! $Id: 5359,v 6.1 1994/07/27 17:04:06 pepsa Exp $ coverpage: title_1: SPECTRA AND CHROMOSPHERES OF CARBON AND M STARS - CYCLE4 MEDIUM sci_cat: COOL STARS sci_subcat: STELLAR ATMOSPHERES proposal_for: GO pi_fname: KENNETH pi_mi: G. pi_lname: CARPENTER pi_inst: NASA GODDARD LASP pi_country: USA hours_pri: 5.00 num_pri: 1 fos: Y hrs: Y funds_amount: 100163 funds_length: 12 off_fname: STEPHEN off_mi: S. off_lname: HOLT off_title: DIR. OF SPACE SCI. off_inst: 2856 off_addr_1: CODE 600 off_city: GREENBELT off_state: MD off_zip: 20771 off_country: USA off_phone: (301)-286-6066 ! end of coverpage abstract: line_1: We propose to use the Faint Object Spectrograph (FOS) and the line_2: Goddard High-Resolution Spectrograph (GHRS) on the HST line_3: to obtain ultraviolet spectra of visually bright N-type line_4: carbon stars and late M-giant stars. These spectra, obtainable only line_5: with HST, will be used with theoretical models to infer the line_6: temperature and density structure and the velocity fields of the line_7: outer atmosphere in these evolutionarily advanced, non-mira line_8: giants. In anticipation of this effort, we have already pushed IUE line_9: to its limit to obtain both low-resolution, and, where possible, line_10: high-resolution spectra of several M, S, and C stars, and these line_11: have been analyzed and published. Based upon the observed line line_12: profiles and continua, we will construct semi-empirical non-LTE models line_13: in both plane-parallel geometry and spherical geometry, including line_14: velocity fields, by attaching a chromosphere to theoretical line_15: photospheric models. Two-component models will be studied. line_16: Using these and ab-initio hydrodynamic models, we will examine line_17: the mechanisms responsible for chromospheric heating and mass line_18: loss. A full range of supporting ground-based observations line_19: will be undertaken to permit us to connect models of the photospheres, line_20: chromospheres, and circumstellar shells. ! ! end of abstract general_form_proposers: lname: CARPENTER fname: KENNETH title: PI mi: G. inst: NASA GODDARD LASP country: USA ! lname: JOHNSON fname: HOLLIS mi: R. inst: INDIANA UNIVERSITY country: USA ! lname: ALEXANDER fname: DAVID mi: R. inst: WICHITA STATE UNIVERSITY country: USA ! lname: AVRETT fname: EUGENE mi: H. inst: SMITHSONIAN ASTROPHYSICAL OBSERVATORY country: USA ! lname: BROWN fname: ALEXANDER inst: U.COLORADO JILA country: USA ! lname: ERIKSSON fname: KJELL inst: UPPSALA ASTRONOMICAL OBSERVATORY country: SWEDEN esa: Y ! lname: GUSTAFSSON fname: BENGT inst: UPPSALA ASTRONOMICAL OBSERVATORY country: SWEDEN esa: Y ! lname: JORGENSEN fname: UFFE mi: G. inst: NIELS BOHR INSTITUTE country: DENMARK esa: Y ! lname: JUDGE fname: PHILIP mi: D. inst: HIGH ALTITUDE OBSERVATORY country: USA ! lname: LINSKY fname: JEFFREY mi: L. inst: U.COLORADO JILA country: USA ! lname: LUTTERMOSER fname: DONALD mi: G. inst: COMPUTER SCIENCES CORPORATION country: USA ! lname: QUERCI fname: FRANCOIS inst: OBSERVATOIRE MIDI PYRENEES, TOULOUSE country: FRANCE esa: Y ! lname: QUERCI fname: MONIQUE inst: OBSERVATOIRE MIDI PYRENEES, TOULOUSE country: FRANCE esa: Y ! lname: ROBINSON fname: RICHARD mi: D. inst: COMPUTER SCIENCES CORPORATION country: USA ! lname: WING fname: ROBERT mi: F. inst: OHIO STATE UNIVERSITY country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: The mid-UV spectrum of TW Hor (HD20234) will be surveyed with line_2: FOS/G270H and the Mg II region will be observed at R=20000 line_3: resolution with GHRS. 30 Her (HD148783) will be observed line_4: with the