! File: 4447C.PROP ! Database: PEPDB ! Date: 22-FEB-1994:12:21:56 coverpage: title_1: DOPPLER IMAGING HR1099: DENSITY AND TEMPERATURE STRUCTURE title_2: OF A PROTOTYPE RS CVN SYSTEM CYC3-MEDIUM sci_cat: COOL STARS sci_subcat: ACTIVE STARS proposal_for: GO longterm: 1 cont_id: 4447 pi_title: DR. pi_fname: ROBERT pi_mi: C. pi_lname: DEMPSEY pi_inst: SPACE TELESCOPE SCIENCE INSTITUTE pi_country: USA pi_phone: (410) 338-1334 keywords_1: CHROMOSPHERIC ACTIVITY hours_pri: 6.53 num_pri: 1 hrs: Y funds_amount: 82532 funds_length: 24 funds_date: JUL-93 pi_position: ASTRONOMER off_fname: STEPHEN off_lname: LEONE off_title: CHAIRMAN off_inst: SPACE TELESCOPE SCIENCE INSTITUTE off_addr_1: 3700 SAN MARTIN DRIVE off_addr_2: ROOM 118 off_city: BALTIMORE off_state: MD off_zip: 21218 off_country: USA off_phone: (410) 338-1334 ! end of coverpage abstract: line_1: Although the Sun is a very slowly-rotating inactive star, images made in high line_2: temperature UV emission lines reveal bright plage regions located above dark line_3: sunspots. This indicates that magnetic fields control the local heating rate, line_4: density and energy balances even for a star with a weak field. Do line_5: rapidly-rotating active stars show the same pattern\? We will test this line_6: hypothesis by using the GHRS to Doppler image one of the brightest of the line_7: active RS CVn systems. Analysis of a sequence of ECH-B spectra obtained at 8 line_8: different orbital phases for the the HR 1099 (V711 Tau) system will yield line_9: images with about 30 resolution elements across the surface of the K1 IV star. line_10: A UNIQUE aspect of our program will be obtaining images in the CIII\] 1909A and line_11: SiIII\] 1892A intersystem lines to study the electron density and the amount of line_12: 30,000 to 60,000 K material in the plage transition regions. These will be the line_13: first Doppler images ever made with the following characteristics: (1) the line_14: lines are density-sensitive, (2) the lines are formed in the high-temperature line_15: plasma above the chromosphere, and (3) the images will have far higher spatial line_16: resolution than before due to the ECH-B spectral resolution of 43,000 (7 km/s). line_17: We will also obtain images in the Mg II h and k and C IV 1548, 1550A lines to line_18: study the size and location of plages in the chromosphere and transition line_19: region. Concurrent EUVE, GTO and ground-based optical studies will complete line_20: the picture of a solar-like star from the photosphere to the transition region. ! ! end of abstract general_form_proposers: lname: DEMPSEY fname: ROBERT title: DR. mi: C. inst: SPACE TELESCOPE SCIENCE INSTITUE country: USA ! lname: LINSKY fname: J. title: DR. mi: L. inst: JOINT INSTITUTE FOR LABORATORY ASTROPHYSICS country: USA ! lname: NEFF fname: JAMES title: DR. mi: E. inst: THE PENNSYLVANIA STATE UNIVERSITY country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: One target (HR 1099) will be observed for a total of 6.5 hours at 8 separate line_2: orbital-rotational phases. Since it is important to have high signal-to-noise, line_3: the observations have to be obtained very carefully. To avoid problems line_4: introduced by the fixed pattern noise in the D1 detector the spectra will be line_5: placed on the right hand half of the detector (diodes 300-500). In addition we line_6: require WSCAN mode where the spectra are shifted in small steps along the line_7: detector. Ideally, the eight observations should be equally spaced in phase line_8: with some overlap to distinguish transient from periodic variations. Since the line_9: phenomena we are studying change slowly, the observations should be line_10: constrained to within a couple of weeks after the first observation. GTO line_11: observations