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

• Published in: The Astrophysical journal 2018-12, Vol.869 (2), p.181
• Main Authors: 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., Leeuwen, J. van
• Format: Article
• Language: English
• Subjects: Astrophysics; Flux density; methods: data analysis; Pipelines; Pulsars; pulsars: general; Radio bursts; Rotation; Sensitivity analysis
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/aaee65

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 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 of the distribution of integral source counts as a function of flux density (N(>S) ∝ S− ) is 1.4 0.5 (95% confidence range). However, this conclusion is dependent on assumptions that require verification.