! $Id: 5478,v 20.1 1994/08/02 12:58:17 pepsa Exp $ coverpage: title_1: TIME-RESOLVED UV AND X-RAY SPECTROMETRY OF X-RAY BINARIES title_2: CYCLE 4 MEDIUM sci_cat: HOT STARS sci_subcat: X-RAY BINARIES proposal_for: GO pi_fname: RICHARD pi_mi: A pi_lname: MCCRAY pi_inst: UNIVERSITY OF COLORADO pi_country: USA pi_phone: (303)-492-7835 hours_pri: 7.20 num_pri: 1 fos: Y hrs: Y off_fname: LARRY off_lname: NELSON off_title: DIRECTOR off_inst: 1760 off_addr_1: OFFICE OF CONTRACTS AND GRANTS off_addr_2: CAMPUS BOX B-19 off_city: BOULDER off_state: CO off_zip: 80309 off_country: USA off_phone: (303)-492-2695 ! end of coverpage abstract: line_1: In simultaneous observations with HST and ASCA, we will observe line_2: rapid variations in the UV and X-ray spectra of the X-ray binary line_3: Her X-1. Our purpose is to understand the accretion flow and X-ray line_4: emission. By observing UV echoes of X-ray variations (especially line_5: pulsations) on time scales down to 0.35 s, we can map the precessing line_6: accretion disk. We will use the HRS (30km/s resolution) line_7: to look for pulsations in the profile of the NV emission line_8: line at 1240 A. During these observations, we will use ASCA to find line_9: the X-ray pulse shape and spectrum, X-ray/UV phase lag, X-ray state, line_10: absorbing column, and X-ray emission lines and edges. The X-ray line_11: and UV observations will complement each other, resulting in greatly line_12: enhanced science. These observations will take place from orbital line_13: phases 0.7 to 1.0, in order to probe the geometry of the X-ray line_14: absorbing and UV fluorescing gas. ! ! end of abstract general_form_proposers: lname: MCCRAY fname: RICHARD mi: A inst: 1760 country: USA ! lname: BOROSON fname: BRAM mi: S inst: 1760 country: USA ! lname: KALLMAN fname: TIMOTHY inst: 2856 country: USA ! lname: NAGASE fname: FUMIAKI inst: 6510 country: JAPAN ! lname: ISHIDA fname: M. inst: 6510 country: JAPAN ! lname: MARGON fname: BRUCE inst: 3760 country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We will observe Her X-1 during the HIGH state of the 35 day line_2: cycle with the HRS for an actual spacecraft time of line_3: 26,000 seconds, corresponding to 1.7d orbital phase 0.74 line_4: through 0.92. This observing time and orbital phase range line_5: is dictated by the desire to search for pulsations in the UV line_6: lines during the phase when optical pulsations from the disk line_7: are strongest and we have a good chance of catching a pre-eclipse line_8: "dip" in the X-ray light curve. The HRS line_9: centered at 1240 A. All observations will be taken with RAPID line_10: (0.35 second) readout mode. We decided to concentrate on this line_11: line (N V) because it is the brightest emission line in the UV line_12: spectrum and because it should be the most sensitive to X-ray line_13: illumination. During the orbital phase interval 0.7-1.0 we will line_14: coordinate simultaneous observations with the ASCA X-ray telescope. ! question: 3 section: 2 line_1: ! question: 4 section: 1 line_1: The HST is the only telescope that can do time-resolved UV spectrometry line_2: of binary X-ray sources, the essence of this proposal. line_3: The HRS G140M velocity resolution, 20 km/s, can easily resolve the line_4: NV 1238,1242 emission lines. With our simultaneous