will be performed at phases 0.25 and 0.75. At these times only line_12: the high resolution C III] and Si III] observations need be obtained in line_13: addition to planned GTO observations (proposals 4873 & 4874). The six remaining line_14: observations will observe 4 regions as listed on the exposure log sheet. ! question: 4 section: 1 line_1: Currently, only IUE and HST provide UV observations in the spectral regions of line_2: interest. IUE does not have the sensitivity required to obtain high-dispersion line_3: spectra of the C III], Si III], and C IV lines. To obtain C III] spectra line_4: using IUE would require almost half of the 2.83 day rotation period of HR 1099, line_5: thereby entirely eliminating any spatial resolution. As with IUE, EUVE does line_6: not have the sensitivity for a rotational study of HR 1099. ! question: 5 section: 1 line_1: GTO observations (proposals 4873 & 4874) at TWO wavelengths will be performed at line_2: phases 0.25 and 0.75 during the period 93-Sep-29 to 93-Oct-8. This interval line_3: has been selected to allow cooridnation with EUVE, IUE, VLA and AT line_4: observations. This GO proposal requested two types of coordination: (1) line_5: observations at TWO wavelengths should be made at the SAME time as line_6: the above GTO observations at phases 0.25 and 0.75 and (2) observations at FOUR line_7: wavelengths made at 6 phases AS CLOSE TO THE GTO INTERVAL AS line_8: POSSIBLE. OBSERVATIONS SHOULD BE AS EVENLY DISTRIBUTED IN PHASE AND WITHIN AS line_9: FEW ROTATION CYCLES AS POSSIBLE (i.e. 3-20 DAYS). The ephemeris of HR 1099 is line_10: phase 0.00 at 2,442,766.080 + 2.83774E. Co-I Dempsey can work closely with line_11: the the STScI staff in planing these observations if required. line_12: IF POSSIBLE, THE LSA OBSERVATIONS SHOULD BE DONE FIRST, FOLLOWED BY line_13: A PEAKUP IN THE SSA AND THE G160 OBSERVATIONS. ! question: 6 section: 1 line_1: We require the best possible wavelength calibration to accurately determine the line_2: plage positions. This means that we need calibrations good to 0.1 diode or line_3: better. Experience with SV and SAO data (Carpenter et al. 1991, HST Workshop) line_4: has demonstrated that the default calibration will produce uncertainties of up line_5: to 3 diodes due to magnetic and thermal drifts within the spectrograph. Using line_6: internal Pt lamp spectra taken during the SPYBAL procedures, we can estimate line_7: the amount of drift and can therefore reduce the degree of uncertainty to line_8: about 0.5 diodes. To obtain the greatest possible wavelength accuracy, about line_9: 0.1 diodes, we require dedicated WAVECAL exposures using the internal Pt lamps line_10: to be connected to each GHRS science exposure. The wavelength calibrations line_11: must be taken at the same carrousel position and close in time to the science line_12: exposures to remove uncertainties caused by the Geomagnetic (GIMP) and thermal line_13: drifts which move the image around on the GHRS photocathode. ! question: 7 section: 1 line_1: All spectra will be analyzed using the software developed by the GHRS team. line_2: Computer codes developed for Doppler imaging the Mg II lines (Neff et al. 1989) line_3: will be applied to the UV observations. We will then compute models for the line_4: chromospheres and transition regions of the plages and background quiescent line_5: regions separately using the line surface fluxes derived from the plage areas. line_6: The latter are derived in the Doppler imaging technique from the time of plage line_7: appearance and disappearance, and the width of the spectral lines for each line_8: plage, which is due in part to differential rotational velocities of the line_9: edges of the plage nearest and furthest from the observer. ! question: 8 section: 1 