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</div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.04224">arXiv:2412.04224</a> <span> [<a href="https://arxiv.org/pdf/2412.04224">pdf</a>, <a href="https://arxiv.org/format/2412.04224">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"> 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/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/2403.13490">arXiv:2403.13490</a> <span> [<a href="https://arxiv.org/pdf/2403.13490">pdf</a>, <a href="https://arxiv.org/format/2403.13490">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/10.1051/0004-6361/202348996">10.1051/0004-6361/202348996 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The ALPINE-ALMA [CII] Survey: Dust emission effective radius up to 3 kpc in the Early Universe </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pozzi%2C+F">F. Pozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">F. Calura</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=Gavarente%2C+M">M. Gavarente</a>, <a href="/search/astro-ph?searchtype=author&query=Bethermin%2C+M">M. Bethermin</a>, <a href="/search/astro-ph?searchtype=author&query=Boquien%2C+M">M. Boquien</a>, <a href="/search/astro-ph?searchtype=author&query=Casasola%2C+V">V. Casasola</a>, <a href="/search/astro-ph?searchtype=author&query=Cimatti%2C+A">A. Cimatti</a>, <a href="/search/astro-ph?searchtype=author&query=Cochrane%2C+R">R. Cochrane</a>, <a href="/search/astro-ph?searchtype=author&query=Dessauges-Zavadsky%2C+M">M. Dessauges-Zavadsky</a>, <a href="/search/astro-ph?searchtype=author&query=Enia%2C+A">A. Enia</a>, <a href="/search/astro-ph?searchtype=author&query=Esposito%2C+F">F. Esposito</a>, <a href="/search/astro-ph?searchtype=author&query=Faisst%2C+A+L">A. L. Faisst</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">R. Gilli</a>, <a href="/search/astro-ph?searchtype=author&query=Ginolfi%2C+M">M. Ginolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">R. Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Gruppioni%2C+C">C. Gruppioni</a>, <a href="/search/astro-ph?searchtype=author&query=Hayward%2C+C+C">C. C. Hayward</a>, <a href="/search/astro-ph?searchtype=author&query=Ibar%2C+E">E. Ibar</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">A. M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Lemaux%2C+B+C">B. C. Lemaux</a>, <a href="/search/astro-ph?searchtype=author&query=Magdis%2C+G+E">G. E. Magdis</a>, <a href="/search/astro-ph?searchtype=author&query=Molina%2C+J">J. Molina</a>, <a href="/search/astro-ph?searchtype=author&query=Talia%2C+M">M. Talia</a>, <a href="/search/astro-ph?searchtype=author&query=Vallini%2C+L">L. Vallini</a> , et al. (2 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="2403.13490v1-abstract-short" style="display: inline;"> Measurements of the size of dust continuum emission are an important tool for constraining the spatial extent of star formation and hence the build-up of stellar mass. Compact dust emission has generally been observed at Cosmic Noon (z~2-3). However, at earlier epochs, toward the end of the Reionization (z~4-6), only the sizes of a handful of IR-bright galaxies have been measured. In this work, we… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.13490v1-abstract-full').style.display = 'inline'; document.getElementById('2403.13490v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.13490v1-abstract-full" style="display: none;"> Measurements of the size of dust continuum emission are an important tool for constraining the spatial extent of star formation and hence the build-up of stellar mass. Compact dust emission has generally been observed at Cosmic Noon (z~2-3). However, at earlier epochs, toward the end of the Reionization (z~4-6), only the sizes of a handful of IR-bright galaxies have been measured. In this work, we derive the dust emission sizes of main-sequence galaxies at z~5 from the ALPINE survey. We measure the dust effective radius r_e,FIR in the uv-plane in Band 7 of ALMA for seven ALPINE galaxies with resolved emission and we compare it with rest-frame UV and [CII]158$渭$m measurements. We study the r_e,FIR-L_IR scaling relation by considering our dust size measurements and all the data in literature at z~4-6. Finally, we compare our size measurements with predictions from simulations. The dust emission in the selected ALPINE galaxies is rather extended (r_e,FIR~1.5-3 kpc), similar to [CII]158 um but a factor of ~2 larger than the rest-frame UV emission. Putting together all the measurements at z~5, spanning 2 decades in luminosity from L_IR ~ 10^11 L_sun to L_IR ~ 10^13 L_sun, the data highlight a steeply increasing trend of the r_e,FIR-L_IR relation at L_IR< 10^12 L_sun, followed by a downturn and a decreasing trend at brighter luminosities. Finally, simulations that extend up to the stellar masses of the ALPINE galaxies considered in the present work predict a sub-set of galaxies (~25% at 10^10 M_sun < M_star < 10^11 M_sun) with sizes as large as those measured. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.13490v1-abstract-full').style.display = 'none'; document.getElementById('2403.13490v1-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, 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">8 pages, Accepted 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 686, A187 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.12427">arXiv:2402.12427</a> <span> [<a href="https://arxiv.org/pdf/2402.12427">pdf</a>, <a href="https://arxiv.org/format/2402.12427">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/10.1051/0004-6361/202346978">10.1051/0004-6361/202346978 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> GalaPy, the highly optimised C++/Python spectral modelling tool for galaxies -- I. Library presentation and photometric fitting </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ronconi%2C+T">Tommaso Ronconi</a>, <a href="/search/astro-ph?searchtype=author&query=Lapi%2C+A">Andrea Lapi</a>, <a href="/search/astro-ph?searchtype=author&query=Torsello%2C+M">Martina Torsello</a>, <a href="/search/astro-ph?searchtype=author&query=Bressan%2C+A">Alessandro Bressan</a>, <a href="/search/astro-ph?searchtype=author&query=Donevski%2C+D">Darko Donevski</a>, <a href="/search/astro-ph?searchtype=author&query=Pantoni%2C+L">Lara Pantoni</a>, <a href="/search/astro-ph?searchtype=author&query=Behiri%2C+M">Meriem Behiri</a>, <a href="/search/astro-ph?searchtype=author&query=Boco%2C+L">Lumen Boco</a>, <a href="/search/astro-ph?searchtype=author&query=Cimatti%2C+A">Andrea Cimatti</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=Danese%2C+L">Luigi Danese</a>, <a href="/search/astro-ph?searchtype=author&query=Giulietti%2C+M">Marika Giulietti</a>, <a href="/search/astro-ph?searchtype=author&query=Perrotta%2C+F">Francesca Perrotta</a>, <a href="/search/astro-ph?searchtype=author&query=Silva%2C+L">Laura Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Talia%2C+M">Margherita Talia</a>, <a href="/search/astro-ph?searchtype=author&query=Massardi%2C+M">Marcella Massardi</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="2402.12427v1-abstract-short" style="display: inline;"> Fostered by upcoming data from new generation observational campaigns, we are about to enter a new era for the study of how galaxies form and evolve. The unprecedented quantity of data that will be collected, from distances only marginally grasped up to now, will require analysis tools designed to target the specific physical peculiarities of the observed sources and handle extremely large dataset… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.12427v1-abstract-full').style.display = 'inline'; document.getElementById('2402.12427v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.12427v1-abstract-full" style="display: none;"> Fostered by upcoming data from new generation observational campaigns, we are about to enter a new era for the study of how galaxies form and evolve. The unprecedented quantity of data that will be collected, from distances only marginally grasped up to now, will require analysis tools designed to target the specific physical peculiarities of the observed sources and handle extremely large datasets. One powerful method to investigate the complex astrophysical processes that govern the properties of galaxies is to model their observed spectral energy distribution (SED) at different stages of evolution and times throughout the history of the Universe. To address these challenges, we have developed GalaPy, a new library for modelling and fitting SEDs of galaxies from the X-ray to the radio band, as well as the evolution of their components and dust attenuation/reradiation. GalaPy incorporates both empirical and physically-motivated star formation histories, state-of-the-art single stellar population synthesis libraries, a two-component dust model for attenuation, an age-dependent energy conservation algorithm to compute dust reradiation, and additional sources of stellar continuum such as synchrotron, nebular/free-free emission and X-ray radiation from low and high mass binary stars. GalaPy has a hybrid implementation that combines the high performance of compiled C++ with the flexibility of Python, and exploits an object-oriented design. It generates models on the fly without relying on templates, and exploits fully Bayesian parameter space sampling. In this first work, we introduce the project and showcase the photometric SED fitting tools already available to users. The library is available on the Python Package Index (PyPI) and comes with extensive online documentation and tutorials. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.12427v1-abstract-full').style.display = 'none'; document.getElementById('2402.12427v1-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 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">41 pages, 31 figures, 7 tables, to be published on A&A, links to documentation and PyPI available in the PDF, comments are very welcome</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 685, A161 (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/2401.13028">arXiv:2401.13028</a> <span> [<a href="https://arxiv.org/pdf/2401.13028">pdf</a>, <a href="https://arxiv.org/format/2401.13028">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/10.1051/0004-6361/202449240">10.1051/0004-6361/202449240 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> HOMERUN a new approach to photoionization modelling. I -- reproducing observed emission lines with percent accuracy and obtaining accurate physical properties of the ionized gas </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Marconi%2C+A">A. Marconi</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+A">A. Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Feltre%2C+A">A. Feltre</a>, <a href="/search/astro-ph?searchtype=author&query=Belfiore%2C+F">F. Belfiore</a>, <a href="/search/astro-ph?searchtype=author&query=Cresci%2C+G">G. Cresci</a>, <a href="/search/astro-ph?searchtype=author&query=Curti%2C+M">M. Curti</a>, <a href="/search/astro-ph?searchtype=author&query=Mannucci%2C+F">F. Mannucci</a>, <a href="/search/astro-ph?searchtype=author&query=Bertola%2C+E">E. Bertola</a>, <a href="/search/astro-ph?searchtype=author&query=Brazzini%2C+M">M. Brazzini</a>, <a href="/search/astro-ph?searchtype=author&query=Carniani%2C+S">S. Carniani</a>, <a href="/search/astro-ph?searchtype=author&query=Cataldi%2C+E">E. Cataldi</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=de+Rosa%2C+G">G. de Rosa</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Teodoro%2C+E">E. Di Teodoro</a>, <a href="/search/astro-ph?searchtype=author&query=Ginolfi%2C+M">M. Ginolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Kumari%2C+N">N. Kumari</a>, <a href="/search/astro-ph?searchtype=author&query=Marconcini%2C+C">C. Marconcini</a>, <a href="/search/astro-ph?searchtype=author&query=Maiolino%2C+R">R. Maiolino</a>, <a href="/search/astro-ph?searchtype=author&query=Magrini%2C+L">L. Magrini</a>, <a href="/search/astro-ph?searchtype=author&query=Marasco%2C+A">A. Marasco</a>, <a href="/search/astro-ph?searchtype=author&query=Mingozzi%2C+M">M. Mingozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Moreschini%2C+B">B. Moreschini</a>, <a href="/search/astro-ph?searchtype=author&query=Nagao%2C+T">T. Nagao</a>, <a href="/search/astro-ph?searchtype=author&query=Oliva%2C+E">E. Oliva</a>, <a href="/search/astro-ph?searchtype=author&query=Scialpi%2C+M">M. Scialpi</a> , et al. (4 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="2401.13028v2-abstract-short" style="display: inline;"> We present HOMERUN (Highly Optimized Multi-cloud Emission-line Ratios Using photo-ionizatioN), a new approach to modelling emission lines from photoionized gas that can simultaneously reproduce all observed line intensities from a wide range of ionization levels and with high accuracy. Our approach is based on the weighted combination of multiple single-cloud photoionization models and, contrary t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.13028v2-abstract-full').style.display = 'inline'; document.getElementById('2401.13028v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.13028v2-abstract-full" style="display: none;"> We present HOMERUN (Highly Optimized Multi-cloud Emission-line Ratios Using photo-ionizatioN), a new approach to modelling emission lines from photoionized gas that can simultaneously reproduce all observed line intensities from a wide range of ionization levels and with high accuracy. Our approach is based on the weighted combination of multiple single-cloud photoionization models and, contrary to previous works, the novelty of our approach consists in using the weights as free parameters of the fit and constraining them with the observed data. One of the main applications of HOMERUN is the accurate determination of gas-phase metallicities and we show that a critical point is to allow for a variation of the N/O and S/O abundance ratios which can significantly improve the quality of the fit and the accuracy of the results. Moreover, our approach provides a major improvement compared to the single-cloud, constant-pressure models commonly used in the literature. By using high-quality literature spectra of H ii regions where 10 to 20 emission lines (including several auroral lines) are detected with high signal-to-noise ratio, we show that all lines are reproduced by the model with an accuracy better than 10%. In particular, the model is able to simultaneously reproduce [O i]6300, 6363, [O ii]3726, 3729, [O iii]4959, 5007, [S ii]6717, 6731, and [S iii]9069, 9532 emission lines which, to our knowledge, is an unprecedented result. Finally, we show that the gas metallicities estimated with our models for HII regions in the Milky Way are in agreement with the stellar metallicities than the estimates based on the Te-method. Overall, our method provides a new accurate tool to estimate the metallicity and the physical conditions of the ionized gas. It can be applied to many different science cases from HII regions to AGN and wherever there are emission lines from photoionized gas. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.13028v2-abstract-full').style.display = 'none'; document.getElementById('2401.13028v2-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 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 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">A&A in press, new version following referee report</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 689, A78 (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/2305.11850">arXiv:2305.11850</a> <span> [<a href="https://arxiv.org/pdf/2305.11850">pdf</a>, <a href="https://arxiv.org/format/2305.11850">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/10.1051/0004-6361/202347242">10.1051/0004-6361/202347242 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MUSE adaptive-optics spectroscopy confirms dual active galactic nuclei and strongly lensed systems at sub-arcsec separation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Scialpi%2C+M">M. Scialpi</a>, <a href="/search/astro-ph?searchtype=author&query=Mannucci%2C+F">F. Mannucci</a>, <a href="/search/astro-ph?searchtype=author&query=Marconcini%2C+C">C. Marconcini</a>, <a href="/search/astro-ph?searchtype=author&query=Venturi%2C+G">G. Venturi</a>, <a href="/search/astro-ph?searchtype=author&query=Pancino%2C+E">E. Pancino</a>, <a href="/search/astro-ph?searchtype=author&query=Marconi%2C+A">A. Marconi</a>, <a href="/search/astro-ph?searchtype=author&query=Cresci%2C+G">G. Cresci</a>, <a href="/search/astro-ph?searchtype=author&query=Belfiore%2C+F">F. Belfiore</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+A">A. Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Bertola%2C+E">E. Bertola</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=Ciurlo%2C+A">A. Ciurlo</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=Ginolfi%2C+M">M. Ginolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Lusso%2C+E">E. Lusso</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=Rubinur%2C+K">K. Rubinur</a>, <a href="/search/astro-ph?searchtype=author&query=Severgnini%2C+P">P. Severgnini</a>, <a href="/search/astro-ph?searchtype=author&query=Tozzi%2C+G">G. Tozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Ulivi%2C+L">L. Ulivi</a>, <a href="/search/astro-ph?searchtype=author&query=Vignali%2C+C">C. Vignali</a>, <a href="/search/astro-ph?searchtype=author&query=Volonteri%2C+M">M. Volonteri</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="2305.11850v3-abstract-short" style="display: inline;"> The novel Gaia Multi Peak (GMP) technique has proven to be able to successfully select dual and lensed AGN candidates at sub-arcsec separations. Both populations are important because dual AGN represent one of the central, still largely untested, predictions of lamdaCDM cosmology, and compact lensed quasars allow to probe the central regions of the lensing galaxies. In this work, we present high s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.11850v3-abstract-full').style.display = 'inline'; document.getElementById('2305.11850v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.11850v3-abstract-full" style="display: none;"> The novel Gaia Multi Peak (GMP) technique has proven to be able to successfully select dual and lensed AGN candidates at sub-arcsec separations. Both populations are important because dual AGN represent one of the central, still largely untested, predictions of lamdaCDM cosmology, and compact lensed quasars allow to probe the central regions of the lensing galaxies. In this work, we present high spatial resolution spectroscopy of twelve GMP-selected systems. We use the the adaptive-optics assisted integral-field spectrograph MUSE at VLT to resolve each system and study the nature of each component. All the targets reveal the presence of two components confirming the GMP selection. We classify five targets as dual AGN, two as lensed systems, and five as a chance alignment of a star and and AGN. Having separations between 0.30" and 0.86", these dual and lensed systems are, to date, among the most compact ever discovered at z >0.3. This is the largest sample of distant dual AGN with sub-arcsec separations ever presented in a single paper. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.11850v3-abstract-full').style.display = 'none'; document.getElementById('2305.11850v3-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 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 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">16 pages, 11 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 690, A57 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.08563">arXiv:2304.08563</a> <span> [<a href="https://arxiv.org/pdf/2304.08563">pdf</a>, <a href="https://arxiv.org/format/2304.08563">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/10.3847/1538-4357/accd72">10.3847/1538-4357/accd72 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Way of Water: ALMA resolves H2O emission lines in a strongly lensed dusty star-forming galaxy at z $\sim$ 3.1 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Perrotta%2C+F">F. Perrotta</a>, <a href="/search/astro-ph?searchtype=author&query=Giulietti%2C+M">M. Giulietti</a>, <a href="/search/astro-ph?searchtype=author&query=Massardi%2C+M">M. Massardi</a>, <a href="/search/astro-ph?searchtype=author&query=Gandolfi%2C+G">G. Gandolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Ronconi%2C+T">T. Ronconi</a>, <a href="/search/astro-ph?searchtype=author&query=Zanchettin%2C+M+V">M. V. Zanchettin</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=Behiri.%2C+M">M. Behiri.