{
  "id": "1602.08511",
  "version": "v1",
  "published": "2016-02-26T21:37:29.000Z",
  "updated": "2016-02-26T21:37:29.000Z",
  "title": "High-precision timing of 42 millisecond pulsars with the European Pulsar Timing Array",
  "authors": [
    "G. Desvignes",
    "R. N. Caballero",
    "L. Lentati",
    "J. P. W. Verbiest",
    "D. J. Champion",
    "B. W. Stappers",
    "G. H. Janssen",
    "P. Lazarus",
    "S. Osłowski",
    "S. Babak",
    "C. G. Bassa",
    "P. Brem",
    "M. Burgay",
    "I. Cognard",
    "J. R. Gair",
    "E. Graikou",
    "L. Guillemot",
    "J. W. T. Hessels",
    "A. Jessner",
    "C. Jordan",
    "R. Karuppusamy",
    "M. Kramer",
    "A. Lassus",
    "K. Lazaridis",
    "K. J. Lee",
    "K. Liu",
    "A. G. Lyne",
    "J. McKee",
    "C. M. F. Mingarelli",
    "D. Perrodin",
    "A. Petiteau",
    "A. Possenti",
    "M. B. Purver",
    "P. A. Rosado",
    "S. Sanidas",
    "A. Sesana",
    "G. Shaifullah",
    "R. Smits",
    "S. R. Taylor",
    "G. Theureau",
    "C. Tiburzi",
    "R. van Haasteren",
    "A . Vecchio"
  ],
  "comment": "42 pages, 11 figures. Accepted for publication in MNRAS",
  "categories": [
    "astro-ph.HE",
    "astro-ph.IM",
    "astro-ph.SR"
  ],
  "abstract": "We report on the high-precision timing of 42 radio millisecond pulsars (MSPs) observed by the European Pulsar Timing Array (EPTA). This EPTA Data Release 1.0 extends up to mid-2014 and baselines range from 7-18 years. It forms the basis for the stochastic gravitational-wave background, anisotropic background, and continuous-wave limits recently presented by the EPTA elsewhere. The Bayesian timing analysis performed with TempoNest yields the detection of several new parameters: seven parallaxes, nine proper motions and, in the case of six binary pulsars, an apparent change of the semi-major axis. We find the NE2001 Galactic electron density model to be a better match to our parallax distances (after correction from the Lutz-Kelker bias) than the M2 and M3 models by Schnitzeler (2012). However, we measure an average uncertainty of 80\\% (fractional) for NE2001, three times larger than what is typically assumed in the literature. We revisit the transverse velocity distribution for a set of 19 isolated and 57 binary MSPs and find no statistical difference between these two populations. We detect Shapiro delay in the timing residuals of PSRs J1600$-$3053 and J1918$-$0642, implying pulsar and companion masses $m_p=1.22_{-0.35}^{+0.5} \\text{M}_{\\odot}$, $m_c = 0.21_{-0.04}^{+0.06} \\text{M}_{\\odot }$ and $m_p=1.25_{-0.4}^{+0.6} \\text{M}_{\\odot}$, $m_c = 0.23_{-0.05}^{+0.07} \\text{M}_{\\odot }$, respectively. Finally, we use the measurement of the orbital period derivative to set a stringent constraint on the distance to PSRs J1012$+$5307 and J1909$-$3744, and set limits on the longitude of ascending node through the search of the annual-orbital parallax for PSRs J1600$-$3053 and J1909$-$3744.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2016-02-26T21:37:29.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "european pulsar timing array",
      "millisecond pulsars",
      "high-precision timing",
      "ne2001 galactic electron density model",
      "psrs j1600"
    ],
    "publication": {
      "doi": "10.1093/mnras/stw483"
    },
    "note": {
      "typesetting": "TeX",
      "pages": 42,
      "language": "en",
      "license": "arXiv",
      "status": "editable",
      "inspire": 1424775
    }
  }
}