Document Type
Article
Publication Date
4-10-2016
Abstract
We present Clusterrank, a new algorithm for identifying dispersed astrophysical pulses. Such pulses are commonly detected from Galactic pulsars and rotating radio transients (RRATs), which are neutron stars with sporadic radio emission. More recently, isolated, highly dispersed pulses dubbed fast radio bursts (FRBs) have been identified as the potential signature of an extragalactic cataclysmic radio source distinct from pulsars and RRATs. Clusterrank helped us discover 14 pulsars and 8 RRATs in data from the Arecibo 327 MHz Drift Pulsar Survey (AO327). The new RRATs have DMs in the range 23.5-86.6 pc cm-3 and periods in the range 0.172-3.901 s. The new pulsars have DMs in the range 23.6-133.3 pc cm-3 and periods in the range 1.249-5.012 s, and include two nullers and a mode-switching object. We estimate an upper limit on the all-sky FRB rate of 105 day-1 for bursts with a width of 10 ms and flux density ≳83 mJy. The DMs of all new discoveries are consistent with a Galactic origin. In comparing statistics of the new RRATs with sources from the RRATalog, we find that both sets are drawn from the same period distribution. In contrast, we find that the period distribution of the new pulsars is different from the period distributions of canonical pulsars in the ATNF catalog or pulsars found in AO327 data by a periodicity search. This indicates that Clusterrank is a powerful complement to periodicity searches and uncovers a subset of the pulsar population that has so far been underrepresented in survey results and therefore in Galactic pulsar population models.
Recommended Citation
Deneva, J. S., K. Stovall, M. A. McLaughlin, M. Bagchi, S. D. Bates, P. C. C. Freire, J. G. Martinez, F. Jenet, and N. Garver-Daniels. "New discoveries from the Arecibo 327 MHz drift pulsar survey radio transient search." The Astrophysical Journal 821, no. 1 (2016): 10. http://doi.org/10.3847/0004-637X/821/1/10
Publication Title
Astrophysical Journal
DOI
10.3847/0004-637X/821/1/10
Comments
© Astrophysical Journal. Original version available at: http://doi.org/10.3847/0004-637X/821/1/10