GHRS/G270M with frames centered at 2810, 2345, line_5: and 2850 A. line_13: The proposed new observations are pure Cycle 4: line_15: Primary Hours: Parallel Hours: Exposures: line_16: 5.0 0.0 ****** ! question: 4 section: 1 line_1: To understand mass loss and to model the outer atmospheres (including line_2: chromospheres and circumstellar layers) require detailed profiles of line_3: key spectral lines, which in turn requires high-resolution ultraviolet line_4: spectra. We have pushed IUE to its limit. That effort has produced line_5: low-resolution LWP/LWR spectra of the brighter R stars of all classes, line_6: a few brighter N-type stars, and several late M giant stars. line_7: High-resolution spectra have been obtained in long exposures for a few line_8: bright early-R stars and a few bright M giant stars. A 13-hour line_9: high-resolution LWP exposure of the best N-type star (TX Psc) was line_10: considerably underexposed and showed clearly only the Mg II emission line_11: lines while a few other lines were weakly present (Eriksson et al. line_12: 1986). To make further progress, it is absolutely necessary to use line_13: HST. ! question: 5 section: 1 line_1: Narrow-band photometry and calibrated spectra will be obtained from the line_2: ground at approximately the same time to determine the properties of line_3: the underlying photosphere and the CSE. ! question: 6 section: 1 line_1: Wavelength calibration exposures on the internal Pt-lamps are requested line_2: for each GHRS exposure since we require the highest possible wavelength line_3: accuracy in order to measure flow velocities in the chromospheres and line_4: circumstellar shells of our target stars. ! ! ! ! question: 8 section: 1 line_1: none ! question: 9 section: 1 line_1: a. List HST program numbers and titles, and specify whether they are line_2: related to this project or not. line_4: HST GTO Programs on which Carpenter is PI: line_6: GTO 1195: Outer Atmospheres of Cool Luminous Stars - Cycle 0 (Alpha Ori) line_7: 3212: Outer Atmospheres of Cool Luminous Stars - Cycle 1 (Gamma Cru) line_9: GTO 1198: Physical Conditions and Velocity Structures in the Red Giant line_10: 3934: Winds in the Binaries CI Cyg and EG And - Cycle 2 (2 targets) line_12: GTO 1199: Alpha Ori Team Project - Cycle 1 line_14: HST GTO programs on which Linsky is PI: line_16: GTO 1175/3943: Local Interstellar Medium and D/H Ratio line_18: GTO 1176/3964: The dynamics of stellar chromospheres & transition regions line_20: GTO 1177: Atmospheres of very inactive K giant stars line_22: GTO 1179/3961: Hybrid-chromosphere stars line_23: GTO Program 1180: The chromospheres of the very coolest M dwarf stars ! question: 9 section: 2 line_1: HST Programs on which Linsky and/or Carpenter are Co-I's: line_3: GTO 1210: Age dependence of non-radiative heating in stellar line_4: chromospheres line_6: GO 2238: Lyman-ALPHA Observations Of High Radial Velocity Stars line_8: GO 2321: Search for proton acceleration in flare stars - AU Mic line_10: GO 3626: Empirical determination of the wind velocity and density laws line_11: for the K supergiant Zeta Aurigae from eclipse ingress spectra line_13: HST programs on which Gustafsson is Co-I: line_14: GO P3479: Boron in Pop II Dwarfs line_16: THERE ARE NO OBSERVATIONS OF CARBON STARS IN THESE GTO PROGRAMS. line_18: The only M-giant included in these GTO programs is Gamma Cru, in GTO line_19: 3212 - a cycle 1 program which executed late in that cycle. The line_20: observations cover a broader range of wavelengths and purposes than line_21: those planned for the M-stars in this GO