line_1: Observations will be coordinated with EUVE. If the target is above the line_2: horizon at the appropriate time when observed with HST we will obtain line_3: VLA and groundbased optical observations. DI can be applied to the line_4: optical data to provide simultaneous spot distributions which will then line_5: be directly compared to the UV images. ! question: 9 section: 1 line_1: GTO program 1175 (and 3943) - Local Interstellar Medium and D/H Ratio (J. line_2: Linsky PI). GTO Program 1176 (and 3964) - The dynamics of stellar line_3: chromospheres and transition regions (J. Linsky PI) GTO Program 1177 - line_4: Atmospheres of very inactive K giant stars (J. Linsky PI) GTO Program 1179 (and line_5: 3961) - Hybrid-chromosphere stars (J. Linsky PI) GTO Program 1180 - The line_6: chromospheres of the very coolest M dwarf stars (J. Linsky PI) GTO Program line_7: 1195 - Alpha Orionis (K. Carpenter PI, J. Linsky et al.) GTO Program 1199 - line_8: Alpha Orionis Team Project (K. Carpenter PI, J. Linsky et al.) GTO Program 1210 line_9: - Age dependence of non-radiative heating in stellar chromospheres (F. Walter line_11: PI, J. Linsky) GO program 2238 - Lyman-ALPHA Observations Of High Radial line_12: Velocity Stars (Jay Bookbinder PI, A.Brown, P.Judge, W.Landsman, J.Linsky, J. line_13: Neff) GO Program 2321 - Search for proton acceleration in flare stars - AU Mic line_14: (B. Woodgate PI, J. Linsky, M. Kundu, K. Carpenter, R. Robinson, S. Maran) GO line_15: Program 3626 - Empirical determination of the wind velocity and density laws line_16: for the K supergiant Zeta Aurigae from eclipse ingress spectra (A. Brown PI, line_17: J. Linsky, R. Weyman, D. Reimers, R. Baade, T. Kirsch) GO Programs with J. E. line_18: Neff as a Co-I include: GO P2238: Lyman-Alpha Observations of High Radial line_19: Velocity Stars. ! question: 10 section: 1 line_1: The Joint Institute for Laboratory Astrophysics, line_2: Space Telescope Science Institute, and The Pennsylvania State line_3: University will both provide SUN SPARCstations with IRAF, SDAS, AIPS line_4: and IDL software sufficient to reduce and analyze the data. ! !end of general form text general_form_address: lname: DEMPSEY fname: ROBERT mi: C. title: DR. category: PI inst: SPACE TELESCOPE SCIENCE INSTITUE addr_1: 3700 SAN MARTIN DRIVE addr_2: ROOM 118 city: BALTIMORE state: MD zip: 21218 country: USA phone: (410)338-1334 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: HD22468 name_2: HR1099 name_3: V711TAU descr_1: A,167 pos_1: RA=03H34M13.169S +/- 0.01S, pos_2: DEC=+00D25'33.17" +/- 0.1" equinox: 1950 pm_or_par: Y pos_epoch_bj: B pos_epoch_yr: 1950.00 ra_pm_val: -0.002000 ra_pm_unct: 0.000067 dec_pm_val: -0.1610 dec_pm_unct: 0.0010 an_prlx_val: 0.0320 rv_or_z: V=-15 fluxnum_1: 1 fluxval_1: V=5.71 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.010 targname: HD22468 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 2.7S fluxnum_1: 1 priority: 1 param_1: BRIGHT=RETURN req_1: CYCLE 3; req_2: AT 15-SEP-1993 +/- 7.5D; req_3: SEQ 1.010-1.450 NO GAP; req_4: ONBOARD ACQ FOR 1.015; comment_1: IDEALLY OBSERVATIONS SHOULD comment_2: BE IN AS SHORT AN INTERVAL comment_3: AS POSSIBLE (E.G. 3-4 DAYS). comment_4: STEP-TIME=0.3S ! linenum: 1.015 targname: HD22468 config: HRS opmode: ACQ/PEAKUP aperture: 0.25 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 40S fluxnum_1: 1 priority: 1 req_1: CYCLE 3; req_4: ONBOARD ACQ FOR 1.1-1.45; comment_1: JUST PRIOR TO 0.25 OBSERVATIONS comment_2: WHICH SHOULD BE AFTER THE 2.0 comment_3: OBSERVATIONS comment_4: STEP-TIME=1.6S ! linenum: 1.100 targname: HD22468 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1549 num_exp: 1 time_per_exp: 10M s_to_n: 50 fluxnum_1: 1 priority: 4 param_1: STEP-PATT=5 param_2: FP-SPLIT=STD req_1: CYCLE 3; req_2: