期刊
ASTROPHYSICAL JOURNAL
卷 850, 期 1, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.3847/1538-4357/aa9700
关键词
radio continuum: stars; stars: neutron; supernovae: general; techniques: interferometric
资金
- National Aeronautics and Space Administration
- University of California Office of the President [237863]
- NSF [1611606, 1458952]
- European Research Council under the European Union's Seventh Framework Programme/ERC [337062]
- NWO
- McGill Astrophysics Fellowship
- Oxford Centre for Astrophysical Surveys - Hintze Family Charitable Foundation
- European Research Council [ERC-2012-StG-307215 LODESTONE]
- UK Science and Technology Facilities Council (STFC)
- University of Cambridge
- National Science Foundation of the University Radio Observatory [1139974]
- NSERC
- CIFAR
- Canada Research Chair Program
- Lorne Trottier Chair in Astrophysics Cosmology
- [NSF/AST-1156780]
- Direct For Mathematical & Physical Scien [1611606] Funding Source: National Science Foundation
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [1139974] Funding Source: National Science Foundation
- Division Of Astronomical Sciences [1611606] Funding Source: National Science Foundation
- Office of Integrative Activities
- Office Of The Director [1458952] Funding Source: National Science Foundation
- STFC [ST/P000649/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/P000649/1] Funding Source: researchfish
We present results of the coordinated observing campaign that made the first subarcsecond localization of a fast radio burst, FRB 121102. During this campaign, we made the first simultaneous detection of an FRB burst using multiple telescopes: the VLA at 3 GHz and the Arecibo Observatory at 1.4 GHz. Of the nine bursts detected by the Very Large Array at 3 GHz, four had simultaneous observing coverage at other observatories at frequencies from 70. MHz to 15 GHz. The one multi-observatory detection and three non-detections of bursts seen at 3 GHz confirm earlier results showing that burst spectra are not well modeled by a power law. We find that burst spectra are characterized by a similar to 500. MHz envelope and apparent radio energy as high as 10(40). erg. We measure significant changes in the apparent dispersion between bursts that can be attributed to frequency-dependent profiles or some other intrinsic burst structure that adds a systematic error to the estimate of dispersion measure by up to 1%. We use FRB 121102 as a prototype of the FRB class to estimate a volumetric birth rate of FRB sources R-FRB approximate to 5 x 10(-5)/N-r Mpc(-3) yr(-1), where N-r is the number of bursts per source over its lifetime. This rate is broadly consistent with models of FRBs from young pulsars or magnetars born in superluminous supernovae or long gamma-ray bursts if the typical FRB repeats on the order of thousands of times during its lifetime.
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