proposal, but they do not line_22: include a satisfactory match to the carbon-star observations for our line_23: detailed comparison purposes. ! question: 9 section: 3 line_1: SAO program 3023 (Alpha Tau) observations have been used to assess the line_2: feasibility of programs such as these which involve observations of line_3: narrow emission-line sources (see the Ap.J. reference below). line_6: b. Summarize the main results obtained from previous related programs. line_8: The observations of Alpha Tauri in SAO 3023 provided the first direct line_9: measurment of the turbulence in the chromosphere of a cool giant (K5 line_10: III), the discovery of a downflow of the C II] chromospheric plasma, line_11: the detection of 25 new emission features in the 2320-2370 A region, line_12: and the first evidence for optically thin emission lines (of CII 2325A) line_13: that have extended wings. Other results are summarized in the papers line_14: listed in part (c). line_16: Highlights of Carpenter GTO (Programs 1195/3212) and SAO results line_17: include: 1) the unambiguous detection of a far-UV continuum in Alpha line_18: Ori and Gamma Cru, which will provide a very important and previously line_19: unrecognized diagnostic of their chromospheric plasmas (formation line_20: temperature in alpha Ori ranges from 3500-5000 K and increases steadily line_21: with decreasing wavelength); 2) the discovery of circumstellar CO (4th line_22: positive A-X system) absorption bands superposed on the far-UV line_23: continuum from Alpha Ori, providing a probe of regions of the ! question: 9 section: 4 line_1: circumstellar shell not available at visible or IR wavelengths (initial line_2: analysis indicates T=500 K, Vturb=5 km/s, N(CO)=1.0e18 cm-2); 3) line_3: detection of myriad new Fe II fluorescent line products, producing by line_4: Lyman Alpha radiation in Alpha Ori; 4) a determination that, in Alpha line_5: Ori, the resonance lines of OI and CI are very weak due to line_6: self-absorption and that the asymmetries seen in the MgII resonance line_7: lines are probably due to different velocity shifts between the line_8: self-absorption and emission in the two lines; and 5) the first direct line_9: measurement of the chromospheric turbulence (24 km/sec) and the line_10: detection of a downflow of about 4 km/sec in chromospheric C II] plasma line_11: in Alpha Tau. High quality observations of Gamma Cru in program 3212 line_12: have recently been acquired and detailed analysis is now in progress. line_14: GTO Program 1175: Linsky and collaborators obtained SSA echelle spectra line_15: of Capella in the Lyman alpha, FeII, and MgII lines on 15 April 1991. line_16: The purpose was to obtain very accurate measurements of the D/H ratio line_17: and interstellar properties for the 12.5-pc line of sight towards this line_18: star. They derived the ratio D/H = 1.65 (+0.07 -0.18) x 10c{-5}, line_19: temperature 7000 (+/- 200) K, and turbulent velocity of 1.66 (+/-0.03) line_20: km/s. The local D/H ratio was used to infer the primordial value which line_21: is a major constraint on models of the early universe. Observations of line_22: Alpha Cen A and B, Procyon, HR 1099, and a reobservation of Capella are line_23: planned. ! question: 9 section: 5 line_1: GTO Program 1176: Low and moderate dispersion GHRS spectra of Capella line_2: were obtained on 15 April 1991 and of Beta Draconis on 23 April 1992. line_3: The Capella observations show downflowing transition region gas from line_4: both stars in the system and intersystem lines of many different ions line_5: that allow the