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 have assembled a sample of 5 X-ray-absorbed and submm-luminous type 1 QSOsat $z \sim 2$ which are simultaneously growing their central black holesthrough accretion and forming stars copiously. We present here the analysis oftheir rest-frame UV to submm Spectral Energy Distributions (SEDs), includingnew Herschel data. Both AGN (direct and reprocessed) and Star Formation (SF)emission are needed to model their SEDs. From the SEDs and their UV-opticalspectra we have estimated the masses of their black holes $M_{BH}\sim10^{9}-10^{10}\,M_{\odot}$, their intrinsic AGN bolometric luminosities$L_{BOL}\sim(0.8 - 20)\times 10^{13} L_{\odot}$, Eddington ratios$L_{BOL}/L_{Edd}\sim 0.1 - 1.1$ and bolometric corrections$L_{BOL}/L_{X,2-10}\sim 30 - 500$. These values are common among optically andX-ray-selected type 1 QSOs (except for RX~J1249), except for the bolometriccorrections, which are higher. These objects show very high far-infraredluminosities $L_{FIR}\sim$ (2 - 8)$\times10^{12}\,M_{\odot}$ and Star FormationRates SFR$\sim 1000 M_{\odot}/$y. From their $L_{FIR}$ and the shape of theirFIR-submm emission we have estimated star-forming dust masses of $M_{DUST}\sim10^9\,M_\odot$. We have found evidence of a tentative correlation between thegas column densities of the ionized absorbers detected in X-ray (N$_{H_{ion}}$)and $SFR$. Our computed black hole masses are amongst the most massive known.

Submm-bright X-ray absorbed QSOs at z~2: insights into the co-evolution of AGN and star-formation