Revealing an evolving corona around a prototypical intermediate-mass black hole
Abstract
Abstract X-ray observations of accreting black holes reveal X-ray reverberation \citep{Uttley2014}, which is an effective approach to infer the geometrical arrangement of the disc-corona system \citep{Emmanoulopoulos2014} and the dynamics of the inner accretion flow \citep{Reynolds1999}. A promising scenario to explain rapid X-ray variations is that they are a consequence of both accretion rate and coronal height changes \citep{Parker2014Mrk335, Wilkins2015}. While supermassive black holes (SMBHs) \citep[e.g.][]{2009Natur.459..540F, Zoghbi2012NGC4151, Cackett2013, Kara2016FeKlag} mostly, and a handful of stellar mass black holes (sBHs) \citep[e.g.][]{Uttley2011, DeMarco2011, Wang2022, Uttley-Malzac2025} show reverberation, it is not often seen in the intermediate-mass black hole (IMBH) regime due to the low count rate from the inner disc, except for a few low mass objects, $M_{\rm BH}
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