Details

Autor(en) / Beteiligte

• Andersen, B. C.
• Bandura, K.
• Bhardwaj, M.
• Boubel, P.
• Boyce, M. M.
• Boyle, P. J.
• Brar, C.
• Cassanelli, T.
• Chawla, P.
• Cubranic, D.
• Deng, M.
• Dobbs, M.
• Fandino, M.
• Fonseca, E.
• Gaensler, B. M.
• Gilbert, A. J.
• Giri, U.
• Good, D. C.
• Halpern, M.
• Hill, A. S.
• Hinshaw, G.
• Höfer, C.
• Josephy, A.
• Kaspi, V. M.
• Kothes, R.
• Landecker, T. L.
• Lang, D. A.
• Li, D. Z.
• Lin, H.-H.
• Masui, K. W.
• Mena-Parra, J.
• Merryfield, M.
• Mckinven, R.
• Michilli, D.
• Milutinovic, N.
• Naidu, A.
• Newburgh, L. B.
• Ng, C.
• Patel, C.
• Pen, U.
• Pinsonneault-Marotte, T.
• Pleunis, Z.
• Rafiei-Ravandi, M.
• Rahman, M.
• Ransom, S. M.
• Renard, A.
• Scholz, P.
• Siegel, S. R.
• Singh, S.
• Smith, K. M.
• Stairs, I. H.
• Tendulkar, S. P.
• Tretyakov, I.
• Vanderlinde, K.
• Yadav, P.
• Zwaniga, A. V.

Titel

CHIME/FRB Discovery of Eight New Repeating Fast Radio Burst Sources

Ist Teil von

• Astrophysical journal. Letters, 2019-11, Vol.885 (1), p.L24

Ort / Verlag

Austin: The American Astronomical Society

Erscheinungsjahr

2019

Quelle

EZB Electronic Journals Library

Beschreibungen/Notizen

• We report on the discovery of eight repeating fast radio burst (FRB) sources found using the Canadian Hydrogen Intensity Mapping Experiment (CHIME) telescope. These sources span a dispersion measure (DM) range of 103.5-1281 pc cm−3. They display varying degrees of activity: six sources were detected twice, another three times, and one 10 times. These eight repeating FRBs likely represent the bright and/or high-rate end of a distribution of infrequently repeating sources. For all sources, we determine sky coordinates with uncertainties of ∼10′. FRB 180916.J0158+65 has a burst-averaged DM = 349.2 0.3 pc cm−3 and a low DM excess over the modeled Galactic maximum (as low as ∼20 pc cm−3); this source also has a Faraday rotation measure (RM) of −114.6 0.6 rad m−2, which is much lower than the RM measured for FRB 121102. FRB 181030.J1054+73 has the lowest DM for a repeater, 103.5 0.3 pc cm−3, with a DM excess of ∼70 pc cm−3. Both sources are interesting targets for multi-wavelength follow-up due to their apparent proximity. The DM distribution of our repeater sample is statistically indistinguishable from that of the first 12 CHIME/FRB sources that have not yet repeated. We find, with 4 significance, that repeater bursts are generally wider than those of CHIME/FRB bursts that have not repeated, suggesting different emission mechanisms. Many of our repeater events show complex morphologies that are reminiscent of the first two discovered repeating FRBs. The repetitive behavior of these sources will enable interferometric localizations and subsequent host galaxy identifications.