</a>, <a href="/search/astro-ph?searchtype=author&query=Torsello%2C+M">M. Torsello</a>, <a href="/search/astro-ph?searchtype=author&query=Gabrielli%2C+F">F. Gabrielli</a>, <a href="/search/astro-ph?searchtype=author&query=Boco%2C+L">L. Boco</a>, <a href="/search/astro-ph?searchtype=author&query=Galluzzi%2C+V">V. Galluzzi</a>, <a href="/search/astro-ph?searchtype=author&query=Lapi%2C+A">A. Lapi</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="2304.08563v2-abstract-short" style="display: inline;"> We report ALMA high-resolution observations of water emission lines $p-{\rm{H_2O}} (2_{02}-1_{11}$), $o-{\rm{H_2O}} (3_{21}-3_{12})$, $p-{\rm{H_2O}} (4_{22}-4_{13})$, in the strongly lensed galaxy HATLASJ113526.2-01460 at redshift z $\sim$ 3.1. From the lensing-reconstructed maps of water emission and line profiles, we infer the general physical properties of the ISM in the molecular clouds where… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.08563v2-abstract-full').style.display = 'inline'; document.getElementById('2304.08563v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.08563v2-abstract-full" style="display: none;"> We report ALMA high-resolution observations of water emission lines $p-{\rm{H_2O}} (2_{02}-1_{11}$), $o-{\rm{H_2O}} (3_{21}-3_{12})$, $p-{\rm{H_2O}} (4_{22}-4_{13})$, in the strongly lensed galaxy HATLASJ113526.2-01460 at redshift z $\sim$ 3.1. From the lensing-reconstructed maps of water emission and line profiles, we infer the general physical properties of the ISM in the molecular clouds where the lines arise. We find that the water vapor lines $o-{\rm{H_2O}} (3_{21}-3_{12})$, $p-{\rm{H_2O}} (4_{22}-4_{13})$ are mainly excited by FIR pumping from dust radiation in a warm and dense environment, with dust temperatures ranging from 70 K to $\sim 100$ K, as suggested by the line ratios. The $p-{\rm{H_2O}} (2_{02}-1_{11})$ line instead, is excited by a complex interplay between FIR pumping and collisional excitation in the dense core of the star-forming region. This scenario is also supported by the detection of the medium-level excitation of CO resulting in the line emission CO (J=8-7). Thanks to the unprecedented high resolution offered by the combination of ALMA capabilities and gravitational lensing, we discern the different phases of the ISM and locate the hot molecular clouds into a physical scale of $\sim$ 500 pc. We discuss the possibility of J1135 hosting an AGN in its accretion phase. Finally, we determine the relation between the water emission lines and the total IR luminosity of J1135, as well as the SFR as a function of water emission intensities, comparing the outcomes to local and high-$z$ galactic samples from the literature. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.08563v2-abstract-full').style.display = 'none'; document.getElementById('2304.08563v2-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 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">22 pages, 10 figures, final version to be published in Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.13575">arXiv:2303.13575</a> <span> [<a href="https://arxiv.org/pdf/2303.13575">pdf</a>, <a href="https://arxiv.org/format/2303.13575">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/10.1051/0004-6361/202245513">10.1051/0004-6361/202245513 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> LBT-MODS spectroscopy of high-redshift candidates in the Chandra J1030 field. A newly discovered z$\sim$2.8 large scale structure </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=Mazzolari%2C+G">Giovanni Mazzolari</a>, <a href="/search/astro-ph?searchtype=author&query=Signorini%2C+M">Matilde Signorini</a>, <a href="/search/astro-ph?searchtype=author&query=Brienza%2C+M">Marisa Brienza</a>, <a href="/search/astro-ph?searchtype=author&query=Bisogni%2C+S">Susanna Bisogni</a>, <a href="/search/astro-ph?searchtype=author&query=Bolzonella%2C+M">Micol Bolzonella</a>, <a href="/search/astro-ph?searchtype=author&query=Cucciati%2C+O">Olga Cucciati</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=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=Comastri%2C+A">Andrea Comastri</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="2303.13575v1-abstract-short" style="display: inline;"> We present the results of a spectroscopic campaign with the Multi-Object Double Spectrograph (MODS) instrument mounted on the Large Binocular Telescope (LBT), aimed at obtaining a spectroscopic redshift for seven Chandra J1030 sources with a photometric redshift >=2.7 and optical magnitude r_AB=[24.5-26.5]. We obtained a spectroscopic redshift for five out of seven targets: all of them have z_spec… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.13575v1-abstract-full').style.display = 'inline'; document.getElementById('2303.13575v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.13575v1-abstract-full" style="display: none;"> We present the results of a spectroscopic campaign with the Multi-Object Double Spectrograph (MODS) instrument mounted on the Large Binocular Telescope (LBT), aimed at obtaining a spectroscopic redshift for seven Chandra J1030 sources with a photometric redshift >=2.7 and optical magnitude r_AB=[24.5-26.5]. We obtained a spectroscopic redshift for five out of seven targets: all of them have z_spec>=2.5, thus probing the reliability of the Chandra J1030 photometric redshifts. The spectroscopic campaign led to the serendipitous discovery of a z~2.78 large scale structure (LSS) in the J1030 field: the structure contains four X-ray sources (three of which were targeted in the LBT-MODS campaign) and two non-X-ray detected galaxies for which a VLT-MUSE spectrum was already available. The X-ray members of the LSS are hosted in galaxies that are significantly more massive (log(M_*/M_sun)=[10.0-11.1]) than those hosting the two MUSE-detected sources (log(M_*/M_sun)<10). Both observations and simulations show that massive galaxies, and particularly objects having log(M_*/M_sun)>10, are among the best tracers of large scale structures and filaments in the cosmic web. Consequently, our result can explain why X-ray-detected AGN have also been shown to be efficient tracers of large scale structures. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.13575v1-abstract-full').style.display = 'none'; document.getElementById('2303.13575v1-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> 23 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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, 9 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 673, A97 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.11977">arXiv:2302.11977</a> <span> [<a href="https://arxiv.org/pdf/2302.11977">pdf</a>, <a href="https://arxiv.org/format/2302.11977">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/10.1051/0004-6361/202245247">10.1051/0004-6361/202245247 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> AGN feedback in an infant galaxy cluster: the LOFAR-Chandra view of the giant FRII radio galaxy J103025+052430 at z=1.7 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Brienza%2C+M">M. Brienza</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">R. Gilli</a>, <a href="/search/astro-ph?searchtype=author&query=Prandoni%2C+I">I. Prandoni</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=Rajpurohit%2C+K">K. Rajpurohit</a>, <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">F. Calura</a>, <a href="/search/astro-ph?searchtype=author&query=Chiaberge%2C+M">M. Chiaberge</a>, <a href="/search/astro-ph?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/astro-ph?searchtype=author&query=Iwasawa%2C+K">K. Iwasawa</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzuisi%2C+G">G. Lanzuisi</a>, <a href="/search/astro-ph?searchtype=author&query=Liuzzo%2C+E">E. Liuzzo</a>, <a href="/search/astro-ph?searchtype=author&query=Marchesi%2C+S">S. Marchesi</a>, <a href="/search/astro-ph?searchtype=author&query=Mignoli%2C+M">M. Mignoli</a>, <a href="/search/astro-ph?searchtype=author&query=Miley%2C+G">G. Miley</a>, <a href="/search/astro-ph?searchtype=author&query=Norman%2C+C">C. Norman</a>, <a href="/search/astro-ph?searchtype=author&query=Peca%2C+A">A. Peca</a>, <a href="/search/astro-ph?searchtype=author&query=Raciti%2C+M">M. Raciti</a>, <a href="/search/astro-ph?searchtype=author&query=Shimwell%2C+T">T. Shimwell</a>, <a href="/search/astro-ph?searchtype=author&query=Tozzi%2C+P">P. Tozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Vignali%2C+C">C. Vignali</a>, <a href="/search/astro-ph?searchtype=author&query=Vitello%2C+F">F. Vitello</a>, <a href="/search/astro-ph?searchtype=author&query=Vito%2C+F">F. Vito</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="2302.11977v2-abstract-short" style="display: inline;"> In the nearby universe jets from AGN are observed to have a dramatic impact on their surrounding extragalactic environment. Their effect at the `cosmic noon' (z>1.5), the epoch when star formation and AGN activity peak, is instead much less constrained. Here we present a study of the giant (750 kpc) radio galaxy 103025+052430 located at the centre of a protocluster at redshift z=1.7, with a focus… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.11977v2-abstract-full').style.display = 'inline'; document.getElementById('2302.11977v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.11977v2-abstract-full" style="display: none;"> In the nearby universe jets from AGN are observed to have a dramatic impact on their surrounding extragalactic environment. Their effect at the `cosmic noon' (z>1.5), the epoch when star formation and AGN activity peak, is instead much less constrained. Here we present a study of the giant (750 kpc) radio galaxy 103025+052430 located at the centre of a protocluster at redshift z=1.7, with a focus on its interaction with the external medium. We present new LOFAR observations at 144 MHz, which we combine with VLA 1.4 GHz and 0.5-7 keV Chandra archival data. The new map at 144 MHz confirms that the source has a complex morphology, possibly consistent with the `hybrid morphology' classification. The large size of the source gave us the possibility to perform a resolved radio spectral index analysis, a very unique opportunity for a source at such high redshift. This reveals a tentative flattening of the radio spectral index at the edge of the backflow in the Western lobe, which might be indicating plasma compression. The spatial coincidence between this region and the thermal X-ray bubble C suggests a causal connection between the two. Contrary to previous estimates for the bright X-ray component A, we find that inverse Compton scattering between the radio-emitting plasma of the Eastern lobe and the CMB photons can account for a large fraction (~45%-80%) of its total 0.5-7 keV measured flux. Finally, the X-ray bubble C, which is consistent with a thermal origin, is found to be significantly overpressurised with respect to the ambient medium. This suggests that it will tend to expand and release its energy in the surroundings, contributing to the overall intracluster medium heating. Overall, 103025+052430 gives us the chance to investigate the interaction between AGN jets and the surrounding gas in a system that is likely the predecessor of the rich galaxy clusters we all well know at z=0. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.11977v2-abstract-full').style.display = 'none'; document.getElementById('2302.11977v2-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 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 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">12 pages, 5 figures, 2 tables, 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/2210.15595">arXiv:2210.15595</a> <span> [<a href="https://arxiv.org/pdf/2210.15595">pdf</a>, <a href="https://arxiv.org/format/2210.15595">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/10.1051/0004-6361/202244452">10.1051/0004-6361/202244452 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A deep 1.4 GHz survey of the J1030 equatorial field: a new window on radio source populations across cosmic time </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=D%27Amato%2C+Q">Q. D'Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Prandoni%2C+I">I. Prandoni</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">R. Gilli</a>, <a href="/search/astro-ph?searchtype=author&query=Vignali%2C+C">C. Vignali</a>, <a href="/search/astro-ph?searchtype=author&query=Massardi%2C+M">M. Massardi</a>, <a href="/search/astro-ph?searchtype=author&query=Liuzzo%2C+E">E. Liuzzo</a>, <a href="/search/astro-ph?searchtype=author&query=Jagannathan%2C+P">P. Jagannathan</a>, <a href="/search/astro-ph?searchtype=author&query=Brienza%2C+M">M. Brienza</a>, <a href="/search/astro-ph?searchtype=author&query=Paladino%2C+R">R. Paladino</a>, <a href="/search/astro-ph?searchtype=author&query=Mignoli%2C+M">M. Mignoli</a>, <a href="/search/astro-ph?searchtype=author&query=Marchesi%2C+S">S. Marchesi</a>, <a href="/search/astro-ph?searchtype=author&query=Peca%2C+A">A. Peca</a>, <a href="/search/astro-ph?searchtype=author&query=Chiaberge%2C+M">M. Chiaberge</a>, <a href="/search/astro-ph?searchtype=author&query=Mazzolari%2C+G">G. Mazzolari</a>, <a href="/search/astro-ph?searchtype=author&query=Norman%2C+C">C. 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="2210.15595v1-abstract-short" style="display: inline;"> We present deep L-Band observations of the equatorial field centered on the z=6.3 SDSS QSO, reaching a 1 sigma sensitivity of ~2.5 uJy at the center of the field. We extracted a catalog of 1489 radio sources down to a flux density of ~12.5 uJy (5 sigma) over a field of view of ~ 30' diameter. We derived the source counts accounting for catalog reliability and completeness, and compared them with o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.15595v1-abstract-full').style.display = 'inline'; document.getElementById('2210.15595v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.15595v1-abstract-full" style="display: none;"> We present deep L-Band observations of the equatorial field centered on the z=6.3 SDSS QSO, reaching a 1 sigma sensitivity of ~2.5 uJy at the center of the field. We extracted a catalog of 1489 radio sources down to a flux density of ~12.5 uJy (5 sigma) over a field of view of ~ 30' diameter. We derived the source counts accounting for catalog reliability and completeness, and compared them with others available in the literature. Our source counts are among the deepest available so far, and, overall, are consistent with recent counts' determinations and models. We detected for the first time in the radio band the SDSS J1030+0524 QSO (26 +/- 5 uJy). We derived its optical radio loudness R_O = 0.62 +/- 0.12, which makes it the most radio quiet AGN at z >~ 6 discovered so far and detected at radio wavelengths. We unveiled extended diffuse radio emission associated with the lobes of a bright FRII radio galaxy located close to the center of the J1030 field, which is likely to become the future BCG of a protocluster at z=1.7. The lobes' complex morphology, coupled with the presence of X-ray diffuse emission detected around the FRII galaxy lobes, may point toward an interaction between the radio jets and the external medium. We also investigated the relation between radio and X-ray luminosity for a sample of 243 X-ray-selected objects obtained from 500 ks Chandra observations of the same field, and spanning a wide redshift range (0 ~< z ~< 3). Focused on sources with a spectroscopic redshift and classification, we found that sources hosted by ETG and AGN follow Log(L_R)/Log(L_X) linear correlations with slopes of ~0.6 and ~0.8, respectively. This is interpreted as a likely signature of different efficiency in the accretion process. Finally, we found that most of these sources (>~87%) show a radio-to-X-ray radio loudness R_X < -3.5, classifying these objects as radio quiet. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.15595v1-abstract-full').style.display = 'none'; document.getElementById('2210.15595v1-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 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">18 pages, 15 figures, 5 table. 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 668, A133 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.00466">arXiv:2207.00466</a> <span> [<a href="https://arxiv.org/pdf/2207.00466">pdf</a>, <a href="https://arxiv.org/format/2207.00466">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/10.3847/1538-4357/aca53f">10.3847/1538-4357/aca53f <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> ALMA resolves the first strongly-lensed Optical/NIR-dark galaxy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Giulietti%2C+M">M. Giulietti</a>, <a href="/search/astro-ph?searchtype=author&query=Lapi%2C+A">A. Lapi</a>, <a href="/search/astro-ph?searchtype=author&query=Massardi%2C+M">M. Massardi</a>, <a href="/search/astro-ph?searchtype=author&query=Behiri%2C+M">M. Behiri</a>, <a href="/search/astro-ph?searchtype=author&query=Torsello%2C+M">M. Torsello</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=Ronconi%2C+T">T. Ronconi</a>, <a href="/search/astro-ph?searchtype=author&query=Perrotta%2C+F">F. Perrotta</a>, <a href="/search/astro-ph?searchtype=author&query=Bressan%2C+A">A. Bressan</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="2207.00466v1-abstract-short" style="display: inline;"> We present high-resolution ($\lesssim0.1$arcsec) ALMA observations of the strongly-lensed galaxy HATLASJ113526.2-01460 at redshift $z\sim3.1$ discovered in the Gama 12$^{\rm th}$ field of the Herschel-ATLAS survey. The gravitationally lensed system is remarkably peculiar in that neither the background source nor the foreground lens show a clearly detected optical/NIR emission. We perform accurate… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.00466v1-abstract-full').style.display = 'inline'; document.getElementById('2207.00466v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.00466v1-abstract-full" style="display: none;"> We present high-resolution ($\lesssim0.1$arcsec) ALMA observations of the strongly-lensed galaxy HATLASJ113526.2-01460 at redshift $z\sim3.1$ discovered in the Gama 12$^{\rm th}$ field of the Herschel-ATLAS survey. The gravitationally lensed system is remarkably peculiar in that neither the background source nor the foreground lens show a clearly detected optical/NIR emission. We perform accurate lens modeling and source morphology reconstruction in three different (sub-)mm continuum bands, and in the C[II] and CO(8-7) spectral lines. The modeling indicates a foreground lensing (likely elliptical) galaxy with mass $\gtrsim10^{11}\, M_\odot$ at $z\gtrsim1.5$, while the source (sub-)mm continuum and line emissions are amplified by factors $渭\sim6-13$. We estimate extremely compact sizes $\lesssim0.5$ kpc for the star-forming region and $\lesssim 1$ kpc for the gas component, with no clear evidence of rotation or of ongoing merging events. We perform broadband SED-fitting and retrieve the intrinsic de-magnified physical properties of the source, which is found to feature a very high star-formation rate $\gtrsim10^3\, M_\odot$ yr$^{-1}$, that given the compact sizes is on the verge of the Eddington limit for starbursts; the radio luminosity at 6 cm from available EVLA observations is consistent with the star-formation activity. The galaxy is found to be extremely rich in gas $\sim10^{11}\, M_\odot$ and dust $\gtrsim10^9\, M_\odot$. The stellar content $\lesssim10^{11}\, M_\odot$ places the source well above the main sequence of starforming galaxies, indicating that the starburst is rather young with estimated age $\sim10^8$ yr. Our results indicate that the overall properties of HATLASJ113526.2-01460 are consistently explained by in-situ galaxy formation and evolution scenarios. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.00466v1-abstract-full').style.display = 'none'; document.getElementById('2207.00466v1-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 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">17 Pages, 12 Figures, 7 Tables. Submitted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.03508">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/2202.00019">arXiv:2202.00019</a> <span> [<a href="https://arxiv.org/pdf/2202.00019">pdf</a>, <a href="https://arxiv.org/format/2202.00019">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> </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/10.3847/1538-4357/ac51ca">10.3847/1538-4357/ac51ca <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A new estimate of the cosmic star formation density from a radio-selected sample, and the contribution of $H$-dark galaxies at $z \geq 3$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Enia%2C+A">A. Enia</a>, <a href="/search/astro-ph?searchtype=author&query=Talia%2C+M">M. Talia</a>, <a href="/search/astro-ph?searchtype=author&query=Pozzi%2C+F">F. Pozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Cimatti%2C+A">A. Cimatti</a>, <a href="/search/astro-ph?searchtype=author&query=Delvecchio%2C+I">I. Delvecchio</a>, <a href="/search/astro-ph?searchtype=author&query=Zamorani%2C+G">G. Zamorani</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=Bisigello%2C+L">L. Bisigello</a>, <a href="/search/astro-ph?searchtype=author&query=Gruppioni%2C+C">C. Gruppioni</a>, <a href="/search/astro-ph?searchtype=author&query=Rodighiero%2C+G">G. Rodighiero</a>, <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">F. Calura</a>, <a href="/search/astro-ph?searchtype=author&query=Dallacasa%2C+D">D. Dallacasa</a>, <a