English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We present the first high signal-to-noise broadband X-ray spectrum of theradio-quiet type-2 Seyfert ESO 033-G002, combining data from $XMM$-$Newton$ and$NuSTAR$. The nuclear X-ray spectrum is complex, showing evidence for bothneutral and ionised absorption, as well as reflection from both the accretiondisc and more distant material, but our broadband coverage allows us todisentangle all of these different components. The total neutral column duringthis epoch is $N_{\rm{H}} \sim 5-6 \times 10^{22}$ cm$^{-2}$, consistent withthe optical classification of ESO 033-G002 as a type-2 Seyfert but not so largeas to prevent us from robustly determining the properties of the innermostaccretion flow. The ionised absorption - dominated by lines from Fe XXV and FeXXVI - reveals a moderately rapid outflow ($v_{\rm{out}} \sim 5400$ kms$^{-1}$) which has a column comparable to the neutral absorption. We find thedisc reflection from the innermost regions to be extreme, with a reflectionfraction of $R_{\rm{frac}} \sim 5$. This requires strong gravitationallightbending and, in turn, both an extremely compact corona (within $\sim$2$R_{\rm{G}}$ of the black hole) and a rapidly rotating black hole ($a^* >0.96$). Despite this tight size constraint, with a temperature of $kT_{\rm{e}}= 40-70$ keV the X-ray corona in ESO 033-G002 appears similar to other AGN interms of its placement in the compactness-temperature plane, consistent withsitting close to the limit determined by runaway pair production. Finally,combining X-ray spectroscopy, timing and updated optical spectroscopy, we alsoestimate the mass of the black hole to be $\log[M_{\rm{BH}} / M_{\odot}] \sim7.0 - 7.5$.

Extreme Relativistic Reflection in the Active Galaxy ESO 033-G002