The Green Bank Northern Celestial Cap Pulsar Survey. II. the Discovery and Timing of 10 Pulsars

A. M. Kawash, M. A. McLaughlin, D. L. Kaplan, M. E. Decesar, L. Levin, D. R. Lorimer, R. S. Lynch, K. Stovall, J. K. Swiggum, E. Fonseca, A. M. Archibald, S. Banaszak, C. M. Biwer, J. Boyles, B. Cui, L. P. Dartez, D. Day, S. Ernst, A. J. Ford, J. FlaniganS. A. Heatherly, J. W.T. Hessels, J. Hinojosa, F. A. Jenet, C. Karako-Argaman, V. M. Kaspi, V. I. Kondratiev, S. Leake, G. Lunsford, J. G. Martinez, A. Mata, T. D. Matheny, A. E. McEwen, M. G. Mingyar, A. L. Orsini, S. M. Ransom, M. S.E. Roberts, M. D. Rohr, X. Siemens, R. Spiewak, I. H. Stairs, J. Van Leeuwen, A. N. Walker, B. L. Wells

Research output: Contribution to journalArticlepeer-review


We present timing solutions for 10 pulsars discovered in 350 MHz searches with the Green Bank Telescope. Nine of these were discovered in the Green Bank Northern Celestial Cap survey and one was discovered by students in the Pulsar Search Collaboratory program during an analysis of drift-scan data. Following the discovery and confirmation with the Green Bank Telescope, timing has yielded phase-connected solutions with high-precision measurements of rotational and astrometric parameters. Eight of the pulsars are slow and isolated, including PSR J0930-2301, a pulsar with a nulling fraction lower limit of ∼30% and a nulling timescale of seconds to minutes. This pulsar also shows evidence of mode changing. The remaining two pulsars have undergone recycling, accreting material from binary companions, resulting in higher spin frequencies. PSR J0557-2948 is an isolated, 44 ms pulsar that has been partially recycled and is likely a former member of a binary system that was disrupted by a second supernova. The paucity of such so-called "disrupted binary pulsars" (DRPs) compared to double neutron star (DNS) binaries can be used to test current evolutionary scenarios, especially the kicks imparted on the neutron stars in the second supernova. There is some evidence that DRPs have larger space velocities, which could explain their small numbers. PSR J1806+2819 is a 15 ms pulsar in a 44-day orbit with a low-mass white dwarf companion. We did not detect the companion in archival optical data, indicating that it must be older than 1200 Myr.

Original languageEnglish (US)
Article number131
JournalAstrophysical Journal
Issue number2
StatePublished - Apr 20 2018


  • pulsars: individual (PSR J05572948, PSR J09302301, PSR J1806+2819)

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science


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