2017MNRAS.468.3746C


C.D.S. - SIMBAD4 rel 1.7 - 2021.04.14CEST13:03:43

2017MNRAS.468.3746C - Mon. Not. R. Astron. Soc., 468, 3746-3756 (2017/July-1)

The first interferometric detections of fast radio bursts.

CALEB M., FLYNN C., BAILES M., BARR E.D., BATEMAN T., BHANDARI S., CAMPBELL-WILSON D., FARAH W., GREEN A.J., HUNSTEAD R.W., JAMESON A., JANKOWSKI F., KEANE E.F., PARTHASARATHY A., RAVI V., ROSADO P.A., VAN STRATEN W. and VENKATRAMAN KRISHNAN V.

Abstract (from CDS):

We present the first interferometric detections of fast radio bursts (FRBs), an enigmatic new class of astrophysical transient. In a 180-d survey of the Southern sky, we discovered three FRBs at 843 MHz with the UTMOST array, as a part of commissioning science during a major ongoing upgrade. The wide field of view of UTMOST (≃9 deg2) is well suited to FRB searches. The primary beam is covered by 352 partially overlapping fan-beams, each of which is searched for FRBs in real time with pulse widths in the range 0.655-42 ms, and dispersion measures <=2000 pc cm–3. Detections of FRBs with the UTMOST array place a lower limit on their distances of ≃104 km (limit of the telescope near-field) supporting the case for an astronomical origin. Repeating FRBs at UTMOST or an FRB detected simultaneously with the Parkes radio telescope and UTMOST would allow a few arcsec localization, thereby providing an excellent means of identifying FRB host galaxies, if present. Up to 100 h of followup for each FRB has been carried out with the UTMOST, with no repeating bursts seen. From the detected position, we present 3σ error ellipses of 15 arcsec x 8.4 on the sky for the point of origin for the FRBs. We estimate an all-sky FRB rate at 843 MHz above a fluence Flim of 11 Jy ms of ∼78 events sky–1 d–1 at the 95 per cent confidence level. The measured rate of FRBs at 843 MHz is two times higher than we had expected, scaling from the FRB rate at the Parkes radio telescope, assuming that FRBs have a flat spectral index and a uniform distribution in Euclidean space. We examine how this can be explained by FRBs having a steeper spectral index and/or a flatter logN-log F distribution than expected for a Euclidean Universe.

Abstract Copyright: © 2017 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society

Journal keyword(s): instrumentation: interferometers - methods: data analysis - surveys - intergalactic medium - radio continuum - radio continuum

Simbad objects: 15

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Number of rows : 15

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 FRB 010724 rB 01 18 06.0 -72 12 19           ~ 62 0
2 FRB 121102 rB 05 32 09.60 +33 05 13.4           ~ 418 0
3 V* CM Tau Psr 05 34 31.93830 +22 00 52.1758           ~ 4879 1
4 FRB 131104 rB 06 44 10.4 -51 16 40           ~ 70 0
5 FRB 150418 rB 07 16 30.9 -19 02 24           ~ 97 0
6 FRB 160608 rB 07 36 42.0 -40 47 52           ~ 14 0
7 PSR B0736-40 Psr 07 38 32.2620 -40 42 39.420           ~ 173 0
8 FRB 160317 rB 07 53 47.0 -29 36 31           ~ 19 0
9 NAME SGR 0755-2933 ev 07 55 32.0 -29 33 08           ~ 5 0
10 NAME Vela Pulsar Psr 08 35 20.65525 -45 10 35.1545     15.10     ~ 2105 1
11 PSR B0834+06 Psr 08 37 05.642 +06 10 14.56           ~ 400 0
12 FRB 160410 rB 08 41 25.0 +06 05 05           ~ 14 0
13 PSR B1641-45 Psr 16 44 49.2730 -45 59 09.710     12.60     ~ 181 0
14 FRB 110523 rB 21 45 31.0 -00 15 23           ~ 71 0
15 FRB 150807 rB 22 41 33.75 -53 05 39.9           ~ 50 0

    Equat.    Gal    SGal    Ecl

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2021.04.14-13:03:43

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