Simultaneous X-Ray and Radio Observations of the Repeating Fast Radio Burst FRB similar to 180916.J0158+65
Artikel i vetenskaplig tidskrift, 2020

We report on simultaneous radio and X-ray observations of the repeating fast radio burst source FRB 180916.J0158+65 using the Canadian Hydrogen Intensity Mapping Experiment (CHIME), Effelsberg, and Deep Space Network (DSS-14 and DSS-63) radio telescopes and the Chandra X-ray Observatory. During 33 ks of Chandra observations, we detect no radio bursts in overlapping Effelsberg or Deep Space Network observations and a single burst during CHIME/FRB source transits. We detect no X-ray events in excess of the background during the Chandra observations. These non-detections imply a 5 sigma limit of <5 x 10(-10)erg cm(-2)for the 0.5-10 keV fluence of prompt emission at the time of the radio burst and 1.3 x 10(-9)erg cm(-2)at any time during the Chandra observations. Given the host-galaxy redshift of FRB 180916.J0158+65 (z similar to 0.034), these correspond to energy limits of <1.6 x 10(45)erg and <4 x 10(45)erg, respectively. We also place a 5 sigma limit of <8 x 10(-15)erg s(-1) cm(-2)on the 0.5-10 keV absorbed flux of a persistent source at the location of FRB 180916.J0158+65. This corresponds to a luminosity limit of <2 x 10(40)erg s(-1). Using an archival set of radio bursts from FRB 180916.J0158+65, we search for prompt gamma-ray emission in Fermi/GBM data but find no significant gamma-ray bursts, thereby placing a limit of 9 x 10(-9)erg cm(-2)on the 10-100 keV fluence. We also search Fermi/LAT data for periodic modulation of the gamma-ray brightness at the 16.35 days period of radio burst activity and detect no significant modulation. We compare these deep limits to the predictions of various fast radio burst models, but conclude that similar X-ray constraints on a closer fast radio burst source would be needed to strongly constrain theory.

X-ray bursts

Radio transient sources

High energy astrophysics

Neutron stars

Författare

P. Scholz

University of Toronto

A. Cook

University of Toronto

M. Cruces

Max-Planck-Gesellschaft

J. W. T. Hessels

Universiteit Van Amsterdam

Netherlands Institute for Radio Astronomy (ASTRON)

V. M. Kaspi

McGill University

W. A. Majid

California Institute of Technology (Caltech)

A. Naidu

McGill University

A. B. Pearlman

California Institute of Technology (Caltech)

L. G. Spitler

Max-Planck-Gesellschaft

K. M. Bandura

West Virginia University

M. Bhardwaj

McGill University

T. Cassanelli

University of Toronto

P. Chawla

McGill University

B. M. Gaensler

University of Toronto

D. C. Good

University of British Columbia (UBC)

A. Josephy

McGill University

R. Karuppusamy

Max-Planck-Gesellschaft

A. Keimpema

Joint Institute for VLBI in Europe (JIVE)

A. Yu Kirichenko

Russian Academy of Sciences

Universidad Nacional Autonoma de Mexico

Franz Kirsten

Chalmers, Rymd-, geo- och miljövetenskap, Astronomi och plasmafysik, Galaktisk astrofysik

J. Kocz

California Institute of Technology (Caltech)

C. Leung

Massachusetts Institute of Technology (MIT)

B. Marcote

Joint Institute for VLBI in Europe (JIVE)

K. Masui

Massachusetts Institute of Technology (MIT)

J. Mena-Parra

Massachusetts Institute of Technology (MIT)

M. Merryfield

McGill University

D. Michilli

McGill University

C. J. Naudet

California Institute of Technology (Caltech)

K. Nimmo

Universiteit Van Amsterdam

Netherlands Institute for Radio Astronomy (ASTRON)

Z. Pleunis

McGill University

T. A. Prince

California Institute of Technology (Caltech)

M. Rafiei-Ravandi

Perimeter Institute for Theoretical Physics

M. Rahman

University of Toronto

K. Shin

Massachusetts Institute of Technology (MIT)

K. M. Smith

Perimeter Institute for Theoretical Physics

I. H. Stairs

University of British Columbia (UBC)

S. P. Tendulkar

McGill University

K. Vanderlinde

University of Toronto

Astrophysical Journal

0004-637X (ISSN) 1538-4357 (eISSN)

Vol. 901 2 165

Ämneskategorier

Subatomär fysik

Astronomi, astrofysik och kosmologi

Annan fysik

DOI

10.3847/1538-4357/abb1a8

Mer information

Senast uppdaterat

2020-11-30