! $Id: 6288,v 4.1 1995/04/12 18:12:11 pepsa Exp $ ! Z627REP.PHASE2 ! 1995 APRIL 3 AB ! RPSS Template file with all keywords specified COVERPAGE: TITLE_1: ECLIPSE MAPPING OF THE CHROMOPSHERIC AND TRANSITION REGION TITLE_2: STRUCTURE OF HR2554 (G6 II) -- REPEAT - HOPR 0247 SCI_CAT: COOL STARS ! Item #2a: Scientific category, X20 SCI_SUBCAT: ATMOSPHERES & WINDS ! Item #2b: Scientific subcategory, X20 PROPOSAL_FOR: GO PI_TITLE: DR. PI_FNAME: ALEXANDER PI_LNAME: BROWN PI_INST: U. OF COLORADO PI_COUNTRY: USA PI_PHONE: (303) 492-7810 KEYWORDS_1: G6II+A1 ECLIPSING BINARY SYSTEM ! X55 list of keywords HOURS_PRI: 33.2 NUM_PRI: 1 HRS: Y TIME_CRIT: Y ! Time-critical obs., or CVZ target? Y or blank FUNDS_AMOUNT: 170000 FUNDS_LENGTH: 24 FUNDS_DATE: MAR-93 PI_POSITION: SENIOR RES ASSOCIATE ! X20 OFF_FNAME: CARL OFF_LNAME: WIEMAN OFF_TITLE: CHAIRMAN OFF_INST: JOINT INSTITUTE FOR LABORATORY ASTROPHYSICS OFF_ADDR_1: UNIVERSITY OF COLORADO OFF_ADDR_2: CAMPUS BOX 440 OFF_CITY: BOULDER OFF_STATE: CO OFF_ZIP: 803090440 ! X9 OFF_COUNTRY: USA OFF_PHONE: (303) 492 5128 OFF_TELEX: (303) 492 5235 ABSTRACT: LINE_1:We propose to observe an eclipse of the Zeta Aurigae-type binary HR2554 LINE_2:using the GHRS. Every 195 days the A1 dwarf secondary passes behind the LINE_3:outer atmosphere of the G6 II primary and can be used as light source to LINE_4:observe absorption lines from plasma in the G star atmopshere. The G LINE_5:star has a hybrid-chromosphere structure with hot transition region LINE_6:plasma and a cool stellar wind. THESE OBSERVATIONS WOULD BE THE FIRST LINE_7:ECLIPSE OBSRRVATIONS OF THIS TYPE OF ATMOSPHERE WITH GHRS AND COMPARED LINE_8:WITH OUR RESULTS FOR THE K4 SUPERGIANT Zeta Aur, which shows only the LINE_9:typical red supergiant wind. We shall model the observed line profiles LINE_10:and determine the temperature structure, density stratification, wind LINE_11:acceleration/turbulence/ionization as a function of distance above the LINE_12:G star photosphere. The hot and cool plasma are intermixed in this LINE_13:outer atmosphere and we will quantify this "thermal bifurcation". Both LINE_14:the static and outflowing components of the atmopshere will be modelled. LINE_15:The mass loss rate and the wind velocity and density laws as a function LINE_16:of radius will be determined. The vast majority of the needed modelling LINE_17:code will have been developed already for our Zeta Aur analysis. This LINE_18:project represents an opportunity to significantly advance LINE_19:knowledge about the spatial structuring of cool star outer atmospheres LINE_20:and the physical process operating within them. GENERAL_FORM_PROPOSERS: lname: BROWN fname: ALEXANDER title: PI inst: 1764 country: USA ! lname: LINSKY fname: JEFFREY mi: L. inst: 1764 country: USA ! LNAME: Bennett ! Investigator's last name, X20 FNAME: