! File: 4285C.PROP ! Database: PEPDB ! Date: 20-FEB-1994:20:22:01 coverpage: title_1: TIME-RESOLVED UV SPECTROMETRY OF MASSIVE X-RAY BINARIES: title_2: CYCLE 3 MEDIUM sci_cat: HOT STARS sci_subcat: X-RAY BINARIES proposal_for: GO pi_title: DR. pi_fname: RICHARD pi_mi: A pi_lname: MCCRAY pi_inst: UNIVERSITY OF COLORADO pi_country: USA pi_phone: 303-492-7835 hours_pri: 5.39 num_pri: 1 fos: Y time_crit: Y funds_length: 12 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: We will observe pulsations and rapid variability in the UV P-Cygni lines of line_2: the optical counterpart of Vela X-1. We will use the FOS G130H in the line_3: RAPID mode to look for spectral variability at timescales ranging from 20 s line_4: to 30 m. The HST observations will be coordinated with simultaneous X-ray line_5: observations to look for correlations of the UV variability with X-ray line_6: variability and lags in the pulse waveforms. This approach yielded a line_7: successful detection of pulsations in the Si IV 1402 and N V 1238 absorption line_8: lines of Vela X-1 in a Cycle 1 HST observation that was coordinated with X- line_9: ray observations with the GINGA satellite. We will see how the UV line line_10: profile, pulse amplitude, and phase lag change with X-ray luminosity and line_11: orbital phase, in order to map the dynamics of the stellar wind and the line_12: geometry of the X-ray beam. Finally, we will search for polarization line_13: expected in the UV spectrum of Vela X-1. ! ! end of abstract general_form_proposers: lname: MCCRAY fname: RICHARD title: PI mi: A inst: UNIVERSITY OF COLORADO country: USA esa: N ! lname: KALLMAN fname: TIMOTHY mi: R inst: NASA GODDARD SPACE FLIGHT CENTER country: USA esa: N ! lname: BOROSON fname: BRAM mi: S inst: UNIVERSITY OF COLORADO country: USA esa: N ! lname: NAGASE fname: FUMIAKI inst: INSTITUTE OF SPACE AND ASTRONAUTICAL SCIENCE country: JAPAN esa: N ! lname: ISHIDA fname: M. inst: INSTITUTE OF SPACE AND ASTRONAUTICAL SCIENCE country: JAPAN esa: N ! ! end of general_form_proposers block general_form_text: question: 2 section: 1 line_1: text ! question: 3 section: 1 line_1: We will take four 30 minute exposures of Vela X-1 at various orbital line_2: phases. At orbital phase 0.5 we will use the RAPID (20 second readout) line_3: mode of the FOS and the G130H grating to search for pulsations and line_4: rapid variability in the UV P-Cygni lines. We have already observed line_5: pulsations at this phase, but the source may be in a more favorable line_6: state in a second observation. At orbital phase 0.6 we will line_7: use the same configuration to search for similar pulsations, but with line_8: different lags relative to the X-rays and with a different velocity line_9: structure. An exposure during X-ray eclipse (with the same line_10: configuration) will show us the P-Cygni absorption profiles in the line_11: absence of X-ray illumination, and may show pulsations in the red- line_12: shifted emission, since the X-ray source is near the receeding flow. line_13: Finally, an observation at orbital phase 0.6 using the line_14: spectropolarmetric ability of the FOS with the G130H grating can line_15: reveal a wavelength-dependent linear polarization in the P-Cygni lines, line_16: resulting from scattering in