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Pulkovo compilation of radial velocities for 35495 stars in a common system.
Not Available
| Merged catalogue of reflection nebulae
Several catalogues of reflection nebulae are merged to create a uniformcatalogue of 913 objects. It contains revised coordinates,cross-identifications of nebulae and stars, as well as identificationswith IRAS point sources.The catalogue is only available in electronic form at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/399/141
| Spectroscopic investigations of classical Cepheids and main-sequence stars in galactic open clusters and associations. II. Open cluster Platais 1 (C2128+488) and small-amplitude Cepheid V1726 Cygni
The small-amplitude Cepheid V1726 Cyg and two membersof open cluster Platais 1 (Platais 1 star No. 1(1921) and Platais 1 star No. 111 (1600))were investigated, using high-resolution CCD spectra. The followingresults were obtained: 1) All objects have the same metallicities, closeto that of the Sun (for V1726 Cyg weighted average [Fe/H]=+0.05, forPlatais 1 star No. 1 (1921) [Fe/H]=+0.13); 2) values of Teffand log g for the B-stars are in excellent agreement with thosedetermined from (B-V) colour indices using a (B-V) ~ (Teff,log g) calibration; 3) the elemental abundances indicate that V1726 Cygis in the post first dredge-up stage with an age near 1.5 x108, and is crossing the Cepheid instability strip for thethird time. Mean values of Teff=6100 K and log g=2.35 +/-0.05 permit us to refine its colour excess to EB-V=0fm 33,which for a distance of d = 1568+/- 13 pc corresponds toMV=-2fm 99. The Cepheid could therefore be pulsating in thefundamental tone, although pulsation in the first overtone is notexcluded; 4) Platais 1 Star No. 1 (1921) is a slowly rotating HgMn-starwith a high helium content, while Platais 1 star No. 111 (1600) is arapidly rotating main-sequence star with a helium content comparable tothat of the Sun; 5) the age of the open cluster is estimated to be about2.5 x 108 yr. Based on the spectra collected with the 6-mtelescope SAO RAS.
| Spectroscopic investigations of classical Cepheids and main-sequence stars in galactic open clusters and associations. I. Association Cas OB2 and the small-amplitude Cepheid SU Cassiopeae
The small-amplitude Cepheid SU Cas and four membersof the association Cas OB2 (HD 16893, HD17327a and b, HD 17443) were investigated,using high-resolution CCD spectra. The following results were obtained:1) All these objects have the same metallicity values, close to that ofthe Sun; 2) Elemental abundance indicates that SU Cas is a post firstdredge-up star with an age from 1 108 to 1.45 108yr, and it is not crossing the Cepheid instability strip for the firsttime. The mean value of log g = 2.35 corresponds to pulsations in thefundamental tone, although errors in gravity estimations provideovertone pulsations. The questions about its pulsational mode andmembership in Cas OB2 remained open; 3) HD17327a is a slowly rotating HgMn-star with the highest heliumcontent among such objects, while HD 16893 also has a manganeseoverabundance and might be classified as an Am-star; 4) HD17327b and HD 17443 are rapidly rotating main-sequence stars,while HD 17443 has a helium content comparable with that of the Sun.
| Polarization measurements of Vega-like stars
Optical linear polarization measurements are presented for about 30Vega-like stars. These are then compared with the polarization observedfor normal field stars. A significant fraction of the Vega-like starsare found to show polarization much in excess of that expected to be dueto interstellar matter along the line of sight to the star. The excesspolarization must be intrinsic to the star, caused by circumstellarscattering material that is distributed in a flattened disk. Acorrelation between infrared excess and optical polarization is foundfor the Vega-like stars.