X-ray observations, line_5: we will know the brightness, spectrum, and pulse profile and phase line_6: of the X-ray beam. With ASCA we can study the Fe K line, line_7: and compare its pulsation with the UV pulses. ! question: 5 section: 1 line_1: The Her X-1 system orbits in 1.7 days and the X-rays vary in 35 days line_2: (attributed to shadowing by a twisted, tilted accretion disk.) line_3: We seek to observe Her X-1 when the chance to detect pulsations line_4: peaks. We are also interested in observing the eclipse ingress. line_5: Thus our plan calls for continuous observation from orbital phase line_6: 0.75 thru 0.93, and during the most favorable state of the 35 day line_7: variation. Observations are to be coordinated with the ASCA X-ray, line_8: telescope, a procedure that worked smoothly for our 1991 joint HST/Ginga line_9: observation. ! question: 6 section: 1 line_1: ! ! question: 8 section: 1 line_1: ! question: 9 section: 1 line_1: 1051-GTO/FOS-86G: MASS EXCHANGE BINARIES (B. Margon, P.I.) line_2: Observations with FOS were successful. We will use different line_3: orbital phases, RAPID readout for all exposures, and a better line_4: spectral resolution in our current proposal. line_6: P2572-GO/FOS: TIME RESOLVED UV SPECTROMETRY OF VELA X-1 line_7: This program is related to the present proposal. We did time- line_8: resolved UV spectrometry of the massive X-ray binary Vela X-1 with line_9: the FOS and simultaneous observations with the Japanese X-ray line_10: satellite GINGA. line_12: The observations took place August 19, 1991. They were successful line_13: in every sense. We obtained simultaneous X-ray and HST data. line_14: We found pulsations in the UV absorption lines and were able to line_15: measure phase shifts between the UV and X-ray pulse waveforms. line_16: This observation was the first successful demonstration of line_17: pulse phase spectroscopy of X-ray binaries. line_19: P2492-GO/HRS: CONDUCTIVE INTERFACES IN STELLAR WIND BUBBLES line_20: This program is unrelated to that of the present proposal. The line_21: observations have been executed recently and the data are now line_22: being analyzed. ! question: 10 section: 1 line_1: The University of Colorado operates computer facilities currently line_2: based on VAX mainframes running VMS, and SUN and DEC workstations line_3: running UNIX. For the analysis of the HST/FOS and HRS data we will line_4: use the SUN And DECstations which run IRAF and IDL in a UNIX line_5: environment. A graduate student (Mr. Bram Boroson) in the line_6: Department of Astrophysical, Planetary, and Atmospheric Sciences line_7: is currently working with the P.I. on the preparation of this line_8: proposal. If the proposed observation is successful, work based line_9: on modelling and interpreting the HST data will be a major part line_10: of Mr. Boroson's Ph.D. thesis. ! !end of general form text general_form_address: lname: McCray fname: Richard mi: A category: PI inst: 1764 addr_1: Box 440 city: Boulder state: CO zip: 80309 country: USA phone: (303)-492-7835 ! lname: Boroson fname: Bram mi: S category: CON inst: 1760 addr_1: Graduate Student city: Boulder state: CO zip: 80309 country: USA phone: (303)-492-7805 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: HER-X-1 name_2: HZ-HER descr_1: A,165,906 pos_1: RA=16H 57M 