the asymmetric wind. We will line_17: simultaneously observe X-rays with the ASTRO-D telescope. line_18: If an unexpected problem prevents us from using ASTRO-D, line_19: OSSE aboard the Gamma Ray Observatory (GRO) frequently line_20: monitors pulsations from Vela X-1, and can do so during our HST observation. ! question: 4 section: 1 line_1: Searches for X-ray heating effects using optical lines or broad-band line_2: optical or UV fluxes (generally associated with the companion star's line_3: photosphere) are virtually impossible. The stellar wind can only be line_4: observed in the UV resonance lines of ions such as N V 1240, Si IV line_5: 1393, 1402, and C IV 1550. The HST is the only telescope that can do line_6: time-resolved UV spectometry of binary X-ray sources, the essence of line_7: this proposal. We did not detect any P-Cygni pulsations using IUE line_8: with special modifications to achieve the needed time-resolution line_9: (Kallman, McCray, and Voit 1987). The pulsations we detected with line_10: HST were clearly too weak to be observed with any other instrument. ! question: 5 section: 1 line_1: The observations must be taken during the appropriate orbital phases line_2: of Vela X-1: 0.0 (X-ray eclipse), 0.5, and 0.6. We also plan line_3: simultaneous X-ray observations. We will line_4: provide STScI with a list of all windows for which our selected X-ray line_5: instrument can observe Vela X-1 and we will provide the latest line_6: ephemeris to Vela X-1 orbital phases. Then HST scheduling can choose line_7: from among these windows and coordinate with ASTRO-D if available. line_8: Such a procedure worked smoothly in a simultaneous HST -- GINGA line_9: observation of Vela X-1 that took place August 19, 1991. ! question: 7 section: 1 line_1: We will analyze the observations at the University of Colorado line_2: Center for Astrophysics and Space Astronomy (CASA), where we have a line_3: full range of computer and software support. We will do a time- line_4: series analysis of both the HST and X-ray data. From the Fourier line_5: transformed signals, we will construct power spectra and reconstruct line_6: pulse waveforms for each spectral resolution element of both the X- line_7: ray and UV data, and for the signals in broader bands. We will also line_8: examine cross-spectra to look for phase lags between the X-ray line_9: continuum and Fe-K line pulsations and the UV pulsations. We will line_10: also construct theoretical models to fit the data. Starting with line_11: models for the dynamics of the stellar wind, we will compute the line_12: P-Cygni line variation in response to illumination by an X-ray beam line_13: using a code developed by T. Kallman and R. McCray (1982, Ap. J. line_14: Suppl., 50, 263). We will then calculate the pulsation of the line line_15: profiles, taking into account light travel time delays. ! question: 9 section: 1 line_1: P 2572-GO/FOS: Time-Resolved UV Spectrometry of Vela X-1 line_2: P 2492-GO/HRS: Conductive Interfaces in Stellar Wind Bubbles, line_3: R. McCray, P.I. This program is unrelated to the present one. line_4: Observations have not yet taken place. line_5: consistent with our picture of ionization in the wind. The line_6: simultaneous GINGA spectra also helped us understand the