J/A+A/492/277 Analysis of Collinder 69 stars with VOSA (Bayo+, 2008)
VOSA: virtual observatory SED analyzer.
An application to the Collinder 69 open cluster.
Bayo A., Rodrigo C., Barrado Y Navascues D., Solano E., Gutierrez R.,
Morales-Calderon M., Allard F.
<Astron. Astrophys., 492, 277-287 (2008)>
=2008A&A...492..277B 2008A&A...492..277B
ADC_Keywords: Stars, dwarfs ; Stars, atmospheres ; Associations, stellar ;
Effective temperatures ; Isochrones
Keywords: astronomical data bases: miscellaneous - stars: formation -
stars: circumstellar matter - stars: low-mass, brown dwarfs -
stars: Hertzsprung-Russell (HR) and C-M diagrams -
Galaxy: open clusters and associations: individual: Collinder 69
Abstract:
The physical properties of almost any kind of astronomical object can
be derived by fitting synthetic spectra or photometry extracted from
theoretical models to observational data.
We want to develop an automatic procedure to perform this kind of
fitting to a relatively large sample of members of a stellar
association and apply this methodology to the case of Collinder 69.
We combine the multiwavelength data of our sources and follow a
work-flow to derive the physical parameters of the sources. The key
step of the work-flow is performed by a new VO-tool, VOSA. All the
steps in this process are done in a VO environment.
Description:
Parameters derived for each individual source of the sample. For
some of the sources, we have not been able to interpolate between
the isochrones and evolutionary tracks (to infer ages and masses),
because of their peculiar location in the HR diagram; we have grouped
these sources in four possible categories according to the probable
cause for this peculiar location (last column of the table).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 63 167 Parameters derived for each individual source
of the sample (167 sources)
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See also:
J/ApJ/664/481 : Collinder 69 optical/IR photometry (Barrado y Navascues+ 2007)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- --- [LOri]
5- 7 I03 --- LOri Name of the source as in Barrado et al.
(2007, Cat. J/ApJ/664/481)
9- 15 A7 --- Model Best fitting model collection
17- 20 I4 K Teff Effective temperature
22- 24 F3.1 [cm/s2] log(g) Surface gravity (log)
26- 29 F4.2 --- Fobs/Ftot Ratio of observed to total flux
31- 37 E7.3 solLum Lbol Bolometric luminosity
39- 45 E7.2 solLum e_Lbol Error in Bolometric Luminosity
47- 50 F4.1 Myr Age ? Estimated Age
52- 57 F6.4 solMass Mass ? Stellar mass
61 A1 --- --- [[]
62 A1 --- Note Peculiar location in HR diagram (1)
63 A1 --- --- []]
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Note (1): Categories of peculiarities as follows:
[1] = Source with disk
[2] = Previous "non-member" candidates according to the photometric
properties (see Barrado et al. (2007, Cat. J/ApJ/664/481)
for further details)
[3] = Degenerated fit due the small number of points to be fitted vs
number of free parameters
[4] = possible foreground cool source
[*] = For a more detailed analysis in LOri167 see Barrado et al.
(2007A&A...468L...5B 2007A&A...468L...5B).
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Acknowledgements:
Amelia Bayo, abayo(at)eso.org
References:
Barrado et al., 2007ApJ...664..481B 2007ApJ...664..481B, Cat. J/ApJ/664/481
Spitzer: Accretion in Low-Mass Stars and Brown Dwarfs in the
lambda Orionis Cluster
Barrado et al., 2007A&A...468L...5B 2007A&A...468L...5B
The young, wide and very low mass visual binary Lambda Orionis 167
(End) Amelia Bayo [LAEFF-CAB, INTA-CSIS], Patricia Vannier [CDS] 27-Nov-2008