ZERO-PHASE JD2442766.080 +/- 0.005D; req_3: PERIOD 2.83774D +/- 0.00005D; req_4: PHASE 0.00 +/- 0.05; ! linenum: 1.150 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1549 num_exp: 1 time_per_exp: 108.8S s_to_n: 100 priority: 4 param_1: STEP-PATT=3 req_1: CYCLE 3; req_3: SEQ 1.100-1.150; req_4: CALIB FOR 1.100 NO SLEW; comment_1: MUST BE FREE OF STELLAR COUNTS comment_2: IF AT POSSIBLE ! linenum: 1.200 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B wavelength: 2800 num_exp: 1 time_per_exp: 108.8S s_to_n: 200 priority: 1 param_1: STEP-PATT=3 req_1: CYCLE 3; req_2: SEQ 1.200-1.250; req_3: CALIB FOR 1.250 NO SLEW; ! linenum: 1.250 targname: HD22468 config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B wavelength: 2800 num_exp: 1 time_per_exp: 108.8S s_to_n: 100 fluxnum_1: 1 priority: 1 param_1: STEP-PATT=7 param_2: FP-SPLIT=STD req_1: CYCLE 3; comment_1: SIGNAL-TO-NOISE SHOULD BE BETTER comment_2: THAN 100, PREFER 150 ! linenum: 1.300 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B wavelength: 1909 num_exp: 1 time_per_exp: 108.8S s_to_n: 100 priority: 2 param_1: STEP-PATT=3 req_1: CYCLE 3; req_2: SEQ 1.300-1.350; req_3: CALIB FOR 1.350 NO SLEW; ! linenum: 1.350 targname: HD22468 config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B wavelength: 1909 num_exp: 1 time_per_exp: 20M s_to_n: 30 fluxnum_1: 1 priority: 2 param_1: STEP-PATT=7 param_2: FP-SPLIT=STD req_1: CYCLE 3; ! linenum: 1.400 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B wavelength: 1892 num_exp: 1 time_per_exp: 108.8S s_to_n: 100 priority: 3 param_1: STEP-PATT=3 req_1: CYCLE 3; req_2: SEQ 1.400-1.450; req_3: CALIB FOR 1.450 NO SLEW; ! linenum: 1.450 targname: HD22468 config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B wavelength: 1892 num_exp: 1 time_per_exp: 20M s_to_n: 30 fluxnum_1: 1 priority: 3 param_1: STEP-PATT=7 param_2: FP-SPLIT=STD req_1: CYCLE 3; ! linenum: 2.010 targname: HD22468 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 2.7S fluxnum_1: 1 priority: 1 param_1: BRIGHT=RETURN req_1: CYCLE 3; req_2: AT 15-SEP-1993 +/- 7.5D; req_3: SEQ 2.010-2.450 NO GAP; req_4: ONBOARD ACQ FOR 2.015; comment_1: IDEALLY OBSERVATIONS SHOULD comment_2: BE IN AS SHORT AN INTERVAL comment_3: AS POSSIBLE (E.G. 3-4 DAYS). comment_4: STEP-TIME=0.3S ! linenum: 2.015 targname: HD22468 config: HRS opmode: ACQ/PEAKUP aperture: 0.25 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 40S fluxnum_1: 1 priority: 1 req_1: CYCLE 3; req_4: ONBOARD ACQ FOR 2.1-2.45; comment_1: JUST PRIOR TO 0.25 OBSERVATIONS comment_2: WHICH SHOULD BE AFTER THE 2.0 comment_3: OBSERVATIONS comment_4: STEP-TIME=1.6S ! linenum: 2.100 targname: HD22468 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1549 num_exp: 1 time_per_exp: 10M s_to_n: 50 fluxnum_1: 1 priority: 4 param_1: STEP-PATT=5 param_2: FP-SPLIT=STD req_1: CYCLE 3; req_2: PHASE 0.125 +/- 0.05 OF REF 1.10; ! linenum: 2.150 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1549 num_exp: 1 time_per_exp: 108.8S s_to_n: 100 priority: 4 param_1: STEP-PATT=3 req_1: CYCLE 3; req_2: SEQ 2.100-2.150; req_3: CALIB FOR 2.100 NO SLEW; comment_1: MUST BE FREE OF STELLAR COUNTS comment_2: IF AT POSSIBLE ! linenum: 2.200 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B wavelength: 2800 num_exp: 1 time_per_exp: 108.8S s_to_n: 200 priority: 1 param_1: STEP-PATT=3 req_1: CYCLE 3; req_2: SEQ 2.200-2.250; req_3: CALIB FOR 2.250 NO SLEW; ! linenum: 2.250 targname: HD22468 config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B wavelength: 2800 num_exp: 1 time_per_exp: 108.8S s_to_n: 100 fluxnum_1: 1 priority: 1 param_1: STEP-PATT=7 param_2: FP-SPLIT=STD req_1: CYCLE 3; comment_1: SIGNAL-TO-NOISE SHOULD BE BETTER comment_2: THAN 100, PREFER 150 ! linenum: 2.300 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B