A sudden period of high activity from repeating Fast Radio Burst 20201124A. (arXiv:2109.09254v2 [astro-ph.HE] UPDATED)

A sudden period of high activity from repeating Fast Radio Burst 20201124A. (arXiv:2109.09254v2 [astro-ph.HE] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Lanman_A/0/1/0/all/0/1">Adam E. Lanman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Andersen_B/0/1/0/all/0/1">Bridget C. Andersen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chawla_P/0/1/0/all/0/1">Pragya Chawla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Josephy_A/0/1/0/all/0/1">Alexander Josephy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kaspi_V/0/1/0/all/0/1">Victoria M. Kaspi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bandura_K/0/1/0/all/0/1">Kevin Bandura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bhardwaj_M/0/1/0/all/0/1">Mohit Bhardwaj</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boyle_P/0/1/0/all/0/1">Patrick J. Boyle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brar_C/0/1/0/all/0/1">Charanjot Brar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Breitman_D/0/1/0/all/0/1">Daniela Breitman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cassanelli_T/0/1/0/all/0/1">Tomas Cassanelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dong_F/0/1/0/all/0/1">Fengqi Dong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fonseca_E/0/1/0/all/0/1">Emmanuel Fonseca</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gaensler_B/0/1/0/all/0/1">Bryan M. Gaensler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Good_D/0/1/0/all/0/1">Deborah Good</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kaczmarek_J/0/1/0/all/0/1">Jane Kaczmarek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Leung_C/0/1/0/all/0/1">Calvin Leung</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Masui_K/0/1/0/all/0/1">Kiyoshi W. Masui</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Meyers_B/0/1/0/all/0/1">Bradley W. Meyers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ng_C/0/1/0/all/0/1">Cherry Ng</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Patel_C/0/1/0/all/0/1">Chitrang Patel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pearlman_A/0/1/0/all/0/1">Aaron B. Pearlman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Petroff_E/0/1/0/all/0/1">Emily Petroff</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pleunis_Z/0/1/0/all/0/1">Ziggy Pleunis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rafiei_Ravandi_M/0/1/0/all/0/1">Masoud Rafiei-Ravandi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rahman_M/0/1/0/all/0/1">Mubdi Rahman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sanghavi_P/0/1/0/all/0/1">Pranav Sanghavi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Scholz_P/0/1/0/all/0/1">Paul Scholz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shin_K/0/1/0/all/0/1">Kaitlyn Shin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stairs_I/0/1/0/all/0/1">Ingrid Stairs</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tendulkar_S/0/1/0/all/0/1">Shriharsh Tendulkar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zwaniga_A/0/1/0/all/0/1">Andrew Zwaniga</a>

The repeating FRB 20201124A was first discovered by CHIME/FRB in November of
2020, after which it was seen to repeat a few times over several months. FRB
20201124A entered a period of high activity in April of 2021, at which time
several observatories recorded tens to hundreds more bursts from the source.
These follow-up observations enabled precise localization and host galaxy
identification. In this paper, we report on the CHIME/FRB-detected bursts from
FRB 20201124A, including their best-fit morphologies, fluences, and arrival
times. The large exposure time of the CHIME/FRB telescope to the location of
this source allows us to constrain its rates of activity. We analyze the
repetition rates over different spans of time, constraining the rate prior to
discovery to $< 3.4$ day$^{-1}$ (at 3$sigma$), and demonstrate significant
change in the event rate following initial detection. Lastly, we perform a
maximum-likelihood estimation of a power-law luminosity function, finding a
best-fit index $alpha = -4.5 pm 1.5 pm 0.7$, with a break at a fluence
threshold of $F_{rm min} sim 17$~Jy~ms, consistent with the fluence
completeness limit of the observations. This index is consistent within
uncertainties with those of other repeating FRBs for which it has been
determined.

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