Characterizing the Fast Radio Burst Host Galaxy Population and its Connection to Transients in the Local and Extragalactic Universe

Creators: Bhandari, Shivani; Heintz, Kasper E.; Aggarwal, Kshitij; Marnoch, Lachlan; Day, Cherie K.; Sydnor, Jessica; Burke-Spolaor, Sarah; Law, Casey J.; Prochaska, J. Xavier; Tejos, Nicolas; Bannister, Keith W.; Butler, Bryan J.; Deller, Adam T.; Ekers, R. D.; Flynn, Chris; Fong, Wen-fai; James, Clancy W.; Lazio, T. Joseph W.; Luo, Rui; Mahony, Elizabeth K.; Ryder, Stuart D.; Sadler, Elaine M.; Shannon, Ryan M.; Han, JinLin; Lee, Kejia; Zhang, Bing

Abstract

We present the localization and host galaxies of one repeating and two apparently nonrepeating fast radio bursts (FRBs). FRB 20180301A was detected and localized with the Karl G. Jansky Very Large Array to a star-forming galaxy at z = 0.3304. FRB20191228A and FRB20200906A were detected and localized by the Australian Square Kilometre Array Pathfinder to host galaxies at z = 0.2430 and z = 0.3688, respectively. We combine these with 13 other well-localized FRBs in the literature, and analyze the host galaxy properties. We find no significant differences in the host properties of repeating and apparently nonrepeating FRBs. FRB hosts are moderately star forming, with masses slightly offset from the star-forming main sequence. Star formation and low-ionization nuclear emission-line region emission are major sources of ionization in FRB host galaxies, with the former dominant in repeating FRB hosts. FRB hosts do not track stellar mass and star formation as seen in field galaxies (more than 95% confidence). FRBs are rare in massive red galaxies, suggesting that progenitor formation channels are not solely dominated by delayed channels which lag star formation by gigayears. The global properties of FRB hosts are indistinguishable from core-collapse supernovae and short gamma-ray bursts hosts, and the spatial offset (from galaxy centers) of FRBs is mostly inconsistent with that of the Galactic neutron star population (95% confidence). The spatial offsets of FRBs (normalized to the galaxy effective radius) also differ from those of globular clusters in late- and early-type galaxies with 95% confidence.

Additional Information

© 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Received 2021 August 2; revised 2021 November 10; accepted 2021 November 16; published 2022 January 17. All of the data and the majority of the software used for the host analysis are available at https://github.com/FRBs/FRB. S.B. would like to thank Themiya Nanayakkara, Arash Bahramian, and Kristen Dage for useful discussions. R.M.S. acknowledges support from the Australian Research Council Future Fellowship FT190100155. K.E.H. acknowledges support by a Postdoctoral Fellowship Grant (217690–051) from The Icelandic Research Fund. K.A. acknowledges support from NSF grant No. AAG-1714897. L.M. acknowledges the receipt of an MQ-RES scholarship from Macquarie University. S.B.S acknowledges support from NSF grant No. AAG-1714897. She is a CIFAR Azrieli Global Scholar in the Gravity and the Extreme Universe program, which helped support J.S. for this project. A.T.D. is the recipient of an Australian Research Council Future Fellowship (FT150100415). W.F. acknowledges support by the National Science Foundation under grant Nos. AST-1814782, AST-1909358, and CAREER grant No. AST-2047919. C.J.L. acknowledges support from the National Science Foundation under grant No. 2022546. N.T. acknowledges support by FONDECYT grant No. 11191217. K.J.L. is supported by CAS XDB23010200, Max-Planck Partner Group, National SKA program of China grant No. 2020SKA0120100, NSFC grant No. 11690024, CAS Cultivation Project for FAST Scientific. The NANOGrav project receives support from the National Science Foundation (NSF) Physics Frontiers Center, award number 1430284. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Authors S.S., N.T., J.X.P., and K.G.L. as members of the Fast and Fortunate for FRB Follow-up team, acknowledge support from NSF grant Nos. AST-1911140 and AST-1910471. The Australian Square Kilometre Array Pathfinder and Australia Telescope Compact Array (ATCA) are part of the Australia Telescope National Facility, which is managed by CSIRO. Operation of ASKAP is funded by the Australian Government with support from the National Collaborative Research Infrastructure Strategy. ASKAP uses the resources of the Pawsey Supercomputing Centre. Establishment of ASKAP, the Murchison Radio-astronomy Observatory and the Pawsey Supercomputing Centre are initiatives of the Australian Government, with support from the Government of Western Australia and the Science and Industry Endowment Fund. We acknowledge the Wajarri Yamatji as the traditional owners of the Murchison Radio-astronomy Observatory site. We acknowledge the Gomeroi people as the traditional owners of the Paul Wild (ATCA) Observatory site. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Spectra were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among Caltech, the University of California, and the National Aeronautics and Space Administration (NASA). W. M. Keck Observatory and MMT Observatory access was in part supported by Northwestern University and the Centre for Interdisciplinary Exploration and Research in Astrophysics (CIERA). The Keck Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Observations reported here were obtained at the MMT Observatory, a joint facility of the University of Arizona and the Smithsonian Institution. Based on observations collected at the European Southern Observatory under ESO program 0105.A-0687(A). Based on observations obtained at the international Gemini Observatory, a program of NSF's NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation on behalf of the Gemini Observatory partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigación y Desarrollo (Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina), Ministério da Ciência, Tecnologia, Inovações e Comunicações (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). The Gemini data were obtained from program GS-2020B-Q-138, and were processed using the Data Reduction for Astronomy from Gemini Observatory North and South (DRAGONS) package. Software: PYSE (Spreeuw et al. 2018), ESOReflex (Freudling et al. 2013), Montage (Jacob et al. 2010), Source-Extractor (Bertin & Arnouts 1996), Astropy (Robitaille et al. 2013), Burstfit (Aggarwal et al. 2021a), Scipy (Jones et al. 2001), CASA (McMullin et al. 2007), CIGALE (Noll et al. 2009), pPXF (Cappellari 2017).

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