! File: 4656C.PROP ! Database: PEPDB ! Date: 22-FEB-1994:21:23:48 coverpage: title_1: SPIN-CYCLE VARIATIONS OF THE UV EMISSION LINES OF INTERMEDIATE POLARS: title_2: CYCLE3 MEDIUM sci_cat: HOT STARS sci_subcat: ERUPTIVE BINARIES proposal_for: GO pi_title: DR. pi_fname: COEL pi_lname: HELLIER pi_inst: DEPARTMENT OF ASTRONOMY, UNIVERSITY OF TEXAS AT AUSTIN pi_country: USA pi_phone: 512 471 3000 keywords_1: CATACLYSMIC VARIABLES, INTERMEDIATE POLARS hours_pri: 6.90 num_pri: 1 hrs: Y pi_position: HUBBLE FELLOW off_fname: J. off_mi: L. off_lname: CULHANE off_title: PROFESSOR off_inst: 8054 off_addr_1: HOLMBURY ST MARY off_addr_2: DORKING off_addr_3: SURREY off_country: UK off_phone: +44 483 274111 ! end of coverpage abstract: line_1: The intermediate polars are a prime opportunity for observing the interaction line_2: of an accretion flow with a strong magnetic field. Yet many fundamental issues line_3: remain unresolved. For instance, it is not known whether the accretion flow line_4: passes through a partial accretion disk, as suggested by many optical studies, line_5: or whether material accretes through the direct impact of the accretion stream line_6: with the magnetosphere, as suggested by the presence of beat period modulations line_7: in intermediate polar X-ray light curves. The low energy optical emission might line_8: not trace the dominant accretion flow, but we have no velocity information in line_9: the X-ray band. Spin-cycle resolved UV spectroscopy will both give velocity line_10: information and trace the accretion flow to within 1-2 white dwarf radii of line_11: the white dwarf surface, allowing a direct link to the X-ray studies. AO Psc line_12: is a typical intermediate polar, is one of the brightest in the UV, and shows line_13: the clearest spin-cycle variations in the optical emission lines - it is thus line_14: the best target for the first HST spectroscopic study of an intermediate polar. line_15: We propose to use the GHRS to obtain high time and spectral resolution line_16: observations of the CIV 1550 line, which is prominent in the spectrum of line_17: AO Psc. Watching how the line profile changes around the 805-s spin cycle will line_18: reveal the accretion flow as it approaches the X-ray emitting shock, settling line_19: many uncertainties regarding the flow of material from the magnetosphere line_20: onto the white dwarf. ! ! end of abstract general_form_proposers: lname: HELLIER fname: COEL title: DR. inst: DEPARTMENT OF ASTRONOMY, UNIVERSITY OF TEXAS AT AUSTIN country: USA ! lname: MASON fname: KEITH mi: O. inst: MULLARD SPACE SCIENCE LABORATORY country: UNITED KINGDOM esa: Y ! lname: ROBINSON fname: EDWARD mi: L. inst: DEPARTMENT OF ASTRONOMY, UNIVERSITY OF TEXAS AT AUSTIN country: USA ! ! end of general_form_proposers block general_form_text: question: 2 section: 1 line_1: ! question: 3 section: 1 line_1: We will obtain time-resolved GHRS spectroscopy of the CIV 1550 line of the line_2: magnetic cataclysmic variable AO Psc. We will use the G160M grating giving a line_3: 34 ang range covering the whole line (FWZI 25 ang). We will use the RAPID line_4: mode to obtain a time resolution of 10 secs. This is required to resolve line_5: the rapid line profile changes through the 805 sec spin cycle of AO Psc. line_6: The requested exposure time is calculated both to give sufficient signal to line_7: noise, to cover enough 30 spin cycles to reduce random flickering, and line_8: to cover 2 orbital cycles (3.5 hrs). We aim to obtain a signal to noise of line_9: about 20 in each of 20 phase bins round the spin cycle with a velocity line_10: resolution of 50 Km s-1 in the GHRS spectra (which at 1550 ang corresponds line_11: to 4 diodes in the array. The phase-averaged IUE spectrum of AO Psc gives line_12: flux levels of 1.4 e-13 and 3.0 e-13 erg s-1 cm-2 A-1 at the base and peak line_13: of the CIV 1550 line respectively. Using the quoted sensitivity for our line_14: instrumental setup of 4.41 e11, we obtain count rates of 0.06 & 0.13 s-1 line_15: diode-1 respectively, or 0.24 & 0.52 counts s-1 per 50 km s-1 resolution line_16: element. Hence with our exposure time of 6.9 hrs we will obtain 300 & 650 line_17: counts for the base and peak of the line respectively in each resolution line_18: element in each spin-phase bin, corresponding to S/N values of 17 & 25. This line_19: time cover 30 spin pulses, and thus the data will record genuine spin-cycle line_20: variations; observations of a small number of spin cycles can be affected line_21: by random flickering in these stars. The time will also cover two 3.5-hr line_22: binary periods of AO Psc. This will ensure that after allowing for the line_23: effects of earth occultations, SAA etc, the orbital cycle is fully sampled. ! question: 4 section: 1 line_1: The program involves UV spectroscopy of a 13th mag star with a high time line_2: resolution (resolving a 13 min period) and a high spectral resolution (< 0.5 line_3: ang). The IUE has very long readout times (30 mins) and low sensitivity, which line_4: mean that it cannot undertake this project - only low resolution, phase line_5: averaged spectra can be obtained. Hence, the program can only by done with the line_6: HST. The proposal is to look at high ionization lines (C IV) which are not line_7: accessible from the ground. Complementary work on emission lines seen in the line_8: optical has been pursued on our target object and several similar systems - line_9: this work points to the large gains likely to be made from observing in the UV. ! question: 5 section: 1 line_1: None required. ! question: 6 section: 1 line_1: None required. ! question: 7 section: 1 line_1: The applicants have substantial experience in similar projects with line_2: ground-based optical spectroscopy. Standard reduction procedures will be line_3: adequate while the analysis is likely to use similar procedures and software line_4: to those developed for the optical studies. To aid interpretation of the line_5: results, we also intend further developing our code modelling the geometry line_6: of the accretion flow to investigate emission line profiles. ! question: 8 section: 1 line_1: None. ! question: 9 section: 1 line_1: PI HELLIER has not previously applied for HST time. line_2: Co-I MASON has been awarded GO time for 2 projects, line_3: neither of which are related to the current proposal. line_4: 3578 `Line eclipse mapping of an accretion disk wind' line_5: 3579 `The UV orbital lightcurve of the X-ray binary X1822-371' line_6: Co-I ROBINSON is a member of the High-Speed Photometer IDT and was actively line_7: involved in Orbital and Science Verification of the instrument. line_8: So far, he has received data from two GTO science programs: line_9: Program GTO-3253 "Optical and Ultraviolet Observations of Radio Pulsars" line_10: Results have been presented at two international meetings, line_11: and a paper reporting the results has been submitted to the Astrophysical line_12: Journal. The program is not related to this proposal. line_13: Program GTO-1092 "Eclipses of Cataclysmic Variable Stars" line_14: Preliminary results were presented at the Columbus AAS meeting. The line_15: program is only peripherally related to this