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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=Gobat%2C+R&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Gobat%2C+R&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Gobat%2C+R&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Gobat%2C+R&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </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/2412.09363">arXiv:2412.09363</a> <span> [<a href="https://arxiv.org/pdf/2412.09363">pdf</a>, <a href="https://arxiv.org/format/2412.09363">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"> Behind the dust veil: A panchromatic view of an optically dark galaxy at z=4.82 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sillassen%2C+N+B">Nikolaj B. Sillassen</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+S">Shuowen Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Magdis%2C+G+E">Georgios E. Magdis</a>, <a href="/search/astro-ph?searchtype=author&query=Hodge%2C+J">Jacqueline Hodge</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">Raphael Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">Emanuele Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Knudsen%2C+K">Kirsten Knudsen</a>, <a href="/search/astro-ph?searchtype=author&query=Finoguenov%2C+A">Alexis Finoguenov</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+W">Wei-Hao Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Gao%2C+Z">Zhen-Kai Gao</a>, <a href="/search/astro-ph?searchtype=author&query=Weaver%2C+J+R">John R. Weaver</a>, <a href="/search/astro-ph?searchtype=author&query=Algera%2C+H">Hiddo Algera</a>, <a href="/search/astro-ph?searchtype=author&query=Andika%2C+I+T">Irham T. Andika</a>, <a href="/search/astro-ph?searchtype=author&query=Brinch%2C+M">Malte Brinch</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+C">Chian-Chou Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Cochrane%2C+R">Rachel Cochrane</a>, <a href="/search/astro-ph?searchtype=author&query=Enia%2C+A">Andrea Enia</a>, <a href="/search/astro-ph?searchtype=author&query=Faisst%2C+A">Andreas Faisst</a>, <a href="/search/astro-ph?searchtype=author&query=Gillman%2C+S">Steven Gillman</a>, <a href="/search/astro-ph?searchtype=author&query=Gomez-Guijarro%2C+C">Carlos Gomez-Guijarro</a>, <a href="/search/astro-ph?searchtype=author&query=Gozaliasl%2C+G">Ghassem Gozaliasl</a>, <a href="/search/astro-ph?searchtype=author&query=Hayward%2C+C">Chris Hayward</a>, <a href="/search/astro-ph?searchtype=author&query=Kokorev%2C+V">Vasily Kokorev</a>, <a href="/search/astro-ph?searchtype=author&query=Merchant%2C+M">Maya Merchant</a> , et al. (8 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2412.09363v1-abstract-short" style="display: inline;"> Optically dark dusty star-forming galaxies (DSFGs) play an essential role in massive galaxy formation at early cosmic time, however their nature remains elusive. Here we present a detailed case study of all the baryonic components of a $z=4.821$ DSFG, XS55. Selected from the ultra-deep COSMOS-XS 3GHz map with a red SCUBA-2 450$渭$m/850$渭$m colour, XS55 was followed up with ALMA 3mm line scans and s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.09363v1-abstract-full').style.display = 'inline'; document.getElementById('2412.09363v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.09363v1-abstract-full" style="display: none;"> Optically dark dusty star-forming galaxies (DSFGs) play an essential role in massive galaxy formation at early cosmic time, however their nature remains elusive. Here we present a detailed case study of all the baryonic components of a $z=4.821$ DSFG, XS55. Selected from the ultra-deep COSMOS-XS 3GHz map with a red SCUBA-2 450$渭$m/850$渭$m colour, XS55 was followed up with ALMA 3mm line scans and spectroscopically confirmed to be at $z=4.821$ via detections of the CO(5-4) and [CI](1-0) lines. JWST/NIRCam imaging reveals that XS55 is a F150W-dropout with red F277W/F444W colour, and a complex morphology: a compact central component embedded in an extended structure with a likely companion. XS55 is tentatively detected in X-rays with both Chandra and XMM-Newton, suggesting an active galactic nucleus (AGN) nature. By fitting a panchromatic SED spanning NIR to radio wavelengths, we revealed that XS55 is a massive main-sequence galaxy with a stellar mass of $M_\ast=(5\pm1)\times10^{10}\,{\rm M_\odot}$ and a star formation rate of ${\rm SFR}=540\pm177~{\rm M_\odot\,yr^{-1}}$. The dust of XS55 is optically thick in the far infrared (FIR) with a surprisingly cold dust temperature of $T_{\rm dust}=33\pm2\,{\rm K}$, making XS55 one of the coldest DSFGs at $z>4$ known to date. This work unveils the nature of a radio-selected F150W-dropout, suggesting the existence of a population of DSFGs hosting active black holes embedded in optically thick dust. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.09363v1-abstract-full').style.display = 'none'; document.getElementById('2412.09363v1-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 7 figures, accepted in Astronomy & Astrophysics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.08124">arXiv:2411.08124</a> <span> [<a href="https://arxiv.org/pdf/2411.08124">pdf</a>, <a href="https://arxiv.org/format/2411.08124">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The ALPINE-ALMA [CII] Survey: Modelling ALMA and JWST lines to constrain the interstellar medium of $z\sim 5$ galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Veraldi%2C+E">E. Veraldi</a>, <a href="/search/astro-ph?searchtype=author&query=Vallini%2C+L">L. Vallini</a>, <a href="/search/astro-ph?searchtype=author&query=Pozzi%2C+F">F. Pozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Esposito%2C+F">F. Esposito</a>, <a href="/search/astro-ph?searchtype=author&query=Bethermin%2C+M">M. Bethermin</a>, <a href="/search/astro-ph?searchtype=author&query=Boquien%2C+M">M. Boquien</a>, <a href="/search/astro-ph?searchtype=author&query=Faisst%2C+A">A. Faisst</a>, <a href="/search/astro-ph?searchtype=author&query=Ginolfi%2C+M">M. Ginolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">R. Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Gruppioni%2C+C">C. Gruppioni</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N">N. Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Ibar%2C+E">E. Ibar</a>, <a href="/search/astro-ph?searchtype=author&query=Molina%2C+J">J. Molina</a>, <a href="/search/astro-ph?searchtype=author&query=Rizzo%2C+F">F. Rizzo</a>, <a href="/search/astro-ph?searchtype=author&query=Romano%2C+M">M. Romano</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="2411.08124v1-abstract-short" style="display: inline;"> In this work, we devise a model for estimating UV and optical line emission (i.e., CIII] $1909$A, H$尾$, [OIII] $5007$A, H$伪$, [NII] $6583$A) tracing HII regions in the interstellar medium (ISM) of galaxies at $z\sim4-6$ from the ALMA Large Programme ALPINE. The aim is to investigate the impact of binary stars in the stellar population along with an abrupt quenching in the Star Formation History (S… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.08124v1-abstract-full').style.display = 'inline'; document.getElementById('2411.08124v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.08124v1-abstract-full" style="display: none;"> In this work, we devise a model for estimating UV and optical line emission (i.e., CIII] $1909$A, H$尾$, [OIII] $5007$A, H$伪$, [NII] $6583$A) tracing HII regions in the interstellar medium (ISM) of galaxies at $z\sim4-6$ from the ALMA Large Programme ALPINE. The aim is to investigate the impact of binary stars in the stellar population along with an abrupt quenching in the Star Formation History (SFH) on line emission. This is crucial for understanding the ISM's properties in early galaxies and identifying new star formation tracers in high-$z$ galaxies. The model simulates HII+Photodissociation Region (PDR) complexes through radiative transfer in 1D slabs, characterized by gas density ($n$), ionisation parameter ($U$), and metallicity ($Z$). It considers: (a) heating from star formation (SF), simulated with Starburst99 and BPASS to quantify binary stars impact; (b) constant, exponentially declining, and quenched SFH scenarios. For each galaxy, we select theoretical ratios from CLOUDY models between [CII] line emission, tracing PDRs, and nebular lines from HII regions, using these to derive expected optical/UV lines from observed [CII]. We find binary stars strongly impact line emission post-quenching, keeping UV photon flux higher for longer, maintaining free electron temperature and ionised column density in HII regions up to 5 Myr after quenching. We constrain ISM properties of our subsample, finding a low ionisation parameter $\log U{\approx}-3.8\pm 0.2$ and moderate/high densities $\log(n/\rm cm^{-3}){\approx}2.9\pm 0.6$. Finally, we derive UV/optical line luminosities-SFR relations for different burstiness parameters ($k_s$). In the fiducial BPASS model, relations show negligible SFH dependence but depend on $k_s$, while in the SB99 case, dependence is on SFH. We propose their use for characterising the burstiness of high-$z$ galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.08124v1-abstract-full').style.display = 'none'; document.getElementById('2411.08124v1-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 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 8 figures. Accepted for publication in A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.07585">arXiv:2407.07585</a> <span> [<a href="https://arxiv.org/pdf/2407.07585">pdf</a>, <a href="https://arxiv.org/format/2407.07585">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/10.1051/0004-6361/202451445">10.1051/0004-6361/202451445 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A photo-z cautionary tale: Redshift confirmation of COSBO-7 at z=2.625 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jin%2C+S">Shuowen Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Sillassen%2C+N+B">Nikolaj B. Sillassen</a>, <a href="/search/astro-ph?searchtype=author&query=Hodge%2C+J">Jacqueline Hodge</a>, <a href="/search/astro-ph?searchtype=author&query=Magdis%2C+G+E">Georgios E. Magdis</a>, <a href="/search/astro-ph?searchtype=author&query=Rizzo%2C+F">Francesca Rizzo</a>, <a href="/search/astro-ph?searchtype=author&query=Casey%2C+C">Caitlin Casey</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Valentino%2C+F">Francesco Valentino</a>, <a href="/search/astro-ph?searchtype=author&query=Kokorev%2C+V">Vasily Kokorev</a>, <a href="/search/astro-ph?searchtype=author&query=Magnelli%2C+B">Benjamin Magnelli</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">Raphael Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Gillman%2C+S">Steven Gillman</a>, <a href="/search/astro-ph?searchtype=author&query=Franco%2C+M">Maximilien Franco</a>, <a href="/search/astro-ph?searchtype=author&query=Faisst%2C+A">Andreas Faisst</a>, <a href="/search/astro-ph?searchtype=author&query=Kartaltepe%2C+J">Jeyhan Kartaltepe</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Toft%2C+S">Sune Toft</a>, <a href="/search/astro-ph?searchtype=author&query=Algera%2C+H+S+B">Hiddo S. B. Algera</a>, <a href="/search/astro-ph?searchtype=author&query=Harish%2C+S">Santosh Harish</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+M">Minju Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+D">Daizhong Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Shuntov%2C+M">Marko Shuntov</a>, <a href="/search/astro-ph?searchtype=author&query=Talia%2C+M">Margherita Talia</a>, <a