Page 1 PROPOSAL FOR HUBBLE SPACE TELESCOPE OBSERVATIONS ST ScI Use Only ID 5694 Report Date: 18-Jul-95:17:52 Version: ********** Check-in Date: ********** 1.Proposal Title: SPECTRA AND CHROMOSPHERES OF CARBON AND M STARS - CYCLE 4 CARRYOVER ------------------------------------------------------------------------------------ 2. Scientific Category 3. Proposal For 4. Proposal Type 5. Continuation ID COOL STARS GO/CAR 4685 Sub Category STELLAR ATMOSPHERES ------------------------------------------------------------------------------------ 6. Principal Investigator Institution Country Telephone Hollis R. Johnson INDIANA UNIVERSITY USA ------------------------------------------------------------------------------------ 7. Abstract We propose to use the Goddard High-Resolution Spectrograph (GHRS) on the HST to obtain ultraviolet spectra of the visually bright N-type carbon star TX Psc. These spectra, obtainable only with HST, will be used with theoretical models to infer the density and temperature structure and the velocity fields of the outer atmosphere in these evolutionarily advanced, non-mira giants. In anticipation of this effort, we have pushed IUE to its limit to obtain a weak high-resolution spectra of this star, and observations of a second carbon star (UU Aur) with HST are being analyzed. Based upon the observed line profiles and continua, we will construct semi-empirical non-LTE models in both plane-parallel geometry and spherical geometry, including velocity fields, by attaching a chromosphere to theoretical photospheric models. Two-component models will be studied. Using these and ab-initio hydrodynamic models, we will examine the mechanisms responsible for chromospheric heating and mass loss. A full range of supporting ground-based observations will be undertaken to permit us to connect models of the photospheres, chromospheres, and circumstellar shells. ------------------------------------------------------------------------------------ ------------------------------------------------------------------------------------ 9. Est obs time (hours) pri: 7.18 par: 0 10. Num targs pri: 1 par: 0 ------------------------------------------------------------------------------------ 11. Instruments requested: HRS ------------------------------------------------------------------------------------ ------------------------------------------------------------------------------------ Page 2 I. GENERAL FORM Proposal 5694 PI: Hollis R. Johnson Proposal Title: SPECTRA AND CHROMOSPHERES OF CARBON AND M STARS - CYCLE 4 CARRYOVER ------------------------------------------------------------------------------------ 1. Proposers: Proposers Institution Country ESA ------------------------------------------------------------------------------------ Pi Hollis R. Johnson INDIANA UNIVERSITY USA David R. Alexander WICHITA STATE UNIVERSITY USA Eugene H. Avrett SMITHSONIAN ASTROPHYSICAL USA OBSERVATORY Alexander Brown U.COLORADO JILA USA Kenneth G. Carpenter NASA GODDARD LASP USA Kjell Eriksson UPPSALA ASTRONOMICAL OBSERVATORY SWEDEN X Bengt Gustafsson UPPSALA ASTRONOMICAL OBSERVATORY SWEDEN X Uffe G. Jorgensen NIELS BOHR INSTITUTE DENMARK X Philip D. Judge HIGH ALTITUDE OBSERVATORY USA Jeffrey L. Linsky U.COLORADO JILA USA Donald G. Luttermoser IOWA STATE UNIVERSITY USA Francois Querci OBSERVATOIRE MIDI PYRENEES, FRANCE X TOULOUSE Monique Querci OBSERVATOIRE MIDI PYRENEES, FRANCE X TOULOUSE Richard D. Robinson COMPUTER SCIENCES CORPORATION USA Robert F. Wing OHIO STATE UNIVERSITY USA ------------------------------------------------------------------------------------ 3. Description of proposed observations. Part a) High-resolution spectra of the bright N-type carbon star (TX Psc: N0, C6,2) will be obtained using the HST G270M mode in three spectral regions centered on 2345 A (C II]), 2754 A (Fe II), and 2810 A (Mg II). The exposure times are summarized in Section 4. The project is pure Cycle 3: Primary Hours: Parallel Hours: Exposures: 7.18 0.0 3 Part b) N/A Page 3 ------------------------------------------------------------------------------------ 4. Justification of need for HST observations. Part a) To understand mass loss and to model the outer atmospheres (including chromospheres and circumstellar layers) require detailed profiles of key spectral lines, which in turn requires high-resolution ultraviolet spectra. We have pushed IUE to its limit. That effort has produced low-resolution LWP/LWR spectra of the brighter stars of all spectral