proposal. line_16: ROBINSON is also a Co-PI on two GO programs: line_17: Program 3600 "Oscillations, Flaring and Tomography of AE Aquarii" line_18: The observations have not yet been scheduled. The program line_19: is closely related to this proposal. line_20: Program GO-3683 "Accretion Disk Mapping in Eclipsing Cataclysmic Variables" line_21: The observations have not yet been scheduled. The program is only line_22: peripherally related to this proposal. ! question: 10 section: 1 line_1: A SPARC-2 workstation will be assigned to this project. line_2: Facilities for contemporaneous ground based observations will be line_3: provided by McDonald Observatory. ! !end of general form text general_form_address: lname: HELLIER fname: COEL title: DR. category: PI inst: 3550 addr_1: Department of Astronomy, addr_2: University of Texas city: Austin state: TX zip: 78712 country: USA phone: 512 471 3000 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: AO-PSC name_2: GSC5238-0223 descr_1: A,151,154,161,906 pos_1: PLATE-ID=03U1, pos_2: RA = 22H 55M 17.9S +/- 1", pos_3: DEC = -03D 10' 39" +/- 1" equinox: 2000 fluxnum_1: 1 fluxval_1: V=13.4 +/- 0.3 fluxnum_2: 2 fluxval_2: F-LINE(1549) = 2.4 +/- 0.5 E-13 fluxnum_3: 3 fluxval_3: W-LINE(1549) = 15 +/- 3 fluxnum_4: 4 fluxval_4: F-CONT(1520) = 1.5 +/- 0.5 E-13 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: AO-PSC config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 1.8S fluxnum_1: 4 priority: 1 param_1: BRIGHT=RETURN req_1: ONBOARD ACQ FOR 2-9; req_2: CYCLE 3; req_3: GROUP 1-13 WITHIN 30H ! linenum: 2.000 targname: AO-PSC config: HRS opmode: RAPID aperture: 2.0 sp_element: G160M wavelength: 1548 num_exp: 1 time_per_exp: 38M s_to_n: 10 s_to_n_time: 20M fluxnum_1: 2 fluxnum_2: 3 fluxnum_3: 4 priority: 1 param_1: SAMPLE-TIME=10.0 req_1: CYCLE 3 comment_1: EXPOSURE TIME IS NOT CALCULATED SOLELY comment_2: ON SIGNAL TO NOISE RATIO, THE 6.9H IS comment_3: ALSO CALCULATED TO COVER 30 SPIN comment_4: CYCLES AND 2 ORBITAL CYCLES OF AO PSC, comment_5: SEE QUESTION 3 FOR FULL DETAILS. ! linenum: 3.000 targname: AO-PSC config: HRS opmode: RAPID aperture: 2.0 sp_element: G160M wavelength: 1548 num_exp: 1 time_per_exp: 38M s_to_n: 10 s_to_n_time: 20M fluxnum_1: 2 fluxnum_2: 3 fluxnum_3: 4 priority: 1 param_1: SAMPLE-TIME=10.0 req_1: CYCLE 3 comment_1: EXPOSURE TIME IS NOT CALCULATED SOLELY comment_2: ON SIGNAL TO NOISE RATIO, THE 6.9H IS comment_3: ALSO CALCULATED TO COVER 30 SPIN comment_4: CYCLES AND 2 ORBITAL CYCLES OF AO PSC, comment_5: SEE QUESTION 3 FOR FULL DETAILS. ! linenum: 4.000 targname: AO-PSC config: HRS opmode: RAPID aperture: 2.0 sp_element: G160M wavelength: 1548 num_exp: 1 time_per_exp: 38M s_to_n: 10 s_to_n_time: 20M fluxnum_1: 2 fluxnum_2: 3 fluxnum_3: 4 priority: 1 param_1: SAMPLE-TIME=10.0 req_1: CYCLE 3 comment_1: EXPOSURE TIME IS NOT CALCULATED SOLELY comment_2: ON SIGNAL TO NOISE RATIO, THE 6.9H IS comment_3: ALSO CALCULATED TO COVER 30 SPIN comment_4: CYCLES AND 2 ORBITAL CYCLES OF AO PSC, comment_5: SEE QUESTION 3 FOR FULL DETAILS. ! linenum: 5.000 targname: AO-PSC config: HRS opmode: RAPID aperture: 2.0 sp_element: G160M wavelength: 1548 num_exp: 1 time_per_exp: 38M s_to_n: 10 s_to_n_time: 20M fluxnum_1: 2 fluxnum_2: 3 fluxnum_3: 4 priority: 1 param_1: SAMPLE-TIME=10.0 req_1: CYCLE 3 comment_1: EXPOSURE TIME IS NOT CALCULATED SOLELY comment_2: ON SIGNAL TO NOISE RATIO, THE 6.9H IS comment_3: ALSO CALCULATED TO COVER 30 SPIN comment_4: CYCLES AND 2 ORBITAL CYCLES OF AO PSC, comment_5: SEE QUESTION 3 FOR FULL DETAILS. ! linenum: 6.000 targname: AO-PSC config: HRS opmode: RAPID aperture: 2.0 sp_element: