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J/A+AS/146/217 Library of Spectra (0.5 to 2.5um) of Cool Stars (Lancon+ 2000)
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A library of 0.5 to 2.5 micron spectra of luminous cool stars
Lancon A., Wood P.R.
<Astron. Astrophys. Suppl. Ser. 146, 217 (2000)>
=2000A&AS..146..217L
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ADC_Keywords: Spectra, red ; Spectra, infrared ; Stars, late-type ;
Spectrophotometry; Stars, luminous
Keywords: catalogs - stars: AGB - stars: individual: CL Car -
stars: individual: R Lep - stars: variables: general - infrared: stars
Description:
The present catalogue contains 182 low resolution optical spectra,
145 medium resolution (R~1100) near-IR spectra, and 112 merged
optical+near-IR spectra that range from about 510 to 24,500 nm.
The observed stars are luminous cool objects: the sample includes
red giants, red supergiants, oxygen rich and carbon rich long period
variables (asymptotic giant branch stars), as well as a few Galactic
Bulge and LMC/SMC stars.
The optical data were acquired on the so-called 74 inch Telescope at
Mount Stromlo Observatory. The near-IR data were acquired with the
Cryogenic Array Spectrometer and Imager CASPIR on the 2.3 meter Australian
National University Telescope at Siding Spring Observatory. Optical
and near-IR data for variable objects have been merged only when both
were taken less than 15 days apart; but both spectral ranges are also
provided separately.
The spectra are corrected for telluric absorption. However, in regions
where the transmission of the Earth atmosphere is close to zero the
fluxes recovered remain highly uncertain.
The flux calibration is based on a series of reference stars, for
which a theoretical intrinsic energy distribution was assumed. An
absolute flux calibration (to about 10% accuracy) was only achieved in
exceptional cases; in the other cases, the absolute fluxes can be off
their real values by an order of magnitude due to slit losses (for the
programme star and/or the reference star) and to non-photometric
wheather. Uncertainties in the relative values of fluxes along each
spectrum are described in the paper.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
stars.dat 155 80 Star positions
vi/* . 182 Optical spectra
ik/* . 145 Near-IR spectra (I band)
vk/* . 112 Merged optical/near-IR spectra
ikrefs.dat 24 60 Log of reference stars used per night
iklog.dat 61 145 Log of near-IR observations
vilog.dat 60 182 Log of optical observations
mbol.dat 28 88 Bolometric magnitude estimates
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See also:
III/140 : Carbon stars from Baldone telescope (Alksne+ 1987)
III/156 : Cool Galactic Carbon Stars, 2nd Edition (Stephenson 1989)
J/AJ/99/784 : IR photometry of LMC long-period variables (Hughes+ 1990)
J/A+AS/115/41 : UBV(RI) photometry of cool stars (Cutispoto+, 1996)
J/A+A/325/1115 : Near-simultaneous ROSAT and Mt Wilson data (Piters+ 1997)
J/AJ/119/1448 : Improved properties for cool stars (Houdashelt+, 2000)
Byte-by-byte Description of file: stars.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Star Star name
15- 16 I2 h RAh Right ascension (J2000)
18- 19 I2 min RAm Right ascension (J2000)
21- 24 F4.1 s RAs Right ascension (J2000)
26 A1 --- DE- Declination sign (J2000)
27- 28 I2 deg DEd Declination (J2000)
30- 31 I2 arcmin DEm Declination (J2000)
33- 34 I2 arcsec DEs Declination (J2000)
38- 42 F5.2 mag Bmag ? B magnitude
44- 48 F5.2 mag Vmag ? V magnitude
50- 65 A16 --- SpType Spectral type
67-155 A89 --- Files Comma-separated list of spectra files
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Byte-by-byte Description of files under: vi/ vk/
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Bytes Format Units Label Explanations
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2- 7 F6.0 0.1nm Lambda Wavelength
10- 21 E12.5 --- FluxDen Flux density, in arbitrary units of
energy per wavelength interval.
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Byte-by-byte Description of files under: ik/
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Bytes Format Units Label Explanations
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2- 7 F6.0 0.1nm Lambda Wavelength
10- 21 E12.5 --- FluxDen Flux density, in erg/s/cm2/{AA} (mW/m2/0.1nm)
when an absolute flux calibration was
available (cf. iklog.dat below), otherwise
in arbitrary units of energy per wavelength
interval.
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Byte-by-byte Description of file: ikrefs.dat
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Bytes Format Units Label Explanations
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1- 10 A10 "Y-M-D" Date Observation date
12 I1 --- Nref [0/6] Numbered atmospheric reference name
14- 19 A6 --- Star Name of the reference star.
22- 24 F3.1 --- Airmass Typical airmass of the observations
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Byte-by-byte Description of file: iklog.dat vilog.dat
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Bytes Format Units Label Explanations
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1- 16 A16 --- File Name of the file with spectrum
18- 27 A10 "Y-M-D" Date Observation date ("YYYY-MM-DD")
29- 32 F4.2 --- Airmass ? Airmass (1)
34- 40 A7 --- Nref ? Number of the reference star(s) used
separated by '+'. Refers to ikrefs.dat file (1)
42- 49 F8.0 --- HJD Julian date of the observation (rounded to
the nearest integer)
50- 51 A2 --- n_HJD +last digit of HJD when two days of observation
53- 57 F5.1 --- Phase ? GCVS phase of the observation when available.
See Appendix B for comments on individual stars
See note (2)
59- 61 A3 --- Note [yes ] if absolute flux calibration available (1)
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Note (1): Only in iklog.dat file
Note (2): Additional information about phases, from lightcurves
provided by amateur astronomer groups:
AAVSO (American Association of Variable Star Observers)
AFOEV (Association Francaise des Amateurs d'Etoiles Variables).
These groups should be contacted for scientific use of their data:
the data provided is only meant as an indication.
Approximate Julian date of a recent maximum of the visual light curve:
S Phe : 2490045 (versus 2430060 in the GCVS) -- AAVSO
R Phe : 2449716 (versus 2439486 in the GCVS) -- AAVSO
S Car : 2442129.8 (versus 2442112 in the GCVS) -- AFOEV
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Byte-by-byte Description of file: mbol.dat
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Bytes Format Units Label Explanations
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1- 14 A14 --- File Object name for merged spectrum
16- 22 A7 "YYYY-MM" Date Observation date
24- 28 F5.2 mag Mbol Estimated absolute bolometric magnitude, derived
using the period - K band relation of Hughes and
Wood (1990, Cat. <J/AJ/99/784>) and an
instantaneous bolometric correction estimated
from the data itself. (1)
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Note (1):
Absolute K magnitudes were computed from the GCVS period (where available)
using the LMC relations of Hughes & Wood, 1990 (Cat. <J/AJ/99/784>),
and a distance modulus of 18.55 for the LMC. Using the relation of
Kanbur et al. (1997MNRAS.289..428K) would not change the results
significantly for C stars, and change them by less than 0.1mag (except for
a few cases) for O-rich stars.
The phase dependence of M_bol_ is included through the instantaneous
bolometric correction BC_K_. The latter was obtained from the energy
distribution of the relevant spectrum itself. As a first order correction
for the limited wavelength range, the energy distributions were extrapolated
to zero flux at 3500{AA} on the blue side and at 3.5{mu} on the red side (an
additional correction was added only in the case of R Lep, whose spectrum
still rises with wavelength at 2.5{mu}).
Variations in the K band luminosity with phase have been neglected here.
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Acknowledgements: Ariane Lancon <lancon@astro.u-strasbg.fr>
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(End) Patricia Bauer [CDS] 20-Jul-2000