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 µm.
    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: stars: atlas - stars: infrared spectroscopy -
          stars: temperature and colours

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:

       FileName      Lrecl  Records   Explanations

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/*             0       95   Subdirectory with the 95 FITS spectra

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 "" should be changed into ""--------------------------------------------------------------------------------

Byte-by-byte Description of file: stars.dat


Byte-by-byte Description of file: stars.dat

   Bytes Format Units   Label    Explanations

       1  A1    ---     LC       [dgc] Luminosity 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 "fits" subdirectory (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

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.


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