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<button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Brusa%2C+M&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Brusa%2C+M&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Brusa%2C+M&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Brusa%2C+M&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=Brusa%2C+M&start=150" class="pagination-link " aria-label="Page 4" aria-current="page">4 </a> </li> <li> <a 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data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> The radio properties of the JWST-discovered AGN </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mazzolari%2C+G">G. Mazzolari</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">R. Gilli</a>, <a href="/search/astro-ph?searchtype=author&query=Maiolino%2C+R">R. Maiolino</a>, <a href="/search/astro-ph?searchtype=author&query=Prandoni%2C+I">I. Prandoni</a>, <a href="/search/astro-ph?searchtype=author&query=Delvecchio%2C+I">I. Delvecchio</a>, <a href="/search/astro-ph?searchtype=author&query=Norman%2C+C">C. Norman</a>, <a href="/search/astro-ph?searchtype=author&query=Jimenez-Andrade%2C+E+F">E. F. Jimenez-Andrade</a>, <a href="/search/astro-ph?searchtype=author&query=Belladitta%2C+S">S. Belladitta</a>, <a href="/search/astro-ph?searchtype=author&query=Vito%2C+F">F. Vito</a>, <a href="/search/astro-ph?searchtype=author&query=Momjian%2C+E">E. Momjian</a>, <a href="/search/astro-ph?searchtype=author&query=Chiaberge%2C+M">M. Chiaberge</a>, <a href="/search/astro-ph?searchtype=author&query=Trefoloni%2C+B">B. Trefoloni</a>, <a href="/search/astro-ph?searchtype=author&query=Signorini%2C+M">M. Signorini</a>, <a href="/search/astro-ph?searchtype=author&query=Ji%2C+X">X. Ji</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Amato%2C+Q">Q. D'Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Risaliti%2C+G">G. Risaliti</a>, <a href="/search/astro-ph?searchtype=author&query=Baldi%2C+R+D">R. D. Baldi</a>, <a href="/search/astro-ph?searchtype=author&query=Fabian%2C+A">A. Fabian</a>, <a href="/search/astro-ph?searchtype=author&query=%C3%9Cbler%2C+H">H. 脺bler</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Eugenio%2C+F">F. D'Eugenio</a>, <a href="/search/astro-ph?searchtype=author&query=Scholtz%2C+J">J. Scholtz</a>, <a href="/search/astro-ph?searchtype=author&query=Juod%C5%BEbalis%2C+I">I. Juod啪balis</a>, <a href="/search/astro-ph?searchtype=author&query=Mignoli%2C+M">M. Mignoli</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Murphy%2C+E">E. Murphy</a> , et al. (1 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2412.04224v1-abstract-short" style="display: inline;"> We explore the radio emission of spectroscopically confirmed, X-ray weak, Broad Line AGN (BLAGN, or type 1) selected with JWST in the GOODS-N field, one of the fields with the best combination of deep radio observations and statistics of JWST-selected BLAGN. We use deep radio data at different frequencies (144\,MHz, 1.5\,GHz, 3\,GHz, 5.5\,GHz, 10\,GHz), and we find that none of the 22 sources inve… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.04224v1-abstract-full').style.display = 'inline'; document.getElementById('2412.04224v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.04224v1-abstract-full" style="display: none;"> We explore the radio emission of spectroscopically confirmed, X-ray weak, Broad Line AGN (BLAGN, or type 1) selected with JWST in the GOODS-N field, one of the fields with the best combination of deep radio observations and statistics of JWST-selected BLAGN. We use deep radio data at different frequencies (144\,MHz, 1.5\,GHz, 3\,GHz, 5.5\,GHz, 10\,GHz), and we find that none of the 22 sources investigated is detected at any of the aforementioned frequencies. Similarly, the radio stacking analysis does not reveal any detection down to an rms of $\sim 0.2渭$Jy beam$^{-1}$, corresponding to a $3蟽$ upper limit at rest frame 5 GHz of $L_{5GHz}=2\times10^{39}$ erg s$^{-1}$ at the mean redshift of the sample $z\sim 5.2$. We compared this and individual sources upper limits with expected radio luminosities estimated assuming different AGN scaling relations. For most of the sources the radio luminosity upper limits are still compatible with expectations for radio-quiet (RQ) AGN; nevertheless, the more stringent stacking upper limits and the fact that no detection is found would suggest that JWST-selected BLAGN are weaker than standard AGN even at radio frequencies. We discuss some scenarios that could explain the possible radio weakness, such as free-free absorption from a dense medium, or the lack of either magnetic field or a corona, possibly as a consequence of super-Eddington accretion. These scenarios would also explain the observed X-ray weakness. We also conclude that $\sim$1 dex more sensitive radio observations are needed to better constrain the level of radio emission (or lack thereof) for the bulk of these sources. The Square Kilometer Array Observatory (SKAO) will likely play a crucial role in assessing the properties of this AGN population. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.04224v1-abstract-full').style.display = 'none'; document.getElementById('2412.04224v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to A&A, comments are welcome</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.02105">arXiv:2411.02105</a> <span> [<a href="https://arxiv.org/pdf/2411.02105">pdf</a>, <a href="https://arxiv.org/format/2411.02105">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> HYPERION: broad-band X-ray-to-near-infrared emission of Quasars in the first billion years of the Universe </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Saccheo%2C+I">I. Saccheo</a>, <a href="/search/astro-ph?searchtype=author&query=Bongiorno%2C+A">A. Bongiorno</a>, <a href="/search/astro-ph?searchtype=author&query=Piconcelli%2C+E">E. Piconcelli</a>, <a href="/search/astro-ph?searchtype=author&query=Zappacosta%2C+L">L. Zappacosta</a>, <a href="/search/astro-ph?searchtype=author&query=Bischetti%2C+M">M. Bischetti</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Odorico%2C+V">V. D'Odorico</a>, <a href="/search/astro-ph?searchtype=author&query=Done%2C+C">C. Done</a>, <a href="/search/astro-ph?searchtype=author&query=Temple%2C+M+J">M. J. Temple</a>, <a href="/search/astro-ph?searchtype=author&query=Testa%2C+V">V. Testa</a>, <a href="/search/astro-ph?searchtype=author&query=Tortosa%2C+A">A. Tortosa</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Carniani%2C+S">S. Carniani</a>, <a href="/search/astro-ph?searchtype=author&query=Civano%2C+F">F. Civano</a>, <a href="/search/astro-ph?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/astro-ph?searchtype=author&query=Cristiani%2C+S">S. Cristiani</a>, <a href="/search/astro-ph?searchtype=author&query=De+Cicco%2C+D">D. De Cicco</a>, <a href="/search/astro-ph?searchtype=author&query=Elvis%2C+M">M. Elvis</a>, <a href="/search/astro-ph?searchtype=author&query=Fan%2C+X">X. Fan</a>, <a href="/search/astro-ph?searchtype=author&query=Feruglio%2C+C">C. Feruglio</a>, <a href="/search/astro-ph?searchtype=author&query=Fiore%2C+F">F. Fiore</a>, <a href="/search/astro-ph?searchtype=author&query=Gallerani%2C+S">S. Gallerani</a>, <a href="/search/astro-ph?searchtype=author&query=Giallongo%2C+E">E. Giallongo</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">R. Gilli</a>, <a href="/search/astro-ph?searchtype=author&query=Grazian%2C+A">A. Grazian</a>, <a href="/search/astro-ph?searchtype=author&query=Guainazzi%2C+M">M. Guainazzi</a> , et al. (19 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.02105v1-abstract-short" style="display: inline;"> We aim at characterizing the X-ray-to-optical/near-infrared broad-band emission of luminous QSOs in the first Gyr of cosmic evolution to understand whether they exhibit differences compared to the lower-\textit{z} QSO population. Our goal is also to provide for these objects a reliable and uniform catalog of SED fitting derivable properties such as bolometric and monochromatic luminosities, Edding… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.02105v1-abstract-full').style.display = 'inline'; document.getElementById('2411.02105v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.02105v1-abstract-full" style="display: none;"> We aim at characterizing the X-ray-to-optical/near-infrared broad-band emission of luminous QSOs in the first Gyr of cosmic evolution to understand whether they exhibit differences compared to the lower-\textit{z} QSO population. Our goal is also to provide for these objects a reliable and uniform catalog of SED fitting derivable properties such as bolometric and monochromatic luminosities, Eddington ratios, dust extinction, strength of the hot dust emission. We characterize the X-ray/UV emission of each QSO using average SEDs from luminous Type 1 sources and calculate bolometric and monochromatic luminosities. Finally we construct a mean SED extending from the X-rays to the NIR bands. We find that the UV-optical emission of these QSOs can be modelled with templates of $z\sim$2 luminous QSOs. We observe that the bolometric luminosities derived adopting some bolometric corrections at 3000 脜 ($BC_{3000\text脜}$) largely used in the literature are slightly overestimated by 0.13 dex as they also include reprocessed IR emission. We estimate a revised value, i.e. $BC_{3000\text脜}=3.3 $ which can be used for deriving $L_\text{bol}$ in \textit{z} $\geq$ 6 QSOs. A sub-sample of 11 QSOs is provided with rest-frame NIR photometry, showing a broad range of hot dust emission strength, with two sources exhibiting low levels of emission. Despite potential observational biases arising from non-uniform photometric coverage and selection biases, we produce a X-ray-to-NIR mean SED for QSOs at \textit{z} $\gtrsim$ 6, revealing a good match with templates of lower-redshift, luminous QSOs up to the UV-optical range, with a slightly enhanced contribution from hot dust in the NIR. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.02105v1-abstract-full').style.display = 'none'; document.getElementById('2411.02105v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.12786">arXiv:2410.12786</a> <span> [<a href="https://arxiv.org/pdf/2410.12786">pdf</a>, <a href="https://arxiv.org/format/2410.12786">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> HYPERION. Shedding light on the first luminous quasars: A correlation between UV disc winds and X-ray continuum </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Tortosa%2C+A">A. Tortosa</a>, <a href="/search/astro-ph?searchtype=author&query=Zappacosta%2C+L">L. Zappacosta</a>, <a href="/search/astro-ph?searchtype=author&query=Piconcelli%2C+E">E. Piconcelli</a>, <a href="/search/astro-ph?searchtype=author&query=Bischetti%2C+M">M. Bischetti</a>, <a href="/search/astro-ph?searchtype=author&query=Done%2C+C">C. Done</a>, <a href="/search/astro-ph?searchtype=author&query=Miniutti%2C+G">G. Miniutti</a>, <a href="/search/astro-ph?searchtype=author&query=Saccheo%2C+I">I. Saccheo</a>, <a href="/search/astro-ph?searchtype=author&query=Vietri%2C+G">G. Vietri</a>, <a href="/search/astro-ph?searchtype=author&query=Bongiorno%2C+A">A. Bongiorno</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Carniani%2C+S">S. Carniani</a>, <a href="/search/astro-ph?searchtype=author&query=Chilingarian%2C+I+V">I. V. Chilingarian</a>, <a href="/search/astro-ph?searchtype=author&query=Civano%2C+F">F. Civano</a>, <a href="/search/astro-ph?searchtype=author&query=Cristiani%2C+S">S. Cristiani</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Odorico%2C+V">V. D'Odorico</a>, <a href="/search/astro-ph?searchtype=author&query=Elvis%2C+M">M. Elvis</a>, <a href="/search/astro-ph?searchtype=author&query=Fan%2C+X">X. Fan</a>, <a href="/search/astro-ph?searchtype=author&query=Feruglio%2C+C">C. Feruglio</a>, <a href="/search/astro-ph?searchtype=author&query=Fiore%2C+F">F. Fiore</a>, <a href="/search/astro-ph?searchtype=author&query=Gallerani%2C+S">S. Gallerani</a>, <a href="/search/astro-ph?searchtype=author&query=Giallongo%2C+E">E. Giallongo</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">R. Gilli</a>, <a href="/search/astro-ph?searchtype=author&query=Grazian%2C+A">A. Grazian</a>, <a href="/search/astro-ph?searchtype=author&query=Guainazzi%2C+M">M. Guainazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Haardt%2C+F">F. Haardt</a> , et al. (19 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.12786v1-abstract-short" style="display: inline;"> One of the main open questions in the field of luminous ($L_{\rm bol}>10^{47}\,\rm erg\,s^{-1}$) quasars (QSOs) at $z \gtrsim 6$ is the rapid formation ($< 1\,$Gyr) of their supermassive black holes (SMBHs). For this work we analysed the relation between the X-ray properties and other properties describing the physics and growth of both the accretion disc and the SMBH in QSOs at the Epoch of Reion… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.12786v1-abstract-full').style.display = 'inline'; document.getElementById('2410.12786v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.12786v1-abstract-full" style="display: none;"> One of the main open questions in the field of luminous ($L_{\rm bol}>10^{47}\,\rm erg\,s^{-1}$) quasars (QSOs) at $z \gtrsim 6$ is the rapid formation ($< 1\,$Gyr) of their supermassive black holes (SMBHs). For this work we analysed the relation between the X-ray properties and other properties describing the physics and growth of both the accretion disc and the SMBH in QSOs at the Epoch of Reionization (EoR). The sample consists of 21 $z>6$ QSOs, which includes 16 sources from the rapidly grown QSOs from the HYPERION sample and five other luminous QSOs with available high-quality archival X-ray data. We discovered a strong and statistically significant ($>3蟽$) relation between the X-ray continuum photon index ($螕$) and the $\rm C\,IV$ disc wind velocity ($v_{\rm C\,IV}$) in $z>6$ luminous QSOs, whereby the higher the $v_{\rm C\,IV}$, the steeper the $螕$. This relation suggests a link between the disc-corona configuration and the kinematics of disc winds. Furthermore, we find evidence at $>2-3蟽$ level that $螕$ and $v_{\rm C\,IV}$ are correlated to the growth rate history of the SMBH. Although additional data are needed to confirm it, this result may suggest that, in luminous $z>6$ QSOs, the SMBH predominantly grows via fast accretion rather than via initial high seed BH mass. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.12786v1-abstract-full').style.display = 'none'; document.getElementById('2410.12786v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astronomy & Astrophysics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.07941">arXiv:2410.07941</a> <span> [<a href="https://arxiv.org/pdf/2410.07941">pdf</a>, <a href="https://arxiv.org/format/2410.07941">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202451877">10.1051/0004-6361/202451877 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Incidence of afterglow plateaus in gamma-ray bursts associated with binary neutron star mergers </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Guglielmi%2C+L">Luca Guglielmi</a>, <a href="/search/astro-ph?searchtype=author&query=Stratta%2C+G">Giulia Stratta</a>, <a href="/search/astro-ph?searchtype=author&query=Dall%27Osso%2C+S">Simone Dall'Osso</a>, <a href="/search/astro-ph?searchtype=author&query=Singh%2C+P">Paramvir Singh</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">Marcella Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Perna%2C+R">Rosalba Perna</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.07941v2-abstract-short" style="display: inline;"> One of the most surprising gamma-ray burst (GRB) features discovered with the Swift-X ray telescope (XRT) is a plateau phase in the early X-ray afterglow light curves. These plateaus are observed in the majority of long GRBs, while their incidence in short GRBs (SGRBs) is still uncertain due to their fainter X-ray afterglow luminosity with respect to long GRBs. An accurate estimate of the fraction… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.07941v2-abstract-full').style.display = 'inline'; document.getElementById('2410.07941v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.07941v2-abstract-full" style="display: none;"> One of the most surprising gamma-ray burst (GRB) features discovered with the Swift-X ray telescope (XRT) is a plateau phase in the early X-ray afterglow light curves. These plateaus are observed in the majority of long GRBs, while their incidence in short GRBs (SGRBs) is still uncertain due to their fainter X-ray afterglow luminosity with respect to long GRBs. An accurate estimate of the fraction of SGRBs with plateaus is of utmost relevance given the implications that the plateau may have for our understanding of the jet structure and possibly of the nature of the binary neutron star (BNS) merger remnant. This work presents the results of an extensive data analysis of the largest and most up-to-date sample of short GRBs observed with the XRT, and for which the redshift has been measured. We find a plateau incidence of 18-37% in short GRBs, which is a significantly lower fraction than that measured in long GRBs (>50%). Although still debated, the plateau phase could be explained as energy injection from the spin-down power of a newly born magnetized neutron star (NS; magnetar). We show that this scenario can nicely reproduce the observed short GRB plateaus, while at the same time providing a natural explanation for the different plateau fractions between short and long GRBs. In particular, our findings may imply that only a minority of BNS mergers generating short GRBs leave behind a sufficiently stable or long-lived neutron star (NS) to form a plateau. From the probability distribution of the BNS remnant mass, a fraction 18-37% of short GRB plateaus implies a maximum NS mass in the range $\sim$ 2.3 - 2.35 M$_{\odot}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.07941v2-abstract-full').style.display = 'none'; document.getElementById('2410.07941v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 9 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 692, A73 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.16821">arXiv:2408.16821</a> <span> [<a href="https://arxiv.org/pdf/2408.16821">pdf</a>, <a href="https://arxiv.org/format/2408.16821">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> KASHz+SUPER: Evidence of cold molecular gas depletion in AGN hosts at cosmic noon </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bertola%2C+E">E. Bertola</a>, <a href="/search/astro-ph?searchtype=author&query=Circosta%2C+C">C. Circosta</a>, <a href="/search/astro-ph?searchtype=author&query=Ginolfi%2C+M">M. Ginolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Mainieri%2C+V">V. Mainieri</a>, <a href="/search/astro-ph?searchtype=author&query=Vignali%2C+C">C. Vignali</a>, <a href="/search/astro-ph?searchtype=author&query=Rivera%2C+G+C">G. Calistro Rivera</a>, <a href="/search/astro-ph?searchtype=author&query=Ward%2C+S+R">S. R. Ward</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+I+E">I. E. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Pensabene%2C+A">A. Pensabene</a>, <a href="/search/astro-ph?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/astro-ph?searchtype=author&query=Bischetti%2C+M">M. Bischetti</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Cappi%2C+M">M. Cappi</a>, <a href="/search/astro-ph?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/astro-ph?searchtype=author&query=Contursi%2C+A">A. Contursi</a>, <a href="/search/astro-ph?searchtype=author&query=Cicone%2C+C">C. Cicone</a>, <a href="/search/astro-ph?searchtype=author&query=Cresci%2C+G">G. Cresci</a>, <a href="/search/astro-ph?searchtype=author&query=Dadina%2C+M">M. Dadina</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Amato%2C+Q">Q. D'Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Feltre%2C+A">A. Feltre</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+C+M">C. M. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Kakkad%2C+D">D. Kakkad</a>, <a href="/search/astro-ph?searchtype=author&query=Lamperti%2C+I">I. Lamperti</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzuisi%2C+G">G. Lanzuisi</a>, <a href="/search/astro-ph?searchtype=author&query=Mannucci%2C+F">F. Mannucci</a> , et al. (10 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.16821v1-abstract-short" style="display: inline;"> The energy released by AGN has the potential to heat or remove the gas of the ISM, thus likely impacting the cold molecular gas reservoir of host galaxies at first, with star formation following on longer timescales. Previous works on high-z galaxies have yielded conflicting results, possibly due to selection biases and other systematics. To provide a reliable benchmark for galaxy evolution models… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.16821v1-abstract-full').style.display = 'inline'; document.getElementById('2408.16821v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.16821v1-abstract-full" style="display: none;"> The energy released by AGN has the potential to heat or remove the gas of the ISM, thus likely impacting the cold molecular gas reservoir of host galaxies at first, with star formation following on longer timescales. Previous works on high-z galaxies have yielded conflicting results, possibly due to selection biases and other systematics. To provide a reliable benchmark for galaxy evolution models at cosmic noon (z=1-3), two surveys were conceived: SUPER and KASHz, both targeting unbiased X-ray-selected AGN at z>1 that span a wide bolometric luminosity range. In this paper, we assess the effects of AGN feedback on the molecular gas content of host galaxies in a statistically robust, uniformly selected, coherently analyzed sample of AGN at z=1-2.6, drawn from the KASHz and SUPER surveys. By using ALMA data in combination with dedicated SED modeling, we retrieve CO and FIR luminosity as well as $M_*$ of SUPER and KASHz AGN. We selected non-active galaxies from PHIBBS, ASPECS and multiple ALMA/NOEMA surveys of sub-mm galaxies. By matching the samples in z, $M_*$ and $L_{FIR}$, we compared the properties of AGN and non-active galaxies within a Bayesian framework. We find that AGN hosts at given $L_{FIR}$ are on average CO depleted compared to non-active galaxies, confirming what was previously found in the SUPER survey. Moreover, the molecular gas fraction distributions of AGN and non-active galaxies are statistically different, with that of of AGN being skewed to lower values. Our results indicate that AGN can indeed reduce the total cold molecular gas reservoir of their host galaxies. Lastly, by comparing our results with predictions from three cosmological simulations (TNG, Eagle and Simba) filtered to match the observed properties, we confirm already known discrepancies and highlight new ones between observations and simulations.[Abridged] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.16821v1-abstract-full').style.display = 'none'; document.getElementById('2408.16821v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">26 pages (17 in the main body of the paper and 9 in the appendix), 14 figures (11 in the main body of the paper and 3 in the appendix), 8 tables (2 in the main body of the paper and 6 in the appendix). Accepted for publication in A&A, in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.15615">arXiv:2408.15615</a> <span> [<a href="https://arxiv.org/pdf/2408.15615">pdf</a>, <a href="https://arxiv.org/format/2408.15615">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Narrow line AGN selection in CEERS: spectroscopic selection, physical properties, X-ray and radio analysis </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mazzolari%2C+G">Giovanni Mazzolari</a>, <a href="/search/astro-ph?searchtype=author&query=Scholtz%2C+J">Jan Scholtz</a>, <a href="/search/astro-ph?searchtype=author&query=Maiolino%2C+R">Roberto Maiolino</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">Roberto Gilli</a>, <a href="/search/astro-ph?searchtype=author&query=Traina%2C+A">Alberto Traina</a>, <a href="/search/astro-ph?searchtype=author&query=L%C3%B3pez%2C+I+E">Ivan E. L贸pez</a>, <a href="/search/astro-ph?searchtype=author&query=%C3%9Cbler%2C+H">Hannah 脺bler</a>, <a href="/search/astro-ph?searchtype=author&query=Trefoloni%2C+B">Bartolomeo Trefoloni</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Eugenio%2C+F">Francesco D'Eugenio</a>, <a href="/search/astro-ph?searchtype=author&query=Ji%2C+X">Xihan Ji</a>, <a href="/search/astro-ph?searchtype=author&query=Mignoli%2C+M">Marco Mignoli</a>, <a href="/search/astro-ph?searchtype=author&query=Vito%2C+F">Fabio Vito</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">Marcella Brusa</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.15615v1-abstract-short" style="display: inline;"> In this work, we spectroscopically select narrow-line AGN (NLAGN) among the $\sim 300$ publicly available medium-resolution spectra of the CEERS Survey. Using both traditional and newly identified emission line NLAGN diagnostics diagrams, we identified 52 NLAGN at $2\lesssim z\lesssim 9$ on which we performed a detailed multiwavelength analysis. We also identified 4 new $z\lesssim 2$ broad-line AG… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.15615v1-abstract-full').style.display = 'inline'; document.getElementById('2408.15615v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.15615v1-abstract-full" style="display: none;"> In this work, we spectroscopically select narrow-line AGN (NLAGN) among the $\sim 300$ publicly available medium-resolution spectra of the CEERS Survey. Using both traditional and newly identified emission line NLAGN diagnostics diagrams, we identified 52 NLAGN at $2\lesssim z\lesssim 9$ on which we performed a detailed multiwavelength analysis. We also identified 4 new $z\lesssim 2$ broad-line AGN (BLAGN), in addition to the 8 previously reported high-$z$ BLAGN. We found that the traditional BPT diagnostic diagrams are not suited to identify high-$z$ AGN, while most of the high-$z$ NLAGN are selected using the recently proposed AGN diagnostic diagrams based on the [OIII]$位$4363 auroral line or high-ionization emission lines. We compared the emission line velocity dispersion and the obscuration of the sample of NLAGN with those of the parent sample without finding significant differences between the two distributions, suggesting a population of AGN heavily buried and not significantly impacting the host galaxies' physical properties, as further confirmed by SED-fitting. The bolometric luminosities of the high-$z$ NLAGNs selected in this work are well below those sampled by surveys before JWST, potentially explaining the weak impact of these AGN. Finally, we investigate the X-ray properties of the selected NLAGN and of the sample of high-$z$ BLAGN. We find that all but 4 NLAGN are undetected in the deep X-ray image of the field, as well as all the high-$z$ BLAGN. We do not obtain a detection even by stacking the undetected sources, resulting in an X-ray weakness of $\sim 1-2$ dex from what is expected based on their bolometric luminosities. To discriminate between a heavily obscured AGN scenario or an intrinsic X-ray weakness of these sources, we performed a radio stacking analysis, which did not reveal any detection leaving open the questions about the origin of the X-ray weakness. