coverpage: title_1: SPECTRA AND CHROMOSPHERES OF CARBON AND M STARS - CYCLE 4 CARRYOVER sci_cat: COOL STARS sci_subcat: STELLAR ATMOSPHERES proposal_for: GO/CAR cont_id: 4685 pi_fname: HOLLIS pi_mi: R. pi_lname: JOHNSON pi_inst: INDIANA UNIVERSITY pi_country: USA hours_pri: 7.18 num_pri: 1 fos: N hrs: Y funds_length: 24 off_fname: GEORGE off_mi: E. off_lname: WALKER off_title: ASSOC. V. PRESIDENT off_inst: 2270 off_addr_1: RESEARCH & UNIVERSITY GRADUATE SCHOOL off_addr_2: BRYAN HALL, ROOM 104 off_city: BLOOMINGTON off_state: IN off_zip: 47405 off_country: USA off_phone: (812)-855-6153 ! end of coverpage abstract: line_1: We propose to use the Goddard High-Resolution line_2: Spectrograph (GHRS) on the HST to obtain ultraviolet line_3: spectra of the visually bright N-type carbon star line_4: TX Psc. These spectra, obtainable only with HST, will line_5: be used with theoretical models to infer the density and line_6: temperature 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 pushed IUE line_9: to its limit to obtain a weak high-resolution spectra of line_10: this star, and observations of a second carbon star (UU Aur) with HST are being line_11: analyzed. Based upon the observed line profiles and line_12: 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: JOHNSON fname: HOLLIS title: PI 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: CARPENTER fname: KENNETH mi: G. inst: NASA GODDARD LASP 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: IOWA STATE UNIVERSITY 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: Part a) line_2: High-resolution spectra of the bright N-type carbon star (TX line_3: Psc: N0, C6,2) will be obtained using the HST G270M mode line_4: in three spectral regions centered on 2345 A (C II]), 2754 line_5: A (Fe II), and 2810 A (Mg II). line_8: line_9: The exposure times are summarized in Section 4. line_13: The project is pure Cycle 3: line_14: Primary Hours: Parallel Hours: Exposures: line_15: 7.18 0.0 3 line_17: Part b) line_18: N/A ! question: 4 section: 1 line_1: Part a) line_2: To understand mass loss and to model the outer atmospheres (including line_3: chromospheres and circumstellar layers) require detailed profiles of key line_4: spectral lines, which in turn requires high-resolution ultraviolet spectra. We line_5: have pushed IUE to its limit. That effort has produced low-resolution LWP/LWR line_6: spectra of the brighter stars of all spectral classes, including carbon line_7: stars. A 13-hour high-resolution LWP exposure of the best N-type star (TX Psc) line_8: was considerably underexposed and showed clearly only the Mg II emission lines line_9: while a few other lines were weakly present (Eriksson et al. 1986). To make line_10: further progress, it is absolutely necessary to use HST. We have already line_11: obtained FOS medium-resolution spectra of the line_12: carbon star UU Aur (N3: C5,3) and one high-resolution spectrum in the line_13: region of the Mg II lines at 2800 A. These are far superior to any line_14: previously obtained and confirm the necessity for high-resolution line_15: observations, especially in other wavelength regions. line_16: Narrow-band photometry and calibrated spectra will be obtained line_17: at approximately the same time to determine the properties of the underlying line_18: photosphere and the CSE. ! question: 4 section: 2 line_1: Part b) line_2: Summary of Exposure Times line_4: Exposure GHRS Time/ line_5: Target Factor G270M/CII G270M/FeII G270M/MgII Star line_7: TX Psc 1.0 - - line_8: line_11: line_14: subtotal 3.00 1.60 0.75 5.35 line_16: The total exposure time is 5.35 hours. line_17: The number of targets is 1. line_18: The number of wavelength settings is 3. line_19: The GHRS 0.25x0.25 arcsec science apertures are used. line_21: The exposure times