! File: 3626C.PROP ! Database: PEPDB ! Date: 19-FEB-1994:14:19:37 coverpage: title_1: EMPIRICAL DETERMINATION OF THE WIND VELOCITY AND DENSITY LAWS title_2: FOR THE K SUPERGIANT ZETA AURIGAE sci_cat: STELLAR ASTROPHYSICS sci_subcat: STELLAR ATMOSPHERES proposal_for: GO cont_id: 3626 pi_title: DR. pi_fname: ALEXANDER pi_lname: BROWN pi_inst: COLORADO, UNIVERSITY OF pi_country: USA pi_phone: (303) 492-7810 keywords_1: K4IB+B8 ECLIPSING BINARY SYSTEM hours_pri: 13.00 num_pri: 1 hrs: Y time_crit: Y funds_amount: 130510 funds_length: 24 funds_date: JUL-92 pi_position: SENIOR RES ASSOCIATE off_fname: LAURENCE off_mi: D. off_lname: NELSON off_title: DIRECTOR off_inst: UNIVERSITY OF COLORADO off_addr_1: OFFICE OF CONTRACTS AND GRANTS off_addr_2: CAMPUS BOX 19 off_city: BOULDER off_state: CO off_zip: 803090019 off_country: USA off_phone: (303) 492-2695 ! end of coverpage abstract: line_1: We will derive the velocity and density laws and mass loss rate for the line_2: K4 supergiant in the eclipsing Zeta Aurigae binary system. The slow line_3: passage of the geometrically small B dwarf with its bright UV continuum line_4: behind the extended atmosphere of the K supergiant provides a splendid line_5: opportunity to probe the column densities and velocities of many line_6: absorption lines of various strengths as a function of stellar impact line_7: parameter. Our empirical determination of the wind physical parameters line_8: throughout the acceleration region will place tight constraints on the line_9: physical processes responsible for mass loss in evolved, massive stars line_10: that contribute significantly to the enrichment of the interstellar line_11: medium with chemically processed material. We request time for line_12: observations of lines of Fe I-II, Si II, Ti II, and V II at 6 orbital line_13: phases, including the terminal velocity wind, wind aceleration line_14: region, eclipse by the K star chromosphere, and total eclipse. This line_15: program is time critical but with typical tolerances of 1-7 days due line_16: to the long (972 day) orbital period. ! ! end of abstract general_form_proposers: lname: BROWN fname: ALEXANDER title: PI inst: COLORADO, UNIVERSITY OF country: USA ! lname: LINSKY fname: JEFFREY mi: L. inst: COLORADO, UNIVERSITY OF country: USA ! lname: WEYMAN fname: RAY inst: MT. WILSON AND LAS CAMPANAS OBSERVATORIES country: USA ! lname: REIMERS fname: DIETER inst: HAMBURG, UNIVERSITY OF country: GERMANY esa: Y ! lname: BAADE fname: ROBERT inst: HAMBURG, UNIVERSITY OF country: GERMANY esa: Y ! lname: KIRSCH fname: THOMAS inst: HAMBURG, UNIVERSITY OF country: GERMANY esa: Y ! ! end of general_form_proposers block general_form_text: question: 2 section: 1 line_1: _______________________________________________________________________ line_2: Ion UV Mult Mode Lambda(A) Epochs Phase line_3: ______________________________________________________________________ line_4: Si II 5 G160M 1194.5,1197.4 1,6 wind, totality line_5: Fe II 9 G160M 1253.8,1266.7,1277.6 1,2,3,6 wind,w.acc.,tot. line_6: (+S II 1 1253.8 ) line_7: Si II 2 G160M 1526.7,1533.4 1,6 wind, totality line_8: Fe II 44,45 G160M 1563.8,1580.6,1588.3 2,3 wind acc. line_9: Fe II 8 G160M 1629.2,1631.1 2,3 wind acc. line_10: (+Fe II 43 1640.2 ) line_11: Fe II 39 ECH-B 1704.6 2,3,4,5 w. acc., chrom. line_12: Fe II 191 ECH-B 1785.3,1786.8,1788.0 6 totality line_13: Fe II 6 ECH-B 2146.1,2153.9 4,5 chrom. line_14: Fe II 3 ECH-B 2332.8,2338.0 1,2,3,6 wind,w.acc.,tot. line_15: Fe II 1 ECH-B 2607.1,2613.8 