Philip ! Investigator's first name, X20 INST: 1764 ! Investigator's institution code number (or full institut` COUNTRY: USA ! Investigator's country, X20 ESA: ! Is investigator affiliated with ESA or an ! ESA member-state institution? Y or blank LNAME: Harper ! Investigator's last name, X20 FNAME: Graham ! Investigator's first name, X20 INST: 1764 ! Investigator's institution code number (or full institut` COUNTRY: USA ! Investigator's country, X20 ESA: ! Is investigator affiliated with ESA or an ! ESA member-state institution? Y or blank ! LNAME: Baade ! Investigator's last name, X20 FNAME: Robert ! Investigator's first name, X20 INST: 5580 ! Investigator's institution code number (or full in` COUNTRY: Germany ! Investigator's country, X20 ESA: Y ! Is investigator affiliated with ESA or an ! ESA member-state institution? Y or blank LNAME: Kirsch ! Investigator's last name, X20 FNAME: Thomas ! Investigator's first name, X20 INST: 5580 ! Investigator's institution code number (or full instit` COUNTRY: Germany ! Investigator's country, X20 ESA: Y ! Is investigator affiliated with ESA or an ! ESA member-state institution? Y or blank LNAME: Reimers ! Investigator's last name, X20 FNAME: Dieter ! Investigator's first name, X20 INST: 5580 ! Investigator's institution code number (or full in` COUNTRY: Germany ! Investigator's country, X20 ESA: Y ! Is investigator affiliated with ESA or an ! ESA member-state institution? Y or blank ! ! end of general_form_proposers block GENERAL_FORM_TEXT: QUESTION: 3 ! n, 2 < n < 13 SECTION: 1 ! n, 1 < n < 9 LINE_1:Our proposed observations will provide the first high-quality (S/N = 60- LINE_2:80) UV spectrum of HR2554 during atmospheric and photospheric eclipse. LINE_3:Requested exposures are listed below. The exposure times at short LINE_4:wavelengths during partial eclipse are increased by 50% to compensate LINE_5:somewhat for the decrease continuum signal. The quoted signal-to-noise LINE_6:values are calculated per resolution element (i.e. per two diodes on the LINE_7:detector). The large dynamic range and low noise of the GHRS ensures LINE_8:that many weak features can be accurately measured in these exposures. LINE_9:**** SEVERAL OBSERVATIONS FAILED IN APRIL 1994 AND NEW SPECTRA WERE LINE_10:****APPROVED FOR MAY 1995 IN RESPONSE TO HOPR 0247. LINE_11:****EPOCHS 2, 4, AND 8 ARE REPEATED (SUs 03, 07, and 0F) IN FULL, LINE_12:****WHILE EPOCH 1 (SU 01) IS PARTIALLY REPEATED. LINE_13: QUESTION: 3 ! n, 2 < n < 13 SECTION: 2 ! n, 1 < n < 9 LINE_1:The observations requested in Phase 1 were: LINE_2:---------------------------------------------------------------------- LINE_3: Ion UV Lambda Grating Continuum Cts/ S/N Exp. LINE_4: mult. (A) Flux*E-12 sec Time LINE_5: erg/(cm^2*s*A) (min) LINE_6:---------------------------------------------------------------------- LINE_7: C IV 1 1548.20, 1550.77 G160M 5.0 2.3 80 24 LINE_8: (ALSO includes Si II UV2 1533.4, C I UV3 1560-61, LINE_9: Fe II UV45 1559.1, 1563.8, CO A-X (0-0) 1544 bandhead ) LINE_10:Si IV 1 1393.76, 1402.77 G160M 2.5 1.3 60 23 LINE_11: (ALSO includes CO A-X (5-0;4-0) 1393,1419 bandheads, LINE_12: Si II UV 13.02 1409.0, 1410.2, O IV 1401.2 ) LINE_13:Si II 1 1816.93 G200M 4.5 3.7 80 15 LINE_14: (ALSO includes S I UV2 1820.3 1826.2, Al III UV1 1854.7 ) LINE_15:Mg II 1 2795.52, 2802.70 ECH-B 4.5 5.4 80 10 LINE_16:Fe II 1 2607.09, 2613.82 ECH-B 2.8 1.3 60 23 LINE_17: 2611.87 LINE_18:Fe II 3 2332.80, 2338.01 ECH-B 3.6 2.4 80 23 LINE_19: (ALSO includes Si II UV0.01 2334.6, Fe II UV35 2331.3 ) QUESTION: 4 ! n, 2 < n < 13 SECTION: 1 ! n, 1 < n < 9 LINE_1:The continuum of the A dwarf secondary of Zeta Aur is prominent only in LINE_2: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 (Carpenter et al. 1992, Ap.J. Lett., 377, L45.) LINE_8:will allow more accurate and detailed modelling of the circumstellar LINE_9:environment around the G6 hybrid-atmosphere bright giant primary of LINE_10:HR2554. ONLY THE GHRS IS CAPABLE OF PROVIDING THE VERY HIGH PRECISION LINE_11:LINE PROFILES, FLUXES, AND ABSOLUTE VELOCITIES NEEDED FOR OUR MODELLING. LINE_12: QUESTION: 5 ! n, 2 < n < 13 SECTION: 1 ! n, 1 < n < 9 LINE_1:The observations must be scheduled at specific phases during the eclipse LINE_2:of the A1 dwarf secondary by the extended atmosphere of the bright giant LINE_3:primary. Eclipses of HR2554 occur every 195 days and during Cycle 4 LINE_4:eclipses are centered on 1994 April 18 and 1994 October 30. The system LINE_5:lies near the ecliptic pole so the beta angle (star-antiSun angle) is LINE_6:always close to 90 degrees. Therefore, the star is observable by HST at LINE_7:all dates during Cycle 4. Coordinated IUE observations will be possible LINE_8:if the April eclipse is observed. LINE_9:Times of mideclipse are given by t = JD2447898.57 + n*195.28days. LINE_10:***REPEAT OBSERVATIONS ARE REQUESTED AT +3, +4.5, +6, and +30 days LINE_11:****RELATIVE TO MID-ECLIPSE. LINE_12:The time between first and fourth contacts is 3.2 days. LINE_13:(See Schroder 19 90, A&A, 236,165 for details). Eclipses during LINE_14:Cycle 4 occur on 1994 April 18.31, Oct 30.59, and 1995 May 13.7. LINE_15:***The Exposure Logsheet of repeat observations is constructed LINE_16:***specifically for the May 1995 eclipse. QUESTION: 6 ! n, 2 < n < 13 SECTION: 1 ! n, 1 < n < 9 LINE_1:We require high wavelength accuracy in order to measure absolute LINE_2:velocities in the chromosphere and wind of our target star. We therefore LINE_3:request one WAVECAL exposure for ECH-B and G160M at each epoch. LINE_4:Wavelength matching between different spectra at each epoch and between LINE_5:epochs will be done using interstellar features. Routine SPYBAL