G160M wavelength: 1548 num_exp: 1 time_per_exp: 38M s_to_n: 10 s_to_n_time: 20M fluxnum_1: 2 fluxnum_2: 3 fluxnum_3: 4 priority: 1 param_1: SAMPLE-TIME=10.0 req_1: CYCLE 3 comment_1: EXPOSURE TIME IS NOT CALCULATED SOLELY comment_2: ON SIGNAL TO NOISE RATIO, THE 6.9H IS comment_3: ALSO CALCULATED TO COVER 30 SPIN comment_4: CYCLES AND 2 ORBITAL CYCLES OF AO PSC, comment_5: SEE QUESTION 3 FOR FULL DETAILS. ! linenum: 7.000 targname: AO-PSC config: HRS opmode: RAPID aperture: 2.0 sp_element: G160M wavelength: 1548 num_exp: 1 time_per_exp: 38M s_to_n: 10 s_to_n_time: 20M fluxnum_1: 2 fluxnum_2: 3 fluxnum_3: 4 priority: 1 param_1: SAMPLE-TIME=10.0 req_1: CYCLE 3 comment_1: EXPOSURE TIME IS NOT CALCULATED SOLELY comment_2: ON SIGNAL TO NOISE RATIO, THE 6.9H IS comment_3: ALSO CALCULATED TO COVER 30 SPIN comment_4: CYCLES AND 2 ORBITAL CYCLES OF AO PSC, comment_5: SEE QUESTION 3 FOR FULL DETAILS. ! linenum: 8.000 targname: AO-PSC config: HRS opmode: RAPID aperture: 2.0 sp_element: G160M wavelength: 1548 num_exp: 1 time_per_exp: 38M s_to_n: 10 s_to_n_time: 20M fluxnum_1: 2 fluxnum_2: 3 fluxnum_3: 4 priority: 1 param_1: SAMPLE-TIME=10.0 req_1: CYCLE 3 comment_1: EXPOSURE TIME IS NOT CALCULATED SOLELY comment_2: ON SIGNAL TO NOISE RATIO, THE 6.9H IS comment_3: ALSO CALCULATED TO COVER 30 SPIN comment_4: CYCLES AND 2 ORBITAL CYCLES OF AO PSC, comment_5: SEE QUESTION 3 FOR FULL DETAILS. ! linenum: 9.000 targname: AO-PSC config: HRS opmode: RAPID aperture: 2.0 sp_element: G160M wavelength: 1548 num_exp: 1 time_per_exp: 38M s_to_n: 10 s_to_n_time: 20M fluxnum_1: 2 fluxnum_2: 3 fluxnum_3: 4 priority: 1 param_1: SAMPLE-TIME=10.0 req_1: CYCLE 3 comment_1: EXPOSURE TIME IS NOT CALCULATED SOLELY comment_2: ON SIGNAL TO NOISE RATIO, THE 6.9H IS comment_3: ALSO CALCULATED TO COVER 30 SPIN comment_4: CYCLES AND 2 ORBITAL CYCLES OF AO PSC, comment_5: SEE QUESTION 3 FOR FULL DETAILS. ! linenum: 10.000 targname: AO-PSC config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 1.8S fluxnum_1: 4 priority: 1 param_1: BRIGHT=RETURN req_1: ONBOARD ACQ FOR 11-13; req_2: CYCLE 3 ! linenum: 11.000 targname: AO-PSC config: HRS opmode: RAPID aperture: 2.0 sp_element: G160M wavelength: 1548 num_exp: 1 time_per_exp: 38M s_to_n: 10 s_to_n_time: 20M fluxnum_1: 2 fluxnum_2: 3 fluxnum_3: 4 priority: 1 param_1: SAMPLE-TIME=10.0 req_1: CYCLE 3 comment_1: EXPOSURE TIME IS NOT CALCULATED SOLELY comment_2: ON SIGNAL TO NOISE RATIO, THE 6.9H IS comment_3: ALSO CALCULATED TO COVER 30 SPIN comment_4: CYCLES AND 2 ORBITAL CYCLES OF AO PSC, comment_5: SEE QUESTION 3 FOR FULL DETAILS. ! linenum: 12.000 targname: AO-PSC config: HRS opmode: RAPID aperture: 2.0 sp_element: G160M wavelength: 1548 num_exp: 1 time_per_exp: 38M s_to_n: 10 s_to_n_time: 20M fluxnum_1: 2 fluxnum_2: 3 fluxnum_3: 4 priority: 1 param_1: SAMPLE-TIME=10.0 req_1: CYCLE 3 comment_1: EXPOSURE TIME IS NOT CALCULATED SOLELY comment_2: ON SIGNAL TO NOISE RATIO, THE 6.9H IS comment_3: ALSO CALCULATED TO COVER 30 SPIN comment_4: CYCLES AND 2 ORBITAL CYCLES OF AO PSC, comment_5: SEE QUESTION 3 FOR FULL DETAILS. ! linenum: 13.000 targname: AO-PSC config: HRS opmode: RAPID aperture: 2.0 sp_element: G160M wavelength: 1548 num_exp: 1 time_per_exp: 38M s_to_n: 10 s_to_n_time: 20M fluxnum_1: 2 fluxnum_2: 3 fluxnum_3: 4 priority: 1 param_1: SAMPLE-TIME=10.0 req_1: CYCLE 3 comment_1: EXPOSURE TIME IS NOT CALCULATED SOLELY comment_2: ON SIGNAL TO NOISE RATIO, THE 6.9H IS comment_3: ALSO CALCULATED TO COVER 30 SPIN comment_4: CYCLES AND 2 ORBITAL CYCLES OF AO PSC, comment_5: SEE QUESTION 3 FOR FULL DETAILS. ! ! end of exposure logsheet ! No scan data records found