1,6 wind, totality line_16: Fe I 9 ECH-B 3001.0,3008.1 4,5 chrom. line_17: Fe I 9 ECH-B 3047.6 4,5 chrom. line_18: Ti II 5 ECH-B 3072.1,3073.0 2,3,4,5 w. acc., chrom. line_19: 3075.2,3078.7 line_20: V II 1 ECH-B 3126.2,3133.3 4,5 chrom. line_21: _____________________________________________________________________ ! question: 3 section: 1 line_1: The exposures requested are summarized above. The exposure times line_2: have been estimated using absolute fluxes previously measured with the line_3: IUE. The echelle exposure times were estimated from pre-launch line_4: calibrations and increased by a factor of 1.4 to account for reduced line_5: throughput of the large science aperture (LSA). The effect of the line_6: echelle ripple was included. The LSA allows high signal-to-noise spectra line_7: to be obtained in much shorter exposures than with the SSA. The line_8: resulting observed resolution will be 43,500 (7.5 km/s), line_9: but spectral deconvolution using the observed point-spread function line_10: should allow spectra with a resolution of at least 60,000 (5.0 km/s) line_11: to be retrieved without loss of spectral fidelity. Medium resolution line_12: grating (G160M) spectra will be obtained below 1700A using the small line_13: science aperture (SSA) to reach the orignal design resolution (17,000- line_14: 22,000) for this mode. IN-orbit sensitivities and aperture throughputs line_15: were used to estimate exposure times for G160M. The choosen lines will line_16: provide optimum modelling information for each particular line_17: phase of the eclipse. The list of lines to be observed has been line_18: reduced as requested by the TAC; HOWEVER, it was not possible to retain line_19: the 8 phases originally proposed due to the severely reduced time line_20: allocation provided by the TAC. line_21: Mid-totality of the eclipse occurrs on 1993 April 2.7; total eclipse line_22: lasts 36.8 days but the partial eclipse lasts only 1.4 days. THESE line_23: OBSERVATIONS ARE TIME-CRITICAL. ! question: 4 section: 1 line_1: The continnuum of the B dwarf secondary of Zeta Aur is prominent only line_2: in the ultraviolet and data required for this program are not therefore line_3: obtainable from the ground. IUE has been used extensively to study this line_4: target and further observational advances depend on the acquisition of line_5: higher S/N spectra with GHRS. The increased sensitivity, wavelength line_6: resolution, dynamic range and S/N characteristics of the GHRS over those line_7: obtainable with the IUE line_8: (Carpenter et al. 1991, Ap.J. (letters), in press.) will allow more line_9: accurate and detailed modelling of the circumstellar environment line_10: around the K5 mass-losing supergiant primary of Zeta Aur. Only the line_11: GHRS is capable of providing us with the very high precision line line_12: profiles, fluxes, and absolute velocities required for our program. ! question: 5 section: 1 line_1: These observations during the Zeta Aur eclipse are TIME-CRITICAL. line_2: The phases and dates for the required observations are: line_4: Epoch Days before eclipse Date DOY +/- range Eclipse Phase line_5: ______________________________________________________________________ line_6: 1 -221 +/- 14 1992 Aug 25 238 +/- 14 Wind line_7: 2 -55 +/- 5 1993 Feb 07 38 +/- 5 Wind Acceleration line_8: 3 -40 +/- 5 1993 Feb 22 53 +/- 5 " " line_9: 4 -28 +/- 1 1993 Mar 06 65 +/- 1 Chromospheric Ecl. line_10: 5 -22 +/- 1 1993 Mar 12 71 +/- 1 " " line_11: 6 0 +/- 6 1993 Apr 03 93 +/- 