spectra LINE_6:will be used to calibrate spectra without dedicated WAVCALS. The WAVCAL LINE_7:exposures must be taken at the same carrousel position and close in time LINE_8:to the science exposures to remove uncertainties caused by GIMP and LINE_9:thermal drifts which move the image around on the GHRS photocathode. QUESTION: 7 ! n, 2 < n < 13 SECTION: 1 ! n, 1 < n < 9 LINE_1:The data will be reduced and analyzed with in-house software developed LINE_2:for analysis of IUE and GHRS data. Software developed by the GHRS IDT LINE_3:will be used to optimize the calibration of the observations. Line LINE_4:widths, profiles, and wavelengths will be carefully measured to extract LINE_5:information on the temperature, density, and velocity structure of the LINE_6:outer atmosphere, including both random non-thermal velocities and LINE_7:systematic flows. Relative and absolute fluxes will be measured to LINE_8:estimate densities and temperatures in the outer atmosphere. LINE_9:The NLTE code developed at the University of Hamburg over the past LINE_10:decade will be used to construct models of the chromospheric and wind LINE_11:structure. The integral-operator method of Baade (A&A 233, 486, 1990) LINE_12:will be used to calculate line profiles and emergent fluxes for the 2D LINE_13:axisymmetric geometry of the binary system. Synthetic spectra LINE_14:calculated from these models will be compared with the observations and LINE_15:used to deduce the actual structure of the stellar atmosphere. QUESTION: 7 ! n, 2 < n < 13 SECTION: 2 ! n, 1 < n < 9 LINE_1:At JILA, we will model the G star chromosphere and wind using SMULTI, LINE_2:a spherical version of MULTI (Scharmer & Carlsson, 1985) developed by LINE_3:Harper (1993). Photospheric models of the G star (needed for the LINE_4:boundary radiation field input to SMULTI) will be calculated using the LINE_5:existing ATHENA spherical code (Bennett, 1991). The A star radiation LINE_6:field will be calculated using the NLTE code of Hubeny & Lanz (1988). We LINE_7:will investigate the interaction of the G star wind dynamics with the LINE_8:orbital motion of the binary system. We will use a smooth particle LINE_9:hydrodynamics (SPH) code (Monaghan, 1988; Benz, 1988) for this purpose. LINE_10:In-house 2D axisymmetric radiative transfer codes, based on the 2D LINE_11:double-splitting iteration method (Castor, Dykema & Klein, 1990, in LINE_12:'Stellar Atmospheres: Beyond Classical Models', p.49) developed for the LINE_13:analysis of the zeta Aurigae system will be used to construct models of LINE_14:the circumstellar environment consistent with the wind from the G star LINE_15:and the A star radiation field. Line profiles will be calculated with a LINE_16:comoving frame radiative transfer code using the Short Characteristic LINE_17:method of Kunasz & Auer (JQSRT 