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Dissecting the Local Environment of FRB 190608 in the Spiral Arm of its Host Galaxy

Authors :
Chittidi, Jay S.
Simha, Sunil
Mannings, Alexandra
Prochaska, J. Xavier
Ryder, Stuart D.
Rafelski, Marc
Neeleman, Marcel
Macquart, Jean-Pierre
Tejos, Nicolas
Jorgenson, Regina A.
Day, Cherie K.
Marnoch, Lachlan
Bhandari, Shivani
Deller, Adam T.
Qiu, Hao
Bannister, Keith W.
Shannon, Ryan M.
Heintz, Kasper E.
Source :
Volume 922, Number 2, 2021, Page 173
Publication Year :
2020

Abstract

We present a high-resolution analysis of the host galaxy of fast radio burst (FRB)~190608, an SB(r)c galaxy at $z=0.11778$ (hereafter HG 190608), to dissect its local environment and its contributions to the FRB properties. Our Hubble Space Telescope Wide Field Camera 3 ultraviolet and visible light image reveals that the subarcsecond localization of FRB~190608 is coincident with a knot of star-formation ($\Sigma_{\rm SFR} = 1.5 \times 10^{-2}~ M_{\odot} \, \rm \, yr^{-1} \, kpc^{-2}$) in the northwest spiral arm of HG~190608. Using H$\beta$ emission present in our Keck Cosmic Web Imager integral field spectrum of the galaxy with a surface brightness of $\mu_{\rm H\beta}= \mathrm{(3.36\pm0.21)\times10^{-17}\;erg\;s^{-1}\;cm^{-2}\;arcsec^{-2}}$, we infer an extinction-corrected H$\alpha$ surface brightness and compute a dispersion measure (DM) from the interstellar medium of HG 190608 of $\rm DM_{\rm Host,ISM} = 94 \pm 38~ \;pc\;cm^{-3}$. The galaxy rotates with a circular velocity $v_{\rm circ} = \rm 141 \pm 8~ km\;s^{-1}$ at an inclination $i_{\mathrm{gas}} = 37 \pm 3^\circ$, giving a dynamical mass $M_{\rm halo}^{\rm dyn} \approx 10^{11.96 \pm 0.08}~M_{\odot}$. This implies a halo contribution to the DM of $\rm DM_{\rm Host,Halo}= \rm 55\pm25 \;pc\;cm^{-3}$ subject to assumptions on the density profile and fraction of baryons retained. From the galaxy rotation curve, we infer a bar-induced pattern speed of $\Omega_p=34\pm 6\;\mathrm{km\;s^{-1}\;kpc^{-1}}$ using linear resonance theory. We then calculate the maximum time since star-formation for a progenitor using the furthest distance to the arm's leading edge within the localization, and find $t_{\mathrm{enc}} = 21_{-6}^{+25}$ Myr. Unlike previous high-resolution studies of FRB environments, we find no evidence of disturbed morphology, emission, or kinematics for FRB 190608.<br />Comment: 21 pages, 11 figure files, 10 figures in paper, 3 tables. Accepted to ApJ on Sept. 16, 2021, published Nov. 29, 2021

Details

Database :
arXiv
Journal :
Volume 922, Number 2, 2021, Page 173
Publication Type :
Report
Accession number :
edsarx.2005.13158
Document Type :
Working Paper
Full Text :
https://doi.org/10.3847/1538-4357/ac2818