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J/A+A/418/103 86GHz SiO maser survey in the Inner Galaxy (Messineo+, 2004)
The following files can be converted to FITS (extension .fit .fgz or .fiZ)
table2.dat
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Query from: http://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/A+A/418/103
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Beginning of ReadMe :J/A+A/418/103 86GHz SiO maser survey in the Inner Galaxy (Messineo+, 2004)
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86 GHz SiO maser survey of late-type stars in the Inner Galaxy.
II. Infrared photometry of the SiO target stars
Messineo M., Habing H.J., Menten K.M., Omont A., Sjouwerman L.O.
<Astron. Astrophys. 418, 103 (2004)>
=2004A&A...418..103M
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ADC_Keywords: Stars, late-type ; Masers ; Photometry, infrared ;
Cross identifications ; Milky Way ; Galactic plane
Keywords: stars: AGB and post-AGB - infrared: stars -
stars: variables: general - circumstellar matter - masers -
Galaxy: stellar content
Abstract:
We present a compilation and study of DENIS, 2MASS, ISOGAL, MSX and
IRAS 1-25 microns photometry for a sample of 441 late-type stars in
the inner Galaxy, which we previously searched for 86GHz SiO maser
emission (Messineo et al., 2002, Cat. J/A+A/393/115). The comparison
of the DENIS and 2MASS J and Ks magnitudes shows that most of the SiO
targets are indeed variable stars. The MSX colours and the IRAS
[12]-[25] colour of our SiO targets are consistent with those of Mira
type stars with dust silicate feature at 9.7 microns feature in
emission, indicating only a moderate mass-loss rate.
Description:
A catalogue of infrared photometry from DENIS (bulge PSC), 2MASS (all
sky data release), ISOGAL (PSC 1.0), MSX (PSC 1.2) and IRAS (PSC 2.0)
is presented for a sample of stars which we previously searched for
SiO maser emission. The identification source numbers (e.g #99) are
taken from Table 2 (86GHz SiO maser detections) and Table 3
(non-detections) in Messineo et al. (2002, Cat. J/A+A/393/115). The
number of targeted positions searched for SiO maser emission in
Messineo et al. (2002, Cat. J/A+A/393/115) is 441. As three
positions showed a double 86GHz SiO maser detection, the line
identification number goes up to 444. For two of these three
positions, we were able to identify two distinct possible infrared
counterparts within the IRAM beam.