39, 67, 1988). Synthetic spectra and LINE_18:line profiles produced by this analysis will be compared with LINE_19:observations and used to determine structural details of the G star LINE_20:chromosphere and wind. This will provide an analysis independent of the LINE_21:binary profile fitting technique employed at Hamburg. We emphasize that LINE_22:this analysis is analogous to that employed for the Zeta Aurigae system, LINE_23:and will require only a modest amount of additional development. QUESTION: 8 ! n, 2 < n < 13 SECTION: 1 ! n, 1 < n < 9 LINE_1: None. QUESTION: 9 ! n, 2 < n < 13 SECTION: 1 ! n, 1 < n < 9 LINE_1: GO Program 3626 - Empirical determination of the wind velocity and LINE_2: density laws for the K supergiant Zeta Aurigae from eclipse ingress LINE_3: Spectra (A. Brown PI, J. Linsky, R. Weyman, D. Reimers, R. Baade, LINE_4: T. Kirsch) QUESTION: 10 ! n, 2 < n < 13 SECTION: 1 ! n, 1 < n < 9 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 workstation at JILA LINE_3: connected to the CASA cluster is available for data reduction and LINE_4: analysis. GENERAL_FORM_ADDRESS: lname: Brown fname: Alexander title: Dr. category: PI inst: Center for Astrophysics and Space Astronomy addr_1: University of Colorado city: Boulder state: CO zip: 803090389 country: USA phone: (303) 492-7810 telex: 755842 JILA FIXED_TARGETS: ! Sect.'s refer to Phase II Proposal Instructions TARGNUM: 1 NAME_1: HD50337 DESCR_1: A,138,123 POS_1: RA=06H48M46.13S+/-0.01S, POS_2: DEC=-53D33'47.15"+/-0.2" EQUINOX: 1950 ! X7 Equinox for coordinates. Sect 5.1.5 PM_OR_PAR: Y ! Y if prop. mot. or parallax relevent. Sect 5.1.6 POS_EPOCH_BJ: B ! Epoch of position (B or J). POS_EPOCH_YR: 1950 ! F4.2 Epoch of position (year). RA_PM_VAL: -0.0004 ! F5.4 RA proper motion (seconds-of-time/yr) RA_PM_UNCT: 0.0006 ! F4.4 RA proper motion uncertainty DEC_PM_VAL: +0.030 ! F4.4 Dec proper motion value (arc-sec/yr). DEC_PM_UNCT: 0.005 ! F4.4 Dec proper motion uncertainty. AN_PRLX_VAL: 0.0 ! F4.4 Annual parallax value (arc-sec). AN_PRLX_UNCT: 0.0 ! F4.4 Annual parallax uncertainty. RV_OR_Z: V=0.0 ! X15 Radial velocity FLUXNUM_1: 1 ! I3 Flux reference number. Sect 5.1.9 FLUXVAL_1: V=4.40 ! X40 Flux data. FLUXNUM_2: 1 ! I3 Flux reference number. Sect 5.1.9 FLUXVAL_2: B-V=+0.92 ! X40 Flux data. FLUXNUM_3: 2 ! I3 Flux reference number. Sect 5.1.9 FLUXVAL_3: F-CONT(1835) = 4.5E-12 ! X40 Flux data. FLUXNUM_4: 3 ! I3 Flux reference number. Sect 5.1.9 FLUXVAL_4: F-CONT(1543) = 5.0E-12 ! X40 Flux data. FLUXNUM_5: 4 ! I3 Flux reference number. Sect 5.1.9 FLUXVAL_5: F-CONT(1400) = 2.5E-12 ! X40 Flux data. FLUXNUM_6: 5 ! I3 Flux reference number. Sect 5.1.9 FLUXVAL_6: F-CONT(2334) = 3.6E-12 ! X40 Flux data. FLUXNUM_7: 6 ! I3 Flux reference number. Sect 5.1.9 FLUXVAL_7: F-CONT(2611) = 2.8E-12 ! X40 Flux data. FLUXNUM_8: 7 ! I3 Flux reference