! $Id: 5418,v 4.1 1994/07/27 17:44:00 pepsa Exp $ coverpage: title_1: THE ORIGIN OF THE ULTRA-VIOLET SPECTRAL COMPONENTS IN title_2: THE POLAR-LIKE INTERMEDIATE POLAR, RE075 CYCLE 4 HIGH sci_cat: HOT STARS sci_subcat: ERUPTIVE BINARIES proposal_for: GO pi_fname: SIMON pi_mi: R pi_lname: ROSEN pi_inst: UNIVERSITY OF LEICESTER pi_country: U.K. hours_pri: 8.50 num_pri: 1 fos: Y time_crit: N off_fname: KEN off_lname: POUNDS off_title: HEAD OF DEPT. off_inst: 8042 off_addr_1: DEPT. OF PHYSICS off_addr_2: UNIVERSITY OF LEICESTER off_addr_3: UNIVERSITY RD. off_city: LEICESTER off_country: U.K. off_phone: UK-533-523509 ! end of coverpage abstract: line_1: RE0751+14, is arguably the most important magnetic cataclysmic variable (CV) to line_2: be discovered for many years. Although it is undoubtedly an intermediate polar, line_3: it also exhibits highly unusual properties (e.g. a strong EUV component, line_4: modulated optical/IR polarization, X-ray, optical and IR dips in its rotational line_5: light curve and a very red rotational pulsation) which strongly suggest that line_6: its white dwarf possesses a powerful magnetic field, similar to that associated line_7: with the strongly magnetic (B>10MG) polars. Thus RE0751+14 is apparently an line_8: interloper, occupying a new, uncharted domain in the field distribution of the line_9: magnetic CVs which was previously thought to be bimodal. The study of RE0751+14 line_10: is therefore of fundamental importance to our knowledge of the field line_11: distribution in magnetic CVs and consequently of their evolutionary line_12: relationship. The UV waveband is crucial to this study because magnetic line_13: disruption and control of the accretion flow occurs at radii where the hot UV line_14: emitting material exists. We are proposing to use the HST FOS to secure the line_15: first highly time-resolved UV spectroscopy of RE0751+14. These will enable us, line_16: for the first time, to a) segregate the different UV continuum components (via line_17: their different temporal behaviour) and characterize their sources and b) line_18: measure the emission line flux variations to probe physical structure within line_19: the system. These observations will be complemented by a parallel HRS proposal line_20: to study the CIV line in detail. ! ! end of abstract general_form_proposers: lname: ROSEN fname: SIMON title: PI mi: R inst: UNIVERSITY OF LEICESTER country: UNITED KINGDOM esa: Y ! lname: DE MARTINO fname: DOMITILLA inst: 7650 country: SPAIN esa: Y ! lname: MOUCHET fname: MARTINE inst: 5414 country: FRANCE esa: Y ! lname: MASON fname: KEITH inst: 8054 country: UK esa: Y ! lname: WATSON fname: MIKE inst: 8042 country: UK esa: Y ! lname: KING fname: ANDREW inst: 8042 country: UK esa: Y ! lname: HOWELL fname: STEVE inst: 3180 country: USA esa: N ! lname: HELLIER fname: COEL inst: 3550 country: USA esa: N ! lname: PONMAN fname: TREVOR inst: DEPT OF SPACE RESEARCH, UNIVERSITY OF BIRMINGHAM country: UK esa: Y ! lname: BONNET-BIDAUD fname: JEAN-MARC inst: 5414 country: FRANCE esa: Y ! lname: MITTAZ fname: JON inst: 8054 country: UK esa: Y ! lname: HAKALA fname: PASI inst: 5330 country: FINLAND esa: N ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We are proposing to secure highly time-resolved FOS UV line_2: spectra of the polar-like intermediate polar, RE0751+14. line_3: Before we can fully assess exactly why this new object is so line_4: different from other IPs and how it fits into the line_5: evolutionary and structural framework of the magnetic CVs, line_6: we must identify and establish the nature of the various line_7: sources of emission in the system. Separating the different line_8: components (emission sources) such as the magnetically line_9: dominated accretion flow, any disk and perhaps a disk bright line_10: spot, is facilitated by the fact that they will vary on line_11: different timescales (i.e. the white dwarf rotation period, line_12: the orbital period and the beat period between them). We aim line_13: to identify spectral variability on these different line_14: timescales to isolate and quantitatively characterize the line_15: sources of continuum emission in the UV which probes the line_16: vitally important inner regions on and around the white line_17: dwarf. These observations, together with a parallel HRS line_18: proposal to study the C IV line in detail, will provide line_19: essential information about the relationship between the line_20: line and continuum sources. ! question: 3 section: 2 line_1: To achieve these objectives we will use the FOS with the line_2: 0.9" aperture and the G160L grating to cover the 1150-2500A line_3: wavelength range. Use of the blue digicon detector is line_4: preferred so as to provide coverage down to the shortest UV line_5: wavelengths (essential to monitor the putative steep line_6: component in the far UV). We request coverage of one binary line_7: orbital period (6 hrs). Observations should be carried out line_8: using FOS RAPID mode, acquiring continuous sequences of 10s line_9: exposures. ! question: 4 section: 1 line_1: Testing for the presence of the UV emitting inner disk, line_2: constraining the tail of the emission from the heated line_3: accretion region and identifying the source of the beat line_4: period variations in RE0751+14 are all issues that can only line_5: (or are best) resolved by spectral studies in the UV, hence line_6: the need for space-borne instrumentation. line_7: We recently (Feb 1993) secured an IUE observation of line_8: RE0751+14 which, when combined with our optical and IR line_9: spectra, shows a distinct flattening at UV wavelengths. line_10: Moreover, these spectra show evidence for continuum and line line_11: variations on timescales comparable to the 5.3 hr orbital line_12: period. However, we also expect spectral variability to line_13: occur on the 13.9 minute white dwarf rotation period in line_14: RE0751+14 which means we must subsample this timescale. The line_15: relative faintness of RE0751+14 (V~14.5) demands line_16: lengthy exposure times (multiples of the 13.9 minute spin line_17: cycle) with IUE to achieve adequate spectral quality. In any line_18: case, the readout and preparation times (~30 mins) line_19: inherent with the IUE cameras severely limit the rapidity line_20: with which exposures could be taken. To achieve our line_21: objectives, we must sample the UV spectrum on timescales at line_22: least as short as 1 minute and this can only be done with HST. ! question: 5 section: 1 line_1: We are not requesting time-critical observations. However, line_2: it is particularly worth noting that the binary orbital line_3: period of ~5.3 hours in RE0751+14 is very well suited to the line_4: use of contiguous HST orbits. The requested exposure of 6 line_5: hours, assuming we get about 40 mins of data per HST orbit, line_6: requires about 9 orbits (each 40 minute window covers line_7: about 0.13 orbital cycles). Fortuitously, it turns out that line_8: (because the 96 minute HST orbit is almost exactly 0.3 of a line_9: binary cycle) if these orbits are scheduled contiguously, line_10: the phase sampling is near perfect and is extremely line_11: efficient, leaving essentially no gaps in the orbital line_12: coverage. We will also cover more than 2 spin cycles in each line_13: HST orbital window (ie >20 spin cycles in total). ! question: 6 section: 1 line_1: Routine FOS calibration data will be sufficient for our purposes. ! ! ! question: 