Deep Synoptic Array Science: Polarimetry of 25 New Fast Radio Bursts Provides Insights into Their Origins

Myles B. Sherman; Liam Connor; Vikram Ravi; Casey Law; Ge Chen; Morgan Catha; Jakob T. Faber; Gregg Hallinan; Charlie Harnach; Greg Hellbourg; Rick Hobbs; David Hodge; Mark Hodges; James W. Lamb; Paul Rasmussen; Kritti Sharma; Jun Shi; Dana Simard; Jean Somalwar; Reynier Squillace; Sander Weinreb; David P. Woody; Nitika Yadlapalli; The Deep Synoptic Array team

doi:10.3847/1538-4357/ad275e

The Astrophysical Journal (Jan 2024)

Deep Synoptic Array Science: Polarimetry of 25 New Fast Radio Bursts Provides Insights into Their Origins

Myles B. Sherman,
Liam Connor,
Vikram Ravi,
Casey Law,
Ge Chen,
Morgan Catha,
Jakob T. Faber,
Gregg Hallinan,
Charlie Harnach,
Greg Hellbourg,
Rick Hobbs,
David Hodge,
Mark Hodges,
James W. Lamb,
Paul Rasmussen,
Kritti Sharma,
Jun Shi,
Dana Simard,
Jean Somalwar,
Reynier Squillace,
Sander Weinreb,
David P. Woody,
Nitika Yadlapalli,
The Deep Synoptic Array team

Affiliations

Myles B. Sherman: ORCiD; Cahill Center for Astronomy and Astrophysics, MC 249-17, California Institute of Technology , Pasadena, CA 91125, USA ; [email protected]
Liam Connor: ORCiD; Cahill Center for Astronomy and Astrophysics, MC 249-17, California Institute of Technology , Pasadena, CA 91125, USA ; [email protected]
Vikram Ravi: ORCiD; Cahill Center for Astronomy and Astrophysics, MC 249-17, California Institute of Technology , Pasadena, CA 91125, USA ; [email protected]; Owens Valley Radio Observatory, California Institute of Technology , Big Pine, CA 93513, USA
Casey Law: ORCiD; Cahill Center for Astronomy and Astrophysics, MC 249-17, California Institute of Technology , Pasadena, CA 91125, USA ; [email protected]; Owens Valley Radio Observatory, California Institute of Technology , Big Pine, CA 93513, USA
Ge Chen: ORCiD; Cahill Center for Astronomy and Astrophysics, MC 249-17, California Institute of Technology , Pasadena, CA 91125, USA ; [email protected]
Morgan Catha: Owens Valley Radio Observatory, California Institute of Technology , Big Pine, CA 93513, USA
Jakob T. Faber: ORCiD; Cahill Center for Astronomy and Astrophysics, MC 249-17, California Institute of Technology , Pasadena, CA 91125, USA ; [email protected]
Gregg Hallinan: ORCiD; Cahill Center for Astronomy and Astrophysics, MC 249-17, California Institute of Technology , Pasadena, CA 91125, USA ; [email protected]; Owens Valley Radio Observatory, California Institute of Technology , Big Pine, CA 93513, USA
Charlie Harnach: Owens Valley Radio Observatory, California Institute of Technology , Big Pine, CA 93513, USA
Greg Hellbourg: Cahill Center for Astronomy and Astrophysics, MC 249-17, California Institute of Technology , Pasadena, CA 91125, USA ; [email protected]; Owens Valley Radio Observatory, California Institute of Technology , Big Pine, CA 93513, USA
Rick Hobbs: Owens Valley Radio Observatory, California Institute of Technology , Big Pine, CA 93513, USA
David Hodge: Cahill Center for Astronomy and Astrophysics, MC 249-17, California Institute of Technology , Pasadena, CA 91125, USA ; [email protected]
Mark Hodges: Owens Valley Radio Observatory, California Institute of Technology , Big Pine, CA 93513, USA
James W. Lamb: ORCiD; Owens Valley Radio Observatory, California Institute of Technology , Big Pine, CA 93513, USA
Paul Rasmussen: Owens Valley Radio Observatory, California Institute of Technology , Big Pine, CA 93513, USA
Kritti Sharma: ORCiD; Cahill Center for Astronomy and Astrophysics, MC 249-17, California Institute of Technology , Pasadena, CA 91125, USA ; [email protected]
Jun Shi: Cahill Center for Astronomy and Astrophysics, MC 249-17, California Institute of Technology , Pasadena, CA 91125, USA ; [email protected]
Dana Simard: Cahill Center for Astronomy and Astrophysics, MC 249-17, California Institute of Technology , Pasadena, CA 91125, USA ; [email protected]
Jean Somalwar: ORCiD; Cahill Center for Astronomy and Astrophysics, MC 249-17, California Institute of Technology , Pasadena, CA 91125, USA ; [email protected]
Reynier Squillace: ORCiD; Department of Astronomy, University of Virginia , 530 McCormick Road, Charlottesville, VA 22904, USA
Sander Weinreb: Cahill Center for Astronomy and Astrophysics, MC 249-17, California Institute of Technology , Pasadena, CA 91125, USA ; [email protected]
David P. Woody: Owens Valley Radio Observatory, California Institute of Technology , Big Pine, CA 93513, USA
Nitika Yadlapalli: ORCiD; Cahill Center for Astronomy and Astrophysics, MC 249-17, California Institute of Technology , Pasadena, CA 91125, USA ; [email protected]
The Deep Synoptic Array team

DOI: https://doi.org/10.3847/1538-4357/ad275e
Journal volume & issue: Vol. 964, no. 2
p. 131

Abstract

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We report on a full-polarization analysis of the first 25 as yet nonrepeating fast radio bursts (FRBs) detected at 1.4 GHz by the 110-antenna Deep Synoptic Array (DSA-110) during commissioning observations. We present details of the data-reduction, calibration, and analysis procedures developed for this novel instrument. Faraday rotation measures (RMs) are searched between ±10 ^6 rad m ^−2 and detected for 20 FRBs, with magnitudes ranging from 4 to 4670 rad m ^−2 . Fifteen out of 25 FRBs are consistent with 100% polarization, 10 of which have high (≥70%) linear-polarization fractions and two of which have high (≥30%) circular-polarization fractions. Our results disfavor multipath RM scattering as a dominant depolarization mechanism. Polarization-state and possible RM variations are observed in the four FRBs with multiple subcomponents. We combine the DSA-110 sample with polarimetry of previously published FRBs, and compare the polarization properties of FRB subpopulations and FRBs with Galactic pulsars. Although FRB polarization fractions are typically higher than those of Galactic pulsars, and cover a wider range than those of pulsar single pulses, they resemble those of the youngest (characteristic ages <10 ^5 yr) pulsars. Our results support a scenario wherein FRB emission is intrinsically highly linearly polarized, and propagation effects can result in conversion to circular polarization and depolarization. Young pulsar emission and magnetospheric propagation geometries may form a useful analogy for the origin of FRB polarization.

Published in The Astrophysical Journal

ISSN: 1538-4357 (Online)
Publisher: IOP Publishing
Country of publisher: United Kingdom
LCC subjects: Science: Astronomy: Astrophysics
Website: https://iopscience.iop.org/journal/0004-637X

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