Wang, PingChen, WeiLin, 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.Stubbs, ChristopherSweeney, W.Tonry, J. L.Wainscoat, R. J.Waters, C.2017-11-282014Wang, 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/784/1/57.0004-637Xhttp://nrs.harvard.edu/urn-3:HUL.InstRepos:34388862Membership 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.en-USJournal Article2017-11-2810.1088/0004-637x/784/1/57