! $Id: 5362,v 4.1 1994/07/27 17:06:12 pepsa Exp $ coverpage: title_1: A TIME_RESOLVED, HIGH_RESOLUTION UV STUDY OF THE WIND OUTFLOW title_2: IN THE EXCEPTIONAL CATACLYSMIC VARIABLE, V795 HER: CYCLE4 MEDIUM sci_cat: HOT STARS sci_subcat: ERUPTIVE BINARIES proposal_for: GO pi_fname: SIMON pi_lname: ROSEN pi_inst: UNIVERSITY OF LEICESTER pi_country: U.K. hours_pri: 13.85 num_pri: 1 fos: Y time_crit: Y 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: We propose to exploit the unique UV capabilities of the HST FOS to obtain the line_2: first time-resolved, high-resolution UV spectroscopy of the wind outflow in the line_3: enigmatic cataclysmic binary, V795 Her. Our previous IUE observations of this line_4: star have revealed extraordinary UV properties. Specifically, the SiIV and CIV line_5: line profiles change markedly on timescales at least as fast as the 30 minute line_6: exposure limit imposed by the sensitivity of IUE. Moreover, repeat observations line_7: over several allocation rounds have confirmed a coherent modulation on a period line_8: of 4.86hrs rather than at the known optical periods. It is well-established line_9: that many disk-accreting CVs show periodic UV line profile variation, but V795 line_10: Her breaks the mould in varying on a period that appears not to be the orbital line_11: period. A plausible origin for the usual orbital variation is wind shadowing line_12: of asymmetric disk structure induced by the mass transfer stream. However, it line_13: remains to be established whether such a model can be applied to the peculiar line_14: case of V795 Her. Indeed, it is unlikely that the intrinsic wind properties line_15: hold the key to the periodic UV line behaviour since the natural timescale of line_16: the wind source, believed to be seated in the inner disk, is of order minutes. line_17: The primary objectives are 1) to investigate and quantify radial velocity line_18: motion in the CIV emission component, 2) to define the nature and shortest line_19: timescales of variation in both the SiIV and CIV line profiles, 3) to measure line_20: any correlated continuum flux changes. ! ! end of abstract general_form_proposers: lname: ROSEN fname: SIMON title: PI mi: R inst: UNIVERSITY OF LEICESTER country: UNITED KINGDOM esa: Y ! lname: PRINJA fname: RAMAN inst: UNIVERSITY COLLEGE LONDON country: UNITED KINGDOM esa: Y ! lname: DREW fname: JANET inst: UNIVERSITY OF OXFORD country: UNITED KINGDOM esa: Y ! lname: HOWELL fname: STEVE inst: PLANETARY SCIENCES INSTITUTE country: USA esa: N ! lname: ROBINSON fname: EDWARD inst: UNIVERSITY OF TEXAS country: USA esa: N ! lname: SHAFTER fname: ALLEN inst: CALIFORNIA STATE UNIVERSITY,SAN DIEGO country: USA esa: N ! lname: MASON fname: KEITH inst: MULLARD SPACE SCIENCE LABORATORY country: UNITED KINGDOM esa: Y ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We will use the FOS (blue side digicon detector) with the G130H line_2: grating to access the far UV wavelength range between 1150A line_3: and 1600A. Using the 0.9 arc second aperture should provide line_4: data at about 1A resolution, a factor 5-6 improvement over our line_5: IUE data. Spectra will be recorded using 20s integrations line_6: with FOS RAPID mode to probe the fastest changes in the wind, line_7: enabling us to search for features within the CIV and SiIV line_8: absorption profiles that might be associated with clumping in line_9: the wind or other phenomena reflecting the inner disk rotation line_10: timescales. We anticipate a S/N of >10 per diode at the CIV line_11: continuum per 20s exposure. Co-adding spectra into 2-3 minute line_12: time bins will enhance the S/N for longer timescale studies line_13: (we can expect a S/N level ~30 per diode at the CIV continuum). line_14: This will permit close monitoring of the development of the line_15: absorption and emission components of the CIV line and for line_16: tracking