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uvby Hβ CCD photometry and membership segregation of the open cluster NGC 2548; gaps in the Main Sequence of open clusters
Deep CCD photometry in the uvby-Hβ intermediate-bandsystem is presented for the cluster NGC 2548 (M 48). A completemembership analysis based on astrometric and photometric criteria isapplied. The photometric analysis of a selected sample of stars yields areddening value of E(b-y)= 0.06±0.03, a distance modulus ofV_0-M_V= 9.3±0.5 (725 pc) and a metallicity of [ Fe/H] = - 0.24±0.27. Through isochrone fitting we find an age of log t = 8.6±0.1 (400 Myr). Our optical photometry and JHK from 2MASS arecombined to derive effective temperatures of cluster member stars. Theeffective temperature distribution along the main sequence of thecluster shows several gaps. A test to study the significance of thesegaps in the main sequence of the HR diagram has been applied. The methodis also applied to several other open clusters (Pleiades, Hyades, NGC1817 and M 67) to construct a sequence of metallicities and ages. Thecomparison of the results of each cluster gives four gaps with highsignificance (one of them, centred at 4900 K, has not been previouslyreported).
| Improved Astrometry and Photometry for the Luyten Catalog. II. Faint Stars and the Revised Catalog
We complete construction of a catalog containing improved astrometry andnew optical/infrared photometry for the vast majority of NLTT starslying in the overlap of regions covered by POSS I and by the secondincremental Two Micron All Sky Survey (2MASS) release, approximately 44%of the sky. The epoch 2000 positions are typically accurate to 130 mas,the proper motions to 5.5 mas yr-1, and the V-J colors to0.25 mag. Relative proper motions of binary components are measured to 3mas yr-1. The false-identification rate is ~1% for11<~V<~18 and substantially less at brighter magnitudes. Theseimprovements permit the construction of a reduced proper-motion diagramthat, for the first time, allows one to classify NLTT stars intomain-sequence (MS) stars, subdwarfs (SDs), and white dwarfs (WDs). We inturn use this diagram to analyze the properties of both our catalog andthe NLTT catalog on which it is based. In sharp contrast to popularbelief, we find that NLTT incompleteness in the plane is almostcompletely concentrated in MS stars, and that SDs and WDs are detectedalmost uniformly over the sky δ>-33deg. Our catalogwill therefore provide a powerful tool to probe these populationsstatistically, as well as to reliably identify individual SDs and WDs.
| Determination of proper motions and membership of the open star cluster NGC 2548
Absolute proper motions, their corresponding errors and membershipprobabilities of 501 stars in the intermediate-age open cluster NGC 2548region are determined from MAMA measurements of 10 photographic plates.The plates have the maximum epoch difference of 82 years and they weretaken with the double astrograph at Zô-Sèstation ofShanghai Observatory, which has an aperture of 40 cm and a plate scaleof 30 arcsec mm-1. The average proper motion precision is1.18 mas yr-1. These proper motions are used to determine themembership probabilities of stars in the region. The number of starswith membership probabilities higher than 0.7 is 165. Table 5 is onlyavailable in electronic form at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/ A+A/381/464, and by e-mail requestto Lola.Balaguer@am.ub.es MAMA (Machine Automatique àMesurer pourl'Astronomie, http://dsmama.obspm.fr) is developed and operated byINSU/CNRS and Observatoire de Paris.
| 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
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