for TX Psc are derived using fluxes from IUE observations line_22: taken during 1981, when the star was in a "low" state, to ensure that we obtain line_23: at least the minimum desired S/N of 20. If the star is brighter at the time ! question: 4 section: 3 line_1: of the HST observations, we will be delighted to achieve a higher S/N. line_2: line_3: line_4: We require the use of the GHRS small aperture line_5: to preserve the design spectral resolution and the true line profiles. line_6: Monochromatic peak line fluxes, as measured in IUE low-resolution spectra of line_7: TX Psc are: line_8: C II 2325 A Al II 2670 Fe II 2750 A Mg II 2800 A line_9: ----------- ----------- ------------ ------------ line_10: 4.0e-15 3.0e-15 5.0e-15 2.0e-14 ergs/cm2/s/A line_12: The PEAK S/N achieved in the GHRS observations will be higher than predicted line_13: using these figures directly, since, unlike IUE, GHRS will resolve the lines. line_14: The GHRS exposure times have been checked using the new sensitivities in the line_15: Cycle 3 handbook, modified to account for the improved GHRS SSA sensitivity line_16: recently achieved with an improved centering of targets in the GHRS SSA. line_17: line_18: line_20: The total estimated spacecraft time = 7.18 hours ! question: 5 section: 1 line_1: Wavelength calibration exposures on the internal Pt-lamps are requested for line_2: each GHRS exposure since we require the highest possible wavelength accuracy line_3: in order to measure flow velocities in the chromospheres and circumstellar line_4: shells of our target stars. ! question: 6 section: 1 line_1: Special Calibration Requirement(s) line_2: __________________________________ line_3: Wavelength calibrations at each GHRS line_4: grating setting (no motion of line_5: carrousel between science and line_6: calibration exposure) are required to line_7: obtain the required wavelength/velocity precision. ! question: 7 section: 1 line_1: To support the important HST observations several types of concurrent line_2: ground-based observations will be made. (1) The Swedish wing of the team will line_3: make radio observations of circumstellar gas through CO and HCN lines line_4: (Olofsson, et al., 1993 Ap. J. Supp. 87, 267) and high-resolution (120,000) line_5: spectroscopic observations of CS matter in the Na D and K I resonance lines line_6: with the new HRS at the Nordic Optical 2.5-m telescope at La Palma. (2) the line_7: French and Ohio State groups will make concurrent ground-based, high-resolution line_8: spectra in the visual region and ultraviolet regions. We have already line_9: obtained spectra of the CO fundamental lines in TX Psc, and we hope to line_10: obtain similar spectra for the other stars. line_11: The analysis will proceed in several steps. line_12: (1) The initial data reduction, calibration, and analysis of the observations line_13: will be done by the GSFC/CSC group (Carpenter, Robinson). The raw data files line_14: will be wavelength-calibrated using the explicit WAVE observations obtained line_15: along with the science data and transformed onto an absolute flux scale using line_16: the latest radiometric calibration of the GHRS. Software and techniques line_17: developed by the GHRS IDT will be used to optimize these calibrations. Copies line_18: of both the raw and calibrated spectra will then be sent to all investigators, line_19: and analysis will proceed through parallel and cooperative, independent line_20: ventures. ! question: 7 section: 2 line_1: (2) The GSFC/CSC group will perform the initial measurement and analysis of the line_2: UV data, obtaining observed wavelengths, line widths, and detailed line line_3: profiles. From these results we will infer the turbulent and flow velocities line_4: and velocity gradients in the stellar