[ Previous | Next | ADS ]

Real-time detection of a low-latitude Fast Radio Burst during observations of PSR J1545-4550

ATel #11046; Shannon R. M. (Swinburne University of Technology [SUT]) and Oslowski, S. (SUT); Zhang, S. (Purple Mountain Observatory); Bailes, M. (SUT); Bhat, N. D. R. (Curtin University of Technology); Coles, W. A.(University of California San Diego); Dai, S. (Commonwealth Scientific and Industrial Research Organisation [CSIRO]); Dempsey, J. (CSIRO); Hobbs, G. (CSIRO); Keith, M. J. (University of Manchester); Kerr, M. (Naval Research Laboratory); Jameson, A. (SUT); Manchester, R. N.(CSIRO); Lasky, P. D. (Monash University [Monash]); Levin, Y. (Flatiron Institute); Parthasarathy, A. (SUT); Ravi, V. (California Institute of Technology); Reardon, D. J. (Monash); Rosado, P. A. (SUT); Russell, C. J. (CSIRO); Sarkissian, J. M. (CSIRO); Spiewak, R. (SUT); van Straten, W. (Auckland University of Technology); Toomey, L. (CSIRO); Wang, J. B. (Xinjiang Astronomical Observatory); Wen, L. (University of Western Australia); You, X.-P. (SU); Zhang, L. (National Astronomical Observatory, CAS); Zhu, X.-J. (Monash)
on 10 Dec 2017; 08:00 UT
Distributed as an Instant Email Notice Transients
Credential Certification: Igor Andreoni (igor.andreoni@gmail.com)

Subjects: Radio, Fast Radio Burst

The Parkes Pulsar Timing Array (Manchester et al. 2013) project monitors pulse times of arrival for 24 millisecond pulsars in the Galaxy on a fortnightly cadence. Since 2017 June, we have been commensally searching for fast radio bursts (FRBs) when timing pulsars with the 13-beam 20-cm multibeam receiver. These data are recorded with standard instrumentation (Keith et al, MNRAS, 2010) and searched in real time for FRBs using the Heimdall algorithm (Barsdell et al. 2011)

On 2017-12-09 at 20:34:23.5 UTC (2017-12-09.8572164352), we detected a burst with a signal to noise ratio (S/N) of 40, at the dispersion measure (DM) of 1458 pc cm-3, in the field of the millisecond pulsar PSR J1545-4550 (DM = 68.39 pc cm-3). The burst was detected in beam 13 of the receiver, which at the time was pointed at a position of (RA, DEC = 15:50:25, -46:10:20). The burst width (full width at half maximum) was 2.5 ms and its measured fluence was 2.3 Jy ms. We note that the location of the burst within the telescope beam is highly uncertain (> 0.25 deg); consequently, the fluence measurement is biased low (Macquart & Ekers 2017)

This position is approximately 6 degrees off of the galactic plane. The galactic contribution is estimated to be 343 pc cm^-3 from the NE2001 model (Cordes & Lazio, 2001) and 235 from the YMW16 model (Yao et al. 2017). Assuming host contribution to the DM of 100 pc cm-3, we estimate the redshift to be around 0.87.

We encourage prompt follow-up with available facilities.

References:
Barsdell et al. 2012
Cordes & Lazio, 2001
Keith et al. 2010
Manchester et al. 2013
Macquart & Ekers 2017
Yao et al. 2017