORTANT OBSERVE ASAP AFTER TARGET ID'D ACQ/PEAK EXP TIME FOR 10000 COUNTS PLEASE NOTIFY P.I. WHEN DATES ARE SCHEDULED OR CHANGED ------------------------------------------------------------------------------------------------------------------------------------ 1.2 SXT FOS/RD ACQ/ 1.0 MIRROR SEARCH-SIZE-X=6 1 0.34S 1 ONBOARD ACQ FOR PEAK SEARCH-SIZE-Y=2 1.3-1.8 SCAN-STEP- X=.602 SCAN-STEP- Y=.602 Comments: FOS/BL ACQ/PEAK/MIRROR EXP=0.55S ORDER OF EXP 1.3-1.8 UNIMPORTANT IF FOS/BL FIRST DO ACQ/PEAK FOR FOS/BL/MIRROR CLOSE TO (OVER?) BRIGHTNESS LIMIT ------------------------------------------------------------------------------------------------------------------------------------ 1.3 SXT FOS/RD RAPID 4.3 G270H READ-TIME=6.18 1 401.7S 1 Comments: DETAILED OBSERVING PLAN IS LIKELY TO CHANGE WHEN ACTUAL TARGET IS ID'D THESE EXPOSURES ARE GUIDELINES ONLY ------------------------------------------------------------------------------------------------------------------------------------ 1.4 SXT FOS/RD RAPID 4.3 G400H READ-TIME=6.18 1 401.7S 1 Comments: PLEASE CONSULT PI IF TIMING CONSTRAINTS PRECLUDE SCHEDULING ------------------------------------------------------------------------------------------------------------------------------------ 1.5 SXT FOS/BL RAPID 4.3 G130H READ-TIME=6.18 1 401.7S 1 ------------------------------------------------------------------------------------------------------------------------------------ 1.6 SXT FOS/BL RAPID 4.3 G190H READ-TIME=6.18 1 401.7S 1 ------------------------------------------------------------------------------------------------------------------------------------ 1.8 SXT FOS/BL RAPID 4.3 G160L READ-TIME=6.18 1 1198.92 1 ------------------------------------------------------------------------------------------------------------------------------------ 2.1 SXT FOS/RD ACQ/ 4.3 MIRROR SEARCH-SIZE-X=1 1 0.44S 1 ONBOARD ACQ FOR PEAK SEARCH-SIZE-Y=3 2.2 SCAN-STEP- AFTER 1.1 BY 10D + Y=1.204 /- 2D Comments: FOS/BL ACQ/PEAK/MIRROR EXP=0.71S ORDER OF EXP 2.3-2.8 UNIMPORTANT ACQ/PEAK EXP TIME FOR 10000 COUNTS PLEASE NOTIFY P.I. WHEN DATES ARE SCHEDULED OR CHANGED ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 5499 [ 9] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 | 9 |10 | 11 | 12 |13 |14| 15 ------------------------------------------------------------------------------------------------------------------------------------ Line | Seq | Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | S/N |Flx|Pr| Special Number | Name | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| |Rel. Time|Ref| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 2.2 SXT FOS/RD ACQ/ 1.0 MIRROR SEARCH-SIZE-X=6 1 0.44S 1 ONBOARD ACQ FOR PEAK SEARCH-SIZE-Y=2 2.3-2.8 SCAN-STEP- X=.602 SCAN-STEP- Y=.602 Comments: FOS/BL ACQ/PEAK/MIRROR EXP=0.71S ORDER OF EXP 2.3-2.8 UNIMPORTANT IF FOS/BL FIRST DO ACQ/PEAK FOR FOS/BL/MIRROR CLOSE TO (OVER?) BRIGHTNESS LIMIT ------------------------------------------------------------------------------------------------------------------------------------ 2.3 SXT FOS/RD RAPID 4.3 G270H READ-TIME=6.18 1 364.62S 1 Comments: DETAILED OBSERVING PLAN IS LIKELY TO CHANGE WHEN ACTUAL TARGET IS ID'D THESE EXPOSURES ARE GUIDELINES ONLY ------------------------------------------------------------------------------------------------------------------------------------ 2.4 SXT FOS/RD RAPID 4.3 G400H READ-TIME=6.18 1 364.62S 1 Comments: PLEASE CONSULT PI IF TIMING CONSTRAINTS PRECLUDE SCHEDULING ------------------------------------------------------------------------------------------------------------------------------------ 2.5 SXT FOS/BL RAPID 4.3 G130H READ-TIME=6.18 1 364.62S 1 ------------------------------------------------------------------------------------------------------------------------------------ 