classes, including carbon stars. A 13-hour high-resolution LWP exposure of the best N-type star (TX Psc) was considerably underexposed and showed clearly only the Mg II emission lines while a few other lines were weakly present (Eriksson et al. 1986). To make further progress, it is absolutely necessary to use HST. We have already obtained FOS medium- resolution spectra of the carbon star UU Aur (N3: C5,3) and one high-resolution spectrum in the region of the Mg II lines at 2800 A. These are far superior to any previously obtained and confirm the necessity for high-resolution observations, especially in other wavelength regions. Narrow-band photometry and calibrated spectra will be obtained at approximately the same time to determine the properties of the underlying photosphere and the CSE. Part b) Summary of Exposure Times Exposure GHRS Time/ Target Factor G270M/CII G270M/FeII G270M/MgII Star TX Psc 1.0 - - subtotal 3.00 1.60 0.75 5.35 The total exposure time is 5.35 hours. The number of targets is 1. The number of wavelength settings is 3. The GHRS 0.25x0.25 arcsec science apertures are used. The exposure times for TX Psc are derived using fluxes from IUE observations taken during 1981, when the star was in a "low" state, to ensure that we obtain at least the minimum desired S/N of 20. If the star is brighter at the time of the HST observations, we will be delighted to achieve a higher S/N. We require the use of the GHRS small aperture to preserve the design spectral resolution and the true line profiles. Monochromatic peak line fluxes, as measured in IUE low-resolution spectra of TX Psc are: C II 2325 A Al II 2670 Fe II 2750 A Mg II 2800 A ----------- ----------- ------ ------ ------------ 4.0e-15 3.0e-15 5.0e-15 2.0e-14 ergs/cm2/s/A The PEAK S/N achieved in the GHRS observations will be higher than predicted using these figures directly, since, unlike IUE, GHRS will resolve the lines. The GHRS exposure times have been checked using the new sensitivities in the Cycle 3 handbook, modified to account for the improved GHRS SSA sensitivity recently achieved with an improved centering of targets in the GHRS SSA. The total estimated spacecraft time = 7.18 hours ------------------------------------------------------------------------------------ 5. Description of special scheduling requirements. Wavelength calibration exposures on the internal Pt-lamps are requested for each GHRS exposure since we require the highest possible wavelength accuracy in order to measure flow velocities in the chromospheres and circumstellar shells of our target stars. ------------------------------------------------------------------------------------ 6. Description of special calibration exposures. Special Calibration Requirement(s) __________________________________ Wavelength calibrations at each GHRS grating setting (no motion of carrousel between science and calibration exposure) are required to obtain the required wavelength/velocity precision. Page 4 ------------------------------------------------------------------------------------ 7. Data reduction and analysis plans. To support the important HST observations several types of concurrent ground- based observations will be made. (1) The Swedish wing of the team will make radio observations of circumstellar gas through CO and HCN lines (Olofsson, et al., 1993 Ap. J. Supp. 87, 267) and high-resolution (120,000) spectroscopic observations of CS matter in the Na D and K I resonance lines with the new HRS at the Nordic Optical 2.5-m telescope at La Palma. (2) the French and Ohio State groups will make concurrent ground-based, high-resolution spectra in the visual region and ultraviolet regions. We have already obtained spectra of the CO fundamental lines in TX Psc, and we hope to obtain similar spectra for the other stars. The analysis will proceed in several steps. (1) The initial data reduction, calibration, and analysis of the observations will be done by the GSFC/CSC group (Carpenter, Robinson). The raw data files will be wavelength- calibrated using the explicit WAVE observations obtained along with the science data and transformed onto an absolute flux scale using the latest radiometric calibration of the GHRS. Software and techniques developed by the GHRS IDT will be used to optimize these calibrations. Copies of both the raw and calibrated spectra will then be sent to all investigators, and analysis will proceed through parallel and cooperative, independent ventures. (2) The GSFC/CSC