wavelength: 1909 num_exp: 1 time_per_exp: 108.8S s_to_n: 100 priority: 2 param_1: STEP-PATT=3 req_1: CYCLE 3; req_2: SEQ 2.300-2.350; req_3: CALIB FOR 2.350 NO SLEW; ! linenum: 2.350 targname: HD22468 config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B wavelength: 1909 num_exp: 1 time_per_exp: 20M s_to_n: 30 fluxnum_1: 1 priority: 2 param_1: STEP-PATT=7 param_2: FP-SPLIT=STD req_1: CYCLE 3; ! linenum: 2.400 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B wavelength: 1892 num_exp: 1 time_per_exp: 108.8S s_to_n: 100 priority: 3 param_1: STEP-PATT=3 req_1: CYCLE 3; req_2: SEQ 2.400-2.450; req_3: CALIB FOR 2.450 NO SLEW; ! linenum: 2.450 targname: HD22468 config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B wavelength: 1892 num_exp: 1 time_per_exp: 20M s_to_n: 30 fluxnum_1: 1 priority: 3 param_1: STEP-PATT=7 param_2: FP-SPLIT=STD req_1: CYCLE 3; ! linenum: 3.010 targname: HD22468 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 2.7S fluxnum_1: 1 priority: 1 param_1: BRIGHT=RETURN req_1: CYCLE 3; req_2: AT 15-SEP-1993 +/- 7.5D; req_3: SEQ 3.010-3.250 NO GAP; req_4: ONBOARD ACQ FOR 3.10-3.25; comment_1: SHOULD BE COORDINATED WITH GTO PROPS comment_2: 4873 & 4874 IF POSSIBLE comment_3: STEP-TIME=0.3S ! linenum: 3.100 targname: HD22468 config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B wavelength: 1909 num_exp: 1 time_per_exp: 20M s_to_n: 30 fluxnum_1: 1 priority: 1 param_1: STEP-PATT=7 param_2: FP-SPLIT=STD req_1: CYCLE 3; req_2: PHASE 0.25 +/- 0.05 OF REF 1.10; comment_1: SHOULD BE COORDINATED WITH GTO PROPS comment_2: 4873 & 4874 IF AT ALL POSSIBLE ! linenum: 3.150 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B wavelength: 1909 num_exp: 1 time_per_exp: 108.8S s_to_n: 100 priority: 1 param_1: STEP-PATT=3 req_1: CYCLE 3; req_2: SEQ 3.100-3.150; req_3: CALIB FOR 3.100 NO SLEW; ! linenum: 3.200 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B wavelength: 1892 num_exp: 1 time_per_exp: 108.8S s_to_n: 100 priority: 2 param_1: STEP-PATT=3 req_1: CYCLE 3; req_2: SEQ 3.200-3.250; req_3: CALIB FOR 3.250 NO SLEW; ! linenum: 3.250 targname: HD22468 config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B wavelength: 1892 num_exp: 1 time_per_exp: 20M s_to_n: 30 fluxnum_1: 1 priority: 2 param_1: STEP-PATT=7 param_2: FP-SPLIT=STD req_1: CYCLE 3; comment_1: SHOULD BE COORDINATED WITH GTO PROPS comment_2: 4873 & 4874 IF AT ALL POSSIBLE ! linenum: 4.010 targname: HD22468 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 2.7S fluxnum_1: 1 priority: 1 param_1: BRIGHT=RETURN req_1: CYCLE 3; req_2: AT 15-SEP-1993 +/- 7.5D; req_3: SEQ 4.010-4.450 NO GAP; req_4: ONBOARD ACQ FOR 4.015; comment_1: IDEALLY OBSERVATIONS SHOULD comment_2: BE IN AS SHORT AN INTERVAL comment_3: AS POSSIBLE (E.G. 3-4 DAYS). comment_4: STEP-TIME=1.6S ! linenum: 4.015 targname: HD22468 config: HRS opmode: ACQ/PEAKUP aperture: 0.25 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 40S fluxnum_1: 1 priority: 1 req_1: CYCLE 3; req_4: ONBOARD ACQ FOR 4.1-4.45; comment_1: JUST PRIOR TO 0.25 OBSERVATIONS comment_2: WHICH SHOULD BE AFTER THE 2.0 comment_3: OBSERVATIONS comment_4: STEP-TIME=1.6S ! linenum: 4.100 targname: HD22468 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1549 num_exp: 1 time_per_exp: 10M s_to_n: 50 fluxnum_1: 1 priority: 4 param_1: STEP-PATT=5 param_2: FP-SPLIT=STD req_1: CYCLE 3; req_2: PHASE 0.375+/- 0.05 OF REF 1.10; ! linenum: 4.150 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1549 num_exp: 1 time_per_exp: 108.8S s_to_n: 100 priority: 4 param_1: STEP-PATT=3 req_1: CYCLE 3; req_2: SEQ 4.100-4.150; req_3: CALIB FOR 4.100 NO SLEW; comment_1: MUST BE FREE OF STELLAR COUNTS comment_2: IF AT POSSIBLE ! linenum: 4.200 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B wavelength: 