href="/search/astro-ph?searchtype=author&query=Giulietti%2C+M">M. Giulietti</a>, <a href="/search/astro-ph?searchtype=author&query=Barchiesi%2C+L">L. Barchiesi</a>, <a href="/search/astro-ph?searchtype=author&query=Behiri%2C+M">M. Behiri</a>, <a href="/search/astro-ph?searchtype=author&query=Romano%2C+M">M. Romano</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="2202.00019v1-abstract-short" style="display: inline;"> The Star Formation Rate Density (SFRD) history of the Universe is well constrained up to redshift $z \sim 2$. At earlier cosmic epochs, the picture has been largely inferred from UV-selected galaxies (e.g. Lyman-break galaxies, LBGs). However, LBGs' inferred SFRs strongly depend on the assumed dust extinction correction, which is not well-constrained at high-$z$, while observations in the radio do… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.00019v1-abstract-full').style.display = 'inline'; document.getElementById('2202.00019v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.00019v1-abstract-full" style="display: none;"> The Star Formation Rate Density (SFRD) history of the Universe is well constrained up to redshift $z \sim 2$. At earlier cosmic epochs, the picture has been largely inferred from UV-selected galaxies (e.g. Lyman-break galaxies, LBGs). However, LBGs' inferred SFRs strongly depend on the assumed dust extinction correction, which is not well-constrained at high-$z$, while observations in the radio domain are not affected by this issue. In this work we measure the SFRD from a 1.4 GHz-selected sample of $\sim$600 galaxies in the GOODS-N field up to redshift $\sim 3.5$. We take into account the contribution of Active Galactic Nuclei from the Infrared-Radio correlation. We measure the radio luminosity function, fitted with a modified Schechter function, and derive the SFRD. The cosmic SFRD shows a rise up to $z \sim 2$ and then an almost flat plateau up to $z \sim 3.5$. Our SFRD is in agreement with the ones from other FIR/radio surveys and a factor 2 higher than those from LBG samples. We also estimate that galaxies lacking a counterpart in the HST/WFC3 H-band ($H$-dark) make up $\sim 25\%$ of the $蠁$-integrated SFRD relative to the full sample at z $\sim 3.2$, and up to $58\%$ relative to LBG samples. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.00019v1-abstract-full').style.display = 'none'; document.getElementById('2202.00019v1-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, 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">20 pages, 11 figures. Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.06466">arXiv:2201.06466</a> <span> [<a href="https://arxiv.org/pdf/2201.06466">pdf</a>, <a href="https://arxiv.org/format/2201.06466">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/10.1093/mnras/stac145">10.1093/mnras/stac145 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The far-infrared/radio correlation for a sample of strongly lensed dusty star-forming galaxies detected by Herschel </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Giulietti%2C+M">M. Giulietti</a>, <a href="/search/astro-ph?searchtype=author&query=Massardi%2C+M">M. Massardi</a>, <a href="/search/astro-ph?searchtype=author&query=Lapi%2C+A">A. Lapi</a>, <a href="/search/astro-ph?searchtype=author&query=Bonato%2C+M">M. Bonato</a>, <a href="/search/astro-ph?searchtype=author&query=Enia%2C+A+F+M">A. F. M. Enia</a>, <a href="/search/astro-ph?searchtype=author&query=Negrello%2C+M">M. Negrello</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=Behiri%2C+M">M. Behiri</a>, <a href="/search/astro-ph?searchtype=author&query=De+Zotti%2C+G">G. De Zotti</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="2201.06466v2-abstract-short" style="display: inline;"> We investigate the radio-far infrared (FIR) correlation for a sample of $28$ bright high-redshift ($1 \lesssim z \lesssim 4$) star-forming galaxies selected in the FIR from the Herschel-ATLAS fields as candidates to be strongly gravitationally lensed. The radio information comes either from high sensitivity dedicated ATCA observations at $2.1$ GHz or from cross-matches with the FIRST survey at… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.06466v2-abstract-full').style.display = 'inline'; document.getElementById('2201.06466v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.06466v2-abstract-full" style="display: none;"> We investigate the radio-far infrared (FIR) correlation for a sample of $28$ bright high-redshift ($1 \lesssim z \lesssim 4$) star-forming galaxies selected in the FIR from the Herschel-ATLAS fields as candidates to be strongly gravitationally lensed. The radio information comes either from high sensitivity dedicated ATCA observations at $2.1$ GHz or from cross-matches with the FIRST survey at $1.4$ GHz. By taking advantage of source brightness possibly enhanced by lensing magnification, we identify a weak evolution with redshift out to $z\lesssim 4$ of the FIR-to-radio luminosity ratio $q_{\rm FIR}$. We also find that the $q_{\rm FIR}$ parameter as a function of the radio power $L_{1.4\,\rm GHz}$ displays a clear decreasing trend, similarly to what is observed for optically/radio selected lensed quasars found in literature, yet covering a complementary region in the $q_{\rm FIR}-L_{1.4\,\rm GHz}$ diagram. We interpret such a behavior in the framework of an in-situ galaxy formation scenario, as a result of the transition from an early dust-obscured star-forming phase (mainly pinpointed by our FIR selection) to a late radio-loud quasar phase (preferentially sampled by the optical/radio selection). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.06466v2-abstract-full').style.display = 'none'; document.getElementById('2201.06466v2-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 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">12 pages, 6 figures. Minor changes and references updated to match the published version</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2112.03658">arXiv:2112.03658</a> <span> [<a href="https://arxiv.org/pdf/2112.03658">pdf</a>, <a href="https://arxiv.org/format/2112.03658">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-Wavelength Study of a Proto-BCG at z = 1.7 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=D%27Amato%2C+Q">Q. D'Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Prandoni%2C+I">I. Prandoni</a>, <a href="/search/astro-ph?searchtype=author&query=Brienza%2C+M">M. Brienza</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">R. Gilli</a>, <a href="/search/astro-ph?searchtype=author&query=Vignali%2C+C">C. Vignali</a>, <a href="/search/astro-ph?searchtype=author&query=Paladino%2C+R">R. Paladino</a>, <a href="/search/astro-ph?searchtype=author&query=Loi%2C+F">F. Loi</a>, <a href="/search/astro-ph?searchtype=author&query=Massardi%2C+M">M. Massardi</a>, <a href="/search/astro-ph?searchtype=author&query=Mignoli%2C+M">M. Mignoli</a>, <a href="/search/astro-ph?searchtype=author&query=Marchesi%2C+S">S. Marchesi</a>, <a href="/search/astro-ph?searchtype=author&query=Peca%2C+A">A. Peca</a>, <a href="/search/astro-ph?searchtype=author&query=Jagannathan%2C+P">P. Jagannathan</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="2112.03658v2-abstract-short" style="display: inline;"> In this work we performed a spectral energy distribution (SED) analysis in the optical/infrared band of the host galaxy of a proto-brightest cluster galaxy (BCG, NVSS J103023+052426) in a proto-cluster at z = 1.7. We found that it features a vigorous star formation rate (SFR) of ${\sim}$570 $\mathrm{M_{\odot}}$/yr and a stellar mass of $M_{\ast} \sim 3.7 \times 10^{11}$ $\mathrm{M_{\odot}}$; the h… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.03658v2-abstract-full').style.display = 'inline'; document.getElementById('2112.03658v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.03658v2-abstract-full" style="display: none;"> In this work we performed a spectral energy distribution (SED) analysis in the optical/infrared band of the host galaxy of a proto-brightest cluster galaxy (BCG, NVSS J103023+052426) in a proto-cluster at z = 1.7. We found that it features a vigorous star formation rate (SFR) of ${\sim}$570 $\mathrm{M_{\odot}}$/yr and a stellar mass of $M_{\ast} \sim 3.7 \times 10^{11}$ $\mathrm{M_{\odot}}$; the high corresponding specific SFR = $1.5 \pm 0.5$ $\mathrm{Gyr^{-1}}$ classifies this object as a starburst galaxy that will deplete its molecular gas reservoir in $\sim$ $3.5 \times 10^8$ yr. Thus, this system represents a rare example of a proto-BCG caught during the short phase of its major stellar mass assembly. Moreover, we investigated the nature of the host galaxy emission at 3.3 mm. We found that it originates from the cold dust in the interstellar medium, even though a minor non-thermal AGN contribution cannot be completely ruled out. Finally, we studied the polarized emission of the lobes at 1.4 GHz. We unveiled a patchy structure where the polarization fraction increases in the regions in which the total intensity shows a bending morphology; in addition, the magnetic field orientation follows the direction of the bendings. We interpret these features as possible indications of an interaction with the intracluster medium. This strengthens the hypothesis of positive AGN feedback, as inferred in previous studies of this object on the basis of X-ray/mm/radio analysis. In this scenario, the proto-BCG heats the surrounding medium and possibly enhances the SFR in nearby galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.03658v2-abstract-full').style.display = 'none'; document.getElementById('2112.03658v2-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 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 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">13 pages, 3 figures, 1 table. Accepted for publication in Galaxies</span> </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/2108.05596">arXiv:2108.05596</a> <span> [<a href="https://arxiv.org/pdf/2108.05596">pdf</a>, <a href="https://arxiv.org/format/2108.05596">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/10.1093/mnras/stab2346">10.1093/mnras/stab2346 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An ALMA view of 11 Dusty Star Forming Galaxies at the peak of Cosmic Star Formation History </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pantoni%2C+L">L. Pantoni</a>, <a href="/search/astro-ph?searchtype=author&query=Massardi%2C+M">M. Massardi</a>, <a href="/search/astro-ph?searchtype=author&query=Lapi%2C+A">A. Lapi</a>, <a href="/search/astro-ph?searchtype=author&query=Donevski%2C+D">D. Donevski</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=Giulietti%2C+M">M. Giulietti</a>, <a href="/search/astro-ph?searchtype=author&query=Pozzi%2C+F">F. Pozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Talia%2C+M">M. Talia</a>, <a href="/search/astro-ph?searchtype=author&query=Vignali%2C+C">C. Vignali</a>, <a href="/search/astro-ph?searchtype=author&query=Cimatti%2C+A">A. Cimatti</a>, <a href="/search/astro-ph?searchtype=author&query=Silva%2C+L">L. Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Bressan%2C+A">A. Bressan</a>, <a href="/search/astro-ph?searchtype=author&query=Ronconi%2C+T">T. Ronconi</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="2108.05596v1-abstract-short" style="display: inline;"> We present the ALMA view of 11 main-sequence DSFGs, (sub-)millimeter selected in the GOODS-S field, and spectroscopically confirmed to be at the peak of Cosmic SFH (z = 2-3). Our study combines the analysis of galaxy SED with ALMA continuum and CO spectral emission, by using ALMA Science Archive products at the highest spatial resolution currently available for our sample (< 1 arcsec). We include… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.05596v1-abstract-full').style.display = 'inline'; document.getElementById('2108.05596v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.05596v1-abstract-full" style="display: none;"> We present the ALMA view of 11 main-sequence DSFGs, (sub-)millimeter selected in the GOODS-S field, and spectroscopically confirmed to be at the peak of Cosmic SFH (z = 2-3). Our study combines the analysis of galaxy SED with ALMA continuum and CO spectral emission, by using ALMA Science Archive products at the highest spatial resolution currently available for our sample (< 1 arcsec). We include galaxy multi-band images and photometry (in the optical, radio and X-rays) to investigate the interlink between dusty, gaseous and stellar components and the eventual presence of AGN. We use multi-band sizes and morphologies to gain an insight on the processes that lead galaxy evolution, e.g. gas condensation, star formation, AGN feedback. The 11 DSFGs are very compact in the (sub-)millimeter (median r(ALMA) = 1.15 kpc), while the optical emission extends tolarger radii (median r(H)/r(ALMA) = 2.05). CO lines reveal the presence of a rotating disc of molecular gas, but we can not exclude either the presence of interactions and/or molecular outflows. Images at higher (spectral and spatial) resolution are needed to disentangle from the possible scenarios. Most of the galaxies are caught in the compaction phase, when gas cools and falls into galaxy centre, fuelling the dusty burst of star formation and the growing nucleus. We expect these DSFGs to be the high-zstar-forming counterparts of massive quiescent galaxies. Some features of CO emission in three galaxies are suggestive of forthcoming/ongoing AGN feedback, that is thought to trigger the morphological transition from star-forming disks to ETGs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.05596v1-abstract-full').style.display = 'none'; document.getElementById('2108.05596v1-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> 12 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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, 6 figures, 7 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2011.06051">arXiv:2011.06051</a> <span> [<a href="https://arxiv.org/pdf/2011.06051">pdf</a>, <a href="https://arxiv.org/format/2011.06051">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/10.3847/1538-4357/abd800">10.3847/1538-4357/abd800 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Extremely Low Molecular Gas Content in the Vicinity of a Red Nugget Galaxy at $z=1.91$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Morishita%2C+T">T. Morishita</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=Abramson%2C+L+E">L. E. Abramson</a>, <a href="/search/astro-ph?searchtype=author&query=Abdurro%27uf"> Abdurro'uf</a>, <a href="/search/astro-ph?searchtype=author&query=Stiavelli%2C+M">M. Stiavelli</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+R+A">R. A. Lucas</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="2011.06051v3-abstract-short" style="display: inline;"> We present Atacama Large Millimeter/submillimeter Array (ALMA) Band 5 observations of a galaxy at $z=1.91$, GDS24569, in search of molecular gas in its vicinity via the [C I] $^3$P$_1$-$^3$P$_0$ line. GDS24569 is a massive ($\log M_*/M_\odot=11$) passively evolving galaxy, and characterized by compact morphology with an effective radius of $\sim0.5$ kpc. We apply two blind detection algorithms to… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.06051v3-abstract-full').style.display = 'inline'; document.getElementById('2011.06051v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.06051v3-abstract-full" style="display: none;"> We present Atacama Large Millimeter/submillimeter Array (ALMA) Band 5 observations of a galaxy at $z=1.91$, GDS24569, in search of molecular gas in its vicinity via the [C I] $^3$P$_1$-$^3$P$_0$ line. GDS24569 is a massive ($\log M_*/M_\odot=11$) passively evolving galaxy, and characterized by compact morphology with an effective radius of $\sim0.5$ kpc. We apply two blind detection algorithms to the spectral data cubes, and find no promising detection in or around GDS24569 out to projected distance of $\sim320$ kpc, while a narrow tentative line ($4.1 蟽$) is identified at $+1200$ km/s by one of the algorithms. From the non-detection of [C I], we place a $3蟽$ upper limit on molecular hydrogen mass, $\sim 7.1 \times 10^9 M_\odot$, which converts to an extremely low gas-to-stellar mass fraction, $< 5 \%$. We conduct a spectral energy distribution modeling by including optical-to-far-infrared data, and find a considerably high ($\sim0.1\%$) dust-to-stellar mass ratio, $\sim10$-$100\times$ higher than those of local early-type galaxies. In combination with a previous result of an insufficient number of surrounding satellite galaxies, it is suggested that GDS24569 is unlikely to experience significant size evolution via satellite mergers. We discuss possible physical mechanisms that quenched GDS24569. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.06051v3-abstract-full').style.display = 'none'; document.getElementById('2011.06051v3-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, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2020. </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 ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2010.07302">arXiv:2010.07302</a> <span> [<a href="https://arxiv.org/pdf/2010.07302">pdf</a>, <a href="https://arxiv.org/format/2010.07302">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/10.1093/mnras/staa3185">10.1093/mnras/staa3185 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraints on the [CII] luminosity of a proto-globular cluster at z~6 obtained with ALMA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">F. Calura</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Carniani%2C+S">S. Carniani</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">R. Gilli</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">M. Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Paladino%2C+R">R. Paladino</a>, <a href="/search/astro-ph?searchtype=author&query=Decarli%2C+R">R. Decarli</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Lupi%2C+A">A. Lupi</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=Bergamini%2C+P">P. Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Caminha%2C+.+G+B">. G. B. Caminha</a>, <a href="/search/astro-ph?searchtype=author&query=-"> -</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="2010.07302v1-abstract-short" style="display: inline;"> We report on ALMA observations of D1, a system at z~6.15 with stellar mass M_* ~ 10^7 M_sun containing globular cluster (GC) precursors, strongly magnified by the galaxy cluster MACS J0416.1-2403. Since the discovery of GC progenitors at high redshift, ours is the first attempt to probe directly the physical properties of their neutral gas through infrared observations. A careful analysis of our d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.07302v1-abstract-full').style.display = 'inline'; document.getElementById('2010.07302v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.07302v1-abstract-full" style="display: none;"> We report on ALMA observations of D1, a system at z~6.15 with stellar mass M_* ~ 10^7 M_sun containing globular cluster (GC) precursors, strongly magnified by the galaxy cluster MACS J0416.1-2403. Since the discovery of GC progenitors at high redshift, ours is the first attempt to probe directly the physical properties of their neutral gas through infrared observations. A careful analysis of our dataset, performed with a suitable procedure designed to identify faint narrow lines and which can test various possible values for the unknown linewidth value, allowed us to identify a 4-sigma tentative detection of [CII] emission with intrinsic luminosity L_CII=(2.9 +/- 1.4) 10^6 L_sun, one of the lowest values ever detected at high redshift. This study offers a first insight on previously uncharted regions of the L_CII-SFR relation. Despite large uncertainties affecting our measure of the star formation rate, if taken at face value our estimate lies more than 1 dex below the values observed in local and high redshift systems. Our weak detection indicates a deficiency of [CII] emission, possibly ascribed to various explanations, such as a low-density gas and/or a strong radiation field caused by intense stellar feedback, and a low metal content. From the non-detection in the continuum we derive constraints on the dust mass, with 3-sigma upper limit values as low as a few 10^4 M_sun, consistent with the values measured in local metal-poor galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.07302v1-abstract-full').style.display = 'none'; document.getElementById('2010.07302v1-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> 14 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2020. </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">MNRAS, accepted. 