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<button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Sani%2C+E&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Sani%2C+E&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Sani%2C+E&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> </ul> </nav> <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/2407.20327">arXiv:2407.20327</a> <span> [<a href="https://arxiv.org/pdf/2407.20327">pdf</a>, <a href="https://arxiv.org/format/2407.20327">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/10.1051/0004-6361/202451696">10.1051/0004-6361/202451696 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Extreme Ionizing Properties of Metal-Poor, Muv ~ -12 Star Complex in the first Gyr </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Loiacono%2C+F">F. Loiacono</a>, <a href="/search/astro-ph?searchtype=author&query=Messa%2C+M">M. Messa</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">P. Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Zanella%2C+A">A. Zanella</a>, <a href="/search/astro-ph?searchtype=author&query=Annibali%2C+F">F. Annibali</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+B">B. Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">M. Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Adamo%2C+A">A. Adamo</a>, <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">F. Calura</a>, <a href="/search/astro-ph?searchtype=author&query=Ricotti%2C+M">M. Ricotti</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=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Bradac%2C+M">M. Bradac</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C+J">C. J. Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=Yan%2C+H">H. Yan</a>, <a href="/search/astro-ph?searchtype=author&query=Bolamperti%2C+A">A. Bolamperti</a>, <a href="/search/astro-ph?searchtype=author&query=Mestric%2C+U">U. Mestric</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">R. Gilli</a>, <a href="/search/astro-ph?searchtype=author&query=Gronke%2C+M">M. Gronke</a>, <a href="/search/astro-ph?searchtype=author&query=Willott%2C+C">C. Willott</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Acebron%2C+A">A. Acebron</a> , et al. (16 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="2407.20327v1-abstract-short" style="display: inline;"> We report the serendipitous discovery of a faint (M_UV > -12.2), low-metallicity (Z ~ 0.02 Zsun), ionizing source (dubbed T2c) with a spectroscopic redshift of z=6.146. T2c is part of a larger structure amplified by the Hubble Frontier Field galaxy cluster MACSJ0416, and was observed with JWST/NIRSpec IFU. Stacking the short-wavelength NIRCam data reveals no stellar continuum detection down to a m… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.20327v1-abstract-full').style.display = 'inline'; document.getElementById('2407.20327v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.20327v1-abstract-full" style="display: none;"> We report the serendipitous discovery of a faint (M_UV > -12.2), low-metallicity (Z ~ 0.02 Zsun), ionizing source (dubbed T2c) with a spectroscopic redshift of z=6.146. T2c is part of a larger structure amplified by the Hubble Frontier Field galaxy cluster MACSJ0416, and was observed with JWST/NIRSpec IFU. Stacking the short-wavelength NIRCam data reveals no stellar continuum detection down to a magnitude limit of m_UV ~ 31.0 (3 sigma). However, prominent Hb, [OIII]4959,5007, and Ha emissions are detected, with equivalent widths exceeding 200A, 800A, and 1300A (3 sigma), respectively. The corresponding intrinsic (magnification-corrected x23 +/- 3) ultraviolet and optical rest-frame magnitudes exceed 34.4 and 33.9 (corresponding to M_uv and M_opt fainter than -12.2 and -12.8, at lambda_rest ~ 2000A and ~5000A, respectively), suggesting a stellar mass lower than a few 10^4 Msun under an instantaneous burst scenario. The inferred ionizing photon production efficiency (xi_ion) is high, xi_ion >~ 26.08(25.86) 3(5)sigma, assuming no dust attenuation and no Lyman continuum leakage, indicating the presence of massive stars despite the low mass of the object. The very poor sampling of the initial mass function at such low mass star-forming complex suggests that the formation of very massive stars might be favored in very low metallicity environments. T2c is surrounded by Balmer and weak oxygen emission on a spatial scale of a few hundred parsecs after correcting for lensing effects. This system resembles an HII region potentially powered by currently undetected, extremely efficient, low-metallicity star complexes or clusters. We propose that massive O-type stars populate this low-mass and metallicity high-redshift satellites, likely caught in an early and short formation phase, contributing to the ionization of the surrounding medium. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.20327v1-abstract-full').style.display = 'none'; document.getElementById('2407.20327v1-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 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 5 figures, 1 table. Submitted to A&A. Comments are welcome</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 691, A251 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.17552">arXiv:2405.17552</a> <span> [<a href="https://arxiv.org/pdf/2405.17552">pdf</a>, <a href="https://arxiv.org/format/2405.17552">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/10.1051/0004-6361/202449247">10.1051/0004-6361/202449247 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The host galaxy of low-luminosity compact sources </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vietri%2C+A">A. Vietri</a>, <a href="/search/astro-ph?searchtype=author&query=Berton%2C+M">M. Berton</a>, <a href="/search/astro-ph?searchtype=author&query=J%C3%A4rvel%C3%A4%2C+E">E. J盲rvel盲</a>, <a href="/search/astro-ph?searchtype=author&query=Kunert-Bajraszewska%2C+M">M. Kunert-Bajraszewska</a>, <a href="/search/astro-ph?searchtype=author&query=Ciroi%2C+S">S. Ciroi</a>, <a href="/search/astro-ph?searchtype=author&query=Varglund%2C+I">I. Varglund</a>, <a href="/search/astro-ph?searchtype=author&query=Barba%2C+B+D">B. Dalla Barba</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Crepaldi%2C+L">L. Crepaldi</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.17552v1-abstract-short" style="display: inline;"> The term 'active galactic nuclei' (AGN) subtends a huge variety of objects, classified on their properties at different wavelengths. Peaked sources (PS) represent a class of AGN at the first stage of evolution, characterised by a peaked radio spectrum. Among these radio sources, low-luminosity compact (LLC) sources can be identified as PS accreting with a high Eddington rate, harbouring low-power… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.17552v1-abstract-full').style.display = 'inline'; document.getElementById('2405.17552v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.17552v1-abstract-full" style="display: none;"> The term 'active galactic nuclei' (AGN) subtends a huge variety of objects, classified on their properties at different wavelengths. Peaked sources (PS) represent a class of AGN at the first stage of evolution, characterised by a peaked radio spectrum. Among these radio sources, low-luminosity compact (LLC) sources can be identified as PS accreting with a high Eddington rate, harbouring low-power jets and hosting low-mass black holes. These properties are also shared by narrow-line Seyfert 1 galaxies (NLS1s). In 2016, LLCs were hypothesised to be the parent population of NLS1s with a flat radio spectrum (F-NLS1s), suggesting the former to be the same objects as the latter, seen at higher inclination. Based on radio luminosity functions and optical spectra analysis, 10 LLCs were identified as valid candidates for F-NLS1s. To account for the missing puzzle piece, verifying if these LLCs could be hosted in late-type galaxies as NLS1s, we performed the photometric decomposition of their Pan-STARRS1 images in all five filters. We used the 2D fitting algorithm GALFIT for the single-band analysis, and its extension GALFITM for the multi-band analysis. Considering that the morphological type and the structural parameters of the host can be dependent on the wavelength, we found six out of ten LLCs hosted in late-type galaxies, probably with pseudo-bulges, three point-like sources and one object of uncertain classification. Although this study is based on a small sample, it represents the first morphological analysis of LLC host galaxies. The results confirm the trend observed in NLS1s, indicating late-type/disc-like host galaxies for LLCs and supporting the validity of the parent population scenario. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.17552v1-abstract-full').style.display = 'none'; document.getElementById('2405.17552v1-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 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 21 figures, accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 689, A123 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.10238">arXiv:2403.10238</a> <span> [<a href="https://arxiv.org/pdf/2403.10238">pdf</a>, <a href="https://arxiv.org/format/2403.10238">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"> JWST NIRSpec Spectroscopy of the Remarkable Bright Galaxy GHZ2/GLASS-z12 at Redshift 12.34 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">Marco Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Napolitano%2C+L">Lorenzo Napolitano</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">Adriano Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Roberts-Borsani%2C+G">Guido Roberts-Borsani</a>, <a href="/search/astro-ph?searchtype=author&query=Treu%2C+T">Tommaso Treu</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">Eros Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Zavala%2C+J+A">Jorge A. Zavala</a>, <a href="/search/astro-ph?searchtype=author&query=Haro%2C+P+A">Pablo Arrabal Haro</a>, <a href="/search/astro-ph?searchtype=author&query=Calabr%C3%B2%2C+A">Antonello Calabr貌</a>, <a href="/search/astro-ph?searchtype=author&query=Llerena%2C+M">Mario Llerena</a>, <a href="/search/astro-ph?searchtype=author&query=Mascia%2C+S">Sara Mascia</a>, <a href="/search/astro-ph?searchtype=author&query=Merlin%2C+E">Emiliano Merlin</a>, <a href="/search/astro-ph?searchtype=author&query=Paris%2C+D">Diego Paris</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">Laura Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Santini%2C+P">Paola Santini</a>, <a href="/search/astro-ph?searchtype=author&query=Bakx%2C+T+J+L+C">Tom J. L. C. Bakx</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">Pietro Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Cupani%2C+G">Guido Cupani</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">Mark Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Filippenko%2C+A+V">Alexei V. Filippenko</a>, <a href="/search/astro-ph?searchtype=author&query=Glazebrook%2C+K">Karl Glazebrook</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">Claudio Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Kelly%2C+P+L">Patrick L. Kelly</a>, <a href="/search/astro-ph?searchtype=author&query=Malkan%2C+M+A">Matthew A. Malkan</a>, <a href="/search/astro-ph?searchtype=author&query=Mason%2C+C+A">Charlotte A. Mason</a> , et al. (6 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="2403.10238v2-abstract-short" style="display: inline;"> We spectroscopically confirm the $M_{\rm UV} = -20.5$ mag galaxy GHZ2/GLASS-z12 to be at redshift $z=12.34$. The source was selected via NIRCam photometry in GLASS-JWST ERS data, providing the first evidence of a surprising abundance of bright galaxies at $z \gtrsim 10$. The NIRSpec PRISM spectrum shows detections of N IV, C IV, He II, O III, C III, O II, and Ne III lines, and the first detection… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.10238v2-abstract-full').style.display = 'inline'; document.getElementById('2403.10238v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.10238v2-abstract-full" style="display: none;"> We spectroscopically confirm the $M_{\rm UV} = -20.5$ mag galaxy GHZ2/GLASS-z12 to be at redshift $z=12.34$. The source was selected via NIRCam photometry in GLASS-JWST ERS data, providing the first evidence of a surprising abundance of bright galaxies at $z \gtrsim 10$. The NIRSpec PRISM spectrum shows detections of N IV, C IV, He II, O III, C III, O II, and Ne III lines, and the first detection at high-redshift of the O III Bowen fluorescence line at 3133 脜 rest-frame. The prominent C IV line with rest-frame equivalent width (EW) $\approx 46$ 脜 puts GHZ2 in the category of extreme C IV emitters. GHZ2 displays UV lines with EWs that are only found in active galactic nuclei (AGNs) or composite objects at low/intermediate redshifts. The UV line-intensity ratios are compatible both with AGNs and star formation in a low-metallicity environment, with the low limit on the [Ne IV]/[N IV] ratio favoring a stellar origin of the ionizing photons. We discuss a possible scenario in which the high ionizing output is due to low metallicity stars forming in a dense environment. We estimate a metallicity $\lesssim 0.1 Z/{\rm Z}_{\odot}$, a high ionization parameter logU $> -2$, a N/O abundance 4--5 times the solar value, and a subsolar C/O ratio similar to the recently discovered class of nitrogen-enhanced objects. Considering its abundance patterns and the high stellar mass density ($10^4$~M$_{\odot}$~pc$^{-2}$), GHZ2 is an ideal formation site for the progenitors of today's globular clusters. The remarkable brightness of GHZ2 makes it a ``Rosetta stone'' for understanding the physics of galaxy formation within just 360 Myr after the Big Bang. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.10238v2-abstract-full').style.display = 'none'; document.getElementById('2403.10238v2-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> 3 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 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">Accepted for publication in The Astrophysical Journal. 20 pages, 7 figures, 2 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/2309.10956">arXiv:2309.10956</a> <span> [<a href="https://arxiv.org/pdf/2309.10956">pdf</a>, <a href="https://arxiv.org/format/2309.10956">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/10.3847/1538-4365/ace1f5">10.3847/1538-4365/ace1f5 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Powerful Radio Sources in the Southern Sky. II. A SWIFT X-Ray Perspective </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Massaro%2C+F">F. Massaro</a>, <a href="/search/astro-ph?searchtype=author&query=White%2C+S+V">S. V. White</a>, <a href="/search/astro-ph?searchtype=author&query=Paggi%2C+A">A. Paggi</a>, <a href="/search/astro-ph?searchtype=author&query=Jimenez-Gallardo%2C+A">A. Jimenez-Gallardo</a>, <a href="/search/astro-ph?searchtype=author&query=Madrid%2C+J+P">J. P. Madrid</a>, <a href="/search/astro-ph?searchtype=author&query=Mazzucchelli%2C+C">C. Mazzucchelli</a>, <a href="/search/astro-ph?searchtype=author&query=Forman%2C+W+R">W. R. Forman</a>, <a href="/search/astro-ph?searchtype=author&query=Capetti%2C+A">A. Capetti</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+C">C. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia-Perez%2C+A">A. Garcia-Perez</a>, <a href="/search/astro-ph?searchtype=author&query=Cheung%2C+C+C">C. C. Cheung</a>, <a href="/search/astro-ph?searchtype=author&query=Chavushyan%2C+V">V. Chavushyan</a>, <a href="/search/astro-ph?searchtype=author&query=Nesvadba%2C+N+P+H">N. P. H. Nesvadba</a>, <a href="/search/astro-ph?searchtype=author&query=Andruchow%2C+I">I. Andruchow</a>, <a href="/search/astro-ph?searchtype=author&query=Pena-Herazo%2C+H+A">H. A. Pena-Herazo</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Grossova%2C+R">R. Grossova</a>, <a href="/search/astro-ph?searchtype=author&query=Reynaldi%2C+V">V. Reynaldi</a>, <a href="/search/astro-ph?searchtype=author&query=Kraft%2C+R+P">R. P. Kraft</a>, <a href="/search/astro-ph?searchtype=author&query=Balmaverde%2C+B">B. Balmaverde</a>, <a href="/search/astro-ph?searchtype=author&query=Cellone%2C+S">S. Cellone</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2309.10956v1-abstract-short" style="display: inline;"> We recently constructed the G4Jy-3CRE, a catalog of extragalactic radio sources based on the GLEAM 4-Jy (G4Jy) sample, with the aim of increasing the number of powerful radio galaxies and quasars with similar selection criteria to those of the revised release of the Third Cambridge catalog (3CR). The G4Jy-3CRE consists of a total of 264 radio sources mainly visible from the Southern Hemisphere. He… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.10956v1-abstract-full').style.display = 'inline'; document.getElementById('2309.10956v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.10956v1-abstract-full" style="display: none;"> We recently constructed the G4Jy-3CRE, a catalog of extragalactic radio sources based on the GLEAM 4-Jy (G4Jy) sample, with the aim of increasing the number of powerful radio galaxies and quasars with similar selection criteria to those of the revised release of the Third Cambridge catalog (3CR). The G4Jy-3CRE consists of a total of 264 radio sources mainly visible from the Southern Hemisphere. Here, we present an initial X-ray analysis of 89 G4Jy-3CRE radio sources with archival X- ray observations from the Neil Gehrels Swift Observatory. We reduced a total of 615 Swift observations, for about 0.89 Msec of integrated exposure time, we found X-ray counterparts for 61 radio sources belonging to the G4Jy-3CRE, 11 of them showing extended X-ray emission. The remaining 28 sources do not show any X-ray emission associated with their radio cores. Our analysis demonstrates that X-ray snapshot observations, even if lacking uniform exposure times, as those carried out with Swift, allow us to (i) verify and/or re ne the host galaxy identi cation; (ii) discover the extended X-ray emission around radio galaxies of the intracluster medium when harbored in galaxy clusters, as the case of G4Jy 1518 and G4Jy 1664, and (iii) detect X-ray radiation arising from their radio lobes, as for G4Jy 1863. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.10956v1-abstract-full').style.display = 'none'; document.getElementById('2309.10956v1-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 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">35 pages, 17 figures, 2 tables; second paper of a series, pre-proof version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal Supplement Series, 268, 32 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.10071">arXiv:2308.10071</a> <span> [<a href="https://arxiv.org/pdf/2308.10071">pdf</a>, <a href="https://arxiv.org/format/2308.10071">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/10.3847/1538-4365/acaf05">10.3847/1538-4365/acaf05 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Powerful Radio Sources in the Southern Sky. I. Optical Identifications </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Massaro%2C+F">F. Massaro</a>, <a href="/search/astro-ph?searchtype=author&query=White%2C+S+V">S. V. White</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia-Perez%2C+A">A. Garcia-Perez</a>, <a href="/search/astro-ph?searchtype=author&query=Jimenez-Gallardo%2C+A">A. Jimenez-Gallardo</a>, <a href="/search/astro-ph?searchtype=author&query=Capetti%2C+A">A. Capetti</a>, <a href="/search/astro-ph?searchtype=author&query=Cheung%2C+C+C">C. C. Cheung</a>, <a href="/search/astro-ph?searchtype=author&query=Forman%2C+W+R">W. R. Forman</a>, <a href="/search/astro-ph?searchtype=author&query=Mazzucchelli%2C+C">C. Mazzucchelli</a>, <a href="/search/astro-ph?searchtype=author&query=Paggi%2C+A">A. Paggi</a>, <a href="/search/astro-ph?searchtype=author&query=Nesvadba%2C+N+P+H">N. P. H. Nesvadba</a>, <a href="/search/astro-ph?searchtype=author&query=Madrid%2C+J+P">J. P. Madrid</a>, <a href="/search/astro-ph?searchtype=author&query=Andruchow%2C+I">I. Andruchow</a>, <a href="/search/astro-ph?searchtype=author&query=Cellone%2C+S">S. Cellone</a>, <a href="/search/astro-ph?searchtype=author&query=Pena-Herazo%2C+H+A">H. A. Pena-Herazo</a>, <a href="/search/astro-ph?searchtype=author&query=Grossova%2C+R">R. Grossova</a>, <a href="/search/astro-ph?searchtype=author&query=Balmaverde%2C+B">B. Balmaverde</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Chavushyan%2C+V">V. Chavushyan</a>, <a href="/search/astro-ph?searchtype=author&query=Kraft%2C+R+P">R. P. Kraft</a>, <a href="/search/astro-ph?searchtype=author&query=Reynaldi%2C+V">V. Reynaldi</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+C">C. Leto</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="2308.10071v1-abstract-short" style="display: inline;"> Since the early sixties, our view of radio galaxies and quasars has been drastically shaped by discoveries made thanks to observations of radio sources listed in the Third Cambridge catalog and its revised version (3CR). However, the largest fraction of data collected to date on 3CR sources was performed with relatively old instruments, rarely repeated and/or updated. Importantly, the 3CR contains… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.10071v1-abstract-full').style.display = 'inline'; document.getElementById('2308.10071v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.10071v1-abstract-full" style="display: none;"> Since the early sixties, our view of radio galaxies and quasars has been drastically shaped by discoveries made thanks to observations of radio sources listed in the Third Cambridge catalog and its revised version (3CR). However, the largest fraction of data collected to date on 3CR sources was performed with relatively old instruments, rarely repeated and/or updated. Importantly, the 3CR contains only objects located in the Northern Hemisphere thus having limited access to new and innovative astronomical facilities. To mitigate these limitations we present a new catalog of powerful radio sources visible from the Southern Hemisphere, extracted from the GLEAM 4-Jy (G4Jy) catalog and based on equivalent selection criteria as the 3CR. This new catalog, named G4Jy- 3CRE, where the E stands for "equivalent", lists a total of 264 sources at declination below -5 degrees and with 9 Jy limiting sensitivity at ~178 MHz. We explored archival radio maps obtained with different surveys and compared then with optical images available in the Pan-STARRS, DES and DSS databases to search for optical counterparts of their radio cores. We compared mid-infrared counterparts, originally associated in the G4Jy, with the optical ones identified here and we present results of a vast literature search carried out to collect redshift estimates for all G4Jy-3CRE sources resulting in a total of 145 reliable z measurements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.10071v1-abstract-full').style.display = 'none'; document.getElementById('2308.10071v1-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 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">72 pages, 35 figures, 5 Tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal Supplement Series, 265, 32 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.14413">arXiv:2305.14413</a> <span> [<a href="https://arxiv.org/pdf/2305.14413">pdf</a>, <a href="https://arxiv.org/format/2305.14413">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/10.1051/0004-6361/202346981">10.1051/0004-6361/202346981 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An extremely metal poor star complex in the reionization era: Approaching Population III stars with JWST </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Loiacono%2C+F">F. Loiacono</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">P. Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Mestric%2C+U">U. Mestric</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</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=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">F. Calura</a>, <a href="/search/astro-ph?searchtype=author&query=Mignoli%2C+M">M. Mignoli</a>, <a href="/search/astro-ph?searchtype=author&query=Bradac%2C+M">M. Bradac</a>, <a href="/search/astro-ph?searchtype=author&query=Adamo%2C+A">A. Adamo</a>, <a href="/search/astro-ph?searchtype=author&query=Rihtarsic%2C+G">G. Rihtarsic</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">M. Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Gronke%2C+M">M. Gronke</a>, <a href="/search/astro-ph?searchtype=author&query=Zanella%2C+A">A. Zanella</a>, <a href="/search/astro-ph?searchtype=author&query=Annibali%2C+F">F. Annibali</a>, <a href="/search/astro-ph?searchtype=author&query=Willott%2C+C">C. Willott</a>, <a href="/search/astro-ph?searchtype=author&query=Messa%2C+M">M. Messa</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Acebron%2C+A">A. Acebron</a>, <a href="/search/astro-ph?searchtype=author&query=Bolamperti%2C+A">A. Bolamperti</a>, <a href="/search/astro-ph?