2800 num_exp: 1 time_per_exp: 108.8S s_to_n: 200 priority: 1 param_1: STEP-PATT=3 req_1: CYCLE 3; req_2: SEQ 4.200-4.250; req_3: CALIB FOR 4.250 NO SLEW; ! linenum: 4.250 targname: HD22468 config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B wavelength: 2800 num_exp: 1 time_per_exp: 108.8S s_to_n: 100 fluxnum_1: 1 priority: 1 param_1: STEP-PATT=7 param_2: FP-SPLIT=STD req_1: CYCLE 3; comment_1: SIGNAL-TO-NOISE SHOULD BE BETTER comment_2: THAN 100, PREFER 150 ! linenum: 4.300 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B wavelength: 1909 num_exp: 1 time_per_exp: 108.8S s_to_n: 100 priority: 2 param_1: STEP-PATT=3 req_1: CYCLE 3; req_2: SEQ 4.300-4.350; req_3: CALIB FOR 4.350 NO SLEW; ! linenum: 4.350 targname: HD22468 config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B wavelength: 1909 num_exp: 1 time_per_exp: 20M s_to_n: 30 fluxnum_1: 1 priority: 2 param_1: STEP-PATT=7 param_2: FP-SPLIT=STD req_1: CYCLE 3; ! linenum: 4.400 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B wavelength: 1892 num_exp: 1 time_per_exp: 108.8S s_to_n: 100 priority: 3 param_1: STEP-PATT=3 req_1: CYCLE 3; req_2: SEQ 4.400-4.450; req_3: CALIB FOR 4.450 NO SLEW; ! linenum: 4.450 targname: HD22468 config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B wavelength: 1892 num_exp: 1 time_per_exp: 20M s_to_n: 30 fluxnum_1: 1 priority: 3 param_1: STEP-PATT=7 param_2: FP-SPLIT=STD req_1: CYCLE 3; ! linenum: 5.010 targname: HD22468 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 2.7S fluxnum_1: 1 priority: 1 param_1: BRIGHT=RETURN req_1: CYCLE 3; req_2: AT 15-SEP-1993 +/- 7.5D; req_3: SEQ 5.010-5.450 NO GAP; req_4: ONBOARD ACQ FOR 5.015; comment_1: IDEALLY OBSERVATIONS SHOULD comment_2: BE IN AS SHORT AN INTERVAL comment_3: AS POSSIBLE (E.G. 3-4 DAYS). comment_4: STEP-TIME=0.3S ! linenum: 5.015 targname: HD22468 config: HRS opmode: ACQ/PEAKUP aperture: 0.25 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 40S fluxnum_1: 1 priority: 1 req_1: CYCLE 3; req_4: ONBOARD ACQ FOR 5.1-5.45; comment_1: JUST PRIOR TO 0.25 OBSERVATIONS comment_2: WHICH SHOULD BE AFTER THE 2.0 comment_3: OBSERVATIONS comment_4: STEP-TIME=1.6S ! linenum: 5.100 targname: HD22468 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1549 num_exp: 1 time_per_exp: 10M s_to_n: 50 fluxnum_1: 1 priority: 4 param_1: STEP-PATT=5 param_2: FP-SPLIT=STD req_1: CYCLE 3; req_2: PHASE 0.50 +/- 0.05 OF REF 1.10; ! linenum: 5.150 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1549 num_exp: 1 time_per_exp: 108.8S s_to_n: 100 priority: 4 param_1: STEP-PATT=3 req_1: CYCLE 3; req_2: SEQ 5.100-5.150; req_3: CALIB FOR 5.100 NO SLEW; comment_1: MUST BE FREE OF STELLAR COUNTS comment_2: IF AT POSSIBLE ! linenum: 5.200 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B wavelength: 2800 num_exp: 1 time_per_exp: 108.8S s_to_n: 200 priority: 1 param_1: STEP-PATT=3 req_1: CYCLE 3; req_2: SEQ 5.200-5.250; req_3: CALIB FOR 5.250 NO SLEW; ! linenum: 5.250 targname: HD22468 config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B wavelength: 2800 num_exp: 1 time_per_exp: 108.8S s_to_n: 100 fluxnum_1: 1 priority: 1 param_1: STEP-PATT=7 param_2: FP-SPLIT=STD req_1: CYCLE 3; comment_1: SIGNAL-TO-NOISE SHOULD BE BETTER comment_2: THAN 100, PREFER 150 ! linenum: 5.300 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B wavelength: 1909 num_exp: 1 time_per_exp: 108.8S s_to_n: 100 priority: 2 param_1: STEP-PATT=3 req_1: CYCLE 3; req_2: SEQ 5.300-5.350; req_3: CALIB FOR 5.350 NO SLEW; ! linenum: 5.350 targname: HD22468 config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B wavelength: 1909 num_exp: 1 time_per_exp: 20M s_to_n: 30 fluxnum_1: 1 priority: 2 param_1: STEP-PATT=7 param_2: FP-SPLIT=STD req_1: CYCLE 3; ! linenum: 5.400 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B