determination of the electron density as a function of line_6: the temperature of the emissing plasma. Observations of Procyon, line_7: Epsilon Eri, HR 1099, and Alpha Cen A and B are planned. The Beta line_8: Draconis data are being analyzed. line_10: SV observations of Gamma Draconis obtained on 6 April 1991 by Carpenter line_11: et al. provide clear evidence of such high temperature lines as CIV and line_12: SIIV in the atmosphere of this hybrid-chromosphere star. The surface line_13: fluxes in the 100,000 K plasma lines are the smallest ever observed in line_14: any star. line_16: GO Program 2321: Evidence for proton beams was obtained by Woodgate et line_17: al. from GHRS spectra of AU Mic during a flare. This discovery was line_18: described in a recent NASA press release and in an ApJ paper. line_20: There have been no observations yet in any of the other programs. ! question: 9 section: 6 line_1: c. List publications resulting from the above data (Format: Title, line_2: Authors,Journal, Volume, Page, and Year.) line_4: Results have been presented: in the Ap.J. & MNRAS, at AAS meeting (1/91, 5/91 line_5: & 1/92), the HST Joint Discussion at the IAU General Assembly (7/91), the 7th line_6: Cambridge Cool Star Workshop (10/91), and at both HST Workshops (5/91 & 7/92), line_7: including two invited reviews (AAS 1/91 and Cool Star Workshop 10/91). line_9: "GHRS Observations of Cool, Low-Gravity Stars. I. The Far-UV Spectrum of line_10: Alpha Ori (M2 Iab)", Carpenter, K., Robinson, R., Wahlgren, G., Linsky, J., line_11: and Brown, A., 1993 Ap.J., submitted. line_13: "First Results from the Goddard High Resolution Spectrograph: The Chromosphere line_14: of Alpha Tauri", Carpenter, K. G., Robinson, R., Wahlgren, G., Ake, T., Linsky, line_15: J., Brown, A., and Walter, F., Ap.J. (Letters), 377, L45, 1991. line_17: "Si II Emission Line Diagnostics," Judge, P. G., Carpenter, K. G., and line_18: Harper, G.M., MNRAS, 253, 123, 1991. line_20: "Early Scientific Results from the Goddard High Resolution Spectrograph" line_21: Carpenter, K. G. , Invited Review presented at the AAS Meeting, 1/13-17/91. ! question: 9 section: 7 line_1: "GHRS Chromospheric Emission Line Spectra of the Red Giant Alpha Tau" line_2: Carpenter, K. G., Robinson, R. D., Ebbets, D. C., Brown, A., and Linsky, J., line_3: in `The First Year of HST Observations,' 1991. line_5: "Chromospheres and Winds of Cool Stars", Carpenter, K.G., IAU General Assembly line_6: Joint Discussion, 'First Results from the Hubble Space Telescope', 7/31/91. line_8: "HST Observations of Late-Type Stars," (Invited Review) Carpenter, K. G., in line_9: `Proceedings of the 7th Cambridge Workshop on Cool Stars, Stellar Systems, and line_10: the Sun,' in press, 1992. line_12: "Molecular Absorption in the UV Spectrum of Alpha Ori," Wahlgren, G. M., line_13: Robinson, R. D., and Carpenter, K. G., Proceedings of the Seventh line_14: Cambridge Workshop on Cool Stars, Stellar Systems and the Sun, ed. M. Giampapa line_15: and J. Bookbinder, A.S.P. Conference Series, in press, 1992. line_17: "The Chromosphere and Circumstellar Shell of Alpha Orionis as Observed with the line_18: Goddard High Resolution Spectrograph," Carpenter, K. G., Robinson, R. D., line_19: Wahlgren, G. M., Linsky, J. L., Brown, A., in Science with the Hubble line_20: Space Telescope (European Southern Observatory), eds. P. Benvenuti and line_21: E. Schreier, in press, 1992. ! question: 9 section: 8 line_1: "The Far-UV Spectrum of alpha Ori," Carpenter, K. G., Robinson, R. D., line_2: Wahlgren, G. M., Linsky, J.L., and Brown, A., Ap. J., submitted, 