{
  "id": "1607.03543",
  "version": "v1",
  "published": "2016-07-12T23:17:36.000Z",
  "updated": "2016-07-12T23:17:36.000Z",
  "title": "Anomalous Spectral Types and Intrinsic Colors of Young Stars",
  "authors": [
    "Mark J. Pecaut"
  ],
  "comment": "6 pages, 4 figures; Proceedings IAU Symposium No. 314, 2015, Young Stars & Planets Near the Sun",
  "journal": "IAUS, 314, 85-90 (2016)",
  "doi": "10.1017/S1743921315006079",
  "categories": [
    "astro-ph.SR"
  ],
  "abstract": "We highlight differences in spectral types and intrinsic colors observed in pre-main sequence (pre-MS) stars. Spectral types of pre-MS stars are wavelength-dependent, with near-infrared spectra being 3-5 spectral sub-classes later than the spectral types determined from optical spectra. In addition, the intrinsic colors of young stars differ from that of main-sequence stars at a given spectral type. We caution observers to adopt optical spectral types over near-infrared types, since Hertzsprung-Russell (H-R) diagram positions derived from optical spectral types provide consistency between dynamical masses and theoretical evolutionary tracks. We also urge observers to deredden pre-MS stars with tabulations of intrinsic colors specifically constructed for young stars, since their unreddened colors differ from that of main sequence dwarfs. Otherwise, V-band extinctions as much as ~0.6 mag erroneously higher than the true extinction may result, which would introduce systematic errors in the H-R diagram positions and thus bias the inferred ages.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2016-07-12T23:17:36.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "intrinsic colors",
      "anomalous spectral types",
      "young stars differ",
      "main sequence dwarfs",
      "adopt optical spectral types"
    ],
    "tags": [
      "journal article"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 6,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}