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">R. Gilli</a>, <a href="/search/astro-ph?searchtype=author&query=Caputi%2C+K+I">K. I. Caputi</a> , et al. (9 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2305.14413v1-abstract-short" style="display: inline;"> We present JWST/NIRSpec integral field spectroscopy (IFS) of a lensed Population III candidate stellar complex (dubbed Lensed And Pristine 1, LAP1), with a lensing-corrected stellar mass ~<10^4 Msun, absolute luminosity M_UV > -11.2 (m_UV > 35.6), confirmed at redshift 6.639 +/- 0.004. The system is strongly amplified (渭>~ 100) by straddling a critical line of the Hubble Frontier Field galaxy clus… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.14413v1-abstract-full').style.display = 'inline'; document.getElementById('2305.14413v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.14413v1-abstract-full" style="display: none;"> We present JWST/NIRSpec integral field spectroscopy (IFS) of a lensed Population III candidate stellar complex (dubbed Lensed And Pristine 1, LAP1), with a lensing-corrected stellar mass ~<10^4 Msun, absolute luminosity M_UV > -11.2 (m_UV > 35.6), confirmed at redshift 6.639 +/- 0.004. The system is strongly amplified (渭>~ 100) by straddling a critical line of the Hubble Frontier Field galaxy cluster MACS J0416. Despite the stellar continuum is currently not detected in the Hubble and JWST/NIRCam and NIRISS imaging, arclet-like shapes of Lyman and Balmer lines, Lya, Hg, Hb and Ha are detected with NIRSpec IFS with signal-to-noise ratios SNR=5-13 and large equivalent widths (>300-2000A), along with a remarkably weak [OIII]4959-5007 at SNR ~ 4. LAP1 shows a large ionizing photon production efficiency, log(尉_{ion}[erg~Hz^{-1}])>26. From the metallicity indexes R23 = ([OIII]4959-5007 + [OII]3727) / Hb ~< 0.74 and R3 = ([OIII]5007 / Hb) = 0.55 +/- 0.14, we derive an oxygen abundance 12+log(O/H) ~< 6.3. Intriguingly, the Ha emission is also measured in mirrored sub-components where no [OIII] is detected, providing even more stringent upper limits on the metallicity if in-situ star formation is ongoing in this region (12+log(O/H) < 6, or Z < 0.002 Zsun). The formal stellar mass limit of the sub-components would correspond to ~10^{3} Msun or M_UV fainter than -10. Alternatively, such a metal-free pure line emitting region could be the first case of a fluorescing HI gas region, induced by transverse escaping ionizing radiation from a nearby star-complex. The presence of large equivalent-width hydrogen lines and the deficiency of metal lines in such a small region, make LAP1 the most metal poor star-forming region currently known in the reionization era and a promising site that may host isolated, pristine stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.14413v1-abstract-full').style.display = 'none'; document.getElementById('2305.14413v1-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 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">15 pages, 10 figures, 1 table. Submitted to A&A. Comments welcome</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 678, A173 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.12109">arXiv:2303.12109</a> <span> [<a href="https://arxiv.org/pdf/2303.12109">pdf</a>, <a href="https://arxiv.org/format/2303.12109">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202245184">10.1051/0004-6361/202245184 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A redshifted excess in the broad emission lines after the flare of the $纬$-ray narrow-line Seyfert 1 PKS 2004-447 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hon%2C+W">W. Hon</a>, <a href="/search/astro-ph?searchtype=author&query=Berton%2C+M">M. Berton</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Webster%2C+R">R. Webster</a>, <a href="/search/astro-ph?searchtype=author&query=Wolf%2C+C">C. Wolf</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas%2C+A+F">A. F. Rojas</a>, <a href="/search/astro-ph?searchtype=author&query=Marziani%2C+P">P. Marziani</a>, <a href="/search/astro-ph?searchtype=author&query=Kotilainen%2C+J">J. Kotilainen</a>, <a href="/search/astro-ph?searchtype=author&query=Congiu%2C+E">E. Congiu</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="2303.12109v1-abstract-short" style="display: inline;"> PKS 2004-447 is a narrow-line Seyfert 1 (NLS1) harbouring a relativistic jet with gamma-ray emission. On 2019-10-25, the Fermi-Large Area Telescope captured a $纬$-ray flare from this source, offering a chance to study the broad-line region (BLR) and jet during such violent events. This can provide insights to the BLR structure and jet interactions, which are important for active galactic nuclei an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.12109v1-abstract-full').style.display = 'inline'; document.getElementById('2303.12109v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.12109v1-abstract-full" style="display: none;"> PKS 2004-447 is a narrow-line Seyfert 1 (NLS1) harbouring a relativistic jet with gamma-ray emission. On 2019-10-25, the Fermi-Large Area Telescope captured a $纬$-ray flare from this source, offering a chance to study the broad-line region (BLR) and jet during such violent events. This can provide insights to the BLR structure and jet interactions, which are important for active galactic nuclei and host galaxy coevolution. We report X-Shooter observations of enhancements in the broad line components of Balmer, Paschen and He I lines seen only during the post-flare and vanishing 1.5 years after. These features are biased redward up to $\sim$250 km s$^{-1}$ and are narrower than the pre-existing broad line profiles. This indicates a connection between the relativistic jet and the BLR of a young AGN, and how $纬$-ray production can lead to localised addition of broad emission lines. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.12109v1-abstract-full').style.display = 'none'; document.getElementById('2303.12109v1-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> 21 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">19 pages, 14 figures, 3 tables, including appendix. Accepted for publication on A&A Letters</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 672, L14 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.04481">arXiv:2211.04481</a> <span> [<a href="https://arxiv.org/pdf/2211.04481">pdf</a>, <a href="https://arxiv.org/format/2211.04481">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/10.3847/1538-4357/aca08b">10.3847/1538-4357/aca08b <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The cavity of 3CR 196.1: H$伪$ emission spatially associated with an X-ray cavity </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jimenez-Gallardo%2C+A">A. Jimenez-Gallardo</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">F. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Mazzucchelli%2C+C">C. Mazzucchelli</a>, <a href="/search/astro-ph?searchtype=author&query=Balmaverde%2C+B">B. Balmaverde</a>, <a href="/search/astro-ph?searchtype=author&query=Massaro%2C+F">F. Massaro</a>, <a href="/search/astro-ph?searchtype=author&query=Capetti%2C+A">A. Capetti</a>, <a href="/search/astro-ph?searchtype=author&query=Forman%2C+W+R">W. R. Forman</a>, <a href="/search/astro-ph?searchtype=author&query=Kraft%2C+R+P">R. P. Kraft</a>, <a href="/search/astro-ph?searchtype=author&query=Venturi%2C+G">G. Venturi</a>, <a href="/search/astro-ph?searchtype=author&query=Gendron-Marsolais%2C+M">M. Gendron-Marsolais</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+M+A">M. A. Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Marconi%2C+A">A. Marconi</a>, <a href="/search/astro-ph?searchtype=author&query=Pe%C3%B1a-Herazo%2C+H+A">H. A. Pe帽a-Herazo</a>, <a href="/search/astro-ph?searchtype=author&query=Baum%2C+S+A">S. A. Baum</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Dea%2C+C+P">C. P. O'Dea</a>, <a href="/search/astro-ph?searchtype=author&query=Lovisari%2C+L">L. Lovisari</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">R. Gilli</a>, <a href="/search/astro-ph?searchtype=author&query=Torresi%2C+E">E. Torresi</a>, <a href="/search/astro-ph?searchtype=author&query=Paggi%2C+A">A. Paggi</a>, <a href="/search/astro-ph?searchtype=author&query=Missaglia%2C+V">V. Missaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Tremblay%2C+G+R">G. R. Tremblay</a>, <a href="/search/astro-ph?searchtype=author&query=Wilkes%2C+B+J">B. J. Wilkes</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2211.04481v1-abstract-short" style="display: inline;"> We present a multifrequency analysis of the radio galaxy 3CR 196.1 ($z = 0.198$), associated with the brightest galaxy of the cool core cluster CIZAJ0815.4-0303. This nearby radio galaxy shows a hybrid radio morphology and an X-ray cavity, all signatures of a turbulent past activity, potentially due to merger events and AGN outbursts. We present results of the comparison between $Chandra$ and VLT/… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.04481v1-abstract-full').style.display = 'inline'; document.getElementById('2211.04481v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.04481v1-abstract-full" style="display: none;"> We present a multifrequency analysis of the radio galaxy 3CR 196.1 ($z = 0.198$), associated with the brightest galaxy of the cool core cluster CIZAJ0815.4-0303. This nearby radio galaxy shows a hybrid radio morphology and an X-ray cavity, all signatures of a turbulent past activity, potentially due to merger events and AGN outbursts. We present results of the comparison between $Chandra$ and VLT/MUSE data for the inner region of the galaxy cluster, on a scale of tens of kpc. We discovered H$伪$ + [N II]$\lambda6584$ emission spatially associated with the X-ray cavity (at $\sim$10 kpc from the galaxy nucleus) instead of with its rim. This result differs from previous discoveries of ionized gas surrounding X-ray cavities in other radio galaxies harbored in galaxy clusters and could represent the first reported case of ionized gas filling an X-ray cavity, either due to different AGN outbursts or to the cooling of warm ($10^4<T\leq10^7$ K) AGN outflows. We also found that the H$伪$, [N II]$位\lambda6548,6584$ and [S II]$位\lambda6718,6733$ emission lines show an additional redward component, at $\sim$1000 km$\,$s$^{-1}$ from rest frame, with no detection in H$尾$ or [O III]$位\lambda4960,5008$. We believe the most likely explanation for this redward component is the presence of a background gas cloud since there appears to be a discrete difference in velocities between this component and the rest frame. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.04481v1-abstract-full').style.display = 'none'; document.getElementById('2211.04481v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 8 figures, ApJ accepted, pre-proof 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/2204.05321">arXiv:2204.05321</a> <span> [<a href="https://arxiv.org/pdf/2204.05321">pdf</a>, <a href="https://arxiv.org/format/2204.05321">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/10.3847/1538-4365/ac6602">10.3847/1538-4365/ac6602 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> BASS XXV: DR2 Broad-line Based Black Hole Mass Estimates and Biases from Obscuration </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mej%C4%B1a-Restrepo%2C+J+E">Julian E. Mej谋a-Restrepo</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">Benny Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Koss%2C+M+J">Michael J. Koss</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+K">Kyuseok Oh</a>, <a href="/search/astro-ph?searchtype=author&query=Brok%2C+J+d">Jakob den Brok</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Powell%2C+M+C">Meredith C. Powell</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">Federica Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Caglar%2C+T">Turgay Caglar</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Treister%2C+E">Ezequiel Treister</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F+A">Fiona A. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Urry%2C+C+M">C. M. Urry</a>, <a href="/search/astro-ph?searchtype=author&query=Ananna%2C+T+T">Tonima Tasnim Ananna</a>, <a href="/search/astro-ph?searchtype=author&query=Asmus%2C+D">Daniel Asmus</a>, <a href="/search/astro-ph?searchtype=author&query=Assef%2C+R+J">Roberto J. Assef</a>, <a href="/search/astro-ph?searchtype=author&query=Bar%2C+R+E">Rudolf E. Bar</a>, <a href="/search/astro-ph?searchtype=author&query=Bessiere%2C+P+S">Patricia S. Bessiere</a>, <a href="/search/astro-ph?searchtype=author&query=Burtscher%2C+L">Leonard Burtscher</a>, <a href="/search/astro-ph?searchtype=author&query=Ichikawa%2C+K">Kohei Ichikawa</a>, <a href="/search/astro-ph?searchtype=author&query=Kakkad%2C+D">Darshan Kakkad</a>, <a href="/search/astro-ph?searchtype=author&query=Kamraj%2C+N">Nikita Kamraj</a>, <a href="/search/astro-ph?searchtype=author&query=Mushotzky%2C+R">Richard Mushotzky</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</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="2204.05321v2-abstract-short" style="display: inline;"> We present measurements of broad emission lines and virial estimates of supermassive black hole masses ($M_{BH}$) for a large sample of ultra-hard X-ray selected active galactic nuclei (AGNs) as part of the second data release of the BAT AGN Spectroscopic Survey (BASS/DR2). Our catalog includes $M_{BH}$ estimates for a total 689 AGNs, determined from the H$伪$, H$尾$, $MgII\lambda2798$, and/or… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.05321v2-abstract-full').style.display = 'inline'; document.getElementById('2204.05321v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.05321v2-abstract-full" style="display: none;"> We present measurements of broad emission lines and virial estimates of supermassive black hole masses ($M_{BH}$) for a large sample of ultra-hard X-ray selected active galactic nuclei (AGNs) as part of the second data release of the BAT AGN Spectroscopic Survey (BASS/DR2). Our catalog includes $M_{BH}$ estimates for a total 689 AGNs, determined from the H$伪$, H$尾$, $MgII\lambda2798$, and/or $CIV\lambda1549$ broad emission lines. The core sample includes a total of 512 AGNs drawn from the 70-month Swift/BAT all-sky catalog. We also provide measurements for 177 additional AGNs that are drawn from deeper Swift/BAT survey data. We study the links between $M_{BH}$ estimates and line-of-sight obscuration measured from X-ray spectral analysis. We find that broad H$伪$ emission lines in obscured AGNs ($\log (N_{\rm H}/{\rm cm}^{-2})> 22.0$) are on average a factor of $8.0_{-2.4}^{+4.1}$ weaker, relative to ultra-hard X-ray emission, and about $35_{-12}^{~+7}$\% narrower than in unobscured sources (i.e., $\log (N_{\rm H}/{\rm cm}^{-2}) < 21.5$). This indicates that the innermost part of the broad-line region is preferentially absorbed. Consequently, current single-epoch $M_{BH}$ prescriptions result in severely underestimated ($>$1 dex) masses for Type 1.9 sources (AGNs with broad H$伪$ but no broad H$尾$) and/or sources with $\log (N_{\rm H}/{\rm cm}^{-2}) > 22.0$. We provide simple multiplicative corrections for the observed luminosity and width of the broad H$伪$ component ($L[{\rm b}{\rm H}伪]$ and FWHM[bH$伪$]) in such sources to account for this effect, and to (partially) remedy $M_{BH}$ estimates for Type 1.9 objects. As key ingredient of BASS/DR2, our work provides the community with the data needed to further study powerful AGNs in the low-redshift Universe. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.05321v2-abstract-full').style.display = 'none'; document.getElementById('2204.05321v2-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> 25 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">published in ApJS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2202.09377">arXiv:2202.09377</a> <span> [<a href="https://arxiv.org/pdf/2202.09377">pdf</a>, <a href="https://arxiv.org/format/2202.09377">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/stac2309">10.1093/mnras/stac2309 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Exploring the physical properties of lensed star-forming clumps at $2\lesssim z \lesssim6$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Me%C5%A1tri%C4%87%2C+U">U. Me拧tri膰</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Zanella%2C+A">A. Zanella</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">F. Calura</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">P. Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">A. Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">M. Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">C. Grillo</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=Nonino%2C+M">M. Nonino</a>, <a href="/search/astro-ph?searchtype=author&query=Merlin%2C+E">E. Merlin</a>, <a href="/search/astro-ph?searchtype=author&query=Cupani%2C+G">G. Cupani</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</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="2202.09377v2-abstract-short" style="display: inline;"> We study the physical properties (size, stellar mass, luminosity, star formation rate) and scaling relations for a sample of 166 star-forming clumps with redshift $z \sim 2-6.2$. They are magnified by the Hubble Frontier Field galaxy cluster MACS~J0416 and have robust lensing magnification ($2\lesssim 渭\lesssim 82$) computed by using our high-precision lens model, based on 182 multiple images. Our… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.09377v2-abstract-full').style.display = 'inline'; document.getElementById('2202.09377v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.09377v2-abstract-full" style="display: none;"> We study the physical properties (size, stellar mass, luminosity, star formation rate) and scaling relations for a sample of 166 star-forming clumps with redshift $z \sim 2-6.2$. They are magnified by the Hubble Frontier Field galaxy cluster MACS~J0416 and have robust lensing magnification ($2\lesssim 渭\lesssim 82$) computed by using our high-precision lens model, based on 182 multiple images. Our sample extends by $\sim 3$ times the number of spectroscopically-confirmed lensed clumps at $z \gtrsim 2$. We identify clumps in ultraviolet continuum images and find that, whenever the effective spatial resolution (enhanced by gravitational lensing) increases, they fragment into smaller entities, likely reflecting the hierarchically-organized nature of star formation. Kpc-scale clumps, most commonly observed in field, are not found in our sample. The physical properties of our sample extend the parameter space typically probed by $z \gtrsim 1$ field observations and simulations, by populating the low mass (M$_\star \lesssim 10^7$ M$_\odot$), low star formation rate (SFR $\lesssim 0.5$ M$_\odot$ yr$^{-1}$), and small size (R$_\mathrm{eff} \lesssim 100$ pc) regime. The new domain probed by our study approaches the regime of compact stellar complexes and star clusters. In the mass-size plane, our sample spans the region between galaxies and globular clusters, with a few clumps in the region populated by young star clusters and globular-clusters. For the bulk of our sample, we measure star-formation rates which are higher than those observed locally in compact stellar systems, indicating different conditions for star formation at high redshift than in the local Universe. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.09377v2-abstract-full').style.display = 'none'; document.getElementById('2202.09377v2-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 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages, 20 figures, 3 table. Accepted to publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.04149">arXiv:2201.04149</a> <span> [<a href="https://arxiv.org/pdf/2201.04149">pdf</a>, <a href="https://arxiv.org/format/2201.04149">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stac103">10.1093/mnras/stac103 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> BASS XXXI: Outflow scaling relations in low redshift X-ray AGN host galaxies with MUSE </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kakkad%2C+D">D. Kakkad</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas%2C+A+F">A. F. Rojas</a>, <a href="/search/astro-ph?searchtype=author&query=Mallmann%2C+N+D">Nicolas D. Mallmann</a>, <a href="/search/astro-ph?searchtype=author&query=Veilleux%2C+S">S. Veilleux</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">F. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Mushotsky%2C+R">R. Mushotsky</a>, <a href="/search/astro-ph?searchtype=author&query=Koss%2C+M">M. Koss</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">C. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Treister%2C+E">E. Treister</a>, <a href="/search/astro-ph?searchtype=author&query=Privon%2C+G+C">George C. Privon</a>, <a href="/search/astro-ph?searchtype=author&query=Nguyen%2C+N">N. Nguyen</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%A4r%2C+R">R. B盲r</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">F. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+K">K. Oh</a>, <a href="/search/astro-ph?searchtype=author&query=Powell%2C+M">M. Powell</a>, <a href="/search/astro-ph?searchtype=author&query=Riffel%2C+R">R. Riffel</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">D. Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">B. Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Urry%2C+C+M">C. M. Urry</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="2201.04149v1-abstract-short" style="display: inline;"> Ionised gas kinematics provide crucial evidence of the impact that active galactic nuclei (AGN) have in regulating star formation in their host galaxies. Although the presence of outflows in AGN host galaxies has been firmly established, the calculation of outflow properties such as mass outflow rates and kinetic energy remains challenging. We present the [OIII]5007 ionised gas outflow properties… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.04149v1-abstract-full').style.display = 'inline'; document.getElementById('2201.04149v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.04149v1-abstract-full" style="display: none;"> Ionised gas kinematics provide crucial evidence of the impact that active galactic nuclei (AGN) have in regulating star formation in their host galaxies. Although the presence of outflows in AGN host galaxies has been firmly established, the calculation of outflow properties such as mass outflow rates and kinetic energy remains challenging. We present the [OIII]5007 ionised gas outflow properties of 22 z$<$0.1 X-ray AGN, derived from the BAT AGN Spectroscopic Survey using MUSE/VLT. With an average spatial resolution of 1" (0.1-1.2 kpc), the observations resolve the ionised gas clouds down to sub-kiloparsec scales. Resolved maps show that the [OIII] velocity dispersion is, on average, higher in regions ionised by the AGN, compared to star formation. We calculate the instantaneous outflow rates in individual MUSE spaxels by constructing resolved mass outflow rate maps, incorporating variable outflow density and velocity. We compare the instantaneous values with time-averaged outflow rates by placing mock fibres and slits on the MUSE field-of-view, a method often used in the literature. The instantaneous outflow rates (0.2-275 $M_{\odot}$ yr$^{-1}$) tend to be 2 orders of magnitude higher than the time-averaged outflow rates (0.001-40 $M_{\odot}$ yr$^{-1}$). The outflow rates correlate with the AGN bolometric luminosity ($L_{\rm bol}\sim$ 10$^{42.71}$-10$^{45.62}$ erg/s) but we find no correlations with black hole mass (10$^{6.1}$-10$^{8.9}$ M$_{\odot}$), Eddington ratio (0.002-1.1) and radio luminosity (10$^{21}$-10$^{26}$ W/Hz). We find the median coupling between the kinetic energy and $L_{\rm bol}$ to be 1%, consistent with the theoretical predictions for an AGN-driven outflow. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.04149v1-abstract-full').style.display = 'none'; document.getElementById('2201.04149v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 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">Main paper: 20 pages, 15 figures, 3 tables. Accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.12536">arXiv:2106.12536</a> <span> [<a href="https://arxiv.org/pdf/2106.12536">pdf</a>, <a href="https://arxiv.org/format/2106.12536">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202141409">10.1051/0004-6361/202141409 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Hunting for the nature of the enigmatic narrow-line Seyfert 1 galaxy PKS 2004-447 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Berton%2C+M">M. Berton</a>, <a href="/search/astro-ph?searchtype=author&query=Peluso%2C+G">G. Peluso</a>, <a href="/search/astro-ph?searchtype=author&query=Marziani%2C+P">P. Marziani</a>, <a href="/search/astro-ph?searchtype=author&query=Komossa%2C+S">S. Komossa</a>, <a href="/search/astro-ph?searchtype=author&query=Foschini%2C+L">L. Foschini</a>, <a href="/search/astro-ph?searchtype=author&query=Ciroi%2C+S">S. Ciroi</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S">S. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Congiu%2C+E">E. Congiu</a>, <a href="/search/astro-ph?searchtype=author&query=Gallo%2C+L+C">L. C. Gallo</a>, <a href="/search/astro-ph?searchtype=author&query=Bj%C3%B6rklund%2C+I">I. Bj枚rklund</a>, <a href="/search/astro-ph?searchtype=author&query=Crepaldi%2C+L">L. Crepaldi</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Mille%2C+F">F. Di Mille</a>, <a href="/search/astro-ph?searchtype=author&query=J%C3%A4rvel%C3%A4%2C+E">E. J盲rvel盲</a>, <a href="/search/astro-ph?searchtype=author&query=Kotilainen%2C+J">J. Kotilainen</a>, <a href="/search/astro-ph?searchtype=author&query=Kreikenbohm%2C+A">A. Kreikenbohm</a>, <a href="/search/astro-ph?searchtype=author&query=Morrell%2C+N">N. Morrell</a>, <a href="/search/astro-ph?searchtype=author&query=Romano%2C+P">P. Romano</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Terreran%2C+G">G. Terreran</a>, <a href="/search/astro-ph?searchtype=author&query=Tornikoski%2C+M">M. Tornikoski</a>, <a href="/search/astro-ph?searchtype=author&query=Vercellone%2C+S">S. Vercellone</a>, <a href="/search/astro-ph?searchtype=author&query=Vietri%2C+A">A. Vietri</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2106.12536v2-abstract-short" style="display: inline;"> Narrow-line Seyfert 1 (NLS1) galaxies are a class of active galactic nuclei (AGN) that, in some cases, can harbor powerful relativistic jets. One of them, PKS 2004-447, shows gamma-ray emission, and underwent its first recorded multifrequency flare in 2019. However, past studies revealed that in radio this source can be classified as a compact steep-spectrum source (CSS), suggesting that, unlike o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.12536v2-abstract-full').style.display = 'inline'; document.getElementById('2106.12536v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.12536v2-abstract-full" style="display: none;"> Narrow-line Seyfert 1 (NLS1) galaxies are a class of active galactic nuclei (AGN) that, in some cases, can harbor powerful relativistic jets. One of them, PKS 2004-447, shows gamma-ray emission, and underwent its first recorded multifrequency flare in 2019. However, past studies revealed that in radio this source can be classified as a compact steep-spectrum source (CSS), suggesting that, unlike other gamma-ray sources, the relativistic jets of PKS 2004-447 have a large inclination with respect to the line of sight. We present here a set of spectroscopic observations of this object, aimed at carefully measuring its black hole mass and Eddington ratio, determining the properties of its emission lines, and characterizing its long term variability. We find that the black hole mass is $(1.5\pm0.2)\times10^7$ M$_\odot$, and the Eddington ratio is 0.08. Both values are within the typical range of NLS1s. The spectra also suggest that the 2019 flare was caused mainly by the relativistic jet, while the accretion disk played a minor role during the event. In conclusion, we confirm that PKS 2004-447 is one of the rare examples of gamma-ray emitting CSS/NLS1s hybrid, and that these two classes of objects are likely connected in the framework of AGN evolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.12536v2-abstract-full').style.display = 'none'; document.getElementById('2106.12536v2-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 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 8 figures, 4 tables, resubmitted to A&A after minor comments from the referee</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 654, A125 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.10280">arXiv:2106.10280</a> <span> [<a href="https://arxiv.org/pdf/2106.10280">pdf</a>, <a href="https://arxiv.org/format/2106.10280">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/10.1051/0004-6361/202141590">10.1051/0004-6361/202141590 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> High star cluster formation efficiency in the strongly lensed Sunburst Lyman-continuum galaxy at z=2.37 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">P. Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">M. Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Zanella%2C+A">A. Zanella</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=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Cupani%2C+G">G. Cupani</a>, <a href="/search/astro-ph?searchtype=author&query=Mestric%2C+U">U. Mestric</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G">G. Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Tozzi%2C+P">P. Tozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">A. Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Cristiani%2C+S">S. Cristiani</a>, <a href="/search/astro-ph?searchtype=author&query=Nonino%2C+M">M. Nonino</a>, <a href="/search/astro-ph?searchtype=author&query=Merlin%2C+E">E. Merlin</a>, <a href="/search/astro-ph?searchtype=author&query=Pignataro%2C+G+V">G. V. Pignataro</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2106.10280v2-abstract-short" style="display: inline;"> We investigate the strongly lensed (渭x10-100) Lyman continuum (LyC) galaxy, dubbed Sunburst, at z=2.37, taking advantage of a new accurate model of the lens. A characterization of the intrinsic (delensed) properties of the galaxy yields a size of ~3 sq.kpc, a luminosity Muv=-20.3,and a stellar mass M~10^9 Msun;16% of the ultraviolet light is located in a 3 Myr old gravitationally-bound young massi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.10280v2-abstract-full').style.display = 'inline'; document.getElementById('2106.10280v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.10280v2-abstract-full" style="display: none;"> We investigate the strongly lensed (渭x10-100) Lyman continuum (LyC) galaxy, dubbed Sunburst, at z=2.37, taking advantage of a new accurate model of the lens. A characterization of the intrinsic (delensed) properties of the galaxy yields a size of ~3 sq.kpc, a luminosity Muv=-20.3,and a stellar mass M~10^9 Msun;16% of the ultraviolet light is located in a 3 Myr old gravitationally-bound young massive star cluster (YMC) with an effective radius of Re~8 pc and a dynamical mass of ~10^7 Msun (similar to the stellar mass), from which LyC radiation is detected (位< 912A). The inferred outflowing gas velocity (>300 km/s) exceeds the escape velocity of the star cluster. The resulting escape fraction of the ionizing radiation emerging from the Sunburst galaxy is >6-12%, whilst it is >46-93% if inferred from the YMC. 12 additional likely star clusters with 3<Re<20 pc are identified in the galaxy from which we derive a cluster formation efficiency 螕>~30%, which is consistent with the high 螕derived in local galaxies experiencing extreme gas physical conditions. The presence of the YMC influences the morphology (nucleation), photometry (photometric jumps) and spectroscopic output (nebular emission) of the entire galaxy. The de-lensed LyC and UV (1600A) magnitudes of the YMC are ~30.6 and ~26.9, whilst the galaxy has m1600~24.8. A relatively large rest-frame equivalent width of EWrest(Hb+[OIII]4959-5007)~450A emerges from the galaxy with the YMC contributing to ~30%. If O-type stars are mainly forged in star clusters, then such engines were the key ionizing agents during reionization and the increasing occurrence of high EW lines (Hb+[OIII]) observed at z>6.5 might be an indirect signature of a high 螕at reionization.Future facilities (like VLT/MAVIS or ELT), will probe bound clusters on moderately magnified (渭<5-10) galaxies across cosmic epochs up to reionization[ABRIDGED] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.10280v2-abstract-full').style.display = 'none'; document.getElementById('2106.10280v2-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> 10 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages (12 main body), 10 Figures and 1 Table. Accepted for publication in Astronomy & Astrophysics. Figure 6 shows the stellar cluster formation efficiency of the Sunburst galaxy; Figure C.1 shows the MUSE narrow field mode image of the counter-arc</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 659, A2 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.06474">arXiv:2105.06474</a> <span> [<a href="https://arxiv.org/pdf/2105.06474">pdf</a>, <a href="https://arxiv.org/format/2105.06474">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4365/ac00b6">10.3847/1538-4365/ac00b6 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Hidden treasures in the unknown 3CR extragalactic radio sky: a multi-wavelength approach </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Missaglia%2C+V">V. Missaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Massaro%2C+F">F. Massaro</a>, <a href="/search/astro-ph?searchtype=author&query=Liuzzo%2C+E">E. Liuzzo</a>, <a href="/search/astro-ph?searchtype=author&query=Paggi%2C+A">A. Paggi</a>, <a href="/search/astro-ph?searchtype=author&query=Kraft%2C+R+P">R. P. Kraft</a>, <a href="/search/astro-ph?searchtype=author&query=Forman%2C+W+R">W. R. Forman</a>, <a href="/search/astro-ph?searchtype=author&query=Jimenez-Gallardo%2C+A">A. Jimenez-Gallardo</a>, <a href="/search/astro-ph?searchtype=author&query=Madrid%2C+J+P">J. P. Madrid</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">F. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Stuardi%2C+C">C. Stuardi</a>, <a href="/search/astro-ph?searchtype=author&query=Wilkes%2C+B+J">B. J. Wilkes</a>, <a href="/search/astro-ph?searchtype=author&query=Baum%2C+S+A">S. A. Baum</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Dea%2C+C+P">C. P. O'Dea</a>, <a href="/search/astro-ph?searchtype=author&query=Kuraszkiewicz%2C+J">J. Kuraszkiewicz</a>, <a href="/search/astro-ph?searchtype=author&query=Tremblay%2C+G+R">G. R. Tremblay</a>, <a href="/search/astro-ph?searchtype=author&query=Maselli%2C+A">A. Maselli</a>, <a href="/search/astro-ph?searchtype=author&query=Capetti%2C+A">A. Capetti</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Balmaverde%2C+B">B. Balmaverde</a>, <a href="/search/astro-ph?searchtype=author&query=Harris%2C+D+E">D. E. Harris</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="2105.06474v1-abstract-short" style="display: inline;"> We present the analysis of multi-wavelength observations of seven extragalactic radio sources, listed as unidentified in the Third Cambridge Revised Catalog (3CR). X-ray observations, performed during Chandra Cycle 21, were compared to VLA, WISE and Pan-STARRS observations in the radio, infrared and optical bands, respectively. All sources in this sample lack a clear optical counterpart, and are t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.06474v1-abstract-full').style.display = 'inline'; document.getElementById('2105.06474v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.06474v1-abstract-full" style="display: none;"> We present the analysis of multi-wavelength observations of seven extragalactic radio sources, listed as unidentified in the Third Cambridge Revised Catalog (3CR). X-ray observations, performed during Chandra Cycle 21, were compared to VLA, WISE and Pan-STARRS observations in the radio, infrared and optical bands, respectively. All sources in this sample lack a clear optical counterpart, and are thus missing their redshift and optical classification. In order to confirm the X-ray and infrared radio counterparts of core and extended components, here we present for the first time radio maps obtained manually reducing VLA archival data. As in previous papers on the Chandra X-ray snapshot campaign, we report X-ray detections of radio cores and two sources, out of the seven presented here, are found to be members of galaxy clusters. For these two cluster sources (namely, 3CR 409 and 3CR 454.2), we derived surface brightness profiles in four directions. For all seven sources, we measured X-ray intensities of the radio sources and we also performed standard X-ray spectral analysis for the four sources (namely, 3CR 91, 3CR 390, 3CR 409 and 3CR 428) with the brightest nuclei (more than 400 photons in the 2'' nuclear region). We also detected extended X-ray emission around 3CR 390 and extended X-ray emission associated with the northern jet of 3CR 158. This paper represents the first attempt to give a multi-wavelength view of the unidentified radio sources listed in the 3CR catalog. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.06474v1-abstract-full').style.display = 'none'; document.getElementById('2105.06474v1-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 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 19 figures, 5 tables, accepted for publication on ApJS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2104.07677">arXiv:2104.07677</a> <span> [<a href="https://arxiv.org/pdf/2104.07677">pdf</a>, <a href="https://arxiv.org/format/2104.07677">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/10.3847/2041-8213/abf6db">10.3847/2041-8213/abf6db <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Raining in MKW 3s: a Chandra-MUSE analysis of X-ray cold filaments around 3CR 318.1 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jimenez-Gallardo%2C+A">A. Jimenez-Gallardo</a>, <a href="/search/astro-ph?searchtype=author&query=Massaro%2C+F">F. Massaro</a>, <a href="/search/astro-ph?searchtype=author&query=Balmaverde%2C+B">B. Balmaverde</a>, <a href="/search/astro-ph?searchtype=author&query=Paggi%2C+A">A. Paggi</a>, <a href="/search/astro-ph?searchtype=author&query=Capetti%2C+A">A. Capetti</a>, <a href="/search/astro-ph?searchtype=author&query=Forman%2C+W+R">W. R. Forman</a>, <a href="/search/astro-ph?searchtype=author&query=Kraft%2C+R+P">R. P. Kraft</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=Mahatma%2C+V+H">V. H. Mahatma</a>, <a href="/search/astro-ph?searchtype=author&query=Mazzucchelli%2C+C">C. Mazzucchelli</a>, <a href="/search/astro-ph?searchtype=author&query=Missaglia%2C+V">V. Missaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">F. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Venturi%2C+G">G. Venturi</a>, <a href="/search/astro-ph?searchtype=author&query=Bam%2C+S+A">S. A. Bam</a>, <a href="/search/astro-ph?searchtype=author&query=Liuzzo%2C+E">E. Liuzzo</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Dea%2C+C+P">C. P. O'Dea</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+M+A">M. A. Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=R%C3%B6ttgering%2C+H+J+A">H. J. A. R枚ttgering</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Sparks%2C+W+B">W. B. Sparks</a>, <a href="/search/astro-ph?searchtype=author&query=Tremblay%2C+G+R">G. R. Tremblay</a>, <a href="/search/astro-ph?searchtype=author&query=van+Weeren%2C+R+J">R. J. van Weeren</a>, <a href="/search/astro-ph?searchtype=author&query=Wilkes%2C+B+J">B. J. Wilkes</a>, <a href="/search/astro-ph?searchtype=author&query=Harwood%2C+J+J">J. J. Harwood</a>, <a href="/search/astro-ph?searchtype=author&query=Mazzotta%2C+P">P. Mazzotta</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="2104.07677v1-abstract-short" style="display: inline;"> We present the analysis of X-ray and optical observations of gas filaments observed in the radio source 3CR 318.1, associated with NGC 5920, the Brightest Cluster Galaxy (BCG) of MKW 3s, a nearby cool core galaxy cluster. This work is one of the first X-ray and optical analyses of filaments in cool core clusters carried out using MUSE observations. We aim at identifying the main excitation process… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.07677v1-abstract-full').style.display = 'inline'; document.getElementById('2104.07677v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2104.07677v1-abstract-full" style="display: none;"> We present the analysis of X-ray and optical observations of gas filaments observed in the radio source 3CR 318.1, associated with NGC 5920, the Brightest Cluster Galaxy (BCG) of MKW 3s, a nearby cool core galaxy cluster. This work is one of the first X-ray and optical analyses of filaments in cool core clusters carried out using MUSE observations. We aim at identifying the main excitation processes responsible for the emission arising from these filaments. We complemented the optical VLT/MUSE observations, tracing the colder gas phase, with X-ray $\textit{Chandra}$ observations of the hotter highly ionized gas phase. Using the MUSE observations, we studied the emission line intensity ratios along the filaments to constrain the physical processes driving the excitation, and, using the $\textit{Chandra}$ observations, we carried out a spectral analysis of the gas along these filaments. We found a spatial association between the X-ray and optical morphology of these filaments, which are colder and have lower metal abundance than the surrounding intra-cluster medium (ICM), as already seen in other BCGs. Comparing with previous results from the literature for other BCGs, we propose that the excitation process that is most likely responsible for these filaments emission is a combination of star formation and shocks, with a likely contribution from self-ionizing, cooling ICM. Additionally, we conclude that the filaments most likely originated from AGN-driven outflows in the direction of the radio jet. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.07677v1-abstract-full').style.display = 'none'; document.getElementById('2104.07677v1-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> 15 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 5 figures, ApJL accepted, pre-proof 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/2009.08458">arXiv:2009.08458</a> <span> [<a href="https://arxiv.org/pdf/2009.08458">pdf</a>, <a href="https://arxiv.org/format/2009.08458">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/10.1051/0004-6361/202039466">10.1051/0004-6361/202039466 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MUSE Deep Lensed Field on the Hubble Frontier Field MACS~J0416 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</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=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">A. Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">M. Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">P. Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">F. Calura</a>, <a href="/search/astro-ph?searchtype=author&query=Caputi%2C+K">K. Caputi</a>, <a href="/search/astro-ph?searchtype=author&query=Cristiani%2C+S">S. Cristiani</a>, <a href="/search/astro-ph?searchtype=author&query=Cupani%2C+G">G. Cupani</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">A. Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">R. Gilli</a>, <a href="/search/astro-ph?searchtype=author&query=Grazian%2C+A">A. Grazian</a>, <a href="/search/astro-ph?searchtype=author&query=Gronke%2C+M">M. Gronke</a>, <a href="/search/astro-ph?searchtype=author&query=Mignoli%2C+M">M. Mignoli</a>, <a href="/search/astro-ph?searchtype=author&query=Nonino%2C+M">M. Nonino</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">L. Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Tozzi%2C+P">P. Tozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Treu%2C+T">T. Treu</a>, <a href="/search/astro-ph?searchtype=author&query=Balestra%2C+I">I. Balestra</a>, <a href="/search/astro-ph?searchtype=author&query=Dijkstra%2C+M">M. Dijkstra</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="2009.08458v2-abstract-short" style="display: inline;"> Context: A census of faint and tiny star forming complexes at high redshift is key to improving our understanding of reionizing sources, galaxy growth and the formation of globular clusters. Aims: We present the MUSE Deep Lensed Field (MDLF) program. Methods: We describe Deep MUSE observations of 17.1 hours integration on a single pointing over the Hubble Frontier Field galaxy cluster MACS~J0416.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.08458v2-abstract-full').style.display = 'inline'; document.getElementById('2009.08458v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.08458v2-abstract-full" style="display: none;"> Context: A census of faint and tiny star forming complexes at high redshift is key to improving our understanding of reionizing sources, galaxy growth and the formation of globular clusters. Aims: We present the MUSE Deep Lensed Field (MDLF) program. Methods: We describe Deep MUSE observations of 17.1 hours integration on a single pointing over the Hubble Frontier Field galaxy cluster MACS~J0416. Results: We confirm spectroscopic redshifts for all 136 multiple images of 48 source galaxies at 0.9<z<6.2. Within those galaxies, we securely identify 182 multiple images of 66 galaxy components that we use to constrain our lens model. We identify 116 clumps belonging to background high-z galaxies; the majority of them are multiple images and span magnitude, size and redshift intervals of [-18,-10], [~400-3] parsec and 1<z<6.6, respectively, with the most magnified ones probing possible single gravitationally bound star clusters. The depth of the MDLF combined with lensing magnification lead us to reach a detection limit for unresolved emission lines of a few 10$^{-20}$ erg/s/cm2, after correction for lensing magnification. Ultraviolet high-ionization metal lines (and HeII1640) are detected with S/N>10 for individual objects down to de-lensed magnitude 28-30 suggesting that they are common in such faint sources. Conclusions:Deep MUSE observations, in combination with existing HST imaging, allowed us to:(1) confirm redshifts for extremely faint high-z sources;(2) peer into their internal clumps (down to 100-200 pc scale);(3) in some cases break down such clumps into bound star clusters (<20 pc scale);(4) double the number of constraints for the lens model,reaching an unprecedented set of 182 bona-fide multiple images and confirming up to 213 galaxy cluster members. These results demonstrate the power that JWST and future ELTs will have when combined to study gravitational telescopes.[abridged] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.08458v2-abstract-full').style.display = 'none'; document.getElementById('2009.08458v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">43 pages total (17 pages main body); 5 appendices. Accepted for publication in A&A on October 26</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 646, A57 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2008.10658">arXiv:2008.10658</a> <span> [<a href="https://arxiv.org/pdf/2008.10658">pdf</a>, <a href="https://arxiv.org/format/2008.10658">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="Solar and Stellar Astrophysics">astro-ph.SR</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/10.1051/0004-6361/202038439">10.1051/0004-6361/202038439 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Spectroscopic observations of the machine-learning selected anomaly catalogue from the AllWISE Sky Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Solarz%2C+A">A. Solarz</a>, <a href="/search/astro-ph?searchtype=author&query=Thomas%2C+R">R. Thomas</a>, <a href="/search/astro-ph?searchtype=author&query=Montenegro-Montes%2C+F+M">F. M. Montenegro-Montes</a>, <a href="/search/astro-ph?searchtype=author&query=Gromadzki%2C+M">M. Gromadzki</a>, <a href="/search/astro-ph?searchtype=author&query=Donoso%2C+E">E. Donoso</a>, <a href="/search/astro-ph?searchtype=author&query=Koprowski%2C+M">M. Koprowski</a>, <a href="/search/astro-ph?searchtype=author&query=Wyrzykowski%2C+L">L. Wyrzykowski</a>, <a href="/search/astro-ph?searchtype=author&query=Diaz%2C+C+G">C. G. Diaz</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Bilicki%2C+M">M. Bilicki</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="2008.10658v1-abstract-short" style="display: inline;"> We present the results of a programme to search and identify the nature of unusual sources within the All-sky Wide-field Infrared Survey Explorer (WISE) that is based on a machine-learning algorithm for anomaly detection, namely one-class support vector machines (OCSVM). Designed to detect sources deviating from a training set composed of known classes, this algorithm was used to create a model fo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.10658v1-abstract-full').style.display = 'inline'; document.getElementById('2008.10658v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.10658v1-abstract-full" style="display: none;"> We present the results of a programme to search and identify the nature of unusual sources within the All-sky Wide-field Infrared Survey Explorer (WISE) that is based on a machine-learning algorithm for anomaly detection, namely one-class support vector machines (OCSVM). Designed to detect sources deviating from a training set composed of known classes, this algorithm was used to create a model for the expected data based on WISE objects with spectroscopic identifications in the Sloan Digital Sky Survey (SDSS). Subsequently, it marked as anomalous those sources whose WISE photometry was shown to be inconsistent with this model. We report the results from optical and near-infrared spectroscopy follow-up observations of a subset of 36 bright ($g_{AB}$<19.5) objects marked as 'anomalous' by the OCSVM code to verify its performance. Among the observed objects, we identified three main types of sources: i) low redshift (z~0.03-0.15) galaxies containing large amounts of hot dust (53%), including three Wolf-Rayet galaxies; ii) broad-line quasi-stellar objects (QSOs) (33%) including low-ionisation broad absorption line (LoBAL) quasars and a rare QSO with strong and narrow ultraviolet iron emission; iii) Galactic objects in dusty phases of their evolution (3%). The nature of four of these objects (11%) remains undetermined due to low signal-to-noise or featureless spectra. The current data show that the algorithm works well at detecting rare but not necessarily unknown objects among the brightest candidates. They mostly represent peculiar sub-types of otherwise well-known sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.10658v1-abstract-full').style.display = 'none'; document.getElementById('2008.10658v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 August, 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">17 pages, 17 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 642, A103 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.11002">arXiv:2007.11002</a> <span> [<a href="https://arxiv.org/pdf/2007.11002">pdf</a>, <a href="https://arxiv.org/format/2007.11002">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/10.1051/0004-6361/201936649">10.1051/0004-6361/201936649 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Co-evolution of black hole accretion and star formation in galaxies up to z=3.5 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Carraro%2C+R">R. Carraro</a>, <a href="/search/astro-ph?searchtype=author&query=Rodighiero%2C+G">G. Rodighiero</a>, <a href="/search/astro-ph?searchtype=author&query=Cassata%2C+P">P. Cassata</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Shankar%2C+F">F. Shankar</a>, <a href="/search/astro-ph?searchtype=author&query=Baronchelli%2C+I">I. Baronchelli</a>, <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">E. Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Delvecchio%2C+I">I. Delvecchio</a>, <a href="/search/astro-ph?searchtype=author&query=Franceschini%2C+A">A. Franceschini</a>, <a href="/search/astro-ph?searchtype=author&query=Griffiths%2C+R">R. Griffiths</a>, <a href="/search/astro-ph?searchtype=author&query=Gruppioni%2C+C">C. Gruppioni</a>, <a href="/search/astro-ph?searchtype=author&query=L%C3%B3pez-Navas%2C+E">E. L贸pez-Navas</a>, <a href="/search/astro-ph?searchtype=author&query=Mancini%2C+C">C. Mancini</a>, <a href="/search/astro-ph?searchtype=author&query=Marchesi%2C+S">S. Marchesi</a>, <a href="/search/astro-ph?searchtype=author&query=Negrello%2C+M">M. Negrello</a>, <a href="/search/astro-ph?searchtype=author&query=Puglisi%2C+A">A. Puglisi</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Suh%2C+H">H. Suh</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="2007.11002v2-abstract-short" style="display: inline;"> We study the co-evolution between the black hole accretion rate (BHAR) and the star formation rate (SFR) in different galaxy life phases: main sequence star-forming galaxies, quiescent and starburst galaxies at different cosmic epochs. We take advantage of the X-ray data from the Chandra COSMOS-Legacy survey and of the extensive multiwavelength ancillary observations in the COSMOS field presente… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.11002v2-abstract-full').style.display = 'inline'; document.getElementById('2007.11002v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.11002v2-abstract-full" style="display: none;"> We study the co-evolution between the black hole accretion rate (BHAR) and the star formation rate (SFR) in different galaxy life phases: main sequence star-forming galaxies, quiescent and starburst galaxies at different cosmic epochs. We take advantage of the X-ray data from the Chandra COSMOS-Legacy survey and of the extensive multiwavelength ancillary observations in the COSMOS field presented in the COSMOS2015 catalog. We perform an X-ray stacking analysis and combine it with detected sources, in a broad redshift interval ($0.1<z<3.5$). The X-ray luminosity is used to predict the BHAR, while a similar stacking analysis on far-infrared Herschel maps is used to measure the corresponding SFR. We focus on the evolution of the average SFR-stellar mass (M*) relation and compare it with the BHAR-M* relation. We find that the ratio between BHAR and SFR does not evolve with redshift, although it depends on stellar mass. For the star-forming populations, this dependence on M* has a logarithmic slope of $\sim0.6$, for the starburst sample of $\sim0.4$, both at odds with quiescent sources where it remains constant ($\log(\rm {BHAR}/{\rm SFR})\sim -3.4$). By studying the specific BHAR and specific SFR we find signs of downsizing for both M* and black hole mass (M$_{\rm BH}$): quiescents grew their super-massive black hole at very early times, while star-forming and starburst galaxies had an accretion that endured until more recent times. Our results support the idea that the same physical processes feed and sustain both star formation and black hole accretion. Our integrated estimates of the M*-M$_{\rm BH}$ relation at all redshifts are consistent with independent determinations of the local M*-M$_{\rm BH}$ relation, thus adding key evidence to a weak evolution in the BHAR/SFR, and its low normalization compared to local dynamical M*-M$_{\rm BH}$ relations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.11002v2-abstract-full').style.display = 'none'; document.getElementById('2007.11002v2-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> 3 August, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">18 pages, 6 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 642, A65 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2004.08400">arXiv:2004.08400</a> <span> [<a href="https://arxiv.org/pdf/2004.08400">pdf</a>, <a href="https://arxiv.org/format/2004.08400">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/mnrasl/slaa163">10.1093/mnrasl/slaa163 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Probing the circum-stellar medium 2.8 Gyr after the Big Bang: detection of Bowen fluorescence in the Sunburst arc </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">M. Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Pastorello%2C+A">A. Pastorello</a>, <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">F. Calura</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Cupani%2C+G">G. Cupani</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=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Odorico%2C+V">V. D'Odorico</a>, <a href="/search/astro-ph?searchtype=author&query=Cristiani%2C+S">S. Cristiani</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">A. Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Nonino%2C+M">M. Nonino</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G+B">G. B. Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Hartman%2C+H">H. Hartman</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="2004.08400v2-abstract-short" style="display: inline;"> We discovered Bowen emission arising from a strongly lensed (i.e., with magnification factor $渭$>20) source hosted in the Sunburst arc at z=2.37. We claim this source is plausibly a transient stellar object and study the unique ultraviolet lines emerging from it. In particular, narrow ($蟽$_v ~ 40 km/s) ionisation lines of Fe fluoresce after being exposed to Lya radiation that pumps selectively the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.08400v2-abstract-full').style.display = 'inline'; document.getElementById('2004.08400v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2004.08400v2-abstract-full" style="display: none;"> We discovered Bowen emission arising from a strongly lensed (i.e., with magnification factor $渭$>20) source hosted in the Sunburst arc at z=2.37. We claim this source is plausibly a transient stellar object and study the unique ultraviolet lines emerging from it. In particular, narrow ($蟽$_v ~ 40 km/s) ionisation lines of Fe fluoresce after being exposed to Lya radiation that pumps selectively their atomic levels. Data from VLT/MUSE, X-Shooter and ESPRESSO observations (the latter placed at the focus of the four UTs) at increasing spectral resolution of R=2500, 11400 and R=70000, respectively, confirm such fluorescent lines are present since at least 3.3 years (~ 1 year rest-frame). Additional Fe forbidden lines have been detected, while C and Si doublets probe an electron density n_e >~ $10^6$ cm$^{-3}$. Similarities with the spectral features observed in the circum-stellar Weigelt blobs of Eta-Carinae probing the circum-stellar dense gas condensations in radiation-rich conditions are observed. We discuss the physical origin of the transient event, which remains unclear. We expect such transient events (including also supernova or impostors) will be easily recognised with ELTs thanks to high angular resolution provided by adaptive optics and large collecting area, especially in modest ($渭< 3$) magnification regime. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.08400v2-abstract-full').style.display = 'none'; document.getElementById('2004.08400v2-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> 10 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 April, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">5 pages, 4 figures. MNRAS accepted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2001.09984">arXiv:2001.09984</a> <span> [<a href="https://arxiv.org/pdf/2001.09984">pdf</a>, <a href="https://arxiv.org/ps/2001.09984">ps</a>, <a href="https://arxiv.org/format/2001.09984">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/10.1051/0004-6361/201936817">10.1051/0004-6361/201936817 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Universal bolometric corrections for AGN over 7 luminosity decades </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Duras%2C+F">F. Duras</a>, <a href="/search/astro-ph?searchtype=author&query=Bongiorno%2C+A">A. Bongiorno</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">F. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Piconcelli%2C+E">E. Piconcelli</a>, <a href="/search/astro-ph?searchtype=author&query=Shankar%2C+F">F. Shankar</a>, <a href="/search/astro-ph?searchtype=author&query=Lusso%2C+E">E. Lusso</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+S">S. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Fiore%2C+F">F. Fiore</a>, <a href="/search/astro-ph?searchtype=author&query=Maiolino%2C+R">R. Maiolino</a>, <a href="/search/astro-ph?searchtype=author&query=Marconi%2C+A">A. Marconi</a>, <a href="/search/astro-ph?searchtype=author&query=Onori%2C+F">F. Onori</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Schneider%2C+R">R. Schneider</a>, <a href="/search/astro-ph?searchtype=author&query=Vignali%2C+C">C. Vignali</a>, <a href="/search/astro-ph?searchtype=author&query=La+Franca%2C+F">F. La Franca</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="2001.09984v1-abstract-short" style="display: inline;"> The AGN bolometric correction is a key element to understand BH demographics and compute accurate BH accretion histories from AGN luminosities. However, current estimates still differ from each other by up to a factor of two to three, and rely on extrapolations at the lowest and highest luminosities. Here we revisit this fundamental issue presenting general hard X-ray ($K_{X}$) and optical (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.09984v1-abstract-full').style.display = 'inline'; document.getElementById('2001.09984v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2001.09984v1-abstract-full" style="display: none;"> The AGN bolometric correction is a key element to understand BH demographics and compute accurate BH accretion histories from AGN luminosities. However, current estimates still differ from each other by up to a factor of two to three, and rely on extrapolations at the lowest and highest luminosities. Here we revisit this fundamental issue presenting general hard X-ray ($K_{X}$) and optical ($K_{O}$) bolometric corrections, computed combining several AGN samples spanning the widest (about 7 dex) luminosity range ever used for this kind of studies. We analysed a total of $\sim 1000$ type 1 and type 2 AGN for which a dedicated SED-fitting has been carried out. We provide a bolometric correction separately for type 1 and type 2 AGN; the two bolometric corrections results to be in agreement in the overlapping luminosity range and therefore, for the first time, a universal bolometric correction for the whole AGN sample (both type 1 and type 2) has been computed. We found that $K_{X}$ is fairly constant at $log(L_{BOL}/L_{\odot}) < 11$, while it increases up to about one order of magnitude at $log(L_{BOL}/L_{\odot}) \sim 14.5$. A similar increasing trend has been observed when its dependence on either the Eddington ratio or the BH mass is considered, while no dependence on redshift up to $z\sim3.5$ has been found. On the contrary, the optical bolometric correction appears to be fairly constant (i.e. $K_{O} \sim 5$) whatever is the independent variable. We also verified that our bolometric corrections correctly predict the AGN bolometric luminosity functions. According to this analysis, our bolometric corrections can be applied to the whole AGN population in a wide range of luminosity and redshift. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.09984v1-abstract-full').style.display = 'none'; document.getElementById('2001.09984v1-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 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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 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, A73 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2001.03619">arXiv:2001.03619</a> <span> [<a href="https://arxiv.org/pdf/2001.03619">pdf</a>, <a href="https://arxiv.org/format/2001.03619">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/mnrasl/slaa041">10.1093/mnrasl/slaa041 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Candidate Population III stellar complex at z=6.629 in the MUSE Deep Lensed Field </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">M. Meneghetti</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=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">F. Calura</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Dijkstra%2C+M">M. Dijkstra</a>, <a href="/search/astro-ph?searchtype=author&query=Gronke%2C+M">M. Gronke</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">A. Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Tozzi%2C+P">P. Tozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Nonino%2C+M">M. Nonino</a>, <a href="/search/astro-ph?searchtype=author&query=Cristiani%2C+S">S. Cristiani</a>, <a href="/search/astro-ph?searchtype=author&query=Mignoli%2C+M">M. Mignoli</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">L. Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">R. Gilli</a>, <a href="/search/astro-ph?searchtype=author&query=Treu%2C+T">T. Treu</a>, <a href="/search/astro-ph?searchtype=author&query=Caputi%2C+K">K. Caputi</a>, <a href="/search/astro-ph?searchtype=author&query=Cupani%2C+G">G. Cupani</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">A. Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Grazian%2C+A">A. Grazian</a>, <a href="/search/astro-ph?searchtype=author&query=Balestra%2C+I">I. Balestra</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="2001.03619v2-abstract-short" style="display: inline;"> We discovered a strongly lensed (渭>40) Lya emission at z=6.629 (S/N~18) in the MUSE Deep Lensed Field (MDLF) targeting the Hubble Frontier Field galaxy cluster MACS~J0416. Dedicated lensing simulations imply that the Lya emitting region necessarily crosses the caustic. The arc-like shape of the Lya extends 3 arcsec on the observed plane and is the result of two merged multiple images, each one wit… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.03619v2-abstract-full').style.display = 'inline'; document.getElementById('2001.03619v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2001.03619v2-abstract-full" style="display: none;"> We discovered a strongly lensed (渭>40) Lya emission at z=6.629 (S/N~18) in the MUSE Deep Lensed Field (MDLF) targeting the Hubble Frontier Field galaxy cluster MACS~J0416. Dedicated lensing simulations imply that the Lya emitting region necessarily crosses the caustic. The arc-like shape of the Lya extends 3 arcsec on the observed plane and is the result of two merged multiple images, each one with a de-lensed Lya luminosity L<~2.8 x 10^(40) erg/s arising from a confined region (< 150 pc effective radius). A spatially unresolved HST counterpart is barely detected at S/N~2 after stacking the near-infrared bands, corresponding to an observed(intrinsic) magnitude m_(1500)>~30.8(>~35.0). The inferred rest-frame Lya equivalent width is EWo > 1120 A if the IGM transmission is T(IGM)<0.5. The low luminosities and the extremely large Lya EWo match the case of a Population~III star complex made of several dozens stars (~ 10^4 Msun) which irradiate a HII region crossing the caustic. While the Lya and stellar continuum are among the faintest ever observed at this redshift, the continuum and the Lya emissions could be affected by differential magnification, possibly biasing the EWo estimate. The aforementioned tentative HST detection tend to favor a large EWo, making such a faint Pop~III candidate a key target for the James Webb Space Telescope and Extremely Large Telescopes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.03619v2-abstract-full').style.display = 'none'; document.getElementById('2001.03619v2-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 March, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">5 pages, 3 figures and 1 table. Accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1911.12395">arXiv:1911.12395</a> <span> [<a href="https://arxiv.org/pdf/1911.12395">pdf</a>, <a href="https://arxiv.org/format/1911.12395">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/stz3386">10.1093/mnras/stz3386 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> BAT AGN Spectroscopic Survey -- XIX: Type 1 versus Type 2 AGN dichotomy from the point of view of ionized outflows </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rojas%2C+A+F">A. F. Rojas</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Gavignaud%2C+I">I. Gavignaud</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">C. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Lamperti%2C+I">I. Lamperti</a>, <a href="/search/astro-ph?searchtype=author&query=Koss%2C+M">M. Koss</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">B. Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Schawinski%2C+K">K. Schawinski</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+K">K. Oh</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">F. E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Bischetti%2C+M">M. Bischetti</a>, <a href="/search/astro-ph?searchtype=author&query=Boissay-Malaquin%2C+R">R. Boissay-Malaquin</a>, <a href="/search/astro-ph?searchtype=author&query=Bongiorno%2C+A">A. Bongiorno</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F">F. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Kakkad%2C+D">D. Kakkad</a>, <a href="/search/astro-ph?searchtype=author&query=Masetti%2C+N">N. Masetti</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">F. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Shimizu%2C+T">T. Shimizu</a>, <a href="/search/astro-ph?searchtype=author&query=Stalevski%2C+M">M. Stalevski</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">D. Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Vietri%2C+G">G. Vietri</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="1911.12395v1-abstract-short" style="display: inline;"> We present a detailed study of ionized outflows in a large sample of ~650 hard X-ray detected AGN. Using optical spectroscopy from the BAT AGN Spectroscopic Survey (BASS) we are able to reveal the faint wings of the [OIII] emission lines associated with outflows covering, for the first time, an unexplored range of low AGN bolometric luminosity at low redshift (z~0.05). We test if and how the incid… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.12395v1-abstract-full').style.display = 'inline'; document.getElementById('1911.12395v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1911.12395v1-abstract-full" style="display: none;"> We present a detailed study of ionized outflows in a large sample of ~650 hard X-ray detected AGN. Using optical spectroscopy from the BAT AGN Spectroscopic Survey (BASS) we are able to reveal the faint wings of the [OIII] emission lines associated with outflows covering, for the first time, an unexplored range of low AGN bolometric luminosity at low redshift (z~0.05). We test if and how the incidence and velocity of ionized outflow is related to AGN physical parameters: black hole mass, gas column density, Eddington Ratio, [OIII], X-ray, and bolometric luminosities. We find a higher occurrence of ionized outflows in type 1.9 (55%) and type 1 AGN (46%) with respect to type 2 AGN (24%). While outflows in type 2 AGN are evenly balanced between blue and red velocity offsets with respect to the [OIII] narrow component, they are almost exclusively blueshifted in type 1 and type 1.9 AGN. We observe a significant dependence between the outflow occurrence and accretion rate, which becomes relevant at high Eddington ratios (> -1.7). We interpret such behaviour in the framework of covering factor-Eddington ratio dependence. We don't find strong trends of the outflow maximum velocity with AGN physical parameters, as an increase with bolometric luminosity can be only identified when including samples of AGN at high luminosity and high redshift taken from literature. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.12395v1-abstract-full').style.display = 'none'; document.getElementById('1911.12395v1-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 November, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">Accepted for publication in MNRAS, 15 pages, 19 figures, 1 table</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1908.07981">arXiv:1908.07981</a> <span> [<a href="https://arxiv.org/pdf/1908.07981">pdf</a>, <a href="https://arxiv.org/format/1908.07981">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/10.3847/2041-8213/ab3c64">10.3847/2041-8213/ab3c64 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Counter-Rotation and High Velocity Outflow in the Parsec-Scale Molecular Torus of NGC 1068 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Impellizzeri%2C+C+M+V">C. M. Violette Impellizzeri</a>, <a href="/search/astro-ph?searchtype=author&query=Gallimore%2C+J+F">Jack F. Gallimore</a>, <a href="/search/astro-ph?searchtype=author&query=Baum%2C+S+A">Stefi A. Baum</a>, <a href="/search/astro-ph?searchtype=author&query=Elitzur%2C+M">Moshe Elitzur</a>, <a href="/search/astro-ph?searchtype=author&query=Davies%2C+R">Richard Davies</a>, <a href="/search/astro-ph?searchtype=author&query=Lutz%2C+D">Dieter Lutz</a>, <a href="/search/astro-ph?searchtype=author&query=Maiolino%2C+R">Roberto Maiolino</a>, <a href="/search/astro-ph?searchtype=author&query=Marconi%2C+A">Alessandro Marconi</a>, <a href="/search/astro-ph?searchtype=author&query=Nikutta%2C+R">Robert Nikutta</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Dea%2C+C+P">Christopher P. O'Dea</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">Eleonora Sani</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="1908.07981v2-abstract-short" style="display: inline;"> We present 1.4 pc resolution observations of 256 GHz nuclear radio continuum and HCN ($J=3 \to 2$) in the molecular torus of NGC 1068. The integrated radio continuum emission has a flat spectrum consistent with free-free emission and resolves into an X-shaped structure resembling an edge-brightened bicone. HCN is detected in absorption against the continuum, and the absorption spectrum shows a pro… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.07981v2-abstract-full').style.display = 'inline'; document.getElementById('1908.07981v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1908.07981v2-abstract-full" style="display: none;"> We present 1.4 pc resolution observations of 256 GHz nuclear radio continuum and HCN ($J=3 \to 2$) in the molecular torus of NGC 1068. The integrated radio continuum emission has a flat spectrum consistent with free-free emission and resolves into an X-shaped structure resembling an edge-brightened bicone. HCN is detected in absorption against the continuum, and the absorption spectrum shows a pronounced blue wing that suggests a high-velocity molecular outflow with speeds reaching 450 km/s. Analysis of the off-nucleus emission line kinematics and morphology reveals two nested, rotating disk components. The inner disk, inside $r\sim 1.2$ pc, has kinematics consistent with the nearly edge-on, geometrically thin water megamaser disk in Keplerian rotation around a central mass of $1.66\times 10^7\,\mbox{M}_\odot$. The outer disk, which extends to $\sim 7$~pc radius, counter-rotates relative to the inner disk. The rotation curve of the outer disk is consistent with rotation around the same central mass as the megamaser disk but in the opposite sense. The morphology of the molecular gas is asymmetric around the nuclear continuum source. We speculate that the outer disk formed from more recently introduced molecular gas falling out of the host galaxy or from a captured dwarf satellite galaxy. In NGC 1068, we find direct evidence that the molecular torus consists of counter-rotating and misaligned disks on parsec scales. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.07981v2-abstract-full').style.display = 'none'; document.getElementById('1908.07981v2-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 August, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 August, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">8 pages, 4 figures; accepted for publication in The Astrophysical Journal Letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1908.07546">arXiv:1908.07546</a> <span> [<a href="https://arxiv.org/pdf/1908.07546">pdf</a>, <a href="https://arxiv.org/format/1908.07546">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stz2309">10.1093/mnras/stz2309 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> BAT AGN Spectroscopic Survey -- XIII. The nature of the most luminous obscured AGN in the low-redshift universe </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=B%C3%A4r%2C+R+E">Rudolf E. B盲r</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">Benny Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+K">Kyuseok Oh</a>, <a href="/search/astro-ph?searchtype=author&query=Koss%2C+M+J">Michael J. Koss</a>, <a href="/search/astro-ph?searchtype=author&query=Wong%2C+O+I">O. Ivy Wong</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">Claudio Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Schawinski%2C+K">Kevin Schawinski</a>, <a href="/search/astro-ph?searchtype=author&query=Weigel%2C+A+K">Anna K. Weigel</a>, <a href="/search/astro-ph?searchtype=author&query=Sartori%2C+L+F">Lia F. Sartori</a>, <a href="/search/astro-ph?searchtype=author&query=Ichikawa%2C+K">Kohei Ichikawa</a>, <a href="/search/astro-ph?searchtype=author&query=Secrest%2C+N+J">Nathan J. Secrest</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Pacucci%2C+F">Fabio Pacucci</a>, <a href="/search/astro-ph?searchtype=author&query=Mushotzky%2C+R">Richard Mushotzky</a>, <a href="/search/astro-ph?searchtype=author&query=Powell%2C+M+C">Meredith C. Powell</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">Federica Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">Eleonora Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+K+L">Krista L. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+F+A">Fiona A. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Lamperti%2C+I">Isabella Lamperti</a>, <a href="/search/astro-ph?searchtype=author&query=Urry%2C+C+M">C. Megan Urry</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="1908.07546v1-abstract-short" style="display: inline;"> We present a multi wavelength analysis of 28 of the most luminous low-redshift narrow-line, ultra-hard X-ray selected active galactic nuclei (AGN) drawn from the 70 month Swift/BAT all-sky survey, with bolometric luminosities of log(L_bol/erg/s) > 45.25. The broad goal of our study is to determine whether these objects have any distinctive properties, potentially setting them aside from lower-lumi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.07546v1-abstract-full').style.display = 'inline'; document.getElementById('1908.07546v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1908.07546v1-abstract-full" style="display: none;"> We present a multi wavelength analysis of 28 of the most luminous low-redshift narrow-line, ultra-hard X-ray selected active galactic nuclei (AGN) drawn from the 70 month Swift/BAT all-sky survey, with bolometric luminosities of log(L_bol/erg/s) > 45.25. The broad goal of our study is to determine whether these objects have any distinctive properties, potentially setting them aside from lower-luminosity obscured AGN in the local Universe. Our analysis relies on the first data release of the BAT AGN Spectroscopic Survey (BASS/DR1) and on dedicated observations with the VLT, Palomar, and Keck observatories. We find that the vast majority of our sources agree with commonly used AGN selection criteria which are based on emission line ratios and on mid-infrared colours. Our AGN are predominantly hosted in massive galaxies (9.8 < log(M_*/M_sun) < 11.7); based on visual inspection of archival optical images, they appear to be mostly ellipticals. Otherwise, they do not have distinctive properties. Their radio luminosities, determined from publicly available survey data, show a large spread of almost 4 orders of magnitude - much broader than what is found for lower X-ray luminosity obscured AGN in BASS. Moreover, our sample shows no preferred combination of black hole masses (M_BH) and/or Eddington ratio (lambda_Edd), covering 7.5 < log(M_BH/M_sun) < 10.3 and 0.01 < lambda_Edd < 1. Based on the distribution of our sources in the lambda_Edd-N_H plane, we conclude that our sample is consistent with a scenario where the amount of obscuring material along the line of sight is determined by radiation pressure exerted by the AGN on the dusty circumnuclear gas. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.07546v1-abstract-full').style.display = 'none'; document.getElementById('1908.07546v1-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 August, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">Accepted for publication in MNRAS (ID: stz2309)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1904.07941">arXiv:1904.07941</a> <span> [<a href="https://arxiv.org/pdf/1904.07941">pdf</a>, <a href="https://arxiv.org/format/1904.07941">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/stz2286">10.1093/mnras/stz2286 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Ionising the Intergalactic Medium by Star Clusters: The first empirical evidence </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</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=Calura%2C+F">F. Calura</a>, <a href="/search/astro-ph?searchtype=author&query=Cupani%2C+G">G. Cupani</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">M. Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">A. Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">C. Grillo</a>, <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=Comastri%2C+A">A. Comastri</a>, <a href="/search/astro-ph?searchtype=author&query=Nonino%2C+M">M. Nonino</a>, <a href="/search/astro-ph?searchtype=author&query=Cristiani%2C+S">S. Cristiani</a>, <a href="/search/astro-ph?searchtype=author&query=Giavalisco%2C+M">M. Giavalisco</a>, <a href="/search/astro-ph?searchtype=author&query=Caputi%2C+K">K. Caputi</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="1904.07941v3-abstract-short" style="display: inline;"> We present a VLT/X-Shooter spectroscopy of the Lyman continuum (LyC) emitting galaxy 'Ion2' at z=3.2121 and compare it to that of the recently discovered strongly lensed LyC-emitter at z=2.37, known as the 'Sunburst' arc. Three main results emerge from the X-Shooter spectrum: (a) the Lya has three distinct peaks with the central one at the systemic redshift, indicating a ionised tunnel through whi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.07941v3-abstract-full').style.display = 'inline'; document.getElementById('1904.07941v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1904.07941v3-abstract-full" style="display: none;"> We present a VLT/X-Shooter spectroscopy of the Lyman continuum (LyC) emitting galaxy 'Ion2' at z=3.2121 and compare it to that of the recently discovered strongly lensed LyC-emitter at z=2.37, known as the 'Sunburst' arc. Three main results emerge from the X-Shooter spectrum: (a) the Lya has three distinct peaks with the central one at the systemic redshift, indicating a ionised tunnel through which both Lya and LyC radiation escape; (b) the large O32 oxygen index ([OIII]4959-5007 / [OII]3727-3729) of 9.18(-1.32/+1.82) is compatible to those measured in local (z~0.4) LyC leakers; (c) there are narrow nebular high-ionisation metal lines with 蟽_v < 20 km/s, which confirms the presence of young hot, massive stars. The HeII1640 appears broad, consistent with a young stellar component including Wolf-Rayet stars. Similarly, the Sunburst LyC-emitter shows a triple-peaked Lya profile and from VLT/MUSE spectroscopy the presence of spectral features arising from young hot and massive stars. The strong lensing magnification, (渭> 20), suggests that this exceptional object is a gravitationally-bound star cluster observed at a cosmological distance, with a stellar mass M <~ 10^7 Msun and an effective radius smaller than 20 pc. Intriguingly, sources like Sunburst but without lensing magnification might appear as Ion2-like galaxies, in which unresolved massive star clusters dominate the ultraviolet emission. This work supports the idea that dense young star clusters can contribute to the ionisation of the IGM through holes created by stellar feedback. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.07941v3-abstract-full').style.display = 'none'; document.getElementById('1904.07941v3-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 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">13 pages, 9 figures and 1 table, MNRAS accepted. Some typos fixed</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1811.07935">arXiv:1811.07935</a> <span> [<a href="https://arxiv.org/pdf/1811.07935">pdf</a>, <a href="https://arxiv.org/format/1811.07935">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/10.1051/0004-6361/201834372">10.1051/0004-6361/201834372 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MAGNUM survey: different gas properties in the outflowing and disk components in nearby active galaxies with MUSE </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mingozzi%2C+M">M. Mingozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Cresci%2C+G">G. Cresci</a>, <a href="/search/astro-ph?searchtype=author&query=Venturi%2C+G">G. Venturi</a>, <a href="/search/astro-ph?searchtype=author&query=Marconi%2C+A">A. Marconi</a>, <a href="/search/astro-ph?searchtype=author&query=Mannucci%2C+F">F. Mannucci</a>, <a href="/search/astro-ph?searchtype=author&query=Perna%2C+M">M. Perna</a>, <a href="/search/astro-ph?searchtype=author&query=Belfiore%2C+F">F. Belfiore</a>, <a href="/search/astro-ph?searchtype=author&query=Carniani%2C+S">S. Carniani</a>, <a href="/search/astro-ph?searchtype=author&query=Balmaverde%2C+B">B. Balmaverde</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Cicone%2C+C">C. Cicone</a>, <a href="/search/astro-ph?searchtype=author&query=Feruglio%2C+C">C. Feruglio</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">A. Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Mainieri%2C+V">V. Mainieri</a>, <a href="/search/astro-ph?searchtype=author&query=Maiolino%2C+R">R. Maiolino</a>, <a href="/search/astro-ph?searchtype=author&query=Nagao%2C+T">T. Nagao</a>, <a href="/search/astro-ph?searchtype=author&query=Nardini%2C+E">E. Nardini</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Tozzi%2C+P">P. Tozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Zibetti%2C+S">S. Zibetti</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="1811.07935v2-abstract-short" style="display: inline;"> We investigated the interstellar medium properties of the disc and outflowing gas in the central regions of nine nearby Seyfert galaxies, all characterised by prominent outflows. These objects are part of the Measuring Active Galactic Nuclei Under MUSE Microscope survey, which aims to probe their physical conditions and ionisation mechanism by exploiting MUSE unprecedented sensitivity. We studied… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.07935v2-abstract-full').style.display = 'inline'; document.getElementById('1811.07935v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1811.07935v2-abstract-full" style="display: none;"> We investigated the interstellar medium properties of the disc and outflowing gas in the central regions of nine nearby Seyfert galaxies, all characterised by prominent outflows. These objects are part of the Measuring Active Galactic Nuclei Under MUSE Microscope survey, which aims to probe their physical conditions and ionisation mechanism by exploiting MUSE unprecedented sensitivity. We studied the different properties of the gas in the disc and outflow with spatially and kinematically resolved maps by dividing the strongest emission lines in velocity bins. We associated the core of the lines with the disc, consistent with the stellar velocity, and the redshifted and the blueshifted wings with the outflow. We find that the outflowing gas is characterised by higher values of density and ionisation parameter than the disc, which presents a higher dust extinction. Moreover, we distinguish high- and low-ionisation regions across the portion of spatially resolved narrow-line region traced by the outflowing gas. The high-ionisation regions characterised by the lowest [NII]/H伪 and [SII]/H伪 line ratios generally trace the innermost parts along the axis of the emitting cones where the [SIII]/[SII] line ratio is enhanced, while the low-ionisation regions follow the cone edges and/or the regions perpendicular to the axis of the outflows, also characterised by a higher [OIII] velocity dispersion. A possible scenario to explain these features relies on the presence of two distinct populations of line emitting clouds: one is optically thin to the radiation and is characterised by the highest excitation, while the other is optically thick and is impinged by a filtered, and thus harder, radiation field which generates strong low-excitation lines. The highest values of [NII]/H伪 and [SII]/H伪 line ratios may be due to shocks and/or a hard filtered radiation field from the AGN. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.07935v2-abstract-full').style.display = 'none'; document.getElementById('1811.07935v2-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 January, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 November, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">28 pages, 19 figures. Forthcoming article 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 622, A146 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1809.01206">arXiv:1809.01206</a> <span> [<a href="https://arxiv.org/pdf/1809.01206">pdf</a>, <a href="https://arxiv.org/format/1809.01206">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/10.1051/0004-6361/201833668">10.1051/0004-6361/201833668 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MAGNUM survey: A MUSE-Chandra resolved view on ionized outflows and photoionization in the Seyfert galaxy NGC 1365 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Venturi%2C+G">G. Venturi</a>, <a href="/search/astro-ph?searchtype=author&query=Nardini%2C+E">E. Nardini</a>, <a href="/search/astro-ph?searchtype=author&query=Marconi%2C+A">A. Marconi</a>, <a href="/search/astro-ph?searchtype=author&query=Carniani%2C+S">S. Carniani</a>, <a href="/search/astro-ph?searchtype=author&query=Mingozzi%2C+M">M. Mingozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Cresci%2C+G">G. Cresci</a>, <a href="/search/astro-ph?searchtype=author&query=Mannucci%2C+F">F. Mannucci</a>, <a href="/search/astro-ph?searchtype=author&query=Risaliti%2C+G">G. Risaliti</a>, <a href="/search/astro-ph?searchtype=author&query=Maiolino%2C+R">R. Maiolino</a>, <a href="/search/astro-ph?searchtype=author&query=Balmaverde%2C+B">B. Balmaverde</a>, <a href="/search/astro-ph?searchtype=author&query=Bongiorno%2C+A">A. Bongiorno</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Capetti%2C+A">A. Capetti</a>, <a href="/search/astro-ph?searchtype=author&query=Cicone%2C+C">C. Cicone</a>, <a href="/search/astro-ph?searchtype=author&query=Ciroi%2C+S">S. Ciroi</a>, <a href="/search/astro-ph?searchtype=author&query=Feruglio%2C+C">C. Feruglio</a>, <a href="/search/astro-ph?searchtype=author&query=Fiore%2C+F">F. Fiore</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">A. Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=La+Franca%2C+F">F. La Franca</a>, <a href="/search/astro-ph?searchtype=author&query=Mainieri%2C+V">V. Mainieri</a>, <a href="/search/astro-ph?searchtype=author&query=Matsuoka%2C+K">K. Matsuoka</a>, <a href="/search/astro-ph?searchtype=author&query=Nagao%2C+T">T. Nagao</a>, <a href="/search/astro-ph?searchtype=author&query=Perna%2C+M">M. Perna</a>, <a href="/search/astro-ph?searchtype=author&query=Piconcelli%2C+E">E. Piconcelli</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</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="1809.01206v1-abstract-short" style="display: inline;"> Ionized outflows, revealed by broad asymmetric wings of the [OIII] line, are commonly observed in AGN but the low intrinsic spatial resolution of observations has generally prevented a detailed characterization of their properties. The MAGNUM survey aims at overcoming these limitations by focusing on the nearest AGN, including NGC 1365, a nearby Seyfert galaxy (D~17 Mpc), hosting a low-luminosity… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1809.01206v1-abstract-full').style.display = 'inline'; document.getElementById('1809.01206v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1809.01206v1-abstract-full" style="display: none;"> Ionized outflows, revealed by broad asymmetric wings of the [OIII] line, are commonly observed in AGN but the low intrinsic spatial resolution of observations has generally prevented a detailed characterization of their properties. The MAGNUM survey aims at overcoming these limitations by focusing on the nearest AGN, including NGC 1365, a nearby Seyfert galaxy (D~17 Mpc), hosting a low-luminosity AGN (Lbol ~ 2x10^43 erg/s). We want to obtain a detailed picture of the ionized gas in the central ~5 kpc of NGC 1365 in terms of physical properties, kinematics, and ionization mechanisms. We also aim to characterize the warm ionized outflow as a function of distance from the nucleus and its relation with the nuclear X-ray wind. We employed VLT/MUSE optical integral field spectroscopic observations to investigate the warm ionized gas and Chandra ACIS-S X-ray data for the hot highly-ionized phase. We obtained flux, kinematic, and diagnostic maps of the optical emission lines, which we used to disentangle outflows from disk motions and measure the gas properties down to a spatial resolution of ~70 pc. [OIII] emission mostly traces an AGN-ionized kpc-scale biconical outflow with velocities up to ~200 km/s. H伪 emission traces instead star formation in a circumnuclear ring and along the bar, where we detect non-circular motions. Soft X-rays are mostly due to thermal emission from the star-forming regions, but we could isolate the AGN photoionized component which matches the [OIII] emission. The mass outflow rate of the extended ionized outflow matches that of the nuclear X-ray wind and then decreases with radius. However, the hard X-ray emission from the circumnuclear ring suggests that star formation might contribute to the outflow. The integrated mass outflow rate, kinetic energy rate, and outflow velocity are broadly consistent with the typical relations observed in more luminous AGN. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1809.01206v1-abstract-full').style.display = 'none'; document.getElementById('1809.01206v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 September, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">Accepted for publication on Astronomy and Astrophysics. 22 pages, 14 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 619, A74 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1806.09493">arXiv:1806.09493</a> <span> [<a href="https://arxiv.org/pdf/1806.09493">pdf</a>, <a href="https://arxiv.org/format/1806.09493">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/10.1051/0004-6361/201833052">10.1051/0004-6361/201833052 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Spectroscopic characterization of the protocluster of galaxies around 7C 1756+6520 at z ~ 1.4 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Casasola%2C+V">V. Casasola</a>, <a href="/search/astro-ph?searchtype=author&query=Magrini%2C+L">L. Magrini</a>, <a href="/search/astro-ph?searchtype=author&query=Combes%2C+F">F. Combes</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Fritz%2C+J">J. Fritz</a>, <a href="/search/astro-ph?searchtype=author&query=Rodighiero%2C+G">G. Rodighiero</a>, <a href="/search/astro-ph?searchtype=author&query=Poggianti%2C+B">B. Poggianti</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+S">S. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Liuzzo%2C+E">E. Liuzzo</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="1806.09493v2-abstract-short" style="display: inline;"> The aim of this paper is the spectroscopic study of 13 galaxies belonging to the field of the protocluster associated with the radio galaxy (RG) 7C 1756+6520 at z = 1.4156. In particular, we focus on the characterization of the nuclear activity. This analysis has been performed on rest-frame optical spectra taken with LBT-LUCI. The spectral coverage allowed us to observe emission lines such as Hal… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.09493v2-abstract-full').style.display = 'inline'; document.getElementById('1806.09493v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1806.09493v2-abstract-full" style="display: none;"> The aim of this paper is the spectroscopic study of 13 galaxies belonging to the field of the protocluster associated with the radio galaxy (RG) 7C 1756+6520 at z = 1.4156. In particular, we focus on the characterization of the nuclear activity. This analysis has been performed on rest-frame optical spectra taken with LBT-LUCI. The spectral coverage allowed us to observe emission lines such as Halpha, Hbeta, [Oiii]5007 A, and [Nii]6583 A at the z of the central RG. We observed the central part of the protocluster, which is suitable to include the radio galaxy, several spectroscopically confirmed AGN belonging to the protocluster, and other objects that might be members of the protocluster. For four previously identified protocluster members, we derived the redshift by detecting emission lines that have never detected before for these galaxies. The stacked spectrum of the galaxies in which we detected the [Oiii]5007 A emission line revealed the presence of the second line of the [Oiii] doublet at 4959 A and of Hbeta, which confirms that they belong to the protocluster. By collecting all members identified so far in this work and other members from the literature, we defined 31 galaxies, including the central RG, around z = 1.4152 +/- 0.056, corresponding to peculiar velocities <~5000 km/s with respect to the RG. The PV phase-space diagram suggests that 3 protocluster AGN and the central RG might be a virialized population that has been coexisting for a long time in the densest core region of this forming structure. This protocluster is characterized by a high fraction of AGN (23%). For one of them, AGN1317, we produced 2 BPT diagrams. The high fraction of AGN and their distribution within the protocluster seem to be consistent with predictions of some theoretical models on AGN growth and feedback. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.09493v2-abstract-full').style.display = 'none'; document.getElementById('1806.09493v2-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 June, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 June, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">Accepted for publication in A&A, 17 pages, 8 Figures, 2 Tables. Revised 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/1804.04842">arXiv:1804.04842</a> <span> [<a href="https://arxiv.org/pdf/1804.04842">pdf</a>, <a href="https://arxiv.org/format/1804.04842">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/aabe30">10.3847/1538-4357/aabe30 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Resolving the nuclear obscuring disk in the Compton-thick Seyfert galaxy NGC5643 with ALMA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Alonso-Herrero%2C+A">A. Alonso-Herrero</a>, <a href="/search/astro-ph?searchtype=author&query=Pereira-Santaella%2C+M">M. Pereira-Santaella</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa-Burillo%2C+S">S. Garc铆a-Burillo</a>, <a href="/search/astro-ph?searchtype=author&query=Davies%2C+R+I">R. I. Davies</a>, <a href="/search/astro-ph?searchtype=author&query=Combes%2C+F">F. Combes</a>, <a href="/search/astro-ph?searchtype=author&query=Asmus%2C+D">D. Asmus</a>, <a href="/search/astro-ph?searchtype=author&query=Bunker%2C+A">A. Bunker</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%ADaz-Santos%2C+T">T. D铆az-Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Gandhi%2C+P">P. Gandhi</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez-Mart%C3%ADn%2C+O">O. Gonz谩lez-Mart铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1n-Caballero%2C+A">A. Hern谩n-Caballero</a>, <a href="/search/astro-ph?searchtype=author&query=Hicks%2C+E">E. Hicks</a>, <a href="/search/astro-ph?searchtype=author&query=H%C3%B6nig%2C+S">S. H枚nig</a>, <a href="/search/astro-ph?searchtype=author&query=Labiano%2C+A">A. Labiano</a>, <a href="/search/astro-ph?searchtype=author&query=Levenson%2C+N+A">N. A. Levenson</a>, <a href="/search/astro-ph?searchtype=author&query=Packham%2C+C">C. Packham</a>, <a href="/search/astro-ph?searchtype=author&query=Almeida%2C+C+R">C. Ramos Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+C">C. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Rigopoulou%2C+D">D. Rigopoulou</a>, <a href="/search/astro-ph?searchtype=author&query=Rosario%2C+D">D. Rosario</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Ward%2C+M+J">M. J. Ward</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="1804.04842v2-abstract-short" style="display: inline;"> We present ALMA Band 6 $^{12}$CO(2--1) line and rest-frame 232GHz continuum observations of the nearby Compton-thick Seyfert galaxy NGC5643 with angular resolutions 0.11-0.26arcsec (9-21pc). The CO(2--1) integrated line map reveals emission from the nuclear and circumnuclear region with a two-arm nuclear spiral extending 10arcsec on each side. The circumnuclear CO(2--1) kinematics can be fitted wi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.04842v2-abstract-full').style.display = 'inline'; document.getElementById('1804.04842v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1804.04842v2-abstract-full" style="display: none;"> We present ALMA Band 6 $^{12}$CO(2--1) line and rest-frame 232GHz continuum observations of the nearby Compton-thick Seyfert galaxy NGC5643 with angular resolutions 0.11-0.26arcsec (9-21pc). The CO(2--1) integrated line map reveals emission from the nuclear and circumnuclear region with a two-arm nuclear spiral extending 10arcsec on each side. The circumnuclear CO(2--1) kinematics can be fitted with a rotating disk, although there are regions with large residual velocities and/or velocity dispersions. The CO(2--1) line profiles of these regions show two different velocity components. One is ascribed to the circular component and the other to the interaction of the AGN outflow, as traced by the [O III]5007AA emission, with molecular gas in the disk a few hundred parsecs from the AGN. On nuclear scales, we detected an inclined CO(2--1) disk (diameter 26 pc, FWHM) oriented almost in a north-south direction. The CO(2--1) nuclear kinematics can be fitted with a rotating disk which appears to be tilted with respect to the large scale disk. There are strong non-circular motions in the central 0.2-0.3 arcsec with velocities of up to 110km/s. In the absence of a nuclear bar, these motions could be explained as radial outflows in the nuclear disk. We estimate a total molecular gas mass for the nuclear disk of $M({\rm H}_2)=1.1\times 10^7\,M_\odot$ and an H$_2$ column density toward the location of the AGN of $N({\rm H}_2)\sim 5 \times 10^{23}\,{\rm cm}^{-2}$, for a standard CO-to-H$_2$ conversion factor. We interpret this nuclear molecular gas disk as the obscuring torus of NGC5643 as well as the collimating structure of the ionization cone. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.04842v2-abstract-full').style.display = 'none'; document.getElementById('1804.04842v2-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> 10 May, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 April, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">16 papes, 9 figures. Accepted to ApJ. Updated Fig.4</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1803.11013">arXiv:1803.11013</a> <span> [<a href="https://arxiv.org/pdf/1803.11013">pdf</a>, <a href="https://arxiv.org/format/1803.11013">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/10.3389/fspas.2018.00002">10.3389/fspas.2018.00002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> NGC 1275: an outlier of the black hole-host scaling relations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">Eleonora Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">Federica Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=La+Franca%2C+F">Fabio La Franca</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+S">Stefano Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Bongiorno%2C+A">Angela Bongiorno</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">Marcella Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Marconi%2C+A">Alessandro Marconi</a>, <a href="/search/astro-ph?searchtype=author&query=Onori%2C+F">Francesca Onori</a>, <a href="/search/astro-ph?searchtype=author&query=Shankar%2C+F">Francesco Shankar</a>, <a href="/search/astro-ph?searchtype=author&query=Vignali%2C+C">Cristian 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="1803.11013v1-abstract-short" style="display: inline;"> The active galaxy NGC 1275 lies at the center of the Perseus cluster of galaxies, being an archetypal BH-galaxy system that is supposed to fit well with the M_BH-host scaling relations obtained for quiescent galaxies. Since it harbours an obscured AGN, only recently our group has been able to estimate its black hole mass. Here our aim is to pinpoint NGC 1275 on the less dispersed scaling relations… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1803.11013v1-abstract-full').style.display = 'inline'; document.getElementById('1803.11013v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1803.11013v1-abstract-full" style="display: none;"> The active galaxy NGC 1275 lies at the center of the Perseus cluster of galaxies, being an archetypal BH-galaxy system that is supposed to fit well with the M_BH-host scaling relations obtained for quiescent galaxies. Since it harbours an obscured AGN, only recently our group has been able to estimate its black hole mass. Here our aim is to pinpoint NGC 1275 on the less dispersed scaling relations, namely the M_BH-sigma_star and M_BH-L_bul planes. Starting from our previous work Ricci et al. 2017b, we estimate that NGC 1275 falls well outside the intrinsic dispersion of the M_BH-sigma_star plane being ~1.2 dex (in black hole mass) displaced with respect to the scaling relations. We then perform a 2D morphological decomposition analysis on Spitzer/IRAC images at 3.6 mic and find that, beyond the bright compact nucleus that dominates the central emission, NGC 1275 follows a de Vaucouleurs profile with no sign of significant star formation nor clear merger remnants. Nonetheless, its displacement on the M_BH-L_(3.6,bul) plane with respect to the scaling relation is as high as observed in the M_BH-sigma_star. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1803.11013v1-abstract-full').style.display = 'none'; document.getElementById('1803.11013v1-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 March, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">12 pages, 3 figures. Published in Frontiers in Astronomy and Space Sciences</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Front. Astron. Space Sci. 5:2 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1802.05613">arXiv:1802.05613</a> <span> [<a href="https://arxiv.org/pdf/1802.05613">pdf</a>, <a href="https://arxiv.org/format/1802.05613">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/10.1051/0004-6361/201832694">10.1051/0004-6361/201832694 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The 500 ks Chandra observation of the z = 6.31 QSO SDSS J1030+0524 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Nanni%2C+R">R. Nanni</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=Mignoli%2C+M">M. Mignoli</a>, <a href="/search/astro-ph?