wavelength: 1892 num_exp: 1 time_per_exp: 108.8S s_to_n: 100 priority: 3 param_1: STEP-PATT=3 req_1: CYCLE 3; req_2: SEQ 5.400-5.450; req_3: CALIB FOR 5.450 NO SLEW; ! linenum: 5.450 targname: HD22468 config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B wavelength: 1892 num_exp: 1 time_per_exp: 20M s_to_n: 30 fluxnum_1: 1 priority: 3 param_1: STEP-PATT=7 param_2: FP-SPLIT=STD req_1: CYCLE 3; ! linenum: 6.010 targname: HD22468 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 2.7S fluxnum_1: 1 priority: 1 param_1: BRIGHT=RETURN req_1: CYCLE 3; req_2: AT 15-SEP-1993 +/- 7.5D; req_3: SEQ 6.010-6.450 NO GAP; req_4: ONBOARD ACQ FOR 6.015; comment_1: IDEALLY OBSERVATIONS SHOULD comment_2: BE IN AS SHORT AN INTERVAL comment_3: AS POSSIBLE (E.G. 3-4 DAYS). comment_4: STEP-TIME=0.3S ! linenum: 6.015 targname: HD22468 config: HRS opmode: ACQ/PEAKUP aperture: 0.25 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 40S fluxnum_1: 1 priority: 1 req_1: CYCLE 3; req_4: ONBOARD ACQ FOR 6.1-6.45; comment_1: JUST PRIOR TO 0.25 OBSERVATIONS comment_2: WHICH SHOULD BE AFTER THE 2.0 comment_3: OBSERVATIONS comment_4: STEP-TIME=1.6S ! linenum: 6.100 targname: HD22468 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1549 num_exp: 1 time_per_exp: 10M s_to_n: 50 fluxnum_1: 1 priority: 4 param_1: STEP-PATT=5 param_2: FP-SPLIT=STD req_1: CYCLE 3; req_2: PHASE 0.625 +/- 0.05OF REF 1.10; ! linenum: 6.150 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1549 num_exp: 1 time_per_exp: 108.8S s_to_n: 100 priority: 4 param_1: STEP-PATT=3 req_1: CYCLE 3; req_2: SEQ 6.100-6.150; req_3: CALIB FOR 6.100 NO SLEW; comment_1: MUST BE FREE OF STELLAR COUNTS comment_2: IF AT POSSIBLE ! linenum: 6.200 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B wavelength: 2800 num_exp: 1 time_per_exp: 108.8S s_to_n: 200 priority: 1 param_1: STEP-PATT=3 req_1: CYCLE 3; req_2: SEQ 6.200-6.250; req_3: CALIB FOR 6.250 NO SLEW; ! linenum: 6.250 targname: HD22468 config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B wavelength: 2800 num_exp: 1 time_per_exp: 108.8S s_to_n: 100 fluxnum_1: 1 priority: 1 param_1: STEP-PATT=7 param_2: FP-SPLIT=STD req_1: CYCLE 3; comment_1: SIGNAL-TO-NOISE SHOULD BE BETTER comment_2: THAN 100, PREFER 150 ! linenum: 6.300 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B wavelength: 1909 num_exp: 1 time_per_exp: 108.8S s_to_n: 100 priority: 2 param_1: STEP-PATT=3 req_1: CYCLE 3; req_2: SEQ 6.300-6.350; req_3: CALIB FOR 6.350 NO SLEW; ! linenum: 6.350 targname: HD22468 config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B wavelength: 1909 num_exp: 1 time_per_exp: 20M s_to_n: 30 fluxnum_1: 1 priority: 2 param_1: STEP-PATT=7 param_2: FP-SPLIT=STD req_1: CYCLE 3; ! linenum: 6.400 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B wavelength: 1892 num_exp: 1 time_per_exp: 108.8S s_to_n: 100 priority: 3 param_1: STEP-PATT=3 req_1: CYCLE 3; req_2: SEQ 6.400-6.450; req_3: CALIB FOR 6.450 NO SLEW; ! linenum: 6.450 targname: HD22468 config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B wavelength: 1892 num_exp: 1 time_per_exp: 20M s_to_n: 30 fluxnum_1: 1 priority: 3 param_1: STEP-PATT=7 param_2: FP-SPLIT=STD req_1: CYCLE 3; ! linenum: 7.010 targname: HD22468 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 2.7S fluxnum_1: 1 priority: 1 param_1: BRIGHT=RETURN req_1: CYCLE 3; req_2: AT 15-SEP-1993 +/- 7.5D; req_3: SEQ 7.010-7.250 NO GAP; req_4: ONBOARD ACQ FOR 7.10-7.25; comment_1: SHOULD BE COORDINATED WITH GTO PROPS comment_2: 4873 & 4874 IF AT ALL POSSIBLE comment_3: STEP-TIME=0.3S ! linenum: 7.100 targname: HD22468 config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B wavelength: 1909 num_exp: 1 time_per_exp: 20M s_to_n: 30 fluxnum_1: 1 priority: 2 param_1: STEP-PATT=7 param_2: FP-SPLIT=STD