chromosphere and wind. This information line_5: will be combined with velocities from visual and radio observations and line_6: deductions from the mass-loss rate and mass continuity to yield as complete a line_7: picture as possible of the velocity structure of the photospheric, line_8: chromospheric, and CS regions. The GSFC/CSC, Boulder, Swedish, and Ohio State line_9: groups will participate. line_10: (3) Photospheric models, including polyatomic molecular opacities, in both line_11: plane-parallel and spherical geometry, will be computed for both carbon stars line_12: and M stars by the Midwest, Danish, French, and Swedish groups. This will line_13: include experimentation with two-component models. The SAO group will make line_14: detailed comparisons of synthetic spectra with visual observations, and the line_15: Danish and Swedish groups will do the same in the red and infrared regions. line_16: (4) Careful modeling of the chromospheric temperature structure will be line_17: undertaken, beginning with a carbon star. (However, to compute line_18: inhomogeneous NLTE models for both C and M stars will surely require line_19: several years.) A best theoretical photosphere-chromosphere model (including line_20: departures from LTE) will be selected by comparison of predicted fluxes with line_21: observations of both lines and continua. The Boulder, Indiana, Iowa State, ! question: 7 section: 3 line_1: Goddard, and Smithsonian groups currently possess the necessary programs for line_2: NLTE chromospheric modeling, and these groups will work in parallel and in line_3: collaboration in checking NLTE results in this extremely complex research. line_4: (5) At Smithsonian synthetic spectra in the visual and ultraviolet line_5: regions will be calculated and carefully compared to observations. line_6: Comparisons of capacities in red giants and the sun will be made. line_7: (6) Results will be published in a timely fashion. ! question: 8 section: 1 line_1: line_2: None. ! question: 9 section: 1 line_1: part a) line_2: HST GTO Programs on which Carpenter is PI: line_4: GTO 1195: Outer Atmospheres of Cool Luminous Stars - Cycle 0 (Alpha Ori) line_5: 3212: Outer Atmospheres of Cool Luminous Stars - Cycle 1 (Gamma Cru) line_7: GTO 1198: Physical Conditions and Velocity Structures in the Red Giant line_8: 3934: Winds in the Binaries CI Cyg and EG And - Cycle 2 (2 targets) line_10: GTO 1199: Alpha Ori Team Project - Cycle 1 line_12: HST GTO programs on which Linsky is PI: line_14: GTO 1175/3943: Local Interstellar Medium and D/H Ratio line_16: GTO 1176/3964: The dynamics of stellar chromospheres & transition regions line_18: GTO 1177: Atmospheres of very inactive K giant stars line_20: GTO 1179/3961: Hybrid-chromosphere stars line_22: 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_2: : line_3: GTO 1210: Age dependence of non-radiative heating in stellar chromospheres line_5: GO 2238: Lyman-ALPHA Observations Of High Radial Velocity Stars line_7: GO 2321: Search for proton acceleration in flare stars - AU Mic line_9: GO 3626: Empirical determination of the wind velocity and density laws line_10: for the K supergiant Zeta Aurigae from eclipse ingress spectra line_12: 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 3212 - a line_19: cycle 1 program which executed late in that cycle. The observations cover a line_20: broader range of wavelengths and purposes than those planned for the M-stars in line_21: this GO proposal, but they do not include a satisfactory match to the line_22: carbon-star observations for our 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 narrow line_3: emission-line sources (see the Ap.J. reference below). line_4: Part b) line_5: The observations of Alpha Tauri in SAO 3023 provided the first direct line_6: measurement of the turbulence in the chromosphere of a cool giant (K5 III), the line_7: discovery of a downflow of the C II] chromospheric plasma, the detection of 25 line_8: new emission features in the 2320-2370 A region, and the first evidence for line_9: optically thin emission lines (of CII 2335A) that have extended wings. Other line_10: results are summarized in the papers listed in part (c). line_12: Highlights of Carpenter GTO (Programs 1195/3212) and SAO results include: line_13: 1) the unambiguous detection of a far-UV continuum in Alpha Ori and Gamma Cru, line_14: which will provide a very important and previously unrecognized diagnostic of line_15: their chromospheric plasmas (formation temperature in Alpha Ori ranges from line_16: 3500-5000 K and increases steadily with decreasing wavelength); 2) the line_17: discovery of circumstellar CO (4th positive A-X system) absorption bands line_18: superposed on the far-UV continuum from Alpha Ori, providing a probe of regions line_19: of the circumstellar shell not available at visible or IR wavelengths (initial line_20: analysis indicates T=500 K, Vturb=5 km/s, N(CO)=1.0e18 cm-2); 3) detection of line_21: myriad new Fe II fluorescent line products, producing by Lyman Alpha radiation line_22: in Alpha Ori; 4) a determination that, in Alpha Ori, the resonance lines of OI line_23: and CI are very weak due to self-absorption and that the asymmetries seen in ! question: 9 section: 4 line_1: the MgII resonance lines are probably due to different velocity shifts between line_2: the self-absorption and emission in the two lines; and 5) the first direct line_3: measurement of the chromospheric turbulence (24 km/sec) and the detection of a line_4: downflow of about 4 km/sec in chromospheric C II] plasma in Alpha Tau. High line_5: quality observations of Gamma Cru in program 3212 have recently been acquired line_6: and detailed analysis is now in progress. line_8: GTO Program 1175: Linsky and collaborators obtained SSA echelle spectra of line_9: Capella in the Lyman alpha, FeII, and MgII lines on 15 April 1991. The purpose line_10: was to obtain very accurate measurements of the D/H ratio and interstellar line_11: properties for the 12.5-pc line of sight towards this star. They derived the line_12: ratio D/H = 1.65 (+0.07 -0.18) x 10e-5, temperature 7000 (+/- 200) K, and line_13: turbulent velocity of 1.66 (+/-0.03) km/s. The local D/H ratio was used to line_14: infer the primordial value which is a major constraint on models of the early line_15: universe. Observations of Alpha Cen A and B, Procyon, HR 1099, and a line_16: reobservation of Capella are planned. line_18: GTO Program 1176: Low and moderate dispersion GHRS spectra of Capella were line_19: obtained on 15 April 1991 and of Beta Draconis on 23 April 1992. The Capella line_20: observations show downflowing transition region gas from both stars in the line_21: system and intersystem lines of many different ions that allow the line_22: determination of the electron density as a function of the temperature of the line_23: emitting plasma. Observations of Procyon, Epsilon Eri, HR 1099, and Alpha Cen A ! question: 9 section: 5 line_1: and B are planned. The Beta Draconis data are being analyzed. line_3: SV observations of Gamma Draconis obtained on 6 April 1991 by Carpenter et al. line_4: provide clear evidence of such high temperature lines as CIV and SIIV in the line_5: atmosphere of this hybrid-chromosphere star. The surface fluxes in the 100,000 line_6: K plasma lines are the smallest ever observed in any star. line_8: GO Program 2321: Evidence for proton beams was obtained by Woodgate et line_9: al. from line_10: GHRS spectra of AU Mic during a flare. This discovery was described line_11: in a recent NASA press release and in an ApJ paper. line_13: There have been no observations yet in any of the other programs. line_15: Part c) line_16: Results have been presented: in the Ap.J. & MNRAS, at AAS meeting (1/91, 5/91 line_17: & 1/92), the HST Joint Discussion at the IAU General Assembly (7/91), the 7th line_18: Cambridge Cool Star Workshop (10/91), and at both HST Workshops (5/91 & 7/92), line_19: including two invited reviews (AAS 1/91 and Cool Star Workshop 10/91). line_21: "First Results from the Goddard High Resolution Spectrograph: The Chromosphere line_22: of Alpha Tauri", Carpenter, K. G., Robinson, R., Wahlgren, G., Ake, T., Linsky, line_23: J., Brown, A., and Walter, F., Ap.J. (Letters), 377, L45, 1991. ! question: 9 section: 6 line_1: "Si II Emission Line Diagnostics," Judge, P. G., Carpenter, K. G., and line_2: Harper, G.M., MNRAS, 253, 123, 1991. line_4: "Early Scientific Results from the Goddard High Resolution Spectrograph" line_5: Carpenter, K. G. , Invited Review presented at the AAS Meeting, 1/13-17/91. line_7: "GHRS Chromospheric Emission Line Spectra of the Red Giant Alpha Tau" line_8: Carpenter, K. G., Robinson, R. D., Ebbets, D. C., Brown, A., and Linsky, J., line_9: in `The First Year of HST Observations,' 1991. line_11: "Chromospheres and Winds of Cool Stars", Carpenter, K.G., IAU General Assembly line_12: Joint Discussion, 'First Results from the Hubble Space Telescope', 7/31/91. line_14: "HST Observations of Late-Type Stars," (Invited Review) Carpenter, K. G., in line_15: `Proceedings of the 7th Cambridge Workshop on Cool Stars, Stellar Systems, and line_16: the Sun,' in press, 1992. line_18: "Molecular Absorption in the UV Spectrum of Alpha Ori," Wahlgren, G. M., line_19: Robinson, R. D., and Carpenter, K. G., Proceedings of the Seventh line_20: Cambridge Workshop on Cool Stars, Stellar Systems and the Sun, ed. M. Giampapa line_21: and J. Bookbinder, A.S.P. Conference Series, in press, 1992. ! question: 9 section: 7 line_1: "The Chromosphere and Circumstellar Shell of Alpha Orionis as Observed with the line_2: Goddard High Resolution Spectrograph," Carpenter, K. G., Robinson, R. D., line_3: Wahlgren, G. M., Linsky, J. L., Brown, A., in Science with the Hubble line_4: Space Telescope (European Southern Observatory), eds. P. Benvenuti and line_5: E. Schreier, in press, 1992. line_7: "The Far-UV Spectrum of alpha Ori," Carpenter, K. G., Robinson, R. D., line_8: Wahlgren, G. M., Linsky, J.L., and Brown, A., Ap. J., submitted, 1992. line_10: `GHRS observations of the local interstellar medium and the deuterium/hydrogen line_11: ratio along the line of sight towards Capella,' Linsky, J.L., Brown, A., line_12: Gayley, K., Diplas, A., Savage, B. D., Ayres, T. R., Landsman, W., Shore, S., line_13: and Heap, S. R., Astrophysical Journal, to appear 10 Jan 1993. line_15: `The hydrogen Lyman alpha emission of Capella', Ayres, T.R., Brown, A., Gayley, line_16: K.G., and Linsky, J.L., Astrophysical Journal, to appear 10 Jan 1993. line_18: `GHRS Far-ultraviolet spectra of coronal and noncoronal stars: Capella and line_19: Gamma Draconis', Linsky, J.L., Brown, A., and Carpenter, K.G., in The First line_20: Year of HST Observations, ed. A.L. Kinney and J.C. Blades (Baltimore: Space line_21: Telescope Science Institute), p. 70 (1991). line_23: `The Deuterium abundance in the local interstellar medium', Linsky, J.L.to ! question: 9 section: 8 line_1: appear in Highlights of the IAU, Vol. 9. line_3: `Ultraviolet observations of stellar coronae: early results from HST', Linsky, line_4: J.L., to appear in Memorie della Societa Astronomica Italiana. line_6: `Ultraviolet observations of stellar coronae; early results from the Hubble line_7: Space Telescope', Linsky, J.L., IAU Joint Commission VI on `Solar and Stellar line_8: Coronae', Buenos Aires, Argentina, to be