15 pages, 5 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/2008.13665">arXiv:2008.13665</a> <span> [<a href="https://arxiv.org/pdf/2008.13665">pdf</a>, <a href="https://arxiv.org/format/2008.13665">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"> Discovery of molecular gas fueling galaxy growth in a protocluster at z=1.7 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=D%27Amato%2C+Q">Q. D'Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">R. Gilli</a>, <a href="/search/astro-ph?searchtype=author&query=Prandoni%2C+I">I. Prandoni</a>, <a href="/search/astro-ph?searchtype=author&query=Vignali%2C+C">C. Vignali</a>, <a href="/search/astro-ph?searchtype=author&query=Massardi%2C+M">M. Massardi</a>, <a href="/search/astro-ph?searchtype=author&query=Mignoli%2C+M">M. Mignoli</a>, <a href="/search/astro-ph?searchtype=author&query=Cucciati%2C+O">O. Cucciati</a>, <a href="/search/astro-ph?searchtype=author&query=Morishita%2C+T">T. Morishita</a>, <a href="/search/astro-ph?searchtype=author&query=Decarli%2C+R">R. Decarli</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">F. Calura</a>, <a href="/search/astro-ph?searchtype=author&query=Balmaverde%2C+B">B. Balmaverde</a>, <a href="/search/astro-ph?searchtype=author&query=Chiaberge%2C+M">M. Chiaberge</a>, <a href="/search/astro-ph?searchtype=author&query=Liuzzo%2C+E">E. Liuzzo</a>, <a href="/search/astro-ph?searchtype=author&query=Nanni%2C+R">R. Nanni</a>, <a href="/search/astro-ph?searchtype=author&query=Peca%2C+A">A. Peca</a>, <a href="/search/astro-ph?searchtype=author&query=Pensabene%2C+A">A. Pensabene</a>, <a href="/search/astro-ph?searchtype=author&query=Tozzi%2C+P">P. Tozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Norman%2C+C">C. 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="2008.13665v1-abstract-short" style="display: inline;"> Based on ALMA Band 3 observations of the CO(2-1) line transition, we report the discovery of three new gas-rich (M_H2 ~ 1.5-4.8 x 10^10 M_sun, SFRs in the range ~5-100 M_sun/yr) galaxies in an overdense region at z=1.7, that already contains eight spectroscopically confirmed members. This leads to a total of 11 confirmed overdensity members, within a projected distance of ~ 1.15 Mpc and in a redsh… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.13665v1-abstract-full').style.display = 'inline'; document.getElementById('2008.13665v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.13665v1-abstract-full" style="display: none;"> Based on ALMA Band 3 observations of the CO(2-1) line transition, we report the discovery of three new gas-rich (M_H2 ~ 1.5-4.8 x 10^10 M_sun, SFRs in the range ~5-100 M_sun/yr) galaxies in an overdense region at z=1.7, that already contains eight spectroscopically confirmed members. This leads to a total of 11 confirmed overdensity members, within a projected distance of ~ 1.15 Mpc and in a redshift range of Dz = 0.012. Under simple assumptions, we estimate that the system has a total mass of >= 3-6 x 10^13 M_sun, and show that it will likely evolve into a >~ 10^14 M_sun cluster at z = 0. The overdensity includes a powerful Compton-thick Fanaroff-Riley type II (FRII) radio-galaxy, around which we discovered a large molecular gas reservoir (M_H2 ~ 2 x 10^11 M_sun). We fitted the FRII resolved CO emission with a 2-D Gaussian model with major (minor) axis of ~ 27 (~ 17) kpc, that is a factor of ~3 larger than the optical rest-frame emission. Under the assumption of a simple edge-on disk morphology, we find that the galaxy interstellar medium produces a column density towards the nucleus of ~ 5.5 x 10^23 cm^-2. Such a dense ISM may then contribute significantly to the total nuclear obscuration measured in the X-rays (N_(H,X) ~ 1.5 x 10^24 cm^-2) in addition to a small, pc-scale absorber around the central engine. The velocity map of this source unveils a rotational motion of the gas that is perpendicular to the radio-jets. The FRII is located at the center of the projected spatial distribution of the structure members, and its velocity offset from the peak of the redshift distribution is well within the structure's velocity dispersion. All this, coupled with the large amount of gas around the FRII, its stellar mass of ~ 3 x 10^11 M_sun, SFR of ~ 200-600 M_sun/yr, and powerful radio-to-X-ray emission, suggests that this source is the likely progenitor of the future brightest cluster galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.13665v1-abstract-full').style.display = 'none'; document.getElementById('2008.13665v1-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 August, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2020. </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">7 pages, 4 figures, 2 tables. Accepted for publication as a Letter 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/2003.08631">arXiv:2003.08631</a> <span> [<a href="https://arxiv.org/pdf/2003.08631">pdf</a>, <a href="https://arxiv.org/format/2003.08631">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/10.1051/0004-6361/201936175">10.1051/0004-6361/201936175 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Dust and gas content of high-redshift galaxies hosting obscured AGN in the CDF-S </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=D%27Amato%2C+Q">Q. D'Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">R. Gilli</a>, <a href="/search/astro-ph?searchtype=author&query=Vignali%2C+C">C. Vignali</a>, <a href="/search/astro-ph?searchtype=author&query=Massardi%2C+M">M. Massardi</a>, <a href="/search/astro-ph?searchtype=author&query=Pozzi%2C+F">F. Pozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Zamorani%2C+G">G. Zamorani</a>, <a href="/search/astro-ph?searchtype=author&query=Circosta%2C+C">C. Circosta</a>, <a href="/search/astro-ph?searchtype=author&query=Vito%2C+F">F. Vito</a>, <a href="/search/astro-ph?searchtype=author&query=Fritz%2C+J">J. Fritz</a>, <a href="/search/astro-ph?searchtype=author&query=Cresci%2C+G">G. Cresci</a>, <a href="/search/astro-ph?searchtype=author&query=Casasola%2C+V">V. Casasola</a>, <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">F. Calura</a>, <a href="/search/astro-ph?searchtype=author&query=Feltre%2C+A">A. Feltre</a>, <a href="/search/astro-ph?searchtype=author&query=Manieri%2C+V">V. Manieri</a>, <a href="/search/astro-ph?searchtype=author&query=Rigopoulou%2C+D">D. Rigopoulou</a>, <a href="/search/astro-ph?searchtype=author&query=Tozzi%2C+P">P. Tozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Norman%2C+C">C. 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="2003.08631v1-abstract-short" style="display: inline;"> Obscured AGN represent a significant fraction of the entire AGN population, especially at high redshift (~70% at z=3--5). They are often characterized by the presence of large gas and dust reservoirs that are thought to sustain and possibly obscure vigorous star formation processes that make these objects shine at far-IR and sub-mm wavelengths. We exploit ALMA Cycle 4 observations of the continuum… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.08631v1-abstract-full').style.display = 'inline'; document.getElementById('2003.08631v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2003.08631v1-abstract-full" style="display: none;"> Obscured AGN represent a significant fraction of the entire AGN population, especially at high redshift (~70% at z=3--5). They are often characterized by the presence of large gas and dust reservoirs that are thought to sustain and possibly obscure vigorous star formation processes that make these objects shine at far-IR and sub-mm wavelengths. We exploit ALMA Cycle 4 observations of the continuum (~2.1mm) and high-J CO emission of a sample of six X-ray selected SMGs hosting an obscured AGN at z_spec>2.5 in the 7 Ms CDF-S. We measured the masses and sizes of the dust and molecular gas and we derived the gas density and column density on the basis of a uniform sphere geometry. Finally, we compared the measured column densities with those derived from the Chandra X-ray spectra. We detected both the continuum and line emission for three sources for which we measured both the flux density and size. For the undetected sources, we derived an upper limit on the flux density. We found that the detected galaxies are rich in gas and dust (molecular gas mass in the range <0.5 - 2.7 x 10^10 M_sun for 伪_CO=0.8 and up to ~2 x 10^11~M_sun for 伪_CO=6.5, and dust mass <0.9 - 4.9 x 10^8 M_sun) and compact (gas major axis 2.1-3.0 kpc, dust major axis 1.4-2.7 kpc). The column densities associated with the ISM are on the order of 10^(23-24) cm-2, which is comparable with those derived from the X-ray spectra. For the detected sources we also derived dynamical masses in the range 0.8 - 3.7 x 10^10 M_sun. We conclude that the ISM of high redshift galaxies can substantially contribute to nuclear obscuration up to the Compton-thick (>10^24 cm-2) regime. In addition, we found that all the detected sources show a velocity gradient reminding one rotating system, even though two of them show peculiar features in their morphology that can be associated with a chaotic, possibly merging, structure. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.08631v1-abstract-full').style.display = 'none'; document.getElementById('2003.08631v1-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 March, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2020. </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, 6 figures, 7 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 636, A37 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1909.00814">arXiv:1909.00814</a> <span> [<a href="https://arxiv.org/pdf/1909.00814">pdf</a>, <a href="https://arxiv.org/format/1909.00814">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/10.1051/0004-6361/201936121">10.1051/0004-6361/201936121 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery of a galaxy overdensity around a powerful, heavily obscured FRII radio galaxy at z=1.7: star formation promoted by large-scale AGN feedback? </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=Mignoli%2C+M">M. Mignoli</a>, <a href="/search/astro-ph?searchtype=author&query=Peca%2C+A">A. Peca</a>, <a href="/search/astro-ph?searchtype=author&query=Nanni%2C+R">R. Nanni</a>, <a href="/search/astro-ph?searchtype=author&query=Prandoni%2C+I">I. Prandoni</a>, <a href="/search/astro-ph?searchtype=author&query=Liuzzo%2C+E">E. Liuzzo</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=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">F. Calura</a>, <a href="/search/astro-ph?searchtype=author&query=Caminha%2C+G+B">G. B. Caminha</a>, <a href="/search/astro-ph?searchtype=author&query=Chiaberge%2C+M">M. Chiaberge</a>, <a href="/search/astro-ph?