! File: 4685C.PROP ! Database: PEPDB ! Date: 22-FEB-1994:22:23:39 coverpage: title_1: SPECTRA AND CHROMOSPHERES OF CARBON AND M STARS - CYC3-HIGH sci_cat: COOL STARS sci_subcat: STELLAR ATMOSPHERES proposal_for: GO pi_fname: HOLLIS pi_mi: R. pi_lname: JOHNSON pi_inst: INDIANA UNIVERSITY pi_country: USA hours_pri: 16.00 num_pri: 3 fos: Y 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 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: 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: Two carbon stars of differing spectral class (TX Psc and UU Aur) line_3: will be surveyed using the FOS G270H mode for the 2220-3300 A region. The Mg line_4: II h&k lines will be observed in the latter star with the G270M GHRS mode, line_5: while Mg II in TX Psc will be observed using GHRS Echelle-B. line_8: A comparison M-star will be observed with G270M/GHRS. 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: 16.00 0.0 8 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 R stars of all classes, a few brighter N-type stars, line_7: and several late M giant stars. High-resolution spectra have been obtained in line_8: long exposures for a few bright early-R stars and a few bright M giant stars. line_9: A 13-hour 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 lines line_11: while a few other lines were weakly present (Eriksson et al. 1986). To make line_12: further progress, it is absolutely necessary to use HST. line_14: Narrow-band photometry and calibrated spectra will be obtained from the ground line_15: at approximately the same time to determine the properties of the underlying line_16: photosphere and the CSE. ! question: 4 section: 2 line_1: Part b) line_2: Summary of Exposure Times line_4: Exposure FOS ----------------- GHRS ----------------------- Time/ line_5: Target Factor G270H G270M/MgII G270M/CII/FeII/FeII/MgI Ech-B/MgII Star line_7: TX Psc 1.0 0.25 - - 4.0 4.25 line_8: UU Aur 2.3 0.50 2.3 - - 2.80 line_11: Mu Gem 0.08 - 0.1 0.5+0.25+0.25+0.25 - 1.35 line_14: subtotal 0.75 2.4 1.25 4.0 8.40 line_16: The total exposure time is 8.40 hours. line_17: The number of targets is 3. line_18: The number of wavelength settings is 8. line_19: The FOS 0.25x2.0 and 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 10. 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. We have line_2: increased exposure times, relative to pre-launch values, by 3.3x for the FOS line_3: exposures and 4.0x for the GHRS (small aperture) exposures, to account for the line_4: effects of spherical aberration. 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: Exposure times for the other targets are scaled, using the observed line_18: U-magnitude, from those calculated for TX Psc. line_20: The total estimated spacecraft time = 15.98 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., 1987, Astr. Ap., 183, 43) 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_12: The analysis will proceed in several steps. line_14: (1) The initial data reduction, calibration, and analysis of the observations line_15: will be done by the GSFC/CSC group (Carpenter, Robinson). The raw data files line_16: will be wavelength-calibrated using the explicit WAVE observations obtained line_17: along with the science data and transformed onto an absolute flux scale using line_18: the latest radiometric calibration of the GHRS. Software and techniques line_19: developed by the GHRS IDT will be used to optimize these calibrations. Copies line_20: of both the raw and calibrated spectra will then be sent to all investigators, line_21: and analysis will proceed through parallel and cooperative, independent line_22: 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_11: (3) Photospheric models, including polyatomic molecular opacities, in both line_12: plane-parallel and spherical geometry, will be computed for both carbon stars line_13: and M stars by the Midwest, Danish, French, and Swedish groups. This will line_14: include experimentation with two-component models. The SAO group will make line_15: detailed comparisons of synthetic spectra with visual observations, and the line_16: Danish and Swedish groups will do the same in the red and infrared regions. line_18: (4) Careful modeling of the chromospheric temperature structure will be line_19: undertaken, beginning with a carbon star. (However, to compute