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Zamorani%2C+G">G. Zamorani</a>, <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">F. Calura</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzuisi%2C+G">G. Lanzuisi</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Tozzi%2C+P">P. Tozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Iwasawa%2C+K">K. Iwasawa</a>, <a href="/search/astro-ph?searchtype=author&query=Cappi%2C+M">M. Cappi</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=Costa%2C+T">T. Costa</a>, <a href="/search/astro-ph?searchtype=author&query=Risaliti%2C+G">G. Risaliti</a>, <a href="/search/astro-ph?searchtype=author&query=Paolillo%2C+M">M. Paolillo</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=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Chiaberge%2C+M">M. Chiaberge</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=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Cappelluti%2C+N">N. Cappelluti</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="1802.05613v1-abstract-short" style="display: inline;"> We present the results from a $\sim500$ ks Chandra observation of the $z=6.31$ QSO SDSS J1030+0524. This is the deepest X-ray observation to date of a $z\sim6$ QSO. The QSO is detected with a total of 125 net counts in the full ($0.5-7$ keV) band and its spectrum can be modeled by a single power-law model with photon index of $螕= 1.81 \pm 0.18$ and full band flux of $f=3.95\times 10^{-15}$ erg s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.05613v1-abstract-full').style.display = 'inline'; document.getElementById('1802.05613v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1802.05613v1-abstract-full" style="display: none;"> We present the results from a $\sim500$ ks Chandra observation of the $z=6.31$ QSO SDSS J1030+0524. This is the deepest X-ray observation to date of a $z\sim6$ QSO. The QSO is detected with a total of 125 net counts in the full ($0.5-7$ keV) band and its spectrum can be modeled by a single power-law model with photon index of $螕= 1.81 \pm 0.18$ and full band flux of $f=3.95\times 10^{-15}$ erg s$^{-1}$ cm$^{-2}$. When compared with the data obtained by XMM-Newton in 2003, our Chandra observation in 2017 shows a harder ($螖螕\approx -0.6$) spectrum and a 2.5 times fainter flux. Such a variation, in a timespan of $\sim2$ yrs rest-frame, is unexpected for such a luminous QSO powered by a $> 10^9 \: M_{\odot}$ black hole. The observed source hardening and weakening could be related to an intrinsic variation in the accretion rate. However, the limited photon statistics does not allow us to discriminate between an intrinsic luminosity and spectral change, and an absorption event produced by an intervening gas cloud along the line of sight. We also report the discovery of diffuse X-ray emission that extends for 30"x20" southward the QSO with a signal-to-noise ratio of $\sim$6, hardness ratio of $HR=0.03_{-0.25}^{+0.20}$, and soft band flux of $f_{0.5-2 \: keV}= 1.1_{-0.3}^{+0.3} \times 10^{-15}$ erg s$^{-1}$ cm$^{-2}$, that is not associated to a group or cluster of galaxies. We discuss two possible explanations for the extended emission, which may be either associated with the radio lobe of a nearby, foreground radio galaxy (at $z \approx 1-2$), or ascribed to the feedback from the QSO itself acting on its surrounding environment, as proposed by simulations of early black hole formation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.05613v1-abstract-full').style.display = 'none'; document.getElementById('1802.05613v1-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> 15 February, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">13 pages, 9 figures, A&A accepted</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 614, A121 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1802.03423">arXiv:1802.03423</a> <span> [<a href="https://arxiv.org/pdf/1802.03423">pdf</a>, <a href="https://arxiv.org/format/1802.03423">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/10.1051/0004-6361/201732335">10.1051/0004-6361/201732335 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The WISSH Quasars Project IV. BLR versus kpc-scale winds </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vietri%2C+G">G. Vietri</a>, <a href="/search/astro-ph?searchtype=author&query=Piconcelli%2C+E">E. Piconcelli</a>, <a href="/search/astro-ph?searchtype=author&query=Bischetti%2C+M">M. Bischetti</a>, <a href="/search/astro-ph?searchtype=author&query=Duras%2C+F">F. Duras</a>, <a href="/search/astro-ph?searchtype=author&query=Martocchia%2C+S">S. Martocchia</a>, <a href="/search/astro-ph?searchtype=author&query=Bongiorno%2C+A">A. Bongiorno</a>, <a href="/search/astro-ph?searchtype=author&query=Marconi%2C+A">A. Marconi</a>, <a href="/search/astro-ph?searchtype=author&query=Zappacosta%2C+L">L. Zappacosta</a>, <a href="/search/astro-ph?searchtype=author&query=Bisogni%2C+S">S. Bisogni</a>, <a href="/search/astro-ph?searchtype=author&query=Bruni%2C+G">G. Bruni</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/astro-ph?searchtype=author&query=Cresci%2C+G">G. Cresci</a>, <a href="/search/astro-ph?searchtype=author&query=Feruglio%2C+C">C. Feruglio</a>, <a href="/search/astro-ph?searchtype=author&query=Giallongo%2C+E">E. Giallongo</a>, <a href="/search/astro-ph?searchtype=author&query=La+Franca%2C+F">F. La Franca</a>, <a href="/search/astro-ph?searchtype=author&query=Mainieri%2C+V">V. Mainieri</a>, <a href="/search/astro-ph?searchtype=author&query=Mannucci%2C+F">F. Mannucci</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">F. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Testa%2C+V">V. Testa</a>, <a href="/search/astro-ph?searchtype=author&query=Tombesi%2C+F">F. Tombesi</a>, <a href="/search/astro-ph?searchtype=author&query=Vignali%2C+C">C. Vignali</a>, <a href="/search/astro-ph?searchtype=author&query=Fiore%2C+F">F. Fiore</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="1802.03423v1-abstract-short" style="display: inline;"> We have undertaken a multi-band observing program aimed at obtaining a complete census of winds in a sample of WISE/SDSS selected hyper-luminous (WISSH) QSOs at z~2-4. We have analyzed the rest-frame optical (LBT/LUCI and VLT/SINFONI) and UV (SDSS) spectra of 18 randomly selected WISSH QSOs to measure the SMBH mass and study the properties of winds both in the NLR and BLR traced by blueshifted/ske… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.03423v1-abstract-full').style.display = 'inline'; document.getElementById('1802.03423v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1802.03423v1-abstract-full" style="display: none;"> We have undertaken a multi-band observing program aimed at obtaining a complete census of winds in a sample of WISE/SDSS selected hyper-luminous (WISSH) QSOs at z~2-4. We have analyzed the rest-frame optical (LBT/LUCI and VLT/SINFONI) and UV (SDSS) spectra of 18 randomly selected WISSH QSOs to measure the SMBH mass and study the properties of winds both in the NLR and BLR traced by blueshifted/skewed [OIII] and CIV emission lines, respectively. These WISSH QSOs are powered by SMBH with masses $\ge$10$^9$ Msun accreting at 0.4<$位_{Edd}$<3.1. We have found the existence of two sub-populations characterized by the presence of outflows at different distances from the SMBH. One population ([OIII] sources) exhibits powerful [OIII] outflows, rest-frame EW (REW) of the CIV emission REW$_{CIV}\approx$20-40 A and modest CIV velocity shift (v$_{CIV}^{peak}$) with respect to the systemic redshift (<=2000 km/s). The second population (Weak [OIII] sources), representing ~70% of the analyzed WISSH QSOs, shows weak/absent [OIII] emission and an extremely large v$_{CIV}^{peak}$ (up to ~8000 km/s and REW$_{CIV}$<=20 A). We propose two explanations for the observed behavior of the strength of the [OIII] emission in terms of orientation effects of the line of sight and ionization cone. The dichotomy in the presence of BLR and NLR winds could be likely due to inclination effects considering a polar geometry scenario for the BLR winds. We find a strong correlation with L$_{Bol}$ and an anti-correlation with $伪_{ox}$, whereby the higher L$_{Bol}$, the steeper $伪_{ox}$ and the larger is the v$_{CIV}^{peak}$. Finally, the observed dependence v$_{CIV}^{peak}\propto L_{Bol}^{0.28\pm0.04}$ is consistent with radiatively driven winds scenario, where strong UV continuum is necessary to launch the wind and a weakness of the X-ray emission is fundamental to prevent overionization of the wind itself. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.03423v1-abstract-full').style.display = 'none'; document.getElementById('1802.03423v1-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, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">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 617, A81 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1712.07661">arXiv:1712.07661</a> <span> [<a href="https://arxiv.org/pdf/1712.07661">pdf</a>, <a href="https://arxiv.org/format/1712.07661">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/mnrasl/sly023">10.1093/mnrasl/sly023 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Direct Lyman continuum and Lyman-alpha escape observed at redshift 4 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Nonino%2C+M">M. Nonino</a>, <a href="/search/astro-ph?searchtype=author&query=Cupani%2C+G">G. Cupani</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Mignoli%2C+M">M. Mignoli</a>, <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">F. Calura</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">M. Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">R. Gilli</a>, <a href="/search/astro-ph?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">A. Mercurio</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=Caputi%2C+K">K. Caputi</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Cristiani%2C+S">S. Cristiani</a>, <a href="/search/astro-ph?searchtype=author&query=Balestra%2C+I">I. Balestra</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">A. Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Giavalisco%2C+M">M. Giavalisco</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="1712.07661v2-abstract-short" style="display: inline;"> We report on the serendipitous discovery of a z=4.0, M1500=-22.20 star-forming galaxy (Ion3) showing copious Lyman continuum (LyC) leakage (~60% escaping), a remarkable multiple peaked Lya emission, and significant Lya radiation directly emerging at the resonance frequency. This is the highest redshift confirmed LyC emitter in which the ionising and Lya radiation possibly share a common ionised ca… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1712.07661v2-abstract-full').style.display = 'inline'; document.getElementById('1712.07661v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1712.07661v2-abstract-full" style="display: none;"> We report on the serendipitous discovery of a z=4.0, M1500=-22.20 star-forming galaxy (Ion3) showing copious Lyman continuum (LyC) leakage (~60% escaping), a remarkable multiple peaked Lya emission, and significant Lya radiation directly emerging at the resonance frequency. This is the highest redshift confirmed LyC emitter in which the ionising and Lya radiation possibly share a common ionised cavity (with N_HI<10^17.2 cm^-2). Ion3 is spatially resolved, it shows clear stellar winds signatures like the P-Cygni NV1240 profile, and has blue ultraviolet continuum (尾= -2.5 +/- 0.25, F_位~ 位^尾) with weak low-ionisation interstellar metal lines. Deep VLT/HAWKI Ks and Spitzer/IRAC 3.6um and 4.5um imaging show a clear photometric signature of the Halpha line with equivalent width of 1000A rest-frame emerging over a flat continuum (Ks-4.5um ~ 0). From the SED fitting we derive a stellar mass of 1.5x10^9 Msun, SFR of 140 Msun/yr and age of ~10 Myr, with a low dust extinction, E(B-V)< 0.1, placing the source in the starburst region of the SFR-M^* plane. Ion3 shows similar properties of another LyC emitter previously discovered (z=3.21, Ion2, Vanzella et al. 2016). Ion3 (and Ion2) represents ideal high-redshift reference cases to guide the search for reionising sources at z>6.5 with JWST. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1712.07661v2-abstract-full').style.display = 'none'; document.getElementById('1712.07661v2-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 March, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 December, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in MNRAS. 5 pages, 4 figures, 1 table</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1706.08987">arXiv:1706.08987</a> <span> [<a href="https://arxiv.org/pdf/1706.08987">pdf</a>, <a href="https://arxiv.org/format/1706.08987">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/10.1051/0004-6361/201730672">10.1051/0004-6361/201730672 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> AGN feedback on molecular gas reservoirs in quasars at $z\sim$2.4 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Carniani%2C+S">S. Carniani</a>, <a href="/search/astro-ph?searchtype=author&query=Marconi%2C+A">A. Marconi</a>, <a href="/search/astro-ph?searchtype=author&query=Maiolino%2C+R">R. Maiolino</a>, <a href="/search/astro-ph?searchtype=author&query=Feruglio%2C+C">C. Feruglio</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Cresci%2C+G">G. Cresci</a>, <a href="/search/astro-ph?searchtype=author&query=Cano-D%C3%ADaz%2C+M">M. Cano-D铆az</a>, <a href="/search/astro-ph?searchtype=author&query=Cicone%2C+C">C. Cicone</a>, <a href="/search/astro-ph?searchtype=author&query=Balmaverde%2C+B">B. Balmaverde</a>, <a href="/search/astro-ph?searchtype=author&query=Fiore%2C+F">F. Fiore</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrara%2C+A">A. Ferrara</a>, <a href="/search/astro-ph?searchtype=author&query=Gallerani%2C+S">S. Gallerani</a>, <a href="/search/astro-ph?searchtype=author&query=La+Franca%2C+F">F. La Franca</a>, <a href="/search/astro-ph?searchtype=author&query=Mainieri%2C+V">V. Mainieri</a>, <a href="/search/astro-ph?searchtype=author&query=Mannucci%2C+F">F. Mannucci</a>, <a href="/search/astro-ph?searchtype=author&query=Netzer%2C+H">H. Netzer</a>, <a href="/search/astro-ph?searchtype=author&query=Piconcelli%2C+E">E. Piconcelli</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Schneider%2C+R">R. Schneider</a>, <a href="/search/astro-ph?searchtype=author&query=Shemmer%2C+O">O. Shemmer</a>, <a href="/search/astro-ph?searchtype=author&query=Testi%2C+L">L. Testi</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="1706.08987v2-abstract-short" style="display: inline;"> We present new ALMA observations aimed at mapping molecular gas reservoirs through the CO(3-2) transition in three quasars at $z\simeq2.4$, LBQS 0109+0213, 2QZ J002830.4-281706, and [HB89] 0329-385. Previous [OIII]5007 observations of these quasars showed evidence for ionised outflows quenching star formation in their host galaxies. Systemic CO(3-2) emission has been detected only in one quasar, L… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1706.08987v2-abstract-full').style.display = 'inline'; document.getElementById('1706.08987v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1706.08987v2-abstract-full" style="display: none;"> We present new ALMA observations aimed at mapping molecular gas reservoirs through the CO(3-2) transition in three quasars at $z\simeq2.4$, LBQS 0109+0213, 2QZ J002830.4-281706, and [HB89] 0329-385. Previous [OIII]5007 observations of these quasars showed evidence for ionised outflows quenching star formation in their host galaxies. Systemic CO(3-2) emission has been detected only in one quasar, LBQS 0109+0213, where the CO(3-2) emission is spatially anti-correlated with the ionised outflow, suggesting that most of the molecular gas may have been dispersed or heated in the region swept by the outflow. In all three sources, including the one detected in CO, our constraints on the molecular gas mass indicate a significantly reduced reservoir compared to main-sequence galaxies at the same redshift, supporting a negative feedback scenario. In the quasar 2QZ J002830.4-281706, we tentatively detect an emission line blob blue-shifted by $v\sim-2000$ km/s with respect to the galaxy systemic velocity and spatially offset by 0.2 arcsec (1.7 kpc) with respect to the ALMA continuum peak. Interestingly, such emission feature is coincident in both velocity and space with the ionised outflow as seen in [OIII]5007. This tentative detection must be confirmed with deeper observations but, if real, it could represent the molecular counterpart of the ionised gas outflow driven by the AGN. Finally, in all ALMA maps we detect the presence of serendipitous line emitters within a projected distance $\sim 160$ kpc from the quasars. By identifying these features with the CO(3-2) transition, the serendipitous line emitters would be located within |$螖v$|$<$500 km/s from the quasars, hence suggesting an overdensity of galaxies in two out of three quasars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1706.08987v2-abstract-full').style.display = 'none'; document.getElementById('1706.08987v2-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 July, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 June, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 13 figures, 4 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 605, A105 (2017) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1706.06110">arXiv:1706.06110</a> <span> [<a href="https://arxiv.org/pdf/1706.06110">pdf</a>, <a href="https://arxiv.org/ps/1706.06110">ps</a>, <a href="https://arxiv.org/format/1706.06110">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/mnrasl/slx103">10.1093/mnrasl/slx103 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Detection of faint broad emission lines in type 2 AGN: III. On the $M_{BH} - 蟽_\star$ relation of type 2 AGN </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">F. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=La+Franca%2C+F">F. La Franca</a>, <a href="/search/astro-ph?searchtype=author&query=Marconi%2C+A">A. Marconi</a>, <a href="/search/astro-ph?searchtype=author&query=Onori%2C+F">F. Onori</a>, <a href="/search/astro-ph?searchtype=author&query=Shankar%2C+F">F. Shankar</a>, <a href="/search/astro-ph?searchtype=author&query=Schneider%2C+R">R. Schneider</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+S">S. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Bongiorno%2C+A">A. Bongiorno</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Fiore%2C+F">F. Fiore</a>, <a href="/search/astro-ph?searchtype=author&query=Maiolino%2C+R">R. Maiolino</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="1706.06110v1-abstract-short" style="display: inline;"> Type 2 active galactic nuclei (AGN) represent the majority of the AGN population. However, due to the difficulties in measuring their black hole (BH) masses, it is still unknown whether they follow the same BH mass-host galaxy scaling relations valid for quiescent galaxies and type 1 AGN. Here we present the locus of type 2 AGN having virial BH mass estimates in the $M_{BH}-蟽_\star$ plane. Our ana… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1706.06110v1-abstract-full').style.display = 'inline'; document.getElementById('1706.06110v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1706.06110v1-abstract-full" style="display: none;"> Type 2 active galactic nuclei (AGN) represent the majority of the AGN population. However, due to the difficulties in measuring their black hole (BH) masses, it is still unknown whether they follow the same BH mass-host galaxy scaling relations valid for quiescent galaxies and type 1 AGN. Here we present the locus of type 2 AGN having virial BH mass estimates in the $M_{BH}-蟽_\star$ plane. Our analysis shows that the BH masses of type 2 AGN are $\sim0.9$ dex smaller than type 1 AGN at $蟽_\star\sim 185$ km s$^{-1}$, regardless of the (early/late) AGN host galaxy morphology. Equivalently, type 2 AGN host galaxies have stellar velocity dispersions $\sim 0.2$ dex higher than type 1 AGN hosts at $M_{BH}\sim10^7$ M$_\odot$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1706.06110v1-abstract-full').style.display = 'none'; document.getElementById('1706.06110v1-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 June, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2017. </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">6 pages, 3 figures, accepted for publication in MNRAS Letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1706.02317">arXiv:1706.02317</a> <span> [<a href="https://arxiv.org/pdf/1706.02317">pdf</a>, <a href="https://arxiv.org/format/1706.02317">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/10.1051/0004-6361/201730683">10.1051/0004-6361/201730683 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The primordial environment of supermassive black holes (II): deep Y and J band images around the z=6.3 quasar SDSS J1030+0524 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Balmaverde%2C+B">B. Balmaverde</a>, <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=Bolzonella%2C+M">M. Bolzonella</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Cappelluti%2C+N">N. Cappelluti</a>, <a href="/search/astro-ph?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</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=Zamorani%2C+G">G. Zamorani</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1706.02317v1-abstract-short" style="display: inline;"> Many cosmological studies predict that early supermassive black holes (SMBHs) can only form in the most massive dark matter halos embedded within large scale structures marked by galaxy over-densities that may extend up to 10 physical Mpc. This scenario, however, has not been confirmed observationally, as the search for galaxy over-densities around high-z quasars has returned conflicting results.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1706.02317v1-abstract-full').style.display = 'inline'; document.getElementById('1706.02317v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1706.02317v1-abstract-full" style="display: none;"> Many cosmological studies predict that early supermassive black holes (SMBHs) can only form in the most massive dark matter halos embedded within large scale structures marked by galaxy over-densities that may extend up to 10 physical Mpc. This scenario, however, has not been confirmed observationally, as the search for galaxy over-densities around high-z quasars has returned conflicting results. The field around the z=6.28 quasar SDSSJ1030+0524 (J1030) is unique for multi-band coverage and represents an excellent data legacy for studying the environment around a primordial SMBH. In this paper we present wide-area (25x25 arcmin), Y- and J-band imaging of the J1030 field obtained with the near infrared camera WIRCam at the Canada-France-Hawaii Telescope (CFHT). We built source catalogues in the Y- and J-band, and matched those with our photometric catalogue in the r, z, i bands presented in Morselli et al. (2014). We used these new infrared data together with H and K and Spitzer/IRAC data to refine our selection of Lyman Break Galaxies (LBGs), extending our selection criteria to galaxies in the range 25.2<zAB<25.7. We selected 21 robust high-z candidates in the J1030 field with photometric redshift around 6 and colors i-z>=1.3. We found a significant asymmetry in the distribution of the high-z galaxies in J1030, supporting the existence of a coherent large-scale structure around the quasar. We compared our results with those of Bowler et al. (2015), who adopted similar LBGs selection criteria, and estimated an over-density of galaxies in the field of delta = 2.4, which is significant at >4 sigma. The over-density value and its significance are higher than those found in Morselli et al. (2014), and we interpret this as evidence of an improved LBG selection. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1706.02317v1-abstract-full').style.display = 'none'; document.getElementById('1706.02317v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 June, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2017. </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, 8 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 606, A23 (2017) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1703.05167">arXiv:1703.05167</a> <span> [<a href="https://arxiv.org/pdf/1703.05167">pdf</a>, <a href="https://arxiv.org/ps/1703.05167">ps</a>, <a href="https://arxiv.org/format/1703.05167">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/mnrasl/slx032">10.1093/mnrasl/slx032 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Detection of faint broad emission lines in type 2 AGN: II. On the measurement of the BH mass of type 2 AGN and the unified model </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Onori%2C+F">F. Onori</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">F. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=La+Franca%2C+F">F. La Franca</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+S">S. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Bongiorno%2C+A">A. Bongiorno</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Fiore%2C+F">F. Fiore</a>, <a href="/search/astro-ph?searchtype=author&query=Maiolino%2C+R">R. Maiolino</a>, <a href="/search/astro-ph?searchtype=author&query=Marconi%2C+A">A. Marconi</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</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="1703.05167v1-abstract-short" style="display: inline;"> We report the virial measurements of the BH mass of a sample of 17 type 2 AGN, drawn from the Swift/BAT 70-month 14-195 keV hard X-ray catalogue, where a faint BLR component has been measured via deep NIR (0.8-2.5 $渭$m) spectroscopy. We compared the type 2 AGN with a control sample of 33 type 1 AGN. We find that the type 2 AGN BH masses span the 5$<$ log(M$_{BH}$ /M$_{\odot}$) $< $7.5 range, with… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.05167v1-abstract-full').style.display = 'inline'; document.getElementById('1703.05167v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1703.05167v1-abstract-full" style="display: none;"> We report the virial measurements of the BH mass of a sample of 17 type 2 AGN, drawn from the Swift/BAT 70-month 14-195 keV hard X-ray catalogue, where a faint BLR component has been measured via deep NIR (0.8-2.5 $渭$m) spectroscopy. We compared the type 2 AGN with a control sample of 33 type 1 AGN. We find that the type 2 AGN BH masses span the 5$<$ log(M$_{BH}$ /M$_{\odot}$) $< $7.5 range, with an average log(M$_{BH}$/M$_{\odot}$) = 6.7, which is $\sim$ 0.8 dex smaller than found for type 1 AGN. If type 1 and type 2 AGN of the same X-ray luminosity log($L_{14-195}$/erg s$^{-1}$) $\sim$ 43.5 are compared, type 2 AGN have 0.5 dex smaller BH masses than type 1 AGN. Although based on few tens of objects, this result disagrees with the standard AGN unification scenarios in which type 1 and type 2 AGN are the same objects observed along different viewing angles with respect to a toroidal absorbing material. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.05167v1-abstract-full').style.display = 'none'; document.getElementById('1703.05167v1-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> 15 March, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2017. </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">6 pages, 5 figures, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1703.00354">arXiv:1703.00354</a> <span> [<a href="https://arxiv.org/pdf/1703.00354">pdf</a>, <a href="https://arxiv.org/ps/1703.00354">ps</a>, <a href="https://arxiv.org/format/1703.00354">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/10.1051/0004-6361/201730447">10.1051/0004-6361/201730447 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Lyman Continuum escape fraction of faint galaxies at z~3.3 in the CANDELS/GOODS-North, EGS, and COSMOS fields with LBC </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Grazian%2C+A">A. Grazian</a>, <a href="/search/astro-ph?searchtype=author&query=Giallongo%2C+E">E. Giallongo</a>, <a href="/search/astro-ph?searchtype=author&query=Paris%2C+D">D. Paris</a>, <a href="/search/astro-ph?searchtype=author&query=Boutsia%2C+K">K. Boutsia</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">M. Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Santini%2C+P">P. Santini</a>, <a href="/search/astro-ph?searchtype=author&query=Windhorst%2C+R+A">R. A. Windhorst</a>, <a href="/search/astro-ph?searchtype=author&query=Jansen%2C+R+A">R. A. Jansen</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+S+H">S. H. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Ashcraft%2C+T+A">T. A. Ashcraft</a>, <a href="/search/astro-ph?searchtype=author&query=Scarlata%2C+C">C. Scarlata</a>, <a href="/search/astro-ph?searchtype=author&query=Rutkowski%2C+M+J">M. J. Rutkowski</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Cusano%2C+F">F. Cusano</a>, <a href="/search/astro-ph?searchtype=author&query=Cristiani%2C+S">S. Cristiani</a>, <a href="/search/astro-ph?searchtype=author&query=Giavalisco%2C+M">M. Giavalisco</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+H+C">H. C. Ferguson</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A">A. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Grogin%2C+N+A">N. A. Grogin</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Fiore%2C+F">F. Fiore</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">A. Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Marchi%2C+F">F. Marchi</a>, <a href="/search/astro-ph?searchtype=author&query=Pedichini%2C+F">F. Pedichini</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">L. Pentericci</a> , et al. (19 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1703.00354v1-abstract-short" style="display: inline;"> The reionization of the Universe is one of the most important topics of present day astrophysical research. The most plausible candidates for the reionization process are star-forming galaxies, which according to the predictions of the majority of the theoretical and semi-analytical models should dominate the HI ionizing background at z~3. We aim at measuring the Lyman continuum escape fraction, w… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.00354v1-abstract-full').style.display = 'inline'; document.getElementById('1703.00354v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1703.00354v1-abstract-full" style="display: none;"> The reionization of the Universe is one of the most important topics of present day astrophysical research. The most plausible candidates for the reionization process are star-forming galaxies, which according to the predictions of the majority of the theoretical and semi-analytical models should dominate the HI ionizing background at z~3. We aim at measuring the Lyman continuum escape fraction, which is one of the key parameters to compute the contribution of star-forming galaxies to the UV background. We have used ultra-deep U-band imaging (U=30.2mag at 1sigma) by LBC/LBT in the CANDELS/GOODS-North field, as well as deep imaging in COSMOS and EGS fields, in order to estimate the Lyman continuum escape fraction of 69 star-forming galaxies with secure spectroscopic redshifts at 3.27<z<3.40 to faint magnitude limits (L=0.2L*, or equivalently M1500~-19). We have measured through stacks a stringent upper limit (<1.7% at 1sigma) for the relative escape fraction of HI ionizing photons from bright galaxies (L>L*), while for the faint population (L=0.2L*) the limit to the escape fraction is ~10%. We have computed the contribution of star-forming galaxies to the observed UV background at z~3 and we have found that it is not enough to keep the Universe ionized at these redshifts, unless their escape fraction increases significantly (>10%) at low luminosities (M1500>-19). We compare our results on the Lyman continuum escape fraction of high-z galaxies with recent estimates in the literature and discuss future prospects to shed light on the end of the Dark Ages. In the future, strong gravitational lensing will be fundamental to measure the Lyman continuum escape fraction down to faint magnitudes (M1500~-16) which are inaccessible with the present instrumentation on blank fields. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.00354v1-abstract-full').style.display = 'none'; document.getElementById('1703.00354v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 March, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A, 16 pages, 6 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 602, A18 (2017) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1612.03728">arXiv:1612.03728</a> <span> [<a href="https://arxiv.org/pdf/1612.03728">pdf</a>, <a href="https://arxiv.org/ps/1612.03728">ps</a>, <a href="https://arxiv.org/format/1612.03728">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/10.1051/0004-6361/201629301">10.1051/0004-6361/201629301 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The WISSH Quasars Project I. Powerful ionised outflows in hyper-luminous quasars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bischetti%2C+M">M. Bischetti</a>, <a href="/search/astro-ph?searchtype=author&query=Piconcelli%2C+E">E. Piconcelli</a>, <a href="/search/astro-ph?searchtype=author&query=Vietri%2C+G">G. Vietri</a>, <a href="/search/astro-ph?searchtype=author&query=Bongiorno%2C+A">A. Bongiorno</a>, <a href="/search/astro-ph?searchtype=author&query=Fiore%2C+F">F. Fiore</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Marconi%2C+A">A. Marconi</a>, <a href="/search/astro-ph?searchtype=author&query=Duras%2C+F">F. Duras</a>, <a href="/search/astro-ph?searchtype=author&query=Zappacosta%2C+L">L. Zappacosta</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Comastri%2C+A">A. Comastri</a>, <a href="/search/astro-ph?searchtype=author&query=Cresci%2C+G">G. Cresci</a>, <a href="/search/astro-ph?searchtype=author&query=Feruglio%2C+C">C. Feruglio</a>, <a href="/search/astro-ph?searchtype=author&query=Giallongo%2C+E">E. Giallongo</a>, <a href="/search/astro-ph?searchtype=author&query=La+Franca%2C+F">F. La Franca</a>, <a href="/search/astro-ph?searchtype=author&query=Mainieri%2C+V">V. Mainieri</a>, <a href="/search/astro-ph?searchtype=author&query=Mannucci%2C+F">F. Mannucci</a>, <a href="/search/astro-ph?searchtype=author&query=Martocchia%2C+S">S. Martocchia</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">F. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Schneider%2C+R">R. Schneider</a>, <a href="/search/astro-ph?searchtype=author&query=Testa%2C+V">V. Testa</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="1612.03728v1-abstract-short" style="display: inline;"> Models and observations suggest that both power and effects of AGN feedback should be maximised in hyper-luminous (L_Bol>10^47 erg/s) quasars, i.e. objects at the brightest end of the AGN luminosity function. We present the first results of a multi-wavelength observing program, focusing on a sample of WISE/SDSS selected hyper-luminous (WISSH) broad-line quasars at z~1.5-5. The WISSH quasars projec… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1612.03728v1-abstract-full').style.display = 'inline'; document.getElementById('1612.03728v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1612.03728v1-abstract-full" style="display: none;"> Models and observations suggest that both power and effects of AGN feedback should be maximised in hyper-luminous (L_Bol>10^47 erg/s) quasars, i.e. objects at the brightest end of the AGN luminosity function. We present the first results of a multi-wavelength observing program, focusing on a sample of WISE/SDSS selected hyper-luminous (WISSH) broad-line quasars at z~1.5-5. The WISSH quasars project has been designed to reveal the most energetic AGN-driven outflows, estimate their occurrence at the peak of quasar activity and extend the study of correlations between outflows and nuclear properties up to poorly-investigated extreme AGN luminosities (L_Bol~10^47 -10^48 erg/s). We present NIR, long-slit LBT/LUCI1 spectroscopy of five WISSH quasars at z~2.3-3.5 showing prominent [OIII] emission lines with broad (FWHM~1200-2200 km/s) and skewed profiles. The luminosities of the broad [OIII] wings are the highest measured so far (L_[OIII]^broad >~5x10^44 erg/s) and reveal the presence of powerful ionised outflows with mass outflow rates Mdot >~1700 M_Sun/yr and kinetic powers Edot >~10^45 erg/s. Although these estimates are affected by large uncertainties, due to the use of [OIII] as tracer of ionized outflows and the very basic outflow model we assume, these results suggest that the AGN is highly efficient in pushing outwards large amounts of ionised gas in our targets. The mechanical outflow luminosities for WISSH quasars correspond to higher fractions (~1-3%) of L_Bol than those derived for lower L_Bol AGN. Our targets host very massive (M_BH>~2x10^9 M_Sun) black holes which are still accreting at a high rate (i.e. a factor of ~0.4-3 of the Eddington limit). These findings demonstrate that WISSH quasars offer the opportunity of probing the extreme end of both luminosity and SMBH mass functions and revealing powerful ionised outflows able to affect the evolution of their host galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1612.03728v1-abstract-full').style.display = 'none'; document.getElementById('1612.03728v1-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 December, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2016. </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, 11 figures, A&A accepted</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 598, A122 (2017) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1610.06243">arXiv:1610.06243</a> <span> [<a href="https://arxiv.org/pdf/1610.06243">pdf</a>, <a href="https://arxiv.org/format/1610.06243">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/stw2368">10.1093/mnras/stw2368 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Detection of faint broad emission lines in type 2 AGN: I. Near infrared observations and spectral fitting </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Onori%2C+F">F. Onori</a>, <a href="/search/astro-ph?searchtype=author&query=La+Franca%2C+F">F. La Franca</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">F. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Maiolino%2C+R">R. Maiolino</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+S">S. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Bongiorno%2C+A">A. Bongiorno</a>, <a href="/search/astro-ph?searchtype=author&query=Fiore%2C+F">F. Fiore</a>, <a href="/search/astro-ph?searchtype=author&query=Marconi%2C+A">A. Marconi</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="1610.06243v1-abstract-short" style="display: inline;"> We present medium resolution near infrared spectroscopic observations of 41 obscured and intermediate class AGN (type 2, 1.9 and 1.8; AGN2) with redshift $z \lesssim$0.1, selected from the Swift/BAT 70-month catalogue. The observations have been carried out in the framework of a systematic study of the AGN2 near infrared spectral properties and have been executed using ISAAC/VLT, X-shooter/VLT and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1610.06243v1-abstract-full').style.display = 'inline'; document.getElementById('1610.06243v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1610.06243v1-abstract-full" style="display: none;"> We present medium resolution near infrared spectroscopic observations of 41 obscured and intermediate class AGN (type 2, 1.9 and 1.8; AGN2) with redshift $z \lesssim$0.1, selected from the Swift/BAT 70-month catalogue. The observations have been carried out in the framework of a systematic study of the AGN2 near infrared spectral properties and have been executed using ISAAC/VLT, X-shooter/VLT and LUCI/LBT, reaching an average S/N ratio of $\sim$30 per resolution element. For those objects observed with X-shooter we also obtained simultaneous optical and UV spectroscopy. We have identified a component from the broad line region in 13 out of 41 AGN2, with FWHM ${\rm > 800 }$ km/s. We have verified that the detection of the broad line region components does not significantly depend on selection effects due to the quality of the spectra, the X-ray or near infrared fluxes, the orientation angle of the host galaxy or the hydrogen column density measured in the X-ray band. The average broad line region components found in AGN2 has a significantly (a factor 2) smaller FWHM if compared with a control sample of type 1 AGN. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1610.06243v1-abstract-full').style.display = 'none'; document.getElementById('1610.06243v1-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 October, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2016. </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 in press; published on MNRAS Advance Access, issue September 16, 2016</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1608.02210">arXiv:1608.02210</a> <span> [<a href="https://arxiv.org/pdf/1608.02210">pdf</a>, <a href="https://arxiv.org/format/1608.02210">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/10.3847/2041-8205/829/1/L7">10.3847/2041-8205/829/1/L7 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> High-Velocity Bipolar Molecular Emission from an AGN Torus </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gallimore%2C+J+F">Jack F. Gallimore</a>, <a href="/search/astro-ph?searchtype=author&query=Elitzur%2C+M">Moshe Elitzur</a>, <a href="/search/astro-ph?searchtype=author&query=Maiolino%2C+R">Roberto Maiolino</a>, <a href="/search/astro-ph?searchtype=author&query=Marconi%2C+A">Alessandro Marconi</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Dea%2C+C+P">Christopher P. O'Dea</a>, <a href="/search/astro-ph?searchtype=author&query=Lutz%2C+D">Dieter Lutz</a>, <a href="/search/astro-ph?searchtype=author&query=Baum%2C+S+A">Stefi A. Baum</a>, <a href="/search/astro-ph?searchtype=author&query=Nikutta%2C+R">Robert Nikutta</a>, <a href="/search/astro-ph?searchtype=author&query=Impellizzeri%2C+C+M+V">C. M. V. Impellizzeri</a>, <a href="/search/astro-ph?searchtype=author&query=Davies%2C+R">Richard Davies</a>, <a href="/search/astro-ph?searchtype=author&query=Kimball%2C+A+E">Amy E. Kimball</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">Eleonora Sani</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="1608.02210v1-abstract-short" style="display: inline;"> We have detected in ALMA observations CO J = 6 - 5 emission from the nucleus of the Seyfert galaxy NGC 1068. The low-velocity (up to +/- 70 km/s relative to systemic) CO emission resolves into a 12x7 pc structure, roughly aligned with the nuclear radio source. Higher-velocity emission (up to +/- 400 km/s) is consistent with a bipolar outflow in a direction nearly perpendicular (roughly 80 degrees)… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1608.02210v1-abstract-full').style.display = 'inline'; document.getElementById('1608.02210v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1608.02210v1-abstract-full" style="display: none;"> We have detected in ALMA observations CO J = 6 - 5 emission from the nucleus of the Seyfert galaxy NGC 1068. The low-velocity (up to +/- 70 km/s relative to systemic) CO emission resolves into a 12x7 pc structure, roughly aligned with the nuclear radio source. Higher-velocity emission (up to +/- 400 km/s) is consistent with a bipolar outflow in a direction nearly perpendicular (roughly 80 degrees) to the nuclear disk. The position-velocity diagram shows that in addition to the outflow, the velocity field may also contain rotation about the disk axis. These observations provide compelling evidence in support of the disk-wind scenario for the AGN obscuring torus. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1608.02210v1-abstract-full').style.display = 'none'; document.getElementById('1608.02210v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 August, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in the Astrophysical Journal Letters. 6 pages, 3 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/1605.06253">arXiv:1605.06253</a> <span> [<a href="https://arxiv.org/pdf/1605.06253">pdf</a>, <a href="https://arxiv.org/format/1605.06253">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/10.3389/fspas.2016.00012">10.3389/fspas.2016.00012 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Detection of Faint BLR Components in the Starburst/Seyfert Galaxy NGC 6221 and Measure of the Central BH Mass </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=La+Franca%2C+F">Fabio La Franca</a>, <a href="/search/astro-ph?searchtype=author&query=Onori%2C+F">Francesca Onori</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">Federica Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+S">Stefano Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Marconi%2C+A">Alessandro Marconi</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">Eleonora Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Vignali%2C+C">Cristian 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="1605.06253v1-abstract-short" style="display: inline;"> In the last decade, using single epoch virial based techniques in the optical band, it has been possible to measure the central black hole mass on large AGN1 samples. However these measurements use the width of the broad line region as a proxy of the virial velocities and are therefore difficult to be carried out on those obscured (type 2) or low luminosity AGN where the nuclear component does not… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.06253v1-abstract-full').style.display = 'inline'; document.getElementById('1605.06253v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1605.06253v1-abstract-full" style="display: none;"> In the last decade, using single epoch virial based techniques in the optical band, it has been possible to measure the central black hole mass on large AGN1 samples. However these measurements use the width of the broad line region as a proxy of the virial velocities and are therefore difficult to be carried out on those obscured (type 2) or low luminosity AGN where the nuclear component does not dominate in the optical. Here we present the optical and near infrared spectrum of the starburst/Seyfert galaxy NGC 6221, observed with X-shooter/VLT. Previous observations of NGC 6221 in the X-ray band show an absorbed (N_H=8.5 +/- 0.4 x 10^21 cm^-2) spectrum typical of a type 2 AGN with luminosity log(L_14-195 keV) = 42.05 erg/s, while in the optical band its spectrum is typical of a reddened (A_V=3) starburst. Our deep X-shooter/VLT observations have allowed us to detect faint broad emission in the H_alpha, HeI and Pa_beta lines (FWHM ~1400-2300 km/s) confirming previous studies indicating that NGC 6221 is a reddened starburst galaxy which hosts an AGN. We use the measure of the broad components to provide a first estimate of its central black hole mass (M_BH = 10^(6.6 +/- 0.3) Msol, lambda_Edd=0.01-0.03), obtained using recently calibrated virial relations suitable for moderately obscured (N_H<10^24 cm^-2) AGN. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.06253v1-abstract-full').style.display = 'none'; document.getElementById('1605.06253v1-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 May, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2016. </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. Published in Frontiers in Astronomy and Space Sciences</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Front. Astron. Space Sci. 3:12 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1511.07437">arXiv:1511.07437</a> <span> [<a href="https://arxiv.org/pdf/1511.07437">pdf</a>, <a href="https://arxiv.org/format/1511.07437">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/10.3847/0004-637X/817/1/21">10.3847/0004-637X/817/1/21 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Supermassive black holes and their host spheroids II. The red and blue sequence in the $M_{\rm BH} - M_{\rm *,sph}$ diagram </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Savorgnan%2C+G+A+D">Giulia A. D. Savorgnan</a>, <a href="/search/astro-ph?searchtype=author&query=Graham%2C+A+W">Alister W. Graham</a>, <a href="/search/astro-ph?searchtype=author&query=Marconi%2C+A">Alessandro Marconi</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">Eleonora Sani</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="1511.07437v1-abstract-short" style="display: inline;"> In our first paper, we performed a detailed (i.e. bulge, disks, bars, spiral arms, rings, halo, nucleus, etc.) decomposition of 66 galaxies, with directly measured black hole masses, $M_{BH}$, that had been imaged at $3.6~渭m$ with Spitzer. Our sample is the largest to date and, for the first time, the decompositions were checked for consistency with the galaxy kinematics. We present correlations b… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.07437v1-abstract-full').style.display = 'inline'; document.getElementById('1511.07437v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1511.07437v1-abstract-full" style="display: none;"> In our first paper, we performed a detailed (i.e. bulge, disks, bars, spiral arms, rings, halo, nucleus, etc.) decomposition of 66 galaxies, with directly measured black hole masses, $M_{BH}$, that had been imaged at $3.6~渭m$ with Spitzer. Our sample is the largest to date and, for the first time, the decompositions were checked for consistency with the galaxy kinematics. We present correlations between $M_{ BH}$ and the host spheroid (and galaxy) luminosity, $L_{sph}$ (and $L_{gal}$), and also stellar mass, $M_{*,sph}$. While most previous studies have used galaxy samples that were overwhelmingly dominated by high-mass, early-type galaxies, our sample includes 17 spiral galaxies, half of which have $M_{BH} < 10^7~M_\odot$, and allows us to better investigate the poorly studied low-mass end of the $M_{BH} - M_{*,sph}$ correlation. The bulges of early-type galaxies follow $M_{BH} \propto M_{*,sph}^{1.04 \pm 0.10}$ and define a tight red sequence with intrinsic scatter $蔚= 0.43 \pm 0.06~dex$ and a median $M_{BH}/M_{*,sph}$ ratio of $0.68 \pm 0.04\%$, i.e.~a $\pm 2蟽$ range of 0.1-5%. At the low-mass end, the bulges of late-type galaxies define a much steeper blue sequence, with $M_{BH} \propto M_{*,sph}^{2-3}$, indicating that gas-rich processes feed the black hole more efficiently than the host bulge as they coevolve. We additionally report that: i) our Sersic galaxy sample follows a less steep sequence than previously reported; ii) bulges with Sersic index $n<2$, argued by some to be pseudo-bulges, are not offset to lower $M_{BH}$ from the correlation defined by the current bulge sample with $n>2$; and iii) $L_{sph}$ and $L_{gal}$ correlate equally well with $M_{BH}$, in terms of intrinsic scatter, only for early-type galaxies - once reasonable numbers of spiral galaxies are included, the correlation with $L_{ sph}$ is better than that with $L_{gal}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.07437v1-abstract-full').style.display = 'none'; document.getElementById('1511.07437v1-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 November, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">To appear 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/1508.04464">arXiv:1508.04464</a> <span> [<a href="https://arxiv.org/pdf/1508.04464">pdf</a>, <a href="https://arxiv.org/format/1508.04464">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/10.1051/0004-6361/201526581">10.1051/0004-6361/201526581 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MAGNUM survey: Positive feedback in the nuclear region of NGC 5643 suggested by MUSE </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cresci%2C+G">G. Cresci</a>, <a href="/search/astro-ph?searchtype=author&query=Marconi%2C+A">A. Marconi</a>, <a href="/search/astro-ph?searchtype=author&query=Zibetti%2C+S">S. Zibetti</a>, <a href="/search/astro-ph?searchtype=author&query=Risaliti%2C+G">G. Risaliti</a>, <a href="/search/astro-ph?searchtype=author&query=Carniani%2C+S">S. Carniani</a>, <a href="/search/astro-ph?searchtype=author&query=Mannucci%2C+F">F. Mannucci</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">A. Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Maiolino%2C+R">R. Maiolino</a>, <a href="/search/astro-ph?searchtype=author&query=Balmaverde%2C+B">B. Balmaverde</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Capetti%2C+A">A. Capetti</a>, <a href="/search/astro-ph?searchtype=author&query=Cicone%2C+C">C. Cicone</a>, <a href="/search/astro-ph?searchtype=author&query=Feruglio%2C+C">C. Feruglio</a>, <a href="/search/astro-ph?searchtype=author&query=Bland-Hawthorn%2C+J">J. Bland-Hawthorn</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=Salvato%2C+M">M. Salvato</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Tozzi%2C+P">P. Tozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Urrutia%2C+T">T. Urrutia</a>, <a href="/search/astro-ph?searchtype=author&query=Venturi%2C+G">G. Venturi</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1508.04464v1-abstract-short" style="display: inline;"> We study the ionization and kinematics of the ionized gas in the nuclear region of the barred Seyfert 2 galaxy NGC~5643 using MUSE integral field observations in the framework of the MAGNUM (Measuring Active Galactic Nuclei Under MUSE Microscope) survey. The data were used to identify regions with different ionization conditions and to map the gas density and the dust extinction. We find evidence… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1508.04464v1-abstract-full').style.display = 'inline'; document.getElementById('1508.04464v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1508.04464v1-abstract-full" style="display: none;"> We study the ionization and kinematics of the ionized gas in the nuclear region of the barred Seyfert 2 galaxy NGC~5643 using MUSE integral field observations in the framework of the MAGNUM (Measuring Active Galactic Nuclei Under MUSE Microscope) survey. The data were used to identify regions with different ionization conditions and to map the gas density and the dust extinction. We find evidence for a double sided ionization cone, possibly collimated by a dusty structure surrounding the nucleus. At the center of the ionization cone, outflowing ionized gas is revealed as a blueshifted, asymmetric wing of the [OIII] emission line, up to projected velocity v(10)~-450 km/s. The outflow is also seen as a diffuse, low luminosity radio and X-ray jet, with similar extension. The outflowing material points in the direction of two clumps characterized by prominent line emission with spectra typical of HII regions, located at the edge of the dust lane of the bar. We propose that the star formation in the clumps is due to `positive feedback' induced by gas compression by the nuclear outflow, providing the first candidate for outflow induced star formation in a Seyfert-like radio quiet AGN. This suggests that positive feedback may be a relevant mechanism in shaping the black hole-host galaxy coevolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1508.04464v1-abstract-full').style.display = 'none'; document.getElementById('1508.04464v1-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 August, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">9 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 582, A63 (2015) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1505.03538">arXiv:1505.03538</a> <span> [<a href="https://arxiv.org/pdf/1505.03538">pdf</a>, <a href="https://arxiv.org/ps/1505.03538">ps</a>, <a href="https://arxiv.org/format/1505.03538">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"> Variable stars and stellar populations in Andromeda XXI: II. Another merged galaxy satellite of M31? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cusano%2C+F">F. Cusano</a>, <a href="/search/astro-ph?searchtype=author&query=Garofalo%2C+A">A. Garofalo</a>, <a href="/search/astro-ph?searchtype=author&query=Clementini%2C+G">G. Clementini</a>, <a href="/search/astro-ph?searchtype=author&query=Cignoni%2C+M">M. Cignoni</a>, <a href="/search/astro-ph?searchtype=author&query=Federici%2C+L">L. Federici</a>, <a href="/search/astro-ph?searchtype=author&query=Marconi%2C+M">M. Marconi</a>, <a href="/search/astro-ph?searchtype=author&query=Musella%2C+I">I. Musella</a>, <a href="/search/astro-ph?searchtype=author&query=Ripepi%2C+V">V. Ripepi</a>, <a href="/search/astro-ph?searchtype=author&query=Speziali%2C+R">R. Speziali</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Merighi%2C+R">R. Merighi</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="1505.03538v1-abstract-short" style="display: inline;"> B and V time-series photometry of the M31 dwarf spheroidal satellite Andromeda XXI (And XXI) was obtained with the Large Binocular Cameras at the Large Binocular Telescope. We have identified 50 variables in And XXI, of which 41 are RR Lyrae stars (37 fundamental-mode RRab, and 4 first-overtone RRc, pulsators) and 9 are Anomalous Cepheids (ACs). The average period of the RRab stars (<Pab> = 0.64 d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1505.03538v1-abstract-full').style.display = 'inline'; document.getElementById('1505.03538v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1505.03538v1-abstract-full" style="display: none;"> B and V time-series photometry of the M31 dwarf spheroidal satellite Andromeda XXI (And XXI) was obtained with the Large Binocular Cameras at the Large Binocular Telescope. We have identified 50 variables in And XXI, of which 41 are RR Lyrae stars (37 fundamental-mode RRab, and 4 first-overtone RRc, pulsators) and 9 are Anomalous Cepheids (ACs). The average period of the RRab stars (<Pab> = 0.64 days) and the period-amplitude diagram place And~XXI in the class of Oosterhoff II - Oosterhoff-Intermediate objects. From the average luminosity of the RR Lyrae stars we derived the galaxy distance modulus of (m-M)$_0$=$24.40\pm0.17$ mag, which is smaller than previous literature estimates, although still consistent with them within 1 $蟽$. The galaxy color-magnitude diagram shows evidence for the presence of three different stellar generations in And~XXI: 1) an old ($\sim$ 12 Gyr) and metal poor ([Fe/H]=$-$1.7 dex) component traced by the RR Lyrae stars; 2) a slightly younger (10-6 Gyr) and more metal rich ([Fe/H]=$-$1.5 dex) component populating the red horizontal branch, and 3) a young age ($\sim$ 1 Gyr) component with same metallicity, that produced the ACs. Finally, we provide hints that And~XXI could be the result of a minor merging event between two dwarf galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1505.03538v1-abstract-full').style.display = 'none'; document.getElementById('1505.03538v1-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 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">accepted for publications 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/1504.07068">arXiv:1504.07068</a> <span> [<a href="https://arxiv.org/pdf/1504.07068">pdf</a>, <a href="https://arxiv.org/ps/1504.07068">ps</a>, <a href="https://arxiv.org/format/1504.07068">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"> WISE colours and star-formation in the host galaxies of radio-loud narrow-line Seyfert 1 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Caccianiga%2C+A">A. Caccianiga</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+S">S. Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Ballo%2C+L">L. Ballo</a>, <a href="/search/astro-ph?searchtype=author&query=Foschini%2C+L">L. Foschini</a>, <a href="/search/astro-ph?searchtype=author&query=Maccacaro%2C+T">T. Maccacaro</a>, <a href="/search/astro-ph?searchtype=author&query=Della+Ceca%2C+R">R. Della Ceca</a>, <a href="/search/astro-ph?searchtype=author&query=Severgnini%2C+P">P. Severgnini</a>, <a href="/search/astro-ph?searchtype=author&query=Marcha%2C+M+J">M. J. Marcha</a>, <a href="/search/astro-ph?searchtype=author&query=Mateos%2C+S">S. Mateos</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</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="1504.07068v1-abstract-short" style="display: inline;"> We investigate the mid-infrared properties of the largest (42 objects) sample of radio-loud narrow-line Seyfert 1 (RL NLS1) collected to date, using data from the Wide-field Infrared Survey Explorer (WISE). We analyse the mid-IR colours of these objects and compare them to what is expected from different combinations of AGN and galaxy templates. We find that, in general, the host-galaxy emission g… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1504.07068v1-abstract-full').style.display = 'inline'; document.getElementById('1504.07068v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1504.07068v1-abstract-full" style="display: none;"> We investigate the mid-infrared properties of the largest (42 objects) sample of radio-loud narrow-line Seyfert 1 (RL NLS1) collected to date, using data from the Wide-field Infrared Survey Explorer (WISE). We analyse the mid-IR colours of these objects and compare them to what is expected from different combinations of AGN and galaxy templates. We find that, in general, the host-galaxy emission gives an importan contribution to the observed mid-IR flux in particular at the longest wavelengths (W3, at 12micron, and W4, at 22micron). In about half of the sources (22 objects) we observe a very red mid-IR colour (W4-W3>2.5) that can be explained only using a starburst galaxy template (M82). Using the 22micron luminosities, corrected for the AGN contribution, we have then estimated the star-formation rate for 20 of these "red" RL NLS1, finding values ranging from 10 to 500 Msun/y. For the RL NLS1 showing bluer colours, instead, we cannot exclude the presence of a star-forming host galaxy although, on average, we expect a lower star-formation rate. Studying the radio (1.4GHz) to mid-IR (22micron) flux ratios of the RL NLS1 in the sample we found that in ~10 objects the star-forming activity could represent the most important component also at radio frequencies, in addition (or in alternative) to the relativistic jet. We conclude that both the mid-IR and the radio emission of RL NLS1 are a mixture of different components, including the relativistic jet, the dusty torus and an intense star-forming activity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1504.07068v1-abstract-full').style.display = 'none'; document.getElementById('1504.07068v1-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 April, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">Accepted for publication in MNRAS, 11 pages, 7 figures, 2 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/1502.07234">arXiv:1502.07234</a> <span> [<a href="https://arxiv.org/pdf/1502.07234">pdf</a>, <a href="https://arxiv.org/format/1502.07234">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/stv368">10.1093/mnras/stv368 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Extending Virial Black Hole Mass Estimates to Low-Luminosity or Obscured AGN: the cases of NGC 4395 and MCG -01-24-012 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=La+Franca%2C+F">Fabio La Franca</a>, <a href="/search/astro-ph?searchtype=author&query=Onori%2C+F">Francesca Onori</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">Federica Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">Eleonora Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">Marcella Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Maiolino%2C+R">Roberto Maiolino</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+S">Stefano Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Bongiorno%2C+A">Angela Bongiorno</a>, <a href="/search/astro-ph?searchtype=author&query=Fiore%2C+F">Fabrizio Fiore</a>, <a href="/search/astro-ph?searchtype=author&query=Marconi%2C+A">Alessandro Marconi</a>, <a href="/search/astro-ph?searchtype=author&query=Vignali%2C+C">Cristian 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="1502.07234v2-abstract-short" style="display: inline;"> In the last decade, using single epoch (SE) virial based spectroscopic optical observations, it has been possible to measure the black hole (BH) mass on large type 1 Active Galactic Nuclei (AGN) samples. However this kind of measurements can not be applied on those obscured type 2 and/or low luminosity AGN where the nuclear component does not dominate in the optical. We have derived new SE relatio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1502.07234v2-abstract-full').style.display = 'inline'; document.getElementById('1502.07234v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1502.07234v2-abstract-full" style="display: none;"> In the last decade, using single epoch (SE) virial based spectroscopic optical observations, it has been possible to measure the black hole (BH) mass on large type 1 Active Galactic Nuclei (AGN) samples. However this kind of measurements can not be applied on those obscured type 2 and/or low luminosity AGN where the nuclear component does not dominate in the optical. We have derived new SE relationships, based on the FWHM and luminosity of the broad line region component of the Pabeta emission line and/or the hard X-ray luminosity in the 14-195 keV band, which have the prospect of better working with low luminosity or obscured AGN. The SE relationships have been calibrated in the 10^5-10^9 M_sol mass range, using a sample of AGN whose BH masses have been previously measured using reverberation mapping techniques. Our tightest relationship between the reverberation-based BH mass and the SE virial product has an intrinsic spread of 0.20 dex. Thanks to these SE relations, in agreement with previous estimates, we have measured a BH mass of M_BH =1.7^+1.3_-0.7 X 10^5 M_sol for the low luminosity, type 1, AGN NGC 4395 (one of the smallest active galactic BH known). We also measured, for the first time, a BH mass of M_BH = 1.5^+1.1_-0.6 X 10^7 M_sol for the Seyfert 2 galaxy MCG -01-24-012. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1502.07234v2-abstract-full').style.display = 'none'; document.getElementById('1502.07234v2-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 February, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 February, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">10 pages, 7 figures. Accepted by MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1412.5857">arXiv:1412.5857</a> <span> [<a href="https://arxiv.org/pdf/1412.5857">pdf</a>, <a href="https://arxiv.org/format/1412.5857">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/10.1051/0004-6361/201425262">10.1051/0004-6361/201425262 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The StEllar Counterparts of COmpact high velocity clouds (SECCO) survey. I. Photos of ghosts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bellazzini%2C+M">M. Bellazzini</a>, <a href="/search/astro-ph?searchtype=author&query=Beccari%2C+G">G. Beccari</a>, <a href="/search/astro-ph?searchtype=author&query=Battaglia%2C+G">G. Battaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+N">N. Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Testa%2C+V">V. Testa</a>, <a href="/search/astro-ph?searchtype=author&query=Ibata%2C+R">R. Ibata</a>, <a href="/search/astro-ph?searchtype=author&query=Correnti%2C+M">M. Correnti</a>, <a href="/search/astro-ph?searchtype=author&query=Cusano%2C+F">F. Cusano</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</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="1412.5857v2-abstract-short" style="display: inline;"> We present an imaging survey aimed at searching for the stellar counterparts of recently discovered ultra-compact high-velocity HI clouds (UCHVC). Adams et al. (2013) proposed these clouds to be candidate mini-haloes in the Local Group and/or its surroundings, within a distance range of 0.25-2.0 Mpc. Using the Large Binocular Telescope we obtain wide-field (~ 23' X 23') g- and r-band images of the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1412.5857v2-abstract-full').style.display = 'inline'; document.getElementById('1412.5857v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1412.5857v2-abstract-full" style="display: none;"> We present an imaging survey aimed at searching for the stellar counterparts of recently discovered ultra-compact high-velocity HI clouds (UCHVC). Adams et al. (2013) proposed these clouds to be candidate mini-haloes in the Local Group and/or its surroundings, within a distance range of 0.25-2.0 Mpc. Using the Large Binocular Telescope we obtain wide-field (~ 23' X 23') g- and r-band images of the twenty-five most promising and most compact clouds among the fifty-nine identified by Adams et al. Careful visual inspection of all the images does not reveal any stellar counterpart even slightly resembling LeoP, the only local dwarf galaxy that was found as a counterpart to a previously detected high velocity cloud. Only a possible distant (D>3.0 Mpc) counterpart to HVC274.68+74.70-123 has been identified on our images. The point source photometry in the central 17.3' X 7.7' chips reaches r<= 26.5, and is expected to contain most of the stellar counterparts to the UCHVCs. However, no obvious stellar over-density is detected in any of our fields, in marked contrast to our comparison LeoP field in which the dwarf galaxy is detected at a >30 sigma significance level. Only HVC352.45+59.06+263 may be associated with a weak over-density, whose nature cannot be ascertained with our data. Sensitivity tests shows that our survey would have detected any dwarf galaxy dominated by an old stellar population, with an integrated absolute magnitude M_V<= -8.0, a half-light radius r_h<= 300 pc, and lying within 1.5 Mpc from us, thereby confirming that it is unlikely that the observed UCHVCs are associated with stellar counterparts typical of known Local Group dwarf galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1412.5857v2-abstract-full').style.display = 'none'; document.getElementById('1412.5857v2-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 January, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 December, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication by A&A. PdfLaTex. 24 pages, 27 figures. Minor changes; A&A language editing</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1408.5753">arXiv:1408.5753</a> <span> [<a href="https://arxiv.org/pdf/1408.5753">pdf</a>, <a href="https://arxiv.org/format/1408.5753">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/10.1051/0004-6361/201423792">10.1051/0004-6361/201423792 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A bag of tricks: Using proper motions of Galactic stars to identify the Hercules ultra-faint dwarf galaxy members </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Fabrizio%2C+M">M. Fabrizio</a>, <a href="/search/astro-ph?searchtype=author&query=Raimondo%2C+G">G. Raimondo</a>, <a href="/search/astro-ph?searchtype=author&query=Brocato%2C+E">E. Brocato</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+A">A. Bellini</a>, <a href="/search/astro-ph?searchtype=author&query=Libralato%2C+M">M. Libralato</a>, <a href="/search/astro-ph?searchtype=author&query=Testa%2C+V">V. Testa</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">M. Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Musella%2C+I">I. Musella</a>, <a href="/search/astro-ph?searchtype=author&query=Clementini%2C+G">G. Clementini</a>, <a href="/search/astro-ph?searchtype=author&query=Carini%2C+R">R. Carini</a>, <a href="/search/astro-ph?searchtype=author&query=Marconi%2C+M">M. Marconi</a>, <a href="/search/astro-ph?searchtype=author&query=Piotto%2C+G">G. Piotto</a>, <a href="/search/astro-ph?searchtype=author&query=Ripepi%2C+V">V. Ripepi</a>, <a href="/search/astro-ph?searchtype=author&query=Buonanno%2C+R">R. Buonanno</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Speziali%2C+R">R. Speziali</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="1408.5753v2-abstract-short" style="display: inline;"> Hercules is the prototype of the ultra-faint dwarf (UFD) galaxies. To date, there are still no firm constraints on its total luminosity, due to the difficulty of disentangling Hercules bona-fide stars from the severe Galactic field contamination. In order to better constrain Hercules properties we aim at removing foreground and background contaminants in the galaxy field using the proper motions o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1408.5753v2-abstract-full').style.display = 'inline'; document.getElementById('1408.5753v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1408.5753v2-abstract-full" style="display: none;"> Hercules is the prototype of the ultra-faint dwarf (UFD) galaxies. To date, there are still no firm constraints on its total luminosity, due to the difficulty of disentangling Hercules bona-fide stars from the severe Galactic field contamination. In order to better constrain Hercules properties we aim at removing foreground and background contaminants in the galaxy field using the proper motions of the Milky Way stars and the colour-colour diagram. We have obtained images of Hercules in the rSloan, BBessel and Uspec bands with the Large Binocular Telescope (LBT) and LBC-BIN mode capabilities. The rSloan new data-set combined with data from the LBT archive span a time baseline of about 5 yr, allowing us to measure for the first time proper motions of stars in the Hercules direction. The Uspec data along with existing LBT photometry allowed us to use colour-colour diagram to further remove the field contamination. Thanks to a highly-accurate procedure to derive the rSloan-filter geometric distortion solution for the LBC-red, we were able to measure stellar relative proper motions to a precision of better than 5 mas yr^-1 down to rSloan=22 mag and disentangle a significant fraction (\>90\%) of Milky Way contaminants. We ended up with a sample of 528 sources distributed over a large portion of the galaxy body (0.12 deg^2). Of these sources, 171 turned out to be background galaxies and additional foreground stars, from the analysis of the Uspec - BBessel vs. BBessel - rSloan colour-colour diagram. This leaves us with a sample of 357 likely members of the Hercules UFD. We compared the cleaned colour-magnitude diagram (CMD) with evolutionary models and synthetic CMDs, confirming the presence in Hercules of an old population (t=12\pm 2 Gyr), with a wide spread in metallicity (-3.3\<[Fe/H]\<-1.8). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1408.5753v2-abstract-full').style.display = 'none'; document.getElementById('1408.5753v2-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 September, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 August, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2014. </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, 15 figures, 3 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 570, A61 (2014) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1406.3961">arXiv:1406.3961</a> <span> [<a href="https://arxiv.org/pdf/1406.3961">pdf</a>, <a href="https://arxiv.org/format/1406.3961">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/10.1051/0004-6361/201423853">10.1051/0004-6361/201423853 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The primordial environment of super massive black holes: large scale galaxy overdensities around $z\sim6$ QSOs with LBT </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Morselli%2C+L">L. Morselli</a>, <a href="/search/astro-ph?searchtype=author&query=Mignoli%2C+M">M. Mignoli</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=Comastri%2C+A">A. Comastri</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Cappelluti%2C+N">N. Cappelluti</a>, <a href="/search/astro-ph?searchtype=author&query=Zamorani%2C+G">G. Zamorani</a>, <a href="/search/astro-ph?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/astro-ph?searchtype=author&query=Gallozzi%2C+S">S. Gallozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</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="1406.3961v1-abstract-short" style="display: inline;"> We investigated the presence of galaxy overdensities around four $z\sim6$ QSOs, namely SDSS J1030+0524 (z = 6.28), SDSS J1148+5251 (z = 6.41), SDSS J1048+4637 (z = 6.20) and SDSS J1411+1217 (z = 5.95), through deep $r$-, $i$- and $z$- band imaging obtained with the wide-field ($\sim23'\times25'$) Large Binocular Camera (LBC) at the Large Binocular Telescope (LBT). We adopted color-color selections… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1406.3961v1-abstract-full').style.display = 'inline'; document.getElementById('1406.3961v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1406.3961v1-abstract-full" style="display: none;"> We investigated the presence of galaxy overdensities around four $z\sim6$ QSOs, namely SDSS J1030+0524 (z = 6.28), SDSS J1148+5251 (z = 6.41), SDSS J1048+4637 (z = 6.20) and SDSS J1411+1217 (z = 5.95), through deep $r$-, $i$- and $z$- band imaging obtained with the wide-field ($\sim23'\times25'$) Large Binocular Camera (LBC) at the Large Binocular Telescope (LBT). We adopted color-color selections within the $i-z$ vs $r-z$ plane to identify samples of $i$-band dropouts at the QSO redshift and measure their relative abundance and spatial distribution in the four LBC fields, each covering $\sim8\times8$ physical Mpc at $z\sim6$. The same selection criteria were then applied to $z$-band selected sources in the $\sim$1 deg$^2$ Subaru-XMM Newton Deep Survey to derive the expected number of dropouts over a blank LBC-sized field ($\sim$0.14 deg$^2$). The four observed QSO fields host a number of candidates larger than what is expected in a blank field. By defining as $i$-band dropouts objects with $z_{AB}<25$, $i-z>1.4$ and undetected in the $r$-band, we found 16, 10, 9, 12 dropouts in SDSS J1030+0524, SDSS J1148+5251, SDSS J1048+4637, and SDSS J1411+1217, respectively, whereas only 4.3 such objects are expected over a 0.14 deg$^2$ blank field. This corresponds to overdensity significances of 3.3, 1.9, 1.7, 2.5$蟽$, respectively. By considering the total number of dropouts in the four LBC fields and comparing it with what is expected in four blank fields of 0.14 deg$^2$ each, we find that high-z QSOs reside in overdense environments at the $3.7蟽$ level. This is the first direct and unambiguous measurement of the large scale structures around $z\sim6$ QSOs. [shortened] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1406.3961v1-abstract-full').style.display = 'none'; document.getElementById('1406.3961v1-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 June, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2014. </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, 8 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 568, A1 (2014) </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Sani%2C+E&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Sani%2C+E&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Sani%2C+E&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> </ul> </nav> <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> 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