1992. line_4: `GHRS observations of the local interstellar medium and the deuterium/hydrogen line_5: ratio along the line of sight towards Capella,' Linsky, J.L., Brown, A., line_6: Gayley, K., Diplas, A., Savage, B. D., Ayres, T. R., Landsman, W., Shore, S., line_7: and Heap, S. R., Astrophysical Journal, to appear 10 Jan 1993. line_9: `The hydrogen Lyman alpha emission of Capella', Ayres, T.R., Brown, A., Gayley, line_10: K.G., and Linsky, J.L., Astrophysical Journal, to appear 10 Jan 1993. line_13: `GHRS Far-ultraviolet spectra of coronal and noncoronal stars: Capella and line_14: Gamma Draconis', Linsky, J.L., Brown, A., and Carpenter, K.G., in The First line_15: Year of HST Observations, ed. A.L. Kinney and J.C. Blades (Baltimore: Space line_16: Telescope Science Institute), p. 70 (1991). line_18: `The Deuterium abundance in the local interstellar medium', Linsky, J.L.to line_19: appear in Highlights of the IAU, Vol. 9. line_21: `Ultraviolet observations of stellar coronae: early results from HST', Linsky, line_22: J.L., to appear in Memorie della Societa Astronomica Italiana. line_23: (plus others) ! question: 10 section: 1 line_1: Indiana University (I.U.) has been very generous in providing much time line_2: on its computing facilities. Programs, data, and facilities for line_3: computing model atmospheres are in use at I.U., Wichita, Copenhagen, line_4: Toulouse, and Uppsala. Programs for constructing non-LTE model line_5: chromospheres are available at HAO, JILA, Iowa St., GSFC, and line_6: Smithsonian. Radio and optical telescopes for concurrent observations line_7: are available in Sweden, France, ESO-La Silla, and the United States line_8: (Ohio State U.). Software developed by the GHRS IDT will be available line_9: at NASA-GSFC, as well as VAX computing facilities, for reduction and line_10: measurement of GHRS and FOS spectra. ! !end of general form text general_form_address: lname: CARPENTER fname: KENNETH mi: G. category: PI inst: NASA Goddard LASP addr_1: CODE 681 addr_2: NASA/GSFC - LAB. FOR ASTRONOMY AND SOLAR PHYSICS city: GREENBELT state: MD zip: 20771 country: USA phone: (301)-286-3453 telex: 89675 ! ! end of general_form_address records fixed_targets: targnum: 2 name_1: HD20234 name_2: TW-HOR descr_1: A,144 pos_1: RA=03H12M33.15S+/-1.0", pos_2: DEC=-57D19'17.83"+/-1.0" equinox: 2000.0 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 2000.00 ra_pm_val: 0.002000 ra_pm_unct: 0.001000 dec_pm_val: 0.0090 dec_pm_unct: 0.0010 rv_or_z: V=+14 comment_1: (N0; C7,2) CARBON STAR comment_2: PM(RA) IN SEC-OF-TIME/YR fluxnum_1: 1 fluxval_1: V=5.74,TYPE=NOC72 ! targnum: 3 name_1: HD148783 name_2: 30_HER descr_1: A,144 pos_1: RA=16H28M38.55S+/-1.0", pos_2: DEC=+41D52'53.74"+/-1.0" equinox: 2000.0 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 2000.00 ra_pm_val: 0.003000 ra_pm_unct: 0.001000 dec_pm_val: -0.0090 dec_pm_unct: 0.0010 rv_or_z: V=+3 comment_1: M6 III OXYGEN-RICH STAR comment_2: PM(RA) IN SEC-OF-TIME/YR fluxnum_1: 1 fluxval_1: V=5.04,TYPE=M6III ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: HD20234 config: FOS/RD opmode: ACQ/PEAK aperture: 4.3 sp_element: G270H wavelength: 2750 num_exp: 1 time_per_exp: 1.0S priority: 1 param_1: SCAN-STEP-Y=1.204, param_2: SEARCH-SIZE-X=1, param_3: SEARCH-SIZE-Y=3, req_1: CYCLE 4 / 1.0-42.0; req_2: ONBOARD ACQ FOR 1.1; req_3: SEQ 1-2 NO GAP; req_4: GROUP 1-6 WITHIN 2D comment_1: TW HOR IS COMMON NAME OF OBJECT. comment_2: EXPECT 8500 CTS/TIME INTERVAL. ! linenum: 1.100 targname: HD20234 config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: G270H wavelength: 