line_20: inhomogeneous NLTE models for both C and M stars will surely require line_21: several years.) A best theoretical photosphere-chromosphere model (including line_22: departures from LTE) will be selected by comparison of predicted fluxes with line_23: 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_5: (5) At Smithsonian synthetic spectra in the visual and ultraviolet line_6: regions will be calculated and carefully compared to observations. line_7: Comparisons of capacities in red giants and the sun will be made. line_9: (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 ! targnum: 2 name_1: HD46687 name_2: UU-AUR descr_1: A,144 pos_1: RA=06H36M32.83S+/-1.0", pos_2: DEC=+38D26'43.8"+/-1.0" equinox: 2000.0 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 2000.00 ra_pm_val: -0.000851 ra_pm_unct: 0.000085 dec_pm_val: -0.0170 dec_pm_unct: 0.0010 rv_or_z: V=+12 comment_1: (N3; C5,3) CARBON STAR fluxnum_1: 1 fluxval_1: V=5.29,TYPE=N3C53 fluxnum_2: 2 fluxval_2: F(2799)=8.7E-15 ! targnum: 3 name_1: HD44478 name_2: MU-GEM descr_1: A,142 pos_1: RA=06H22M57.62S+/-1.0", pos_2: DEC=+22D30'48.8"+/-1.0" equinox: 2000.0 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 2000.00 ra_pm_val: 0.003969 ra_pm_unct: 0.000072 dec_pm_val: -0.1120 dec_pm_unct: 0.0010 rv_or_z: V=+14 comment_1: (M3 III COMPARISON STAR) fluxnum_1: 1 fluxval_1: V=2.88,TYPE=M3-III fluxnum_2: 2 fluxval_2: F(2799)=2.50E-13 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: HD223075 config: FOS/RD opmode: ACQ/PEAK aperture: 4.3 sp_element: G270H wavelength: 2750 num_exp: 1 time_per_exp: 1.0S priority: 1 req_1: CYCLE 3 / 1.0-44.0; req_2: ONBOARD ACQ FOR 1.1; req_3: SPATIAL SCAN; req_4: SEQ 1-2 NO GAP; req_5: GROUP 1-6 WITHIN 2D comment_1: TX PSC IS COMMON NAME OF OBJECT ! linenum: 1.100 targname: HD223075 config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: G270H wavelength: 2750 num_exp: 1 time_per_exp: 2.0S priority: 1 req_1: ONBOARD ACQ FOR 1.2; req_2: SPATIAL SCAN; ! linenum: 1.200 targname: HD223075 config: FOS/RD opmode: ACQ/PEAK aperture: 0.5 sp_element: G270H wavelength: 2750 num_exp: 1 time_per_exp: 3.0S priority: 1 param_1: SCAN-STEP-X=0.35, param_2: SEARCH-SIZE-X=3, param_3: SCAN-STEP-Y=0.35, param_4: SEARCH-SIZE-Y=3 req_1: ONBOARD ACQ FOR 1.3; ! linenum: 1.300 targname: HD223075 config: FOS/RD opmode: ACQ/PEAK aperture: 0.25X2.0 sp_element: G270H wavelength: 2750 num_exp: 1 time_per_exp: 10.0S priority: 1 req_1: ONBOARD ACQ FOR 2.0; req_2: SPATIAL SCAN; ! linenum: 2.000 targname: HD223075 config: FOS/RD opmode: ACCUM aperture: 0.25X2.0 sp_element: G270H wavelength: 2750 num_exp: 3 time_per_exp: 5.0M priority: 1 ! linenum: 3.000 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 4.000; req_2: SEQ 3 - 6 comment_1: USE STEP-TIME = 1.6 SEC. comment_2: EXPECT ROUGHLY 640-1120 CTS/1.6S ! linenum: 4.000 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 req_1: ONBOARD ACQ FOR 5.0-6.0 comment_1: STEP-TIME = 2.4 SEC (FROM SIB) ! linenum: 5.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B wavelength: 2799 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: ECH-B wavelength: 2799 num_exp: 24 time_per_exp: 10.0M s_to_n: 10 fluxnum_1: 2 priority: 1 param_1: STEP-PATT=7, param_2: FP-SPLIT=NO comment_1: S/N IS FOR SUM OF 24 EXP'S. ! linenum: 11.000 targname: HD46687 config: FOS/RD opmode: ACQ/PEAK aperture: 4.3 sp_element: G270H wavelength: 2750 num_exp: 1 time_per_exp: 1.0S priority: 1 req_1: CYCLE 3 / 1.0-44.0; req_2: ONBOARD ACQ FOR 11.1; req_3: SPATIAL SCAN; req_4: SEQ 11-12 NO GAP; req_5: GROUP 11-16 WITHIN 2D comment_1: UU AUR IS COMMON NAME OF OBJECT ! linenum: 11.100 targname: HD46687 config: FOS/RD opmode: ACQ/PEAK aperture: 1.0 sp_element: G270H wavelength: 2750 num_exp: 1 time_per_exp: 2.0S priority: 1 req_1: ONBOARD ACQ FOR 11.2; req_2: SPATIAL SCAN; ! linenum: 11.200 targname: HD46687 config: FOS/RD opmode: ACQ/PEAK aperture: 0.5 sp_element: G270H wavelength: 2750 num_exp: 1 time_per_exp: 3.0S priority: 1 param_1: SCAN-STEP-X=0.35, param_2: SEARCH-SIZE-X=3, param_3: SCAN-STEP-Y=0.35, param_4: SEARCH-SIZE-Y=3 req_1: ONBOARD ACQ FOR 11.3; ! linenum: 11.300 targname: HD46687 config: FOS/RD opmode: ACQ/PEAK aperture: 0.25X2.0 sp_element: G270H wavelength: 2750 num_exp: 1 time_per_exp: 10.0S priority: 1 req_1: ONBOARD ACQ FOR 12.0; req_2: SPATIAL SCAN; ! linenum: 12.000 targname: HD46687 config: FOS/RD opmode: ACCUM aperture: 0.25X2.0 sp_element: G270H wavelength: 2750 num_exp: 6 time_per_exp: 5.0M priority: 1 ! linenum: 13.000 targname: HD46687 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 80.0S fluxnum_1: 1 priority: 1 param_1: LOCATE=YES, param_2: BRIGHT=RETURN, param_3: SEARCH-SIZE=5 req_1: ONBOARD ACQ FOR 14.000; req_2: SEQ 13 - 16 NO GAP comment_1: STEP-TIME = 3.2 SEC. comment_2: EXPECT ABOUT 800 CTS/3.2S ! linenum: 14.000 targname: HD46687 config: HRS opmode: ACQ/PEAKUP aperture: 0.25 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 120S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 15.0-16.0 comment_1: STEP-TIME = 4.8 SEC (FROM SIB) ! linenum: 15.000 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 16 NO SLEW; req_2: SEQ 15-16 NO GAP ! linenum: 16.000 targname: HD46687 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G270M wavelength: 2810 num_exp: 28 time_per_exp: 5.0M s_to_n: 10 fluxnum_1: 2 priority: 1 param_1: STEP-PATT=5, param_2: FP-SPLIT=NO comment_1: S/N IS FOR SUM OF 28 EXP'S. ! linenum: 33.000 targname: HD44478 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 80.0S 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 - 44 WITHIN 1D comment_1: MU GEM IS COMMON NAME FOR HD44478 comment_2: STEP-TIME = 3.2 SEC. comment_3: EXPECT 192 CTS/3.2 SEC ! linenum: 34.000 targname: HD44478 config: HRS opmode: ACQ/PEAKUP aperture: 0.25 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 10S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 35.0-44.0 comment_1: STEP-TIME = 0.4 SEC (FROM SIB) ! 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: HD44478 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G270M wavelength: 2810 num_exp: 2 time_per_exp: 5.0M s_to_n: 12 fluxnum_1: 2 priority: 1 param_1: STEP-PATT=5, param_2: FP-SPLIT=NO comment_1: S/N IS FOR SUM OF 2 EXP'S. ! linenum: 37.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G270M wavelength: 2335 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: HD44478 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G270M wavelength: 2335 num_exp: 6 time_per_exp: 5.0M s_to_n: 10 fluxnum_1: 2 priority: 1 param_1: STEP-PATT=5, param_2: FP-SPLIT=NO comment_1: S/N IS FOR SUM OF 6 EXP'S. ! linenum: 39.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G270M wavelength: 2612.5 num_exp: 1 time_per_exp: 30S priority: 1 param_1: STEP-PATT=3 req_1: CALIB FOR 40 NO SLEW; req_2: SEQ 39-40 NO GAP ! linenum: 40.000 targname: HD44478 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G270M wavelength: 2612.5 num_exp: 3 time_per_exp: 5.0M s_to_n: 10 fluxnum_1: 2 priority: 1 param_1: STEP-PATT=5, param_2: FP-SPLIT=NO comment_1: S/N IS FOR SUM OF 3 EXP'S. ! linenum: 41.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G270M wavelength: 2756.6 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: HD44478 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G270M wavelength: 2756.5 num_exp: 3 time_per_exp: 5.0M s_to_n: 10 fluxnum_1: 2 priority: 1 param_1: STEP-PATT=5, param_2: FP-SPLIT=NO comment_1: S/N IS FOR SUM OF 3 EXP'S. ! linenum: 43.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G270M wavelength: 2850 num_exp: 1 time_per_exp: 30S priority: 1 param_1: STEP-PATT=3 req_1: CALIB FOR 44 NO SLEW; req_2: SEQ 43-44 NO GAP ! linenum: 44.000 targname: HD44478 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G270M wavelength: 2850 num_exp: 3 time_per_exp: 5.0M s_to_n: 10 fluxnum_1: 2 priority: 1 param_1: STEP-PATT=5, param_2: FP-SPLIT=NO comment_1: S/N IS FOR SUM OF 5 FP-SPLIT EXP'S. ! ! end of exposure logsheet scan_data: line_list: 1.0,11.0 fgs_scan: cont_dwell: D dwell_pnts: 3 dwell_secs: 1.00 scan_width: 0.0000 scan_length: 2.8000 sides_angle: 90.0000 number_lines: 1 scan_rate: 0.0000 first_line_pa: 0.0000 scan_frame: S/C len_offset: 1.400 wid_offset: 0.0 ! line_list: 1.1,11.1 fgs_scan: cont_dwell: D dwell_pnts: 6 dwell_secs: 1.00 scan_width: 0.7000 scan_length: 3.5000 sides_angle: 90.0000 number_lines: 2 scan_rate: 0.0000 first_line_pa: 90.0000 scan_frame: S/C len_offset: 1.750 wid_offset: 0.350 ! line_list: 1.3,11.3 fgs_scan: cont_dwell: D dwell_pnts: 7 dwell_secs: 1.00 scan_width: 0.0000 scan_length: 0.4000 sides_angle: 90.0000 number_lines: 1 scan_rate: 0.0000 first_line_pa: 90.0000 scan_frame: S/C len_offset: 0.200 wid_offset: 0.0 ! ! end of scan data