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.15615v1-abstract-full').style.display = 'none'; document.getElementById('2408.15615v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to A&A, comments are welcome</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.14546">arXiv:2408.14546</a> <span> [<a href="https://arxiv.org/pdf/2408.14546">pdf</a>, <a href="https://arxiv.org/format/2408.14546">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The Extended Mapping Obscuration to Reionization with ALMA (Ex-MORA) Survey: 5$蟽$ Source Catalog and Redshift Distribution </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Long%2C+A+S">Arianna S. Long</a>, <a href="/search/astro-ph?searchtype=author&query=Casey%2C+C+M">Caitlin M. Casey</a>, <a href="/search/astro-ph?searchtype=author&query=McKinney%2C+J">Jed McKinney</a>, <a href="/search/astro-ph?searchtype=author&query=Zavala%2C+J+A">Jorge A. Zavala</a>, <a href="/search/astro-ph?searchtype=author&query=Akins%2C+H+B">Hollis B. Akins</a>, <a href="/search/astro-ph?searchtype=author&query=Cooper%2C+O+R">Olivia R. Cooper</a>, <a href="/search/astro-ph?searchtype=author&query=Lambrides%2C+M+B+E+L">Matthieu Bethermin Erini L. Lambrides</a>, <a href="/search/astro-ph?searchtype=author&query=Franco%2C+M">Maximilien Franco</a>, <a href="/search/astro-ph?searchtype=author&query=Caputi%2C+K">Karina Caputi</a>, <a href="/search/astro-ph?searchtype=author&query=Champagne%2C+J+B">Jaclyn B. Champagne</a>, <a href="/search/astro-ph?searchtype=author&query=Man%2C+A+W+S">Allison W. S. Man</a>, <a href="/search/astro-ph?searchtype=author&query=Treister%2C+E">Ezequiel Treister</a>, <a href="/search/astro-ph?searchtype=author&query=Manning%2C+S+M">Sinclaire M. Manning</a>, <a href="/search/astro-ph?searchtype=author&query=Sanders%2C+D+B">David B. Sanders</a>, <a href="/search/astro-ph?searchtype=author&query=Talia%2C+M">Margherita Talia</a>, <a href="/search/astro-ph?searchtype=author&query=Aravena%2C+M">Manuel Aravena</a>, <a href="/search/astro-ph?searchtype=author&query=Clements%2C+D+L">D. L. Clements</a>, <a href="/search/astro-ph?searchtype=author&query=da+Cunha%2C+E">Elisabete da Cunha</a>, <a href="/search/astro-ph?searchtype=author&query=Faisst%2C+A+L">Andreas L. Faisst</a>, <a href="/search/astro-ph?searchtype=author&query=Gentile%2C+F">Fabrizio Gentile</a>, <a href="/search/astro-ph?searchtype=author&query=Hodge%2C+J">Jacqueline Hodge</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G">Gabriel Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">Marcella Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">Steven L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Fujimoto%2C+S">Seiji Fujimoto</a> , et al. (19 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.14546v1-abstract-short" style="display: inline;"> One of the greatest challenges in galaxy evolution over the last decade has been constraining the prevalence of heavily dust-obscured galaxies in the early Universe. At $z>3$, these galaxies are increasingly rare, and difficult to identify as they are interspersed among the more numerous dust-obscured galaxy population at $z=1-3$, making efforts to secure confident spectroscopic redshifts expensiv… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.14546v1-abstract-full').style.display = 'inline'; document.getElementById('2408.14546v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.14546v1-abstract-full" style="display: none;"> One of the greatest challenges in galaxy evolution over the last decade has been constraining the prevalence of heavily dust-obscured galaxies in the early Universe. At $z>3$, these galaxies are increasingly rare, and difficult to identify as they are interspersed among the more numerous dust-obscured galaxy population at $z=1-3$, making efforts to secure confident spectroscopic redshifts expensive, and sometimes unsuccessful. In this work, we present the Extended Mapping Obscuration to Reionization with ALMA (Ex-MORA) Survey -- a 2mm blank-field survey in the COSMOS-Web field, and the largest ever ALMA blank-field survey to-date covering 577 arcmin$^2$. Ex-MORA is an expansion of the MORA survey designed to identify primarily $z>3$ dusty, star-forming galaxies while simultaneously filtering out the more numerous $z<3$ population by leveraging the very negative $K$-correction at observed-frame 2mm. We identify 37 significant ($>$5$蟽$) sources, 33 of which are robust thermal dust emitters. We measure a median redshift of $\langle z \rangle = 3.6^{+0.1}_{-0.2}$, with two-thirds of the sample at $z>3$, and just under half at $z>4$, demonstrating the overall success of the 2mm-selection technique. The integrated $z>3$ volume density of Ex-MORA sources is $\sim1-3\times10^{-5}$ Mpc$^{-3}$, consistent with other surveys of infrared luminous galaxies at similar epochs. We also find that techniques using rest-frame optical emission (or lack thereof) to identify $z>3$ heavily dust-obscured galaxies miss at least half of Ex-MORA galaxies. This supports the idea that the dusty galaxy population is heterogeneous, and that synergies across observatories spanning multiple energy regimes are critical to understanding their formation and evolution at $z>3$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.14546v1-abstract-full').style.display = 'none'; document.getElementById('2408.14546v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 5 figures, submitted to ApJ; fully reduced mosaic will be shared upon publication</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.04973">arXiv:2408.04973</a> <span> [<a href="https://arxiv.org/pdf/2408.04973">pdf</a>, <a href="https://arxiv.org/format/2408.04973">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> On the correlation between young massive star clusters and gamma-ray unassociated sources </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Peron%2C+G">Giada Peron</a>, <a href="/search/astro-ph?searchtype=author&query=Morlino%2C+G">Giovanni Morlino</a>, <a href="/search/astro-ph?searchtype=author&query=Gabici%2C+S">Stefano Gabici</a>, <a href="/search/astro-ph?searchtype=author&query=Amato%2C+E">Elena Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Purushothaman%2C+A">Archana Purushothaman</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">Marcella Brusa</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.04973v1-abstract-short" style="display: inline;"> Star clusters (SCs) are potential cosmic-ray (CR) accelerators and therefore are expected to emit high-energy radiation. However, a clear detection of gamma-ray emission from this source class has only been possible for a handful of cases. This could in principle result from two different reasons: either detectable SCs are limited to a small fraction of the total number of Galactic SCs, or gamma-r… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.04973v1-abstract-full').style.display = 'inline'; document.getElementById('2408.04973v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.04973v1-abstract-full" style="display: none;"> Star clusters (SCs) are potential cosmic-ray (CR) accelerators and therefore are expected to emit high-energy radiation. However, a clear detection of gamma-ray emission from this source class has only been possible for a handful of cases. This could in principle result from two different reasons: either detectable SCs are limited to a small fraction of the total number of Galactic SCs, or gamma-ray-emitting SCs are not recognized as such and therefore are listed in the ensemble of unidentified sources. In this Letter we investigate this latter scenario, by comparing available catalogs of SCs and HII regions, obtained from Gaia and WISE observations, to the gamma-ray GeV and TeV catalogs built from Fermi-LAT, H.E.S.S. and LHAASO data. The significance of the correlation between catalogs is evaluated by comparing the results with simulations of synthetic populations. A strong correlation emerges between Fermi-LAT unidentified sources and HII regions which trace massive SCs in the earliest (< 1-2 Myr) phase of their life, where no supernova explosions have happened yet, confirming that winds of massive stars can alone accelerate particles and produce gamma-ray emission at least up to GeV energies. The association with TeV-energies sources is less evident. Similarly, no significant association is found between Gaia SCs and GeV nor TeV sources. We ascribe this fact to the larger extension of these objects, but also to an intrinsic bias in the Gaia selection towards SCs surrounded by a lower target gas density, that would otherwise hinder the detection in the optical waveband. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.04973v1-abstract-full').style.display = 'none'; document.getElementById('2408.04973v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApJL</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.04099">arXiv:2407.04099</a> <span> [<a href="https://arxiv.org/pdf/2407.04099">pdf</a>, <a href="https://arxiv.org/format/2407.04099">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202450162">10.1051/0004-6361/202450162 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> SUPER VIII. Fast and Furious at $z\sim2$: obscured type-2 active nuclei host faster ionised winds than type-1 systems </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Tozzi%2C+G">G. Tozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Cresci%2C+G">G. Cresci</a>, <a href="/search/astro-ph?searchtype=author&query=Perna%2C+M">M. Perna</a>, <a href="/search/astro-ph?searchtype=author&query=Mainieri%2C+V">V. Mainieri</a>, <a href="/search/astro-ph?searchtype=author&query=Mannucci%2C+F">F. Mannucci</a>, <a href="/search/astro-ph?searchtype=author&query=Marconi%2C+A">A. Marconi</a>, <a href="/search/astro-ph?searchtype=author&query=Kakkad%2C+D">D. Kakkad</a>, <a href="/search/astro-ph?searchtype=author&query=Marasco%2C+A">A. Marasco</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Bertola%2C+E">E. Bertola</a>, <a href="/search/astro-ph?searchtype=author&query=Bischetti%2C+M">M. Bischetti</a>, <a href="/search/astro-ph?searchtype=author&query=Carniani%2C+S">S. Carniani</a>, <a href="/search/astro-ph?searchtype=author&query=Cicone%2C+C">C. Cicone</a>, <a href="/search/astro-ph?searchtype=author&query=Circosta%2C+C">C. Circosta</a>, <a href="/search/astro-ph?searchtype=author&query=Fiore%2C+F">F. Fiore</a>, <a href="/search/astro-ph?searchtype=author&query=Feruglio%2C+C">C. Feruglio</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+C+M">C. M. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Lamperti%2C+I">I. Lamperti</a>, <a href="/search/astro-ph?searchtype=author&query=Netzer%2C+H">H. Netzer</a>, <a href="/search/astro-ph?searchtype=author&query=Piconcelli%2C+E">E. Piconcelli</a>, <a href="/search/astro-ph?searchtype=author&query=Puglisi%2C+A">A. Puglisi</a>, <a href="/search/astro-ph?searchtype=author&query=Scholtz%2C+J">J. Scholtz</a>, <a href="/search/astro-ph?searchtype=author&query=Vietri%2C+G">G. Vietri</a>, <a href="/search/astro-ph?searchtype=author&query=Vignali%2C+C">C. Vignali</a>, <a href="/search/astro-ph?searchtype=author&query=Zamorani%2C+G">G. Zamorani</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.04099v1-abstract-short" style="display: inline;"> We present spatially resolved VLT/SINFONI spectroscopy with adaptive optics of type-2 active galactic nuclei (AGN) from the SINFONI Survey for Unveiling the Physics and Effect of Radiative feedback (SUPER), which targeted X-ray bright ($L_{2-10 keV}\gtrsim10^{42}$ erg s$^{-1}$) AGN at Cosmic Noon ($z\sim2$). Our analysis of the rest-frame optical spectra unveils ionised outflows in all seven exami… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.04099v1-abstract-full').style.display = 'inline'; document.getElementById('2407.04099v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.04099v1-abstract-full" style="display: none;"> We present spatially resolved VLT/SINFONI spectroscopy with adaptive optics of type-2 active galactic nuclei (AGN) from the SINFONI Survey for Unveiling the Physics and Effect of Radiative feedback (SUPER), which targeted X-ray bright ($L_{2-10 keV}\gtrsim10^{42}$ erg s$^{-1}$) AGN at Cosmic Noon ($z\sim2$). Our analysis of the rest-frame optical spectra unveils ionised outflows in all seven examined targets, as traced via [OIII]$位$5007 line emission, moving at $v\gtrsim600$ km s$^{-1}$. In six objects these outflows are clearly spatially resolved and extend on 2-4 kpc scales, whereas marginally resolved in the remaining one. Interestingly, these SUPER type-2 AGN are all heavily obscured sources ($N_{H}\gtrsim10^{23}$ cm$^{-2}$) and host faster ionised outflows than their type-1 counterparts within the same range of bolometric luminosity ($L_{bol} \sim 10^{44.8-46.5}$ erg s$^{-1}$). SUPER has hence provided observational evidence that the type-1/type-2 dichotomy at $z\sim2$ might not be driven simply by projection effects, but might reflect two distinct obscuring life stages of active galaxies, as predicted by evolutionary models. Within this picture, SUPER type-2 AGN might be undergoing the 'blow-out' phase, where the large amount of obscuring material efficiently accelerates large-scale outflows via radiation pressure on dust, eventually unveiling the central active nucleus and signal the start of the bright, unobscured type-1 AGN phase. Moreover, the overall population of ionised outflows detected in SUPER has velocities comparable with the escape speed of their dark matter halos, and in general high enough to reach 30-50 kpc distances from the centre. These outflows are hence likely to sweep away the gas (at least) out of the baryonic disk and/or to heat the host gas reservoir, thus reducing and possibly quenching star formation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.04099v1-abstract-full').style.display = 'none'; document.getElementById('2407.04099v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 13 figures. Key figure is 8. Accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 690, A141 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.12057">arXiv:2406.12057</a> <span> [<a href="https://arxiv.org/pdf/2406.12057">pdf</a>, <a href="https://arxiv.org/format/2406.12057">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202449194">10.1051/0004-6361/202449194 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The XMM-Newton and NuSTAR view of IRASF11119+3257. I Detection of multiple UFO components and a very cold corona </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lanzuisi%2C+G">G. Lanzuisi</a>, <a href="/search/astro-ph?searchtype=author&query=Matzeu%2C+G">G. Matzeu</a>, <a href="/search/astro-ph?searchtype=author&query=Baldini%2C+P">P. Baldini</a>, <a href="/search/astro-ph?searchtype=author&query=Bertola%2C+E">E. Bertola</a>, <a href="/search/astro-ph?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/astro-ph?searchtype=author&query=Tombesi%2C+F">F. Tombesi</a>, <a href="/search/astro-ph?searchtype=author&query=Luminari%2C+A">A. Luminari</a>, <a href="/search/astro-ph?searchtype=author&query=Braito%2C+V">V. Braito</a>, <a href="/search/astro-ph?searchtype=author&query=Reeves%2C+J">J. Reeves</a>, <a href="/search/astro-ph?searchtype=author&query=Chartas%2C+G">G. Chartas</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+S">S. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Cresci%2C+G">G. Cresci</a>, <a href="/search/astro-ph?searchtype=author&query=Nardini%2C+E">E. Nardini</a>, <a href="/search/astro-ph?searchtype=author&query=Piconcelli%2C+E">E. Piconcelli</a>, <a href="/search/astro-ph?searchtype=author&query=Zappacosta%2C+L">L. Zappacosta</a>, <a href="/search/astro-ph?searchtype=author&query=Serafinelli%2C+R">R. Serafinelli</a>, <a href="/search/astro-ph?searchtype=author&query=Gaspari%2C+M">M. Gaspari</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">R. Gilli</a>, <a href="/search/astro-ph?searchtype=author&query=Cappi%2C+M">M. Cappi</a>, <a href="/search/astro-ph?searchtype=author&query=Dadina%2C+M">M. Dadina</a>, <a href="/search/astro-ph?searchtype=author&query=Perna%2C+M">M. Perna</a>, <a href="/search/astro-ph?searchtype=author&query=Vignali%2C+C">C. Vignali</a>, <a href="/search/astro-ph?searchtype=author&query=Veilleux%2C+S">S. Veilleux</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.12057v1-abstract-short" style="display: inline;"> IRASF11119 is an ultra-luminous IR galaxy with post-merger morphology, hosting a type-1 QSO at z=0.189. Its 2013 Suzaku spectrum shows a prominent Ultra Fast Outflow (UFO) absorption feature (v_out~0.25c). In 2021, we obtained the first XMM-Newton long look of the target, coordinated with a simultaneous NuSTAR observation. The new high-quality data allow us to detect at P>99.8% c.l. multiple absor… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.12057v1-abstract-full').style.display = 'inline'; document.getElementById('2406.12057v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.12057v1-abstract-full" style="display: none;"> IRASF11119 is an ultra-luminous IR galaxy with post-merger morphology, hosting a type-1 QSO at z=0.189. Its 2013 Suzaku spectrum shows a prominent Ultra Fast Outflow (UFO) absorption feature (v_out~0.25c). In 2021, we obtained the first XMM-Newton long look of the target, coordinated with a simultaneous NuSTAR observation. The new high-quality data allow us to detect at P>99.8% c.l. multiple absorption features associated with the known UFO. Furthermore, an emission plus absorption feature at 1.1-1.3 keV reveals the presence of a blueshifted P-Cygni profile in the soft band. We associate the hard band features with blends of FeXXV and FeXXVI He$伪$-Ly$伪$ and He$尾$-Ly$尾$ line pairs and infer a large column (N$_H$~$10^{24}$ cm$^{-2}$) of highly ionized (log$尉$~5) gas outflowing at v_out=0.27c. The 1 keV feature can be associated with a blend of Fe and Ne transitions, produced by a lower column (N$_H$~$10^{21}$ cm$^{-2}$) and ionization (log$尉$~2.6) gas component outflowing at the same speed. Using a radiative-transfer disk wind model to fit the highly ionized UFO, we derive a large mass outflow rate, comparable with the mass accretion rate (M$_{out}$=4.25 M$_{Sun}$/yr, ~1.6 M$_{acc}$), and kinetic energy and momentum flux among the highest reported in the literature. We measure an extremely low high-energy cut-off (E$_c$~25 keV). Several other cases in the literature suggest that a steep X-ray continuum may be related to the formation of powerful winds. The lack of a significant momentum boost between the nuclear UFO and the different phases of the large-scale outflow, observed in IRASF11119 and in a growing number of sources with powerful UFOs, can be explained by (i) a momentum-driven expansion, (ii) an inefficient coupling of the UFO with the host ISM, or (iii) by repeated energy-driven expansion episodes with low duty-cycle, that average out on long time-scales. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.12057v1-abstract-full').style.display = 'none'; document.getElementById('2406.12057v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 13 figures, accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 689, A247 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.06010">arXiv:2405.06010</a> <span> [<a href="https://arxiv.org/pdf/2405.06010">pdf</a>, <a href="https://arxiv.org/format/2405.06010">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202449287">10.1051/0004-6361/202449287 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The miniJPAS Survey: The radial distribution of star formation rates in faint X-ray active galactic nuclei </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Acharya%2C+N">Nischal Acharya</a>, <a href="/search/astro-ph?searchtype=author&query=Bonoli%2C+S">Silvia Bonoli</a>, <a href="/search/astro-ph?searchtype=author&query=Salvato%2C+M">Mara Salvato</a>, <a href="/search/astro-ph?searchtype=author&query=Cortesi%2C+A">Ariana Cortesi</a>, <a href="/search/astro-ph?searchtype=author&query=Delgado%2C+M+R+G">M. Rosa Gonz谩lez Delgado</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+I+E">Ivan Ezequiel Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Marquez%2C+I">Isabel Marquez</a>, <a href="/search/astro-ph?searchtype=author&query=Mart%C3%ADnez-Solaeche%2C+G">Gin茅s Mart铆nez-Solaeche</a>, <a href="/search/astro-ph?searchtype=author&query=Abdurro%27uf"> Abdurro'uf</a>, <a href="/search/astro-ph?searchtype=author&query=Alexander%2C+D">David Alexander</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">Marcella Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Chaves-Montero%2C+J">Jon谩s Chaves-Montero</a>, <a href="/search/astro-ph?searchtype=author&query=Ontiveros%2C+J+A+F">Juan Antonio Fern谩ndez Ontiveros</a>, <a href="/search/astro-ph?searchtype=author&query=Laloux%2C+B">Brivael Laloux</a>, <a href="/search/astro-ph?searchtype=author&query=Lapi%2C+A">Andrea Lapi</a>, <a href="/search/astro-ph?searchtype=author&query=Mountrichas%2C+G">George Mountrichas</a>, <a href="/search/astro-ph?searchtype=author&query=Almeida%2C+C+R">Cristina Ramos Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Mart%C3%ADn%2C+J+E+R">Julio Esteban Rodr铆guez Mart铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Shankar%2C+F">Francesco Shankar</a>, <a href="/search/astro-ph?searchtype=author&query=Soria%2C+R">Roberto Soria</a>, <a href="/search/astro-ph?searchtype=author&query=Vilchez%2C+M+J">M. Jos茅 Vilchez</a>, <a href="/search/astro-ph?searchtype=author&query=Abramo%2C+R">Raul Abramo</a>, <a href="/search/astro-ph?searchtype=author&query=Alcaniz%2C+J">Jailson Alcaniz</a>, <a href="/search/astro-ph?searchtype=author&query=Benitez%2C+N">Narciso Benitez</a>, <a href="/search/astro-ph?searchtype=author&query=Carneiro%2C+S">Saulo Carneiro</a> , et al. (13 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.06010v3-abstract-short" style="display: inline;"> We study the impact of black hole nuclear activity on both the global and radial star formation rate (SFR) profiles in X-ray-selected active galactic nuclei (AGN) in the field of miniJPAS, the precursor of the much wider J-PAS project. Our sample includes 32 AGN with z < 0.3 detected via the XMM-Newton and Chandra surveys. For comparison, we assembled a control sample of 71 star-forming (SF) galax… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.06010v3-abstract-full').style.display = 'inline'; document.getElementById('2405.06010v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.06010v3-abstract-full" style="display: none;"> We study the impact of black hole nuclear activity on both the global and radial star formation rate (SFR) profiles in X-ray-selected active galactic nuclei (AGN) in the field of miniJPAS, the precursor of the much wider J-PAS project. Our sample includes 32 AGN with z < 0.3 detected via the XMM-Newton and Chandra surveys. For comparison, we assembled a control sample of 71 star-forming (SF) galaxies with similar magnitudes, sizes, and redshifts. To derive the global properties of both the AGN and the control SF sample, we used CIGALE to fit the spectral energy distributions derived from the 56 narrowband and 4 broadband filters from miniJPAS. We find that AGN tend to reside in more massive galaxies than their SF counterparts. After matching samples based on stellar mass and comparing their SFRs and specific SFRs (sSFRs), no significant differences appear. This suggests that the presence of AGN does not strongly influence overall star formation. However, when we used miniJPAS as an integral field unit (IFU) to dissect galaxies along their position angle, a different picture emerges. We find that AGN tend to be more centrally concentrated in mass with respect to SF galaxies. Moreover, we find a suppression of the sSFR up to 1Re and then an enhancement beyond 1Re , strongly contrasting with the decreasing radial profile of sSFRs in SF galaxies. This could point to an inside-out quenching of AGN host galaxies. These findings suggest that the reason we do not see differences on a global scale is because star formation is suppressed in the central regions and enhanced in the outer regions of AGN host galaxies. While limited in terms of sample size, this work highlights the potential of the upcoming J-PAS as a wide-field low-resolution IFU for thousands of nearby galaxies and AGN. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.06010v3-abstract-full').style.display = 'none'; document.getElementById('2405.06010v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 20 figures, Accepted for Publication in A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.00504">arXiv:2405.00504</a> <span> [<a href="https://arxiv.org/pdf/2405.00504">pdf</a>, <a href="https://arxiv.org/format/2405.00504">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> JWST meets Chandra: a large population of Compton thick, feedback-free, and X-ray weak AGN, with a sprinkle of SNe </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Maiolino%2C+R">Roberto Maiolino</a>, <a href="/search/astro-ph?searchtype=author&query=Risaliti%2C+G">Guido Risaliti</a>, <a href="/search/astro-ph?searchtype=author&query=Signorini%2C+M">Matilde Signorini</a>, <a href="/search/astro-ph?searchtype=author&query=Trefoloni%2C+B">Bartolomeo Trefoloni</a>, <a href="/search/astro-ph?searchtype=author&query=Juodzbalis%2C+I">Ignas Juodzbalis</a>, <a href="/search/astro-ph?searchtype=author&query=Scholtz%2C+J">Jan Scholtz</a>, <a href="/search/astro-ph?searchtype=author&query=Uebler%2C+H">Hannah Uebler</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Eugenio%2C+F">Francesco D'Eugenio</a>, <a href="/search/astro-ph?searchtype=author&query=Carniani%2C+S">Stefano Carniani</a>, <a href="/search/astro-ph?searchtype=author&query=Fabian%2C+A">Andy Fabian</a>, <a href="/search/astro-ph?searchtype=author&query=Ji%2C+X">Xihan Ji</a>, <a href="/search/astro-ph?searchtype=author&query=Mazzolari%2C+G">Giovanni Mazzolari</a>, <a href="/search/astro-ph?searchtype=author&query=Bertola%2C+E">Elena Bertola</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">Marcella Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Bunker%2C+A+J">Andrew J. Bunker</a>, <a href="/search/astro-ph?searchtype=author&query=Charlot%2C+S">Stephane Charlot</a>, <a href="/search/astro-ph?searchtype=author&query=Comastri%2C+A">Andrea Comastri</a>, <a href="/search/astro-ph?searchtype=author&query=Cresci%2C+G">Giovanni Cresci</a>, <a href="/search/astro-ph?searchtype=author&query=DeCoursey%2C+C+N">Christa Noel DeCoursey</a>, <a href="/search/astro-ph?searchtype=author&query=Egami%2C+E">Eiichi Egami</a>, <a href="/search/astro-ph?searchtype=author&query=Fiore%2C+F">Fabrizio Fiore</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">Roberto Gilli</a>, <a href="/search/astro-ph?searchtype=author&query=Perna%2C+M">Michele Perna</a>, <a href="/search/astro-ph?searchtype=author&query=Tacchella%2C+S">Sandro Tacchella</a>, <a href="/search/astro-ph?searchtype=author&query=Venturi%2C+G">Giacomo Venturi</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.00504v1-abstract-short" style="display: inline;"> We investigate the X-ray properties of a large sample of 71 broad line and narrow line AGN at 2<z<11 discovered by JWST in the GOODS fields, which have the deepest Chandra observations ever obtained. Despite the widespread presence of AGN signatures in their rest-optical and -UV spectra, the vast majority of them is X-ray undetected. The stacked X-ray data of the non-detected sources also results… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.00504v1-abstract-full').style.display = 'inline'; document.getElementById('2405.00504v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.00504v1-abstract-full" style="display: none;"> We investigate the X-ray properties of a large sample of 71 broad line and narrow line AGN at 2<z<11 discovered by JWST in the GOODS fields, which have the deepest Chandra observations ever obtained. Despite the widespread presence of AGN signatures in their rest-optical and -UV spectra, the vast majority of them is X-ray undetected. The stacked X-ray data of the non-detected sources also results in a non-detection. The upper limit on the X-ray emission for many of these AGN is one or even two orders of magnitude lower than expected from a standard AGN SED. Heavy X-ray absorption by clouds with large (Compton thick) column density and low dust content, such as the Broad Line Region (BLR) clouds, can explain the X-ray weakness. In this scenario the BLR covering factor should be much larger than in low-z AGN or luminous quasar; this is supported by the larger equivalent width of the broad component of Halpha in JWST-selected AGN. We also find that the JWST-discovered AGN lack the prominent, fast outflows characterizing low-z AGN and luminous quasars, suggesting that, in JWST-selected AGN, dense gas lingers in the nuclear region, resulting in large covering factors. We also note that a large fraction of JWST-selected AGN match the definition of NLSy1, typically characterized by a steep X-ray spectrum, and this can further contribute to their observed weakness at high-z. Finally, we discuss that the broad Balmer lines used to identify type 1 AGN cannot be ascribed to Very Massive Stars, Tidal Disruption Events, or Supernovae, although we show that a minority of the faintest broad lines could potentially be associated with the echo of superluminous SNe or TDE. Scenarios in which the broad lines are ascribed to galactic outflows are also untenable. We emphasize that confirming any of the scenarios discussed above will require X-ray missions more sensitive than Chandra. (abridged) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.00504v1-abstract-full').style.display = 'none'; document.getElementById('2405.00504v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 15 figures, 2 tables, submitted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.16938">arXiv:2404.16938</a> <span> [<a href="https://arxiv.org/pdf/2404.16938">pdf</a>, <a href="https://arxiv.org/format/2404.16938">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> A Cigale module tailored (not only) for Low-Luminosity AGN </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=L%C3%B3pez%2C+I+E">I. E. L贸pez</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+G">G. Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Mountrichas%2C+G">G. Mountrichas</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/astro-ph?searchtype=author&query=Baldi%2C+R+D">R. D. Baldi</a>, <a href="/search/astro-ph?searchtype=author&query=Bertola%2C+E">E. Bertola</a>, <a href="/search/astro-ph?searchtype=author&query=Bonoli%2C+S">S. Bonoli</a>, <a href="/search/astro-ph?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/astro-ph?searchtype=author&query=Shankar%2C+F">F. Shankar</a>, <a href="/search/astro-ph?searchtype=author&query=Acharya%2C+N">N. Acharya</a>, <a href="/search/astro-ph?searchtype=author&query=Tetilla%2C+A+V+A">A. V. Alonso Tetilla</a>, <a href="/search/astro-ph?searchtype=author&query=Lapi%2C+A">A. Lapi</a>, <a href="/search/astro-ph?searchtype=author&query=Laloux%2C+B">B. Laloux</a>, <a href="/search/astro-ph?searchtype=author&query=L%C3%B3pez%2C+X+L">X. L贸pez L贸pez</a>, <a href="/search/astro-ph?searchtype=author&query=Rodr%C3%ADguez%2C+I+M">I. Mu帽oz Rodr铆guez</a>, <a href="/search/astro-ph?searchtype=author&query=Musiimenta%2C+B">B. Musiimenta</a>, <a href="/search/astro-ph?searchtype=author&query=Clavijo%2C+N+O">N. Osorio Clavijo</a>, <a href="/search/astro-ph?searchtype=author&query=Sala%2C+L">L. Sala</a>, <a href="/search/astro-ph?searchtype=author&query=Sengupta%2C+D">D. Sengupta</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.16938v2-abstract-short" style="display: inline;"> The spectral energy distribution (SED) of low-luminosity active galactic nuclei (LLAGN) presents challenges due to their faint emissions and the complexity of their accretion processes. This study introduces a new CIGALE module tailored for LLAGN, combining the empirical $L_X$-$L_{12渭m}$ relationship with physical models like advection-dominated accretion flows (ADAFs) and truncated accretion disk… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.16938v2-abstract-full').style.display = 'inline'; document.getElementById('2404.16938v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.16938v2-abstract-full" style="display: none;"> The spectral energy distribution (SED) of low-luminosity active galactic nuclei (LLAGN) presents challenges due to their faint emissions and the complexity of their accretion processes. This study introduces a new CIGALE module tailored for LLAGN, combining the empirical $L_X$-$L_{12渭m}$ relationship with physical models like advection-dominated accretion flows (ADAFs) and truncated accretion disks. This module yields a refined depiction of LLAGN emissions, and a mock analysis shows reliable parameter recovery, with only minor biases. We tested the module on a sample of 50 X-ray-detected local galaxies, including LINERs and Seyferts, where it demonstrated good estimation of bolometric luminosities, even in the presence of significant galaxy contamination. Notably, the previous X-ray module failed to provide AGN solutions for this sample, stressing the need for a novel approach. Comparisons with mid-luminosity AGN confirm the module's robustness and applicability to AGN up to $L_X$ < $10^{45}$ erg/s. We also expanded the X-ray to bolometric correction formula, making it applicable to AGN spanning ten orders of magnitude in luminosity, and revealing lower $k_X$ values than typically assumed. Additionally, our analysis of the $伪_{ox}$ index, representing the slope between UV and X-ray emissions, uncovered trends that differ from those observed in high-luminosity AGN, suggesting a shift in accretion physics and photon production mechanisms in low-luminosity regimes. These results underscore the importance of a multiwavelength approach in AGN studies and reveal distinct behaviors in LLAGN compared to quasars. Our findings significantly advance the understanding of LLAGN and offer a comprehensive framework for future research aimed at completing the census of the AGN population. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.16938v2-abstract-full').style.display = 'none'; document.getElementById('2404.16938v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Acepted for publication (A&A)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.18043">arXiv:2403.18043</a> <span> [<a href="https://arxiv.org/pdf/2403.18043">pdf</a>, <a href="https://arxiv.org/format/2403.18043">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202449201">10.1051/0004-6361/202449201 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MUSE view of PDS 456: kpc-scale wind, extended ionized gas and close environment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Travascio%2C+A">A. Travascio</a>, <a href="/search/astro-ph?searchtype=author&query=Piconcelli%2C+E">E. Piconcelli</a>, <a href="/search/astro-ph?searchtype=author&query=Bischetti%2C+M">M. Bischetti</a>, <a href="/search/astro-ph?searchtype=author&query=Cresci%2C+G">G. Cresci</a>, <a href="/search/astro-ph?searchtype=author&query=Feruglio%2C+C">C. Feruglio</a>, <a href="/search/astro-ph?searchtype=author&query=Perna%2C+M">M. Perna</a>, <a href="/search/astro-ph?searchtype=author&query=Vietri%2C+G">G. Vietri</a>, <a href="/search/astro-ph?searchtype=author&query=Carniani%2C+S">S. Carniani</a>, <a href="/search/astro-ph?searchtype=author&query=Cantalupo%2C+S">S. Cantalupo</a>, <a href="/search/astro-ph?searchtype=author&query=Cicone%2C+C">C. Cicone</a>, <a href="/search/astro-ph?searchtype=author&query=Ginolfi%2C+M">M. Ginolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Venturi%2C+G">G. Venturi</a>, <a href="/search/astro-ph?searchtype=author&query=Zubovas%2C+K">K. Zubovas</a>, <a href="/search/astro-ph?searchtype=author&query=Bongiorno%2C+A">A. Bongiorno</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Luminari%2C+A">A. Luminari</a>, <a href="/search/astro-ph?searchtype=author&query=Mainieri%2C+V">V. Mainieri</a>, <a href="/search/astro-ph?searchtype=author&query=Marconi%2C+A">A. Marconi</a>, <a href="/search/astro-ph?searchtype=author&query=Menci%2C+N">N. Menci</a>, <a href="/search/astro-ph?searchtype=author&query=Nardini%2C+E">E. Nardini</a>, <a href="/search/astro-ph?searchtype=author&query=Pensabene%2C+A">A. Pensabene</a>, <a href="/search/astro-ph?searchtype=author&query=Almeida%2C+C+R">C. Ramos Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Tombesi%2C+F">F. Tombesi</a>, <a href="/search/astro-ph?searchtype=author&query=Vignali%2C+C">C. Vignali</a>, <a href="/search/astro-ph?searchtype=author&query=Zappacosta%2C+L">L. Zappacosta</a> , et al. (1 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.18043v1-abstract-short" style="display: inline;"> PDS 456 is the most luminous RQQ at z<0.3 and can be regarded as a local counterpart of the powerful QSOs shining at Cosmic Noon. It hosts a strong nuclear X-ray ultra-fast outflow, and a massive and clumpy CO(3-2) molecular outflow extending up to 5 kpc from the nucleus. We analyzed the first MUSE WFM and AO-NFM optical integral field spectroscopic observations of PDS456. The AO-NFM observations… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.18043v1-abstract-full').style.display = 'inline'; document.getElementById('2403.18043v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.18043v1-abstract-full" style="display: none;"> PDS 456 is the most luminous RQQ at z<0.3 and can be regarded as a local counterpart of the powerful QSOs shining at Cosmic Noon. It hosts a strong nuclear X-ray ultra-fast outflow, and a massive and clumpy CO(3-2) molecular outflow extending up to 5 kpc from the nucleus. We analyzed the first MUSE WFM and AO-NFM optical integral field spectroscopic observations of PDS456. The AO-NFM observations provide an unprecedented spatial resolution, reaching up to 280 pc. Our findings reveal a complex circumgalactic medium around PDS 456, extending up to a maximum projected size of ~46 kpc. This includes a reservoir of gas with a mass of ~1e7-1e8 Modot, along with eight companion galaxies, and a multi-phase outflow. WFM and NFM MUSE data reveal an outflow on a large scale (~12 kpc from the quasar) in [OIII], and on smaller scales (within 3 kpc) with higher resolution (about 280 pc) in Halpha, respectively. The [OIII] outflow mass rate is 2.3 +/- 0.2 Modot/yr which is significantly lower than those typically found in other luminous quasars. Remarkably, the Ha outflow shows a similar scale, morphology, and kinematics to the CO(3-2) molecular outflow, with the latter dominating in terms of kinetic energy and mass outflow rate by two and one orders of magnitude, respectively. Our results therefore indicate that mergers, powerful AGN activity, and feedback through AGN-driven winds will collectively contribute to shaping the host galaxy evolution of PDS 456, and likely, that of similar objects at the brightest end of the AGN luminosity function across all redshifts. Moreover, the finding that the momentum boost of the total outflow deviates from the expected energy-conserving expansion for large-scale outflows highlights the need of novel AGN-driven outflow models to comprehensively interpret these phenomena. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.18043v1-abstract-full').style.display = 'none'; document.getElementById('2403.18043v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 13 figures accepted for publication in Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 686, A250 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.09538">arXiv:2403.09538</a> <span> [<a href="https://arxiv.org/pdf/2403.09538">pdf</a>, <a href="https://arxiv.org/format/2403.09538">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202348908">10.1051/0004-6361/202348908 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Supermassive Black Hole Winds in X-rays -- SUBWAYS. III. A population study on ultra-fast outflows </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gianolli%2C+V+E">V. E. Gianolli</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+S">S. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Petrucci%2C+P">P-O Petrucci</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Chartas%2C+G">G. Chartas</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzuisi%2C+G">G. Lanzuisi</a>, <a href="/search/astro-ph?searchtype=author&query=Matzeu%2C+G+A">G. A. Matzeu</a>, <a href="/search/astro-ph?searchtype=author&query=Parra%2C+M">M. Parra</a>, <a href="/search/astro-ph?searchtype=author&query=Ursini%2C+F">F. Ursini</a>, <a href="/search/astro-ph?searchtype=author&query=Behar%2C+E">E. Behar</a>, <a href="/search/astro-ph?searchtype=author&query=Bischetti%2C+M">M. Bischetti</a>, <a href="/search/astro-ph?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/astro-ph?searchtype=author&query=Costantini%2C+E">E. Costantini</a>, <a href="/search/astro-ph?searchtype=author&query=Cresci%2C+G">G. Cresci</a>, <a href="/search/astro-ph?searchtype=author&query=Dadina%2C+M">M. Dadina</a>, <a href="/search/astro-ph?searchtype=author&query=De+Marco%2C+B">B. De Marco</a>, <a href="/search/astro-ph?searchtype=author&query=De+Rosa%2C+A">A. De Rosa</a>, <a href="/search/astro-ph?searchtype=author&query=Fiore%2C+F">F. Fiore</a>, <a href="/search/astro-ph?searchtype=author&query=Gaspari%2C+M">M. Gaspari</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">R. Gilli</a>, <a href="/search/astro-ph?searchtype=author&query=Giustini%2C+M">M. Giustini</a>, <a href="/search/astro-ph?searchtype=author&query=Guainazzi%2C+M">M. Guainazzi</a>, <a href="/search/astro-ph?searchtype=author&query=King%2C+A+R">A. R. King</a>, <a href="/search/astro-ph?searchtype=author&query=Kraemer%2C+S">S. Kraemer</a>, <a href="/search/astro-ph?searchtype=author&query=Kriss%2C+G">G. Kriss</a> , et al. (22 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.09538v2-abstract-short" style="display: inline;"> The detection of blue-shifted absorption lines likely associated with ionized Iron K-shell transitions in the X-ray spectra of many Active Galactic Nuclei (AGN) suggests the presence of a highly ionized gas outflowing with mildly relativistic velocities (0.03c-0.6c), named Ultra-Fast Outflow (UFO). Within the SUBWAYS project we characterized these winds starting from a sample of 22 radio-quiet qua… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.09538v2-abstract-full').style.display = 'inline'; document.getElementById('2403.09538v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.09538v2-abstract-full" style="display: none;"> The detection of blue-shifted absorption lines likely associated with ionized Iron K-shell transitions in the X-ray spectra of many Active Galactic Nuclei (AGN) suggests the presence of a highly ionized gas outflowing with mildly relativistic velocities (0.03c-0.6c), named Ultra-Fast Outflow (UFO). Within the SUBWAYS project we characterized these winds starting from a sample of 22 radio-quiet quasars at 0.1 < z < 0.4, and compared the results with similar studies in the literature on samples of 42 local radio-quiet Seyfert galaxies and 14 high redshift radio-quiet quasars. The scope of our work is a statistical study of UFO parameters and incidence, considering key physical properties of the sources, e.g. supermassive black hole (SMBH) mass, bolometric luminosity, accretion rates and Spectral Energy Distribution, with the aim of gaining new insights into the UFO launching mechanisms. We find indications that highly luminous AGN with steeper X-ray/UV ratio, are more likely to host UFO. The presence of UFO is not significantly related to any other AGN property in our sample. These findings suggest that the UFO phenomenon may be transient. Focusing on AGN with UFO, other important results are: (1) faster UFO have larger ionization parameters and column densities; (2) X-ray radiation plays a more crucial role in driving highly ionized winds compared to UV; (3) the correlation between outflow velocity and luminosity is significantly flatter than what expected for radiatively driven winds; (4) more massive BH experience higher wind mass-losses, suppressing accretion of matter onto the BH; (5) the UFO launching radius is positively correlated with the Eddington ratio. Furthermore, our analysis suggest the involvement of multiple launching mechanisms, including radiation pressure and magneto-hydrodynamic processes, rather than pointing to a single, universally applicable mechanism. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.09538v2-abstract-full').style.display = 'none'; document.getElementById('2403.09538v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">52 pages, 154 figures and 7 tables. Accepted in Astronomy & Astrophysics, in press</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 687, A235 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.16966">arXiv:2402.16966</a> <span> [<a href="https://arxiv.org/pdf/2402.16966">pdf</a>, <a href="https://arxiv.org/format/2402.16966">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202349071">10.1051/0004-6361/202349071 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Winds of change: the nuclear and galaxy-scale outflows and the X-ray variability of 2MASS 0918+2117 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Baldini%2C+P">P. Baldini</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzuisi%2C+G">G. Lanzuisi</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Merloni%2C+A">A. Merloni</a>, <a href="/search/astro-ph?searchtype=author&query=Gkimisi%2C+K">K. Gkimisi</a>, <a href="/search/astro-ph?searchtype=author&query=Perna%2C+M">M. Perna</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+I+E">I. E. Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Bertola%2C+E">E. Bertola</a>, <a href="/search/astro-ph?searchtype=author&query=Igo%2C+Z">Z. Igo</a>, <a href="/search/astro-ph?searchtype=author&query=Waddell%2C+S">S. Waddell</a>, <a href="/search/astro-ph?searchtype=author&query=Musiimenta%2C+B">B. Musiimenta</a>, <a href="/search/astro-ph?searchtype=author&query=Aydar%2C+C">C. Aydar</a>, <a href="/search/astro-ph?searchtype=author&query=Arcodia%2C+R">R. Arcodia</a>, <a href="/search/astro-ph?searchtype=author&query=Matzeu%2C+G+A">G. A. Matzeu</a>, <a href="/search/astro-ph?searchtype=author&query=Luminari%2C+A">A. Luminari</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+J">J. Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Vignali%2C+C">C. Vignali</a>, <a href="/search/astro-ph?searchtype=author&query=Dadina%2C+M">M. Dadina</a>, <a href="/search/astro-ph?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/astro-ph?searchtype=author&query=Cresci%2C+G">G. Cresci</a>, <a href="/search/astro-ph?searchtype=author&query=Marchesi%2C+S">S. Marchesi</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">R. Gilli</a>, <a href="/search/astro-ph?searchtype=author&query=Tombesi%2C+F">F. Tombesi</a>, <a href="/search/astro-ph?searchtype=author&query=Serafinelli%2C+R">R. Serafinelli</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2402.16966v1-abstract-short" style="display: inline;"> Powerful outflows from active galactic nuclei (AGN) can significantly impact the gas reservoirs of their host galaxies. However, it is still unclear how these outflows can propagate from the very central regions of galaxies to their outskirts, and whether nuclear winds can be driven by and/or be responsible for drastic spectral transitions. In this work we test feedback propagation models on the c… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.16966v1-abstract-full').style.display = 'inline'; document.getElementById('2402.16966v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.16966v1-abstract-full" style="display: none;"> Powerful outflows from active galactic nuclei (AGN) can significantly impact the gas reservoirs of their host galaxies. However, it is still unclear how these outflows can propagate from the very central regions of galaxies to their outskirts, and whether nuclear winds can be driven by and/or be responsible for drastic spectral transitions. In this work we test feedback propagation models on the case test of 2MASS 0918+2117 (2M0918), a z=0.149 X-ray variable AGN, which showed tentative evidence for nuclear ultra-fast outflows (UFOs) in a 2005 XMM-Newton observation. We also investigate whether UFOs can be related to the observed X-ray variability. We observed 2M0918 with XMM-Newton and NuSTAR in 2020 to confirm the presence and characterize the UFOs. We perform a kinematic analysis of the 2005 SDSS optical spectrum to reveal and measure the properties of galaxy-scale ionized outflows. Furthermore, we construct 20-year-long lightcurves of observed flux, line-of-sight column density, and intrinsic accretion rate from the spectra of the first 4 SRG/eROSITA all-sky surveys and archival observations from Chandra and XMM-Newton.We significantly detect UFOs with v$\sim$0.16c and galaxy-scale ionized outflows with velocities of $\sim$ 700 km/s. We also find that the drastic X-ray variability (factors >10) can be explained both in terms of variable obscuration and variable intrinsic luminosity.Comparing the energetics of the two outflow phases, 2M0918 is consistent with momentum-driven wind propagation. 2M0918 expands the sample of AGN with both UFOs and ionized gas winds from 5 to 6, and brings the sample of AGN hosting multiscale outflows to 19, contributing to a clearer picture of feedback physics. From the variations in accretion rate, column density, and ionization level of the obscurer, we propose a scenario that connects obscurers, an accretion enhancement, and the emergence of UFOs <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.16966v1-abstract-full').style.display = 'none'; document.getElementById('2402.16966v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 18 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 686, A217 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.00109">arXiv:2402.00109</a> <span> [<a href="https://arxiv.org/pdf/2402.00109">pdf</a>, <a href="https://arxiv.org/format/2402.00109">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202348072">10.1051/0004-6361/202348072 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Heavily Obscured AGN detection: a Radio vs X-ray challenge </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mazzolari%2C+G">Giovanni Mazzolari</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">Roberto Gilli</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">Marcella Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Mignoli%2C+M">Marco Mignoli</a>, <a href="/search/astro-ph?searchtype=author&query=Vito%2C+F">Fabio Vito</a>, <a href="/search/astro-ph?searchtype=author&query=Prandoni%2C+I">Isabella Prandoni</a>, <a href="/search/astro-ph?searchtype=author&query=Marchesi%2C+S">Stefano Marchesi</a>, <a href="/search/astro-ph?searchtype=author&query=Chiaberge%2C+M">Marco Chiaberge</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzuisi%2C+G">Giorgio Lanzuisi</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Amato%2C+Q">Quirino D'Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Comastri%2C+A">Andrea Comastri</a>, <a href="/search/astro-ph?searchtype=author&query=Vignali%2C+C">Cristian Vignali</a>, <a href="/search/astro-ph?searchtype=author&query=Iwasawa%2C+K">Kazushi Iwasawa</a>, <a href="/search/astro-ph?searchtype=author&query=Norman%2C+C">Colin Norman</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2402.00109v1-abstract-short" style="display: inline;"> In this work, we study the AGN radio detection effectiveness in the major deep extragalactic surveys, considering different AGN obscuration levels, redshift, and AGN bolometric luminosities. We particularly focus on comparing their radio and X-ray detectability, making predictions for present and future radio surveys. We extrapolate the predictions of AGN population synthesis model of cosmic X-ray… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.00109v1-abstract-full').style.display = 'inline'; document.getElementById('2402.00109v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.00109v1-abstract-full" style="display: none;"> In this work, we study the AGN radio detection effectiveness in the major deep extragalactic surveys, considering different AGN obscuration levels, redshift, and AGN bolometric luminosities. We particularly focus on comparing their radio and X-ray detectability, making predictions for present and future radio surveys. We extrapolate the predictions of AGN population synthesis model of cosmic X-ray background (CXB) to the radio band, by deriving the 1.4 GHz luminosity functions of unobscured (i.e. with hydrogen column densities $\log N_{H} <22$), obscured ($22<\log N_{H}<24$) and Compton-thick (CTK, $\log N_{H} >24$) AGN. We then use these functions to forecast the number of detectable AGN based on the area, flux limit, and completeness of a given radio survey and compare it with the AGN number resulting from X-ray predictions. When applied to deep extragalactic fields covered both by radio and X-ray observations, we show that, while X-ray selection is generally more effective in detecting unobscured AGN, the surface density of CTK AGN radio detected is on average $\sim 10$ times larger than the X-ray one, and even greater at high redshifts, considering the current surveys and facilities. Our results suggest that thousands of CTK AGN are already present in current radio catalogs, but most of them escaped any detection in the corresponding X-ray observations. We also present expectations for the number of AGN to be detected by the Square Kilometer Array Observatory (SKAO) in its future deep and wide radio continuum surveys, finding that it will be able to detect more than 2000 AGN at $z>6$ and some tens at $z>10$, more than half of which are expected to be CTK. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.00109v1-abstract-full').style.display = 'none'; document.getElementById('2402.00109v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 11 figures, accepted for publication on A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 687, A120 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.17306">arXiv:2401.17306</a> <span> [<a href="https://arxiv.org/pdf/2401.17306">pdf</a>, <a href="https://arxiv.org/format/2401.17306">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> The SRG/eROSITA all-sky survey: Hard X-ray selected Active Galactic Nuclei </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Waddell%2C+S+G+H">Sophia G. H. Waddell</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+J">J. Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Nandra%2C+K">K. Nandra</a>, <a href="/search/astro-ph?searchtype=author&query=Salvato%2C+M">M. Salvato</a>, <a href="/search/astro-ph?searchtype=author&query=Merloni%2C+A">A. Merloni</a>, <a href="/search/astro-ph?searchtype=author&query=Gauger%2C+I">I. Gauger</a>, <a href="/search/astro-ph?searchtype=author&query=Boller%2C+T">Th. Boller</a>, <a href="/search/astro-ph?searchtype=author&query=Seppi%2C+R">R. Seppi</a>, <a href="/search/astro-ph?searchtype=author&query=Wolf%2C+J">J. Wolf</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+T">T. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Comparat%2C+J">J. Comparat</a>, <a href="/search/astro-ph?searchtype=author&query=Dwelly%2C+T">T. Dwelly</a>, <a href="/search/astro-ph?searchtype=author&query=Igo%2C+Z">Z. Igo</a>, <a href="/search/astro-ph?searchtype=author&query=Musiimenta%2C+B">B. Musiimenta</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.17306v1-abstract-short" style="display: inline;"> The eROSITA instrument aboard the Spectrum Roentgen Gamma (SRG) satellite has performed its first all-sky survey between December 2019 and June 2020. This paper presents the resulting hard X-ray (2.3-5 keV) sample, the first created from an all-sky imaging survey in the 2-8 keV band, for sources within western galactic sky. The 5466 hard X-ray selected sources detected with eROSITA are presented a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.17306v1-abstract-full').style.display = 'inline'; document.getElementById('2401.17306v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.17306v1-abstract-full" style="display: none;"> The eROSITA instrument aboard the Spectrum Roentgen Gamma (SRG) satellite has performed its first all-sky survey between December 2019 and June 2020. This paper presents the resulting hard X-ray (2.3-5 keV) sample, the first created from an all-sky imaging survey in the 2-8 keV band, for sources within western galactic sky. The 5466 hard X-ray selected sources detected with eROSITA are presented and discussed. The Bayesian statistics-based code NWAY is used to identify the counterparts for the X-ray sources. These sources are classified based on their multiwavelength properties, and the literature is searched to identify spectroscopic redshifts, which further inform the source classification. A total of 2547 sources are found to have good-quality counterparts, and 111 of these are detected only in the hard band. Comparing with other hard X-ray selected surveys, the eROSITA hard sample covers a larger redshift range and probes dimmer sources, providing a complementary and expanded sample as compared to Swift-BAT. Examining the column density distribution of missed and detected eROSITA sources present in the follow-up catalog of Swift BAT 70 month sources, it is demonstrated that eROSITA can detect obscured sources with column densities $>10^{24}$ cm$^{-2}$, but that the completeness drops rapidly after $10^{23}$ cm$^{-2}$. A sample of hard-only sources, many of which are likely to be heavily obscured AGN, is also presented and discussed. X-ray spectral fitting reveals that these sources have extremely faint soft X-ray emission and their optical images suggest that they are found in more edge-on galaxies with lower b/a. The resulting X-ray catalog is demonstrated to be a powerful tool for understanding AGN, in particular heavily obscured AGN found in the hard-only sample. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.17306v1-abstract-full').style.display = 'none'; document.getElementById('2401.17306v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 21 figures. Submitted to A&A. Associated with eROSITA data release. Associated catalogs will be released after journal publication</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.17300">arXiv:2401.17300</a> <span> [<a href="https://arxiv.org/pdf/2401.17300">pdf</a>, <a href="https://arxiv.org/format/2401.17300">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The eROSITA Final Equatorial Depth Survey (eFEDS): the hard X-ray selected sample </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Nandra%2C+K">K. Nandra</a>, <a href="/search/astro-ph?searchtype=author&query=Waddell%2C+S+G+H">S. G. H. Waddell</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+T">T. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+J">J. Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Dwelly%2C+T">T. Dwelly</a>, <a href="/search/astro-ph?searchtype=author&query=Salvato%2C+M">M. Salvato</a>, <a href="/search/astro-ph?searchtype=author&query=Shen%2C+Y">Y. Shen</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+Q">Q. Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Arcodia%2C+R">R. Arcodia</a>, <a href="/search/astro-ph?searchtype=author&query=Boller%2C+T">Th. Boller</a>, <a href="/search/astro-ph?searchtype=author&query=Brunner%2C+H">H. Brunner</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Collmar%2C+W">W. Collmar</a>, <a href="/search/astro-ph?searchtype=author&query=Comparat%2C+J">J. Comparat</a>, <a href="/search/astro-ph?searchtype=author&query=Georgakakis%2C+A">A. Georgakakis</a>, <a href="/search/astro-ph?searchtype=author&query=Grau%2C+M">M. Grau</a>, <a href="/search/astro-ph?searchtype=author&query=H%C3%A4mmerich%2C+S">S. H盲mmerich</a>, <a href="/search/astro-ph?searchtype=author&query=Ibarra-Medel%2C+H">H. Ibarra-Medel</a>, <a href="/search/astro-ph?searchtype=author&query=Igo%2C+Z">Z. Igo</a>, <a href="/search/astro-ph?searchtype=author&query=Krumpe%2C+M">M. Krumpe</a>, <a href="/search/astro-ph?searchtype=author&query=Lamer%2C+G">G. Lamer</a>, <a href="/search/astro-ph?searchtype=author&query=Merloni%2C+A">A. Merloni</a>, <a href="/search/astro-ph?searchtype=author&query=Musiimenta%2C+B">B. Musiimenta</a>, <a href="/search/astro-ph?searchtype=author&query=Wolf%2C+J">J. Wolf</a>, <a href="/search/astro-ph?searchtype=author&query=Assef%2C+R+J">R. J. Assef</a> , et al. (3 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.17300v1-abstract-short" style="display: inline;"> During its calibration and performance verification phase, the eROSITA instrument aboard the SRG satellite performed a uniform wide--area X-ray survey of approximately 140 deg$^{2}$ in a region of the sky known as the eROSITA Final Equatorial Depth Survey (eFEDS). The primary aim of eFEDS is to demonstrate the scientific performance to be expected at the end of the 8-pass eROSITA all sky survey. T… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.17300v1-abstract-full').style.display = 'inline'; document.getElementById('2401.17300v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.17300v1-abstract-full" style="display: none;"> During its calibration and performance verification phase, the eROSITA instrument aboard the SRG satellite performed a uniform wide--area X-ray survey of approximately 140 deg$^{2}$ in a region of the sky known as the eROSITA Final Equatorial Depth Survey (eFEDS). The primary aim of eFEDS is to demonstrate the scientific performance to be expected at the end of the 8-pass eROSITA all sky survey. This will provide the first focussed image of the whole sky in the hard X-ray ($>2$~keV) bandpass. The expected source population in this energy range is thus of great interest, particularly for AGN studies. We use the 2.3--5 keV selection presented by Brunner et al. (2022) to construct a sample of 246 point-like hard X-ray sources for further study and characterization. These are classified as either extragalactic ($\sim 90$~\%) or Galactic ($\sim 10$~\%), with the former consisting overwhelmingly of AGN and the latter active stars. We concentrate our further analysis on the extragalactic/AGN sample, describing their X-ray and multiwavelength properties and comparing them to the eFEDS main AGN sample selected in the softer 0.2-2.3 keV band. The eROSITA hard band selects a subsample of sources that is a factor $>10$ brighter than the eFEDS main sample. The AGN within the hard population reach up to $z=3.2$ but on the whole are relatively nearby, with median $z$=0.34 compared to $z$=0.94 for the main sample. The hard survey probes typical luminosities in the range $\log L_{\rm X} = 43-46$. X-ray spectral analysis shows significant intrinsic absorption (with $\log N_{\rm H}>21$) in $\sim 20$~\% of the sources, with a hard X-ray power law continuum with mean $<螕>=1.83\pm0.04$, typical of AGN, but slightly harder than the soft-selected eROSITA sample. (abridged) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.17300v1-abstract-full').style.display = 'none'; document.getElementById('2401.17300v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to A&A as part of eROSITA Data Release 1</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.17299">arXiv:2401.17299</a> <span> [<a href="https://arxiv.org/pdf/2401.17299">pdf</a>, <a href="https://arxiv.org/format/2401.17299">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202449283">10.1051/0004-6361/202449283 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Ionised AGN outflows in the Goldfish galaxy -- The illuminating and interacting red quasar eFEDSJ091157.4+014327 at z $\sim$ 0.6 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Musiimenta%2C+B">Blessing Musiimenta</a>, <a href="/search/astro-ph?searchtype=author&query=Speranza%2C+G">Giovanna Speranza</a>, <a href="/search/astro-ph?searchtype=author&query=Urrutia%2C+T">Tanya Urrutia</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">Marcella Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Almeida%2C+C+R">Cristina Ramos Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Perna%2C+M">Michele Perna</a>, <a href="/search/astro-ph?searchtype=author&query=L%C3%B3pez%2C+I+E">Iv脿n Ezequiel L贸pez</a>, <a href="/search/astro-ph?searchtype=author&query=Alexander%2C+D+M">David M. Alexander</a>, <a href="/search/astro-ph?searchtype=author&query=Laloux%2C+B">Brivael Laloux</a>, <a href="/search/astro-ph?searchtype=author&query=Shankar%2C+F">Francesco Shankar</a>, <a href="/search/astro-ph?searchtype=author&query=Lapi%2C+A">Andrea Lapi</a>, <a href="/search/astro-ph?searchtype=author&query=Salvato%2C+M">Mara Salvato</a>, <a href="/search/astro-ph?searchtype=author&query=Toba%2C+Y">Yoshiki Toba</a>, <a href="/search/astro-ph?searchtype=author&query=Andonie%2C+C">Carolina Andonie</a>, <a href="/search/astro-ph?searchtype=author&query=Rodr%C3%ADguez%2C+I+M">Iv脿n Munoz Rodr铆guez</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.17299v2-abstract-short" style="display: inline;"> Evolutionary models suggest that the initial growth phases of active galactic nuclei (AGN) are dust-enshrouded, and characterised by jet/wind outflows that should gradually clear the interstellar medium (ISM) in the host by heating and/or expelling the surrounding gas. eFEDSJ091157.4$+$014327 (z$\sim$0.6) was selected from X-ray samples for its characteristics that are similar to sources with outf… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.17299v2-abstract-full').style.display = 'inline'; document.getElementById('2401.17299v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.17299v2-abstract-full" style="display: none;"> Evolutionary models suggest that the initial growth phases of active galactic nuclei (AGN) are dust-enshrouded, and characterised by jet/wind outflows that should gradually clear the interstellar medium (ISM) in the host by heating and/or expelling the surrounding gas. eFEDSJ091157.4$+$014327 (z$\sim$0.6) was selected from X-ray samples for its characteristics that are similar to sources with outflows which include red, obscured and X-ray luminous. We aim to explore the environment around this red quasar and characterise kinematics within the system. We used spatially resolved spectroscopic data from Multi Unit Spectroscopic Explorer (MUSE) with an average seeing of 0.6" to construct flux, velocity and velocity dispersions maps. We found that the quasar is embedded in an interacting and merging system with three other galaxies $\sim$ 50 kpc from its nucleus. Spatially resolved kinematics reveal that the quasar has extended ionised outflows of up to 9.2 kpc with positive and negative velocities up to 1000 km s$^{-1}$ and -1200 km s$^{-1}$, respectively. The velocity dispersion (W$_{80}$) ranges from 600-1800 km s$^{-1}$. We associate the presence of turbulent and high-velocity components with the outflow. The total mass outflow rate is estimated to be $\sim$ 10 M$_{\odot}$ yr$^{-1}$ and kinetic power of 2x10$^{42}$ erg s$^{-1}$. The kinetic coupling efficiencies range from 0.01%-0.03% and the momentum boosts are $\sim$ 0.2. These low values indicate that the ionised outflow is not energetically relevant. These values don't align with the theoretical predictions of both radiation-pressure-driven outflows and energy-conserving mechanisms. However, note that our results are based only on the ionised phase while theoretical predictions are multiphase. Moreover, the mass loading factor of $\sim$ 5 is an indication that these outflows are more likely AGN-driven than star formation-driven. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.17299v2-abstract-full').style.display = 'none'; document.getElementById('2401.17299v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Version after addressing referee comments, accepted in Astronomy and Astrophysics(A&A), 17 pages, 12 figures, 1 table</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 687, A111 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.17274">arXiv:2401.17274</a> <span> [<a href="https://arxiv.org/pdf/2401.17274">pdf</a>, <a href="https://arxiv.org/format/2401.17274">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202347165">10.1051/0004-6361/202347165 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The SRG/eROSITA all-sky survey: First X-ray catalogues and data release of the western Galactic hemisphere </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Merloni%2C+A">A. Merloni</a>, <a href="/search/astro-ph?searchtype=author&query=Lamer%2C+G">G. Lamer</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+T">T. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Ramos-Ceja%2C+M+E">M. E. Ramos-Ceja</a>, <a href="/search/astro-ph?searchtype=author&query=Brunner%2C+H">H. Brunner</a>, <a href="/search/astro-ph?searchtype=author&query=Bulbul%2C+E">E. Bulbul</a>, <a href="/search/astro-ph?searchtype=author&query=Dennerl%2C+K">K. Dennerl</a>, <a href="/search/astro-ph?searchtype=author&query=Doroshenko%2C+V">V. Doroshenko</a>, <a href="/search/astro-ph?searchtype=author&query=Freyberg%2C+M+J">M. J. Freyberg</a>, <a href="/search/astro-ph?searchtype=author&query=Friedrich%2C+S">S. Friedrich</a>, <a href="/search/astro-ph?searchtype=author&query=Gatuzz%2C+E">E. Gatuzz</a>, <a href="/search/astro-ph?searchtype=author&query=Georgakakis%2C+A">A. Georgakakis</a>, <a href="/search/astro-ph?searchtype=author&query=Haberl%2C+F">F. Haberl</a>, <a href="/search/astro-ph?searchtype=author&query=Igo%2C+Z">Z. Igo</a>, <a href="/search/astro-ph?searchtype=author&query=Kreykenbohm%2C+I">I. Kreykenbohm</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+A">A. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Maitra%2C+C">C. Maitra</a>, <a href="/search/astro-ph?searchtype=author&query=Malyali%2C+A">A. Malyali</a>, <a href="/search/astro-ph?searchtype=author&query=Mayer%2C+M+G+F">M. G. F. Mayer</a>, <a href="/search/astro-ph?searchtype=author&query=Nandra%2C+K">K. Nandra</a>, <a href="/search/astro-ph?searchtype=author&query=Predehl%2C+P">P. Predehl</a>, <a href="/search/astro-ph?searchtype=author&query=Robrade%2C+J">J. Robrade</a>, <a href="/search/astro-ph?searchtype=author&query=Salvato%2C+M">M. Salvato</a>, <a href="/search/astro-ph?searchtype=author&query=Sanders%2C+J+S">J. S. Sanders</a>, <a href="/search/astro-ph?searchtype=author&query=Stewart%2C+I">I. Stewart</a> , et al. (120 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.17274v1-abstract-short" style="display: inline;"> The eROSITA telescope array aboard the Spektrum Roentgen Gamma (SRG) satellite began surveying the sky in December 2019, with the aim of producing all-sky X-ray source lists and sky maps of an unprecedented depth. Here we present catalogues of both point-like and extended sources using the data acquired in the first six months of survey operations (eRASS1; completed June 2020) over the half sky wh… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.17274v1-abstract-full').style.display = 'inline'; document.getElementById('2401.17274v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.17274v1-abstract-full" style="display: none;"> The eROSITA telescope array aboard the Spektrum Roentgen Gamma (SRG) satellite began surveying the sky in December 2019, with the aim of producing all-sky X-ray source lists and sky maps of an unprecedented depth. Here we present catalogues of both point-like and extended sources using the data acquired in the first six months of survey operations (eRASS1; completed June 2020) over the half sky whose proprietary data rights lie with the German eROSITA Consortium. We describe the observation process, the data analysis pipelines, and the characteristics of the X-ray sources. With nearly 930000 entries detected in the most sensitive 0.2-2.3 keV energy range, the eRASS1 main catalogue presented here increases the number of known X-ray sources in the published literature by more than 60%, and provides a comprehensive inventory of all classes of X-ray celestial objects, covering a wide range of physical processes. A smaller catalogue of 5466 sources detected in the less sensitive but harder 2.3-5 keV band is the result of the first true imaging survey of the entire sky above 2 keV. We show that the number counts of X-ray sources in eRASS1 are consistent with those derived over narrower fields by past X-ray surveys of a similar depth, and we explore the number counts variation as a function of the location in the sky. Adopting a uniform all-sky flux limit (at 50% completeness) of F_{0.5-2 keV} > 5 \times 10^{-14}$ erg\,s$^{-1}$\,cm$^{-2}$, we estimate that the eROSITA all-sky survey resolves into individual sources about 20% of the cosmic X-ray background in the 1-2 keV range. The catalogues presented here form part of the first data release (DR1) of the SRG/eROSITA all-sky survey. Beyond the X-ray catalogues, DR1 contains all detected and calibrated event files, source products (light curves and spectra), and all-sky maps. Illustrative examples of these are provided. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.17274v1-abstract-full').style.display = 'none'; document.getElementById('2401.17274v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">39 pages, 23 figures. Accepted for publication in A&A. Accompanying eROSITA-DE Data Release 1</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A, vol. 682, A34 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.10132">arXiv:2311.10132</a> <span> [<a href="https://arxiv.org/pdf/2311.10132">pdf</a>, <a href="https://arxiv.org/format/2311.10132">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Multi-phase characterization of AGN winds in 5 local type-2 quasars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Speranza%2C+G">G. Speranza</a>, <a href="/search/astro-ph?searchtype=author&query=Almeida%2C+C+R">C. Ramos Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Acosta-Pulido%2C+J+A">J. A. Acosta-Pulido</a>, <a href="/search/astro-ph?searchtype=author&query=Audibert%2C+A">A. Audibert</a>, <a href="/search/astro-ph?searchtype=author&query=Holden%2C+L+R">L. R. Holden</a>, <a href="/search/astro-ph?searchtype=author&query=Tadhunter%2C+C+N">C. N. Tadhunter</a>, <a href="/search/astro-ph?searchtype=author&query=Lapi%2C+A">A. Lapi</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez-Mart%C3%ADn%2C+O">O. Gonz谩lez-Mart铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=L%C3%B3pez%2C+I+E">I. E. L贸pez</a>, <a href="/search/astro-ph?searchtype=author&query=Musiimenta%2C+B">B. Musiimenta</a>, <a href="/search/astro-ph?searchtype=author&query=Shankar%2C+F">F. Shankar</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.10132v1-abstract-short" style="display: inline;"> We present MEGARA (Multi-Espectr贸grafo en GTC de Alta Resoluci贸n para Astronom铆a) Integral Field Unit (IFU) observations of 5 local type-2 quasars (QSO2s, z $\sim 0.1$) from the Quasar Feedback (QSOFEED) sample. These active galactic nuclei (AGN) have bolometric luminosities of 10$^{45.5-46}$ erg/s and stellar masses of $\sim$10$^{11}$ M$_{\odot}$. We explore the kinematics of the ionized gas thro… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.10132v1-abstract-full').style.display = 'inline'; document.getElementById('2311.10132v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.10132v1-abstract-full" style="display: none;"> We present MEGARA (Multi-Espectr贸grafo en GTC de Alta Resoluci贸n para Astronom铆a) Integral Field Unit (IFU) observations of 5 local type-2 quasars (QSO2s, z $\sim 0.1$) from the Quasar Feedback (QSOFEED) sample. These active galactic nuclei (AGN) have bolometric luminosities of 10$^{45.5-46}$ erg/s and stellar masses of $\sim$10$^{11}$ M$_{\odot}$. We explore the kinematics of the ionized gas through the [O~III]$位$5007 $脜$ emission line. The nuclear spectra of the 5 QSO2s, extracted in a circular aperture of $\sim$ 1.2" ($\sim$ 2.2 kpc) in diameter, show signatures of high velocity winds in the form of broad (full width at half maximum; 1300$\leq$FWHM$\leq$2240 km/s and blueshifted components. We find that 4 out of the 5 QSO2s present outflows that we can resolve with our seeing-limited data, and they have radii ranging from 3.1 to 12.6 kpc. In the case of the two QSO2s with extended radio emission, we find that it is well-aligned with the outflows, suggesting that low-power jets might be compressing and accelerating the ionized gas in these radio-quiet QSO2s. In the four QSO2s with spatially resolved outflows, we measure ionized mass outflow rates of 3.3-6.5 Msun/yr when we use [S~II]-based densities, and of 0.7-1.6 Msun/yr when trans-auroral line-based densities are considered instead. We compare them with the corresponding molecular mass outflow rates (8 - 16 Msun/yr), derived from CO(2-1) ALMA observations at 0.2" resolution. Both phases show lower outflow mass rates than those expected from observational scaling relations where uniform assumptions on the outflow properties were adopted. This might be indicating that the AGN luminosity is not the only driver of massive outflows and/or that these relations need to be re-scaled using accurate outflow properties. We do not find a significant impact of the outflows on the global star formation rates. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.10132v1-abstract-full').style.display = 'none'; document.getElementById('2311.10132v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, 13 figures and 4 tables. Accepted for publication in A&A; A&A 665, A55 (2023); doi: 10.1051/0004-6361/202347715</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.16528">arXiv:2309.16528</a> <span> [<a href="https://arxiv.org/pdf/2309.16528">pdf</a>, <a href="https://arxiv.org/format/2309.16528">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202245555">10.1051/0004-6361/202245555 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A new discovery space opened by eROSITA: Ionised AGN outflows from X-ray selected samples </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Musiimenta%2C+B">Blessing Musiimenta</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">Marcella Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+T">Teng Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Salvato%2C+M">Mara Salvato</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+J">Johannes Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Igo%2C+Z">Zsofi Igo</a>, <a href="/search/astro-ph?searchtype=author&query=Waddell%2C+S+G+H">Sophia G. H. Waddell</a>, <a href="/search/astro-ph?searchtype=author&query=Toba%2C+Y">Yoshiki Toba</a>, <a href="/search/astro-ph?searchtype=author&query=Arcodia%2C+R">Riccardo Arcodia</a>, <a href="/search/astro-ph?searchtype=author&query=Comparat%2C+J">Johan Comparat</a>, <a href="/search/astro-ph?searchtype=author&query=Alexander%2C+D+M">David M. Alexander</a>, <a href="/search/astro-ph?searchtype=author&query=Shankar%2C+F">Francesco Shankar</a>, <a href="/search/astro-ph?searchtype=author&query=Lapi%2C+A">Andrea Lapi</a>, <a href="/search/astro-ph?searchtype=author&query=Almeida%2C+C+R">Cristina Ramos Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Georgakakis%2C+A">Antonis Georgakakis</a>, <a href="/search/astro-ph?searchtype=author&query=Merloni%2C+A">Andrea Merloni</a>, <a href="/search/astro-ph?searchtype=author&query=Urrutia%2C+T">Tanya Urrutia</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+J">Junyao Li</a>, <a href="/search/astro-ph?searchtype=author&query=Terashima%2C+Y">Yuichi Terashima</a>, <a href="/search/astro-ph?searchtype=author&query=Shen%2C+Y">Yue Shen</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+Q">Qiaoya Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Dwelly%2C+T">Tom Dwelly</a>, <a href="/search/astro-ph?searchtype=author&query=Nandra%2C+K">Kirpal Nandra</a>, <a href="/search/astro-ph?searchtype=author&query=Wolf%2C+J">Julien Wolf</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2309.16528v1-abstract-short" style="display: inline;"> In the context of an evolutionary model, the outflow phase of an Active Galactic Nuclei (AGN) occurs at the peak of its activity, once the central SMBH is massive enough to generate sufficient power to counterbalance the potential well of the host galaxy. This phase plays a vital role in galaxy evolution. We aim to apply various selection methods to isolate powerful AGNs in the feedback phase, tra… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.16528v1-abstract-full').style.display = 'inline'; document.getElementById('2309.16528v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.16528v1-abstract-full" style="display: none;"> In the context of an evolutionary model, the outflow phase of an Active Galactic Nuclei (AGN) occurs at the peak of its activity, once the central SMBH is massive enough to generate sufficient power to counterbalance the potential well of the host galaxy. This phase plays a vital role in galaxy evolution. We aim to apply various selection methods to isolate powerful AGNs in the feedback phase, trace and characterise their outflows, and explore the link between AGN luminosity and outflow properties. We applied a combination of methods to the eROSITA Final Equatorial Depth survey (eFEDS) catalogue and isolated ~1400 candidates at z>0.5 out of ~11750 AGNs (~12\%). We tested the robustness of our selection on the small subsample of 50 sources with available good quality SDSS spectra at 0.5<z<1, for which we fitted the [OIII] emission line complex and searched for the presence of ionised gas outflows. We identified 23 quasars (~45\%) with evidence of ionised outflows based on the presence of significant broad and shifted components in the [OIII] line. They are on average more luminous and more obscured than the parent sample, although this may be ascribed to selection effects affecting the good quality SDSS spectra sample. By adding 118 outflowing quasars at 0.5<z<3.5 from the literature, we find a weak correlation between the maximum outflow velocity and AGN bolometric luminosity. On the contrary, we find strong correlations between mass outflow rate and outflow kinetic power with the AGN bolometric luminosity. About 30\% of our sample have kinetic coupling efficiencies >1\%. We find that the majority of the outflows have momentum flux ratios lower than 20 which rules out an energy-conserving nature. Our present work points to the unequivocal existence of a rather short AGN outflow phase, paving the way towards a new avenue to dissect AGN outflows in large samples within eROSITA and beyond. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.16528v1-abstract-full').style.display = 'none'; document.getElementById('2309.16528v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astronomy and Astrophysics(A&A), 24 pages, 18 figures, 5 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 679, A84 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.00961">arXiv:2306.00961</a> <span> [<a href="https://arxiv.org/pdf/2306.00961">pdf</a>, <a href="https://arxiv.org/format/2306.00961">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202245572">10.1051/0004-6361/202245572 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The eROSITA Final Equatorial Depth Survey (eFEDS): Complex absorption and soft excesses in hard X-ray--selected active galactic nuclei </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Waddell%2C+S+G+H">Sophia G. H. Waddell</a>, <a href="/search/astro-ph?searchtype=author&query=Nandra%2C+K">Kirpal Nandra</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+J">Johannes Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+Q">Qiaoya Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Shen%2C+Y">Yue Shen</a>, <a href="/search/astro-ph?searchtype=author&query=Arcodia%2C+R">Riccardo Arcodia</a>, <a href="/search/astro-ph?searchtype=author&query=Merloni%2C+A">Andrea Merloni</a>, <a href="/search/astro-ph?searchtype=author&query=Salvato%2C+M">Mara Salvato</a>, <a href="/search/astro-ph?searchtype=author&query=Dauser%2C+T">Thomas Dauser</a>, <a href="/search/astro-ph?searchtype=author&query=Boller%2C+T">Thomas Boller</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+T">Teng Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Comparat%2C+J">Johan Comparat</a>, <a href="/search/astro-ph?searchtype=author&query=Wolf%2C+J">Julien Wolf</a>, <a href="/search/astro-ph?searchtype=author&query=Dwelly%2C+T">Tom Dwelly</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Brownstein%2C+J+R">Joel R. Brownstein</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">Marcella Brusa</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.00961v1-abstract-short" style="display: inline;"> Context. The soft excess, a surplus of X-ray photons above 2 keV with respect to a power law, is a feature of debated physical origin found in the X-ray spectra of many type-1 active galactic nuclei (AGN). The eROSITA instrument aboard the Spectrum-Roentgen-Gamma (SRG) mission will provide an all-sky census of AGN suitable for spectral analysis. Aims. The primary goal of this work is to test a var… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.00961v1-abstract-full').style.display = 'inline'; document.getElementById('2306.00961v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.00961v1-abstract-full" style="display: none;"> Context. The soft excess, a surplus of X-ray photons above 2 keV with respect to a power law, is a feature of debated physical origin found in the X-ray spectra of many type-1 active galactic nuclei (AGN). The eROSITA instrument aboard the Spectrum-Roentgen-Gamma (SRG) mission will provide an all-sky census of AGN suitable for spectral analysis. Aims. The primary goal of this work is to test a variety of models for the soft X-ray emission of AGN (thermal emission, non-thermal emission, ionised absorption, or neutral partial covering absorption) to help identify the physical origin of the soft X-ray spectral complexity. Differences between these models are examined in the context of this sample to understand the physical properties. Methods. We used Bayesian X-ray analysis to fit a sample of 200 AGN from the eFEDS hard X-ray--selected sample with a variety of phenomenological and physically motivated models. Model selection was performed using the Bayes factor to compare the applicability of each model. Results. We find that 29 sources have evidence for a soft excess at a confidence level >97.5%, all of which are better modelled by an additional soft power law than by thermal blackbody emission. We find 23 of these sources prefer a warm corona model, while six sources prefer relativistic blurred reflection. Additionally many sources show evidence for complex absorption, with 29 preferring a warm absorber and 25 a partial covering absorber. Sources with a soft excess show a significantly higher Eddington ratio than those with warm absorbers. We discuss the implication of these results for the physical processes in the central regions of AGN. Conclusions. Spectral fitting with Bayesian statistics is ideal for the identification of complex absorption and soft excesses in the X-ray spectra of AGN and can allow one to distinguish between different physical interpretations. (Abridged) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.00961v1-abstract-full').style.display = 'none'; document.getElementById('2306.00961v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">27 pages, 30 figures, plus 2 appendices. Accepted for publication by A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 690, A132 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.13368">arXiv:2305.13368</a> <span> [<a href="https://arxiv.org/pdf/2305.13368">pdf</a>, <a href="https://arxiv.org/format/2305.13368">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202346364">10.1051/0004-6361/202346364 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> X-ray properties and obscured fraction of AGN in the J1030 Chandra field </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Signorini%2C+M">Matilde Signorini</a>, <a href="/search/astro-ph?searchtype=author&query=Marchesi%2C+S">Stefano Marchesi</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">Roberto Gilli</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">Marcella Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Comastri%2C+A">Andrea Comastri</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Amato%2C+Q">Quirino D'Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Iwasawa%2C+K">Kazushi Iwasawa</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzuisi%2C+G">Giorgio Lanzuisi</a>, <a href="/search/astro-ph?searchtype=author&query=Mazzolari%2C+G">Giovanni Mazzolari</a>, <a href="/search/astro-ph?searchtype=author&query=Mignoli%2C+M">Marco Mignoli</a>, <a href="/search/astro-ph?searchtype=author&query=Peca%2C+A">Alessandro Peca</a>, <a href="/search/astro-ph?searchtype=author&query=Prandoni%2C+I">Isabella Prandoni</a>, <a href="/search/astro-ph?searchtype=author&query=Tozzi%2C+P">Paolo Tozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Vignali%2C+C">Cristian Vignali</a>, <a href="/search/astro-ph?searchtype=author&query=Vito%2C+F">Fabio Vito</a>, <a href="/search/astro-ph?searchtype=author&query=Norman%2C+C">Colin Norman</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2305.13368v1-abstract-short" style="display: inline;"> The 500ks Chandra ACIS-I observation of the field around the $z=6.31$ quasar SDSS J1030+0524 is currently the 5th deepest extragalactic X-ray survey. The rich multi-band coverage of the field allowed for an effective identification and redshift determination of the X-ray source counterparts: to date a catalog of 243 extragalactic X-ray sources with either a spectroscopic or photometric redshift es… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.13368v1-abstract-full').style.display = 'inline'; document.getElementById('2305.13368v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.13368v1-abstract-full" style="display: none;"> The 500ks Chandra ACIS-I observation of the field around the $z=6.31$ quasar SDSS J1030+0524 is currently the 5th deepest extragalactic X-ray survey. The rich multi-band coverage of the field allowed for an effective identification and redshift determination of the X-ray source counterparts: to date a catalog of 243 extragalactic X-ray sources with either a spectroscopic or photometric redshift estimate in the range $z\approx0-6$ is available over a 355 arcmin$^2$ area. Given its depth and the multi-band information, this catalog is an excellent resource to investigate X-ray spectral properties of distant Active Galactic Nuclei (AGN) and derive the redshift evolution of their obscuration. We performed a thorough X-ray spectral analysis for each object in the sample, measuring its nuclear column density $N_{\rm H}$ and intrinsic (de-absorbed) 2-10 keV rest-frame luminosity, $L_{2-10}$. Whenever possible, we also used the presence of the Fe K$_伪$ emission line to improve the photometric redshift estimates. We measured the fractions of AGN hidden by column densities in excess of $10^{22}$ and $10^{23}$cm$^{-2}$ ($f_{22}$ and $f_{23}$, respectively) as a function of $L_{2-10}$ and redshift, and corrected for selection effects to recover the intrinsic obscured fractions. At $z\sim 1.2$, we found $f_{22}\sim0.7-0.8$ and $f_{23}\sim0.5-0.6$, respectively, in broad agreement with the results from other X-ray surveys. No significant variations with X-ray luminosity were found within the limited luminosity range probed by our sample (log$L_{2-10}\sim 42.8-44.3$). When focusing on luminous AGN with log$L_{2-10}\sim44$ to maximize the sample completeness up to large cosmological distances, we did not observe any significant change in $f_{22}$ or $f_{23}$ over the redshift range $z\sim0.8-3$. Nonetheless, the obscured fractions we measure are significantly higher than ... <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.13368v1-abstract-full').style.display = 'none'; document.getElementById('2305.13368v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">A&A, in press</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 676, A49 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.02347">arXiv:2305.02347</a> <span> [<a href="https://arxiv.org/pdf/2305.02347">pdf</a>, <a href="https://arxiv.org/ps/2305.02347">ps</a>, <a href="https://arxiv.org/format/2305.02347">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202346795">10.1051/0004-6361/202346795 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> HYPerluminous quasars at the Epoch of ReionizatION (HYPERION). A new regime for the X-ray nuclear properties of the first quasars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zappacosta%2C+L">L. Zappacosta</a>, <a href="/search/astro-ph?searchtype=author&query=Piconcelli%2C+E">E. Piconcelli</a>, <a href="/search/astro-ph?searchtype=author&query=Fiore%2C+F">F. Fiore</a>, <a href="/search/astro-ph?searchtype=author&query=Saccheo%2C+I">I. Saccheo</a>, <a href="/search/astro-ph?searchtype=author&query=Valiante%2C+R">R. Valiante</a>, <a href="/search/astro-ph?searchtype=author&query=Vignali%2C+C">C. Vignali</a>, <a href="/search/astro-ph?searchtype=author&query=Vito%2C+F">F. Vito</a>, <a href="/search/astro-ph?searchtype=author&query=Volonteri%2C+M">M. Volonteri</a>, <a href="/search/astro-ph?searchtype=author&query=Bischetti%2C+M">M. Bischetti</a>, <a href="/search/astro-ph?