! 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