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Pulkovo compilation of radial velocities for 35495 stars in a common system.
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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
| Radial velocities of giant M stars near the ecliptic
A search dedicated to the identification of new, dwarf and cold starsclose to the Sun has allowed us to measure the radial velocities of aset of stars of late spectral type. The stars selected were M-type starspresent in the Hipparcos Input Catalogue located in a strip of+/-20° around the Ecliptic and observables from La Silla. Our inalset contains 22 M-type stars whose radial velocities Vr havebeen measured with an accuracy of ~ 0.5 km s-1 during asingle observing run. From their velocities, parallaxes and magnitudeswe deduce that all the stars observed are red giants, with spacevelocities relative to the Sun mostly lower than 100 km s-1.Based on observations collected at the CAT telescope, European SouthernObservatory, La Silla, Chile.
| Stars with the Largest Hipparcos Photometric Amplitudes
A list of the 2027 stars that have the largest photometric amplitudes inHipparcos Photometry shows that most variable stars are all Miras. Thepercentage of variable types change as a function of amplitude. Thiscompilation should also be of value to photometrists looking forrelatively unstudied, but large amplitude stars.
| The 74th Special Name-list of Variable Stars
We present the Name-list introducing GCVS names for 3153 variable starsdiscovered by the Hipparcos mission.
| Classification and Identification of IRAS Sources with Low-Resolution Spectra
IRAS low-resolution spectra were extracted for 11,224 IRAS sources.These spectra were classified into astrophysical classes, based on thepresence of emission and absorption features and on the shape of thecontinuum. Counterparts of these IRAS sources in existing optical andinfrared catalogs are identified, and their optical spectral types arelisted if they are known. The correlations between thephotospheric/optical and circumstellar/infrared classification arediscussed.
| Mass-losing stars in the South Galactic CAP
Observations are presented for 162 late-type stars in the South GalacticCap (b<-30 deg) which were selected on the basisof their IRAS 25/12-μm flux ratios as high-mass-loss candidates. JHKLphotometry (over 1100 observations) was obtained for all of the stars,BV(RI)_C photometry for 78 of them and optical spectra for 51. 154 ofthese stars are non-Mira M or S stars, of which many, and possibly all,are semi-regular variables. Of the remaining eight IRAS objects, threeare T Tauri stars, three are interacting binaries and two are carbonstars. A few of the M giants and both of the carbon stars havecircumstellar envelopes of the type more normally associated with Miravariables. These include two 1612-MHz OH maser sources. It is suggestedthat such stars may have been Miras in the recent past, but arecurrently out of the instability strip owing to a recently experiencedhelium-shell flash. Alternatively, some of them could be binary stars,but there is as yet no evidence for the second star. The near-infraredcolours of the M giants are compared with those of similar stars in theBulge. They are similar to those of the inner Bulge and unlike thosefound in either the outer Bulge or the globular clusters. The kinematicsand Galactic distribution of the M giants indicate that they areprobably from a mixed population and that they could be associated withMiras with a range of periods. A comparison of the observed colours withthose derived from models indicates a range of metallicity with the bulkof stars slightly more metal-rich than the Sun. It also revealssignificant numbers of stars with colours outside the predicted range,possible due to the effects of circumstellar reddening or toinadequacies in the models. The most metal-rich examples of the M starshave high mass-loss rates for non-Miras (~10^-6 M_solar yr^-1) and thereare far fewer of them outside than inside the solar circle. This may bedue to a metallicity gradient. These stars have a scaleheight of morethan 500 pc. The two carbon stars have unusual colours and detachedshells. One of them, R Scl, is shown to vary with a period of 379dsuperimposed on a possible second period of about 2300d. The othercarbon star, which is more distant and previously unknown, may also havedouble-period variations.
| Circumstellar dust envelopes of oxygen-rich AGB stars.
