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 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:
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FileName Lrecl Records Explanations
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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
ob92.dat 20 3961 OH/IR template, from O_bin9 reddened with Av=2
ob94.dat 20 3961 OH/IR template, from O_bin9 reddened with Av=4
ob96.dat 20 3961 OH/IR template, from O_bin9 reddened with Av=6
ob98.dat 20 3961 OH/IR template, from O_bin9 reddened with Av=8
ob910.dat 20 3961 OH/IR template, from O_bin9 reddened with Av=10
ob912.dat 20 3961 OH/IR template, from O_bin9 reddened with Av=12
ob914.dat 20 3961 OH/IR template, from O_bin9 reddened with Av=14
ob916.dat 20 3961 OH/IR template, from O_bin9 reddened with Av=16
ob918.dat 20 3961 OH/IR template, from O_bin9 reddened with Av=18
ob920.dat 20 3961 OH/IR template, from O_bin9 reddened with Av=20
ob924.dat 20 3961 OH/IR template, from O_bin9 reddened with Av=24
ob930.dat 20 3961 OH/IR template, from O_bin9 reddened with Av=30
ob940.dat 20 3961 OH/IR template, from O_bin9 reddened with Av=40
cb54.dat 20 3961 IR C-rich star, from C_bin5 reddened with Av=4
cb58.dat 20 3961 IR C-rich star, from C_bin5 reddened with Av=8
cb512.dat 20 3961 IR C-rich star, from C_bin5 reddened with Av=12
cb516.dat 20 3961 IR C-rich star, from C_bin5 reddened with Av=16
cb520.dat 20 3961 IR C-rich star, from C_bin5 reddened with Av=20
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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
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Bytes Format Units Label Explanations
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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)
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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 2001A&A...371.1065L.
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Byte-by-byte Description of file: bins.dat
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Bytes Format Units Label Explanations
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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
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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 1989ApJ...345..245C).
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Byte-by-byte Description of file: o_*.dat c_*.dat
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Bytes Format Units Label Explanations
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2- 7 F6.0 0.1nm Lambda Wavelength
9- 20 E12.5 10W/nm FLambda Flux density: energy per unit wavelength (1)
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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 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).
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Acknowledgements: Ariane Lancon
(End) Patricia Bauer [CDS] 14-Jun-2002