number. Sect 5.1.9 FLUXVAL_8: F-CONT(2799) = 4.5E-12 ! X40 Flux data. EXPOSURE_LOGSHEET: ! LINENUM: 4.0 SEQUENCE_1: DEFINE SEQUENCE_2: HR2554A TARGNAME: HD50337 CONFIG: HRS OPMODE: ACCUM APERTURE: 2.0 SP_ELEMENT: G200M WAVELENGTH: 1835 PARAM_1: STEP-PATT=5 PARAM_2: FP-SPLIT=STD NUM_EXP: 1 TIME_PER_EXP: 980S S_TO_N: 80.0 FLUXNUM_1: 2 PRIORITY: 1 REQ_1: ! LINENUM: 4.1 SEQUENCE_1: DEFINE SEQUENCE_2: HR2554A TARGNAME: HD50337 CONFIG: HRS OPMODE: ACCUM APERTURE: 2.0 SP_ELEMENT: G160M WAVELENGTH: 1548 PARAM_1: STEP-PATT=5 PARAM_2: FP-SPLIT=STD NUM_EXP: 1 TIME_PER_EXP: 1523S S_TO_N: 80.0 FLUXNUM_1: 3 PRIORITY: 1 ! LINENUM: 4.2 SEQUENCE_1: DEFINE SEQUENCE_2: HR2554A TARGNAME: WAVE CONFIG: HRS OPMODE: ACCUM APERTURE: SC2 SP_ELEMENT: G160M WAVELENGTH: 1403 PARAM_1: STEP-PATT=3 NUM_EXP: 1 TIME_PER_EXP: 64S PRIORITY: 3 REQ_1: CALIB FOR 4.3 NO SLEW ! LINENUM: 4.3 SEQUENCE_1: DEFINE SEQUENCE_2: HR2554A TARGNAME: HD50337 CONFIG: HRS OPMODE: ACCUM APERTURE: 2.0 SP_ELEMENT: G160M WAVELENGTH: 1403 PARAM_1: STEP-PATT=5 PARAM_2: FP-SPLIT=STD NUM_EXP: 1 TIME_PER_EXP: 1416S S_TO_N: 60.0 FLUXNUM_1: 4 PRIORITY: 1 ! LINENUM: 4.4 SEQUENCE_1: DEFINE SEQUENCE_2: HR2554A TARGNAME: HD50337 CONFIG: HRS OPMODE: ACCUM APERTURE: 2.0 SP_ELEMENT: ECH-B WAVELENGTH: 2334 PARAM_1: STEP-PATT=7 PARAM_2: FP-SPLIT=STD NUM_EXP: 1 TIME_PER_EXP: 1416S S_TO_N: 80.0 FLUXNUM_1: 5 PRIORITY: 1 ! LINENUM: 4.5 SEQUENCE_1: DEFINE SEQUENCE_2: HR2554A TARGNAME: HD50337 CONFIG: HRS OPMODE: ACCUM APERTURE: 2.0 SP_ELEMENT: ECH-B WAVELENGTH: 2611 PARAM_1: STEP-PATT=7 PARAM_2: FP-SPLIT=STD NUM_EXP: 1 TIME_PER_EXP: 1416S S_TO_N: 60.0 FLUXNUM_1: 6 PRIORITY: 1 ! LINENUM: 4.6 SEQUENCE_1: DEFINE SEQUENCE_2: HR2554A TARGNAME: WAVE CONFIG: HRS OPMODE: ACCUM APERTURE: SC2 SP_ELEMENT: ECH-B WAVELENGTH: 2800 PARAM_1: STEP-PATT=3 NUM_EXP: 1 TIME_PER_EXP: 64S PRIORITY: 3 REQ_1: CALIB FOR 4.7 NO SLEW ! LINENUM: 4.7 SEQUENCE_1: DEFINE SEQUENCE_2: HR2554A TARGNAME: HD50337 CONFIG: HRS OPMODE: ACCUM APERTURE: 2.0 SP_ELEMENT: ECH-B WAVELENGTH: 2800 PARAM_1: STEP-PATT=7 PARAM_2: FP-SPLIT=STD NUM_EXP: 1 TIME_PER_EXP: 600S S_TO_N: 80.0 FLUXNUM_1: 7 PRIORITY: 1 ! LINENUM: 10.0 TARGNAME: HD50337 CONFIG: HRS OPMODE: ACQ APERTURE: 2.0 SP_ELEMENT: MIRROR-A2 NUM_EXP: 1 TIME_PER_EXP: 9S PRIORITY: 1 PARAM_1: BRIGHT=RETURN, PARAM_2: SEARCH-SIZE=3 COMMENT_1: STEP-TIME = 1 SEC COMMENT_2: EXPECT 1300 CT/S WITH A2 NORMALLY. FLUXNUM_1: 1 FLUXNUM_2: 2 REQ_1: CYCLE 4 / 10-13; REQ_2: ONBOARD ACQ FOR 11-13; REQ_3: GROUP 10-13 NO GAP; REQ_4: AT 13-JUN-95 +/- 5D COMMENT_4: PHASE IS 30 DAYS AFTER MID-ECLIPSE ! LINENUM: 11.0 TARGNAME: HD50337 CONFIG: HRS OPMODE: IMAGE APERTURE: 2.0 SP_ELEMENT: MIRROR-N2 NUM_EXP: 1 TIME_PER_EXP: 51.2S PRIORITY: 1 PARAM_1: NX=16, PARAM_2: NY=16, PARAM_3: DELTA-X=4, PARAM_4: DELTA-Y=4 COMMENT_1: STEP-TIME=0.2S ! LINENUM: 11.5 TARGNAME: HD50337 CONFIG: