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III/196 Near-IR stellar spectra from 1.428 to 2.5 um (Lancon+ 1996)
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A library of near-IR stellar spectra from 1.428 to 2.5 {mu}m.
Lancon A., Rocca-Volmerange B.
<Astron. Astrophys. Suppl. Ser. 96, 593 (1992)>
=1992A&AS...96..593L
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ADC_Keywords: Spectra, infrared
Keywords: atlases - stars: infrared spectroscopy -
stars: temperatures - stars: colors
Description:
This library is an EXTENDED VERSION of the library published by
A.Lancon and B.Rocca-Volmerange in 1992.
The catalog contains near-IR spectra of 84 stars, obtained with the
Fourier Transform Spectrograph at the Canada-France-Hawaii Telescope
on Mauna Kea, Hawaii. The spectra cover the H and K atmospheric
windows, i.e. wavelengths from 1.43 to 2.5 microns, with a typical
resolving power of 500.
The spectra have all been reduced again in 1996. The general procedure
was as described in the original article, except that the intrinsic
energy distributions of the stars used as references were assumed to
be well represented by the models of Kurucz, 1993. Making extensive
use of the Simbad data base, we have searched the literature on each
of these stars, looking for effective temperature and extinction
determinations. The new reduction improves the reliability of the
continua, and reduces possible systematic differences between
observing runs.
The files contain the reduced spectra in FITS format, with fluxes in
arbitrary units of energy per unit frequency (normalised to
approximately 1 in the K band) and frequencies in cm^-1^, the
natural units of Fourier Transform spectroscopy.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
stars.dat 168 95 List of spectra
stars.tex 82 359 *LaTeX tables
rawspec.fit 2880 4 *Raw spectrum of an O9V star
fits/* . 95 Subdirectory with the 95 FITS spectra
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Note on rawspec.fit: this file can be used to determine in which
spectral regions the quality is worst due to molecular opacity
in the Earth atmosphere.
Note on stars.tex: the file should be compiled with LaTex in landscape
mode; the text width could well be too big for American paper
format, in this case "\small" should be changed into "\footnotesize"
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Byte-by-byte Description of file: stars.dat
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Bytes Format Units Label Explanations
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1 A1 --- SpClass [dgc] Class (dwarf, giant, supergiant)
3- 13 A11 --- Object Object name
15- 16 I2 h RAh Right Ascension 2000 (hours) (1)
18- 19 I2 min RAm Right Ascension 2000 (minutes) (1)
21- 24 F4.1 s RAs Right Ascension 2000 (seconds) (1)
26 A1 --- DE- Declination 2000 (sign) (1)
27- 28 I2 deg DEd Declination 2000 (degrees) (1)
30- 31 I2 arcmin DEm Declination 2000 (minutes) (1)
33- 34 I2 arcsec DEs Declination 2000 (seconds) (1)
36- 43 A8 --- FITSfile Name of FITS file in directory fits (2)
45 I1 --- Qual [1/3] Quality of spectrum (3)
47- 55 A9 --- Cont Continuum model (4)
57- 62 F6.3 mag H-K Color index (5)
64- 68 F5.2 mag (H-K)lit ? H-K found in the literature (6)
69 A1 --- u_(H-K)lit [?~] Uncertainty flag on (H-K)lit
70- 74 F5.2 mag (H-K)lit2 ? H-K found in the literature (6)
76- 83 A8 --- SpType Spectral type
85-118 A34 --- Comments Other properties found in literature
120-168 A49 --- Names Cross-identifications
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Note (1): Position taken from SIMBAD
Note (2): the full filename is concatenation of FITSfile and extension ".fit";
the corresponding file is in subdirectory fits.
Spectra are normally dereddened, unless FITSname is terminated
by 'r' (e.g. sp101r) which indicates a naturally reddened spectrum.
Note (3): Very rough classification in 3 groups. 1=ok. 2=still ok, but
not as good as 1, 3=poor (some of these would best be discarded).
Note (4): this column is empty, except if the corresponding star has
been used as a reference for the correction for atmospheric
absorption and for the relative flux calibration. In that case,
the column indicates which Kurucz spectrum has been assumed to
represent the continuum of this star. As a result of the calibration
procedure, the final spectrum for a reference star will follow the
Kurucz model closely (reddened, where necessary).
Note (5): Measured H-K (filters of Bessell and Brett, 1988PASP..100.1134B).
The values are given with 3 digits, but +/- 0.015 mag. is a
reasonable estimate of the 2 sigma error in general.
Note (6): the H-K colour index found in the literature could be different
systems.
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References:
Bessel M.S., Brett J.M., 1988PASP..100.1134B
Lancon A., Rocca-Volmerange B., 1992A&AS...96..593L
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(End) Ariane Lancon [Strasbourg], Francois Ochsenbein [CDS] 26-Feb-1997