2750 num_exp: 1 time_per_exp: 1.0S priority: 1 param_1: SCAN-STEP-X=.602, param_2: SCAN-STEP-Y=.602, param_3: SEARCH-SIZE-X=6, param_4: SEARCH-SIZE-Y=2, req_1: ONBOARD ACQ FOR 1.2 ! linenum: 1.200 targname: HD20234 config: FOS/RD opmode: ACQ/PEAK aperture: 0.3 sp_element: G270H wavelength: 2750 num_exp: 1 time_per_exp: 2.0S priority: 1 param_1: SCAN-STEP-X=.172, param_2: SCAN-STEP-Y=.172, param_3: SEARCH-SIZE-X=5, param_4: SEARCH-SIZE-Y=5, req_1: ONBOARD ACQ FOR 2 ! linenum: 2.000 targname: HD20234 config: FOS/RD opmode: ACCUM aperture: 4.3 sp_element: G270H wavelength: 2750 num_exp: 4 time_per_exp: 5.0M priority: 1 ! linenum: 3.000 targname: HD20234 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 40.0S fluxnum_1: 1 priority: 1 param_1: LOCATE=YES, param_2: BRIGHT=RETURN, param_3: SEARCH-SIZE=5 req_1: ONBOARD ACQ FOR 4.000; req_2: SEQ 3 - 6 comment_1: USE STEP-TIME = 1.6 SEC. comment_2: EXPECT ROUGHLY 1400 CTS/1.6S ! linenum: 4.000 targname: HD20234 config: HRS opmode: ACQ/PEAKUP aperture: 0.25 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 40S fluxnum_1: 1 priority: 1 param_1: SEARCH-SIZE=5, req_1: ONBOARD ACQ FOR 5.0-6.0 comment_1: STEP-TIME = 1.6 SEC comment_2: EXP TIME ASSUMES 5X5 SEARCH ! linenum: 5.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G270M wavelength: 2810 num_exp: 1 time_per_exp: 30S priority: 1 param_1: STEP-PATT=3 req_1: CALIB FOR 6 NO SLEW; req_2: SEQ 5-6 NO GAP ! linenum: 6.000 targname: HD20234 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G270M wavelength: 2810 num_exp: 2 time_per_exp: 20.0M s_to_n: 0 priority: 1 param_1: STEP-PATT=5, param_2: FP-SPLIT=STD ! linenum: 33.000 targname: HD148783 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 25.0S fluxnum_1: 1 priority: 1 param_1: LOCATE=YES, param_2: BRIGHT=RETURN, param_3: SEARCH-SIZE=5 req_1: ONBOARD ACQ FOR 34.000; req_2: SEQ 33 - 35; req_3: GROUP 33 - 42 WITHIN 1D comment_1: 30 HER IS COMMON NAME FOR HD148783 comment_2: STEP-TIME = 1.0 SEC. comment_3: EXPECT 4500 CTS/1.0 SEC ! linenum: 34.000 targname: HD148783 config: HRS opmode: ACQ/PEAKUP aperture: 0.25 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 25S fluxnum_1: 1 priority: 1 param_1: SEARCH-SIZE=5, req_1: ONBOARD ACQ FOR 35.0-42.0 comment_1: STEP-TIME = 1.0 SEC comment_2: EXP TIME ASSUMES 5X5 SEARCH ! linenum: 35.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G270M wavelength: 2810 num_exp: 1 time_per_exp: 30S priority: 1 param_1: STEP-PATT=3 req_1: CALIB FOR 36 NO SLEW; req_2: SEQ 35-36 NO GAP ! linenum: 36.000 targname: HD148783 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G270M wavelength: 2810 num_exp: 1 time_per_exp: 20.0M priority: 1 param_1: STEP-PATT=5, param_2: FP-SPLIT=STD ! linenum: 37.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G270M wavelength: 2345 num_exp: 1 time_per_exp: 30S priority: 1 param_1: STEP-PATT=3 req_1: CALIB FOR 38 NO SLEW; req_2: SEQ 37-38 NO GAP ! linenum: 38.000 targname: HD148783 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G270M wavelength: 2345 num_exp: 2 time_per_exp: 22.0M s_to_n: 10 priority: 1 param_1: STEP-PATT=5, param_2: FP-SPLIT=STD ! linenum: 41.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G270M wavelength: 2850.0 num_exp: 1 time_per_exp: 30S priority: 1 param_1: STEP-PATT=3 req_1: CALIB FOR 42 NO SLEW; req_2: SEQ 41-42 NO GAP ! linenum: 42.000 targname: HD148783 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G270M wavelength: 2850.0 num_exp: 1 time_per_exp: 20.0M s_to_n: 10 priority: 1 param_1: STEP-PATT=5, param_2: FP-SPLIT=STD ! ! end of exposure logsheet ! No scan data records found