group will perform the initial measurement and analysis of the UV data, obtaining observed wavelengths, line widths, and detailed line profiles. From these results we will infer the turbulent and flow velocities and velocity gradients in the stellar chromosphere and wind. This information will be combined with velocities from visual and radio observations and deductions from the mass-loss rate and mass continuity to yield as complete a picture as possible of the velocity structure of the photospheric, chromospheric, and CS regions. The GSFC/CSC, Boulder, Swedish, and Ohio State groups will participate. (3) Photospheric models, including polyatomic molecular opacities, in both plane-parallel and spherical geometry, will be computed for both carbon stars and M stars by the Midwest, Danish, French, and Swedish groups. This will include experimentation with two- component models. The SAO group will make detailed comparisons of synthetic spectra with visual observations, and the Danish and Swedish groups will do the same in the red and infrared regions. (4) Careful modeling of the chromospheric temperature structure will be undertaken, beginning with a carbon star. (However, to compute inhomogeneous NLTE models for both C and M stars will surely require several years.) A best theoretical photosphere-chromosphere model (including departures from LTE) will be selected by comparison of predicted fluxes with observations of both lines and continua. The Boulder, Indiana, Iowa State, Goddard, and Smithsonian groups currently possess the necessary programs for NLTE chromospheric modeling, and these groups will work in parallel and in collaboration in checking NLTE results in this extremely complex research. (5) At Smithsonian synthetic spectra in the visual and ultraviolet regions will be calculated and carefully compared to observations. Comparisons of capacities in red giants and the sun will be made. (6) Results will be published in a timely fashion. ------------------------------------------------------------------------------------ 8. Additional comments or special requests. None. Page 5 ------------------------------------------------------------------------------------ 9. Description of previous HST work. part a) HST GTO Programs on which Carpenter is PI: GTO 1195: Outer Atmospheres of Cool Luminous Stars - Cycle 0 (Alpha Ori) 3212: Outer Atmospheres of Cool Luminous Stars - Cycle 1 (Gamma Cru) GTO 1198: Physical Conditions and Velocity Structures in the Red Giant 3934: Winds in the Binaries CI Cyg and EG And - Cycle 2 (2 targets) GTO 1199: Alpha Ori Team Project - Cycle 1 HST GTO programs on which Linsky is PI: GTO 1175/3943: Local Interstellar Medium and D/H Ratio GTO 1176/3964: The dynamics of stellar chromospheres & transition regions GTO 1177: Atmospheres of very inactive K giant stars GTO 1179/3961: Hybrid- chromosphere stars GTO Program 1180: The chromospheres of the very coolest M dwarf stars HST Programs on which Linsky and/or Carpenter are Co-I's: : GTO 1210: Age dependence of non-radiative heating in stellar chromospheres GO 2238: Lyman-ALPHA Observations Of High Radial Velocity Stars GO 2321: Search for proton acceleration in flare stars - AU Mic GO 3626: Empirical determination of the wind velocity and density laws for the K supergiant Zeta Aurigae from eclipse ingress spectra HST programs on which Gustafsson is Co-I: GO P3479: Boron in Pop II Dwarfs THERE ARE NO OBSERVATIONS OF CARBON STARS IN THESE GTO PROGRAMS. The only M-giant included in these GTO programs is Gamma Cru, in GTO 3212 - a cycle 1 program which executed late in that cycle. The observations cover a broader range of wavelengths and purposes than those planned for the M-stars in this GO proposal, but they do not include a satisfactory match to the carbon-star observations for our detailed comparison purposes. SAO program 3023 (Alpha Tau) observations have been used to assess the feasibility of programs such as these which involve observations of narrow emission-line sources (see the Ap.J. reference below). Part b) The observations of Alpha Tauri in SAO 3023 provided the first direct measurement of the turbulence in the chromosphere of a cool giant (K5 III), the discovery of a downflow of the C II] chromospheric plasma, the detection of 25 new emission features in the 2320-2370 A region, and the first evidence for optically thin emission lines (of CII 2335A) that have extended wings. Other results are summarized in the papers listed in part (c). Highlights of Carpenter GTO (Programs 1195/3212) and SAO results include: 1) the unambiguous detection of a far-UV continuum in Alpha Ori and Gamma Cru, which will provide a very important and previously unrecognized diagnostic of their chromospheric plasmas (formation temperature in Alpha Ori ranges from 3500-5000 K and increases steadily with decreasing wavelength); 2) the discovery of circumstellar CO (4th positive A-X system) absorption bands superposed on the far -UV continuum from Alpha Ori, providing a probe of regions of the circumstellar shell not available at visible or IR wavelengths (initial analysis indicates T=500 K, Vturb=5 km/s, N(CO)=1.0e18 cm-2); 3) detection of myriad new Fe II fluorescent line products, producing by Lyman Alpha radiation in Alpha Ori; 4) a determination that, in Alpha Ori, the resonance lines of OI and CI are very weak due to self-absorption and that the asymmetries seen in the MgII resonance lines are probably due to different velocity shifts between the self-absorption and emission in the two lines; and 5) the first direct measurement of the chromospheric turbulence (24 km/sec) and the detection of a downflow of about 4 km/sec in chromospheric C II] plasma in Alpha Tau. High quality observations of Gamma Cru in program 3212 have recently been acquired and detailed analysis is now in progress. GTO Program 1175: Linsky and collaborators obtained SSA echelle spectra of Capella in the Lyman alpha, FeII, and MgII lines on 15 April 1991. The purpose was to obtain very accurate measurements of the D/H ratio and interstellar properties for the 12.5-pc line of sight towards this star. They derived the ratio D/H = 1.65 (+0.07 -0.18) x 10e-5, temperature 7000 (+/- 200) K, and turbulent velocity of 1.66 (+/-0.03) km/s. The local D/H ratio was used to infer the primordial value which is a major constraint on models of the early universe. Observations of Alpha Cen A and B, Procyon, HR 1099, and a reobservation of Capella are planned. GTO Program 1176: Low and moderate dispersion GHRS spectra of Capella were obtained on 15 April 1991 and of Beta Draconis on 23 April 1992. The Capella observations show downflowing transition region gas from both stars in the system and intersystem lines of many different ions that allow the determination of the electron density as a function of the temperature of the emitting plasma. Observations of Procyon, Epsilon Eri, HR 1099, and Alpha Cen A and B are planned. The Beta Draconis data are being analyzed. SV observations of Gamma Draconis obtained on 6 April 1991 by Carpenter et al. provide clear evidence of such high temperature lines as CIV and SIIV in the atmosphere of this hybrid-chromosphere star. The surface fluxes in the 100,000 K plasma lines are the smallest ever observed in any star. GO Program 2321: Evidence for proton beams was obtained by Woodgate et al. from GHRS spectra of AU Mic during a flare. This discovery was described in a recent NASA press release and in an ApJ paper. There have been no observations yet in any of the other programs. Part c) Results have been presented: in the Ap.J. & MNRAS, at AAS meeting (1/91, 5/91 & 1/92), the HST Joint Discussion at the IAU General Assembly (7/91), the 7th Cambridge Cool Star Workshop (10/91), and at both HST Workshops (5/91 & 7/92), including two invited reviews (AAS 1/91 and Cool Star Workshop 10/91). "First Results from the Goddard High Resolution Spectrograph: The Chromosphere of Alpha Tauri", Carpenter, K. G., Robinson, R., Wahlgren, G., Ake, T., Linsky, J., Brown, A., and Walter, F., Ap.J. (Letters), 377, L45, 1991. "Si II Emission Line Diagnostics," Judge, P. G., Carpenter, K. G., and Harper, G.M., MNRAS, 253, 123, 1991. "Early Scientific Results from the Goddard High Resolution Spectrograph" Carpenter, K. G. , Invited Review presented at the AAS Meeting, 1/13-17/91. "GHRS Chromospheric Emission Line Spectra of the Red Giant Alpha Tau" Carpenter, K. G., Robinson, R. D., Ebbets, D. C., Brown, A., and Linsky, J., in `The First Year of HST Observations,' 1991. "Chromospheres and Winds of Cool Stars", Carpenter, K.G., IAU General Assembly Joint Discussion, 'First Results from the Hubble Space Telescope', 7/31/91. "HST Observations of Late-Type Stars," (Invited Review) Carpenter, K. G., in `Proceedings of the 7th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun,' in press, 1992. "Molecular Absorption in the UV Spectrum of Alpha Ori," Wahlgren, G. M., Robinson, R. D., and Carpenter, K. G., Proceedings