Characterization of the Praesepe Star Cluster by Photometry and Proper Motions With 2MASS, PPMXL, and Pan-STARRS
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Lin, C. C.
Pandey, A. K.
Huang, C. K.
Panwar, N.
Lee, C. H.
Tsai, M. F.
Tang, C.-H.
Goldman, B.
Burgett, W. S.
Chambers, K. C.
Draper, P. W.
Flewelling, H.
Grav, T.
Heasley, J. N.
Hodapp, K. W.
Huber, M. E.
Jedicke, R.
Kaiser, N.
Kudritzki, R.-P.
Luppino, G. A.
Lupton, R. H.
Magnier, E. A.
Metcalfe, N.
Monet, D. G.
Morgan, J. S.
Onaka, P. M.
Price, P. A.
Sweeney, W.
Tonry, J. L.
Wainscoat, R. J.
Waters, C.
Note: Order does not necessarily reflect citation order of authors.
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https://doi.org/10.1088/0004-637x/784/1/57Metadata
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Wang, P. F., W. P. Chen, C. C. Lin, A. K. Pandey, C. K. Huang, N. Panwar, C. H. Lee, et al. 2014. “Characterization of the Praesepe Star Cluster by Photometry and Proper Motions with 2MASS, PPMXL, and Pan-STARRS.” The Astrophysical Journal 784 (1) (March 4): 57. doi:10.1088/0004-637x/784/1/57.Abstract
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 ☉, 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.Terms of Use
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