Using XRISM’s high-resolution X-ray spectroscopy, we uncovered a complex, multiphase wind from the supermassive black hole in NGC 4151, ranging from slow warm absorbers to ultra-fast outflows. The fastest winds carry enough kinetic power to significantly affect the host galaxy and potentially suppress star formation. Read the paper
Building on previous work, we analyzed 14 XRISM observations over a year to track how NGC 4151’s disk winds respond to changes in the black hole’s X-ray emission. We found that the fastest winds become strongest about three hours after flares and during faint states, placing them close to their launching site and pointing toward magnetic driving. Read the paper
Using XMM-Newton spectroscopy of the tidal disruption event AT2021ehb, we measured a central black hole mass of roughly 300,000 Suns, probing the elusive low-mass end of the SMBH population. We also identified a possible highly clumpy or short-lived ultrafast wind moving at 20% of the speed of light. Read the paper
Using XMM-Newton observations of the tidal disruption event AT2021ehb, we estimated that its central black hole has a mass of only about 3 x 10^5 Suns, probing the elusive low-mass end of the supermassive black hole population. We also found evidence for a possible ultrafast wind traveling at 20% of the speed of light, which must be highly clumpy or short-lived. Read the paper
A model of the X-ray spectrum of active galactic nuclei that combines ionized reflection and a warm corona
We developed reXcor, a publicly available X-ray spectral model that self-consistently combines relativistic reflection and emission from a warm corona to explain the soft X-ray excess in active galactic nuclei. Applying it to HE 1143−1820 and NGC 4593 showed that both require a warm-corona contribution, providing new insight into how accretion energy is distributed around supermassive black holes. Read the paper
