期刊
ASTRONOMISCHE NACHRICHTEN
卷 333, 期 2, 页码 174-181出版社
WILEY-V C H VERLAG GMBH
DOI: 10.1002/asna.201111643
关键词
color-magnitude diagrams, HRD; methods: data analysis; open clusters: individual (NGC 2264)
Existing photometry for NGC 2264 tied to the Johnson & Morgan (1953) UBV system is reexamined and, in the case of the original observations by Walker (1956), reanalyzed in order to generate a homogeneous data set for cluster stars. Color terms and a Balmer discontinuity effect in Walker's observations were detected and corrected, and the homogenized data were used in a new assessment of the cluster reddening, distance, and age. Average values of E-B (-) (V) = 0.075 +/- 0.003 s.e. and V-0 - M-V = 9.45 +/- 0.03 s.e. (d = 777 +/- 12 pc) are obtained, in conjunction with an inferred cluster age of similar to 5.5x10(6) yr from pre-main-sequence members and the location of the evolved, luminous, O7 V((f)) dwarf S Mon relative to the ZAMS. The cluster main sequence also contains gaps that may have a dynamical origin. The dust responsible for the initial reddening towards NGC 2264 is no more than 465 pc distant, and there are numerous, reddened and unreddened, late-type stars along the line of sight that are difficult to separate from cluster members by standard techniques, except for a small subset of stars on the far side of the cluster embedded in its gas and dust and background B-type ZAMS members of Mon OB2. A compilation of likely NGC 2264 members is presented. Only 3 of the 4 stars recently examined by asteroseismology appear to be likely cluster members. NGC 2264 is also noted to be a double cluster, which has not been mentioned previously in the literature. (C) 2012 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim
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