2026-06-27T11:08:59Zhttps://docta.ucm.es/rest/oai/request

oai:docta.ucm.es:20.500.14352/79722024-09-10T18:41:52Zcom_20.500.14352_14col_20.500.14352_15

00925njm 22002777a 4500 dc Tendulkar, Shriharsh P. author Gil De Paz, Armando author Kirichenko, Aida Yu author Hessels, Jason W. T. author Bhardwaj, Mohit author Ávila, Fernando author Bassa, Cees author Chawla, Pragya author Fonseca, Emmanuel author Kaspi, Victoria M. author Keimpema, Aard author Kirsten, Franz author Lazio, T. Joseph W. author Marcote, Benito author Masui, Kiyoshi author Nimmo, Kenzie author Paragi, Zsolt author Rahman, Mubdi author Reverte Payá, Daniel author Scholz, Paul author Stair, Ingrid author 2021-02 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 . 2041-8205 10.3847/2041-8213/abdb38 https://hdl.handle.net/20.500.14352/7972 http://dx.doi.org/10.3847/2041-8213/abdb38 https://iopscience.iop.org/ https://arxiv.org/abs/2011.03257 The 60 pc environment of FRB 20180916B