HRS OPMODE: ACCUM APERTURE: 2.0 SP_ELEMENT: ECH-B WAVELENGTH: 2334 PARAM_1: STEP-PATT=7 PARAM_2: FP-SPLIT=STD NUM_EXP: 1 TIME_PER_EXP: 1416S S_TO_N: 80.0 FLUXNUM_1: 5 PRIORITY: 1 ! LINENUM: 12.0 TARGNAME: WAVE CONFIG: HRS OPMODE: ACCUM APERTURE: SC2 SP_ELEMENT: ECH-B WAVELENGTH: 2611 PARAM_1: STEP-PATT=3 NUM_EXP: 1 TIME_PER_EXP: 64S PRIORITY: 3 REQ_1: CALIB FOR 13.0 NO SLEW ! LINENUM: 13.0 TARGNAME: HD50337 CONFIG: HRS OPMODE: ACCUM APERTURE: 2.0 SP_ELEMENT: ECH-B WAVELENGTH: 2611 PARAM_1: STEP-PATT=7 PARAM_2: FP-SPLIT=STD NUM_EXP: 1 TIME_PER_EXP: 1416S S_TO_N: 60.0 FLUXNUM_1: 6 PRIORITY: 1 ! LINENUM: 20.0 TARGNAME: HD50337 CONFIG: HRS OPMODE: ACQ APERTURE: 2.0 SP_ELEMENT: MIRROR-A2 NUM_EXP: 1 TIME_PER_EXP: 9S PRIORITY: 1 PARAM_1: BRIGHT=RETURN, PARAM_2: SEARCH-SIZE=3 FLUXNUM_1: 1 FLUXNUM_2: 2 REQ_1: CYCLE 4 / 20-22; REQ_2: ONBOARD ACQ FOR 21-22; REQ_3: GROUP 20-22 NO GAP; REQ_4: AT JD2449855.7 +/- 0.4D COMMENT_1: STEP-TIME = 1 SEC COMMENT_2: EXPECT 1300 CT/S WITH A2 NORMALLY. COMMENT_3: PHASE IS 4.5 DAYS AFTER MID-ECLIPSE ! LINENUM: 21.0 TARGNAME: HD50337 CONFIG: HRS OPMODE: IMAGE APERTURE: 2.0 SP_ELEMENT: MIRROR-N2 NUM_EXP: 1 TIME_PER_EXP: 51.2S PRIORITY: 1 PARAM_1: NX=16, PARAM_2: NY=16, PARAM_3: DELTA-X=4, PARAM_4: DELTA-Y=4 COMMENT_1: STEP-TIME=0.2S ! LINENUM: 22.0 SEQUENCE_1: USE SEQUENCE_2: HR2554A ! LINENUM: 40.0 TARGNAME: HD50337 CONFIG: HRS OPMODE: ACQ APERTURE: 2.0 SP_ELEMENT: MIRROR-A2 NUM_EXP: 1 TIME_PER_EXP: 9S PRIORITY: 1 PARAM_1: BRIGHT=RETURN, PARAM_2: SEARCH-SIZE=3 FLUXNUM_1: 1 FLUXNUM_2: 2 REQ_1: CYCLE 4 / 40-42; REQ_2: ONBOARD ACQ FOR 41-42; REQ_3: GROUP 40-42 NO GAP; REQ_4: AT JD2449857.2 +/- 0.5D COMMENT_1: STEP-TIME = 1 SEC COMMENT_2: EXPECT 1300 CT/S WITH A2 NORMALLY. COMMENT_3: PHASE IS 6 DAYS AFTER MID-ECLIPSE ! LINENUM: 41.0 TARGNAME: HD50337 CONFIG: HRS OPMODE: IMAGE APERTURE: 2.0 SP_ELEMENT: MIRROR-N2 NUM_EXP: 1 TIME_PER_EXP: 51.2S PRIORITY: 1 PARAM_1: NX=16, PARAM_2: NY=16, PARAM_3: DELTA-X=4, PARAM_4: DELTA-Y=4 COMMENT_1: STEP-TIME=0.2S ! LINENUM: 42.0 SEQUENCE_1: USE SEQUENCE_2: HR2554A ! LINENUM: 80.0 TARGNAME: HD50337 CONFIG: HRS OPMODE: ACQ APERTURE: 2.0 SP_ELEMENT: MIRROR-A2 NUM_EXP: 1 TIME_PER_EXP: 9S PRIORITY: 1 PARAM_1: BRIGHT=RETURN, PARAM_2: SEARCH-SIZE=3 FLUXNUM_1: 1 FLUXNUM_2: 2 REQ_1: CYCLE 4 / 80-82; REQ_2: ONBOARD ACQ FOR 81-82; REQ_3: GROUP 80-82 NO GAP; REQ_4: AT JD2449854.2 +/- 0.3D COMMENT_1: STEP-TIME = 1 SEC COMMENT_2: EXPECT 1300 CT/S WITH A2 NORMALLY. COMMENT_3: PHASE IS 3 DAYS AFTER MID-ECLIPSE ! LINENUM: 81.0 TARGNAME: HD50337 CONFIG: HRS OPMODE: IMAGE APERTURE: 2.0 SP_ELEMENT: MIRROR-N2 NUM_EXP: 1 TIME_PER_EXP: 51.2S PRIORITY: 1 PARAM_1: NX=16, PARAM_2: NY=16, PARAM_3: DELTA-X=4, PARAM_4: DELTA-Y=4 COMMENT_1: STEP-TIME=0.2S ! LINENUM: 82.0 SEQUENCE_1: USE SEQUENCE_2: HR2554A ! ! end of exposure logsheet ! No scan data records found