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The 60 pc environment of FRB 20180916B

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Tendulkar, Shriharsh P. and Gil de Paz, Armando and Kirichenko, Aida Yu and Hessels, Jason W. T. and Bhardwaj, Mohit and Ávila, Fernando and Bassa, Cees and Chawla, Pragya and Fonseca, Emmanuel and Kaspi, Victoria M. and Keimpema, Aard and Kirsten, Franz and Lazio, T. Joseph W. and Marcote, Benito and Masui, Kiyoshi and Nimmo, Kenzie and Paragi, Zsolt and Rahman, Mubdi and Reverte Payá, Daniel and Scholz, Paul and Stair, Ingrid (2021) The 60 pc environment of FRB 20180916B. Astrophysical journal letters, 908 (1). ISSN 2041-8205

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Official URL: http://dx.doi.org/10.3847/2041-8213/abdb38




Abstract

Fast Radio Burst FRB 20180916B in its host galaxy SDSS J015800.28+654253.0 at 149 Mpc is by far the closest-known FRB with a robust host galaxy association. The source also exhibits a 16.35- day period in its bursting. Here we present optical and infrared imaging as well as integral field spectroscopy observations of FRB 20180916B with the WFC3 camera on the Hubble Space Telescope and the MEGARA spectrograph on the 10.4-m Gran Telescopio Canarias. The 60–90 milliarcsecond (mas) resolution of the Hubble imaging, along with the previous 2.3-mas localization of FRB 20180916B, allow us to probe its environment with a 30–60 pc resolution. We constrain any point-like star-formation or H II region at the location of FRB 20180916B to have an Hα luminosity L_(Hα) ˂̰ 10^(37) erg s^(−1) and, correspondingly, constrain the local star-formation rate to be ˂̰ 10^(−4) Mꙩ yr^(−1) . The constraint on Hα suggests that possible stellar companions to FRB 20180916B should be of a cooler, less massive spectral type than O6V. FRB 20180916B is 250 pc away (in projected distance) from the brightest pixel of the nearest young stellar clump, which is ∼ 380 pc in size (full-width at half maximum). With the typical projected velocities of pulsars, magnetars, or neutron stars in binaries (60 − 750 km s^(−1) ), FRB 20180916B would need 800 kyr to 7 Myr to traverse the observed distance from its presumed birth site. This timescale is inconsistent with the active ages of magnetars (˂̰ 10 kyr). Rather, the inferred age and observed separation are compatible with the ages of high-mass X-ray binaries and gamma-ray binaries, and their separations from the nearest OB associations .


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© 2021. The American Astronomical Society. Artículo firmado por 21 autores. J.W.T.H. acknowledges funding from an NWO Vici grant (“AstroFlash”; VI.C.192.045). A.G.P. acknowledges financial support from the Spanish Ministry of Economy and Competitiveness (MINECO) under grant RTI2018-096188-B-I00, which is partly funded by the European Regional Development Fund (ERDF). M.B. and P.C. are supported by FRQNT Doctoral Research Awards. V.M.K. holds the Lorne Trottier Chair in Astrophysics & Cosmology and a Distinguished James McGill Professorship and receives support from an NSERC Discovery Grant and Herzberg Award, from an R. Howard Webster Foundation Fellowship from the CIFAR, and from the FRQNT Centre de Recherche en Astrophysique du Québec. P.S. is a Dunlap Fellow and an NSERC Postdoctoral Fellow. The Dunlap Institute is funded through an endowment established by the David Dunlap family and the University of Toronto. B.M. acknowledges the support by the Spanish Ministerio de Ciencia e Innovación (MICINN) under grant PID2019-105510GB-C31 and through the “Center of Excellence María de Maeztu 2020-2023” award to the ICCUB (CEX2019-000918-M). F.K. acknowledges support by the Swedish Research Council. FRB research at UBC is supported by an NSERC Discovery Grant and by the Canadian Institute for Advanced Research. The NANOGrav project receives support from National Science Foundation (NSF) Physics Frontiers Center award number 1430284. This research is based on observations made with the NASA/ESA Hubble Space Telescope obtained from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–26555. These observations are associated with program 16072. This research is also based on observations made with the Gran Telescopio Canarias (GTC), installed at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, in the island of La Palma. This work is partly based on data obtained with MEGARA instrument, funded by European Regional Development Funds (ERDF), through Programa Operativo Canarias FEDER 2014-2020. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/ gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. 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.

Uncontrolled Keywords:Astronomy; Astrophysics
Subjects:Sciences > Physics > Astrophysics
Sciences > Physics > Astronomy
ID Code:64742
Deposited On:13 Apr 2021 09:22
Last Modified:13 Apr 2021 11:11

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