inherent radial velocity motion (we can expect perhaps line_17: 40 time bins through the entire absorption event ($\sim$90 line_18: mins - 0.3 in phase). We will cover two 4.8hr cycles in a line_19: our requested 9.9hr exposure. Mildly time-critical observations line_20: are requested (see section 5) to ensure that we sample all line_21: phases of the 4.86 hr variation. We request three blocks of line_22: observations, each of six contiguous spacecraft orbits, with line_23: the blocks being separated by about 27 spacecraft orbits. ! question: 4 section: 1 line_1: Our 3 IUE observations of V795 Her revealed the 4.8hr periodic line_2: variability in its CIV and SiIV lines. However these obser- line_3: vations, the best that can be realistically achieved with IUE, line_4: can not address the rapid timescales of CIV line line_5: profile variability which is less than the minimum time line_6: between any of our IUE exposures (30 minutes). Only HST line_7: can probe the faster (minutes) timescales that are probably line_8: appropriate, e.g. the rapid evolution of the C IV absorption line_9: component which can convey vital information about the line_10: absorbing wind. Equally, we will exploit the factor ~6 line_11: improvement in spectral resolution of the HST FOS over IUE. line_12: Use of the high resolution IUE mode is not practicable due to line_13: the very low expected count rates and long exposure therefore line_14: needed to secure adequate S/N. Moreover, the poor IUE wavelength line_15: calibration (~ +/- 4A = +/-800 km/s) severely restricts any line_16: unambiguous search for motion of the emission component(s): line_17: we are searching for motion at this or smaller velocities line_18: The combination of enhanced spectral resolution and higher line_19: achievable S/N ratios offered by the HST FOS will be crucial line_20: in pinning down the cause of the profile variability and in line_21: quantifying basic outflow properties and parameters such as line_22: the limiting wind velocity. A further important advantage of line_23: FOS over IUE is the relative internal flux calibration between ! question: 4 section: 2 line_1: spectra. We need an accuracy of about 2% (over a 50A range) to line_2: constrain models but could only achieve ~10% with IUE, the line_3: limit imposed by internal IUE calibration uncertainties. line_4: Our feasibility estimates are based on scaling our observed line_5: IUE spectra by the sensitivity curves of the flat spectrum line_6: presented in the HST FOS documentation. We expect about 3.5, line_7: 6.6 and 8.0 cts/s/diode at the NV (1240) continuum, CIV line_8: continuum and the CIV (1550) line peak respectively or 70, 130 line_9: and 160 cts/diode respectively in each 20s exposure, resulting line_10: in a S/N >11/diode at C IV. To monitor longer timescale line_11: periodic changes, we will coadd the spectra into 2-3 minute line_12: bins yielding ~900 counts at the C IV continuum per bin. Since line_13: our primary interest is in the C IV and Si IV lines, which line_14: lie around the highest region of the FOS sensitivity curve, line_15: we anticipate high quality (S/N~20-30 per diode per 2-3 min line_16: spectrum) spectra for our study. In each 2-3 minute spectrum, line_17: we can expect to secure around 50000 counts in a 50A wide line_18: range at the CIV continuum, permitting us to readily achieve line_19: the objective of monitoring continuum flux changes to around line_20: 1-2% accuracy averaged over such a range. line_21: We seek a total of 9.9 hours on-source time to effectively line_22: sample two 4.8hr cycles (see section 5), allowing us to check line_23: for cycle-to-cycle variability. ! question: 5 section: 1 line_1: We are requesting (mildly) time-critical observations because line_2: the 4.86hr (292 minute) period of the UV lines differs by line_3: only 4 minutes from 3 times the HST Earth-orbital period. line_4: Thus, if we used contiguous orbits, we would sample only a line_5: limited range of phases, leaving large gaps in the phase line_6: coverage. To overcome this, we request that the observation line_7: be split into three blocks, each of six contiguous HST orbits line_8: (slots). This will provide eighteen ~30 minute slots of line_9: data (assuming an on-source window per HST orbit of about line_10: 30 mins) covering an effective interval of two 4.8hr periods. line_11: We further request that the blocks are spaced apart by around line_12: 27 HST orbits (1.8 days). line_13: Although we have declared this request as time-critical, line_14: it does not demand any specific start epoch, merely that the line_15: three blocks be spaced apart by a certain amount and that line_16: 6 contiguous HST orbits be used within each block. ! question: 6 section: 1 line_1: Routine FOS calibration data will be sufficient for our purposes. ! ! question: 8 section: 1 line_1: We will endeavour to obtain simultaneous or near line_2: simultaneous optical spectroscopy of V795 Her with the line_3: HST observations in order to search, in detail, for line_4: correlated optical emission line behaviour. Despite the line_5: substantial amounts of IUE data now taken, such line_6: simultaneous optical observations have yet to be secured. line_7: However, we stress that we will be seeking to arrange line_8: suitable optical observations that fit in with the HST line_9: schedule, rather than requiring HST observations to be line_10: dependent on optical scheduling. This should not be a line_11: problem since several members of this collaboration (SBH, line_12: ELR, AS) have access to suitable telescopes at the Lowell line_13: and McDonald Observatories for which time can be gained line_14: at relatively short notice. Nevertheless, the best time for line_15: ground-based observations of V795 Her is between April and line_16: August with June as the optimum choice. ! question: 9 section: 1 line_1: GO-3578 Line eclipse mapping of an accretion disk wind. line_2: (KOM,JED). Preliminary results presented at UK National line_3: Astronomy meeting in March 93. line_4: GO-3579 The UV orbital lightcurve of the X-ray binary line_5: X1822-371. (KOM) - not done. line_6: GO-3600 Oscillations, flaring and tomography of AE Aqr. line_7: (ELR). line_8: GO-3683 Accretion disk mapping in eclipsing cataclysmic line_9: variables. (ELR) line_10: GO-4661 Ultra-violet eclipse mapping of the accretion flow line_11: in the eclipsing Intermediate Polar, EX Hya. (SRR,KOM,RKP). line_12: This programme failed due to satellite/instrument problems line_13: unrelated to this observation. Could not be rescheduled. line_14: GO-4449 Occultation studies of RE1149+28: An object with line_15: an extreme EUV/optical ratio. (KOM,SRR). Scheduled for cycle 3 line_16: GO-4659 A time-resolved UV study of the wind outflow in the line_17: enigmatic cataclycmic variable, V795 Her. Supplemental time line_18: awarded but for only 2.3 hours. Obs not yet performed. line_19: The proposal GO-4659 was the initial request of this proposal line_20: but was awarded only 2.3 hrs of supplemental time. It will not line_21: by itself resolve the issues. No other programmes are related line_22: to this one. line_23: Papers: The Crab pulsar in the visible and UV with 10 micro- ! question: 9 section: 2 line_1: second time resolution: J.W. Percival, J.D. Biggs, J.F. line_2: Dolan, E.L. Robinson, et al, Ap.J., 407, 276, 1993. line_3: Several other GTO papers involving ELR have been submitted line_4: or are in preparation. ! question: 10 section: 1 line_1: The analysis of our HST data will be undertaken by the PI line_2: and the Co-I's. All proposers have access to DEC Vax line_3: 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: V795-HER descr_1: A, 151 pos_1: RA = 17H 12M 56.10S +/- 0.74", pos_2: DEC = +33D 31' 21.45" +/- 0.74", pos_3: PLATE-ID = 02TX equinox: J2000 comment_1: UV FLUXES ARE FROM IUE. S/N comment_2: ~10/PIXEL/BIN NEEDED PER comment_3: 20S EXPOSURE AT CIV CONTINUUM comment_4: CIV LINE VARIES BETWEEN comment_5: ABSORPTION AND EMISSION. fluxnum_1: 1 fluxval_1: B = 13.0 +/- 0.2 fluxnum_2: 2 fluxval_2: B-V = 0.6 +/- 0.1 fluxnum_3: 3 fluxval_3: E(B-V) = 0.1 +/- 0.1 fluxnum_4: 4 fluxval_4: F-CONT(1200) = 3.2 +/- 0.4 E-13 fluxnum_5: 5 fluxval_5: F-CONT(1550) = 2.8 +/- 0.3 E-13 fluxnum_6: 6 fluxval_6: F-LINE(1550) = 3.4 +/- 1.0 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: V795-HER config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 1S 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 / 1-27 comment_1: STAR VARIES BY ABOUT 0.2 MAGS comment_2: ABOUT ITS MEAN OF B=13.0. ! linenum: 1.500 targname: V795-HER config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: G130H num_exp: 1 time_per_exp: 1S 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 ! linenum: 1.700 targname: V795-HER config: FOS/BL opmode: ACQ/PEAK aperture: 0.5 sp_element: G130H num_exp: 1 time_per_exp: 1S fluxnum_1: 1 fluxnum_2: 3 priority: 1 param_1: SCAN-STEP-X=0.3, param_2: SCAN-STEP-Y=0.3, param_3: SEARCH-SIZE-X=3, param_4: SEARCH-SIZE-Y=3, req_1: ONBOARD ACQ FOR 2-7 ! linenum: 2.000 targname: V795-HER config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G130H wavelength: 1380 num_exp: 1 time_per_exp: 27M s_to_n: 10 s_to_n_time: 20S fluxnum_1: 5 priority: 1 param_1: COMB=YES param_2: READ-TIME=20 comment_1: USE 3 BLOCKS, EACH CONSISTING OF comment_2: ACQUISITION + 6 CONTIGUOUS HST comment_3: ORBITS. BLOCKS SHOULD IDEALLY BE comment_4: ABOUT 27 HST ORBITS APART. START comment_5: EPOCH OF 1ST BLOCK IS ARBITRARY. ! linenum: 3.000 targname: V795-HER config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G130H wavelength: 1380 num_exp: 1 time_per_exp: 27M s_to_n: 10 s_to_n_time: 20S fluxnum_1: 5 priority: 1 param_1: COMB=YES param_2: READ-TIME=20 ! linenum: 4.000 targname: V795-HER config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G130H wavelength: 1380 num_exp: 1 time_per_exp: 27M s_to_n: 10 s_to_n_time: 20S fluxnum_1: 5 priority: 1 param_1: COMB=YES param_2: READ-TIME=20 ! linenum: 5.000 targname: V795-HER config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G130H wavelength: 1380 num_exp: 1 time_per_exp: 27M s_to_n: 10 s_to_n_time: 20S fluxnum_1: 5 priority: 1 param_1: COMB=YES param_2: READ-TIME=20 ! linenum: 6.000 targname: V795-HER config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G130H wavelength: 1380 num_exp: 1 time_per_exp: 27M s_to_n: 10 s_to_n_time: 20S fluxnum_1: 5 priority: 1 param_1: COMB=YES param_2: READ-TIME=20 ! linenum: 7.000 targname: V795-HER config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G130H wavelength: 1380 num_exp: 1 time_per_exp: 27M s_to_n: 10 s_to_n_time: 20S fluxnum_1: 5 priority: 1 param_1: COMB=YES param_2: READ-TIME=20 ! linenum: 11.000 targname: V795-HER config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 1S 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 11.5; req_2: AFTER 1 BY 1.8D +/- .3D comment_1: STAR VARIES BY ABOUT 0.2 MAGS comment_2: ABOUT ITS MEAN OF B=13.0. ! linenum: 11.500 targname: V795-HER config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: G130H num_exp: 1 time_per_exp: 1S 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 11.7 ! linenum: 11.700 targname: V795-HER config: FOS/BL opmode: ACQ/PEAK aperture: 0.5 sp_element: G130H num_exp: 1 time_per_exp: 1S fluxnum_1: 1 fluxnum_2: 3 priority: 1 param_1: SCAN-STEP-X=0.3, param_2: SCAN-STEP-Y=0.3, param_3: SEARCH-SIZE-X=3, param_4: SEARCH-SIZE-Y=3, req_1: ONBOARD ACQ FOR 12-17 ! linenum: 12.000 targname: V795-HER config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G130H wavelength: 1380 num_exp: 1 time_per_exp: 27M s_to_n: 10 s_to_n_time: 20S fluxnum_1: 5 priority: 1 param_1: COMB=YES param_2: READ-TIME=20 comment_1: USE 3 BLOCKS, EACH CONSISTING OF comment_2: ACQUISITION + 6 CONTIGUOUS HST comment_3: ORBITS. BLOCKS SHOULD IDEALLY BE comment_4: ABOUT 27 HST ORBITS APART. START comment_5: EPOCH OF 1ST BLOCK IS ARBITRARY. ! linenum: 13.000 targname: V795-HER config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G130H wavelength: 1380 num_exp: 1 time_per_exp: 27M s_to_n: 10 s_to_n_time: 20S fluxnum_1: 5 priority: 1 param_1: COMB=YES param_2: READ-TIME=20 ! linenum: 14.000 targname: V795-HER config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G130H wavelength: 1380 num_exp: 1 time_per_exp: 27M s_to_n: 10 s_to_n_time: 20S fluxnum_1: 5 priority: 1 param_1: COMB=YES param_2: READ-TIME=20 ! linenum: 15.000 targname: V795-HER config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G130H wavelength: 1380 num_exp: 1 time_per_exp: 27M s_to_n: 10 s_to_n_time: 20S fluxnum_1: 5 priority: 1 param_1: COMB=YES param_2: READ-TIME=20 ! linenum: 16.000 targname: V795-HER config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G130H wavelength: 1380 num_exp: 1 time_per_exp: 27M s_to_n: 10 s_to_n_time: 20S fluxnum_1: 5 priority: 1 param_1: COMB=YES param_2: READ-TIME=20 ! linenum: 17.000 targname: V795-HER config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G130H wavelength: 1380 num_exp: 1 time_per_exp: 27M s_to_n: 10 s_to_n_time: 20S fluxnum_1: 5 priority: 1 param_1: COMB=YES param_2: READ-TIME=20 ! linenum: 21.000 targname: V795-HER config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: G130H num_exp: 1 time_per_exp: 1S 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 21.5; req_2: AFTER 1 BY 3.6D +/- .3D comment_1: STAR VARIES BY ABOUT 0.2 MAGS comment_2: ABOUT ITS MEAN OF B=13.0. ! linenum: 21.500 targname: V795-HER config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: G130H num_exp: 1 time_per_exp: 1S 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 21.7 ! linenum: 21.700 targname: V795-HER config: FOS/BL opmode: ACQ/PEAK aperture: 0.5 sp_element: G130H num_exp: 1 time_per_exp: 1S fluxnum_1: 1 fluxnum_2: 3 priority: 1 param_1: SCAN-STEP-X=0.3, param_2: SCAN-STEP-Y=0.3, param_3: SEARCH-SIZE-X=3, param_4: SEARCH-SIZE-Y=3, req_1: ONBOARD ACQ FOR 22-27 ! linenum: 22.000 targname: V795-HER config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G130H wavelength: 1380 num_exp: 1 time_per_exp: 27M s_to_n: 10 s_to_n_time: 20S fluxnum_1: 5 priority: 1 param_1: COMB=YES param_2: READ-TIME=20 comment_1: USE 3 BLOCKS, EACH CONSISTING OF comment_2: ACQUISITION + 6 CONTIGUOUS HST comment_3: ORBITS. BLOCKS SHOULD IDEALLY BE comment_4: ABOUT 27 HST ORBITS APART. START comment_5: EPOCH OF 1ST BLOCK IS ARBITRARY. ! linenum: 23.000 targname: V795-HER config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G130H wavelength: 1380 num_exp: 1 time_per_exp: 27M s_to_n: 10 s_to_n_time: 20S fluxnum_1: 5 priority: 1 param_1: COMB=YES param_2: READ-TIME=20 ! linenum: 24.000 targname: V795-HER config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G130H wavelength: 1380 num_exp: 1 time_per_exp: 27M s_to_n: 10 s_to_n_time: 20S fluxnum_1: 5 priority: 1 param_1: COMB=YES param_2: READ-TIME=20 ! linenum: 25.000 targname: V795-HER config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G130H wavelength: 1380 num_exp: 1 time_per_exp: 27M s_to_n: 10 s_to_n_time: 20S fluxnum_1: 5 priority: 1 param_1: COMB=YES param_2: READ-TIME=20 ! linenum: 26.000 targname: V795-HER config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G130H wavelength: 1380 num_exp: 1 time_per_exp: 27M s_to_n: 10 s_to_n_time: 20S fluxnum_1: 5 priority: 1 param_1: COMB=YES param_2: READ-TIME=20 ! linenum: 27.000 targname: V795-HER config: FOS/BL opmode: RAPID aperture: 1.0 sp_element: G130H wavelength: 1380 num_exp: 1 time_per_exp: 27M s_to_n: 10 s_to_n_time: 20S fluxnum_1: 5 priority: 1 param_1: COMB=YES param_2: READ-TIME=20 ! ! end of exposure logsheet ! No scan data records found