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/astro-ph?searchtype=author&query=Cucciati%2C+O">O. Cucciati</a>, <a href="/search/astro-ph?searchtype=author&query=Cusano%2C+F">F. Cusano</a>, <a href="/search/astro-ph?searchtype=author&query=Grandi%2C+P">P. Grandi</a>, <a href="/search/astro-ph?searchtype=author&query=Decarli%2C+E">E. Decarli</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>, <a href="/search/astro-ph?searchtype=author&query=Pinna%2C+E">E. Pinna</a>, <a href="/search/astro-ph?searchtype=author&query=Tozzi%2C+P">P. Tozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</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=Balmaverde%2C+B">B. Balmaverde</a>, <a href="/search/astro-ph?searchtype=author&query=Citro%2C+A">A. Citro</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="1909.00814v2-abstract-short" style="display: inline;"> We report the discovery of a galaxy overdensity around a Compton-thick Fanaroff-Riley type II (FRII) radio galaxy at z=1.7 in the deep multiband survey around the z=6.3 QSO SDSS J1030+0524. Based on a 6hr VLT/MUSE and on a 4hr LBT/LUCI observation, we identify at least eight galaxy members in this structure with spectroscopic redshift z=1.687-1.699, including the FRII galaxy at z=1.699. Most of th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.00814v2-abstract-full').style.display = 'inline'; document.getElementById('1909.00814v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1909.00814v2-abstract-full" style="display: none;"> We report the discovery of a galaxy overdensity around a Compton-thick Fanaroff-Riley type II (FRII) radio galaxy at z=1.7 in the deep multiband survey around the z=6.3 QSO SDSS J1030+0524. Based on a 6hr VLT/MUSE and on a 4hr LBT/LUCI observation, we identify at least eight galaxy members in this structure with spectroscopic redshift z=1.687-1.699, including the FRII galaxy at z=1.699. Most of the identified overdensity members are blue, compact galaxies that are actively forming stars at rates of $\sim$8-60 $M_{\odot}$ yr$^{-1}$. Based on a 500ks Chandra ACIS-I observation we found that the FRII nucleus hosts a luminous QSO ($L_{2-10keV}=1.3\times10^{44}$ erg s$^{-1}$, intrinsic and rest-frame) that is obscured by Compton-thick absorption ($N_H=1.5\pm0.6\times 10^{24}$ cm$^{-2}$). Our Chandra observation, the deepest so far for a distant FRII within a galaxy overdensity, revealed significant diffuse X-ray emission within the region covered by the overdensity. In particular, X-ray emission extending for $\sim$240 kpc is found around the Eastern lobe of the FRII. Four out of the six MUSE star forming galaxies in the overdensity are distributed in an arc-like shape at the edge of this diffuse X-ray emission. The probability of observing by chance four out of the six $z=1.7$ sources at the edge of the diffuse emission is negligible. In addition, these four galaxies have the highest specific star formation rates of the MUSE galaxies in the overdensity and lie above the main sequence of field galaxies of equal stellar mass at z=1.7. We propose that the diffuse X-rays originate from an expanding bubble of gas that is shock-heated by the FRII jet, and that star formation is promoted by the compression of the cold interstellar medium of the galaxies around the bubble, which may be remarkable evidence of positive AGN feedback on cosmological scales. [shortened version] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.00814v2-abstract-full').style.display = 'none'; document.getElementById('1909.00814v2-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> 18 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2019. </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, 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 632, A26 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1807.03378">arXiv:1807.03378</a> <span> [<a href="https://arxiv.org/pdf/1807.03378">pdf</a>, <a href="https://arxiv.org/format/1807.03378">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/10.1051/0004-6361/201833040">10.1051/0004-6361/201833040 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The molecular gas content in obscured AGN at z > 1 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Perna%2C+M">M. Perna</a>, <a href="/search/astro-ph?searchtype=author&query=Sargent%2C+M+T">M. T. Sargent</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">E. Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Feruglio%2C+C">C. Feruglio</a>, <a href="/search/astro-ph?searchtype=author&query=Cresci%2C+G">G. Cresci</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzuisi%2C+G">G. Lanzuisi</a>, <a href="/search/astro-ph?searchtype=author&query=Lusso%2C+E">E. Lusso</a>, <a href="/search/astro-ph?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/astro-ph?searchtype=author&query=Coogan%2C+R+T">R. T. Coogan</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=Gilli%2C+R">R. Gilli</a>, <a href="/search/astro-ph?searchtype=author&query=Piconcelli%2C+E">E. Piconcelli</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="1807.03378v1-abstract-short" style="display: inline;"> The standard AGN-galaxy co-evolutionary scenario predicts a phase of deeply buried supermassive black hole growth coexisting with a starburst (SB) before feedback phenomena deplete the cold molecular gas reservoir of the galaxy and an optically luminous QSO is revealed ('SB-QSO evolutionary sequence'). The aim of this work is to measure the cold gas reservoir of three highly obscured QSOs to test… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.03378v1-abstract-full').style.display = 'inline'; document.getElementById('1807.03378v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1807.03378v1-abstract-full" style="display: none;"> The standard AGN-galaxy co-evolutionary scenario predicts a phase of deeply buried supermassive black hole growth coexisting with a starburst (SB) before feedback phenomena deplete the cold molecular gas reservoir of the galaxy and an optically luminous QSO is revealed ('SB-QSO evolutionary sequence'). The aim of this work is to measure the cold gas reservoir of three highly obscured QSOs to test if their gas fraction is similar to that of sub-millimeter galaxies (SMGs), as expected by some models, and place these measurements in the context of the SB-QSO framework. We target CO(1-0) transition in BzK4892, a Compton Thick (CT) QSO at z=2.6, CO(1-0) in BzK8608 and CO(2-1) in CDF153, two highly obscured QSOs at z=2.5 and z=1.5, respectively. For all these targets, we place 3$蟽$ upper limits on the CO, with $L'_{CO} < (1.5梅2.8)\times 10^{10}$ K km/s pc$^2$. We also compare the molecular gas conditions of our targets with those of other systems at z>1, considering normal star forming galaxies and SMGs, unobscured and obscured AGN from the literature. For the AGN samples, we provide an updated and (almost) complete collection of targets with CO follow-up. BzK4892 displays a high star formation efficiency (SFE$=L_{IR}/L'_{CO}>410$ L$_{\odot}$/(K km s$^{-1}$ pc$^2$)) and a gas fraction $f_{gas}<0.1$. Less stringent constraints are derived for the other two targets ($f_{gas}<0.5$ and SFE$>10$). From the comparison with literature data, we found that a) obscured AGN at z>1 are associated with higher SFE and lower $f_{gas}$ with respect to star forming galaxies; b) mildly and highly obscured active galaxies have comparable gas fractions; c) the SFE of CT and obscured AGN are similar to those of unobscured AGN. Within the SB-QSO framework, these findings could be consistent with a scenario where feedback can impact the host galaxy already from the early phases of the SB-QSO sequence. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.03378v1-abstract-full').style.display = 'none'; document.getElementById('1807.03378v1-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 July, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2018. </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, 7 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 619, A90 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1505.02507">arXiv:1505.02507</a> <span> [<a href="https://arxiv.org/pdf/1505.02507">pdf</a>, <a href="https://arxiv.org/format/1505.02507">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/10.1007/s10509-015-2570-6">10.1007/s10509-015-2570-6 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Application of the MST clustering to the high energy gamma-ray sky. I - New possible detection of high-energy gamma-ray emission associated with BL Lac objects </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Campana%2C+R">R. Campana</a>, <a href="/search/astro-ph?searchtype=author&query=Massaro%2C+E">E. Massaro</a>, <a href="/search/astro-ph?searchtype=author&query=Bernieri%2C+E">E. Bernieri</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Amato%2C+Q">Q. D'Amato</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="1505.02507v2-abstract-short" style="display: inline;"> In this paper we show an application of the Minimum Spanning Tree (MST) clustering method to the high-energy gamma-ray sky observed at energies higher than 10 GeV in 6.3 years by the Fermi-Large Area Telescope. We report the detection of 19 new high-energy gamma-ray clusters with good selection parameters whose centroid coordinates were found matching the positions of known BL Lac objects in the 5… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1505.02507v2-abstract-full').style.display = 'inline'; document.getElementById('1505.02507v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1505.02507v2-abstract-full" style="display: none;"> In this paper we show an application of the Minimum Spanning Tree (MST) clustering method to the high-energy gamma-ray sky observed at energies higher than 10 GeV in 6.3 years by the Fermi-Large Area Telescope. We report the detection of 19 new high-energy gamma-ray clusters with good selection parameters whose centroid coordinates were found matching the positions of known BL Lac objects in the 5th Edition of the Roma-BZCAT catalogue. A brief summary of the properties of these sources is presented. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1505.02507v2-abstract-full').style.display = 'none'; document.getElementById('1505.02507v2-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 November, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 May, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2015. </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, 7 figures. Accepted for publication in Astrophysics & Space Science</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophysics and Space Science, Volume 360, article id.19, 2015 </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path 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