req_1: CYCLE 3; req_2: PHASE 0.75 +/- 0.05 OF REF 1.10; comment_1: SHOULD BE COORDINATED WITH GTO PROPS comment_2: 4873 & 4874 IF AT ALL POSSIBLE ! linenum: 7.150 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B wavelength: 1909 num_exp: 1 time_per_exp: 108.8S s_to_n: 100 priority: 2 param_1: STEP-PATT=3 req_1: CYCLE 3; req_2: SEQ 7.100-7.150; req_3: CALIB FOR 7.100 NO SLEW; ! linenum: 7.200 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B wavelength: 1892 num_exp: 1 time_per_exp: 108.8S s_to_n: 100 priority: 3 param_1: STEP-PATT=3 req_1: CYCLE 3; req_2: SEQ 7.200-7.250; req_3: CALIB FOR 7.250 NO SLEW; ! linenum: 7.250 targname: HD22468 config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B wavelength: 1892 num_exp: 1 time_per_exp: 20M s_to_n: 30 fluxnum_1: 1 priority: 3 param_1: STEP-PATT=7 param_2: FP-SPLIT=STD req_1: CYCLE 3; comment_1: SHOULD BE COORDINATED WITH GTO PROPS comment_2: 4873 & 4874 IF AT ALL POSSIBLE ! linenum: 8.010 targname: HD22468 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 2.7S fluxnum_1: 1 priority: 1 param_1: BRIGHT=RETURN req_1: CYCLE 3; req_2: AT 15-SEP-1993 +/- 7.5D; req_3: SEQ 8.010-8.450 NO GAP; req_4: ONBOARD ACQ FOR 8.015; comment_1: IDEALLY OBSERVATIONS SHOULD comment_2: BE IN AS SHORT AN INTERVAL comment_3: AS POSSIBLE (E.G. 3-4 DAYS). comment_4: STEP-TIME=0.3S ! linenum: 8.015 targname: HD22468 config: HRS opmode: ACQ/PEAKUP aperture: 0.25 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 40S fluxnum_1: 1 priority: 1 req_1: CYCLE 3; req_4: ONBOARD ACQ FOR 8.1-8.45; comment_1: JUST PRIOR TO 0.25 OBSERVATIONS comment_2: WHICH SHOULD BE AFTER THE 2.0 comment_3: OBSERVATIONS comment_4: STEP-TIME=1.6S ! linenum: 8.100 targname: HD22468 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1549 num_exp: 1 time_per_exp: 10M s_to_n: 50 fluxnum_1: 1 priority: 4 param_1: STEP-PATT=5 param_2: FP-SPLIT=STD req_1: CYCLE 3; req_2: PHASE 0.875 +/- 0.05 OF REF 1.10; ! linenum: 8.150 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1549 num_exp: 1 time_per_exp: 108.8S s_to_n: 100 priority: 4 param_1: STEP-PATT=3 req_1: CYCLE 3; req_2: SEQ 8.100-8.150; req_3: CALIB FOR 8.100 NO SLEW; comment_1: MUST BE FREE OF STELLAR COUNTS comment_2: IF AT POSSIBLE ! linenum: 8.200 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B wavelength: 2800 num_exp: 1 time_per_exp: 108.8S s_to_n: 200 priority: 1 param_1: STEP-PATT=3 req_1: CYCLE 3; req_2: SEQ 8.200-8.250; req_3: CALIB FOR 8.250 NO SLEW; ! linenum: 8.250 targname: HD22468 config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B wavelength: 2800 num_exp: 1 time_per_exp: 108.8S s_to_n: 100 fluxnum_1: 1 priority: 1 param_1: STEP-PATT=7 param_2: FP-SPLIT=STD req_1: CYCLE 3; comment_1: SIGNAL-TO-NOISE SHOULD BE BETTER comment_2: THAN 100, PREFER 150 ! linenum: 8.300 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B wavelength: 1909 num_exp: 1 time_per_exp: 108.8S s_to_n: 100 priority: 2 param_1: STEP-PATT=3 req_1: CYCLE 3; req_2: SEQ 8.300-8.350; req_3: CALIB FOR 8.350 NO SLEW; ! linenum: 8.350 targname: HD22468 config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B wavelength: 1909 num_exp: 1 time_per_exp: 20M s_to_n: 30 fluxnum_1: 1 priority: 2 param_1: STEP-PATT=7 param_2: FP-SPLIT=STD req_1: CYCLE 3; ! linenum: 8.400 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B wavelength: 1892 num_exp: 1 time_per_exp: 108.8S s_to_n: 100 priority: 3 param_1: STEP-PATT=3 req_1: CYCLE 3; req_2: SEQ 8.400-8.450; req_3: CALIB FOR 8.450 NO SLEW; ! linenum: 8.450 targname: HD22468 config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B wavelength: 1892 num_exp: 1 time_per_exp: 20M s_to_n: 30 fluxnum_1: 1 priority: 3 param_1: STEP-PATT=7 param_2: FP-SPLIT=STD req_1: CYCLE 3; ! ! end of exposure logsheet ! No scan data records found