published. line_10: `Deuterium abundance in the local interstellar medium', Linsky, J.L. in IAU line_11: Joint Discussion VII on `First Results from the Hubble Space Telescope', Buenos line_12: Argentina, to be published. line_14: `GHRS observations of the local interstellar medium and the deuterium/hydrogen line_15: ratio toward Capella', Linsky, J.L., in Science with the Hubble Space line_16: Telescope (European Southern Observatory), in press. line_18: `New stellar plasma determinations by the GHRS: The transition regions of line_19: Capella and Gamma Draconis', Linsky, J.L., Wood, B., and Brown, A., in Science line_20: with the Hubble Space Telescope (European Southern Observatory), in press. ! question: 10 section: 1 line_1: Indiana University (I.U.) has been very generous in providing much time on its line_2: computing facilities. Programs, data, and facilities for computing model line_3: atmospheres are in use at I.U., Wichita, Copenhagen, Toulouse, and Uppsala. line_4: Programs for constructing non-LTE model chromospheres are available at HAO, line_5: JILA, Iowa St., GSFC, and Smithsonian. Radio and optical telescopes for line_6: concurrent observations are available in Sweden, France, ESO-La Silla, and the line_7: United States (Ohio State U.). Software developed by the GHRS IDT will be line_8: available at NASA-GSFC, as well as VAX computing facilities, for reduction and line_9: measurement of GHRS and FOS spectra. ! !end of general form text general_form_address: lname: JOHNSON fname: HOLLIS mi: R. category: PI inst: Indiana University addr_1: ASTRONOMY DEPT., SW 319 city: BLOOMINGTON state: IN zip: 47405 country: USA phone: (812)-855-6915 telex: 272-279 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: HD223075 name_2: TX-PSC descr_1: A,144 pos_1: RA=23H46M23.525S+/-1.0", pos_2: DEC=+03D29'12.5"+/-1.0" equinox: 2000.0 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 2000.00 ra_pm_val: -0.002004 ra_pm_unct: 0.000067 dec_pm_val: -0.0250 dec_pm_unct: 0.0010 rv_or_z: V=+11 comment_1: (N0; C6,2) CARBON STAR fluxnum_1: 1 fluxval_1: V=5.04,TYPE=NOC62 fluxnum_2: 2 fluxval_2: F(2799)=2.0E-14 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: ! linenum: 1.000 targname: HD223075 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 2.000; req_2: SEQ 1-8; req_3: CYCLE 4/1-8 comment_1: USE STEP-TIME = 1.6 SEC. comment_2: EXPECT ROUGHLY 640-1120 CTS/1.6S ! linenum: 2.000 targname: HD223075 config: HRS opmode: ACQ/PEAKUP aperture: 0.25 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 60S fluxnum_1: 1 priority: 1 param_1: SEARCH-SIZE=5, req_1: ONBOARD ACQ FOR 3.0-8.0 comment_1: STEP-TIME = 2.4 SEC (FROM SIB) ! linenum: 3.000 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 4 NO SLEW; req_2: SEQ 3-4 NO GAP ! linenum: 4.000 targname: HD223075 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G270M wavelength: 2345 num_exp: 18 time_per_exp: 10.0M s_to_n: 32 fluxnum_1: 2 priority: 1 param_1: STEP-PATT=5, param_2: FP-SPLIT=NO comment_1: S/N IS FOR SUM OF 18 EXP'S. ! linenum: 5.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G270M wavelength: 2754 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: HD223075 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G270M wavelength: 2754 num_exp: 10 time_per_exp: 9.6M s_to_n: 25 fluxnum_1: 2 priority: 1 param_1: STEP-PATT=5, param_2: FP-SPLIT=NO comment_1: S/N IS FOR SUM OF 10 EXP'S. ! linenum: 7.000 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 8 NO SLEW; req_2: SEQ 7-8 NO GAP ! linenum: 8.000 targname: HD223075 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G270M wavelength: 2810 num_exp: 6 time_per_exp: 9.0M s_to_n: 30 fluxnum_1: 2 priority: 1 param_1: STEP-PATT=5, param_2: FP-SPLIT=NO comment_1: S/N IS FOR SUM OF 5 EXP'S. ! ! end of exposure logsheet