{
  "id": "1001.4958",
  "version": "v1",
  "published": "2010-01-27T14:33:21.000Z",
  "updated": "2010-01-27T14:33:21.000Z",
  "title": "Hard X-ray timing and spectral characteristics of the energetic pulsar PSR J0205+6449 in supernova remnant 3C58",
  "authors": [
    "L. Kuiper",
    "W. Hermsen",
    "J. O. Urama",
    "P. R. den Hartog",
    "A. G. Lyne",
    "B. W. Stappers"
  ],
  "comment": "10 pages; 7 figures (2 in color), resubmitted to A&A, including referee comments",
  "categories": [
    "astro-ph.HE"
  ],
  "abstract": "PSR J0205+6449 is a young rotation-powered pulsar in SNR 3C 58. It is one of only three young (<10,000 year old) pulsars which are so far detected in the radio and the classical X-ray bands, as well as at hard X-rays above 20 keV and at high-energy (>100 MeV) $\\gamma$-rays. The other two young pulsars are the Crab and PSR B1509-58. Our aim is to derive the timing and spectral characteristics of PSR J0205+6449 over the broad X-ray band from ~0.5 to ~270 keV. We used all publicly available RXTE observations of PSR J0205+6449 to first generate accurate ephemerides over the period September 30, 2000 - March 18, 2006. Next, phase-folding procedures yielded pulse profiles using data from RXTE PCA and HEXTE, and XMM-Newton EPIC PN. While our timing solutions are consistent with earlier results, our work shows sharper structures in the PCA X-ray profile. The X-ray pulse profile consists of two sharp pulses, separated in phase by 0.488(2), which can be described with 2 asymmetric Lorentzians, each with the rising wing steeper than the trailing wing, and full-width-half-maximum 1.41(5) ms and 2.35(22) ms, respectively. We find an indication for a flux increase by a factor ~2, about 3.5 sigma above the time-averaged value, for the second, weaker pulse during a two-week interval, while its pulse shape did not change. The spectrum of the pulsed X-ray emission is of non-thermal origin, exhibiting a power-law shape with photon index Gamma = 1.03(2) over the energy band ~0.5 to ~270 keV. In the energy band covered with the PCA (~3-30 keV) the spectra of the two pulses have the same photon index, namely, 1.04(3) and 1.10(8), respectively.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2010-01-27T14:33:21.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "energetic pulsar psr",
      "supernova remnant 3c58",
      "hard x-ray timing",
      "spectral characteristics",
      "procedures yielded pulse profiles"
    ],
    "tags": [
      "journal article"
    ],
    "publication": {
      "doi": "10.1051/0004-6361/200913851",
      "journal": "Astronomy and Astrophysics",
      "year": 2010,
      "month": "Jun",
      "volume": 515
    },
    "note": {
      "typesetting": "TeX",
      "pages": 10,
      "language": "en",
      "license": "arXiv",
      "status": "editable",
      "inspire": 844042,
      "adsabs": "2010A&A...515A..34K"
    }
  }
}