Статья

CHARACTERIZATION OF THE PRAESEPE STAR CLUSTER BY PHOTOMETRY AND PROPER MOTIONS WITH 2MASS, PPMXL, AND Pan-STARRS

P. F. WangDepartment of Physics, National Central University, 300 Jhongda Road, Jhongli 32001, TaiwanW. P. ChenGraduate Institute of Astronomy, National Central University, 300 Jhongda Road, Jhongli 32001, TaiwanC. C. LinGraduate Institute of Astronomy, National Central University, 300 Jhongda Road, Jhongli 32001, TaiwanA. K. PandeyAryabhatta Research Institute of Observational Sciences, Manora peak, Nainital 263129, IndiaChung-Kai HuangGraduate Institute of Astronomy, National Central University, 300 Jhongda Road, Jhongli 32001, TaiwanNeelam PanwarGraduate Institute of Astronomy, National Central University, 300 Jhongda Road, Jhongli 32001, TaiwanChien‐Hsiu LeeGraduate Institute of Astronomy, National Central University, 300 Jhongda Road, Jhongli 32001, TaiwanM. F. TsaiDepartment of Computer Science and Information Engineering, National Central University, 300 Jhongda Road, Jhongli 32001, TaiwanChing-Yen TangDepartment of Computer Science and Information Engineering, National Central University, 300 Jhongda Road, Jhongli 32001, TaiwanB. GoldmanMax-Planck-Institut für Astronomie Königstuhl, 17 D-69117 Heidelberg, GermanyW. S. BurgettInstitute for Astronomy, University of Hawai'i, 2680 Woodlawn Drive, Honolulu, HI 96822, USAK. C. ChambersInstitute for Astronomy, University of Hawai'i, 2680 Woodlawn Drive, Honolulu, HI 96822, USAP. W. DraperDepartment of Physics, Durham University, South Road, Durham DH1 3LE, UK,H. FlewellingInstitute for Astronomy, University of Hawai'i, 2680 Woodlawn Drive, Honolulu, HI 96822, USAT. GravDepartment of Physics and Astronomy Johns Hopkins University 3400 North Charles Street Baltimore MD 21218 USAJ. N. HeasleyInstitute for Astronomy, University of Hawai'i, 2680 Woodlawn Drive, Honolulu, HI 96822, USAK. W. HodappInstitute for Astronomy, University of Hawai'i, 2680 Woodlawn Drive, Honolulu, HI 96822, USAM. E. HuberInstitute for Astronomy, University of Hawai'i, 2680 Woodlawn Drive, Honolulu, HI 96822, USARobert JedickeInstitute for Astronomy, University of Hawai'i, 2680 Woodlawn Drive, Honolulu, HI 96822, USAN. KaiserInstitute for Astronomy, University of Hawai'i, 2680 Woodlawn Drive, Honolulu, HI 96822, USARolf‐Peter KudritzkiInstitute for Astronomy, University of Hawai'i, 2680 Woodlawn Drive, Honolulu, HI 96822, USAG. A. LuppinoInstitute for Astronomy, University of Hawai'i, 2680 Woodlawn Drive, Honolulu, HI 96822, USARobert H. LuptonDept. of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USAE. A. MagnierInstitute for Astronomy, University of Hawai'i, 2680 Woodlawn Drive, Honolulu, HI 96822, USAN. MetcalfeDepartment of Physics, Durham University, South Road, Durham DH1 3LE, UK,D. G. MonetUS Naval Observatory, Flagstaff Station, Flagstaff, AZ 86001, USAJames P. MorganInstitute for Astronomy, University of Hawai'i, 2680 Woodlawn Drive, Honolulu, HI 96822, USAPeter M. OnakaInstitute for Astronomy, University of Hawai'i, 2680 Woodlawn Drive, Honolulu, HI 96822, USAP. A. PriceInstitute for Astronomy, University of Hawai'i, 2680 Woodlawn Drive, Honolulu, HI 96822, USAC. W. StubbsDepartment of Physics , Harvard University , Cambridge, MA, 02138, USAWilliam E. SweeneyInstitute for Astronomy, University of Hawai'i, 2680 Woodlawn Drive, Honolulu, HI 96822, USAJ. TonryInstitute for Astronomy, University of Hawai'i, 2680 Woodlawn Drive, Honolulu, HI 96822, USAR. J. WainscoatInstitute for Astronomy, University of Hawai'i, 2680 Woodlawn Drive, Honolulu, HI 96822, USAC. WatersInstitute for Astronomy, University of Hawai'i, 2680 Woodlawn Drive, Honolulu, HI 96822, USA

2014en

ABI

Аннотация

Membership identification is the first step in determining the properties of a star cluster. Low-mass members in particular could be used to trace the dynamical history, such as mass segregation, stellar evaporation, or tidal stripping, of a star cluster in its Galactic environment. We identified member candidates of the intermediate-age Praesepe cluster (M44) with stellar masses ~0.11-2.4 M &sun;, using Panoramic Survey Telescope And Rapid Response System and Two Micron All Sky Survey photometry, and PPMXL proper motions. Within a sky area of 3° radius, 1040 candidates are identified, of which 96 are new inclusions. Using the same set of selection criteria on field stars, an estimated false positive rate of 16% was determined, suggesting that 872 of the candidates are true members. This most complete and reliable membership list allows us to favor the BT-Settl model over other stellar models. The cluster shows a distinct binary track above the main sequence, with a binary frequency of 20%-40%, and a high occurrence rate of similar mass pairs. The mass function is consistent with that of the disk population but shows a deficit of members below 0.3 solar masses. A clear mass segregation is evidenced, with the lowest-mass members in our sample being evaporated from this disintegrating cluster.

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Идентификаторы

DOI: 10.1088/0004-637x/784/1/57

Цитирования и источники

Цитирований: 2Использованных источников: 0

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