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Hipparcos red stars in the HpV_T2 and V I_C systems
For Hipparcos M, S, and C spectral type stars, we provide calibratedinstantaneous (epoch) Cousins V - I color indices using newly derivedHpV_T2 photometry. Three new sets of ground-based Cousins V I data havebeen obtained for more than 170 carbon and red M giants. These datasetsin combination with the published sources of V I photometry served toobtain the calibration curves linking Hipparcos/Tycho Hp-V_T2 with theCousins V - I index. In total, 321 carbon stars and 4464 M- and S-typestars have new V - I indices. The standard error of the mean V - I isabout 0.1 mag or better down to Hp~9 although it deteriorates rapidly atfainter magnitudes. These V - I indices can be used to verify thepublished Hipparcos V - I color indices. Thus, we have identified ahandful of new cases where, instead of the real target, a random fieldstar has been observed. A considerable fraction of the DMSA/C and DMSA/Vsolutions for red stars appear not to be warranted. Most likely suchspurious solutions may originate from usage of a heavily biased color inthe astrometric processing.Based on observations from the Hipparcos astrometric satellite operatedby the European Space Agency (ESA 1997).}\fnmsep\thanks{Table 7 is onlyavailable in electronic form at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/397/997
| SANTIAGO 91, a right ascension catalogue of 3387 stars (equinox J2000).
The positions in right ascension of 3387 stars belonging to the Santiago67 Catalogue, observed with the Repsold Meridian Circle at Cerro Calan,National Astronomical Observatory, during the period 1989 to 1994, aregiven. The average mean square error of a position, for the wholeCatalogue, is +/-0.009 s. The mean epoch of the catalogue is 1991.84.
| IRAS low-resolution spectral observations of the 10 and 18 micron silicate emission feature
The IRAS LRS Atlas contains 8-23 micron spectra of 1816 stars withsilicate emission features. In order to study the shapes of the silicatedust features, the 117 stars whose emission features appear to beoptically thin and which have the best signal-to-noise ratio at thelongest wavelengths were analyzed. Simple spherical dust shell modelswere calculated in both the optically thin and the slightly opticalthick approximations. From the comparison of the predicted spectra ofthe dust and stellar continuum, the emissivity function Kappa(lambda)was derived. In the different stars, the shape of the 10-micron featureis either narrow or broad and it is peaked either at about 9.7 micronsor at 10 microns. Either particle size effects (particles above 0.75microns in radius) or optical depth effects (central optical depth about1) could broaden the 10-micron feature. Chemical composition differencesno doubt are also important, particularly as regards the position of thepeak of the 10-micron feature. The stars with the peak at 10 microns aremore closely confined to the Galactic plane than the stars with the peakat 9.7 microns. The shape of the 18-micron feature is essentially thesame in all stars, and can be used to extend the interstellar extinctioncurve past 13 to 22 microns.
| Classification of 831 two-micron sky survey sources south of +5 degrees.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1975AJ.....80.1011H&db_key=AST
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