| A HIPPARCOS Census of the Nearby OB Associations
A comprehensive census of the stellar content of the OB associationswithin 1 kpc from the Sun is presented, based on Hipparcos positions,proper motions, and parallaxes. It is a key part of a long-term projectto study the formation, structure, and evolution of nearby young stellargroups and related star-forming regions. OB associations are unbound``moving groups,'' which can be detected kinematically because of theirsmall internal velocity dispersion. The nearby associations have a largeextent on the sky, which traditionally has limited astrometricmembership determination to bright stars (V<~6 mag), with spectraltypes earlier than ~B5. The Hipparcos measurements allow a majorimprovement in this situation. Moving groups are identified in theHipparcos Catalog by combining de Bruijne's refurbished convergent pointmethod with the ``Spaghetti method'' of Hoogerwerf & Aguilar.Astrometric members are listed for 12 young stellar groups, out to adistance of ~650 pc. These are the three subgroups Upper Scorpius, UpperCentaurus Lupus, and Lower Centaurus Crux of Sco OB2, as well as VelOB2, Tr 10, Col 121, Per OB2, alpha Persei (Per OB3), Cas-Tau, Lac OB1,Cep OB2, and a new group in Cepheus, designated as Cep OB6. Theselection procedure corrects the list of previously known astrometricand photometric B- and A-type members in these groups and identifiesmany new members, including a significant number of F stars, as well asevolved stars, e.g., the Wolf-Rayet stars gamma^2 Vel (WR 11) in Vel OB2and EZ CMa (WR 6) in Col 121, and the classical Cepheid delta Cep in CepOB6. Membership probabilities are given for all selected stars. MonteCarlo simulations are used to estimate the expected number of interloperfield stars. In the nearest associations, notably in Sco OB2, thelater-type members include T Tauri objects and other stars in the finalpre-main-sequence phase. This provides a firm link between the classicalhigh-mass stellar content and ongoing low-mass star formation. Detailedstudies of these 12 groups, and their relation to the surroundinginterstellar medium, will be presented elsewhere. Astrometric evidencefor moving groups in the fields of R CrA, CMa OB1, Mon OB1, Ori OB1, CamOB1, Cep OB3, Cep OB4, Cyg OB4, Cyg OB7, and Sct OB2, is inconclusive.OB associations do exist in many of these regions, but they are eitherat distances beyond ~500 pc where the Hipparcos parallaxes are oflimited use, or they have unfavorable kinematics, so that the groupproper motion does not distinguish it from the field stars in theGalactic disk. The mean distances of the well-established groups aresystematically smaller than the pre-Hipparcos photometric estimates.While part of this may be caused by the improved membership lists, arecalibration of the upper main sequence in the Hertzsprung-Russelldiagram may be called for. The mean motions display a systematicpattern, which is discussed in relation to the Gould Belt. Six of the 12detected moving groups do not appear in the classical list of nearby OBassociations. This is sometimes caused by the absence of O stars, but inother cases a previously known open cluster turns out to be (part of) anextended OB association. The number of unbound young stellar groups inthe solar neighborhood may be significantly larger than thoughtpreviously.
| Accurate Positions for MCG Galaxies
We have measured accurate celestial coordinates for 4741 extragalacticobjects, primarily drawn from a list of MCG galaxies with no recentlypublished accurate positions. The standard deviations in the newpositions depend slightly on the measurement method but are on the orderof 1.0" to 1.2". Standard deviations in the original MCG positions areconfirmed to be at the 1.5′-2.0′ level. These new positionswere integrated into NED in 1997 December.
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| A Study of the Kinematics of the Local Dark Clouds
Not Available
| SAO stars with infrared excess in the IRAS Point Source Catalog
We have undertaken a search for SAO stars with infrared excess in theIRAS Point Source Catalog. In contrast to previous searches, the entireIRAS (12)-(25)-(60) color-color diagram was used. This selection yieldeda sample of 462 stars, of which a significant number are stars withcircumstellar material. The stars selected can be identified aspre-main-sequence stars, Be stars, protoplanetary systems, post-AGBstars, etc. A number of objects are (visual) binary stars.Characteristic temperatures and IR excesses are calculated and theirrelations to spectral type are investigated.
| Identification of the pulsation modes of the evolved hot Delta Scuti star SAO 4710
Abstract image available at:http://adsabs.harvard.edu/abs/1990A&A...230...91M
| Space reddenings for six Cepheid variables
Color excesses are derived for six galactic Cepheids from reddeningsfound for neighboring stars which seem likely to be physicallyassociated with each variable. The Cepheids studied are: SU Cas, whichis associated with a dust complex and R association; Zeta Gem and AlphaUMi, which have F dwarfs as close companions; BB Sgr and SZ Tau, whichlie in the coronal regions of the clusters Collinder 394 and NGC 1647,respectively; and SV Vul, which is involved in an older region of theassociation Vul OB1. The derived reddenings are in good agreement withother, independent, estimates from the literature.
| An investigation of the stellar association containing the 1.95 day Cepheid SU Cassiopeiae
The results of photometric and spectroscopic observations of SU Cas andthe surrounding dust complex are reported. UBV photometry was made ofearly type stars in the dust complex on eight nights in 1978-79 and afurther 10 stars were surveyed within 7 arcmin of SU Cas. Spectroscopicmeasurements were also made of the objects in order to obtain radialvelocities and equivalent widths. The data suggest the region has amoving cluster (BA association) 30 pc in angular extent, with the 1.95arcday Cepheid SU Cas as a member. The association is 255-261 pc distantand has a 6 pc spread between members. The association stars are around120 Myr old, typical of 4 solar mass stars. Finally, the core membersinclude visual and spectroscopic binary system and a short-periodCepheid.