of the Seventh Cambridge Workshop on Cool Stars, Stellar Systems and the Sun, ed. M. Giampapa and J. Bookbinder, A.S.P. Conference Series, in press, 1992. "The Chromosphere and Circumstellar Shell of Alpha Orionis as Observed with the Goddard High Resolution Spectrograph," Carpenter, K. G., Robinson, R. D., Wahlgren, G. M., Linsky, J. L., Brown, A., in Science with the Hubble Space Telescope (European Southern Observatory), eds. P. Benvenuti and E. Schreier, in press, 1992. "The Far-UV Spectrum of alpha Ori," Carpenter, K. G., Robinson, R. D., Wahlgren, G. M., Linsky, J.L., and Brown, A., Ap. J., submitted, 1992. `GHRS observations of the local interstellar medium and the deuterium/hydrogen ratio along the line of sight towards Capella,' Linsky, J.L., Brown, A., Gayley, K., Diplas, A., Savage, B. D., Ayres, T. R., Landsman, W., Shore, S., and Heap, S. R., Astrophysical Journal, to appear 10 Jan 1993. `The hydrogen Lyman alpha emission of Capella', Ayres, T.R., Brown, A., Gayley, K.G., and Linsky, J.L., Astrophysical Journal, to appear 10 Jan 1993. `GHRS Far-ultraviolet spectra of coronal and noncoronal stars: Capella and Gamma Draconis', Linsky, J.L., Brown, A., and Carpenter, K.G., in The First Year of HST Observations, ed. A.L. Kinney and J.C. Blades (Baltimore: Space Telescope Science Institute), p. 70 (1991). `The Deuterium abundance in the local interstellar medium', Linsky, J.L.to appear in Highlights of the IAU, Vol. 9. `Ultraviolet observations of stellar coronae: early results from HST', Linsky, J.L., to appear in Memorie della Societa Astronomica Italiana. `Ultraviolet observations of stellar coronae; early results from the Hubble Space Telescope', Linsky, J.L., IAU Joint Commission VI on `Solar and Stellar Coronae', Buenos Aires, Argentina, to be published. `Deuterium abundance in the local interstellar medium', Linsky, J.L. in IAU Joint Discussion VII on `First Results from the Hubble Space Telescope', Buenos Argentina, to be published. `GHRS observations of the local interstellar medium and the deuterium/hydrogen ratio toward Capella', Linsky, J.L., in Science with the Hubble Space Telescope (European Southern Observatory), in press. `New stellar plasma determinations by the GHRS: The transition regions of Capella and Gamma Draconis', Linsky, J.L., Wood, B., and Brown, A., in Science with the Hubble Space Telescope (European Southern Observatory), in press. Page 6 ------------------------------------------------------------------------------------ 10. Resources to be supplied by investigator's institution(s). Indiana University (I.U.) has been very generous in providing much time on its computing facilities. Programs, data, and facilities for computing model atmospheres are in use at I.U., Wichita, Copenhagen, Toulouse, and Uppsala. Programs for constructing non-LTE model chromospheres are available at HAO, JILA, Iowa St., GSFC, and Smithsonian. Radio and optical telescopes for concurrent observations are available in Sweden, France, ESO-La Silla, and the United States (Ohio State U.). Software developed by the GHRS IDT will be available at NASA- GSFC, as well as VAX computing facilities, for reduction and measurement of GHRS and FOS spectra. ------------------------------------------------------------------------------------ 11. Address Information Name: HOLLIS R. JOHNSON Category: PI Institution: Indiana University Address: ASTRONOMY DEPT., SW 319 City: BLOOMINGTON State: IN Zip Code: 47405 Country: USA Telephone: (812)-855-6915 Telex (or e-mail): 272-279 ------------------------------------------------------------------------------------ TARGET LIST a) Fixed Targets ID = 5694 [ 7] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 ------------------------------------------------------------------------------------------------------------------------------------ Tar| Target | Target | Target |Coord | Radial |Acqui|FLX| Flux data No | Name | Description | Position |Eqnx | Vel. |Prblm|REF| | | | | | | | | ------------------------------------------------------------------------------------------------------------------------------------ 1 HD223075 TX- A,144 RA=23H46M23.525S+/-1.0", 2000.0 V=+11 1 V=5.04,TYPE=NOC62 PSC DEC=+03D29'12.5"+/-1.0" 2 F(2799)=2.0E-14 Comments: (N0; C6,2) CARBON STAR Epoch of Position RA proper motion (seconds of time/yr) DEC Proper Motion (arcsec/yr) Annual Parallax (arcsec) J 2000.00 -0.0020 +/- 0.0001 -0.0250 +/- 0.0010 0.0000 +/- 0.0000 ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 