6 Totality line_12: ______________________________________________________________________ ! question: 6 section: 1 line_1: At each epoch one WAVE observation will be obtained to provide a more line_2: accurate velocity measurement than given by default SPYBALs. This line_3: additional accuracy will greatly benefit our modelling. ! question: 7 section: 1 line_1: The data will be reduced and anlayzed primarily with software developed line_2: by us for analysis of IUE and GHRS data. Software developed by the line_3: GHRS team will be used to optimize calibration of the observations. line_4: Line profiles and wavelengths will be carefully measured to extract line_5: information on the density, velocity, and temperature structure of line_6: the K supergiant outer atmosphere. line_8: The non-spherical three-dimensional NLTE radiative transfer code line_9: developed at the University of Hamburg over the past decade will be line_10: used to construct models of the chromospheric and wind structure. The line_11: MULTI code will be used to perform consistency checks. The Hamburg line_12: code was written by Hempe (A&A 115, 133 (1982)) and used by Che et al. line_13: (A&A 126, 225 (1983)) to model IUE spectra of three Zeta Aurigae line_14: systems. Synthetic spectra calculated from these models will be line_15: compared with the observations and used to deduce the actual structure line_16: of the stellar atmosphere. line_18: The analysis and modelling effort will be divided between Dr. Alex line_19: Brown (the PI), Dr. Philip Bennett (a new postdoctoral researcher hired line_20: specifically for this project), an as-yet-unappointed graduate student, line_21: and our German collaborators (Drs. Baade and Kirsch). Trips by both line_22: groups to the other institution are planned to allow full collaboration line_23: in this research effort. ! question: 8 section: 1 line_1: ! question: 9 section: 1 line_1: GTO Programs with J. Linsky as PI include: line_2: GTO 1175: Local Interstellar Medium and D/H Ratio - One star observed line_3: in Cycle 0, further observations planned in Cycles 2-4. line_4: GTO 1176: Dynamics and Energy Balance in Stellar Transition Regions - line_5: Cycles 0-4. Data for one star (Capella, also in GTO1175) has been line_6: obtained in Cycle 0. line_7: GTO 1177: Search for Hot Plasma in the Outer Atmospheres of K Giants - line_8: Cycles 2 and 4. NO DATA YET OBTAINED. line_9: GTO 1179: Hybrid Star Winds and Transition Regions - Cycle 2. line_10: NO DATA YET OBTAINED. line_11: GTO 1180: Transition Regions in Very Late M Dwarfs - Cycles 1-4. line_12: NO DATA YET OBTAINED. line_13: NONE OF THE ABOVE GTO PROGRAMS IS RELATED TO THE TOPIC OF THIS PROPOSAL. ! question: 9 section: 2 line_1: GTO 1175/1176 line_2: We observed Capella at phase 0.25 on 15 April 1991. This excellent line_3: data set consisted of low resolution spectra covering the 1150-1700 A line_4: region, moderate resolution spectra centered on the O I 1304A, Si IV line_5: 1400A, and C IV 1550A lines, and echelle spectra centered on Lyman line_6: alpha, the FeII 2600A, and the MgII 2800 liners. These spectra contain line_7: a wealth of information that we are now analyzing to develope a model line_8: for the chromosphere and transition region of this system. An line_9: unexpected discovery was the detection of the SIV intersystem lines line_10: near 1404A. We will soon submit a paper giving definitive values for line_11: them cosmically-important D/H ratio along the line of sight to Capella. ! question: 