low line_7: level of UV pulsations as the result of an unusually high density line_8: around the neutron star. ! question: 10 section: 1 line_1: CASA at the University of Colorado operates computer facilities line_2: currently based on VAX mainframed running VMS, and SUN and DEC line_3: workstations running UNIX and VMS. For the analysis of the HST/ line_4: FOS data we will use the SUN and DECstations which run IRAF and line_5: IDL. A graduate student (Mr. Bram Boroson) in the Department of line_6: Astrophysical, Planetary, and Atmospheric Sciences will work on line_7: constructing theoretical models for the time-dependent UV emission line_8: line fluorescence in binary X-ray systems, including Vela X-1. line_9: If the proposed observation is successful, that work and the line_10: analysis and interpretation of the data will constitute a major line_11: part of his Ph.D. thesis. ! !end of general form text general_form_address: lname: MCCRAY fname: RICHARD mi: A category: PI inst: University of Colorado addr_1: CASA addr_2: BOX 391 city: BOULDER state: CO zip: 80309 country: USA phone: 303-492-7835 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: HD77581 name_2: 4U0900-40 name_3: VELA-X-1 descr_1: A,113,166,905 pos_1: RA = 09H 02M 06.867S +/- 3.4", pos_2: DEC = -40D 33' 14.73" +/- 3.4" equinox: 2000 comment_1: AP. J., V. 238, 969. fluxnum_1: 1 fluxval_1: V = 6.9 +/- 0.1, TYPE = B0.5IA fluxnum_2: 2 fluxval_2: B-V = 0.5 fluxnum_3: 3 fluxval_3: E(B-V)=0.7 fluxnum_4: 4 fluxval_4: F-LINE(1245) = 3.1 +/- 0.2 E -12 fluxnum_5: 5 fluxval_5: F-LINE(1405) = 4.8 +/- 0.4 E -12 fluxnum_6: 6 fluxval_6: F-LINE(1553) = 5.0 +/- 0.4 E -12 fluxnum_7: 7 fluxval_7: F-CONT(1280) = 2.3 +/- 0.2 E -12 fluxnum_8: 8 fluxval_8: F-CONT(1480) = 3.8 +/- 0.5 E -12 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: HD77581 config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: G130H wavelength: 1200-1600 num_exp: 1 time_per_exp: 0.1S priority: 1 param_1: TYPE = UP, param_2: SEARCH-SIZE-X=1, param_3: SEARCH-SIZE-Y=3, param_5: SCAN-STEP-Y=1.4, req_1: CYCLE 3 / 1-3; req_2: ONBOARD ACQ FOR 2.0; req_3: SEQ 1 - 3 NO GAP comment_1: OBSERVATIONS TO BE COORDINATED WITH comment_2: SIMULTANEOUS X-RAY OBSERVATION ! linenum: 2.000 targname: HD77581 config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: G130H wavelength: 1200-1600 num_exp: 1 time_per_exp: 0.1S priority: 1 param_1: TYPE = UP, param_2: SEARCH-SIZE-X=6, param_3: SEARCH-SIZE-Y=2, param_4: SCAN-STEP-X=0.7, param_5: SCAN-STEP-Y=0.7, req_1: ONBOARD ACQ FOR 2.5 ! linenum: 2.500 targname: HD77581 config: FOS/BL opmode: ACQ/PEAK aperture: 0.5 sp_element: G130H wavelength: 1200-1600 num_exp: 1 time_per_exp: 0.2S priority: 1 param_1: TYPE = UP, param_2: SEARCH-SIZE-X=3, param_3: SEARCH-SIZE-Y=3, param_4: SCAN-STEP-X=0.35, param_5: SCAN-STEP-Y=0.35, req_1: ONBOARD ACQ FOR 3.00 ! linenum: 3.000 targname: HD77581 config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G130H wavelength: 1200-1600 num_exp: 1 time_per_exp: 2080S s_to_n: 30 s_to_n_time: 20S fluxnum_1: 8 priority: 1 param_1: STEP-PATT=DEF, param_2: READ-TIME=20 req_1: PERIOD 8.96426D +/- 0.00018D; req_2: PHASE 0.00 +/- 0.05; req_3: ZERO-PHASE JD2449173.84896 +/- 0.0D; req_4: NON-INT / 3; comment_1: SEE GENERAL FORM FOR SPECIAL comment_2: SCHEDULING