2.6 SXT FOS/BL RAPID 4.3 G190H READ-TIME=6.18 1 364.62S 1 ------------------------------------------------------------------------------------------------------------------------------------ 2.8 SXT FOS/BL RAPID 4.3 G160L READ-TIME=6.18 1 1198.92 1 ------------------------------------------------------------------------------------------------------------------------------------ 3.1 SXT FOS/RD ACQ/ 4.3 MIRROR SEARCH-SIZE-X=1 1 0.55S 1 ONBOARD ACQ FOR PEAK SEARCH-SIZE-Y=3 3.2 SCAN-STEP- AFTER 1.1 BY 20D + Y=1.204 /- 2D Comments: FOS/BL ACQ/PEAK/MIRROR EXP=0.91S ORDER OF EXP 3.3-3.6 UNIMPORTANT OBSERVE ASAP AFTER TARGET ID'D ACQ/PEAK EXP TIME FOR 10000 COUNTS PLEASE NOTIFY P.I. WHEN DATES ARE SCHEDULED OR CHANGED ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 5499 [ 10] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 | 9 |10 | 11 | 12 |13 |14| 15 ------------------------------------------------------------------------------------------------------------------------------------ Line | Seq | Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | S/N |Flx|Pr| Special Number | Name | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| |Rel. Time|Ref| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 3.2 SXT FOS/RD ACQ/ 1.0 MIRROR SEARCH-SIZE-X=6 1 0.55S 1 ONBOARD ACQ FOR PEAK SEARCH-SIZE-Y=2 3.3-3.6 SCAN-STEP- X=.602 SCAN-STEP- Y=.602 Comments: FOS/BL ACQ/PEAK/MIRROR EXP=0.91S ORDER OF EXP 3.3-3.6 UNIMPORTANT IF FOS/BL FIRST DO ACQ/PEAK FOR FOS/BL/MIRROR CLOSE TO (OVER?) BRIGHTNESS LIMIT ------------------------------------------------------------------------------------------------------------------------------------ 3.3 SXT FOS/RD RAPID 4.3 G270H READ-TIME=6.18 1 364.62S 1 Comments: DETAILED OBSERVING PLAN IS LIKELY TO CHANGE WHEN ACTUAL TARGET IS ID'D THESE EXPOSURES ARE GUIDELINES ONLY ------------------------------------------------------------------------------------------------------------------------------------ 3.4 SXT FOS/RD RAPID 4.3 G400H READ-TIME=6.18 1 364.62S 1 Comments: PLEASE CONSULT PI IF TIMING CONSTRAINTS PRECLUDE SCHEDULING ------------------------------------------------------------------------------------------------------------------------------------ 3.5 SXT FOS/BL RAPID 4.3 G130H READ-TIME=6.18 1 364.62S 1 CYCLE 4 ------------------------------------------------------------------------------------------------------------------------------------ 3.6 SXT FOS/BL RAPID 4.3 G190H READ-TIME=6.18 1 364.62S 1 ------------------------------------------------------------------------------------------------------------------------------------ 4.1 SXT FOS/RD ACQ/ 4.3 MIRROR SEARCH-SIZE-X=1 1 0.71S 1 ONBOARD ACQ FOR PEAK SEARCH-SIZE-Y=3 4.2 SCAN-STEP- AFTER 1.1 BY 30D + Y=1.204 /- 2D Comments: FOS/BL ACQ/PEAK/MIRROR EXP=1.17S ORDER OF EXP 4.3-4.6 UNIMPORTANT OBSERVE ASAP AFTER TARGET ID'D ACQ/PEAK EXP TIME FOR 10000 COUNTS PLEASE NOTIFY P.I. WHEN DATES ARE SCHEDULED OR CHANGED ------------------------------------------------------------------------------------------------------------------------------------ 4.2 SXT FOS/RD ACQ/ 1.0 MIRROR SEARCH-SIZE-X=6 1 0.71S 1 ONBOARD ACQ FOR PEAK SEARCH-SIZE-Y=2 4.3-4.6 SCAN-STEP- X=.602 SCAN-STEP- Y=.602 Comments: FOS/BL ACQ/PEAK/MIRROR EXP=1.17S ORDER OF EXP 4.3-4.6 UNIMPORTANT IF FOS/BL FIRST DO ACQ/PEAK FOR FOS/BL/MIRROR 30 + /- 2 DAYS AFTER VISIT 1 (1.1- 1.8) ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 5499 [ 11] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 | 9 |10 | 11 | 12 |13 |14| 15 ------------------------------------------------------------------------------------------------------------------------------------ Line | Seq | Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | S/N |Flx|Pr| Special Number | Name | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| |Rel. Time|Ref| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 4.3 SXT FOS/RD RAPID 4.3 G270H READ-TIME=6.18 1 364.62S 1 Comments: DETAILED OBSERVING PLAN IS LIKELY TO CHANGE WHEN ACTUAL TARGET IS ID'D THESE EXPOSURES ARE GUIDELINES ONLY ------------------------------------------------------------------------------------------------------------------------------------ 4.4 SXT FOS/RD RAPID 4.3 G400H READ-TIME=6.18 1 364.62S 1 Comments: PLEASE CONSULT PI IF TIMING CONSTRAINTS PRECLUDE SCHEDULING ------------------------------------------------------------------------------------------------------------------------------------ 4.5 SXT FOS/BL RAPID 4.3 G130H READ-TIME=6.18 1 364.62S 1 ------------------------------------------------------------------------------------------------------------------------------------ 4.6 SXT FOS/BL RAPID 4.3 G190H READ-TIME=6.18 1 364.62S 1 ------------------------------------------------------------------------------------------------------------------------------------ 5.1 SXT FOS/RD ACQ/ 4.3 MIRROR SEARCH-SIZE-X=1 1 1.55S 1 ONBOARD ACQ FOR PEAK SEARCH-SIZE-Y=3 5.2 SCAN-STEP- AFTER 1.1 BY 60D + Y=1.204 /- 5D Comments: FOS/BL ACQ/PEAK/MIRROR EXP=2.50S ORDER OF EXP 5.3-5.6 UNIMPORTANT OBSERVE ASAP AFTER TARGET ID'D ACQ/PEAK EXP TIME FOR 10000 COUNTS PLEASE NOTIFY P.I. WHEN DATES ARE SCHEDULED OR CHANGED ------------------------------------------------------------------------------------------------------------------------------------ 5.2 SXT FOS/RD ACQ/ 1.0 MIRROR SEARCH-SIZE-X=6 1 1.55S 1 ONBOARD ACQ FOR PEAK SEARCH-SIZE-Y=2 5.3-5.6 SCAN-STEP- X=.602 SCAN-STEP- Y=.602 Comments: FOS/BL ACQ/PEAK/MIRROR EXP=2.50S ORDER OF EXP 5.3-5.6 UNIMPORTANT IF FOS/BL FIRST DO ACQ/PEAK FOR FOS/BL/MIRROR 60 + /- 5 DAYS AFTER VISIT 1 (1.1- 1.8) ------------------------------------------------------------------------------------------------------------------------------------ 5.3 SXT FOS/RD RAPID 4.3 G270H READ-TIME=6.18 1 364.62S 1 Comments: DETAILED OBSERVING PLAN IS LIKELY TO CHANGE WHEN ACTUAL TARGET IS ID'D THESE EXPOSURES ARE GUIDELINES ONLY ------------------------------------------------------------------------------------------------------------------------------------ 5.4 SXT FOS/RD RAPID 4.3 G400H READ-TIME=6.18 1 364.62S 1 Comments: PLEASE CONSULT PI IF TIMING CONSTRAINTS PRECLUDE SCHEDULING ------------------------------------------------------------------------------------------------------------------------------------ 5.5 SXT FOS/BL RAPID 4.3 G130H READ-TIME=6.18 1 364.62S 1 ------------------------------------------------------------------------------------------------------------------------------------ 5.6 SXT FOS/BL RAPID 4.3 G190H READ-TIME=6.18 1 364.62S 1 ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 5499 [ 12] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 | 9 |10 | 11 | 12 |13 |14| 15 ------------------------------------------------------------------------------------------------------------------------------------ Line | Seq | Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | S/N |Flx|Pr| Special Number | Name | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| |Rel. Time|Ref| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 6.1 SXT FOS/RD ACQ/ 4.3 MIRROR SEARCH-SIZE-X=1 1 3.3S 1 ONBOARD ACQ FOR PEAK SEARCH-SIZE-Y=3 6.2 SCAN-STEP- AFTER 1.1 BY 90D + Y=1.204 /- 5D Comments: FOS/BL ACQ/PEAK/MIRROR EXP=5.2S ORDER OF EXP 6.3-6.6 UNIMPORTANT OBSERVE ASAP AFTER TARGET ID'D ACQ/PEAK EXP TIME FOR 10000 COUNTS PLEASE NOTIFY P.I. WHEN DATES ARE SCHEDULED OR CHANGED ------------------------------------------------------------------------------------------------------------------------------------ 