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The Star Formation History and Mass Function of the Double Cluster h and χ Persei
The h and χ Per ``double cluster'' is examined using wide-field(0.98d×0.98d) CCD UBV imaging supplemented by optical spectra ofseveral hundred of the brightest stars. Restricting our analysis to nearthe cluster nuclei, we find identical reddenings [E(B-V)=0.56+/-0.01],distance moduli (11.85+/-0.05), and ages (12.8+/-1.0 Myr) for the twoclusters. In addition, we find an initial mass function slope for eachof the cluster nuclei that is quite normal for high-mass stars,Γ=-1.3+/-0.2, indistinguishable from a Salpeter value. We derivemasses of 3700 Msolar (h) and 2800 Msolar (χ)integrating the present-day mass function from 1 to 120Msolar. There is evidence of mild mass segregation within thecluster cores. Our data are consistent with the stars having formed at asingle epoch; claims to the contrary are very likely due to theinclusion of the substantial population of early-type stars located atsimilar distances in the Perseus spiral arm, in addition tocontamination by G and K giants at various distances. We discuss theuniqueness of the double cluster, citing other examples of suchstructures in the literature but concluding that the nearly identicalnature of the two cluster cores is unusual. We fail to settle thelong-standing controversy regarding whether or not the double cluster isthe core of the Per OB1 association and argue that this may beunanswerable with current techniques. We also emphasize the need forfurther work on the pre-main-sequence population of this nearby andhighly interesting region.
| UBVI and Hα Photometry of the h and χ Persei Cluster
UBVI and Hα photometry is presented for 17319 stars in vicinity ofthe young double cluster h and χ Persei. Our photometry extends overa 37'×1deg field centered on theassociation. We construct reddening contours within the imaged field. Wefind that the two clusters share a common distance modulus of11.75+/-0.05 and ages of logage(yr)=7.1+/-0.1. From the V-Hαcolor, a measure of the Hα emission strength, we conduct a surveyfor emission line objects within the association. We detect a sample of33 Be stars, eight of which are new detections. We present a scenario ofevolutionary enhancement of the Be phenomenon to account for the peak inBe fraction toward the top of the main sequence in the population of hand χ Persei and similar young clusters.
| SAO 23170, a New Beta Cep in the Stellar Cluster H VI 33
Not Available
| Absolute proper motions of open clusters. I. Observational data
Mean proper motions and parallaxes of 205 open clusters were determinedfrom their member stars found in the Hipparcos Catalogue. 360 clusterswere searched for possible members, excluding nearby clusters withdistances D < 200 pc. Members were selected using ground basedinformation (photometry, radial velocity, proper motion, distance fromthe cluster centre) and information provided by Hipparcos (propermotion, parallax). Altogether 630 certain and 100 possible members werefound. A comparison of the Hipparcos parallaxes with photometricdistances of open clusters shows good agreement. The Hipparcos dataconfirm or reject the membership of several Cepheids in the studiedclusters. Tables 1 and 2 are only available in electronic form at theCDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| Vitesses radiales. Catalogue WEB: Wilson Evans Batten. Subtittle: Radial velocities: The Wilson-Evans-Batten catalogue.
We give a common version of the two catalogues of Mean Radial Velocitiesby Wilson (1963) and Evans (1978) to which we have added the catalogueof spectroscopic binary systems (Batten et al. 1989). For each star,when possible, we give: 1) an acronym to enter SIMBAD (Set ofIdentifications Measurements and Bibliography for Astronomical Data) ofthe CDS (Centre de Donnees Astronomiques de Strasbourg). 2) the numberHIC of the HIPPARCOS catalogue (Turon 1992). 3) the CCDM number(Catalogue des Composantes des etoiles Doubles et Multiples) byDommanget & Nys (1994). For the cluster stars, a precise study hasbeen done, on the identificator numbers. Numerous remarks point out theproblems we have had to deal with.
| Catalogue of Hydrogen Line Spectral Profiles of 236 B-Stars A-Stars and F-Stars
Not Available
| 2000 A UV imaging of a 6 deg diameter field around the H and Chi Persei double cluster
A stellar field centered close to the h and Chi per double cluster hasbeen observed at 2000 A by the stratospheric balloon-born telescope ofthe SCAP-2000 program. It is shown that the prevailing extinction lawproduces greater extinction at 1965 A than is predicted by the meanextinction law. The results suggest the presence of an H2 cloud in frontof h and Chi Per in the second absorbing layer and in the local arm. Agroup of hot stars centered at the same distance as the molecular cloudmay form an association of OB stars in the local arm.
| The helium abundance in the atmospheres of the stars in the clusters NGC 869, 884 and 2264
The effective temperature, acceleration due to gravity, atmospherichelium abundance, and rotational velocity of 23 B-stars are determinedusing the model atmosphere method. Photographic spectra in the 3900-4900A range obtained on the main stellar spectrograph of the 6-m telescopewere used. It is concluded that significant differences in the meanhelium abundance do not exist from cluster to cluster.
| Catalog of Indidual Radial Velocities, 0h-12h, Measured by Astronomers of the Mount Wilson Observatory
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1970ApJS...19..387A&db_key=AST
| Vitesses radiales dans la region de h+chi Per.
Not Available
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Pozíciós és asztrometriai adatok
| Csillagkép: | Perszeusz |
| Rektaszcenzió: | 02h19m56.13s |
| Deklináció: | +57°19'05.1" |
| Vizuális fényesség: | 8.257 |
| Távolság: | 2941.176 parszek |
| RA sajátmozgás: | -1.3 |
| Dec sajátmozgás: | -3 |
| B-T magnitude: | 8.528 |
| V-T magnitude: | 8.28 |
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