Using IRAS observational data, the best-fitting models are searched foroxygen-rich AGB stars in various evolutionary stages from opticallyvisible red giant stars to OH/IR stars with heavy mass loss. The modelinfrared spectral energy distributions of the red giant stars withcircumstellar dust envelopes are calculated with the use of a radiativetransfer code. It is found that the oxygen-rich IRAS AGB starssurrounded by circumstellar dust envelopes are divided into threegroups, which can be clearly distinguished by their mass loss rate andthe grain temperature at the inner boundary of the circumstellar dustenvelopes. One group corresponds to Mira type objects with a moderatemass loss rate and a grain formation temperature of about 500 K, thesecond to OH/IR star type objects with a large mass loss rate and a highgrain formation temperature, and the third to M stars with a very coldgrain temperature at the inner boundary, indicating that the moderatemass loss stopped a considerable time ago in these objects. The highergrain formation temperature of the OH/IR star type objects indicates agrain formation point closer to the stellar surface, suggesting aneffective acceleration of dust grains by radiation pressure. Such aneffective acceleration can play an important role in the mass lossphenomena of OH/IR stars with large mass loss rates. From the modelfitting results, it is suggested that an AGB star undergoes severaldozen phases of moderate mass loss of˙(M)~10^-7^-10^-6^Msun_/yr for a period of10^3^-10^4^years with interruptions of 10^3^-10^4^years during theordinary Mira variable phase before becoming an OH/IR star with a massloss rate exceeding 10^-5^Msun_/yr and a lifetime of about10^3^-10^4^years.
| A survey for infrared excesses among high galactic latitude SAO stars
This project involves extending the previous analysis of infraredexcesses among a volume-limited sample of 134 nearby A-K main-sequencestars to a magnitude-limited sample of stars, culled from the SAOCatalog, with excesses determined from the IRAS Point Source Catalogflux density ratios. This new sample includes 5706 B-M type stars, 379of which have infrared excesses. The objective involved use of astatistically complete survey of objects in a standard catalog in orderto assess the frequency with which different physical processes canaffect the infrared output of stars. These processes include, but arenot limited to, orbiting cold particle clouds and the onset of rapidmass loss. It is concluded that cold disks are consistent with theinfrared excesses found among A-G dwarfs and G-K giants in the sample.
| M Giant Populations and Galactic Structure
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1990MNRAS.247..227F&db_key=AST
| Photoelectric photometry of M-type stars
UBVRI photoelectric photometry was obtained for 110 M-type starscontained in the Caltech Two-Micron Survey and the revised AFGL Catalog.Of the 110 stars, 58 have a color index (B-R) greater than or equal to 4mag. A graph is given of (V-R) versus (V-I) for the present stars.
| IRAS catalogues and atlases - Atlas of low-resolution spectra
Plots of all 5425 spectra in the IRAS catalogue of low-resolutionspectra are presented. The catalogue contains the average spectra ofmost IRAS poiont sources with 12 micron flux densities above 10 Jy.
| Late M stars found in a hemispheric survey
An objective-prism survey of somewhat more than half the sky, being theportion more than 10 deg from the Galactic plane and north ofdeclination -25 deg, has been completed, using the visual-red spectralregion. From this survey 583 late M stars (mostly type M6 or later) notcontained in the third edition of the variable star catalog or itssupplements are listed. Many identifications with the Caltech Two-MicronSurvey are given. The great majority of the stars are likely to begiants. For an assumed visual absolute magnituge of -0.9, the distanceof the stars from the Galactic plane is well represented by anexponential (barometric) distribution with scale height 1800 pc; or 900pc for an assumed absolute magnitude of zero. The sample may well berelated, therefore, to the recently discussed 'thick disk' component ofgalactic structure. Carbon stars appear to be at least twice asnumerous, relative to late M stars, at large Galactic Z as at small Z.Although difficult to quantify, it appears unlikely that large numbersof these late M stars are undiscovered variables of appreciableamplitude.
| A survey of infrared stars and planetary nebulae for circumstellar OH emission
The 1000-ft Arecibo antenna was used to survey a total of 76 late-typestars, IRC and CRL infrared sources, and planetary nebulae in the 1612-,1665-, and 1667-MHz lines of the OH molecule. OH was detected for thefirst time in eight objects, most of which are cool, evolved, giantstars. No planetary nebulae were detected nor were any stars previouslyclassified or suggested to be either carbon-rich or S-type, including,for example, CRL 618, IRC+10216, BD 30 deg 3639, Chi Cyg, FG Sge, CRL2688, CRL 3068, NGC 6572, and CRL 3099. High signal-to-noise spectrawere obtained for some known OH maser stars such as NML Tau andIRC+10011.
| Characteristics of OH emission from infrared stars.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1972A&A....17..385W&db_key=AST
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Pozíciós és asztrometriai adatok
| Csillagkép: | Sas |
| Rektaszcenzió: | 22h02m56.36s |
| Deklináció: | +00°04'11.6" |
| Vizuális fényesség: | 9.276 |
| RA sajátmozgás: | 43.9 |
| Dec sajátmozgás: | -2.3 |
| B-T magnitude: | 10.844 |
| V-T magnitude: | 9.406 |
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