49.81S +/- 0.01S, pos_2: DEC=+35D20'32.7" +/- 0.3", pos_3: PLATE-ID=00CK equinox: J2000 pm_or_par: N pos_epoch_bj: J pos_epoch_yr: 2000.00 fluxnum_1: 1 fluxval_1: V=13.2, B-V=-0.1 fluxnum_2: 2 fluxval_2: F-CONT(1500)=5.0 +/- 2.5E-14 fluxnum_3: 3 fluxval_3: F-LINE(1550)=2.0 +/- 1.5E-13 fluxnum_4: 4 fluxval_4: F-LINE(1240)=5.0 +/- 3.5E-13 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: HER-X-1 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 wavelength: 1200-1600 num_exp: 1 time_per_exp: 5S priority: 1 param_1: SEARCH-SIZE = 5 param_2: BRIGHT = RETURN req_1: CYCLE 4 / 1-13; req_2: ONBOARD ACQ FOR 2-13; req_3: SEQ 1-13; req_4: AT 27-AUG-1994:09:00 +/- 1D; comment_1: SIMULTANEOUS OBSERVATIONS WILL BE comment_2: TAKEN BY THE ASCA X-RAY TELESCOPE. comment_3: NOTE PERIODS OF PRIME OBSERVING. comment_4: THERE IS A SECOND PERIODICITY; WE comment_5: WILL PROVIDE TIMES WHEN THIS PHASE comment_6: IS FAVORABLE IN A SEPARATE DOCUMENT. ! linenum: 2.000 targname: HER-X-1 config: HRS opmode: RAPID aperture: 2.0 sp_element: G140L wavelength: 1200-1490 num_exp: 1 time_per_exp: 20M priority: 1 param_1: SAMPLE-TIME = 0.1 req_1: ZERO-PHASE JD2443805.02 +/- 0.0001D; req_2: PERIOD 1.700167788D +/- .000000001D; req_3: PHASE .55 +/- .1; req_4: RT ANALYSIS; ! linenum: 3.000 targname: HER-X-1 config: HRS opmode: RAPID aperture: 2.0 sp_element: G140L wavelength: 1380-1670 num_exp: 1 time_per_exp: 10.4M priority: 1 param_1: SAMPLE-TIME = 0.35 ! linenum: 4.000 targname: HER-X-1 config: HRS opmode: RAPID aperture: 2.0 sp_element: G140M wavelength: 1240 num_exp: 1 time_per_exp: 39.6M priority: 1 param_1: SAMPLE-TIME = 0.35 ! linenum: 5.000 targname: HER-X-1 config: HRS opmode: RAPID aperture: 2.0 sp_element: G140M wavelength: 1240 num_exp: 1 time_per_exp: 39.6M priority: 1 param_1: SAMPLE-TIME = 0.35 ! linenum: 6.000 targname: HER-X-1 config: HRS opmode: RAPID aperture: 2.0 sp_element: G140L wavelength: 1200-1490 num_exp: 1 time_per_exp: 14.4M priority: 1 param_1: SAMPLE-TIME = 0.35 ! linenum: 7.000 targname: HER-X-1 config: HRS opmode: RAPID aperture: 2.0 sp_element: G140L wavelength: 1380-1670 num_exp: 1 time_per_exp: 14.4M priority: 1 param_1: SAMPLE-TIME = 0.35 ! linenum: 8.000 targname: HER-X-1 config: HRS opmode: RAPID aperture: 2.0 sp_element: G140M wavelength: 1240 num_exp: 1 time_per_exp: 39.6M priority: 1 param_1: SAMPLE-TIME = 0.35 ! linenum: 9.000 targname: HER-X-1 config: HRS opmode: RAPID aperture: 2.0 sp_element: G140M wavelength: 1240 num_exp: 1 time_per_exp: 39.6M priority: 1 param_1: SAMPLE-TIME = 0.35 ! linenum: 10.000 targname: HER-X-1 config: HRS opmode: RAPID aperture: 2.0 sp_element: G140L wavelength: 1200-1490 num_exp: 1 time_per_exp: 14.4M priority: 1 param_1: SAMPLE-TIME = 0.35 ! linenum: 11.000 targname: HER-X-1 config: HRS opmode: RAPID aperture: 2.0 sp_element: G140L wavelength: 1380-1670 num_exp: 1 time_per_exp: 14.4M priority: 1 param_1: SAMPLE-TIME = 0.35 ! linenum: 12.000 targname: HER-X-1 config: HRS opmode: RAPID aperture: 2.0 sp_element: G140M wavelength: 1240 num_exp: 1 time_per_exp: 39.6M priority: 1 param_1: SAMPLE-TIME = 0.35 ! linenum: 13.000 targname: HER-X-1 config: HRS opmode: RAPID aperture: 2.0 sp_element: G140M wavelength: 1240 num_exp: 1 time_per_exp: 25M priority: 1 param_1: SAMPLE-TIME = 0.35 ! ! end of exposure logsheet ! No scan data records found