J/A+A/374/968 Photometric and kinematic properties of LPVs (Mennessier+, 2001)
Long Period Variable Stars:
galactic populations and infrared luminosity calibrations.
Mennessier M.O., Mowlavi N., Alvarez R., Luri X.
<Astron. Astrophys. 374, 968 (2001)>
=2001A&A...374..968M 2001A&A...374..968M
=2001A&A...380..198M 2001A&A...380..198M
ADC_Keywords: Stars, variable ; Photometry, infrared ; Magnitudes, absolute
Keywords: stars: absolute magnitude - variable stars - kinematics -
galactic populations - AGB
Description:
The table gives individual absolute K and IRAS 12 and 25 luminosities
of 800 LPVs. They are obtained by applying the Luri-Mennessier (LM,
see below) calibration method to a sample composed of stars which are
either of type M (O-rich), C (C-rich) or S (C/O∼1), including Mira
(M), SR (of both type a and b) and L variables. Astrometric data is
taken exclusively from the HIPPARCOS Catalogue. Radial velocities are
taken from the HIPPARCOS Input Catalogue. K band photometric data are
gathered from various sources. Infrared magnitudes are derived from
the fluxes measured by the IRAS satellite: m(12)=3.63-2.5log(F(12))
and m(25)=2.07-2.5log(F(25))
The stellar population from which the sample is extracted is assumed
to be composed of several distinct groups that can differ in
kinematics, luminosity or spatial distribution. The LM method
determines the number of significant discriminating groups and
produces, for each group, unbiased estimates of the mean parameters of
the galactic and luminosity model. In a second step the method uses a
Bayesian rule to statistically assign each star to a group. Table
gives these assignations denoted as G(G') i.e. to group G in K and
G'in IRAS.
Three groups are identified in the K band. They can be interpreted as
the galactic disk (D), old disk (OD) and extended disk (ED)
populations. Four groups are identified in the IRAS bands. They are
similar to those identified in the K band except that the old disk
group is divided into ``bright'' (ODb) and ``faint'' (ODf) subgroups.
Let us add that D, ODb and ED correspond to thick circumstellar
envelope stars, while ODf is mainly composed of stars with a thin (or
even lacking) envelope.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
annex.dat 61 824 Individual K, 12 and 25 luminosities
annex.tex 80 981 LaTeX version of annex.dat
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See also:
I/239 : The Hipparcos and Tycho Catalogues (ESA 1997)
J/A+AS/124/143 : Light curves of O and C-rich LPV's (Mennessier+ 1997)
Byte-by-byte Description of file: annex.dat
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Bytes Format Units Label Explanations
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1- 6 I6 --- HIP HIPPARCOS (Cat. I/239) number
8- 18 A11 --- Name GCVS or NSV identifier, if known
21- 24 A4 --- Types Variability and spectral types (1)
27- 33 A7 --- Group Assigned groups (2)
36- 40 F5.2 mag KMAG ? estimated K absolute magnitude
43- 48 F6.2 mag 12MAG ? estimated 12µm absolute magnitude
51- 56 F6.2 mag 25MAG ? estimated 25µm absolute magnitude
59- 61 A3 --- pec Specificity (3)
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Note (1): Variability and spectral types:
M = Mira, SR = semi regular, L = irregular
O = O-rich, C = C-rich ,S = S spectral type star
Note (2): Groups:
D: galactic disk
OD: old disk
ODb: bright old disk group
ODf: faint old disk group
ED: extended disk
Note (3): Specificity:
BD: bright galactic disk star from V calibration
pec: peculiar star
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Acknowledgements:
Marie-Odile Mennessier
(End) Patricia Bauer [CDS] 31-May-2001