REQUIREMENTS ! linenum: 7.000 targname: HD77581 config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: G130H wavelength: 1200-1600 num_exp: 1 time_per_exp: 0.1S priority: 1 param_1: TYPE = UP, param_2: SEARCH-SIZE-X=1, param_3: SEARCH-SIZE-Y=3, param_5: SCAN-STEP-Y=1.4, req_1: CYCLE 3 / 7 - 9; req_2: ONBOARD ACQ FOR 8; req_3: SEQ 7 - 9 NO GAP comment_1: OBSERVATIONS TO BE COORDINATED WITH comment_2: SIMULTANEOUS X-RAY OBSERVATION ! linenum: 8.000 targname: HD77581 config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: G130H wavelength: 1200-1600 num_exp: 1 time_per_exp: 0.1S priority: 1 param_1: TYPE = UP, param_2: SEARCH-SIZE-X=6, param_3: SEARCH-SIZE-Y=2, param_4: SCAN-STEP-X=0.7, param_5: SCAN-STEP-Y=0.7, req_1: ONBOARD ACQ FOR 8.5 ! linenum: 8.500 targname: HD77581 config: FOS/BL opmode: ACQ/PEAK aperture: 0.5 sp_element: G130H wavelength: 1200-1600 num_exp: 1 time_per_exp: 0.2S priority: 1 param_1: TYPE = UP, param_2: SEARCH-SIZE-X=3, param_3: SEARCH-SIZE-Y=3, param_4: SCAN-STEP-X=0.35, param_5: SCAN-STEP-Y=0.35, req_1: ONBOARD ACQ FOR 9.0 ! linenum: 9.000 targname: HD77581 config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G130H wavelength: 1200-1600 num_exp: 1 time_per_exp: 2080S s_to_n: 30 s_to_n_time: 20S fluxnum_1: 8 priority: 1 param_1: STEP-PATT=DEF, param_2: READ-TIME=20 req_1: PHASE 0.50 +/- 0.05 OF REF 3; req_2: NON-INT / 9 comment_1: SEE GENERAL FORM FOR SPECIAL comment_2: SCHEDULING REQUIREMENTS ! linenum: 10.000 targname: HD77581 config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: G130H wavelength: 1200-1600 num_exp: 1 time_per_exp: 0.1S priority: 1 param_1: TYPE = UP, param_2: SEARCH-SIZE-X=1, param_3: SEARCH-SIZE-Y=3, param_4: SCAN-STEP-Y=1.4, req_1: CYCLE 3 / 10 - 15; req_2: ONBOARD ACQ FOR 11; req_3: SEQ 10 - 15 NO GAP comment_1: OBSERVATIONS TO BE COORDINATED WITH comment_2: SIMULTANEOUS X-RAY OBSERVATION ! linenum: 11.000 targname: HD77581 config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: G130H wavelength: 1200-1600 num_exp: 1 time_per_exp: 0.1S priority: 1 param_1: TYPE = UP, param_2: SEARCH-SIZE-X=6, param_3: SEARCH-SIZE-Y=2, param_4: SCAN-STEP-X=0.7, param_5: SCAN-STEP-Y=0.7 req_1: ONBOARD ACQ FOR 11.5 ! linenum: 11.500 targname: HD77581 config: FOS/BL opmode: ACQ/PEAK aperture: 0.5 sp_element: G130H wavelength: 1200-1600 num_exp: 1 time_per_exp: 0.2S priority: 1 param_1: TYPE = UP, param_2: SEARCH-SIZE-X=3, param_3: SEARCH-SIZE-Y=3, param_4: SCAN-STEP-X=0.35, param_5: SCAN-STEP-Y=0.35 req_1: ONBOARD ACQ FOR 12 ! linenum: 12.000 targname: HD77581 config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G130H wavelength: 1200-1600 num_exp: 1 time_per_exp: 2080S s_to_n: 30 s_to_n_time: 20S fluxnum_1: 8 priority: 1 param_1: STEP-PATT=DEF, param_2: READ-TIME=20 req_1: PHASE 0.60 +/- 0.05 OF REF 3; req_2: NON-INT / 12 comment_1: SEE GENERAL FORM FOR SPECIAL comment_2: SCHEDULING REQUIREMENTS ! linenum: 15.000 targname: HD77581 config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G130H wavelength: 1200-1600 num_exp: 1 time_per_exp: 30M s_to_n: 30 s_to_n_time: 20S fluxnum_1: 8 priority: 1 param_1: STEP-PATT=DEF req_4: NON-INT / 15; comment_1: SEE GENERAL FORM FOR SPECIAL comment_2: SCHEDULING REQUIREMENTS ! ! end of exposure logsheet ! No scan data records found