href="/search/astro-ph?searchtype=author&query=Vijayan%2C+A">Aswin Vijayan</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.07585v2-abstract-short" style="display: inline;"> Photometric redshifts are widely used in studies of dusty star-forming galaxies (DSFGs), but catastrophic photo-$z$ failure can undermine all redshift-dependent results. Here we report the spectroscopic redshift confirmation of COSBO-7, a strongly lensed DSFG in the COSMOS-PRIMER field. Recently, a photometric redshift solution of $z\gtrsim7.0$ was reported for COSBO-7 based on ten bands of {\it J… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.07585v2-abstract-full').style.display = 'inline'; document.getElementById('2407.07585v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.07585v2-abstract-full" style="display: none;"> Photometric redshifts are widely used in studies of dusty star-forming galaxies (DSFGs), but catastrophic photo-$z$ failure can undermine all redshift-dependent results. Here we report the spectroscopic redshift confirmation of COSBO-7, a strongly lensed DSFG in the COSMOS-PRIMER field. Recently, a photometric redshift solution of $z\gtrsim7.0$ was reported for COSBO-7 based on ten bands of {\it James Webb} Space Telescope (JWST) NIRCam and MIRI imaging data. This $z$ value was favored by four independent spectral energy distribution (SED) fitting codes, and the result provided an appealing candidate for the most distant massive DSFG known to date. This photo-$z$ solution was also supported by a single line detection in Atacama Large Millimeter Array (ALMA) Band 3 consistent with CO(7-6) at $z=7.46$. However, our new ALMA observations robustly detect two lines in Band 6 identified as CO(7-6) and [CI](2-1) at $z_{\rm spec}=2.625$, and thus the Band 3 line as CO(3-2). These three robust line detections decidedly place COSBO-7 at $z=2.625$, refuting the photo-$z$ solution. We derive physical parameters by fitting near-infrared(NIR)-to-millimeter(mm) photometry and lens modeling, revealing that COSBO-7 is a main sequence galaxy. We examine possible reasons for this photo-$z$ failure and attribute it to (1) the likely underestimation of photometric uncertainties at 0.9\,$渭$m and 1.15 \,$渭$m; and (2) the lack of photometry at wavelengths beyond 20\,$渭$m. Notably, we recover a bona fide $z_{\rm phot}\sim 2.3$ by including the existing MIPS $24\,渭$m photometry, demonstrating the critical importance of mid-infrared (MIR) data in bolstering photo-$z$ measurements. This work highlights a common challenge in modeling the SEDs of DSFGs, and provides a cautionary tale regarding the reliability of photometric redshifts as well as pseudo-spectroscopic redshifts based on single line detection. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.07585v2-abstract-full').style.display = 'none'; document.getElementById('2407.07585v2-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 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">Published in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 690, L16 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.02973">arXiv:2407.02973</a> <span> [<a href="https://arxiv.org/pdf/2407.02973">pdf</a>, <a href="https://arxiv.org/format/2407.02973">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/10.1051/0004-6361/202450760">10.1051/0004-6361/202450760 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> NOEMA formIng Cluster survEy (NICE): Characterizing eight massive galaxy groups at $1.5 < z < 4$ in the COSMOS field </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sillassen%2C+N+B">Nikolaj B. Sillassen</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+S">Shuowen Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Magdis%2C+G+E">Georgios E. Magdis</a>, <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">Emanuele Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+T">Tao Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Lu%2C+S">Shiying Lu</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+H">Hanwen Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Arumugam%2C+V">Vinod Arumugam</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+D">Daizhong Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Brinch%2C+M">Malte Brinch</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Eugenio%2C+C">Chiara D'Eugenio</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">Raphael Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%B3mez-Guijarro%2C+C">Carlos G贸mez-Guijarro</a>, <a href="/search/astro-ph?searchtype=author&query=Rich%2C+M">Michael Rich</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Strazzullo%2C+V">Veronica Strazzullo</a>, <a href="/search/astro-ph?searchtype=author&query=Tan%2C+Q">Qinghua Tan</a>, <a href="/search/astro-ph?searchtype=author&query=Valentino%2C+F">Francesco Valentino</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+Y">Yijun Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Xiao%2C+M">Mengyuan Xiao</a>, <a href="/search/astro-ph?searchtype=author&query=Zhou%2C+L">Luwenjia Zhou</a>, <a href="/search/astro-ph?searchtype=author&query=Bl%C3%A1nquez-Ses%C3%A9%2C+D">David Bl谩nquez-Ses茅</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+Z">Zheng Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+Y">Yanmei Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Ciesla%2C+L">Laure Ciesla</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="2407.02973v2-abstract-short" style="display: inline;"> The NOEMA formIng Cluster survEy (NICE) is a large program targeting 69 massive galaxy group candidates at $z>2$ in six deep fields. We report spectroscopic confirmation of eight groups at $1.65\leq z\leq3.61$ in COSMOS. Homogeneously selected as significant overdensities of red IRAC sources with red Herschel colors, four groups are confirmed by CO and [CI] with NOEMA 3mm observations, three are c… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.02973v2-abstract-full').style.display = 'inline'; document.getElementById('2407.02973v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.02973v2-abstract-full" style="display: none;"> The NOEMA formIng Cluster survEy (NICE) is a large program targeting 69 massive galaxy group candidates at $z>2$ in six deep fields. We report spectroscopic confirmation of eight groups at $1.65\leq z\leq3.61$ in COSMOS. Homogeneously selected as significant overdensities of red IRAC sources with red Herschel colors, four groups are confirmed by CO and [CI] with NOEMA 3mm observations, three are confirmed with ALMA, and one is confirmed by H$伪$ from Subaru/FMOS. We constructed the integrated FIR SEDs for the eight groups, obtaining total IR SFR $=260-1300~{\rm M_\odot}$~yr$^{-1}$. We adopted six methods to estimate the dark matter masses, including stellar mass to halo mass relations, overdensity with galaxy bias, and NFW profile fitting to radial stellar mass density. We found the radial stellar mass density are consistent with a NFW profile, supporting that they are collapsed structures hosted by a single dark matter halo. The best halo mass estimates are $\log(M_{\rm h}/{\rm M_\odot})=12.8-13.7$ with uncertainty of 0.3 dex. From halo mass estimates, we derive baryonic accretion rate ${\rm BAR}=(1-8)\times10^{3}\,{\rm M_{\odot}/yr}$ for this sample. We find a quasi-linear correlation between the integrated SFR/BAR and the theoretical halo mass limit for cold streams, $M_{\rm stream}/M_{\rm h}$, with ${\rm SFR/BAR}=10^{-0.46\pm0.22}\left({M_{\rm stream}/M_{\rm h}}\right)^{0.71\pm0.16}$ with a scatter of $0.40\,{\rm dex}$. Further, we compare halo masses and stellar masses with simulations, and find all structures are consistent with being progenitors of $M_{\rm h}(z=0)>10^{14}\,{\rm M_{\odot}}$ galaxy clusters, and the most massive central galaxies have stellar masses consistent with brightest cluster galaxies (BCGs) progenitors in the TNG300 simulation. The results strongly suggest these structures are forming massive galaxy clusters via baryonic and dark matter accretion. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.02973v2-abstract-full').style.display = 'none'; document.getElementById('2407.02973v2-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 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">44 pages (27pp appendix), 32 figures, 18 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 690, A55 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.13490">arXiv:2403.13490</a> <span> [<a href="https://arxiv.org/pdf/2403.13490">pdf</a>, <a href="https://arxiv.org/format/2403.13490">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202348996">10.1051/0004-6361/202348996 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The ALPINE-ALMA [CII] Survey: Dust emission effective radius up to 3 kpc in the Early Universe </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pozzi%2C+F">F. Pozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">F. Calura</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Amato%2C+Q">Q. D'Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Gavarente%2C+M">M. Gavarente</a>, <a href="/search/astro-ph?searchtype=author&query=Bethermin%2C+M">M. Bethermin</a>, <a href="/search/astro-ph?searchtype=author&query=Boquien%2C+M">M. Boquien</a>, <a href="/search/astro-ph?searchtype=author&query=Casasola%2C+V">V. Casasola</a>, <a href="/search/astro-ph?searchtype=author&query=Cimatti%2C+A">A. Cimatti</a>, <a href="/search/astro-ph?searchtype=author&query=Cochrane%2C+R">R. Cochrane</a>, <a href="/search/astro-ph?searchtype=author&query=Dessauges-Zavadsky%2C+M">M. Dessauges-Zavadsky</a>, <a href="/search/astro-ph?searchtype=author&query=Enia%2C+A">A. Enia</a>, <a href="/search/astro-ph?searchtype=author&query=Esposito%2C+F">F. Esposito</a>, <a href="/search/astro-ph?searchtype=author&query=Faisst%2C+A+L">A. L. Faisst</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">R. Gilli</a>, <a href="/search/astro-ph?searchtype=author&query=Ginolfi%2C+M">M. Ginolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">R. Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Gruppioni%2C+C">C. Gruppioni</a>, <a href="/search/astro-ph?searchtype=author&query=Hayward%2C+C+C">C. C. Hayward</a>, <a href="/search/astro-ph?searchtype=author&query=Ibar%2C+E">E. Ibar</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">A. M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Lemaux%2C+B+C">B. C. Lemaux</a>, <a href="/search/astro-ph?searchtype=author&query=Magdis%2C+G+E">G. E. Magdis</a>, <a href="/search/astro-ph?searchtype=author&query=Molina%2C+J">J. Molina</a>, <a href="/search/astro-ph?searchtype=author&query=Talia%2C+M">M. Talia</a>, <a href="/search/astro-ph?searchtype=author&query=Vallini%2C+L">L. Vallini</a> , et al. (2 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.13490v1-abstract-short" style="display: inline;"> Measurements of the size of dust continuum emission are an important tool for constraining the spatial extent of star formation and hence the build-up of stellar mass. Compact dust emission has generally been observed at Cosmic Noon (z~2-3). However, at earlier epochs, toward the end of the Reionization (z~4-6), only the sizes of a handful of IR-bright galaxies have been measured. In this work, we… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.13490v1-abstract-full').style.display = 'inline'; document.getElementById('2403.13490v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.13490v1-abstract-full" style="display: none;"> Measurements of the size of dust continuum emission are an important tool for constraining the spatial extent of star formation and hence the build-up of stellar mass. Compact dust emission has generally been observed at Cosmic Noon (z~2-3). However, at earlier epochs, toward the end of the Reionization (z~4-6), only the sizes of a handful of IR-bright galaxies have been measured. In this work, we derive the dust emission sizes of main-sequence galaxies at z~5 from the ALPINE survey. We measure the dust effective radius r_e,FIR in the uv-plane in Band 7 of ALMA for seven ALPINE galaxies with resolved emission and we compare it with rest-frame UV and [CII]158$渭$m measurements. We study the r_e,FIR-L_IR scaling relation by considering our dust size measurements and all the data in literature at z~4-6. Finally, we compare our size measurements with predictions from simulations. The dust emission in the selected ALPINE galaxies is rather extended (r_e,FIR~1.5-3 kpc), similar to [CII]158 um but a factor of ~2 larger than the rest-frame UV emission. Putting together all the measurements at z~5, spanning 2 decades in luminosity from L_IR ~ 10^11 L_sun to L_IR ~ 10^13 L_sun, the data highlight a steeply increasing trend of the r_e,FIR-L_IR relation at L_IR< 10^12 L_sun, followed by a downturn and a decreasing trend at brighter luminosities. Finally, simulations that extend up to the stellar masses of the ALPINE galaxies considered in the present work predict a sub-set of galaxies (~25% at 10^10 M_sun < M_star < 10^11 M_sun) with sizes as large as those measured. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.13490v1-abstract-full').style.display = 'none'; document.getElementById('2403.13490v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, Accepted by A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 686, A187 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.07414">arXiv:2403.07414</a> <span> [<a href="https://arxiv.org/pdf/2403.07414">pdf</a>, <a href="https://arxiv.org/format/2403.07414">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/10.1038/s41550-024-02391-9">10.1038/s41550-024-02391-9 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Strong spectral features from asymptotic giant branch stars in distant quiescent galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lu%2C+S">Shiying Lu</a>, <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">Emanuele Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Maraston%2C+C">Claudia Maraston</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">Mark Dickinson</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=Gobat%2C+R">Raphael Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Renzini%2C+A">Alvio Renzini</a>, <a href="/search/astro-ph?searchtype=author&query=Giavalisco%2C+M">Mauro Giavalisco</a>, <a href="/search/astro-ph?searchtype=author&query=Bagley%2C+M+B">Micaela B. Bagley</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=Cheng%2C+Y">Yingjie Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Vega%2C+A">Alexander de la Vega</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Eugenio%2C+C">Chiara D'Eugenio</a>, <a href="/search/astro-ph?searchtype=author&query=Elbaz%2C+D">David Elbaz</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">Steven L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%B3mez-Guijarro%2C+C">Carlos G贸mez-Guijarro</a>, <a href="/search/astro-ph?searchtype=author&query=Gu%2C+Q">Qiusheng Gu</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N+P">Nimish P. Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Huertas-Company%2C+M">Marc Huertas-Company</a>, <a href="/search/astro-ph?searchtype=author&query=Kartaltepe%2C+J+S">Jeyhan S. Kartaltepe</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Bail%2C+A+L">Aur茅lien Le Bail</a>, <a href="/search/astro-ph?searchtype=author&query=Lyu%2C+Y">Yipeng Lyu</a>, <a href="/search/astro-ph?searchtype=author&query=Magnelli%2C+B">Benjamin Magnelli</a>, <a href="/search/astro-ph?searchtype=author&query=Mobasher%2C+B">Bahram Mobasher</a> , et al. (5 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="2403.07414v4-abstract-short" style="display: inline;"> Dating the ages and weighting the stellar populations in galaxies are essential steps when studying galaxy formation through cosmic times. Evolutionary population synthesis models with different input physics are used for this purpose. Moreover, the contribution from the thermally pulsing asymptotic giant branch (TP-AGB) stellar phase, which peaks for intermediate-age 0.6-2 Gyr, has been debated f… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.07414v4-abstract-full').style.display = 'inline'; document.getElementById('2403.07414v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.07414v4-abstract-full" style="display: none;"> Dating the ages and weighting the stellar populations in galaxies are essential steps when studying galaxy formation through cosmic times. Evolutionary population synthesis models with different input physics are used for this purpose. Moreover, the contribution from the thermally pulsing asymptotic giant branch (TP-AGB) stellar phase, which peaks for intermediate-age 0.6-2 Gyr, has been debated for decades. Here we report the detection of strong cool-star signatures in the rest-frame near-infrared spectra of three young (~1Gyr), massive (~10^10Msun) quiescent galaxies at large look-back time, z=1-2, using JWST/NIRSpec. The coexistence of oxygen- and carbon-type absorption features, spectral edges and features from rare species, such as vanadium and possibly zirconium, reveal a strong contribution from TP-AGB stars. Population synthesis models with a significant TP-AGB contribution reproduce the observations better than those with a weak TP-AGB, which are commonly used. These findings call for revisions of published stellar population fitting results, as they point to populations with lower masses and younger ages and have further implications for cosmic dust production and chemical enrichment. New generations of improved models are needed, informed by these and future observations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.07414v4-abstract-full').style.display = 'none'; document.getElementById('2403.07414v4-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 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 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">Nature Astronomy, in publication</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2024, oct </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.05248">arXiv:2403.05248</a> <span> [<a href="https://arxiv.org/pdf/2403.05248">pdf</a>, <a href="https://arxiv.org/format/2403.05248">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/ad4986">10.3847/2041-8213/ad4986 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> JWST's first glimpse of a z > 2 forming cluster reveals a top-heavy stellar mass function </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sun%2C+H">Hanwen Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+T">Tao Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+K">Ke Xu</a>, <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">Emanuele Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Gu%2C+Q">Qing Gu</a>, <a href="/search/astro-ph?searchtype=author&query=Kodama%2C+T">Tadayuki Kodama</a>, <a href="/search/astro-ph?searchtype=author&query=Zanella%2C+A">Anita Zanella</a>, <a href="/search/astro-ph?searchtype=author&query=Elbaz%2C+D">David Elbaz</a>, <a href="/search/astro-ph?searchtype=author&query=Tanaka%2C+I">Ichi Tanaka</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">Raphael Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Guo%2C+Q">Qi Guo</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+J">Jiaxin Han</a>, <a href="/search/astro-ph?searchtype=author&query=Lu%2C+S">Shiying Lu</a>, <a href="/search/astro-ph?searchtype=author&query=Zhou%2C+L">Luwenjia Zhou</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="2403.05248v3-abstract-short" style="display: inline;"> Clusters and their progenitors (protoclusters) at z = 2-4, the peak epoch of star formation, are ideal laboratories to study the formation process of both the clusters themselves and their member galaxies. However, a complete census of their member galaxies has been challenging due to observational difficulties. Here we present new JWST/NIRCam observations targeting the distant cluster CLJ1001 at… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.05248v3-abstract-full').style.display = 'inline'; document.getElementById('2403.05248v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.05248v3-abstract-full" style="display: none;"> Clusters and their progenitors (protoclusters) at z = 2-4, the peak epoch of star formation, are ideal laboratories to study the formation process of both the clusters themselves and their member galaxies. However, a complete census of their member galaxies has been challenging due to observational difficulties. Here we present new JWST/NIRCam observations targeting the distant cluster CLJ1001 at z = 2.51 from the COSMOS-Web program, which, in combination with previous narrowband imaging targeting H-alpha emitters and deep millimeter surveys of CO emitters, provide a complete view of massive galaxy assembly in CLJ1001. In particular, JWST reveals a population of massive, extremely red cluster members in the long-wavelength bands that were invisible in previous Hubble Space Telescope (HST)/F160W imaging (HST-dark members). Based on this highly complete spectroscopic sample of member galaxies, we show that the spatial distribution of galaxies in CLJ1001 exhibits a strong central concentration, with the central galaxy density already resembling that of low-z clusters. Moreover, we reveal a "top-heavy" stellar mass function for the star-forming galaxies (SFGs), with an overabundance of massive SFGs piled up in the cluster core. These features strongly suggest that CLJ1001 is caught in a rapid transition, with many of its massive SFGs likely soon becoming quiescent. In the context of cluster formation, these findings suggest that the earliest clusters form from the inside out and top to bottom, with the massive galaxies in the core assembling first, followed by the less massive ones in the outskirts. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.05248v3-abstract-full').style.display = 'none'; document.getElementById('2403.05248v3-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 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 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">14 pages, 9 figures, 1 table, published by ApJL</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJL, 967, L34 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.16473">arXiv:2401.16473</a> <span> [<a href="https://arxiv.org/pdf/2401.16473">pdf</a>, <a href="https://arxiv.org/format/2401.16473">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </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/10.1051/0004-6361/202349060">10.1051/0004-6361/202349060 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The powerful lens galaxy cluster PLCK G287.0+32.9 ($胃_E \sim 43''$) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=D%27Addona%2C+M">Maurizio D'Addona</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">Amata Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">Piero Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">Claudio Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Caminha%2C+G">Gabriel Caminha</a>, <a href="/search/astro-ph?searchtype=author&query=Acebron%2C+A">Ana Acebron</a>, <a href="/search/astro-ph?searchtype=author&query=Angora%2C+G">Giuseppe Angora</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">Pietro Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Bozza%2C+V">Valerio Bozza</a>, <a href="/search/astro-ph?searchtype=author&query=Granata%2C+G">Giovanni Granata</a>, <a href="/search/astro-ph?searchtype=author&query=Annunziatella%2C+M">Marianna Annunziatella</a>, <a href="/search/astro-ph?searchtype=author&query=Gargiulo%2C+A">Adriana Gargiulo</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">Raphael Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Tozzi%2C+P">Paolo Tozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Girardi%2C+M">Marisa Girardi</a>, <a href="/search/astro-ph?searchtype=author&query=Lombardi%2C+M">Marco Lombardi</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">Massimo Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Schipani%2C+P">Pietro Schipani</a>, <a href="/search/astro-ph?searchtype=author&query=Tortorelli%2C+L">Luca Tortorelli</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">Eros 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="2401.16473v2-abstract-short" style="display: inline;"> We present a new high-precision strong lensing model of PLCK G287.0$+$32.9, a massive lens galaxy cluster at $z=0.383$, with the aim to get an accurate estimation of its effective Einstein radius and total mass distribution. We also present a spectroscopic catalog containing accurate redshift measurements for 490 objects, including multiply-lensed sources and cluster member galaxies. We exploit hi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.16473v2-abstract-full').style.display = 'inline'; document.getElementById('2401.16473v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.16473v2-abstract-full" style="display: none;"> We present a new high-precision strong lensing model of PLCK G287.0$+$32.9, a massive lens galaxy cluster at $z=0.383$, with the aim to get an accurate estimation of its effective Einstein radius and total mass distribution. We also present a spectroscopic catalog containing accurate redshift measurements for 490 objects, including multiply-lensed sources and cluster member galaxies. We exploit high-quality spectroscopic data from three pointings of the VLT Multi Unit Spectroscopic Explorer, covering a central $3~\rm{arcmin}^2$ region of the cluster. We complete the spectroscopic catalog by including redshift measurements from VLT-VIMOS and KECK-DEIMOS. We identify 129 spectroscopic cluster member galaxies, with redshift values $0.360 \leq z \leq 0.405$ and $m_{\rm{F160W}} \leq 21$, and 24 photometric ones identified with a Convolutional Neural Network from ancillary HST imaging. We also identify 114 multiple images from 28 background sources, of which 84 images from 16 sources are new and the remaining ones were identified in previous work. The best-fitting lens model shows a root mean square separation value between the predicted and observed positions of the multiple images of $0.75''$, corresponding to an improvement in reconstructing the observed positions of the multiple images of a factor of $2.5$ with respect to previous models. Using the predictive power of our new lens model we find 3 new multiple images and we confirm the configuration of three systems of multiple images that were not used for the optimization of the model. The derived total mass distribution confirms this cluster to be a very prominent gravitational lens with an effective Einstein $胃_{E} = 43.4'' \pm 0.1''$, that is in agreement with previous estimates and corresponds to a total mass enclosed in the critical curve of $M_E = {3.33}_{-0.07}^{+0.02} \times{ 10^{14} M_\odot}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.16473v2-abstract-full').style.display = 'none'; document.getElementById('2401.16473v2-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 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">submitted to "Astronomy & Astrophysics" and accepted the on January 29th 2024</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A Volume 686, June 2024, A4 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.11493">arXiv:2311.11493</a> <span> [<a href="https://arxiv.org/pdf/2311.11493">pdf</a>, <a href="https://arxiv.org/format/2311.11493">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/10.1051/0004-6361/202348511">10.1051/0004-6361/202348511 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The ALMA-ALPINE [CII] survey: sub-kpc morphology of 3 main-sequence galaxy systems at z~4.5 revealed by ALMA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Devereaux%2C+T">T. Devereaux</a>, <a href="/search/astro-ph?searchtype=author&query=Cassata%2C+P">P. Cassata</a>, <a href="/search/astro-ph?searchtype=author&query=Ibar%2C+E">E. Ibar</a>, <a href="/search/astro-ph?searchtype=author&query=Accard%2C+C">C. Accard</a>, <a href="/search/astro-ph?searchtype=author&query=Guillaume%2C+C">C. Guillaume</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%A9thermin%2C+M">M. B茅thermin</a>, <a href="/search/astro-ph?searchtype=author&query=Dessauges-Zavadsky%2C+M">M. Dessauges-Zavadsky</a>, <a href="/search/astro-ph?searchtype=author&query=Faisst%2C+A">A. Faisst</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+G+C">G. C. Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Zanella%2C+A">A. Zanella</a>, <a href="/search/astro-ph?searchtype=author&query=Bardelli%2C+S">S. Bardelli</a>, <a href="/search/astro-ph?searchtype=author&query=Boquien%2C+M">M. Boquien</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Onghia%2C+E">E. D'Onghia</a>, <a href="/search/astro-ph?searchtype=author&query=Giavalisco%2C+M">M. Giavalisco</a>, <a href="/search/astro-ph?searchtype=author&query=Ginolfi%2C+M">M. Ginolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">R. Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Hayward%2C+C+C">C. C. Hayward</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">A. M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Lemaux%2C+B">B. Lemaux</a>, <a href="/search/astro-ph?searchtype=author&query=Magdis%2C+G">G. Magdis</a>, <a href="/search/astro-ph?searchtype=author&query=Mendez-Hernandez%2C+H">H. Mendez-Hernandez</a>, <a href="/search/astro-ph?searchtype=author&query=Molina%2C+J">J. Molina</a>, <a href="/search/astro-ph?searchtype=author&query=Pozzi%2C+F">F. Pozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Romano%2C+M">M. Romano</a>, <a href="/search/astro-ph?searchtype=author&query=Tasca%2C+L">L. Tasca</a> , et al. (3 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.11493v1-abstract-short" style="display: inline;"> Context: From redshift 6 to redshift $\approx$ 4 galaxies grow rapidly from low mass galaxies towards the more mature massive galaxies we see at the cosmic noon. Growth via gas accretion and mergers undoubtedly shape this evolution - however, there currently exists much uncertainty over the contribution of each of these processes to the overall evolution of galaxies. Furthermore, previous characte… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.11493v1-abstract-full').style.display = 'inline'; document.getElementById('2311.11493v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.11493v1-abstract-full" style="display: none;"> Context: From redshift 6 to redshift $\approx$ 4 galaxies grow rapidly from low mass galaxies towards the more mature massive galaxies we see at the cosmic noon. Growth via gas accretion and mergers undoubtedly shape this evolution - however, there currently exists much uncertainty over the contribution of each of these processes to the overall evolution of galaxies. Furthermore, previous characterisations of the morphology of galaxies in the molecular gas phase has been limited by the coarse resolution of previous observations. Aims: The goal of this paper is to derive the morpho-kinematic properties of 3 main-sequence systems at $z\sim4.5$, drawn from the ALPINE survey, using brand new high-resolution ALMA data in band 7. The objects were previously characterised as one merger with three components, and and two dispersion-dominated galaxies. Methods: We use intensity and velocity maps, position-velocity diagrams and radial profiles of [CII], in combination with dust continuum maps, to analyse the morphology and kinematics of the 3 systems.} Results: In general, we find that the high-resolution ALMA data reveal more complex morpho-kinematic properties. We identify in one galaxy interaction-induced clumps, showing the profound effect that mergers have on the molecular gas in galaxies, consistent with what is suggested in recent simulations. A galaxy that was previously classified as dispersion dominated turned out to show two bright [CII] emission regions, that could either be merging galaxies or massive star-forming regions within the galaxy itself. The high resolution data for the other dispersion dominated object also revealed clumps of [CII] that were not previously identified. Within the sample, we might also detect star-formation powered outflows (or outflows from Active Galactic Nuclei) which appear to be fuelling diffuse gas regions and enriching the circumgalactic medium. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.11493v1-abstract-full').style.display = 'none'; document.getElementById('2311.11493v1-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 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to A&A, 13 pages</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 686, A156 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.04867">arXiv:2311.04867</a> <span> [<a href="https://arxiv.org/pdf/2311.04867">pdf</a>, <a href="https://arxiv.org/format/2311.04867">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/10.1051/0004-6361/202348540">10.1051/0004-6361/202348540 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Cosmic Vine: A z=3.44 large-scale structure hosting massive quiescent galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jin%2C+S">Shuowen Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Sillassen%2C+N+B">Nikolaj B. Sillassen</a>, <a href="/search/astro-ph?searchtype=author&query=Magdis%2C+G+E">Georgios E. Magdis</a>, <a href="/search/astro-ph?searchtype=author&query=Brinch%2C+M">Malte Brinch</a>, <a href="/search/astro-ph?searchtype=author&query=Shuntov%2C+M">Marko Shuntov</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G">Gabriel Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">Raphael Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Valentino%2C+F">Francesco Valentino</a>, <a href="/search/astro-ph?searchtype=author&query=Carnall%2C+A+C">Adam C. Carnall</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+M">Minju Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Vijayan%2C+A+P">Aswin P. Vijayan</a>, <a href="/search/astro-ph?searchtype=author&query=Gillman%2C+S">Steven Gillman</a>, <a href="/search/astro-ph?searchtype=author&query=Kokorev%2C+V">Vasily Kokorev</a>, <a href="/search/astro-ph?searchtype=author&query=Bail%2C+A+L">Aur茅lien Le Bail</a>, <a href="/search/astro-ph?searchtype=author&query=Greve%2C+T+R">Thomas R. Greve</a>, <a href="/search/astro-ph?searchtype=author&query=Gullberg%2C+B">Bitten Gullberg</a>, <a href="/search/astro-ph?searchtype=author&query=Gould%2C+K+M+L">Katriona M. L. Gould</a>, <a href="/search/astro-ph?searchtype=author&query=Toft%2C+S">Sune Toft</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.04867v3-abstract-short" style="display: inline;"> We report the discovery of a large-scale structure at z=3.44 revealed by JWST data in the Extended Groth Strip (EGS) field. This structure, called the Cosmic Vine, consists of 20 galaxies with spectroscopic redshifts at 3.43<z<3.45 and six galaxy overdensities ($4-7蟽$) with consistent photometric redshifts, making up a vine-like structure extending over a ~4x0.2 pMpc^2 area. The two most massive g… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.04867v3-abstract-full').style.display = 'inline'; document.getElementById('2311.04867v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.04867v3-abstract-full" style="display: none;"> We report the discovery of a large-scale structure at z=3.44 revealed by JWST data in the Extended Groth Strip (EGS) field. This structure, called the Cosmic Vine, consists of 20 galaxies with spectroscopic redshifts at 3.43<z<3.45 and six galaxy overdensities ($4-7蟽$) with consistent photometric redshifts, making up a vine-like structure extending over a ~4x0.2 pMpc^2 area. The two most massive galaxies ($M_*\approx10^{10.9}~M_\odot$) of the Cosmic Vine are found to be quiescent with bulge-dominated morphologies ($B/T>70\%$). Comparisons with simulations suggest that the Cosmic Vine would form a cluster with halo mass $M_{\rm halo}>10^{14}M_\odot$ at z=0, and the two massive galaxies are likely forming the brightest cluster galaxies (BCGs). The results unambiguously reveal that massive quiescent galaxies can form in growing large-scale structures at z>3, thus disfavoring the environmental quenching mechanisms that require a virialized cluster core. Instead, as suggested by the interacting and bulge-dominated morphologies, the two galaxies are likely quenched by merger-triggered starburst or active galactic nucleus (AGN) feedback before falling into a cluster core. Moreover, we found that the observed specific star formation rates of massive quiescent galaxies in z>3 dense environments are one to two orders of magnitude lower than that of the BCGs in the TNG300 simulation. This discrepancy potentially poses a challenge to the models of massive cluster galaxy formation. Future studies comparing a large sample with dedicated cluster simulations are required to solve the problem. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.04867v3-abstract-full').style.display = 'none'; document.getElementById('2311.04867v3-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 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">A&A Letters in press, open access at https://doi.org/10.1051/0004-6361/202348540</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.15925">arXiv:2310.15925</a> <span> [<a href="https://arxiv.org/pdf/2310.15925">pdf</a>, <a href="https://arxiv.org/format/2310.15925">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/10.1051/0004-6361/202348351">10.1051/0004-6361/202348351 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Noema formIng Cluster survEy (NICE): Discovery of a starbursting galaxy group with a radio-luminous core at z=3.95 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zhou%2C+L">Luwenjia Zhou</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+T">Tao Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">Emanuele Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Coogan%2C+R">Rosemary Coogan</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+H">Hanwen Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+K">Ke Xu</a>, <a href="/search/astro-ph?searchtype=author&query=Arumugam%2C+V">Vinodiran Arumugam</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+S">Shuowen Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+D">Daizhong Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Lu%2C+S">Shiying Lu</a>, <a href="/search/astro-ph?searchtype=author&query=Sillassen%2C+N">Nikolaj Sillassen</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+Y">Yijun Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Shi%2C+Y">Yong Shi</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+Z">Zhi-Yu Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Tan%2C+Q">Qinghua Tan</a>, <a href="/search/astro-ph?searchtype=author&query=Gu%2C+Q">Qiusheng Gu</a>, <a href="/search/astro-ph?searchtype=author&query=Elbaz%2C+D">David Elbaz</a>, <a href="/search/astro-ph?searchtype=author&query=Bail%2C+A+L">Aurelien Le Bail</a>, <a href="/search/astro-ph?searchtype=author&query=Magnelli%2C+B">Benjamin Magnelli</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%B3mez-Guijarro%2C+C">Carlos G贸mez-Guijarro</a>, <a href="/search/astro-ph?searchtype=author&query=d%27Eugenio%2C+C">Chiara d'Eugenio</a>, <a href="/search/astro-ph?searchtype=author&query=Magdis%2C+G+E">Georgios E. Magdis</a>, <a href="/search/astro-ph?searchtype=author&query=Valentino%2C+F">Francesco Valentino</a>, <a href="/search/astro-ph?searchtype=author&query=Ji%2C+Z">Zhiyuan Ji</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">Raphael Gobat</a> , et al. (12 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="2310.15925v2-abstract-short" style="display: inline;"> The study of distant galaxy groups and clusters at the peak epoch of star formation is limited by the lack of a statistically and homogeneously selected and spectroscopically confirmed sample. Recent discoveries of concentrated starburst activities in cluster cores have opened a new window to hunt for these structures based on their integrated IR luminosities. Hereby we carry out the large NOEMA (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.15925v2-abstract-full').style.display = 'inline'; document.getElementById('2310.15925v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.15925v2-abstract-full" style="display: none;"> The study of distant galaxy groups and clusters at the peak epoch of star formation is limited by the lack of a statistically and homogeneously selected and spectroscopically confirmed sample. Recent discoveries of concentrated starburst activities in cluster cores have opened a new window to hunt for these structures based on their integrated IR luminosities. Hereby we carry out the large NOEMA (NOrthern Extended Millimeter Array) program targeting a statistical sample of infrared-luminous sources associated with overdensities of massive galaxies at z>2, the Noema formIng Cluster survEy (NICE). We present the first result from the ongoing NICE survey, a compact group at z=3.95 in the Lockman Hole field (LH-SBC3), confirmed via four massive (M_star>10^10.5M_sun) galaxies detected in CO(4-3) and [CI](1-0) lines. The four CO-detected members of LH-SBC3 are distributed over a 180 kpc physical scale, and the entire structure has an estimated halo mass of ~10^13Msun and total star formation rate (SFR) of ~4000Msun/yr. In addition, the most massive galaxy hosts a radio-loud AGN with L_1.4GHz, rest = 3.0*10^25W/Hz. The discovery of LH-SBC3 demonstrates the feasibility of our method to efficiently identify high-z compact groups or forming cluster cores. The existence of these starbursting cluster cores up to z~4 provides critical insights into the mass assembly history of the central massive galaxies in clusters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.15925v2-abstract-full').style.display = 'none'; document.getElementById('2310.15925v2-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 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">10 pages, 8 figures, published by A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A, 684, A196 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.01601">arXiv:2310.01601</a> <span> [<a href="https://arxiv.org/pdf/2310.01601">pdf</a>, <a href="https://arxiv.org/format/2310.01601">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/10.1051/0004-6361/202347771">10.1051/0004-6361/202347771 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Uncovering the MIR emission of quiescent galaxies with $JWST$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bl%C3%A1nquez-Ses%C3%A9%2C+D">David Bl谩nquez-Ses茅</a>, <a href="/search/astro-ph?searchtype=author&query=Magdis%2C+G+E">G. E. Magdis</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%B3mez-Guijarro%2C+C">C. G贸mez-Guijarro</a>, <a href="/search/astro-ph?searchtype=author&query=Shuntov%2C+M">M. Shuntov</a>, <a href="/search/astro-ph?searchtype=author&query=Kokorev%2C+V">V. Kokorev</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G">G. Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Valentino%2C+F">F. Valentino</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=Paspaliaris%2C+E+-">E. -D. Paspaliaris</a>, <a href="/search/astro-ph?searchtype=author&query=Rigopoulou%2C+D">D. Rigopoulou</a>, <a href="/search/astro-ph?searchtype=author&query=Hjorth%2C+J">J. Hjorth</a>, <a href="/search/astro-ph?searchtype=author&query=Langeroodi%2C+D">D. Langeroodi</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">R. Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+S">S. Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Sillassen%2C+N+B">N. B. Sillassen</a>, <a href="/search/astro-ph?searchtype=author&query=Gillman%2C+S">S. Gillman</a>, <a href="/search/astro-ph?searchtype=author&query=Greve%2C+T+R">T. R. Greve</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+M">M. Lee</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="2310.01601v1-abstract-short" style="display: inline;"> We present a study of the mid-IR (MIR) emission of quiescent galaxies (QGs) beyond the local universe. Using deep $JWST$ imaging in the SMACS-0723 cluster field we identify a mass limited ($M_{*} >10^{9}$M$_{\odot}$) sample of intermediate redshift QGs ($0.2<z<0.7$) and perform modeling of their rest-frame UV to MIR photometry. We find that QGs exhibit a range of MIR spectra that are composed of a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.01601v1-abstract-full').style.display = 'inline'; document.getElementById('2310.01601v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.01601v1-abstract-full" style="display: none;"> We present a study of the mid-IR (MIR) emission of quiescent galaxies (QGs) beyond the local universe. Using deep $JWST$ imaging in the SMACS-0723 cluster field we identify a mass limited ($M_{*} >10^{9}$M$_{\odot}$) sample of intermediate redshift QGs ($0.2<z<0.7$) and perform modeling of their rest-frame UV to MIR photometry. We find that QGs exhibit a range of MIR spectra that are composed of a stellar continuum and a dust component that is 1-2 orders of magnitude fainter to that of star-forming galaxies. The observed scatter in the MIR spectra, especially at $位_{\rm rest} > 5 渭$m, can be attributed to different dust continuum levels and/or the presence of Polycyclic Aromatic Hydrocarbons (PAHs) features. The latter would indicate enhanced 11.3- and 12.7 $渭$m PAHs strengths with respect to those at 6.2- and 7.7$ 渭$m, consistent with the observed spectra of local ellipticals and indicative of soft radiation fields. Finally, we augment the average UV-to-MIR spectrum of the population with cold dust and gas emission in the far-IR/mm and construct a panchromatic UV-to-radio SED that can serve as a template for the future exploration of the interstellar medium of $z>0$ QGs with ALMA and $JWST$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.01601v1-abstract-full').style.display = 'none'; document.getElementById('2310.01601v1-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 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">The panchromatic QG SED has been made publicly available at http://www.georgiosmagdis.com/software</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 679, L2 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.12730">arXiv:2309.12730</a> <span> [<a href="https://arxiv.org/pdf/2309.12730">pdf</a>, <a href="https://arxiv.org/format/2309.12730">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/10.1051/0004-6361/202347233">10.1051/0004-6361/202347233 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The [CII] 158 $渭$m emission line as a gas mass tracer in high redshift quiescent galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=D%27Eugenio%2C+C">C. D'Eugenio</a>, <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">E. Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+D">D. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">R. Gobat</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="2309.12730v1-abstract-short" style="display: inline;"> Many efforts have been done in recent years to probe the gas fraction evolution of massive quiescent galaxies (QGs); however, a clear picture has not yet been established. Recent spectroscopic confirmations at z>3 offer the chance to measure the residual gas reservoirs of massive galaxies a few hundreds of Myr after their death and to study how fast quenching proceeds in a highly star-forming Univ… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.12730v1-abstract-full').style.display = 'inline'; document.getElementById('2309.12730v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.12730v1-abstract-full" style="display: none;"> Many efforts have been done in recent years to probe the gas fraction evolution of massive quiescent galaxies (QGs); however, a clear picture has not yet been established. Recent spectroscopic confirmations at z>3 offer the chance to measure the residual gas reservoirs of massive galaxies a few hundreds of Myr after their death and to study how fast quenching proceeds in a highly star-forming Universe. Even so, stringent constraints at z$>$2 remain hardly accessible with ALMA when adopting molecular gas tracers commonly used for the quenched population. In this letter, we propose overcoming this impasse by using the carbon [CII] 158 $渭$m emission line to systematically probe the gaseous budget of unlensed QGs at z>2.8, when these galaxies could still host non-negligible star formation on an absolute scale and when the line becomes best observable with ALMA (Bands 8 and 7). So far predominantly used for star-forming galaxies, this emission line is the best choice to probe the gas budget of spectroscopically confirmed QGs at $z>3$, reaching 2-4 and 13-30 times deeper than dust continuum (ALMA band 7) and CO(2-1)/(1-0) (VLA K-K$伪$ bands), respectively, at fixed integration time. Exploiting archival ALMA observations, we place conservative 3$蟽$ upper limits on the molecular gas fraction (f$_{\rm{mol}}=M_{\rm{H_2}}/M_{\star}$) of ADF22-QG1 (f$_{\rm{mol}}$<21%), ZF-COS-20115 (f$_{\rm{mol}}$<3.2%), two of the best-studied high-z QGs in the literature, and GS-9209 (f$_{\rm{mol}}$<72%), the most distant massive QG discovered to date. The deep upper limit found for ZF-COS-20115 is 3 times lower than previously anticipated for high-z QGs suggesting, at best, the existence of a large scatter in the f$_{\rm{mol}}$ distribution of the first QGs. Lastly, we discuss the current limitations of the method and propose ways to mitigate some of them by exploiting ALMA bands 9 and 10. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.12730v1-abstract-full').style.display = 'none'; document.getElementById('2309.12730v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 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">7 pages, 2 figures. A&A Letters in press</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 678, L9 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.05202">arXiv:2307.05202</a> <span> [<a href="https://arxiv.org/pdf/2307.05202">pdf</a>, <a href="https://arxiv.org/format/2307.05202">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/acdb5a">10.3847/2041-8213/acdb5a <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Accelerated structural evolution of galaxies in a starbursting cluster at z=2.51 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Xu%2C+C">Can Xu</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+T">Tao Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Gu%2C+Q">Qiusheng Gu</a>, <a href="/search/astro-ph?searchtype=author&query=Zanella%2C+A">Anita Zanella</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+K">Ke Xu</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+H">Hanwen Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Strazzullo%2C+V">Veronica Strazzullo</a>, <a href="/search/astro-ph?searchtype=author&query=Valentino%2C+F">Francesco Valentino</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">Raphael Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">Emanuele Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Elbaz%2C+D">David Elbaz</a>, <a href="/search/astro-ph?searchtype=author&query=Xiao%2C+M">Mengyuan Xiao</a>, <a href="/search/astro-ph?searchtype=author&query=Lu%2C+S">Shiying Lu</a>, <a href="/search/astro-ph?searchtype=author&query=Zhou%2C+L">Luwenjia Zhou</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="2307.05202v1-abstract-short" style="display: inline;"> Structural properties of cluster galaxies during their peak formation epoch, $z \sim 2-4$ provide key information on whether and how environment affects galaxy formation and evolution. Based on deep HST/WFC3 imaging towards the z=2.51 cluster, J1001, we explore environmental effects on the structure, color gradients, and stellar populations of a statistical sample of cluster SFGs. We find that the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.05202v1-abstract-full').style.display = 'inline'; document.getElementById('2307.05202v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.05202v1-abstract-full" style="display: none;"> Structural properties of cluster galaxies during their peak formation epoch, $z \sim 2-4$ provide key information on whether and how environment affects galaxy formation and evolution. Based on deep HST/WFC3 imaging towards the z=2.51 cluster, J1001, we explore environmental effects on the structure, color gradients, and stellar populations of a statistical sample of cluster SFGs. We find that the cluster SFGs are on average smaller than their field counterparts. This difference is most pronounced at the high-mass end ($M_{\star} > 10^{10.5} M_{\odot}$) with nearly all of them lying below the mass-size relation of field galaxies. The high-mass cluster SFGs are also generally old with a steep negative color gradient, indicating an early formation time likely associated with strong dissipative collapse. For low-mass cluster SFGs, we unveil a population of compact galaxies with steep positive color gradients that are not seen in the field. This suggests that the low-mass compact cluster SFGs may have already experienced strong environmental effects, e.g., tidal/ram pressure stripping, in this young cluster. These results provide evidence on the environmental effects at work in the earliest formed clusters with different roles in the formation of low and high-mass galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.05202v1-abstract-full').style.display = 'none'; document.getElementById('2307.05202v1-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 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">13 pages, 10 figures, 1 table</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJL, July 2023, 951, L21 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.08605">arXiv:2306.08605</a> <span> [<a href="https://arxiv.org/pdf/2306.08605">pdf</a>, <a href="https://arxiv.org/format/2306.08605">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/10.1051/0004-6361/202347190">10.1051/0004-6361/202347190 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Near-infrared emission line diagnostics for AGN from the local Universe to redshift 3 </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Pentericci%2C+L">Laura Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Feltre%2C+A">Anna Feltre</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=Radovich%2C+M">Mario Radovich</a>, <a href="/search/astro-ph?searchtype=author&query=Seill%C3%A9%2C+L+M">Lise Marie Seill茅</a>, <a href="/search/astro-ph?searchtype=author&query=Oliva%2C+E">Ernesto Oliva</a>, <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">Emanuele Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Amor%C3%ADn%2C+R">Ricardo Amor铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Bagley%2C+M+B">Micaela B. Bagley</a>, <a href="/search/astro-ph?searchtype=author&query=Bisigello%2C+L">Laura Bisigello</a>, <a href="/search/astro-ph?searchtype=author&query=Buat%2C+V">V茅ronique Buat</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">Marco Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Cleri%2C+N">Nikko Cleri</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">Mark Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez%2C+V">Vital Fern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S">Steven Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Giavalisco%2C+M">Mauro Giavalisco</a>, <a href="/search/astro-ph?searchtype=author&query=Grazian%2C+A">Andrea Grazian</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N">Nimish Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">Michaela Hirschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Juneau%2C+S">St茅phanie Juneau</a>, <a href="/search/astro-ph?searchtype=author&query=Kartaltepe%2C+J+S">Jeyhan S. Kartaltepe</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A">Anton Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Lucas%2C+R+A">Ray A. Lucas</a> , et al. (13 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.08605v2-abstract-short" style="display: inline;"> Optical rest-frame spectroscopic diagnostics are usually employed to distinguish between star formation and AGN-powered emission. However, this method is biased against dusty sources, hampering a complete census of the AGN population across cosmic epochs. To mitigate this effect, it is crucial to observe at longer wavelengths in the rest-frame near-infrared (near-IR), which is less affected by dus… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.08605v2-abstract-full').style.display = 'inline'; document.getElementById('2306.08605v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.08605v2-abstract-full" style="display: none;"> Optical rest-frame spectroscopic diagnostics are usually employed to distinguish between star formation and AGN-powered emission. However, this method is biased against dusty sources, hampering a complete census of the AGN population across cosmic epochs. To mitigate this effect, it is crucial to observe at longer wavelengths in the rest-frame near-infrared (near-IR), which is less affected by dust attenuation and can thus provide a better description of the intrinsic properties of galaxies. AGN diagnostics in this regime have not been fully exploited so far, due to the scarcity of near-IR observations of both AGNs and star-forming galaxies, especially at redshifts higher than 0.5. Using Cloudy photoionization models, we identify new AGN - star formation diagnostics based on the ratio of bright near-infrared emission lines, namely [SIII] 9530 Angstrom, [CI] 9850 Angstrom, [PII] 1.188 $渭m$, [FeII] $1.257 渭m$, and [FeII] $1.64 渭m$ to Paschen lines (either Pa$纬$ or Pa$尾$), providing simple, analytical classification criteria. We apply these diagnostics to a sample of 64 star-forming galaxies and AGNs at 0 < z < 1, and 65 sources at 1 < z < 3 recently observed with JWST-NIRSpec in CEERS. We find that the classification inferred from the near-infrared is broadly consistent with the optical one based on the BPT and the [SII]/H$伪$ ratio. However, in the near-infrared, we find $\sim 60 \%$ more AGNs than in the optical (13 instead of 8), with 5 sources classified as 'hidden' AGNs, showing a larger AGN contribution at longer wavelengths, possibly due to the presence of optically thick dust. The diagnostics we present provide a promising tool to find and characterize AGNs from z=0 to z=3 with low and medium-resolution near-IR spectrographs in future surveys. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.08605v2-abstract-full').style.display = 'none'; document.getElementById('2306.08605v2-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, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Paper accepted for publication in A&A on 05/09/2023. Three public Github repositories include: (1) a table with emission line measurements for the paper sample : https://github.com/Anthony96/Line_measurements_nearIR , Cloudy emission line predictions for star-forming galaxies and AGN models : https://github.com/Anthony96/star-forming_models , https://github.com/Anthony96/AGN_models</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 679, A80 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.12110">arXiv:2303.12110</a> <span> [<a href="https://arxiv.org/pdf/2303.12110">pdf</a>, <a href="https://arxiv.org/format/2303.12110">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/10.1051/0004-6361/202345977">10.1051/0004-6361/202345977 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gas Mass Reservoir of Quiescent Galaxies at Cosmic Noon </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bl%C3%A1nquez-Ses%C3%A9%2C+D">David Bl谩nquez-Ses茅</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%B3mez-Guijarro%2C+C">C. G贸mez-Guijarro</a>, <a href="/search/astro-ph?searchtype=author&query=Magdis%2C+G+E">G. E. Magdis</a>, <a href="/search/astro-ph?searchtype=author&query=Magnelli%2C+B">B. Magnelli</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">R. Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">E. Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Franco%2C+M">M. Franco</a>, <a href="/search/astro-ph?searchtype=author&query=Whitaker%2C+K">K. Whitaker</a>, <a href="/search/astro-ph?searchtype=author&query=Valentino%2C+F">F. Valentino</a>, <a href="/search/astro-ph?searchtype=author&query=Adscheid%2C+S">S. Adscheid</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">E. Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Zanella%2C+A">A. Zanella</a>, <a href="/search/astro-ph?searchtype=author&query=Xiao%2C+M">M. Xiao</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+T">T. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+D">D. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Kokorev%2C+V">V. Kokorev</a>, <a href="/search/astro-ph?searchtype=author&query=Elbaz%2C+D">D. Elbaz</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="2303.12110v1-abstract-short" style="display: inline;"> We present a 1.1mm stacking analysis of moderately massive (log($M_{*}$/$M_{\odot}$) = 10.7 $\pm$ 0.2) quiescent galaxies (QGs) at $\langle z\rangle \sim1.5$, searching for cold dust continuum emission, an excellent tracer of dust and gas mass. Using both the recent GOODS-ALMA survey as well as the full suite of ALMA Band-6 ancillary data in the GOODS-S field, we report the tentative detection of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.12110v1-abstract-full').style.display = 'inline'; document.getElementById('2303.12110v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.12110v1-abstract-full" style="display: none;"> We present a 1.1mm stacking analysis of moderately massive (log($M_{*}$/$M_{\odot}$) = 10.7 $\pm$ 0.2) quiescent galaxies (QGs) at $\langle z\rangle \sim1.5$, searching for cold dust continuum emission, an excellent tracer of dust and gas mass. Using both the recent GOODS-ALMA survey as well as the full suite of ALMA Band-6 ancillary data in the GOODS-S field, we report the tentative detection of dust continuum equivalent of dust mass log($M_{dust}$/$M_{\odot}$) = 7.47 $\pm$ 0.13 and gas mass log($M_{gas}$/$M_{\odot}$) = 9.42 $\pm$ 0.14. The emerging gas fraction is $f_{gas}$ = 5.3 $\pm$ 1.8%, consistent with the results of previous stacking analyses based on lower resolution sub(mm) observations. Our results support the scenario where high-z QGs have an order of magnitude larger $f_{gas}$ compared to their local counterparts and have experienced quenching with a non negligible gas reservoir in their interstellar medium - i.e. with gas retention. Subsequent analysis yields an anti-correlation between the $f_{gas}$ and the stellar mass of QGs, especially in the high mass end where galaxies reside in the most massive haloes. The $f_{gas}$ - $M_{*}$ anti-correlation promotes the selection bias as a possible solution to the tension between the stacking results pointing towards gas retention in high-z QGs of moderate $M_{*}$ and the studies of individual targets that favour a fully depleted ISM in massive (log($M_{*}$/$M_{\odot}$) high-z QGs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.12110v1-abstract-full').style.display = 'none'; document.getElementById('2303.12110v1-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">Accepted to A&A on the 16/03/2023</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 674, A166 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.09372">arXiv:2212.09372</a> <span> [<a href="https://arxiv.org/pdf/2212.09372">pdf</a>, <a href="https://arxiv.org/format/2212.09372">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/10.1051/0004-6361/202245724">10.1051/0004-6361/202245724 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Massive galaxy formation caught in action at z~5 with JWST </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jin%2C+S">Shuowen Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Sillassen%2C+N+B">Nikolaj B. Sillassen</a>, <a href="/search/astro-ph?searchtype=author&query=Magdis%2C+G+E">Georgios E. Magdis</a>, <a href="/search/astro-ph?searchtype=author&query=Vijayan%2C+A+P">Aswin P. Vijayan</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G+B">Gabriel B. Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Kokorev%2C+V">Vasily Kokorev</a>, <a href="/search/astro-ph?searchtype=author&query=Weaver%2C+J+R">John R. Weaver</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">Raphael Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Gim%C3%A9nez-Arteaga%2C+C">Clara Gim茅nez-Arteaga</a>, <a href="/search/astro-ph?searchtype=author&query=Valentino%2C+F">Francesco Valentino</a>, <a href="/search/astro-ph?searchtype=author&query=Brinch%2C+M">Malte Brinch</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%B3mez-Guijarro%2C+C">Carlos G贸mez-Guijarro</a>, <a href="/search/astro-ph?searchtype=author&query=Shuntov%2C+M">Marko Shuntov</a>, <a href="/search/astro-ph?searchtype=author&query=Toft%2C+S">Sune Toft</a>, <a href="/search/astro-ph?searchtype=author&query=Greve%2C+T+R">Thomas R. Greve</a>, <a href="/search/astro-ph?searchtype=author&query=Sese%2C+D+B">David Blanquez Sese</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="2212.09372v3-abstract-short" style="display: inline;"> We report the discovery of a compact group of galaxies, CGG-z5, at z~5.2 in the EGS field covered by the JWST/CEERS survey. CGG-z5 was selected as the highest overdensity of galaxies at z>2 in recent JWST public surveys and it consists of six candidate members lying within a projected area of $1.5"\times3"$ (10$\times$20~kpc$^2$). All group members are HST/F435W and HST/F606W dropouts while secure… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.09372v3-abstract-full').style.display = 'inline'; document.getElementById('2212.09372v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.09372v3-abstract-full" style="display: none;"> We report the discovery of a compact group of galaxies, CGG-z5, at z~5.2 in the EGS field covered by the JWST/CEERS survey. CGG-z5 was selected as the highest overdensity of galaxies at z>2 in recent JWST public surveys and it consists of six candidate members lying within a projected area of $1.5"\times3"$ (10$\times$20~kpc$^2$). All group members are HST/F435W and HST/F606W dropouts while securely detected in the JWST/NIRCam bands, yielding a narrow range of robust photometric redshifts $5.0<z<5.3$. The most massive galaxy in the group has a stellar mass log$(M_{*}/M_{\odot})\approx9.8$, while the rest are low-mass satellites (log$(M_{*}/M_{\odot})\approx8.4-9.2$). While several group members were already detected in the HST and IRAC bands, the low stellar masses and the compactness of the structure required the sensitivity and resolution of JWST for its identification. To assess the nature and evolutionary path of CGG-z5, we searched for similar compact structures in the \textsc{Eagle} simulations and followed their evolution with time. We find that all the identified structures merge into a single galaxy by z=3 and form a massive galaxy (log$(M_{*}/M_{\odot})>11$) at z~1. This implies that CGG-z5 could be a "proto-massive galaxy" captured during a short-lived phase of massive galaxy formation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.09372v3-abstract-full').style.display = 'none'; document.getElementById('2212.09372v3-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 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published in A&A Letter</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 670, L11 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.00841">arXiv:2212.00841</a> <span> [<a href="https://arxiv.org/pdf/2212.00841">pdf</a>, <a href="https://arxiv.org/format/2212.00841">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/10.1051/0004-6361/202245070">10.1051/0004-6361/202245070 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> VST-GAME: Galaxy Assembly as a function of Mass and Environment with VST. Photometric assessment and density field of MACSJ0416 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Estrada%2C+N">Nicolas Estrada</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">Amata Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Vulcani%2C+B">Benedetta Vulcani</a>, <a href="/search/astro-ph?searchtype=author&query=Rodighiero%2C+G">Giulia Rodighiero</a>, <a href="/search/astro-ph?searchtype=author&query=Nonino%2C+M">Mario Nonino</a>, <a href="/search/astro-ph?searchtype=author&query=Annunziatella%2C+M">Marianna Annunziatella</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">Piero Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">Claudio Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Caminha%2C+G+B">Gabriel Bartosch Caminha</a>, <a href="/search/astro-ph?searchtype=author&query=Angora%2C+G">Giuseppe Angora</a>, <a href="/search/astro-ph?searchtype=author&query=Biviano%2C+A">Andrea Biviano</a>, <a href="/search/astro-ph?searchtype=author&query=Brescia%2C+M">Massimo Brescia</a>, <a href="/search/astro-ph?searchtype=author&query=De+Lucia%2C+G">Gabriella De Lucia</a>, <a href="/search/astro-ph?searchtype=author&query=Demarco%2C+R">Ricardo Demarco</a>, <a href="/search/astro-ph?searchtype=author&query=Girardi%2C+M">Marisa Girardi</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">Raphael Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Lemaux%2C+B+C">Brian C. Lemaux</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="2212.00841v2-abstract-short" style="display: inline;"> Observational studies have widely demonstrated that galaxy physical properties are strongly affected by the surrounding environment. On one side, gas inflows provide galaxies with new fuel for star formation. On the other side, the high temperatures and densities of the medium