9 section: 3 line_1: "First Results from the Goddard High Resolution Spectrograph: The line_2: Chromosphere of Alpha Tauri", Carpenter, K., Robinson, R., Wahlgren, line_3: G., Ake, T., Linsky, J., Brown, A., and Walter, F. ApJL 377, L45 1991. line_4: "GHRS Spectroscopy of Cool Stars. I. O I and CO as Diagnostics of line_5: Winds and Circumstellar Shells" Carpenter, K., Robinson, R., Ebbets, line_6: D., Brown, A., Linsky, J., BAAS, 23, #2, 910, 1991. line_7: "GHRS Spectroscopy of Cool Star. II. The Hybrid Giant Gamma Dra line_8: (K5 III)", Brown, A., Linsky, J.L., Carpenter, K., Robinson, R., line_9: Ebbets, D., BAAS, 23, #2, 910, 1991. line_10: "GHRS Far-Ultraviolet Spectra of the Coronal Giant Capella Binary", line_11: Linsky, J.L., Brown, A., Carpenter, K., Robinson, R., line_12: BAAS, 23, #2, 910, 1991. line_13: "GHRS Chromospheric Emission Line Spectra of the Red Giant Alpha Tau" line_14: Carpenter, K. G., Robinson, R. D., Ebbets, D. C., Brown, A., and line_15: Linsky, J., "HST Workshop: The Year of First Light", May 1991. ! question: 10 section: 1 line_1: Software developed by the GHRS IDT and the proposers will be used in the line_2: reduction and analysis of these observations. A SUN workstation at JILA line_3: connected to the CASA cluster will be used for data reduction and line_4: analysis. ! !end of general form text general_form_address: lname: BROWN fname: ALEXANDER title: DR. category: PI inst: COLORADO, UNVERSITY OF addr_1: JOINT INSTITUTE FOR LABORATORY ASTROPHYSICS addr_2: UNIVERSITY OF COLORADO addr_3: CAMPUS BOX 440 city: BOULDER state: CO zip: 803090440 country: USA phone: (303) 492-7810 telex: (303) 492-5235 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: HD32068 name_2: ZETA-AUR descr_1: A,140,112 pos_1: RA = 04H 58M 58.68S +/-.01S, pos_2: DEC = +41D 00' 17.8" +/-.1" equinox: 1950.0 pm_or_par: Y pos_epoch_bj: B pos_epoch_yr: 1950.00 ra_pm_val: 0.000800 ra_pm_unct: 0.000067 dec_pm_val: -0.0220 dec_pm_unct: 0.0010 an_prlx_val: 0.0050 rv_or_z: V = +13 fluxnum_1: 1 fluxval_1: V = 3.75 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 sequence_1: DEFINE sequence_2: CHROM1 targname: HD32068 config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B18 wavelength: 3130 num_exp: 2 time_per_exp: 244.8S priority: 1 param_1: STEP-PATT=7 req_1: SEQ 1.0-4.5 NO GAP ! linenum: 2.000 sequence_1: ^ targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B18 wavelength: 3075.0 num_exp: 1 time_per_exp: 64S priority: 1 param_1: STEP-PATT=3 req_1: CALIB FOR 2.5 NO SLEW; req_2: SEQ 2.0-2.5 NO GAP comment_1: NO CARROUSEL MOTION comment_2: BETWEEN 2.0 AND 2.5 . ! linenum: 2.500 sequence_1: ^ targname: HD32068 config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B18 wavelength: 3075.0 num_exp: 1 time_per_exp: 652.8S priority: ^ param_1: STEP-PATT=7 param_2: FP-SPLIT=STD ! linenum: 3.000 sequence_1: ^ targname: ^ config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B19 wavelength: 3048 num_exp: 1 time_per_exp: 544S priority: ^ param_1: STEP-PATT=7 param_2: FP-SPLIT=STD ! linenum: 3.500 sequence_1: ^ targname: ^ config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B19 wavelength: 3004 num_exp: 1 time_per_exp: 435.2S priority: ^ param_1: STEP-PATT=7 param_2: FP-SPLIT=STD ! linenum: 4.000 sequence_1: ^ targname: ^ config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B26 wavelength: 2150 num_exp: 1 time_per_exp: 435.2S priority: ^ param_1: STEP-PATT=7 param_2: FP-SPLIT=STD ! linenum: 4.500 sequence_1: ^ targname: ^ config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B33 wavelength: 1704 num_exp: 1 time_per_exp: 761.6S priority: ^ param_1: ^ ! linenum: 5.000 sequence_1: DEFINE sequence_2: WECL targname: HD32068 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1190.5 num_exp: 1 time_per_exp: 544S priority: 1 param_1: STEP-PATT=5 param_2: FP-SPLIT=STD req_1: SEQ 5.0-6.5 NO GAP ! linenum: 5.300 sequence_1: ^ targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1263.5 num_exp: 1 time_per_exp: 64S priority: 1 param_1: STEP-PATT=3 req_1: CALIB FOR 5.5 NO SLEW; req_2: SEQ 5.3-5.5 NO GAP comment_1: NO CARROUSEL MOTION comment_2: BETWEEN 5.3 AND 5.5. ! linenum: 5.500 sequence_1: DEFINE sequence_2: WECL targname: HD32068 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1263.5 num_exp: 1 time_per_exp: 544S priority: 1 param_1: STEP-PATT=5 param_2: FP-SPLIT=STD ! linenum: 6.000 sequence_1: ^ targname: ^ config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1540.0 num_exp: 1 time_per_exp: 544S priority: ^ param_1: STEP-PATT=5 param_2: FP-SPLIT=STD ! linenum: 6.300 sequence_1: ^ targname: ^ config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B24 wavelength: 2335.4 num_exp: 1 time_per_exp: 218S priority: ^ param_1: STEP-PATT=7 param_2: FP-SPLIT=STD ! linenum: 6.500 sequence_1: ^ targname: ^ config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B22 wavelength: 2611.4 num_exp: 1 time_per_exp: 544S priority: ^ param_1: STEP-PATT=7 param_2: FP-SPLIT=STD ! linenum: 8.000 sequence_1: DEFINE sequence_2: WACC targname: HD32068 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1573.0 num_exp: 1 time_per_exp: 544S priority: 1 param_1: STEP-PATT=5 param_2: FP-SPLIT=STD req_1: SEQ 8.0-10.5 NO GAP ! linenum: 8.500 sequence_1: ^ targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1263.5 num_exp: 1 time_per_exp: 64S priority: 1 param_1: STEP-PATT=3 req_1: CALIB FOR 9.0 NO SLEW; req_2: SEQ 8.5-9.0 NO GAP comment_1: NO CARROUSEL MOTION comment_2: BETWEEN 8.5 AND 9.0. ! linenum: 9.000 sequence_1: ^ targname: HD32068 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1263.5 num_exp: 1 time_per_exp: 544S priority: 1 param_1: STEP-PATT=5 param_2: FP-SPLIT=STD ! linenum: 9.500 sequence_1: ^ targname: HD32068 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1643.5 num_exp: 1 time_per_exp: 653S priority: 1 param_1: STEP-PATT=5 param_2: FP-SPLIT=STD ! linenum: 10.000 sequence_1: ^ targname: HD32068 config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B33 wavelength: 1705.0 num_exp: 1 time_per_exp: 653S priority: 1 param_1: STEP-PATT=7 param_2: FP-SPLIT=STD ! linenum: 10.300 sequence_1: ^ targname: ^ config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B24 wavelength: 2335.4 num_exp: 1 time_per_exp: 218S priority: ^ param_1: STEP-PATT=7 param_2: FP-SPLIT=STD ! linenum: 10.500 sequence_1: DEFINE sequence_2: WACC targname: HD32068 config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B18 wavelength: 3075.0 num_exp: 1 time_per_exp: 653S priority: 1 param_1: STEP-PATT=7 param_2: FP-SPLIT=STD ! linenum: 14.000 targname: HD32068 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 5S priority: 1 param_1: SEARCH-SIZE=5 param_2: FAINT=3400 req_1: ONBOARD ACQ FOR 15; req_2: AT 25-AUG-92 +/-14D; req_3: SEQ 14-18 NO GAP; req_4: CYCLE 2/14-18; req_5: SEQ 14-15 comment_1: STEP TIME = 200 MSEC comment_2: PHASE IS -221 DAYS FROM MID-ECLIPSE ! linenum: 15.000 targname: HD32068 config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 163.2S priority: 2 req_1: ONBOARD ACQ FOR 18; req_2: AT 25-AUG-92 +/-14D; comment_1: STEP TIME = 1.6 SEC comment_2: CENTER IN LSA AFTER NEW DEFCAL ! linenum: 18.000 sequence_1: USE sequence_2: WECL req_1: AT 25-AUG-92 +/-14D; ! linenum: 24.000 targname: HD32068 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 1.8S priority: 1 param_1: SEARCH-SIZE=3 param_2: BRIGHT=RETURN req_1: ONBOARD ACQ FOR 25; req_2: AT 07-FEB-93 +/-5D; req_3: SEQ 24-25 NO GAP; req_4: CYCLE 2/24-25; req_5: SEQ 24-25 comment_1: STEP TIME = 200 MSEC comment_2: FAINT=3400 comment_3: PHASE IS -55 DAYS FROM MID-ECLIPSE comment_4: NO ACQ/PEAKUP PER INST SCIENTIST comment_5: INSTRUCTIONS. IF NO AUTOMATIC comment_6: PEAKUP IN SSA, REVISION NEEDED. ! linenum: 25.000 sequence_1: USE sequence_2: WACC req_1: AT 07-FEB-93 +/-5D; ! linenum: 34.000 targname: HD32068 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 1.8S priority: 1 param_1: SEARCH-SIZE=3 param_2: BRIGHT=RETURN req_1: ONBOARD ACQ FOR 35; req_2: AT 22-FEB-93 +/-5D; req_3: SEQ 34-35 NO GAP; req_4: CYCLE 2/34-35; req_5: SEQ 34-35 comment_1: STEP TIME = 200 MSEC comment_2: FAINT=3400 comment_3: PHASE IS -40 DAYS FROM MID-ECLIPSE comment_4: NO ACQ/PEAKUP PER INST SCIENTIST comment_5: INSTRUCTIONS. IF NO AUTOMATIC comment_6: PEAKUP IN SSA, REVISION NEEDED. ! linenum: 35.000 sequence_1: USE sequence_2: WACC req_1: AT 22-FEB-93 +/-5D; ! linenum: 44.000 targname: HD32068 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 1.8S priority: 1 param_1: SEARCH-SIZE=3 param_2: BRIGHT=RETURN req_1: ONBOARD ACQ FOR 45; req_2: AT 06-MAR-93 +/-1D; req_3: SEQ 44-48 NO GAP; req_4: CYCLE 2/44-48; req_5: SEQ 44-45 comment_1: STEP TIME = 200 MSEC comment_2: FAINT=3400 comment_3: PHASE IS -28 DAYS FROM MID-ECLIPSE ! linenum: 45.000 targname: HD32068 config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 163.2S priority: 2 req_1: ONBOARD ACQ FOR 48; req_2: AT 06-MAR-93 +/-1D; comment_1: STEP TIME = 1.6 SEC comment_2: CENTER IN LSA AFTER NEW DEFCAL ! linenum: 48.000 sequence_1: USE sequence_2: CHROM1 req_1: AT 06-MAR-93 +/-1D; ! linenum: 54.000 targname: HD32068 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 1.8S priority: 1 param_1: SEARCH-SIZE=3 param_2: BRIGHT=RETURN req_1: ONBOARD ACQ FOR 55; req_2: AT 12-MAR-93 +/-1D; req_3: SEQ 54-58 NO GAP; req_4: CYCLE 2/54-58; req_5: SEQ 54-55 comment_1: STEP TIME = 200 MSEC comment_2: FAINT=3400 comment_3: PHASE IS -22 DAYS FROM MID-ECLIPSE ! linenum: 55.000 targname: HD32068 config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 163.2S priority: 2 req_1: ONBOARD ACQ FOR 58; req_2: AT 12-MAR-93 +/-1D; comment_1: STEP TIME = 1.6 SEC comment_2: CENTER IN LSA AFTER NEW DEFCAL ! linenum: 58.000 sequence_1: USE sequence_2: CHROM1 req_1: AT 12-MAR-93 +/-1D; ! linenum: 64.000 targname: HD32068 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 1.8S priority: 1 param_1: SEARCH-SIZE=3 param_2: FAINT=3400 req_1: ONBOARD ACQ FOR 68-69; req_2: AT 03-APR-93 +/-6D; req_3: SEQ 64-69 NO GAP; req_4: CYCLE 2/64-69; req_5: SEQ 64-69 comment_1: STEP TIME = 200 MSEC comment_2: PHASE IS 0 DAYS FROM MID-ECLIPSE comment_3: NO ACQ/PEAKUP PER INST SCIENTIST comment_4: INSTRUCTIONS. IF NO AUTOMATIC comment_5: PEAKUP IN SSA, REVISION NEEDED. ! linenum: 68.000 sequence_1: USE sequence_2: WECL req_1: AT 03-APR-93 +/-6D; ! linenum: 69.000 targname: HD32068 config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B32 wavelength: 1786.0 num_exp: 1 time_per_exp: 544S priority: 1 param_1: STEP-PATT=7 param_2: FP-SPLIT=STD ! ! end of exposure logsheet ! No scan data records found