{
  "id": "1401.7424",
  "version": "v1",
  "published": "2014-01-29T07:49:38.000Z",
  "updated": "2014-01-29T07:49:38.000Z",
  "title": "Characterization of the Praesepe Star Cluster by Photometry and Proper Motions with 2MASS, PPMXL, and Pan-STARRS",
  "authors": [
    "P. F. Wang",
    "W. P. Chen",
    "C. C. Lin",
    "A. K. Pandey",
    "C. K. Huang",
    "N. Panwar",
    "C. H. Lee",
    "M. F. Tsai",
    "C. -H. Tang",
    "B. Goldman",
    "W. S. Burgett",
    "K. C. Chambers",
    "P. W. Draper",
    "H. Flewelling",
    "T. Grav",
    "J. N. Heasley",
    "K. W. Hodapp",
    "M. E. Huber",
    "R. Jedicke",
    "N. Kaiser",
    "R. -P. Kudritzki",
    "G. A. Luppino",
    "R. H. Lupton",
    "E. A. Magnier",
    "N. Metcalfe",
    "D. G. Monet",
    "J. S. Morgan",
    "P. M. Onaka",
    "P. A. Price",
    "C. W. Stubbs",
    "W. Sweeney",
    "J. L. Tonry",
    "R. J. Wainscoat",
    "C. Waters"
  ],
  "comment": "ApJ accepted",
  "categories": [
    "astro-ph.SR"
  ],
  "abstract": "Membership identification is the first step to determine 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 with stellar masses $\\sim$0.11--2.4 Msun of the intermediate-age Praesepe cluster (M44), by using Pan-STARRS and 2MASS photometry, and PPMXL proper motions. Within a sky area of 3 deg radius, 1040 candidates are identified, of which 96 are new inclusions. Using the same set of selection criteria on field stars led to an estimate of a false positive rate 16%, suggesting 872 of the candidates being true members. This most complete and reliable membership list allows us to favor the BT-Settl model in comparison with 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.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2014-01-29T07:49:38.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "praesepe star cluster",
      "photometry",
      "pan-starrs",
      "characterization",
      "intermediate-age praesepe cluster"
    ],
    "tags": [
      "journal article"
    ],
    "publication": {
      "doi": "10.1088/0004-637X/784/1/57",
      "journal": "The Astrophysical Journal",
      "year": 2014,
      "month": "Mar",
      "volume": 784,
      "number": 1,
      "pages": 57
    },
    "note": {
      "typesetting": "TeX",
      "pages": 0,
      "language": "en",
      "license": "arXiv",
      "status": "editable",
      "adsabs": "2014ApJ...784...57W"
    }
  }
}