{
  "id": "1105.2287",
  "version": "v1",
  "published": "2011-05-11T19:51:28.000Z",
  "updated": "2011-05-11T19:51:28.000Z",
  "title": "Detecting Planets around Very Cool Dwarfs at Near Infrared Wavelengths with the Radial Velocity Technique",
  "authors": [
    "Florian Rodler",
    "Carlos del Burgo",
    "Soeren Witte",
    "Christiane Helling",
    "Peter H. Hauschildt",
    "Eduardo L. Martin",
    "Carlos Alvarez"
  ],
  "comment": "8 pages; A&A, 2011",
  "categories": [
    "astro-ph.SR",
    "astro-ph.EP"
  ],
  "abstract": "Context. Radial velocity monitoring of very cool dwarfs such as late M- and hot L-dwarfs has become a promising tool to search for rocky planets as well as to follow-up planetary candidates around dwarfs found by transit surveys. These stars are faint at optical wavelengths, as their spectral flux distribution peaks at near-infrared (NIR) wavelengths. For this reason, it is desirable to measure the radial velocities in this wavelength regime. However, in the NIR there are only very few medium- and high-resolution spectrographs available which are mounted at large telescopes. In the near future, high-resolution spectrographs for the NIR will be built, which will allow us to search for rocky planets around cool M-dwarfs and L-dwarfs from radial velocities monitoring. Methods. Stellar atmosphere synthetic models for an M- and an L-dwarf with temperatures of 2200 K and 1800 K, respectively, and a theoretical spectrum of the Earth's transmission in the spectral range from 0.9 to 2.5 \\mum are used. We simulate a series of Doppler-shifted spectra observed with different resolving powers and signal-to-noise ratios, and for different rotational broadenings of the dwarf. For different combinations of the input parameters we recover the radial velocity by means of cross-correlation with a high signal-to-noise ratio template and determine the associate uncertainties. Results. The highest precision in radial velocity measurements for the cool M-dwarf is found in the Y band around 1.0 \\mum, while for the L-dwarf it is determined in the J band around 1.25 \\mum. We note that synthetic models may lack of some faint absorption features or underestimate their abundances. Conversely, some instrumental/calibration aspects that are not taken into account in our estimations would rise the uncertainties.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2011-05-11T19:51:28.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "radial velocity technique",
      "cool dwarfs",
      "detecting planets",
      "infrared wavelengths",
      "cool m-dwarf"
    ],
    "tags": [
      "journal article"
    ],
    "publication": {
      "doi": "10.1051/0004-6361/201015490",
      "journal": "Astronomy and Astrophysics",
      "year": 2011,
      "month": "Aug",
      "volume": 532
    },
    "note": {
      "typesetting": "TeX",
      "pages": 8,
      "language": "en",
      "license": "arXiv",
      "status": "editable",
      "inspire": 899222,
      "adsabs": "2011A&A...532A..31R"
    }
  }
}