PALFA Single-pulse Pipeline:New Pulsars, Rotating Radio Transients, and a Candidate Fast Radio Burst

Patel, C., Agarwal, D., Bhardwaj, M., Boyce, M. M., Brazier, A., Chatterjee, S., Chawla, P., Kaspi, V. M., Lorimer, D. R., McLaughlin, M. A., Parent, E., Pleunis, Z., Ransom, S. M., Scholz, P., Wharton, R. S., Zhu, W. W., Alam, M., Valdez, K. Caballero, Camilo, F., Cordes, J. M., Crawford, F., Deneva, J. S., Ferdman, R. D., Freire, P. C.C., Hessels, J. W.T., Nguyen, B., Stairs, I., Stovall, K. and Leeuwen, J. Van (2018) PALFA Single-pulse Pipeline:New Pulsars, Rotating Radio Transients, and a Candidate Fast Radio Burst. Astrophysical Journal, 869 (2). ISSN 0004-637X

Full text not available from this repository. (Request a copy)

Abstract

We present a new single-pulse pipeline for the PALFA survey to efficiently identify single radio pulses from pulsars, rotating radio transients (RRATs), and fast radio bursts (FRBs). We conducted a sensitivity analysis of this new pipeline in which many single pulses were injected into PALFA data and run through the pipeline. We find that for single pulse widths <5 ms, the sensitivity of our new pipeline is at most a factor of ∼2 less sensitive than theoretically predicted. For pulse widths >10 ms, as the DM decreases, the degradation in sensitivity gets worse and can increase up to a factor of ∼4.5. Using this pipeline, we have discovered seven pulsars and two RRATs, and identified three candidate RRATs and one candidate FRB. The confirmed pulsars and RRATs have DMs ranging from 133 to 386 pc cm -3 and flux densities ranging from 20 to 160 mJy. The pulsar periods range from 0.4 to 2.1 s. We report on candidate FRB 141113, which is likely astrophysical and extragalactic, having DM ≃ 400 pc cm -3 , which is over the Galactic maximum along this line of sight by ∼100-200 pc cm -3 . We consider implications for the FRB population and show via simulations that if FRB 141113 is real and extragalactic, the slope α of the distribution of integral source counts as a function of flux density (N(>S) ∝ S -α ) is 1.4 ±0.5 (95% confidence range). However, this conclusion is dependent on assumptions that require verification.

Item Type: Article
Uncontrolled Keywords: methods: data analysis,pulsars: general,astronomy and astrophysics,space and planetary science ,/dk/atira/pure/subjectarea/asjc/3100/3103
Faculty \ School:
Related URLs:
Depositing User: LivePure Connector
Date Deposited: 13 Jun 2019 13:30
Last Modified: 22 Apr 2020 07:41
URI: https://ueaeprints.uea.ac.uk/id/eprint/71389
DOI: 10.3847/1538-4357/aaee65

Actions (login required)

View Item View Item