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J/A+A/393/167       Mean Spectra for upper AGB stars             (Lancon+, 2002)
The modelling of intermediate-age stellar populations.
II. Average spectra for upper AGB stars, and their use.
    Lancon A., Mouhcine M.
   <Astron. Astrophys. 393, 167 (2002)>
   =2002A&A...393..167L
ADC_Keywords: Stars, late-type ; Stars, variable ; Spectra, red ;
              Spectra, infrared
Keywords: stars: AGB and post-AGB - stars: late-type -
                 stars: variable: general  - Hertzsprung-Russell diagram  -
                 infrared: stars - galaxies: stellar content

Description:
    Provided are average spectra extending from 510 to 2490nm for:
    - Oxygen rich, optically visible LPVs (temperature sequence based on
       the colour I-K);
    - Carbon rich, optically visible LPVs (temperature sequence based on
       the colour R-H, and C/O sequence);
    - Oxygen rich, dust-enshrouded LPVs (reddened versions of the coolest
       optically visible average);
    - Carbon rich, dust-enshrouded LPVs (reddened versions of the coolest
       optically visible average).

File Summary:

       FileName      Lrecl  Records   Explanations

ReadMe            80        .   This file
table12.dat       52       85   Contents of the O- and C-rich temperature bins
bins.dat          65       35   Summary of spectra
o_bin1.dat        20     3961   O-rich, opt. visible LPV, bin 1 in I-K sequence
o_bin2.dat        20     3961   O-rich, opt. visible LPV, bin 2 in I-K sequence
o_bin3.dat        20     3961   O-rich, opt. visible LPV, bin 3 in I-K sequence
o_bin4.dat        20     3961   O-rich, opt. visible LPV, bin 4 in I-K sequence
o_bin5.dat        20     3961   O-rich, opt. visible LPV, bin 5 in I-K sequence
o_bin6.dat        20     3961   O-rich, opt. visible LPV, bin 6 in I-K sequence
o_bin7.dat        20     3961   O-rich, opt. visible LPV, bin 7 in I-K sequence
o_bin8.dat        20     3961   O-rich, opt. visible LPV, bin 8 in I-K sequence
o_bin9.dat        20     3961   O-rich, opt. visible LPV, bin 9 in I-K sequence
c_bin1.dat        20     3961   C-rich, opt. visible LPV, bin 1 in R-H sequence
c_bin2.dat        20     3961   C-rich, opt. visible LPV, bin 2 in R-H sequence
c_bin3.dat        20     3961   C-rich, opt. visible LPV, bin 3 in R-H sequence
c_bin4.dat        20     3961   C-rich, opt. visible LPV, bin 4 in R-H sequence
c_bin5.dat        20     3961   C-rich, opt. visible LPV, bin 5 in R-H sequence
c_co101.dat       20     3961   C-rich, opt. visible LPV, C/O=1.01
c_co110.dat       20     3961   C-rich, opt. visible LPV, C/O=1.10
c_co140.dat       20     3961   C-rich, opt. visible LPV, C/O=1.40
o_b9_2.dat        20     3961   OH/IR template, from O_bin9 reddened with Av=2
o_b9_4.dat        20     3961   OH/IR template, from O_bin9 reddened with Av=4
o_b9_6.dat        20     3961   OH/IR template, from O_bin9 reddened with Av=6
o_b9_8.dat        20     3961   OH/IR template, from O_bin9 reddened with Av=8
o_b9_10.dat       20     3961   OH/IR template, from O_bin9 reddened with Av=10
o_b9_12.dat       20     3961   OH/IR template, from O_bin9 reddened with Av=12
o_b9_14.dat       20     3961   OH/IR template, from O_bin9 reddened with Av=14
o_b9_16.dat       20     3961   OH/IR template, from O_bin9 reddened with Av=16
o_b9_18.dat       20     3961   OH/IR template, from O_bin9 reddened with Av=18
o_b9_20.dat       20     3961   OH/IR template, from O_bin9 reddened with Av=20
o_b9_24.dat       20     3961   OH/IR template, from O_bin9 reddened with Av=24
o_b9_30.dat       20     3961   OH/IR template, from O_bin9 reddened with Av=30
o_b9_40.dat       20     3961   OH/IR template, from O_bin9 reddened with Av=40
c_b5_4.dat        20     3961   IR C-rich star, from C_bin5 reddened with Av=4
c_b5_8.dat        20     3961   IR C-rich star, from C_bin5 reddened with Av=8
c_b5_12.dat       20     3961   IR C-rich star, from C_bin5 reddened with Av=12
c_b5_16.dat       20     3961   IR C-rich star, from C_bin5 reddened with Av=16
c_b5_20.dat       20     3961   IR C-rich star, from C_bin5 reddened with Av=20