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/astro-ph?searchtype=author&query=Done%2C+C">C. Done</a>, <a href="/search/astro-ph?searchtype=author&query=Elvis%2C+M">M. Elvis</a>, <a href="/search/astro-ph?searchtype=author&query=Giallongo%2C+E">E. Giallongo</a>, <a href="/search/astro-ph?searchtype=author&query=La+Franca%2C+F">F. La Franca</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzuisi%2C+G">G. Lanzuisi</a>, <a href="/search/astro-ph?searchtype=author&query=Laurenti%2C+M">M. Laurenti</a>, <a href="/search/astro-ph?searchtype=author&query=Miniutti%2C+G">G. Miniutti</a>, <a href="/search/astro-ph?searchtype=author&query=Bongiorno%2C+A">A. Bongiorno</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Civano%2C+F">F. Civano</a>, <a href="/search/astro-ph?searchtype=author&query=Carniani%2C+S">S. Carniani</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Odorico%2C+V">V. D'Odorico</a>, <a href="/search/astro-ph?searchtype=author&query=Feruglio%2C+C">C. Feruglio</a>, <a href="/search/astro-ph?searchtype=author&query=Gallerani%2C+S">S. Gallerani</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">R. Gilli</a> , et al. (18 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2305.02347v2-abstract-short" style="display: inline;"> The existence of luminous quasars (QSO) at the Epoch of Reionization (EoR; i.e. z>6) powered by supermassive black holes (SMBH) with masses $\gtrsim10^9~M_\odot$ challenges models of early SMBH formation. To shed light on the nature of these sources we started a multiwavelength programme based on a sample of 18 HYPerluminous quasars at the Epoch of ReionizatION (HYPERION). These are the luminous Q… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.02347v2-abstract-full').style.display = 'inline'; document.getElementById('2305.02347v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.02347v2-abstract-full" style="display: none;"> The existence of luminous quasars (QSO) at the Epoch of Reionization (EoR; i.e. z>6) powered by supermassive black holes (SMBH) with masses $\gtrsim10^9~M_\odot$ challenges models of early SMBH formation. To shed light on the nature of these sources we started a multiwavelength programme based on a sample of 18 HYPerluminous quasars at the Epoch of ReionizatION (HYPERION). These are the luminous QSOs whose SMBH must have had the fastest mass growth during the Universe first Gyr. In this paper we present the HYPERION sample and report on the first of the 3 years planned observations of the 2.4 Ms XMM-Newton Multi-Year Heritage program on which HYPERION is based. The goal of this program is to accurately characterize the X-ray nuclear properties of QSOs at the EoR. Through a joint X-ray spectral analysis of 10 sources, in the rest-frame $\sim2-50$ keV range, we report a steep average photon index ($螕\sim2.4\pm0.1$). Absorption is not required. The average $螕$ is inconsistent at $\geq4蟽$ level with the canonical 1.8-2 value measured in QSO at z<6. This spectral slope is also much steeper than that reported in lower-z QSOs with similar luminosity or accretion rate, thus suggesting a genuine redshift evolution. Alternatively, we can interpret this result as the presence of an unusually low-energy cutoff $E_{cut}\sim20$ keV on a standard $螕=1.9$ power-law. We also report on mild indications that HYPERION QSOs show higher soft X-ray emission at 2 keV compared to the UV one at 2500A than expected by lower-z luminous AGN. We speculate that a redshift-dependent coupling between the corona and accretion disc or intrinsically different coronal properties may account for the steep spectral slopes, especially in the presence of powerful winds. The reported slopes, if confirmed at lower luminosities, may have an important impact on future X-ray AGN studies in the early Universe. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.02347v2-abstract-full').style.display = 'none'; document.getElementById('2305.02347v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages (including appendix), 12 figures, 4 tables. Accepted for pubblication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 678, A201 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.08405">arXiv:2302.08405</a> <span> [<a href="https://arxiv.org/pdf/2302.08405">pdf</a>, <a href="https://arxiv.org/format/2302.08405">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> The X-ray invisible Universe. A look into the halos undetected by eROSITA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Popesso%2C+P">P. Popesso</a>, <a href="/search/astro-ph?searchtype=author&query=Biviano%2C+A">A. Biviano</a>, <a href="/search/astro-ph?searchtype=author&query=Bulbul%2C+E">E. Bulbul</a>, <a href="/search/astro-ph?searchtype=author&query=Merloni%2C+A">A. Merloni</a>, <a href="/search/astro-ph?searchtype=author&query=Comparat%2C+J">J. Comparat</a>, <a href="/search/astro-ph?searchtype=author&query=Clerc%2C+N">N. Clerc</a>, <a href="/search/astro-ph?searchtype=author&query=Igo%2C+Z">Z. Igo</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+A">A. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Driver%2C+S">S. Driver</a>, <a href="/search/astro-ph?searchtype=author&query=Salvato%2C+M">M. Salvato</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Bahar%2C+Y+E">Y. E. Bahar</a>, <a href="/search/astro-ph?searchtype=author&query=Malavasi%2C+N">N. Malavasi</a>, <a href="/search/astro-ph?searchtype=author&query=Ghirardini%2C+V">V. Ghirardini</a>, <a href="/search/astro-ph?searchtype=author&query=Ponti%2C+G">G. Ponti</a>, <a href="/search/astro-ph?searchtype=author&query=Robotham%2C+A">A. Robotham</a>, <a href="/search/astro-ph?searchtype=author&query=Liske%2C+J">J. Liske</a>, <a href="/search/astro-ph?searchtype=author&query=Grandis%2C+S">S. Grandis</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2302.08405v2-abstract-short" style="display: inline;"> The paper presents the analysis of optically selected GAMA groups and clusters in the SRG/eROSITA X-ray map of eFEDS (eROSITA Final Equatorial Depth Survey), in the halo mass range $10^{13}-5{\times}10^{14}$ $M_{\odot}$ and at $z < 0.2$. All X-ray detections have a clear GAMA counterpart, but most of the GAMA groups in the halo mass range $10^{13}-10^{14}$ $M_{\odot}$ remain undetected. We compare… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.08405v2-abstract-full').style.display = 'inline'; document.getElementById('2302.08405v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.08405v2-abstract-full" style="display: none;"> The paper presents the analysis of optically selected GAMA groups and clusters in the SRG/eROSITA X-ray map of eFEDS (eROSITA Final Equatorial Depth Survey), in the halo mass range $10^{13}-5{\times}10^{14}$ $M_{\odot}$ and at $z < 0.2$. All X-ray detections have a clear GAMA counterpart, but most of the GAMA groups in the halo mass range $10^{13}-10^{14}$ $M_{\odot}$ remain undetected. We compare the X-ray surface brightness profiles of the eROSITA detected groups with the mean stacked profile of the undetected low-mass halos at fixed halo mass. Overall, we find that the undetected groups exhibit less concentrated X-ray surface brightness, dark matter, and galaxy distributions with respect to the X-ray detected halos. The mean gas mass fraction profiles are consistent in the two samples within 1.5$蟽$, indicating that the gas follows the dark matter profile. The low mass concentration and the magnitude gap indicate that these systems are young. They reside with a higher probability in filaments while X-ray detected groups favor the nodes of the Cosmic Web. Because of the lower central emission, the undetected systems tend to be X-ray under-luminous at fixed halo mass and to lie below the $L_X-M_{halo}$ relation. Interestingly, the X-ray detected systems inhabiting the nodes scatter the less around the relation, while those in filaments tend to lie below it. We do not observe any strong relationship between the system X-ray appearance and the AGN activity. We cannot exclude the role of the past AGN feedback in affecting the gas distribution over the halo lifetime. However, the data suggests that the observed differences might be related to the halo assembly bias. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.08405v2-abstract-full').style.display = 'none'; document.getElementById('2302.08405v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 14 figures, Accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.01358">arXiv:2302.01358</a> <span> [<a href="https://arxiv.org/pdf/2302.01358">pdf</a>, <a href="https://arxiv.org/format/2302.01358">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202245168">10.1051/0004-6361/202245168 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The miniJPAS survey: AGN & host galaxy co-evolution of X-ray selected sources </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=L%C3%B3pez%2C+I+E">I. E. L贸pez</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Bonoli%2C+S">S. Bonoli</a>, <a href="/search/astro-ph?searchtype=author&query=Shankar%2C+F">F. Shankar</a>, <a href="/search/astro-ph?searchtype=author&query=Acharya%2C+N">N. Acharya</a>, <a href="/search/astro-ph?searchtype=author&query=Laloux%2C+B">B. Laloux</a>, <a href="/search/astro-ph?searchtype=author&query=Dolag%2C+K">K. Dolag</a>, <a href="/search/astro-ph?searchtype=author&query=Georgakakis%2C+A">A. Georgakakis</a>, <a href="/search/astro-ph?searchtype=author&query=Lapi%2C+A">A. Lapi</a>, <a href="/search/astro-ph?searchtype=author&query=Almeida%2C+C+R">C. Ramos Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Salvato%2C+M">M. Salvato</a>, <a href="/search/astro-ph?searchtype=author&query=Chaves-Montero%2C+J">J. Chaves-Montero</a>, <a href="/search/astro-ph?searchtype=author&query=Coelho%2C+P">P. Coelho</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%ADaz-Garc%C3%ADa%2C+L+A">L. A. D铆az-Garc铆a</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez-Ontiveros%2C+J+A">J. A. Fern谩ndez-Ontiveros</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1n-Caballero%2C+A">A. Hern谩n-Caballero</a>, <a href="/search/astro-ph?searchtype=author&query=Delgado%2C+R+M+G">R. M. Gonz谩lez Delgado</a>, <a href="/search/astro-ph?searchtype=author&query=Marquez%2C+I">I. Marquez</a>, <a href="/search/astro-ph?searchtype=author&query=Povi%C4%87%2C+M">M. Povi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Soria%2C+R">R. Soria</a>, <a href="/search/astro-ph?searchtype=author&query=Queiroz%2C+C">C. Queiroz</a>, <a href="/search/astro-ph?searchtype=author&query=Rahna%2C+P+T">P. T. Rahna</a>, <a href="/search/astro-ph?searchtype=author&query=Abramo%2C+R">R. Abramo</a>, <a href="/search/astro-ph?searchtype=author&query=Alcaniz%2C+J">J. Alcaniz</a>, <a href="/search/astro-ph?searchtype=author&query=Benitez%2C+N">N. Benitez</a> , et al. (13 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2302.01358v1-abstract-short" style="display: inline;"> Studies indicate strong evidence of a scaling relation in the local Universe between the supermassive black hole mass ($M_\rm{BH}$) and the stellar mass of their host galaxies ($M_\star$). They even show similar histories across cosmic times of their differential terms: star formation rate (SFR) and black hole accretion rate (BHAR). However, a clear picture of this coevolution is far from being un… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.01358v1-abstract-full').style.display = 'inline'; document.getElementById('2302.01358v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.01358v1-abstract-full" style="display: none;"> Studies indicate strong evidence of a scaling relation in the local Universe between the supermassive black hole mass ($M_\rm{BH}$) and the stellar mass of their host galaxies ($M_\star$). They even show similar histories across cosmic times of their differential terms: star formation rate (SFR) and black hole accretion rate (BHAR). However, a clear picture of this coevolution is far from being understood. We select an X-ray sample of active galactic nuclei (AGN) up to $z=2.5$ in the miniJPAS footprint. Their X-ray to infrared spectral energy distributions (SEDs) have been modeled with CIGALE, constraining the emission to 68 bands. For a final sample of 308 galaxies, we derive their physical properties (e.g., $M_\star$, $\rm{SFR}$, $\rm{SFH}$, and $L_\rm{AGN}$). We also fit their optical spectra for a subsample of 113 sources to estimate the $M_\rm{BH}$. We calculate the BHAR depending on two radiative efficiency regimes. We find that the Eddington ratios ($位$) and its popular proxy ($L_\rm{X}$/$M_\star$) have 0.6 dex of difference, and a KS-test indicates that they come from different distributions. Our sources exhibit a considerable scatter on the $M_\rm{BH}$-$M_\star$ relation, which can explain the difference between $位$ and its proxy. We also model three evolution scenarios to recover the integral properties at $z=0$. Using the SFR and BHAR, we show a notable diminution in the scattering between $M_\rm{BH}$-$M_\star$. For the last scenario, we consider the SFH and a simple energy budget for the AGN accretion, obtaining a relation similar to the local Universe. Our study covers $\sim 1$ deg$^2$ in the sky and is sensitive to biases in luminosity. Nevertheless, we show that, for bright sources, the link between SFR and BHAR, and their decoupling based on an energy limit is the key that leads to the local $M_\rm{BH}$-$M_\star$ scaling relation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.01358v1-abstract-full').style.display = 'none'; document.getElementById('2302.01358v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 672, A137 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.11060">arXiv:2301.11060</a> <span> [<a href="https://arxiv.org/pdf/2301.11060">pdf</a>, <a href="https://arxiv.org/format/2301.11060">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202346001">10.1051/0004-6361/202346001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Bubbles and outflows: the novel JWST/NIRSpec view of the z=1.59 obscured quasar XID2028 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cresci%2C+G">Giovanni Cresci</a>, <a href="/search/astro-ph?searchtype=author&query=Tozzi%2C+G">Giulia Tozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Perna%2C+M">Michele Perna</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">Marcella Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Marconcini%2C+C">Cosimo Marconcini</a>, <a href="/search/astro-ph?searchtype=author&query=Marconi%2C+A">Alessandro Marconi</a>, <a href="/search/astro-ph?searchtype=author&query=Carniani%2C+S">Stefano Carniani</a>, <a href="/search/astro-ph?searchtype=author&query=Brienza%2C+M">Marisa Brienza</a>, <a href="/search/astro-ph?searchtype=author&query=Giroletti%2C+M">Marcello Giroletti</a>, <a href="/search/astro-ph?searchtype=author&query=Belfiore%2C+F">Francesco Belfiore</a>, <a href="/search/astro-ph?searchtype=author&query=Ginolfi%2C+M">Michele Ginolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Mannucci%2C+F">Filippo Mannucci</a>, <a href="/search/astro-ph?searchtype=author&query=Ulivi%2C+L">Lorenzo Ulivi</a>, <a href="/search/astro-ph?searchtype=author&query=Scholtz%2C+J">Jan Scholtz</a>, <a href="/search/astro-ph?searchtype=author&query=Venturi%2C+G">Giacomo Venturi</a>, <a href="/search/astro-ph?searchtype=author&query=Arribas%2C+S">Santiago Arribas</a>, <a href="/search/astro-ph?searchtype=author&query=%C3%9Cbler%2C+H">Hanna 脺bler</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Eugenio%2C+F">Francesco D'Eugenio</a>, <a href="/search/astro-ph?searchtype=author&query=Mingozzi%2C+M">Matilde Mingozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Balmaverde%2C+B">Barbara Balmaverde</a>, <a href="/search/astro-ph?searchtype=author&query=Capetti%2C+A">Alessandro Capetti</a>, <a href="/search/astro-ph?searchtype=author&query=Parlanti%2C+E">Eleonora Parlanti</a>, <a href="/search/astro-ph?searchtype=author&query=Zana%2C+T">Tommaso Zana</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2301.11060v2-abstract-short" style="display: inline;"> Quasar feedback in the form of powerful outflows is invoked as a key mechanism to quench star formation in galaxies, although direct observational evidence is still scarce and debated. Here we present Early Release Science JWST NIRSpec IFU observations of the z=1.59 prototypical obscured Active Galactic Nucleus (AGN) XID2028: This target represents a unique test case for studying quasar feedback a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.11060v2-abstract-full').style.display = 'inline'; document.getElementById('2301.11060v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.11060v2-abstract-full" style="display: none;"> Quasar feedback in the form of powerful outflows is invoked as a key mechanism to quench star formation in galaxies, although direct observational evidence is still scarce and debated. Here we present Early Release Science JWST NIRSpec IFU observations of the z=1.59 prototypical obscured Active Galactic Nucleus (AGN) XID2028: This target represents a unique test case for studying quasar feedback at the peak epoch of AGN-galaxy co-evolution because extensive multi-wavelength coverage is available and a massive and extended outflow is detected in the ionised and molecular components. With the unprecedented sensitivity and spatial resolution of the JWST, the NIRSpec dataset reveals a wealth of structures in the ionised gas kinematics and morphology that were previously hidden in the seeing-limited ground-based data. In particular, we find evidence of an interaction between the interstellar medium of the galaxy and the quasar-driven outflow and radio jet that produces an expanding bubble from which the fast and extended wind detected in previous observations emerges. The new observations confirm the complex interplay between the AGN jet, wind and the interstellar medium of the host galaxy, highlighting the role of low-luminosity radio jets in AGN feedback. They also clearly show the new window that NIRSpec opens for detailed studies of feedback at high redshift. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.11060v2-abstract-full').style.display = 'none'; document.getElementById('2301.11060v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 11 figures, accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 672, A128 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.02961">arXiv:2212.02961</a> <span> [<a href="https://arxiv.org/pdf/2212.02961">pdf</a>, <a href="https://arxiv.org/format/2212.02961">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202245047">10.1051/0004-6361/202245047 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Supermassive Black Hole Winds in X-rays: SUBWAYS. II. HST UV spectroscopy of winds at intermediate redshifts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mehdipour%2C+M">M. Mehdipour</a>, <a href="/search/astro-ph?searchtype=author&query=Kriss%2C+G+A">G. A. Kriss</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Matzeu%2C+G+A">G. A. Matzeu</a>, <a href="/search/astro-ph?searchtype=author&query=Gaspari%2C+M">M. Gaspari</a>, <a href="/search/astro-ph?searchtype=author&query=Kraemer%2C+S+B">S. B. Kraemer</a>, <a href="/search/astro-ph?searchtype=author&query=Mathur%2C+S">S. Mathur</a>, <a href="/search/astro-ph?searchtype=author&query=Behar%2C+E">E. Behar</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+S">S. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Cappi%2C+M">M. Cappi</a>, <a href="/search/astro-ph?searchtype=author&query=Chartas%2C+G">G. Chartas</a>, <a href="/search/astro-ph?searchtype=author&query=Costantini%2C+E">E. Costantini</a>, <a href="/search/astro-ph?searchtype=author&query=Cresci%2C+G">G. Cresci</a>, <a href="/search/astro-ph?searchtype=author&query=Dadina%2C+M">M. Dadina</a>, <a href="/search/astro-ph?searchtype=author&query=De+Marco%2C+B">B. De Marco</a>, <a href="/search/astro-ph?searchtype=author&query=De+Rosa%2C+A">A. De Rosa</a>, <a href="/search/astro-ph?searchtype=author&query=Dunn%2C+J+P">J. P. Dunn</a>, <a href="/search/astro-ph?searchtype=author&query=Gianolli%2C+V+E">V. E. Gianolli</a>, <a href="/search/astro-ph?searchtype=author&query=Giustini%2C+M">M. Giustini</a>, <a href="/search/astro-ph?searchtype=author&query=Kaastra%2C+J+S">J. S. Kaastra</a>, <a href="/search/astro-ph?searchtype=author&query=King%2C+A+R">A. R. King</a>, <a href="/search/astro-ph?searchtype=author&query=Krongold%2C+Y">Y. Krongold</a>, <a href="/search/astro-ph?searchtype=author&query=La+Franca%2C+F">F. La Franca</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzuisi%2C+G">G. Lanzuisi</a>, <a href="/search/astro-ph?searchtype=author&query=Longinotti%2C+A+L">A. L. Longinotti</a> , et al. (13 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2212.02961v1-abstract-short" style="display: inline;"> We present a UV spectroscopic study of ionized outflows in 21 active galactic nuclei (AGN), observed with the HST. The targets of the SUBWAYS sample were selected with the aim to probe the parameter space of the underexplored AGN between the local Seyfert galaxies and the luminous quasars at high redshifts. Our targets, spanning redshifts of 0.1-0.4 and bolometric luminosities (L_bol) of 10^45-10^… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.02961v1-abstract-full').style.display = 'inline'; document.getElementById('2212.02961v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.02961v1-abstract-full" style="display: none;"> We present a UV spectroscopic study of ionized outflows in 21 active galactic nuclei (AGN), observed with the HST. The targets of the SUBWAYS sample were selected with the aim to probe the parameter space of the underexplored AGN between the local Seyfert galaxies and the luminous quasars at high redshifts. Our targets, spanning redshifts of 0.1-0.4 and bolometric luminosities (L_bol) of 10^45-10^46 erg/s, have been observed with a large multi-wavelength campaign. Here, we model the UV spectra and look for different types of AGN outflows. We find that 60% of our targets show a presence of outflowing H I absorption, while 40% exhibit ionized outflows seen as absorption by either C IV, N V, or O VI. This is comparable to the occurrence of ionized outflows seen in the local Seyfert galaxies. All UV absorption lines in the sample are relatively narrow, with outflow velocities reaching up to -3300 km/s. We did not detect any UV counterparts to the X-ray ultra-fast outflows (UFOs), most likely due to their being too highly ionized. However, all SUBWAYS targets with an X-ray UFO demonstrate the presence of UV outflows at lower velocities. We find significant correlations between the column density (N) of the UV ions and L_bol of the AGN, with N of H I decreasing with L_bol, while N of O VI is increasing with L_bol. This is likely to be a photoionization effect, where toward higher AGN luminosities, the wind becomes more ionized, resulting in less absorption by neutral or low-ionization ions and more absorption by high-ionization ions. In addition, we find that N of the UV ions decreases as their outflow velocity increases. This may be explained by a mechanical power that is evacuating the UV-absorbing medium. Our observed relations are consistent with multiphase AGN feeding and feedback simulations indicating that a combination of both radiative and mechanical processes are in play. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.02961v1-abstract-full').style.display = 'none'; document.getElementById('2212.02961v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astronomy & Astrophysics (A&A), 22 pages, 12 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.02960">arXiv:2212.02960</a> <span> [<a href="https://arxiv.org/pdf/2212.02960">pdf</a>, <a href="https://arxiv.org/format/2212.02960">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202245036">10.1051/0004-6361/202245036 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Supermassive Black Hole Winds in X-rays -- SUBWAYS. I. Ultra-fast outflows in QSOs beyond the local Universe </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Matzeu%2C+G+A">G. A. Matzeu</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzuisi%2C+G">G. Lanzuisi</a>, <a href="/search/astro-ph?searchtype=author&query=Dadina%2C+M">M. Dadina</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+S">S. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Kriss%2C+G">G. Kriss</a>, <a href="/search/astro-ph?searchtype=author&query=Mehdipour%2C+M">M. Mehdipour</a>, <a href="/search/astro-ph?searchtype=author&query=Nardini%2C+E">E. Nardini</a>, <a href="/search/astro-ph?searchtype=author&query=Chartas%2C+G">G. Chartas</a>, <a href="/search/astro-ph?searchtype=author&query=Middei%2C+R">R. Middei</a>, <a href="/search/astro-ph?searchtype=author&query=Piconcelli%2C+E">E. Piconcelli</a>, <a href="/search/astro-ph?searchtype=author&query=Gianolli%2C+V">V. Gianolli</a>, <a href="/search/astro-ph?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/astro-ph?searchtype=author&query=Longinotti%2C+A+L">A. L. Longinotti</a>, <a href="/search/astro-ph?searchtype=author&query=Krongold%2C+Y">Y. Krongold</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">F. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Petrucci%2C+P+O">P. O. Petrucci</a>, <a href="/search/astro-ph?searchtype=author&query=Tombesi%2C+F">F. Tombesi</a>, <a href="/search/astro-ph?searchtype=author&query=Luminari%2C+A">A. Luminari</a>, <a href="/search/astro-ph?searchtype=author&query=Zappacosta%2C+L">L. Zappacosta</a>, <a href="/search/astro-ph?searchtype=author&query=Miniutti%2C+G">G. Miniutti</a>, <a href="/search/astro-ph?searchtype=author&query=Gaspari%2C+M">M. Gaspari</a>, <a href="/search/astro-ph?searchtype=author&query=Behar%2C+E">E. Behar</a>, <a href="/search/astro-ph?searchtype=author&query=Bischetti%2C+M">M. Bischetti</a>, <a href="/search/astro-ph?searchtype=author&query=Mathur%2C+S">S. Mathur</a> , et al. (26 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2212.02960v1-abstract-short" style="display: inline;"> We present a new X-ray spectroscopic study of $22$ luminous ($2\times10^{45}\lesssim L_{\rm bol}\rm /erg\,s^{-1} \lesssim 2\times10^{46}$) active galactic nuclei (AGNs) at intermediate-redshift ($0.1 \lesssim z \lesssim 0.4$), as part of the SUpermassive Black hole Winds in the x-rAYS (SUBWAYS) sample, mostly composed of quasars (QSOs) and type\,1 AGN. Here, 17 targets were observed with \textit{X… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.02960v1-abstract-full').style.display = 'inline'; document.getElementById('2212.02960v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.02960v1-abstract-full" style="display: none;"> We present a new X-ray spectroscopic study of $22$ luminous ($2\times10^{45}\lesssim L_{\rm bol}\rm /erg\,s^{-1} \lesssim 2\times10^{46}$) active galactic nuclei (AGNs) at intermediate-redshift ($0.1 \lesssim z \lesssim 0.4$), as part of the SUpermassive Black hole Winds in the x-rAYS (SUBWAYS) sample, mostly composed of quasars (QSOs) and type\,1 AGN. Here, 17 targets were observed with \textit{XMM-Newton} between 2019--2020 and the remaining 5 are from previous observations. The aim of this large campaign ($1.45\,\rm Ms$ duration) is to characterise the various manifestations of winds in the X-rays driven from supermassive black holes in AGN. In this paper we focus on the search and characterization of ultra-fast outflows (UFOs), which are typically detected through blueshifted absorption troughs in the Fe\,K band ($E>7\,\rm keV$). By following Monte Carlo procedures, we confirm the detection of absorption lines corresponding to highly ionised iron (e.g., Fe\,\textsc{xxv}\,H$伪$, Fe\,\textsc{xxvi}\,Ly$伪$) in 7/22 sources at the $\gtrsim95\%$ confidence level (for each individual line). The global combined probability of such absorption features in the sample is $>99.9\%$. The SUBWAYS campaign extends at higher luminosity and redshifts than previous local studies on Seyferts, obtained using \xmm and \suzaku observations. We find a UFO detection fraction of $\sim30\%$ on the total sample that is in agreement with the previous findings. This work independently provides further support for the existence of highly-ionised matter propagating at mildly relativistic speed ($\gtrsim0.1c$) in a considerable fraction of AGN over a broad range of luminosities, which is expected to play a key role in the self-regulated AGN feeding-feedback cycle, as also supported by hydrodynamical multiphase simulations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.02960v1-abstract-full').style.display = 'none'; document.getElementById('2212.02960v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">30 pages, 10 figures, accepted for publication in A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.13820">arXiv:2211.13820</a> <span> [<a href="https://arxiv.org/pdf/2211.13820">pdf</a>, <a href="https://arxiv.org/format/2211.13820">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202244688">10.1051/0004-6361/202244688 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> X-ray emission from a rapidly accreting narrow-line Seyfert 1 galaxy at z=6.56 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wolf%2C+J">Julien Wolf</a>, <a href="/search/astro-ph?searchtype=author&query=Nandra%2C+K">Kirpal Nandra</a>, <a href="/search/astro-ph?searchtype=author&query=Salvato%2C+M">Mara Salvato</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+J">Johannes Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Onoue%2C+M">Masafusa Onoue</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+T">Teng Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Arcodia%2C+R">Riccardo Arcodia</a>, <a href="/search/astro-ph?searchtype=author&query=Merloni%2C+A">Andrea Merloni</a>, <a href="/search/astro-ph?searchtype=author&query=Ciroi%2C+S">Stefano Ciroi</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Mille%2C+F">Francesco Di Mille</a>, <a href="/search/astro-ph?searchtype=author&query=Burwitz%2C+V">Vadim Burwitz</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">Marcella Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Ishimoto%2C+R">Rikako Ishimoto</a>, <a href="/search/astro-ph?searchtype=author&query=Kashikawa%2C+N">Nobunari Kashikawa</a>, <a href="/search/astro-ph?searchtype=author&query=Matsuoka%2C+Y">Yoshiki Matsuoka</a>, <a href="/search/astro-ph?searchtype=author&query=Urrutia%2C+T">Tanya Urrutia</a>, <a href="/search/astro-ph?searchtype=author&query=Waddell%2C+S">Sophia Waddell</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2211.13820v1-abstract-short" style="display: inline;"> This study aims at identifying luminous quasars at $z>5.7$ among X-ray-selected sources in the eROSITA Final Equatorial-Depth Survey (eFEDS) in order to place a lower limit on black hole accretion well into the epoch of re-ionisation. We confirm the low significance detection with eROSITA of a previously known, optically faint $z=6.56$ quasar from the Subaru High-z Exploration of Low-luminosity Qu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.13820v1-abstract-full').style.display = 'inline'; document.getElementById('2211.13820v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.13820v1-abstract-full" style="display: none;"> This study aims at identifying luminous quasars at $z>5.7$ among X-ray-selected sources in the eROSITA Final Equatorial-Depth Survey (eFEDS) in order to place a lower limit on black hole accretion well into the epoch of re-ionisation. We confirm the low significance detection with eROSITA of a previously known, optically faint $z=6.56$ quasar from the Subaru High-z Exploration of Low-luminosity Quasars (SHELLQs) survey. We obtained a pointed follow-up observation of the source with the Chandra X-ray telescope in order to confirm the eROSITA detection. Using new near-infrared spectroscopy, we derived the physical properties of the super-massive black hole. Finally, we used this detection to infer a lower limit on the black hole accretion density rate at $z>6$. The Chandra observation confirms the eFEDS source as the most distant blind X-ray detection to date. The derived X-ray luminosity is high with respect to the rest-frame optical emission of the quasar. With a narrow MgII line, low derived black hole mass, and high Eddington ratio, as well as its steep photon index, the source shows properties that are similar to local narrow-line Seyfert 1 galaxies, which are thought to be powered by young super-massive black holes. In combination with a previous high-redshift quasar detection in the field, we show that quasars with $L_{2-10 \, \mathrm{keV}} >10^{45} \, \mathrm{erg \, s^{-1}}$ dominate accretion onto super-massive black holes at $z\sim 6$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.13820v1-abstract-full').style.display = 'none'; document.getElementById('2211.13820v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 669, A127 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.00032">arXiv:2211.00032</a> <span> [<a href="https://arxiv.org/pdf/2211.00032">pdf</a>, <a href="https://arxiv.org/format/2211.00032">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stac3114">10.1093/mnras/stac3114 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Cosmic evolution of the incidence of Active Galactic Nuclei in massive clusters: Simulations versus observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rodr%C3%ADguez%2C+I+M">Iv谩n Mu帽oz Rodr铆guez</a>, <a href="/search/astro-ph?searchtype=author&query=Georgakakis%2C+A">Antonis Georgakakis</a>, <a href="/search/astro-ph?searchtype=author&query=Shankar%2C+F">Francesco Shankar</a>, <a href="/search/astro-ph?searchtype=author&query=Allevato%2C+V">Viola Allevato</a>, <a href="/search/astro-ph?searchtype=author&query=Bonoli%2C+S">Silvia Bonoli</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">Marcella Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Lapi%2C+A">Andrea Lapi</a>, <a href="/search/astro-ph?searchtype=author&query=Viitanen%2C+A">Akke Viitanen</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2211.00032v1-abstract-short" style="display: inline;"> This paper explores the role of small-scale environment ($<1$ Mpc) in modulating accretion events onto supermassive black holes by studying the incidence of Active Galactic Nuclei (AGN) in massive clusters of galaxies. A flexible, data-driven semi-empirical model is developed based on a minimal set of parameters and under the zero order assumption that the incidence of AGN in galaxies is independe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.00032v1-abstract-full').style.display = 'inline'; document.getElementById('2211.00032v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.00032v1-abstract-full" style="display: none;"> This paper explores the role of small-scale environment ($<1$ Mpc) in modulating accretion events onto supermassive black holes by studying the incidence of Active Galactic Nuclei (AGN) in massive clusters of galaxies. A flexible, data-driven semi-empirical model is developed based on a minimal set of parameters and under the zero order assumption that the incidence of AGN in galaxies is independent of environment. This is used to predict how the fraction of X-ray selected AGN among galaxies in massive dark matter halos ($\gtrsim 3\times 10^{14}\,M_{\odot}$) evolves with redshift and reveal tensions with observations. At high redshift, $z\sim1.2$, the model underpredicts AGN fractions, particularly at high X-ray luminosities, $L_X(\rm 2-10\,keV) \gtrsim 10^{44}\, erg \, s^{-1}$. At low redshift, $z\sim0.2$, the model estimates fractions of moderate luminosity AGN ($L_X(\rm 2-10\,keV) \gtrsim 10^{43}\, erg \, s^{-1}$) that are a factor of $2-3$ higher than the observations. These findings reject the zero order assumption on which the semi-empirical model hinges and point to a strong and redshift-dependent influence of the small-scale environment on the growth of black holes. Cluster of galaxies appear to promote AGN activity relative to the model expectation at $z\sim1.2$ and suppress it close to the present day. These trends could be explained by the increasing gas content of galaxies toward higher redshift combined with an efficient triggering of AGN at earlier times in galaxies that fall onto clusters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.00032v1-abstract-full').style.display = 'none'; document.getElementById('2211.00032v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted in Monthly Notices of the Royal Astronomical Society</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.04335">arXiv:2208.04335</a> <span> [<a href="https://arxiv.org/pdf/2208.04335">pdf</a>, <a href="https://arxiv.org/format/2208.04335">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202243406">10.1051/0004-6361/202243406 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Unveiling the warm dense ISM in $z>6$ quasar host galaxies via water vapor emission </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pensabene%2C+A">A. Pensabene</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Werf%2C+P">P. van der Werf</a>, <a href="/search/astro-ph?searchtype=author&query=Decarli%2C+R">R. Decarli</a>, <a href="/search/astro-ph?searchtype=author&query=Ba%C3%B1ados%2C+E">E. Ba帽ados</a>, <a href="/search/astro-ph?searchtype=author&query=Meyer%2C+R+A">R. A. Meyer</a>, <a href="/search/astro-ph?searchtype=author&query=Riechers%2C+D">D. Riechers</a>, <a href="/search/astro-ph?searchtype=author&query=Venemans%2C+B">B. Venemans</a>, <a href="/search/astro-ph?searchtype=author&query=Walter%2C+F">F. Walter</a>, <a href="/search/astro-ph?searchtype=author&query=Wei%C3%9F%2C+A">A. Wei脽</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Fan%2C+X">X. Fan</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+F">F. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+J">J. Yang</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2208.04335v1-abstract-short" style="display: inline;"> Water vapor (H$_{2}$O) is one of the brightest molecular emitters after carbon monoxide (CO) in galaxies with high infrared (IR) luminosity, and allows us to investigate the warm dense phase of the interstellar medium (ISM) where star formation occurs. However, due to the complexity of its radiative spectrum, H$_{2}$O is not frequently exploited as an ISM tracer in distant galaxies. Therefore, H… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.04335v1-abstract-full').style.display = 'inline'; document.getElementById('2208.04335v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.04335v1-abstract-full" style="display: none;"> Water vapor (H$_{2}$O) is one of the brightest molecular emitters after carbon monoxide (CO) in galaxies with high infrared (IR) luminosity, and allows us to investigate the warm dense phase of the interstellar medium (ISM) where star formation occurs. However, due to the complexity of its radiative spectrum, H$_{2}$O is not frequently exploited as an ISM tracer in distant galaxies. Therefore, H$_{2}$O studies of the warm and dense gas at high-$z$ remains largely unexplored. In this work we present observations conducted with the Northern Extended Millimeter Array (NOEMA) toward three $z>6$ IR-bright quasars J2310+1855, J1148+5251, and J0439+1634 targeted in their multiple para-/ortho-H$_{2}$O transitions ($3_{12}-3_{03}$, $1_{11}-0_{00}$, $2_{20}-2_{11}$, and $4_{22}-4_{13}$), as well as their far-IR (FIR) dust continuum. By combining our data with previous measurements from the literature we estimate dust masses and temperatures, continuum optical depths, IR luminosities, and the star-formation rates from the FIR continuum. We model the H$_{2}$O lines using the MOLPOP-CEP radiative transfer code and find that water vapor lines in our quasar host galaxies are primarily excited in warm dense (gas kinetic temperature and density of $T_{\rm kin} = 50\,{\rm K}$, $n_{\rm H_{2}}\sim 10^{4.5}-10^{5}\,{\rm cm^{-3}}$) molecular medium with water vapor column density of $N_{\rm H_{2}O}\sim 2\times10^{17}-3\times10^{18}\,{\rm cm^{-3}}$. High-$J$ H$_{2}$O lines are mainly radiatively pumped by the intense optically-thin far-IR radiation field associated with a warm dust component with temperatures of $T_{\rm dust}\sim 80-190\,{\rm K}$ that account for $<5-10\%$ of the total dust mass. Our results are in agreement with expectations based on the H$_{2}$O spectral line energy distribution of local and high-$z$ ultra-luminous IR galaxies and AGN. [abridged] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.04335v1-abstract-full').style.display = 'none'; document.getElementById('2208.04335v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A: 18 pages, 9 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 667, A9 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.13731">arXiv:2207.13731</a> <span> [<a href="https://arxiv.org/pdf/2207.13731">pdf</a>, <a href="https://arxiv.org/format/2207.13731">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stac2155">10.1093/mnras/stac2155 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A New Emulated Monte Carlo Radiative Transfer Disk-Wind Model: X-Ray Accretion Disk-wind Emulator -- XRADE </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Matzeu%2C+G+A">G. A. Matzeu</a>, <a href="/search/astro-ph?searchtype=author&query=Lieu%2C+M">M. Lieu</a>, <a href="/search/astro-ph?searchtype=author&query=Costa%2C+M+T">M. T. Costa</a>, <a href="/search/astro-ph?searchtype=author&query=Reeves%2C+J+N">J. N. Reeves</a>, <a href="/search/astro-ph?searchtype=author&query=Braito%2C+V">V. Braito</a>, <a href="/search/astro-ph?searchtype=author&query=Dadina%2C+M">M. Dadina</a>, <a href="/search/astro-ph?searchtype=author&query=Nardini%2C+E">E. Nardini</a>, <a href="/search/astro-ph?searchtype=author&query=Boorman%2C+P+G">P. G. Boorman</a>, <a href="/search/astro-ph?searchtype=author&query=Parker%2C+M+L">M. L. Parker</a>, <a href="/search/astro-ph?searchtype=author&query=Sim%2C+S+A">S. A. Sim</a>, <a href="/search/astro-ph?searchtype=author&query=Barret%2C+D">D. Barret</a>, <a href="/search/astro-ph?searchtype=author&query=Kammoun%2C+E">E. Kammoun</a>, <a href="/search/astro-ph?searchtype=author&query=Middei%2C+R">R. Middei</a>, <a href="/search/astro-ph?searchtype=author&query=Giustini%2C+M">M. Giustini</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Cabrera%2C+J+P">J. P茅rez Cabrera</a>, <a href="/search/astro-ph?searchtype=author&query=Marchesi%2C+S">S. Marchesi</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2207.13731v1-abstract-short" style="display: inline;"> We present a new X-Ray Accretion Disk-wind Emulator (\textsc{xrade}) based on the 2.5D Monte Carlo radiative transfer code which provides a physically-motivated, self-consistent treatment of both absorption and emission from a disk-wind by computing the local ionization state and velocity field within the flow. \textsc{xrade} is then implemented through a process that combines X-ray tracing with s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.13731v1-abstract-full').style.display = 'inline'; document.getElementById('2207.13731v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.13731v1-abstract-full" style="display: none;"> We present a new X-Ray Accretion Disk-wind Emulator (\textsc{xrade}) based on the 2.5D Monte Carlo radiative transfer code which provides a physically-motivated, self-consistent treatment of both absorption and emission from a disk-wind by computing the local ionization state and velocity field within the flow. \textsc{xrade} is then implemented through a process that combines X-ray tracing with supervised machine learning. We develop a novel emulation method consisting in training, validating, and testing the simulated disk-wind spectra into a purposely built artificial neural network. The trained emulator can generate a single synthetic spectrum for a particular parameter set in a fraction of a second, in contrast to the few hours required by a standard Monte Carlo radiative transfer pipeline. The emulator does not suffer from interpolation issues with multi-dimensional spaces that are typically faced by traditional X-ray fitting packages such as \textsc{xspec}. \textsc{xrade} will be suitable to a wide number of sources across the black-hole mass, ionizing luminosity, and accretion rate scales. As an example, we demonstrate the applicability of \textsc{xrade} to the physical interpretation of the X-ray spectra of the bright quasar PDS 456, which hosts the best-established accretion-disk wind observed to date. We anticipate that our emulation method will be an indispensable tool for the development of high-resolution theoretical models, with the necessary flexibility to be optimized for the next generation micro-calorimeters on board future missions, like \textit{XRISM/resolve} and \textit{Athena/X-IFU}. This tool can also be implemented across a wide variety of X-ray spectral models and beyond. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.13731v1-abstract-full').style.display = 'none'; document.getElementById('2207.13731v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 17 figures, MNRAS accepted for publication</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.15347">arXiv:2206.15347</a> <span> [<a href="https://arxiv.org/pdf/2206.15347">pdf</a>, <a href="https://arxiv.org/format/2206.15347">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202243585">10.1051/0004-6361/202243585 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Warm molecular and ionized gas kinematics in the Type-2 quasar J0945+1737 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Speranza%2C+G">G. Speranza</a>, <a href="/search/astro-ph?searchtype=author&query=Almeida%2C+C+R">C. Ramos Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Acosta-Pulido%2C+J+A">J. A. Acosta-Pulido</a>, <a href="/search/astro-ph?searchtype=author&query=Riffel%2C+R+A">R. A. Riffel</a>, <a href="/search/astro-ph?searchtype=author&query=Tadhunter%2C+C">C. Tadhunter</a>, <a href="/search/astro-ph?searchtype=author&query=Pierce%2C+J+C+S">J. C. S. Pierce</a>, <a href="/search/astro-ph?searchtype=author&query=Rodr%C3%ADguez-Ardila%2C+A">A. Rodr铆guez-Ardila</a>, <a href="/search/astro-ph?searchtype=author&query=Puga%2C+M+C">M. Coloma Puga</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Musiimenta%2C+B">B. Musiimenta</a>, <a href="/search/astro-ph?searchtype=author&query=Alexander%2C+D+M">D. M. Alexander</a>, <a href="/search/astro-ph?searchtype=author&query=Lapi%2C+A">A. Lapi</a>, <a href="/search/astro-ph?searchtype=author&query=Shankar%2C+F">F. Shankar</a>, <a href="/search/astro-ph?searchtype=author&query=Villforth%2C+C">C. Villforth</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2206.15347v1-abstract-short" style="display: inline;"> We analyze Near-Infrared Integral Field Spectrograph (NIFS) observations of the type-2 quasar (QSO2) SDSS J094521.33+173753.2 to investigate its warm molecular and ionized gas kinematics. This QSO2 has a bolometric luminosity of 10$^{45.7}$ erg s$^{-1}$ and a redshift of z = 0.128. The K-band spectra provided by NIFS cover a range of 1.99-2.40 $渭$m where low-ionization (Pa$伪$ and Br$未$), high ioni… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.15347v1-abstract-full').style.display = 'inline'; document.getElementById('2206.15347v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.15347v1-abstract-full" style="display: none;"> We analyze Near-Infrared Integral Field Spectrograph (NIFS) observations of the type-2 quasar (QSO2) SDSS J094521.33+173753.2 to investigate its warm molecular and ionized gas kinematics. This QSO2 has a bolometric luminosity of 10$^{45.7}$ erg s$^{-1}$ and a redshift of z = 0.128. The K-band spectra provided by NIFS cover a range of 1.99-2.40 $渭$m where low-ionization (Pa$伪$ and Br$未$), high ionization ([S XI]$位$1.920 $渭$m and [Si~VI]$位$1.963 $渭$m) and warm molecular lines (from H$_2$ 1-0S(5) to 1-0S(1)) are detected, allowing us to study the multi-phase gas kinematics. Our analysis reveals gas in ordinary rotation in all the emission lines detected and also outflowing gas in the case of the low- and high-ionization emission lines. In the case of the nuclear spectrum, which corresponds to a circular aperture of 0.3\arcsec~(686 pc) in diameter, the warm molecular lines can be characterized using a single Gaussian component of full width at half maximum (FWHM)= 350-400 km s$^{-1}$, while Pa$伪$, Br$未$, and [Si~VI] are best fitted with two blue-shifted Gaussian components of FWHM$\sim$800 and 1700 km s$^{-1}$, in addition to a narrow component of $\sim$300 km s$^{-1}$. We interpret the blue-shifted broad components as outflowing gas, which reaches the highest velocities, of up to $-$840 km s$^{-1}$, in the south-east direction (PA$\sim$125$^{\circ}$), extending up to a distance of $\sim$3.4 kpc from the nucleus. The ionized outflow has a maximum mass outflow rate of $\dot{\text{M}}_{\text{out, max}}$=42-51 M$_\odot$ yr$^{-1}$, and its kinetic power represents 0.1$\%$ of the quasar bolometric luminosity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.15347v1-abstract-full').style.display = 'none'; document.getElementById('2206.15347v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, 20 figures and 5 tables. Accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 665, A55 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.03508">arXiv:2206.03508</a> <span> [<a href="https://arxiv.org/pdf/2206.03508">pdf</a>, <a href="https://arxiv.org/format/2206.03508">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202243708">10.1051/0004-6361/202243708 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Supermassive Black Holes at High Redshift are Expected to be Obscured by their Massive Host Galaxies' Inter Stellar Medium </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">R. Gilli</a>, <a href="/search/astro-ph?searchtype=author&query=Norman%2C+C">C. Norman</a>, <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">F. Calura</a>, <a href="/search/astro-ph?searchtype=author&query=Vito%2C+F">F. Vito</a>, <a href="/search/astro-ph?searchtype=author&query=Decarli%2C+R">R. Decarli</a>, <a href="/search/astro-ph?searchtype=author&query=Marchesi%2C+S">S. Marchesi</a>, <a href="/search/astro-ph?searchtype=author&query=Iwasawa%2C+K">K. Iwasawa</a>, <a href="/search/astro-ph?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzuisi%2C+G">G. Lanzuisi</a>, <a href="/search/astro-ph?searchtype=author&query=Pozzi%2C+F">F. Pozzi</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Amato%2C+Q">Q. D'Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Vignali%2C+C">C. Vignali</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Mignoli%2C+M">M. Mignoli</a>, <a href="/search/astro-ph?searchtype=author&query=Cox%2C+P">P. Cox</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2206.03508v3-abstract-short" style="display: inline;"> We combine results from deep ALMA observations of massive ($M_*>10^{10}\;M_{\odot}$) galaxies at different redshifts to show that the column density of their inter stellar medium (ISM) rapidly increases towards early cosmic epochs. Our analysis includes objects from the ASPECS and ALPINE large programs, as well as individual observations of $z\sim 6$ QSO hosts. When accounting for non-detections a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.03508v3-abstract-full').style.display = 'inline'; document.getElementById('2206.03508v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.03508v3-abstract-full" style="display: none;"> We combine results from deep ALMA observations of massive ($M_*>10^{10}\;M_{\odot}$) galaxies at different redshifts to show that the column density of their inter stellar medium (ISM) rapidly increases towards early cosmic epochs. Our analysis includes objects from the ASPECS and ALPINE large programs, as well as individual observations of $z\sim 6$ QSO hosts. When accounting for non-detections and correcting for selection effects, we find that the median surface density of the ISM of the massive galaxy population evolves as $\sim(1+z)^{3.3}$. This means that the ISM column density towards the nucleus of a $z>3$ galaxy is typically $>100$ times larger than locally, and it may reach values as high as Compton-thick at $z\gtrsim6$. Remarkably, the median ISM column density is of the same order of what is measured from X-ray observations of large AGN samples already at $z\gtrsim2$. We develop a simple analytic model for the spatial distribution of ISM clouds within galaxies, and estimate the total covering factor towards active nuclei when obscuration by ISM clouds on the host scale is added to that of pc-scale circumnuclear material (the so-called 'torus'). The model includes clouds with a distribution of sizes, masses, and surface densities, and also allows for an evolution of the characteristic cloud surface density with redshift, $危_{c,*}\propto(1+z)^纬$. We show that, for $纬=2$, such a model successfully reproduces the increase of the obscured AGN fraction with redshift that is commonly observed in deep X-ray surveys, both when different absorption thresholds and AGN luminosities are considered. Our results suggest that 80-90\% of supermassive black holes in the early Universe ($z>6-8$) are hidden to our view, primarily by the ISM in their hosts. [abridged] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.03508v3-abstract-full').style.display = 'none'; document.getElementById('2206.03508v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 15 figures, accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 666, A17 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2202.09430">arXiv:2202.09430</a> <span> [<a href="https://arxiv.org/pdf/2202.09430">pdf</a>, <a href="https://arxiv.org/format/2202.09430">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202243362">10.1051/0004-6361/202243362 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The eROSITA extragalactic CalPV serendipitous catalog </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Liu%2C+T">Teng Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Merloni%2C+A">Andrea Merloni</a>, <a href="/search/astro-ph?searchtype=author&query=Wolf%2C+J">Julien Wolf</a>, <a href="/search/astro-ph?searchtype=author&query=Salvato%2C+M">Mara Salvato</a>, <a href="/search/astro-ph?searchtype=author&query=Reiprich%2C+T">Thomas Reiprich</a>, <a href="/search/astro-ph?searchtype=author&query=Arcodia%2C+R">Riccardo Arcodia</a>, <a href="/search/astro-ph?searchtype=author&query=Lamer%2C+G">Georg Lamer</a>, <a href="/search/astro-ph?searchtype=author&query=Georgakakis%2C+A">Antonis Georgakakis</a>, <a href="/search/astro-ph?searchtype=author&query=Dwelly%2C+T">Tom Dwelly</a>, <a href="/search/astro-ph?searchtype=author&query=Sanders%2C+J">Jeremy Sanders</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+J">Johannes Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Haberl%2C+F">Frank Haberl</a>, <a href="/search/astro-ph?searchtype=author&query=Ramos-Ceja%2C+M">Miriam Ramos-Ceja</a>, <a href="/search/astro-ph?searchtype=author&query=Wilms%2C+J">Joern Wilms</a>, <a href="/search/astro-ph?searchtype=author&query=Nandra%2C+K">Kirpal Nandra</a>, <a href="/search/astro-ph?searchtype=author&query=Brunner%2C+H">Hermann Brunner</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">Marcella Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Schwope%2C+A">Axel Schwope</a>, <a href="/search/astro-ph?searchtype=author&query=Robrade%2C+J">Jan Robrade</a>, <a href="/search/astro-ph?searchtype=author&query=Freyberg%2C+M+J">Michael J. Freyberg</a>, <a href="/search/astro-ph?searchtype=author&query=Boller%2C+T">Thomas Boller</a>, <a href="/search/astro-ph?searchtype=author&query=Maitra%2C+C">Chandreyee Maitra</a>, <a href="/search/astro-ph?searchtype=author&query=Veronica%2C+A">Angie Veronica</a>, <a href="/search/astro-ph?searchtype=author&query=Malyali%2C+A">Adam Malyali</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2202.09430v2-abstract-short" style="display: inline;"> The eROSITA X-ray telescope on board the Spectrum-Roentgen-Gamma (SRG) observatory performed calibration and performance verification (CalPV) observations between September 2019 and December 2019, ahead of the planned four-year all-sky surveys. Most of them were deep, pointing-mode observations. We present here the X-ray catalog detected from the set of extra-galactic CalPV observations released t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.09430v2-abstract-full').style.display = 'inline'; document.getElementById('2202.09430v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.09430v2-abstract-full" style="display: none;"> The eROSITA X-ray telescope on board the Spectrum-Roentgen-Gamma (SRG) observatory performed calibration and performance verification (CalPV) observations between September 2019 and December 2019, ahead of the planned four-year all-sky surveys. Most of them were deep, pointing-mode observations. We present here the X-ray catalog detected from the set of extra-galactic CalPV observations released to the public by the German eROSITA consortium, and the multiband counterparts of these X-ray sources. We developed a source detection method optimized for point-like X-ray sources by including extended X-ray emission in the background measurement. The multiband counterparts were identified using a Bayesian method from the CatWISE catalog. Combining 11 CalPV fields, we present a catalog containing 9515 X-ray sources, whose X-ray fluxes were measured through spectral fitting. CatWISE counterparts are presented for 77% of the sources. Significant variabilities are found in 99 of the sources, which are also presented with this paper. Most of these fields show similar number counts of point sources as typical extragalactic fields, and a few harbor particular stellar populations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.09430v2-abstract-full').style.display = 'none'; document.getElementById('2202.09430v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">to be published in A&A, 23 pages, 14 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 664, A126 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2112.02026">arXiv:2112.02026</a> <span> [<a href="https://arxiv.org/pdf/2112.02026">pdf</a>, <a href="https://arxiv.org/format/2112.02026">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4365/ac4414">10.3847/1538-4365/ac4414 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Seventeenth Data Release of the Sloan Digital Sky Surveys: Complete Release of MaNGA, MaStar and APOGEE-2 Data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abdurro%27uf"> Abdurro'uf</a>, <a href="/search/astro-ph?searchtype=author&query=Accetta%2C+K">Katherine Accetta</a>, <a href="/search/astro-ph?searchtype=author&query=Aerts%2C+C">Conny Aerts</a>, <a href="/search/astro-ph?searchtype=author&query=Aguirre%2C+V+S">Victor Silva Aguirre</a>, <a href="/search/astro-ph?searchtype=author&query=Ahumada%2C+R">Romina Ahumada</a>, <a href="/search/astro-ph?searchtype=author&query=Ajgaonkar%2C+N">Nikhil Ajgaonkar</a>, <a href="/search/astro-ph?searchtype=author&query=Ak%2C+N+F">N. Filiz Ak</a>, <a href="/search/astro-ph?searchtype=author&query=Alam%2C+S">Shadab Alam</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+C+A">Carlos Allende Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Almeida%2C+A">Andres Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Anders%2C+F">Friedrich Anders</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+S+F">Scott F. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Andrews%2C+B+H">Brett H. Andrews</a>, <a href="/search/astro-ph?searchtype=author&query=Anguiano%2C+B">Borja Anguiano</a>, <a href="/search/astro-ph?searchtype=author&query=Aquino-Ortiz%2C+E">Erik Aquino-Ortiz</a>, <a href="/search/astro-ph?searchtype=author&query=Aragon-Salamanca%2C+A">Alfonso Aragon-Salamanca</a>, <a href="/search/astro-ph?searchtype=author&query=Argudo-Fernandez%2C+M">Maria Argudo-Fernandez</a>, <a href="/search/astro-ph?searchtype=author&query=Ata%2C+M">Metin Ata</a>, <a href="/search/astro-ph?searchtype=author&query=Aubert%2C+M">Marie Aubert</a>, <a href="/search/astro-ph?searchtype=author&query=Avila-Reese%2C+V">Vladimir Avila-Reese</a>, <a href="/search/astro-ph?searchtype=author&query=Badenes%2C+C">Carles Badenes</a>, <a href="/search/astro-ph?searchtype=author&query=Barba%2C+R+H">Rodolfo H. Barba</a>, <a href="/search/astro-ph?searchtype=author&query=Barger%2C+K">Kat Barger</a>, <a href="/search/astro-ph?searchtype=author&query=Barrera-Ballesteros%2C+J+K">Jorge K. Barrera-Ballesteros</a>, <a href="/search/astro-ph?searchtype=author&query=Beaton%2C+R+L">Rachael L. Beaton</a> , et al. (316 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2112.02026v2-abstract-short" style="display: inline;"> This paper documents the seventeenth data release (DR17) from the Sloan Digital Sky Surveys; the fifth and final release from the fourth phase (SDSS-IV). DR17 contains the complete release of the Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey, which reached its goal of surveying over 10,000 nearby galaxies. The complete release of the MaNGA Stellar Library (MaStar) accompanies… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.02026v2-abstract-full').style.display = 'inline'; document.getElementById('2112.02026v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.02026v2-abstract-full" style="display: none;"> This paper documents the seventeenth data release (DR17) from the Sloan Digital Sky Surveys; the fifth and final release from the fourth phase (SDSS-IV). DR17 contains the complete release of the Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey, which reached its goal of surveying over 10,000 nearby galaxies. The complete release of the MaNGA Stellar Library (MaStar) accompanies this data, providing observations of almost 30,000 stars through the MaNGA instrument during bright time. DR17 also contains the complete release of the Apache Point Observatory Galactic Evolution Experiment 2 (APOGEE-2) survey which publicly releases infra-red spectra of over 650,000 stars. The main sample from the Extended Baryon Oscillation Spectroscopic Survey (eBOSS), as well as the sub-survey Time Domain Spectroscopic Survey (TDSS) data were fully released in DR16. New single-fiber optical spectroscopy released in DR17 is from the SPectroscipic IDentification of ERosita Survey (SPIDERS) sub-survey and the eBOSS-RM program. Along with the primary data sets, DR17 includes 25 new or updated Value Added Catalogs (VACs). This paper concludes the release of SDSS-IV survey data. SDSS continues into its fifth phase with observations already underway for the Milky Way Mapper (MWM), Local Volume Mapper (LVM) and Black Hole Mapper (BHM) surveys. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.02026v2-abstract-full').style.display = 'none'; document.getElementById('2112.02026v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">40 pages, 8 figures, 6 tables. In press at ApJSS (arxiv v2 corrects some minor typos and updates references)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2110.09544">arXiv:2110.09544</a> <span> [<a href="https://arxiv.org/pdf/2110.09544">pdf</a>, <a href="https://arxiv.org/format/2110.09544">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202142460">10.1051/0004-6361/202142460 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The eROSITA Final Equatorial-Depth Survey (eFEDS): Galaxy Clusters and Groups in Disguise </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bulbul%2C+E">Esra Bulbul</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+A">Ang Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Pasini%2C+T">Thomas Pasini</a>, <a href="/search/astro-ph?searchtype=author&query=Comparat%2C+J">Johan Comparat</a>, <a href="/search/astro-ph?searchtype=author&query=Hoang%2C+D">Duy Hoang</a>, <a href="/search/astro-ph?searchtype=author&query=Klein%2C+M">Matthias Klein</a>, <a href="/search/astro-ph?searchtype=author&query=Ghirardini%2C+V">Vittorio Ghirardini</a>, <a href="/search/astro-ph?searchtype=author&query=Salvato%2C+M">Mara Salvato</a>, <a href="/search/astro-ph?searchtype=author&query=Merloni%2C+A">Andrea Merloni</a>, <a href="/search/astro-ph?searchtype=author&query=Seppi%2C+R">Riccardo Seppi</a>, <a href="/search/astro-ph?searchtype=author&query=Wolf%2C+J">Julien Wolf</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+S+F">Scott F. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Bahar%2C+Y+E">Y. Emre Bahar</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">Marcella Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Brueggen%2C+M">Marcus Brueggen</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+J">Johannes Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Dwelly%2C+T">Tom Dwelly</a>, <a href="/search/astro-ph?searchtype=author&query=Ibarra-Medel%2C+H">Hector Ibarra-Medel</a>, <a href="/search/astro-ph?searchtype=author&query=Chitham%2C+J+I">Jacob Ider Chitham</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+T">Teng Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Nandra%2C+K">Kirpal Nandra</a>, <a href="/search/astro-ph?searchtype=author&query=Ramos-Ceja%2C+M+E">Miriam E. Ramos-Ceja</a>, <a href="/search/astro-ph?searchtype=author&query=Sanders%2C+J+S">Jeremy S. Sanders</a>, <a href="/search/astro-ph?searchtype=author&query=Shen%2C+Y">Yue Shen</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2110.09544v2-abstract-short" style="display: inline;"> The eROSITA Final Equatorial-Depth Survey (eFEDS), executed during the performance verification phase of the Spectrum-Roentgen-Gamma (SRG)/eROSITA telescope, was completed in Nov. 2019. One of the science goals of this survey is to demonstrate the ability of eROSITA to detect samples of clusters and groups at the final depth of the eROSITA all-sky survey. Because of the sizeable point-spread funct… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.09544v2-abstract-full').style.display = 'inline'; document.getElementById('2110.09544v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.09544v2-abstract-full" style="display: none;"> The eROSITA Final Equatorial-Depth Survey (eFEDS), executed during the performance verification phase of the Spectrum-Roentgen-Gamma (SRG)/eROSITA telescope, was completed in Nov. 2019. One of the science goals of this survey is to demonstrate the ability of eROSITA to detect samples of clusters and groups at the final depth of the eROSITA all-sky survey. Because of the sizeable point-spread function of eROSITA, high-redshift clusters of galaxies or compact nearby groups hosting bright active galactic nuclei (AGN) can be misclassified as point sources by the source detection algorithms. A total of 346 galaxy clusters and groups in the redshift range of 0.1<z<1.3 were identified based on their red sequence in the point source catalog. We examine the multiwavelength properties of these clusters and groups to understand the potential biases in our selection process and the completeness of the extent-selected sample. The majority of the clusters and groups in the point source sample are indeed underluminous and compact compared to the extent-selected sample. Their faint X-ray emission, well below the flux limit of the extent-selected eFEDS clusters, and their compact X-ray emission are likely to be the main reason for this misclassification. In the sample, we confirm that 10% of the sources host AGN in their brightest cluster galaxies (BCGs) through optical spectroscopy and visual inspection. By studying their X-ray, optical, infrared, and radio properties, we establish a method for identifying clusters and groups that host AGN in their BCGs. We successfully test this method on the current point source catalog through the Sloan Digital Sky Survey optical spectroscopy and find eight clusters and groups with active radio-loud AGN that are particularly bright in the infrared. They include eFEDSJ091437.8+024558, eFEDSJ083520.1+012516, and eFEDSJ092227.1+043339 at redshifts 0.3-0.4. [ABRIDGED] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.09544v2-abstract-full').style.display = 'none'; document.getElementById('2110.09544v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">31 pages, 13 figures, 3 tables. Accepted for publication in A&A for the Special Issue: The Early Data Release of eROSITA and Mikhail Pavlinsky ART-XC on the SRG Mission</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 661, A10 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.08162">arXiv:2109.08162</a> <span> [<a href="https://arxiv.org/pdf/2109.08162">pdf</a>, <a href="https://arxiv.org/format/2109.08162">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202141416">10.1051/0004-6361/202141416 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Redshift identification of X-ray selected active galactic nuclei in the J1030 field: searching for large-scale structures and high-redshift sources </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Marchesi%2C+S">Stefano Marchesi</a>, <a href="/search/astro-ph?searchtype=author&query=Mignoli%2C+M">Marco Mignoli</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">Roberto Gilli</a>, <a href="/search/astro-ph?searchtype=author&query=Peca%2C+A">Alessandro Peca</a>, <a href="/search/astro-ph?searchtype=author&query=Bolzonella%2C+M">Micol Bolzonella</a>, <a href="/search/astro-ph?searchtype=author&query=Nanni%2C+R">Riccardo Nanni</a>, <a href="/search/astro-ph?searchtype=author&query=Annunziatella%2C+M">Marianna Annunziatella</a>, <a href="/search/astro-ph?searchtype=author&query=Balmaverde%2C+B">Barbara Balmaverde</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">Marcella Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">Francesco Calura</a>, <a href="/search/astro-ph?searchtype=author&query=Cassar%C3%A0%2C+L+P">Letizia P. Cassar脿</a>, <a href="/search/astro-ph?searchtype=author&query=Chiaberge%2C+M">Marco Chiaberge</a>, <a href="/search/astro-ph?searchtype=author&query=Comastri%2C+A">Andrea Comastri</a>, <a href="/search/astro-ph?searchtype=author&query=Cusano%2C+F">Felice Cusano</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Amato%2C+Q">Quirino D'Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Iwasawa%2C+K">Kazushi Iwasawa</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzuisi%2C+G">Giorgio Lanzuisi</a>, <a href="/search/astro-ph?searchtype=author&query=Marchesini%2C+D">Danilo Marchesini</a>, <a href="/search/astro-ph?searchtype=author&query=Morishita%2C+T">Takahiro Morishita</a>, <a href="/search/astro-ph?searchtype=author&query=Prandoni%2C+I">Isabella Prandoni</a>, <a href="/search/astro-ph?searchtype=author&query=Rossi%2C+A">Andrea Rossi</a>, <a href="/search/astro-ph?searchtype=author&query=Tozzi%2C+P">Paolo Tozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Vignali%2C+C">Cristian Vignali</a>, <a href="/search/astro-ph?searchtype=author&query=Vito%2C+F">Fabio Vito</a>, <a href="/search/astro-ph?searchtype=author&query=Zamorani%2C+G">Giovanni Zamorani</a> , et al. (1 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2109.08162v1-abstract-short" style="display: inline;"> We publicly release the spectroscopic and photometric redshift catalog of the sources detected with Chandra in the field of the $z$=6.3 quasar SDSS J1030+0525. This is currently the fifth deepest X-ray field, and reaches a 0.5-2 keV flux limit $f_{\rm 0.5-2}$=6$\times$10$^{-17}$ erg s$^{-1}$ cm$^{-2}$. By using two independent methods, we measure a photometric redshift for 243 objects, while 123 (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.08162v1-abstract-full').style.display = 'inline'; document.getElementById('2109.08162v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.08162v1-abstract-full" style="display: none;"> We publicly release the spectroscopic and photometric redshift catalog of the sources detected with Chandra in the field of the $z$=6.3 quasar SDSS J1030+0525. This is currently the fifth deepest X-ray field, and reaches a 0.5-2 keV flux limit $f_{\rm 0.5-2}$=6$\times$10$^{-17}$ erg s$^{-1}$ cm$^{-2}$. By using two independent methods, we measure a photometric redshift for 243 objects, while 123 (51%) sources also have a spectroscopic redshift, 110 of which coming from an INAF-Large Binocular Telescope (LBT) Strategic Program. We use the spectroscopic redshifts to determine the quality of the photometric ones, and find it in agreement with that of other X-ray surveys which used a similar number of photometric data-points. In particular, we measure a sample normalized median absolute deviation $蟽_{NMAD}$=1.48||$z_{phot}$-$z_{spec}$||/(1+$z_{spec}$)=0.065. We use these new spectroscopic and photometric redshifts to study the properties of the Chandra J1030 field. We observe several peaks in our spectroscopic redshift distribution between $z$=0.15 and $z$=1.5, and find that the sources in each peak are often distributed across the whole Chandra field of view. This evidence confirms that X-ray selected AGN can efficiently track large-scale structures over physical scales of several Mpc. Finally, we computed the Chandra J1030 $z>$3 number counts: while the spectroscopic completeness at high-redshift of our sample is limited, our results point towards a potential source excess at $z\geq$4, which we plan to either confirm or reject in the near future with dedicated spectroscopic campaigns. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.08162v1-abstract-full').style.display = 'none'; document.getElementById('2109.08162v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 15 figures. Accepted for publication in Astronomy and Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 656, A117 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.14528">arXiv:2106.14528</a> <span> [<a href="https://arxiv.org/pdf/2106.14528">pdf</a>, <a href="https://arxiv.org/format/2106.14528">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202141178">10.1051/0004-6361/202141178 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Establishing the X-ray Source Detection Strategy for eROSITA with Simulations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Liu%2C+T">Teng Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Merloni%2C+A">Andrea Merloni</a>, <a href="/search/astro-ph?searchtype=author&query=Comparat%2C+J">Johan Comparat</a>, <a href="/search/astro-ph?searchtype=author&query=Nandra%2C+K">Kirpal Nandra</a>, <a href="/search/astro-ph?searchtype=author&query=Sanders%2C+J+S">Jeremy S. Sanders</a>, <a href="/search/astro-ph?searchtype=author&query=Lamer%2C+G">Georg Lamer</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+J">Johannes Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Dwelly%2C+T">Tom Dwelly</a>, <a href="/search/astro-ph?searchtype=author&query=Freyberg%2C+M">Michael Freyberg</a>, <a href="/search/astro-ph?searchtype=author&query=Malyali%2C+A">Adam Malyali</a>, <a href="/search/astro-ph?searchtype=author&query=Georgakakis%2C+A">Antonis Georgakakis</a>, <a href="/search/astro-ph?searchtype=author&query=Salvato%2C+M">Mara Salvato</a>, <a href="/search/astro-ph?searchtype=author&query=Brunner%2C+H">Hermann Brunner</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">Marcella Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Klein%2C+M">Matthias Klein</a>, <a href="/search/astro-ph?searchtype=author&query=Ghirardini%2C+V">Vittorio Ghirardini</a>, <a href="/search/astro-ph?searchtype=author&query=Clerc%2C+N">Nicolas Clerc</a>, <a href="/search/astro-ph?searchtype=author&query=Pacaud%2C+F">Florian Pacaud</a>, <a href="/search/astro-ph?searchtype=author&query=Bulbul%2C+E">Esra Bulbul</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+A">Ang Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Schwope%2C+A">Axel Schwope</a>, <a href="/search/astro-ph?searchtype=author&query=Robrade%2C+J">Jan Robrade</a>, <a href="/search/astro-ph?searchtype=author&query=Wilms%2C+J">J枚rn Wilms</a>, <a href="/search/astro-ph?searchtype=author&query=Dauser%2C+T">Thomas Dauser</a>, <a href="/search/astro-ph?searchtype=author&query=Ramos-Ceja%2C+M+E">Miriam E. Ramos-Ceja</a> , et al. (3 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2106.14528v2-abstract-short" style="display: inline;"> The eROSITA X-ray telescope on board the Spectrum-Roentgen-Gamma (SRG) satellite has started to detect new X-ray sources over the full sky at an unprecedented rate. Understanding the performance and selection function of the source detection is important for the subsequent scientific analysis of the eROSITA catalogs. Through simulations, we test and optimize the eROSITA source detection procedures… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.14528v2-abstract-full').style.display = 'inline'; document.getElementById('2106.14528v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.14528v2-abstract-full" style="display: none;"> The eROSITA X-ray telescope on board the Spectrum-Roentgen-Gamma (SRG) satellite has started to detect new X-ray sources over the full sky at an unprecedented rate. Understanding the performance and selection function of the source detection is important for the subsequent scientific analysis of the eROSITA catalogs. Through simulations, we test and optimize the eROSITA source detection procedures, and we characterize the detected catalog quantitatively. Taking the eROSITA Final Equatorial-Depth Survey (eFEDS) as an example, we ran extensive photon-event simulations based on our best knowledge of the instrument characteristics, the background spectrum, and the population of astronomical X-ray sources. We introduce a method of analyzing source detection completeness, purity, and efficiency based on the origin of each photon. According to the source detection efficiency measured in the simulation, we chose a two-pronged strategy to build eROSITA X-ray catalogs, creating a main catalog using only the most sensitive band (0.2-2.3 keV) and an independent hard-band-selected catalog using multiband detection in a range up to 5 keV. Because our mock data are highly representative of the real eFEDS data, we used the mock catalogs to measure the completeness and purity of the eFEDS catalogs as a function of multiple parameters, such as detection likelihood, flux, and luminosity. These measurements provide a basis for choosing the eFEDS catalog selection thresholds. The mock catalogs (available with this paper) can be used to construct the selection function of active galactic nuclei and galaxy clusters. A direct comparison of the output and input mock catalogs also gives rise to a correction curve that converts the raw point-source flux distribution into the intrinsic number counts distribution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.14528v2-abstract-full').style.display = 'none'; document.getElementById('2106.14528v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted by A&A for the Special Issue: The Early Data Release of eROSITA and Mikhail Pavlinsky ART-XC on the SRG Mission</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 661, A27 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.14527">arXiv:2106.14527</a> <span> [<a href="https://arxiv.org/pdf/2106.14527">pdf</a>, <a href="https://arxiv.org/format/2106.14527">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202141547">10.1051/0004-6361/202141547 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The eROSITA Final Equatorial-Depth Survey (eFEDS): A multiwavelength view of WISE mid-infrared galaxies/active galactic nuclei </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Toba%2C+Y">Yoshiki Toba</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+T">Teng Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Urrutia%2C+T">Tanya Urrutia</a>, <a href="/search/astro-ph?searchtype=author&query=Salvato%2C+M">Mara Salvato</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+J">Junyao Li</a>, <a href="/search/astro-ph?searchtype=author&query=Ueda%2C+Y">Yoshihiro Ueda</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">Marcella Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Yutani%2C+N">Naomichi Yutani</a>, <a href="/search/astro-ph?searchtype=author&query=Wada%2C+K">Keiichi Wada</a>, <a href="/search/astro-ph?searchtype=author&query=Nishizawa%2C+A+J">Atsushi J. Nishizawa</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+J">Johannes Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Nagao%2C+T">Tohru Nagao</a>, <a href="/search/astro-ph?searchtype=author&query=Merloni%2C+A">Andrea Merloni</a>, <a href="/search/astro-ph?searchtype=author&query=Akiyama%2C+M">Masayuki Akiyama</a>, <a href="/search/astro-ph?searchtype=author&query=Arcodia%2C+R">Riccardo Arcodia</a>, <a href="/search/astro-ph?searchtype=author&query=Hsieh%2C+B">Bau-Ching Hsieh</a>, <a href="/search/astro-ph?searchtype=author&query=Ichikawa%2C+K">Kohei Ichikawa</a>, <a href="/search/astro-ph?searchtype=author&query=Imanishi%2C+M">Masatoshi Imanishi</a>, <a href="/search/astro-ph?searchtype=author&query=Inoue%2C+K+T">Kaiki T. Inoue</a>, <a href="/search/astro-ph?searchtype=author&query=Kawaguchi%2C+T">Toshihiro Kawaguchi</a>, <a href="/search/astro-ph?searchtype=author&query=Lamer%2C+G">Georg Lamer</a>, <a href="/search/astro-ph?searchtype=author&query=Nandra%2C+K">Kirpal Nandra</a>, <a href="/search/astro-ph?searchtype=author&query=Silverman%2C+J+D">John D. Silverman</a>, <a href="/search/astro-ph?searchtype=author&query=Terashima%2C+Y">Yuichi Terashima</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2106.14527v2-abstract-short" style="display: inline;"> We investigate the physical properties--such as the stellar mass, SFR, IR luminosity, X-ray luminosity, and hydrogen column density--of MIR galaxies and AGN at $z < 4$ in the 140 deg$^2$ field observed by SRG/eROSITA through the eFEDS survey. By cross-matching the WISE 22 $渭$m (W4)-detected sample and the eFEDS X-ray point-source catalog, we find that 692 extragalactic objects are detected by eROS… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.14527v2-abstract-full').style.display = 'inline'; document.getElementById('2106.14527v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.14527v2-abstract-full" style="display: none;"> We investigate the physical properties--such as the stellar mass, SFR, IR luminosity, X-ray luminosity, and hydrogen column density--of MIR galaxies and AGN at $z < 4$ in the 140 deg$^2$ field observed by SRG/eROSITA through the eFEDS survey. By cross-matching the WISE 22 $渭$m (W4)-detected sample and the eFEDS X-ray point-source catalog, we find that 692 extragalactic objects are detected by eROSITA. We have compiled a multiwavelength dataset. We have also performed (i) an X-ray spectral analysis, (ii) SED fitting using X-CIGALE, (iii) 2D image-decomposition analysis using Subaru HSC images, and (iv) optical spectral fitting with QSFit to investigate the AGN and host-galaxy properties. For 7,088 WISE W4 objects that are undetected by eROSITA, we have performed an X-ray stacking analysis to examine the typical physical properties of these X-ray faint and/or probably obscured objects. We find that (i) 82% of the eFEDS-W4 sources are classified as X-ray AGN with $\log\,L_{\rm X} >$ 42 erg s$^{-1}$; (ii) 67% and 24% of the objects have $\log\,(L_{\rm IR}/L_{\odot}) > 12$ and 13, respectively; (iii) the relationship between $L_{\rm X}$ and the 6 $渭$m luminosity is consistent with that reported in previous works; and (iv) the relationship between the Eddington ratio and $N_{\rm H}$ for the eFEDS-W4 sample and a comparison with a model prediction from a galaxy-merger simulation indicates that approximately 5% of the eFEDS-W4 sources in our sample are likely to be in an AGN-feedback phase, in which strong radiation pressure from the AGN blows out the surrounding material from the nuclear region. Thanks to the wide area coverage of eFEDS, we have been able to constrain the ranges of the physical properties of the WISE W4 sample of AGNs at $z < 4$, providing a benchmark for forthcoming studies on a complete census of MIR galaxies selected from the full-depth eROSITA all-sky survey. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.14527v2-abstract-full').style.display = 'none'; document.getElementById('2106.14527v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 19 figures, and 3 tables, accepted to appear on A&A, Special Issue: The Early Data Release of eROSITA and Mikhail Pavlinsky ART-XC on the SRG Mission</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 661, A15 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.14525">arXiv:2106.14525</a> <span> [<a href="https://arxiv.org/pdf/2106.14525">pdf</a>, <a href="https://arxiv.org/format/2106.14525">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202141092">10.1051/0004-6361/202141092 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The eROSITA Final Equatorial-Depth Survey (eFEDS): The first archetypal Quasar in the feedback phase discovered by eROSITA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Urrutia%2C+T">T. Urrutia</a>, <a href="/search/astro-ph?searchtype=author&query=Toba%2C+Y">Y. Toba</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+J">J. Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+J+-">J. -Y. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+T">T. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Perna%2C+M">M. Perna</a>, <a href="/search/astro-ph?searchtype=author&query=Salvato%2C+M">M. Salvato</a>, <a href="/search/astro-ph?searchtype=author&query=Merloni%2C+A">A. Merloni</a>, <a href="/search/astro-ph?searchtype=author&query=Musiimenta%2C+B">B. Musiimenta</a>, <a href="/search/astro-ph?searchtype=author&query=Nandra%2C+K">K. Nandra</a>, <a href="/search/astro-ph?searchtype=author&query=Wolf%2C+J">J. Wolf</a>, <a href="/search/astro-ph?searchtype=author&query=Arcodia%2C+R">R. Arcodia</a>, <a href="/search/astro-ph?searchtype=author&query=Dwelly%2C+T">T. Dwelly</a>, <a href="/search/astro-ph?searchtype=author&query=Georgakakis%2C+A">A. Georgakakis</a>, <a href="/search/astro-ph?searchtype=author&query=Goulding%2C+A">A. Goulding</a>, <a href="/search/astro-ph?searchtype=author&query=Matsuoka%2C+Y">Y. Matsuoka</a>, <a href="/search/astro-ph?searchtype=author&query=Nagao%2C+T">T. Nagao</a>, <a href="/search/astro-ph?searchtype=author&query=Schramm%2C+M">M. Schramm</a>, <a href="/search/astro-ph?searchtype=author&query=Silverman%2C+J+D">J. D. Silverman</a>, <a href="/search/astro-ph?searchtype=author&query=Terashima%2C+Y">Y. Terashima</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2106.14525v1-abstract-short" style="display: inline;"> Theoretical models of galaxy-AGN co-evolution ascribe an important role for the feedback process to a short, luminous, obscured, and dust-enshrouded phase during which the accretion rate of the SMBH is expected to be at its maximum and the associated AGN-driven winds are also predicted to be maximally developed. To test this scenario, we have isolated a text-book candidate from the eROSITA Final E… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.14525v1-abstract-full').style.display = 'inline'; document.getElementById('2106.14525v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.14525v1-abstract-full" style="display: none;"> Theoretical models of galaxy-AGN co-evolution ascribe an important role for the feedback process to a short, luminous, obscured, and dust-enshrouded phase during which the accretion rate of the SMBH is expected to be at its maximum and the associated AGN-driven winds are also predicted to be maximally developed. To test this scenario, we have isolated a text-book candidate from the eROSITA Final Equatorial-Depth Survey (eFEDS) obtained within the Performance and Verification program of the eROSITA telescope on board Spectrum Roentgen Gamma. From an initial catalog of 246 hard X-ray selected sources matched with the photometric and spectroscopic information available within the eROSITA and Hyper Suprime-Cam consortia, three candidates Quasars in the feedback phase have been isolated applying the diagnostic proposed in Brusa et al. (2015). Only one source (eFEDSU J091157.5+014327) has a spectrum already available (from SDSS-DR16, z=0.603) and it unambiguously shows the presence of a broad component (FWHM~1650 km/s) in the [OIII]5007 line. The associated observed L_[OIII] is ~2.6x10^{42} erg/s, one to two orders of magnitude larger than that observed in local Seyferts and comparable to those observed in a sample of z~0.5 Type 1 Quasars. From the multiwavelength data available we derive an Eddington Ratio (L_bol/L_Edd) of ~0.25, and a bolometric correction in the hard X-ray of k_bol~10, lower than those observed for objects at similar bolometric luminosity. The presence of an outflow, the high X-ray luminosity and moderate X-ray obscuration (L_X~10^44.8 erg/s, N_H~2.7x10^22 cm^-2) and the red optical color, all match the prediction of quasars in the feedback phase from merger driven models. Forecasting to the full eROSITA all-sky survey with its spectroscopic follow-up, we predict that by the end of 2024 we will have a sample of few hundreds such objects at z=0.5-2. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.14525v1-abstract-full').style.display = 'none'; document.getElementById('2106.14525v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 6 figures, 2 tables. Resubmitted to A&A for the Special Issue: "The Early Data Release of eROSITA and Mikhail Pavlinsky ART-XC on the SRG Mission"</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 661, A9 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.14522">arXiv:2106.14522</a> <span> [<a href="https://arxiv.org/pdf/2106.14522">pdf</a>, <a href="https://arxiv.org/format/2106.14522">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202141643">10.1051/0004-6361/202141643 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The eROSITA Final Equatorial-Depth Survey (eFEDS): The AGN Catalogue and its X-ray Spectral Properties </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Liu%2C+T">Teng Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+J">Johannes Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Nandra%2C+K">Kirpal Nandra</a>, <a href="/search/astro-ph?searchtype=author&query=Merloni%2C+A">Andrea Merloni</a>, <a href="/search/astro-ph?searchtype=author&query=Dwelly%2C+T">Tom Dwelly</a>, <a href="/search/astro-ph?searchtype=author&query=Sanders%2C+J+S">Jeremy S. Sanders</a>, <a href="/search/astro-ph?searchtype=author&query=Salvato%2C+M">Mara Salvato</a>, <a href="/search/astro-ph?searchtype=author&query=Arcodia%2C+R">Riccardo Arcodia</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">Marcella Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Wolf%2C+J">Julien Wolf</a>, <a href="/search/astro-ph?searchtype=author&query=Georgakakis%2C+A">Antonis Georgakakis</a>, <a href="/search/astro-ph?searchtype=author&query=Boller%2C+T">Thomas Boller</a>, <a href="/search/astro-ph?searchtype=author&query=Krumpe%2C+M">Mirko Krumpe</a>, <a href="/search/astro-ph?searchtype=author&query=Lamer%2C+G">Georg Lamer</a>, <a href="/search/astro-ph?searchtype=author&query=Waddell%2C+S">Sophia Waddell</a>, <a href="/search/astro-ph?searchtype=author&query=Urrutia%2C+T">Tanya Urrutia</a>, <a href="/search/astro-ph?searchtype=author&query=Schwope%2C+A">Axel Schwope</a>, <a href="/search/astro-ph?searchtype=author&query=Robrade%2C+J">Jan Robrade</a>, <a href="/search/astro-ph?searchtype=author&query=Wilms%2C+J">J枚rn Wilms</a>, <a href="/search/astro-ph?searchtype=author&query=Dauser%2C+T">Thomas Dauser</a>, <a href="/search/astro-ph?searchtype=author&query=Comparat%2C+J">Johan Comparat</a>, <a href="/search/astro-ph?searchtype=author&query=Toba%2C+Y">Yoshiki Toba</a>, <a href="/search/astro-ph?searchtype=author&query=Ichikawa%2C+K">Kohei Ichikawa</a>, <a href="/search/astro-ph?searchtype=author&query=Iwasawa%2C+K">Kazushi Iwasawa</a>, <a href="/search/astro-ph?searchtype=author&query=Shen%2C+Y">Yue Shen</a> , et al. (1 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2106.14522v1-abstract-short" style="display: inline;"> Context: After the successful launch of the Spectrum-Roentgen-Gamma (SRG) mission in July 2019, eROSITA, the soft X-ray instrument aboard SRG, performed scanning observations of a large contiguous field, namely the eROSITA Final Equatorial Depth Survey (eFEDS), ahead of the planned four-year all-sky survey. eFEDS yielded a large sample of X-ray sources with very rich multi-band photometric and spe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.14522v1-abstract-full').style.display = 'inline'; document.getElementById('2106.14522v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.14522v1-abstract-full" style="display: none;"> Context: After the successful launch of the Spectrum-Roentgen-Gamma (SRG) mission in July 2019, eROSITA, the soft X-ray instrument aboard SRG, performed scanning observations of a large contiguous field, namely the eROSITA Final Equatorial Depth Survey (eFEDS), ahead of the planned four-year all-sky survey. eFEDS yielded a large sample of X-ray sources with very rich multi-band photometric and spectroscopic coverage. Aims: We present here the eFEDS Active Galactic Nuclei (AGN) catalog and the eROSITA X-ray spectral properties of the eFEDS sources. Methods: Using a Bayesian method, we perform a systematic X-ray spectral analysis for all eFEDS sources. The appropriate model is chosen based on the source classification and the spectral quality, and, in the case of AGN, including the possibility of intrinsic (rest-frame) absorption and/or soft excess emission. Hierarchical Bayesian modeling (HBM) is used to estimate the spectral parameter distribution of the sample. Results: X-ray spectral properties are presented for all eFEDS X-ray sources. There are 21952 candidate AGN, which comprise 79% of the eFEDS sample. Despite a large number of faint sources with low photon counts, our spectral fitting provides meaningful measurements of fluxes, luminosities, and spectral shapes for a majority of the sources. This AGN catalog is dominated by X-ray unobscured sources, with an obscured (logNH>21.5) fraction of 10% derived by HBM. The power-law slope of the catalog can be described by a Gaussian distribution of 1.94+-0.22. Above a photon counts threshold of 500, nine out of 50 AGN have soft excess detected. For the sources with blue UV to optical color (type-I AGN), the X-ray emission is well correlated with the UV emission with the usual anti-correlation between the X-ray to UV spectral slope 伪_{OX} and the UV luminosity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.14522v1-abstract-full').style.display = 'none'; document.getElementById('2106.14522v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to A&A for the Special Issue: The Early Data Release of eROSITA and Mikhail Pavlinsky ART-XC on the SRG Mission 24 pages, 23 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 661, A5 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.14520">arXiv:2106.14520</a> <span> [<a href="https://arxiv.org/pdf/2106.14520">pdf</a>, <a href="https://arxiv.org/format/2106.14520">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202141631">10.1051/0004-6361/202141631 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The eROSITA Final Equatorial-Depth Survey (eFEDS): Identification and characterization of the counterparts to the point-like sources </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Salvato%2C+M">M. Salvato</a>, <a href="/search/astro-ph?searchtype=author&query=Wolf%2C+J">J. Wolf</a>, <a href="/search/astro-ph?searchtype=author&query=Dwelly%2C+T">T. Dwelly</a>, <a href="/search/astro-ph?searchtype=author&query=Georgakakis%2C+A">A. Georgakakis</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Merloni%2C+A">A. Merloni</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+T">T. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Toba%2C+Y">Y. Toba</a>, <a href="/search/astro-ph?searchtype=author&query=Nandra%2C+K">K. Nandra</a>, <a href="/search/astro-ph?searchtype=author&query=Lamer%2C+G">G. Lamer</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+J">J. Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Schneider%2C+C">C. Schneider</a>, <a href="/search/astro-ph?searchtype=author&query=Freund%2C+S">S. Freund</a>, <a href="/search/astro-ph?searchtype=author&query=Rau%2C+A">A. Rau</a>, <a href="/search/astro-ph?searchtype=author&query=Schwope%2C+A">A. Schwope</a>, <a href="/search/astro-ph?searchtype=author&query=Nishizawa%2C+A">A. Nishizawa</a>, <a href="/search/astro-ph?searchtype=author&query=Klein%2C+M">M. Klein</a>, <a href="/search/astro-ph?searchtype=author&query=Arcodia%2C+R">R. Arcodia</a>, <a href="/search/astro-ph?searchtype=author&query=Comparat%2C+J">J. Comparat</a>, <a href="/search/astro-ph?searchtype=author&query=Musiimenta%2C+B">B. Musiimenta</a>, <a href="/search/astro-ph?searchtype=author&query=Nagao%2C+T">T. Nagao</a>, <a href="/search/astro-ph?searchtype=author&query=Brunner%2C+H">H. Brunner</a>, <a href="/search/astro-ph?searchtype=author&query=Malyali%2C+A">A. Malyali</a>, <a href="/search/astro-ph?searchtype=author&query=Finoguenov%2C+A">A. Finoguenov</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+S">S. Anderson</a> , et al. (19 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2106.14520v2-abstract-short" style="display: inline;"> In November 2019, eROSITA on board of SRG observatory started to map the entire sky in X-rays. After the 4-year survey program, it will reach flux limits about 25 times deeper than ROSAT. During the SRG Performance Verification phase, eROSITA observed a contiguous 140 deg$^2$ area of the sky down to the final depth of the eROSITA all-sky survey ("eROSITA Final Equatorial-Depth Survey": eFEDS), wit… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.14520v2-abstract-full').style.display = 'inline'; document.getElementById('2106.14520v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.14520v2-abstract-full" style="display: none;"> In November 2019, eROSITA on board of SRG observatory started to map the entire sky in X-rays. After the 4-year survey program, it will reach flux limits about 25 times deeper than ROSAT. During the SRG Performance Verification phase, eROSITA observed a contiguous 140 deg$^2$ area of the sky down to the final depth of the eROSITA all-sky survey ("eROSITA Final Equatorial-Depth Survey": eFEDS), with the goal of obtaining a census of the X-ray emitting populations (stars, compact objects, galaxies, clusters of galaxies, AGN) that will be discovered over the entire sky. This paper presents the identification of the counterparts to the point-sources detected in eFEDS in the Main and Hard samples described in Brunner et al 2021, and their multi-wavelength properties, including redshift. For the identification of the counterparts we combined the results from two independent methods (NWAY and ASTROMATCH), trained on the multi-wavelength properties of a sample of 23k XMM-Newton sources detected in the DESI Legacy Imaging Survey DR8. Then spectroscopic redshifts and photometry from ancillary surveys are collated for the computation of photometric redshifts. The eFEDS sources with a reliable counterparts are 24774/27369 (90.5\%) in the Main sample and 231/246 (93.9\%) in the Hard sample, including 2514 (3) sources for which a second counterpart is equally likely. [abridged] This paper is accompanying the eROSITA early data release of all the observations performed during the performance and verification phase. Together with the catalogs of primary and secondary counterparts to the Main and Hard samples of the eFEDS survey this paper releases their multi-wavelength properties and redshifts. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.14520v2-abstract-full').style.display = 'none'; document.getElementById('2106.14520v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted by A&A for the Special Issue: The Early Data Release of eROSITA and Mikhail Pavlinsky ART-XC on the SRG Mission. NOTE: Paper completely revised wrt the first version submitted to arXiv. Revised catalogs available via https://erosita.mpe.mpg.de/edr/eROSITAObservations/Catalogues/</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 661, A3 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.14517">arXiv:2106.14517</a> <span> [<a href="https://arxiv.org/pdf/2106.14517">pdf</a>, <a href="https://arxiv.org/format/2106.14517">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202141266">10.1051/0004-6361/202141266 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The eROSITA Final Equatorial Depth Survey (eFEDS): The X-ray catalog </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Brunner%2C+H">H. Brunner</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+T">T. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Lamer%2C+G">G. Lamer</a>, <a href="/search/astro-ph?searchtype=author&query=Georgakakis%2C+A">A. Georgakakis</a>, <a href="/search/astro-ph?searchtype=author&query=Merloni%2C+A">A. Merloni</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Bulbul%2C+E">E. Bulbul</a>, <a href="/search/astro-ph?searchtype=author&query=Dennerl%2C+K">K. Dennerl</a>, <a href="/search/astro-ph?searchtype=author&query=Friedrich%2C+S">S. Friedrich</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+A">A. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Maitra%2C+C">C. Maitra</a>, <a href="/search/astro-ph?searchtype=author&query=Nandra%2C+K">K. Nandra</a>, <a href="/search/astro-ph?searchtype=author&query=Ramos-Ceja%2C+M+E">M. E. Ramos-Ceja</a>, <a href="/search/astro-ph?searchtype=author&query=Sanders%2C+J+S">J. S. Sanders</a>, <a href="/search/astro-ph?searchtype=author&query=Stewart%2C+I+M">I. M. Stewart</a>, <a href="/search/astro-ph?searchtype=author&query=Boller%2C+T">T. Boller</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+J">J. Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Clerc%2C+N">N. Clerc</a>, <a href="/search/astro-ph?searchtype=author&query=Comparat%2C+J">J. Comparat</a>, <a href="/search/astro-ph?searchtype=author&query=Dwelly%2C+T">T. Dwelly</a>, <a href="/search/astro-ph?searchtype=author&query=Eckert%2C+D">D. Eckert</a>, <a href="/search/astro-ph?searchtype=author&query=Finoguenov%2C+A">A. Finoguenov</a>, <a href="/search/astro-ph?searchtype=author&query=Freyberg%2C+M">M. Freyberg</a>, <a href="/search/astro-ph?searchtype=author&query=Ghirardini%2C+V">V. Ghirardini</a>, <a href="/search/astro-ph?searchtype=author&query=Gueguen%2C+A">A. Gueguen</a> , et al. (13 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2106.14517v2-abstract-short" style="display: inline;"> Context. The eROSITA X-ray telescope on board the Spectrum-Roentgen-Gamma (SRG) observatory combines a large field of view and collecting area in the energy range $\sim$0.2 to $\sim$8.0 keV with the capability to perform uniform scanning observations of large sky areas. Aims. SRG/eROSITA performed scanning observations of the $\sim$140 square degrees eROSITA Final Equatorial Depth Survey (eFEDS)… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.14517v2-abstract-full').style.display = 'inline'; document.getElementById('2106.14517v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.14517v2-abstract-full" style="display: none;"> Context. The eROSITA X-ray telescope on board the Spectrum-Roentgen-Gamma (SRG) observatory combines a large field of view and collecting area in the energy range $\sim$0.2 to $\sim$8.0 keV with the capability to perform uniform scanning observations of large sky areas. Aims. SRG/eROSITA performed scanning observations of the $\sim$140 square degrees eROSITA Final Equatorial Depth Survey (eFEDS) field as part of its performance verification phase. The observing time was chosen to slightly exceed the depth of equatorial fields after the completion of the eROSITA all-sky survey. We present a catalog of detected X-ray sources in the eFEDS field providing source positions and extent information, as well as fluxes in multiple energy bands and document a suite of tools and procedures developed for eROSITA data processing and analysis, validated and optimized by the eFEDS work. Methods. A multi-stage source detection procedure was optimized and calibrated by performing realistic simulations of the eROSITA eFEDS observations. We cross-matched the eROSITA eFEDS source catalog with previous XMM-ATLAS observations, confirming excellent agreement of the eROSITA and XMM-ATLAS source fluxes. Result. We present a primary catalog of 27910 X-ray sources, including 542 with significant spatial extent, detected in the 0.2-2.3 keV energy range with detection likelihoods $\ge 6$, corresponding to a (point source) flux limit of $\approx 6.5 \times 10^{-15}$ erg/cm$^2$/s in the 0.5-2.0 keV energy band (80% completeness). A supplementary catalog contains 4774 low-significance source candidates with detection likelihoods between 5 and 6. In addition, a hard band sample of 246 sources detected in the energy range 2.3-5.0 keV above a detection likelihood of 10 is provided. The dedicated data analysis software package, calibration database, and calibrated data products are described in an appendix. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.14517v2-abstract-full').style.display = 'none'; document.getElementById('2106.14517v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages, 15 figures, accepted, A&A Special Issue: The Early Data Release of eROSITA and Mikhail Pavlinsky ART-XC on the SRG Mission</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2104.02462">arXiv:2104.02462</a> <span> [<a href="https://arxiv.org/pdf/2104.02462">pdf</a>, <a href="https://arxiv.org/format/2104.02462">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202140317">10.1051/0004-6361/202140317 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The eROSITA Final Equatorial-Depth Survey (eFEDS): An X-ray bright, extremely luminous infrared galaxy at z = 1.87 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Toba%2C+Y">Yoshiki Toba</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">Marcella Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+T">Teng Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+J">Johannes Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Terashima%2C+Y">Yuichi Terashima</a>, <a href="/search/astro-ph?searchtype=author&query=Urrutia%2C+T">Tanya Urrutia</a>, <a href="/search/astro-ph?searchtype=author&query=Salvato%2C+M">Mara Salvato</a>, <a href="/search/astro-ph?searchtype=author&query=Akiyama%2C+M">Masayuki Akiyama</a>, <a href="/search/astro-ph?searchtype=author&query=Arcodia%2C+R">Riccardo Arcodia</a>, <a href="/search/astro-ph?searchtype=author&query=Goulding%2C+A+D">Andy D. Goulding</a>, <a href="/search/astro-ph?searchtype=author&query=Higuchi%2C+Y">Yuichi Higuchi</a>, <a href="/search/astro-ph?searchtype=author&query=Inoue%2C+K+T">Kaiki T. Inoue</a>, <a href="/search/astro-ph?searchtype=author&query=Kawaguchi%2C+T">Toshihiro Kawaguchi</a>, <a href="/search/astro-ph?searchtype=author&query=Lamer%2C+G">Georg Lamer</a>, <a href="/search/astro-ph?searchtype=author&query=Merloni%2C+A">Andrea Merloni</a>, <a href="/search/astro-ph?searchtype=author&query=Nagao%2C+T">Tohru Nagao</a>, <a href="/search/astro-ph?searchtype=author&query=Ueda%2C+Y">Yoshihiro Ueda</a>, <a href="/search/astro-ph?searchtype=author&query=Nandra%2C+K">Kirpal Nandra</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2104.02462v1-abstract-short" style="display: inline;"> In this study, we investigate the X-ray properties of WISE J090924.01+000211.1 (WISEJ0909+0002), an extremely luminous infrared (IR) galaxy (ELIRG) at $z_{\rm spec}$= 1.871 in the eROSITA final equatorial depth survey (eFEDS). WISEJ0909+0002 is a WISE 22 $渭$m source, located in the GAMA-09 field, detected by eROSITA during the performance and verification phase. The corresponding optical spectrum… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.02462v1-abstract-full').style.display = 'inline'; document.getElementById('2104.02462v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2104.02462v1-abstract-full" style="display: none;"> In this study, we investigate the X-ray properties of WISE J090924.01+000211.1 (WISEJ0909+0002), an extremely luminous infrared (IR) galaxy (ELIRG) at $z_{\rm spec}$= 1.871 in the eROSITA final equatorial depth survey (eFEDS). WISEJ0909+0002 is a WISE 22 $渭$m source, located in the GAMA-09 field, detected by eROSITA during the performance and verification phase. The corresponding optical spectrum indicates that this object is a type-1 active galactic nucleus (AGN). Observations from eROSITA combined with Chandra and XMM-Newton archival data indicate a very luminous ($L$ (2--10 keV) = ($2.1 \pm 0.2) \times 10^{45}$ erg s$^{-1}$) unobscured AGN with a power-law photon index of $螕$ = 1.73$_{-0.15}^{+0.16}$, and an absorption hydrogen column density of $\log\,(N_{\rm H}/{\rm cm}^{-2}) < 21.0$. The IR luminosity was estimated to be $L_{\rm IR}$ = (1.79 $\pm$ 0.09) $\times 10^{14}\, L_{\odot}$ from spectral energy distribution modeling based on 22 photometric data (X-ray to far-IR) with X-CIGALE, which confirmed that WISEJ0909+0002 is an ELIRG. A remarkably high $L_{\rm IR}$ despite very low $N_{\rm H}$ would indicate that we are witnessing a short-lived phase in which hydrogen gas along the line of sight is blown outwards, whereas warm and hot dust heated by AGNs still exist. As a consequence of eROSITA all-sky survey, $6.8_{-5.6}^{+16}\times 10^2$ such X-ray bright ELIRGs are expected to be discovered in the entire extragalactic sky ($|b| > 10^\circ$). This can potentially be the key population to constrain the bright-end of IR luminosity functions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.02462v1-abstract-full').style.display = 'none'; document.getElementById('2104.02462v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 5 figures, and 3 tables, accepted for publication in A&A Letters (special Issue: First science highlights from SRG/eROSITA)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 649, L11 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2103.06901">arXiv:2103.06901</a> <span> [<a href="https://arxiv.org/pdf/2103.06901">pdf</a>, <a href="https://arxiv.org/format/2103.06901">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202140399">10.1051/0004-6361/202140399 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Chandra and Magellan/FIRE follow-up observations of PSO167-13: an X-ray weak QSO at $z=6.515$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vito%2C+F">Fabio Vito</a>, <a href="/search/astro-ph?searchtype=author&query=Brandt%2C+W+N">William Nielsen Brandt</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">Federica Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Congiu%2C+E">Enrico Congiu</a>, <a href="/search/astro-ph?searchtype=author&query=Connor%2C+T">Thomas Connor</a>, <a href="/search/astro-ph?searchtype=author&query=Ba%C3%B1ados%2C+E">Eduardo Ba帽ados</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">Franz Erik Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">Roberto Gilli</a>, <a href="/search/astro-ph?searchtype=author&query=Luo%2C+B">Bin Luo</a>, <a href="/search/astro-ph?searchtype=author&query=Mazzucchelli%2C+C">Chiara Mazzucchelli</a>, <a href="/search/astro-ph?searchtype=author&query=Mignoli%2C+M">Marco Mignoli</a>, <a href="/search/astro-ph?searchtype=author&query=Shemmer%2C+O">Ohad Shemmer</a>, <a href="/search/astro-ph?searchtype=author&query=Vignali%2C+C">Cristian Vignali</a>, <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">Francesco Calura</a>, <a href="/search/astro-ph?searchtype=author&query=Comastri%2C+A">Andrea Comastri</a>, <a href="/search/astro-ph?searchtype=author&query=Decarli%2C+R">Roberto Decarli</a>, <a href="/search/astro-ph?searchtype=author&query=Gallerani%2C+S">Simona Gallerani</a>, <a href="/search/astro-ph?searchtype=author&query=Nanni%2C+R">Riccardo Nanni</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">Marcella Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Cappelluti%2C+N">Nico Cappelluti</a>, <a href="/search/astro-ph?searchtype=author&query=Civano%2C+F">Francesca Civano</a>, <a href="/search/astro-ph?searchtype=author&query=Zamorani%2C+G">Gianni Zamorani</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2103.06901v1-abstract-short" style="display: inline;"> The discovery of hundreds of QSOs in the first Gyr of the Universe powered by already grown SMBHs challenges our knowledge of SMBH formation. In particular, investigations of $z>6$ QSOs presenting notable properties can provide unique information on the physics of fast SMBH growth in the early universe. We present the results of follow-up observations of the $z=6.515$ radio-quiet QSO PSO167-13, wh… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.06901v1-abstract-full').style.display = 'inline'; document.getElementById('2103.06901v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.06901v1-abstract-full" style="display: none;"> The discovery of hundreds of QSOs in the first Gyr of the Universe powered by already grown SMBHs challenges our knowledge of SMBH formation. In particular, investigations of $z>6$ QSOs presenting notable properties can provide unique information on the physics of fast SMBH growth in the early universe. We present the results of follow-up observations of the $z=6.515$ radio-quiet QSO PSO167-13, which is interacting with a close companion galaxy. The PSO167-13 system has been recently proposed to host the first heavily obscured X-ray source at high redshift. We observed PSO167-13 with Chandra/ACIS-S (177 ks), and obtained new spectroscopic observations (7.2 h) with Magellan/FIRE. No significant X-ray emission is detected from the PSO167-13 system, suggesting that the obscured X-ray source previously tentatively detected was either due to a strong background fluctuation or is highly variable. The upper limit (90% confidence level) on the X-ray emission of PSO167-13 ($L_{2-10\,\mathrm{keV}}<8.3\times10^{43}\,\mathrm{erg s^{-1}}$) is the lowest available for a $z>6$ QSO. The ratio between the X-ray and UV luminosity of $伪_{ox}<-1.95$ makes PSO167-13 a strong outlier from the $伪_{ox}-L_{UV}$ and $L_X-L_{\mathrm{bol}}$ relations. In particular, its X-ray emission is $>6$ times weaker than the expectation based on its UV luminosity. The new Magellan/FIRE spectrum of PSO167-13 is strongly affected by the unfavorable sky conditions, but the tentatively detected C IV and Mg II emission lines appear strongly blueshifted. The most plausible explanations for the X-ray weakness of PSO167-13 are intrinsic weakness or small-scale absorption by Compton-thick material. The possible strong blueshift of its emission lines hints at the presence of nuclear winds, which could be related to its X-ray weakness. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.06901v1-abstract-full').style.display = 'none'; document.getElementById('2103.06901v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication on A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 649, A133 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2102.07789">arXiv:2102.07789</a> <span> [<a href="https://arxiv.org/pdf/2102.07789">pdf</a>, <a href="https://arxiv.org/format/2102.07789">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202040190">10.1051/0004-6361/202040190 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Connecting X-ray nuclear winds with galaxy-scale ionised outflows in two $z\sim1.5$ lensed quasars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Tozzi%2C+G">G. Tozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Cresci%2C+G">G. Cresci</a>, <a href="/search/astro-ph?searchtype=author&query=Marasco%2C+A">A. Marasco</a>, <a href="/search/astro-ph?searchtype=author&query=Nardini%2C+E">E. Nardini</a>, <a href="/search/astro-ph?searchtype=author&query=Marconi%2C+A">A. Marconi</a>, <a href="/search/astro-ph?searchtype=author&query=Mannucci%2C+F">F. Mannucci</a>, <a href="/search/astro-ph?searchtype=author&query=Chartas%2C+G">G. Chartas</a>, <a href="/search/astro-ph?searchtype=author&query=Rizzo%2C+F">F. Rizzo</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+A">A. Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/astro-ph?searchtype=author&query=Dadina%2C+M">M. Dadina</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzuisi%2C+G">G. Lanzuisi</a>, <a href="/search/astro-ph?searchtype=author&query=Mainieri%2C+V">V. Mainieri</a>, <a href="/search/astro-ph?searchtype=author&query=Mingozzi%2C+M">M. Mingozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Perna%2C+M">M. Perna</a>, <a href="/search/astro-ph?searchtype=author&query=Venturi%2C+G">G. Venturi</a>, <a href="/search/astro-ph?searchtype=author&query=Vignali%2C+C">C. Vignali</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2102.07789v2-abstract-short" style="display: inline;"> Outflows driven by active galactic nuclei (AGN) are expected to have a significant impact on the host galaxy evolution, but it is still debated how they are accelerated and propagate on galaxy-wide scales. This work addresses these questions by studying the link between X-ray, nuclear ultra-fast outflows (UFOs) and extended ionised outflows, for the first time in two quasars close to the peak of A… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.07789v2-abstract-full').style.display = 'inline'; document.getElementById('2102.07789v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2102.07789v2-abstract-full" style="display: none;"> Outflows driven by active galactic nuclei (AGN) are expected to have a significant impact on the host galaxy evolution, but it is still debated how they are accelerated and propagate on galaxy-wide scales. This work addresses these questions by studying the link between X-ray, nuclear ultra-fast outflows (UFOs) and extended ionised outflows, for the first time in two quasars close to the peak of AGN activity ($z\sim2$), where AGN feedback is expected to be more effective. As targets, we selected two multiple-lensed quasars at $z\sim1.5$, HS 0810+2554 and SDSS J1353+1138, known to host UFOs and observed with the near-IR integral field spectrometer SINFONI at the VLT. We performed a kinematical analysis of the [O III]$位$5007 optical emission line, in order to trace the presence of ionised outflows. We detected spatially resolved ionised outflows in both galaxies, extended more than 8 kpc and moving up to $v>2000$ km/s. We derived mass outflow rates of $\sim$12 M$_{sun}$/yr and $\sim$2 M$_{sun}$/yr for HS 0810+2554 and SDSS J1353+1138. Comparing with the co-hosted UFO energetics, the ionised outflow energetics in HS 0810+2554 is broadly consistent with a momentum-driven regime of wind propagation, while in SDSS J1353+1138 it differs by a factor of $\sim$100 from theoretical predictions, requiring either a massive molecular outflow or a high variability of the AGN activity to account for such a discrepancy. By additionally considering our results with those from the small sample of well-studied objects (all local but one), with both UFO and extended (ionised/atomic/molecular) outflow detections, we found that in 10 out of 12 galaxies the large-scale outflow energetics is consistent with the theoretical predictions of either a momentum- or an energy-driven scenario. This suggests that such models explain relatively well the acceleration mechanism of AGN-driven winds on large scales. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.07789v2-abstract-full').style.display = 'none'; document.getElementById('2102.07789v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 9 figures. Accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 648, A99 (2021) </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Brusa%2C+M&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Brusa%2C+M&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Brusa%2C+M&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Brusa%2C+M&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=Brusa%2C+M&start=150" 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