8 section: 1 line_1: To maximize compatibility between our HST spectra and the line_2: optical distribution, we will be aiming to secure line_3: simultaneous or near simultaneous ground-based optical data. line_4: Long timescale (weeks-years) changes in the system could line_5: invalidate simple combining of our current optical spectra line_6: with the HST UV data. If we can establish that such changes line_7: have not occurred (e.g. if the optical spectra taken line_8: simultaneously with the HST are similar to those we already line_9: possess), we can then incorporate data from a wider line_10: wavelength range (X-ray/EUV and IR) to provide broader line_11: spectral coverage for the model fits. We point out, however, line_12: that whilst these contemporaneous optical observations are line_13: desirable and their arrangement will be vigorously pursued, line_14: the proposed UV study is a stand-alone project which will line_15: provide vital new information on the nature of RE0751+14, line_16: irrespective of whether other data are secured at the same line_17: time. ! question: 8 section: 2 line_1: We stress that we will be seeking to arrange suitable line_2: optical observations that fit in with the HST schedule, line_3: rather than requiring HST observations to be dependent on line_4: optical scheduling. Nevertheless, the optimum ground based line_5: observing time is between November and early March and HST line_6: observations in, or as near to this interval as possible, line_7: will allow maximum continuous ground-based coverage. line_8: Obtaining the necessary optical observing time should not line_9: be a problem as one of the collaborators, SBH, has access to line_10: the Lowell observatory whilst another, CH, has access to the line_11: McDonald observatory. In both cases, observing allocations line_12: can be gained at relatively short notice. To extend the line_13: coverage, we will also apply for observing time on the RGO line_14: (SRR,KOM) or Nordic optical telescope on La Palma (PJH) and line_15: also at the Canada-France-Hawaii and 6m Zelenchuk (MM,JMB-B) line_16: telescopes. ! question: 9 section: 1 line_1: GO-3578 Line eclipse mapping of an accretion disk wind. (KOM). line_2: GO-3579 The UV orbital lightcurve of the X-ray binary X1822-371. line_3: (KOM). line_4: GO-4661 Ultra-violet eclipse mapping of the accretion flow in the line_5: eclipsing Intermediate Polar, EX Hya. (SRR,KOM,MGW). line_6: GO-4449 Occultation studies of RE1149+28: An object with an extreme line_7: EUV/optical ratio. (JPDM,KOM,SRR). line_8: None of these proposals/observations are related to the line_9: objectives being pursued here. ! question: 10 section: 1 line_1: The analysis of our HST data will be undertaken by the PI and the line_2: Co-I's. All proposers have access to DEC Vax and line_3: alpha machines or SUN stations which are dedicated to astronomical line_4: research. ! !end of general form text general_form_address: lname: ROSEN fname: SIMON mi: R category: PI inst: University of Leicester addr_1: Dept. of Physics, addr_3: University Rd., city: Leicester country: UNITED KINGDOM phone: 0533 552077 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: STAR-075117+144424 descr_1: A, 154 pos_1: RA = 07H 51M 17.39S +/- 0.03S, pos_2: DEC = +14D 44' 24.6" +/- 0.4", pos_3: PLATE-ID = 01LS equinox: J2000 fluxnum_1: 1 fluxval_1: V = 14.5 +/- 0.1 fluxnum_2: 2 fluxval_2: B-V = 0.1 +/- 0.2 fluxnum_3: 3 fluxval_3: E(B-V) = 0.0 +/- 0.1 fluxnum_4: 4 fluxval_4: F-CONT(1200) = 3.0 +/- 0.7 E-14 fluxnum_5: 5 fluxval_5: F-CONT(1550) = 2.8 +/- 0.7 E-14 fluxnum_6: 6 fluxval_6: F-LINE(1550) = 2.0 +/- 1.5 E-13 fluxnum_7: 7 fluxval_7: W-LINE(1550) = 10 +/- 3 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: STAR-075117+144424 config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: G400H num_exp: 1 time_per_exp: 0.2S fluxnum_1: 1 fluxnum_2: 3 priority: 1 param_1: SCAN-STEP-Y=1.204, param_2: SEARCH-SIZE-X=1, param_3: SEARCH-SIZE-Y=3, req_1: ONBOARD ACQ FOR 1.5; req_2: CYCLE 4; comment_1: CONTIGUOUS ORBITS FOR LINES 1-10 comment_2: ARE HIGHLY DESIRABLE TO GET MOST comment_3: UNIFORM COVERAGE OF 5.5H ORBIT ! linenum: 1.500 targname: STAR-075117+144424 config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: G400H num_exp: 1 time_per_exp: 0.2S fluxnum_1: 1 fluxnum_2: 3 priority: 1 param_1: SCAN-STEP-X=0.602, param_2: SCAN-STEP-Y=0.602 param_3: SEARCH-SIZE-X=6, param_4: SEARCH-SIZE-Y=2, req_1: ONBOARD ACQ FOR 1.7; req_2: CYCLE 4; ! linenum: 1.700 targname: STAR-075117+144424 config: FOS/BL opmode: ACQ/PEAK aperture: 0.3 sp_element: G400H num_exp: 1 time_per_exp: 1S fluxnum_1: 1 fluxnum_2: 3 priority: 1 param_1: SCAN-STEP-X=.172 param_2: SCAN-STEP-Y=.172 param_3: SEARCH-SIZE-X=5 param_4: SEARCH-SIZE-Y=5 req_1: ONBOARD ACQ FOR 2-10; req_2: CYCLE 4; ! linenum: 2.000 targname: STAR-075117+144424 config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G160L wavelength: 1850 num_exp: 1 time_per_exp: 40M s_to_n: 5 s_to_n_time: 10S fluxnum_1: 5 priority: 1 param_1: COMB=YES param_2: READ-TIME=10 req_1: CYCLE 4 comment_1: THIS IS A 13.9 MIN PULSAR SO DATA comment_2: SEGMENTS SHORTER THAN THIS ARE OF comment_3: LIMITED USE. DATA WILL BE PHASE comment_4: FOLDED FOR S/N. IF 40 MIN EXPOS- comment_5: URES ARE NOT FEASIBLE, MORE, comment_6: SHORTER EXPOSURES CAN BE USED. ! linenum: 3.000 targname: STAR-075117+144424 config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G160L wavelength: 1850 num_exp: 1 time_per_exp: 40M s_to_n: 5 s_to_n_time: 10S fluxnum_1: 5 priority: 1 param_1: COMB=YES param_2: READ-TIME=10 req_1: CYCLE 4 ! linenum: 4.000 targname: STAR-075117+144424 config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G160L wavelength: 1850 num_exp: 1 time_per_exp: 40M s_to_n: 5 s_to_n_time: 10S fluxnum_1: 5 priority: 1 param_1: COMB=YES param_2: READ-TIME=10 req_1: CYCLE 4 ! linenum: 5.000 targname: STAR-075117+144424 config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G160L wavelength: 1850 num_exp: 1 time_per_exp: 40M s_to_n: 5 s_to_n_time: 10S fluxnum_1: 5 priority: 1 param_1: COMB=YES param_2: READ-TIME=10 req_1: CYCLE 4 ! linenum: 6.000 targname: STAR-075117+144424 config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G160L wavelength: 1850 num_exp: 1 time_per_exp: 40M s_to_n: 5 s_to_n_time: 10S fluxnum_1: 5 priority: 1 param_1: COMB=YES param_2: READ-TIME=10 req_1: CYCLE 4 ! linenum: 7.000 targname: STAR-075117+144424 config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G160L wavelength: 1850 num_exp: 1 time_per_exp: 40M s_to_n: 5 s_to_n_time: 10S fluxnum_1: 5 priority: 1 param_1: COMB=YES param_2: READ-TIME=10 req_1: CYCLE 4 ! linenum: 8.000 targname: STAR-075117+144424 config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G160L wavelength: 1850 num_exp: 1 time_per_exp: 40M s_to_n: 5 s_to_n_time: 10S fluxnum_1: 5 priority: 1 param_1: COMB=YES param_2: READ-TIME=10 req_1: CYCLE 4 ! linenum: 9.000 targname: STAR-075117+144424 config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G160L wavelength: 1850 num_exp: 1 time_per_exp: 40M s_to_n: 5 s_to_n_time: 10S fluxnum_1: 5 priority: 1 param_1: COMB=YES param_2: READ-TIME=10 req_1: CYCLE 4 ! linenum: 10.000 targname: STAR-075117+144424 config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G160L wavelength: 1850 num_exp: 1 time_per_exp: 20M s_to_n: 5 s_to_n_time: 10S fluxnum_1: 5 priority: 1 param_1: COMB=YES param_2: READ-TIME=10 req_1: CYCLE 4 ! ! end of exposure logsheet ! No scan data records found