See also:
        III/196 : Near-IR stellar spectra from 1.428 to 2.5 um (Lancon+ 1996)
 J/A+AS/146/217 : Library of Spectra (0.5 to 2.5um) of Cool Stars (Lancon+ 2000)


Byte-by-byte Description of file: table12.dat

   Bytes Format Units   Label     Explanations

   1-  2  A2    ---     Bin       [OC0-9] O-rich (O) or C-rich (C) bin name (1)
   4-  5  A2    ---     XBin      [X1-3] Chemical composition bin name (1)
   8- 13  A6    ---     Name      Star Name
  16- 23  A8    ---     Date      Observation date (Month.YYYY)
  26- 27  A2    ---     VType     Variable type
  28- 31  F4.2  ---     C/O       ? C/O ratio, for C-rich bin only  (2)
  34- 38  F5.1  d       Period    Period
  40- 42  F3.1  mag     deltaV    V band amplitude
  44- 47  F4.2  mag     (I-K)     ? I-K colour index (O-rich bin only)
  49- 52  F4.2  mag     (R-H)     ? R-H colour index (C-rich bin only)

Note (1): This bin number is used also in the "bins.dat" file.

Note (2): Atmospheric number ratio of carbon to oxygen, when available,
       according to the estimates of Loidl et al., 2001A&A...371.1065L.


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

   Bytes Format Units   Label     Explanations

   1-  2  A2    ---     Bin       Bin name (Bin or XBin column of table12.dat)
   4-  5  I2    mag     Abs       Absorption value (1)
   7- 17  A11   ---     File      Name of file with spectrum
  19- 65  A47   ---     Text      Title of spectrum file

Note (1):
    Reddened spectra for dust-enshrouded sources are provided for
    the coolest spectra (O9 and C5), using the extinction law of
    Cardelli et al. (1989ApJ...345..245C).


Byte-by-byte Description of file: o_*.dat c_*.dat

   Bytes Format Units   Label     Explanations

   2-  7  F6.0  0.1nm   Lambda    Wavelength
   9- 20  E12.5 10W/nm  FLambda   Flux density: energy per unit wavelength (1)

Note (1): The spectra are normalized in such a way that the integral of
    Flambda.d(lambda) equals 1 (unit of energy), if the wavelengths are
    taken as is (i.e. in Angstroem). The extrapolation to a nil flux
    density at 3500Å and 50000Å, justified in the paper, has been
    taken into account. In addition, the coolest O-rich spectrum (o_bin9)
    has been divided by 1.05 (this assumes that the standard extrapolation
    misses 5% of the total flux); the second coolest C-rich spectrum
    (c_bin4) has been divided by 1.10 (correction for a 10%
    underestimate); the coolest C-rich spectrum (c_bin5) has been divided
    by 1.25 (correction for a 25% underestimate).

    Reddened spectra for dust-enshrouded sources are also provided. For
    the O-rich series, we have used the coolest spectrum (o_bin9),
    normalized as described above, and applied the extinction law of
    Cardelli et al. (1989ApJ...345..245C), as justified in the paper. For
    the C-rich series, we have proceeded in the same way with the coolest
    C-rich average (c_bin5).

    Example of practical use: If you need a given spectrum to represent a
    star with a luminosity of 1 L☉, use the spectrum as it is, and
    simply consider the flux density units to be in L☉/Angstroem
    (the same is valid for any chosen energy unit).


Acknowledgements: Ariane Lancon 

(End)                                          Patricia Bauer [CDS]  14-Jun-2002