| Wolf 630 - A peculiar astrometric binary
A semimajor photocentric orbit axis of 0.052 + or - 0.007 arc isindicated by an analysis of 55 plates of Wolf 630, in close agreementwith the 0.056 + or - 0.018 arcmin previously reported. A comparison offractional mass and absolute visual magnitude values arrived at in thisinvestigation with those of other M dwarfs of known mass, it appearsthat the A component is the more normal of the two, and that the Bcomponent is underluminous for its mass by two or three magnitudes.
| A Star of Very Low Luminosity
Abstract image available at:http://adsabs.harvard.edu/abs/1981MNRAS.196P..15R
| Metal abundance and microturbulence in F0-G2 stars and the calibration of the Stromgren m1 index
The strengths of two narrow groups of metal lines are measuredphotoelectrically by means of an echelle spectrometer for 16 F0-G2 giantfield stars and for 12 Hyades main-sequence stars. A model-atmosphereanalysis of these observations and similar observations of main-sequencefield stars observed earlier results in the determination of the metalabundance for 179 stars. In addition, the microturbulence parameter isdetermined for 73 of these stars. The internal accuracy of the resultsis estimated to be plus or minus 0.08 for the logarithmicmetal-to-hydrogen ratio and plus or minus 0.2 km/sec for themicroturbulence parameter. The metal abundances are found to agree verysatisfactorily with values of the logarithmic iron-to-hydrogen ratiodetermined from classical coude spectroscopy regarding both zero pointand scale. It is found that the microturbulence parameter is a functionof the effective temperature and the surface gravity. It increases from1.2 km/sec for solar type stars to approximately 3.0 km/sec for earlyF-type giants.
| Molecular clouds associated with reflection nebulae. I - A survey of carbon monoxide emission
The paper presents 2.6 mm wavelength CO and (C-13)O observations of 130molecular clouds associated with reflection nebulae. Enhanced COemission was found in the vicinity of the illuminating star in abouthalf the objects studied. There is a tendency for the CO peak to beslightly displaced from the star. Many examples of peaks that appear toresult from heating of the cloud by the nearby star are found, whileothers appear to be associated with independent concentrations ofmaterial.
| Luminosity and motion of large proper-motion stars. I - Stars with annual proper motion larger than 1 arcsec
The luminosities and motions of stars brighter than visual magnitude 15and annual proper motion greater than one arcsec given in a catalogpublished by the author (1979) are discussed on the basis of the (RI)photometry available for these objects. Pending subsequent discussionsof data contained in two additional catalogs, it is concluded that thefirst catalog contains 100 subdwarfs extending to an infrared magnitudeof +11.5 mag. If these are halo objects, the number density-luminosityfunction has a steeper slope than the general luminosity function,indicating that the mass density may be greater than normallyrecognized. The luminosity law for the old disk stars in this catalogclosely conforms to the slope of the general luminosity function fromvisual magnitude +4.5 to +13; however, there is an excess of stars oflower luminosity.
| The distance of the Cepheid SU CAS and its pulsation mode
Racine (1968) has used field stars which illuminate reflection nebulaenear SU Cas to determine the distance of the Cepheid. These stars havebeen reobserved in the four-color and H-beta system and found to be atseveral different distances. If SU Cas is associated with one of them,HD 17706, it must be a first-overtone pulsator. However, since thereflection nebulae in the region appear to be mostly unrelated to eachother, the case for overtone pulsation in this star is very weak, andits distance can not be reliably determined in this way.
| Distance of the cepheid SU Cas.
Abstract image available at:http://adsabs.harvard.edu/abs/1968AJ.....73..588R
| Stars in reflection nebulae
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1968AJ.....73..233R&db_key=AST
| A study of reflection nebulae.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1966AJ.....71..990V&db_key=AST
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| Takýmyýldýz: | Zincirli Prenses |
| Sað Açýklýk: | 02h51m32.77s |
| Yükselim: | +67°48'54.2" |
| Görünürdeki Parlaklýk: | 8.752 |
| Uzaklýk: | 341.297 parsek |
| özdevim Sað Açýklýk: | 12.3 |
| özdevim Yükselim: | -10.4 |
| B-T magnitude: | 9.118 |
| V-T magnitude: | 8.783 |
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