5694 [ 8] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 | 9 |10 | 11 | 12 |13 |14| 15 ------------------------------------------------------------------------------------------------------------------------------------ Line | Seq | Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | S/N |Flx|Pr| Special Number | Name | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| |Rel. Time|Ref| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 1 HD223075 HRS ACQ 2.0 MIRROR-N2 LOCATE=YES 1 40.0S 1 1 ONBOARD ACQ FOR BRIGHT=RETURN 2.000 SEARCH-SIZE=5 SEQ 1-8 CYCLE 4/1-8 Comments: USE STEP-TIME = 1.6 SEC. EXPECT ROUGHLY 640-1120 CTS/1.6S ------------------------------------------------------------------------------------------------------------------------------------ 2 HD223075 HRS ACQ/ 0.25 MIRROR-N2 SEARCH-SIZE=5 1 60S 1 1 ONBOARD ACQ FOR PEAKUP 3.0-8.0 Comments: STEP-TIME = 2.4 SEC (FROM SIB) ------------------------------------------------------------------------------------------------------------------------------------ 3 WAVE HRS ACCUM SC2 G270M 2345 STEP-PATT=3 1 30S 1 CALIB FOR 4 NO SLEW SEQ 3-4 NO GAP ------------------------------------------------------------------------------------------------------------------------------------ 4 HD223075 HRS ACCUM 0.25 G270M 2345 STEP-PATT=5 18 10.0M 32 2 1 FP-SPLIT=NO Comments: S/N IS FOR SUM OF 18 EXP'S. ------------------------------------------------------------------------------------------------------------------------------------ 5 WAVE HRS ACCUM SC2 G270M 2754 STEP-PATT=3 1 30S 1 CALIB FOR 6 NO SLEW SEQ 5-6 NO GAP ------------------------------------------------------------------------------------------------------------------------------------ 6 HD223075 HRS ACCUM 0.25 G270M 2754 STEP-PATT=5 10 9.6M 25 2 1 FP-SPLIT=NO Comments: S/N IS FOR SUM OF 10 EXP'S. ------------------------------------------------------------------------------------------------------------------------------------ 7 WAVE HRS ACCUM SC2 G270M 2810 STEP-PATT=3 1 30S 1 CALIB FOR 8 NO SLEW SEQ 7-8 NO GAP ------------------------------------------------------------------------------------------------------------------------------------ 8 HD223075 HRS ACCUM 0.25 G270M 2810 STEP-PATT=5 6 9.0M 30 2 1 FP-SPLIT=NO Comments: S/N IS FOR SUM OF 5 EXP'S. ------------------------------------------------------------------------------------------------------------------------------------ Summary Form for Proposal 5694 [ 9] Item Used in this proposal ------------------------------------------------------------------------------------------------------------------------------------ Configurations HRS ------------------------------------------------------------------------------------------------------------------------------------ Opmodes ACQ ACQ/PEAKUP ACCUM ------------------------------------------------------------------------------------------------------------------------------------ Optional Parameters LOCATE=YES BRIGHT=RETURN SEARCH-SIZE=5 STEP-PATT=3 STEP-PATT=5 FP-SPLIT=NO ------------------------------------------------------------------------------------------------------------------------------------ Proposal for GO/CAR ------------------------------------------------------------------------------------------------------------------------------------ S/C Hours 7.18 ------------------------------------------------------------------------------------------------------------------------------------ Scientific Category COOL STARS ------------------------------------------------------------------------------------------------------------------------------------ Scientific Sub-category STELLAR ATMOSPHERES ------------------------------------------------------------------------------------------------------------------------------------ Special Requirements ONBOARD ACQ FOR 2.000; SEQ 1-8; CYCLE 4/1-8 ONBOARD ACQ FOR 3.0-8.0 CALIB FOR 4 NO SLEW; SEQ 3-4 NO GAP CALIB FOR 6 NO SLEW; SEQ 5-6 NO GAP CALIB FOR 8 NO SLEW; SEQ 7-8 NO GAP ------------------------------------------------------------------------------------------------------------------------------------ Spectral Elements MIRROR-N2 G270M ------------------------------------------------------------------------------------------------------------------------------------ Target Names HD223075 TX-PSC ------------------------------------------------------------------------------------------------------------------------------------