6.2 SXT FOS/RD ACQ/ 1.0 MIRROR SEARCH-SIZE-X=6 1 3.3S 1 ONBOARD ACQ FOR PEAK SEARCH-SIZE-Y=2 6.3-6.6 SCAN-STEP- X=.602 SCAN-STEP- Y=.602 Comments: FOS/BL ACQ/PEAK/MIRROR EXP=5.2S ORDER OF EXP 6.3-6.6 UNIMPORTANT IF FOS/BL FIRST DO ACQ/PEAK FOR FOS/BL/MIRROR 90 + /- 5 DAYS AFTER VISIT 1 (1.1- 1.8) ------------------------------------------------------------------------------------------------------------------------------------ 6.3 SXT FOS/RD RAPID 4.3 G270H READ-TIME=6.18 1 364.62S 1 Comments: DETAILED OBSERVING PLAN IS LIKELY TO CHANGE WHEN ACTUAL TARGET IS ID'D THESE EXPOSURES ARE GUIDELINES ONLY ------------------------------------------------------------------------------------------------------------------------------------ 6.4 SXT FOS/RD RAPID 4.3 G400H READ-TIME=6.18 1 364.62S 1 Comments: PLEASE CONSULT PI IF TIMING CONSTRAINTS PRECLUDE SCHEDULING ------------------------------------------------------------------------------------------------------------------------------------ 6.5 SXT FOS/BL RAPID 4.3 G130H READ-TIME=6.18 1 537.66S 1 ------------------------------------------------------------------------------------------------------------------------------------ 6.6 SXT FOS/BL RAPID 4.3 G190H READ-TIME=6.18 1 364.62S 1 ------------------------------------------------------------------------------------------------------------------------------------ Summary Form for Proposal 5499 [ 13] Item Used in this proposal ------------------------------------------------------------------------------------------------------------------------------------ Configurations FOS/RD FOS/BL ------------------------------------------------------------------------------------------------------------------------------------ Opmodes ACQ/PEAK RAPID ------------------------------------------------------------------------------------------------------------------------------------ Optional Parameters SEARCH-SIZE-X=1 SEARCH-SIZE-Y=3 SCAN-STEP-Y=1.204 SEARCH-SIZE-X=6 SEARCH-SIZE-Y=2 SCAN-STEP-X=.602 SCAN-STEP-Y=.602 READ-TIME=6.18 ------------------------------------------------------------------------------------------------------------------------------------ Proposal for GO ------------------------------------------------------------------------------------------------------------------------------------ S/C Hours 10.34 ------------------------------------------------------------------------------------------------------------------------------------ Scientific Category HOT STARS ------------------------------------------------------------------------------------------------------------------------------------ Scientific Sub-category X-RAY BINARIES ------------------------------------------------------------------------------------------------------------------------------------ Special Requirements ONBOARD ACQ FOR 1.2 ; CYCLE 4 / 1.1-6.6; TARG OF OPP / 1.1-6.6 ONBOARD ACQ FOR 1.3-1.8 ONBOARD ACQ FOR 2.2 ; AFTER 1.1 BY 10D +/- 2D ONBOARD ACQ FOR 2.3-2.8 ONBOARD ACQ FOR 3.2 ; AFTER 1.1 BY 20D +/- 2D ONBOARD ACQ FOR 3.3-3.6 CYCLE 4; ONBOARD ACQ FOR 4.2 ; AFTER 1.1 BY 30D +/- 2D ONBOARD ACQ FOR 4.3-4.6 ONBOARD ACQ FOR 5.2 ; AFTER 1.1 BY 60D +/- 5D ONBOARD ACQ FOR 5.3-5.6 ONBOARD ACQ FOR 6.2 ; AFTER 1.1 BY 90D +/- 5D ONBOARD ACQ FOR 6.3-6.6 ------------------------------------------------------------------------------------------------------------------------------------ Spectral Elements MIRROR G270H G400H G130H G190H G160L ------------------------------------------------------------------------------------------------------------------------------------ Target Names SXT ------------------------------------------------------------------------------------------------------------------------------------