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Deep Synoptic Array science: a 50 Mpc fast radio burst constrains the mass of the Milky Way circumgalactic medium

Ravi, Vikram and Catha, Morgan and Chen, Ge and Connor, Liam and Cordes, James M. and Faber, Jakob T. and Lamb, James W. and Hallinan, Gregg and Harnach, Charlie and Hellbourg, Greg and Hobbs, Rick and Hodge, David and Hodges, Mark and Law, Casey and Rasmussen, Paul and Sharma, Kritti and Sherman, Myles B. and Shi, Jun and Simard, Dana and Somalwar, Jean J. and Squillace, Reynier and Weinreb, Sander and Woody, David P. and Yadlapalli, Nitika (2023) Deep Synoptic Array science: a 50 Mpc fast radio burst constrains the mass of the Milky Way circumgalactic medium. . (Unpublished)

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We present the Deep Synoptic Array (DSA-110) discovery and interferometric localization of the so far non-repeating FRB 20220319D. The FRB originates in a young, rapidly star-forming barred spiral galaxy, IRAS 02044+7048, at just 50 Mpc. Although the NE2001 and YMW16 models for the Galactic interstellar-medium (ISM) contribution to the DM of FRB 20220319D exceed its total observed DM, we show that uncertainties in these models accommodate an extragalactic origin for the burst. We derive a conservative upper limit on the DM contributed by the circumgalactic medium (CGM) of the Milky Way: the limit is either 28.7 pc cm⁻³ and 47.3 pc cm⁻³, depending on which of two pulsars nearby on the sky to FRB 20220319D is used to estimate the ISM DM. These limits both imply that the total Galactic CGM mass is <10¹¹ M_⊙, and that the baryonic mass of the Milky Way is ≲60% of the cosmological average given the total halo mass. More stringent albeit less conservative constraints are possible when the DMs of pulsars in the distant globular cluster M53 are additionally considered. Although our constraints are sensitive to possible anisotropy in the CGM and to the assumed form of the radial-density profile, they are not subject to uncertainties in the chemical and thermal properties of the CGM. Our results strongly support scenarios commonly predicted by galaxy-formation simulations wherein feedback processes expel baryonic matter from the halos of galaxies like the Milky Way.

Item Type:Report or Paper (Discussion Paper)
Related URLs:
URLURL TypeDescription Paper InCaltech News
Ravi, Vikram0000-0002-7252-5485
Chen, Ge0000-0003-2867-4544
Connor, Liam0000-0002-7587-6352
Cordes, James M.0000-0002-4049-1882
Faber, Jakob T.0000-0001-9855-5781
Lamb, James W.0000-0002-5959-1285
Hallinan, Gregg0000-0002-7083-4049
Hellbourg, Greg0000-0002-8191-3885
Law, Casey0000-0002-4119-9963
Sharma, Kritti0000-0002-4477-3625
Shi, Jun0000-0003-1647-7762
Simard, Dana0000-0002-8873-8784
Somalwar, Jean J.0000-0001-8426-5732
Weinreb, Sander0000-0002-9353-6204
Yadlapalli, Nitika0000-0003-3255-4617
Additional Information:The authors thank staff members of the Owens Valley Radio Observatory and the Caltech radio group, including Kristen Bernasconi, Stephanie Cha-Ramos, Sarah Harnach, Tom Klinefelter, Lori McGraw, Corey Posner, Andres Rizo, Michael Virgin, Scott White, and Thomas Zentmyer. Their tireless efforts were instrumental to the success of the DSA-110. The DSA-110 is supported by the National Science Foundation Mid-Scale Innovations Program in Astronomical Sciences (MSIP) under grant AST-1836018. We acknowledge use of the VLA calibrator manual and the radio fundamental catalog. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. Facility: Hale Software: astropy, CASA, heimdall, pypeit, Prospector, wsclean
Group:Astronomy Department, Owens Valley Radio Observatory (OVRO)
Funding AgencyGrant Number
W. M. Keck FoundationUNSPECIFIED
Record Number:CaltechAUTHORS:20230224-200149560
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:119502
Deposited By: George Porter
Deposited On:28 Feb 2023 02:59
Last Modified:02 Jun 2023 01:30

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