are expected to induce quenching in the star formation. Observations of large structures, in particular filaments at the c… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.00841v2-abstract-full').style.display = 'inline'; document.getElementById('2212.00841v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.00841v2-abstract-full" style="display: none;"> Observational studies have widely demonstrated that galaxy physical properties are strongly affected by the surrounding environment. On one side, gas inflows provide galaxies with new fuel for star formation. On the other side, the high temperatures and densities of the medium are expected to induce quenching in the star formation. Observations of large structures, in particular filaments at the cluster outskirts (r>2r$_{200}$), are currently limited to the low redshift Universe. We present a multi-band dataset for the cluster MACS J0416.1-2403 (z=0.397), observed in the context of the Galaxy Assembly as a function of Mass and Environment with VST (VST-GAME) survey. The project aims at gathering deep ($r$<24.4) and wide (20x20Mpc$^2$) observations at optical wavelengths for six massive galaxy clusters at 0.2<z<0.6, complemented with near infrared data. This work describes the photometric analysis of the cluster, defines a density field and studies galaxy properties in the cluster outskirts. We extract sources paying particular attention to recover the faintest ones. We combine all the extractions in a multi-band catalog and compute photometric redshifts. We then define cluster memberships up to 5r$_{200}$ from the cluster core and measure the density field, comparing galaxy properties in different environments. We found that the $g-r$ colors show bimodal behaviours in all the environments, but the peak of the distribution of red galaxies shifts toward redder colors with increasing density and the fraction of galaxies in the blue cloud increases with decreasing density. We also found 3 overdense regions in the cluster outskirts at r$\sim$5r$_{200}$. The color of galaxies suggests the presence of evolved galaxy populations, an insight for pre-processing phenomena over these substructures. We release the multi-band catalog, down to the completeness limit $r$<24.4 mag. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.00841v2-abstract-full').style.display = 'none'; document.getElementById('2212.00841v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 15 figures and 5 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 671, A146 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.14131">arXiv:2211.14131</a> <span> [<a href="https://arxiv.org/pdf/2211.14131">pdf</a>, <a href="https://arxiv.org/format/2211.14131">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/10.1051/0004-6361/202244995">10.1051/0004-6361/202244995 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The uncertain interstellar medium of high-redshift quiescent galaxies: Impact of methodology </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">Rapha毛l Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Eugenio%2C+C">Chiara D'Eugenio</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+D">Daizhong Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Caminha%2C+G+B">Gabriel Bartosch Caminha</a>, <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">Emanuele Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Bl%C3%A1nquez%2C+D">David Bl谩nquez</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="2211.14131v1-abstract-short" style="display: inline;"> How much gas and dust is contained in high-redshift quiescent galaxies (QGs) is currently an open question with relatively few and contradictory answers, as well as important implications for our understanding of the nature of star formation quenching processes at cosmic noon. Here we revisit far-infrared (FIR) observations of the REQUIEM-ALMA sample of six z = 1.6 - 3.2 QGs strongly lensed by int… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.14131v1-abstract-full').style.display = 'inline'; document.getElementById('2211.14131v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.14131v1-abstract-full" style="display: none;"> How much gas and dust is contained in high-redshift quiescent galaxies (QGs) is currently an open question with relatively few and contradictory answers, as well as important implications for our understanding of the nature of star formation quenching processes at cosmic noon. Here we revisit far-infrared (FIR) observations of the REQUIEM-ALMA sample of six z = 1.6 - 3.2 QGs strongly lensed by intermediate-redshift galaxy clusters. We measured their continuum emission using priors obtained from high resolution near-infrared (NIR) imaging, as opposed to focusing on point-source extraction, converted it into dust masses using a FIR dust emission model derived from statistical samples of QGs, and compared the results to those of the reference work. We find that, while at least the most massive sample galaxy is indeed dust-poor, the picture is much more nuanced than previously reported. In particular, these more conservative constraints remain consistent with high dust fractions in early QGs. We find that these measurements are very sensitive to the adopted extraction method and conversion factors: the use of an extended light model to fit the FIR emission increases the flux of detections by up to 50% and the upper limit by up to a factor 6. Adding the FIR-to-dust conversion, this amounts to an order of magnitude difference in dust fraction, casting doubts on the power of these data to discriminate between star formation quenching scenarios. Unless these are identified by other means, mapping the dust and gas in high-redshift QGs will continue to require somewhat costly observations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.14131v1-abstract-full').style.display = 'none'; document.getElementById('2211.14131v1-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 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">7 pages, 5 figures, 2 tables; accepted for publication in Astronomy & Astrophysics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.15467">arXiv:2209.15467</a> <span> [<a href="https://arxiv.org/pdf/2209.15467">pdf</a>, <a href="https://arxiv.org/format/2209.15467">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/10.1051/0004-6361/202244337">10.1051/0004-6361/202244337 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The 700 ks Chandra Spiderweb Field II: Evidence for inverse-Compton and thermal diffuse emission in the Spiderweb galaxy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Tozzi%2C+P">P. Tozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">R. Gilli</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+A">A. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Borgani%2C+S">S. Borgani</a>, <a href="/search/astro-ph?searchtype=author&query=Lepore%2C+M">M. Lepore</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Mascolo%2C+L">L. Di Mascolo</a>, <a href="/search/astro-ph?searchtype=author&query=Saro%2C+A">A. Saro</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">L. Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Carilli%2C+C">C. Carilli</a>, <a href="/search/astro-ph?searchtype=author&query=Miley%2C+G">G. Miley</a>, <a href="/search/astro-ph?searchtype=author&query=Mroczkowski%2C+T">T. Mroczkowski</a>, <a href="/search/astro-ph?searchtype=author&query=Pannella%2C+M">M. Pannella</a>, <a href="/search/astro-ph?searchtype=author&query=Rasia%2C+E">E. Rasia</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+C+S">C. S. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Calabro%27%2C+A">A. Calabro'</a>, <a href="/search/astro-ph?searchtype=author&query=Churazov%2C+E">E. Churazov</a>, <a href="/search/astro-ph?searchtype=author&query=Dannerbauer%2C+H">H. Dannerbauer</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=Gobat%2C+R">R. Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+S">S. Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Nonino%2C+M">M. Nonino</a>, <a href="/search/astro-ph?searchtype=author&query=Norman%2C+C">C. Norman</a>, <a href="/search/astro-ph?searchtype=author&query=Rottgering%2C+H+J+A">H. J. A. Rottgering</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="2209.15467v1-abstract-short" style="display: inline;"> We present the X-ray imaging and spectral analysis of the diffuse emission around the Spiderweb galaxy at z=2.16 and of its nuclear emission, based on a deep (700 ks) Chandra observation. We characterize the nuclear emission and computed the contamination in the surrounding regions due to the wings of the instrument PSF. Then, we quantified the extended emission within 12". We find that the Spider… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.15467v1-abstract-full').style.display = 'inline'; document.getElementById('2209.15467v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.15467v1-abstract-full" style="display: none;"> We present the X-ray imaging and spectral analysis of the diffuse emission around the Spiderweb galaxy at z=2.16 and of its nuclear emission, based on a deep (700 ks) Chandra observation. We characterize the nuclear emission and computed the contamination in the surrounding regions due to the wings of the instrument PSF. Then, we quantified the extended emission within 12". We find that the Spiderweb galaxy hosts a mildly absorbed quasar, with modest yet significant variability on a timescale of ~1 year. We find that the emission in the jet regions is well described by a power law with Gamma~2-2.5, and it is consistent with IC upscattering of the CMB photons by the relativistic electrons. We also find a roughly symmetric, diffuse emission within a radius of ~100 kpc. This emission is consistent with thermal bremsstrahlung from a hot ICM with a temperature of kT=2.0_{-0.4}^{+0.7} keV, and a metallicity of Z<1.6Z_sun. The average electron density within 100 kpc is n_e=(1.51+-0.24+-0.14)E-2 cm^{-3}, corresponding to an upper limit for the total ICM mass of <=(1.76+-0.30+-0.17)E+12 M_sun (where error bars are 1 sigma statistical and systematic, respectively). If we apply hydrostatic equilibrium to the ICM, we measure a total gravitational mass M(<100 kpc)=(1.5^{+0.5}_{-0.3})E+13 M_sun and, extrapolating at larger radii, we estimate a total mass M_{500}=(3.2^{+1.1}_{-0.6})E+13 M_sun within a radius of r_{500}=(220+-30) kpc. We conclude that the Spiderweb protocluster shows significant diffuse emission within a radius of 12 arcsec, whose major contribution is provided by IC scattering associated with the radio jets. Outside the jet regions, we also identified thermal emission within a radius of ~100 kpc, revealing the presence of hot, diffuse baryons that may represent the embryonic virialized halo of the forming cluster. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.15467v1-abstract-full').style.display = 'none'; document.getElementById('2209.15467v1-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 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">19 pages, 16 figures, accepted in Astronomy & Astrophysics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.05895">arXiv:2209.05895</a> <span> [<a href="https://arxiv.org/pdf/2209.05895">pdf</a>, <a href="https://arxiv.org/format/2209.05895">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/10.1051/0004-6361/202244661">10.1051/0004-6361/202244661 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A galaxy group candidate at z~3.7 in the COSMOS field </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sillassen%2C+N+B">Nikolaj Bjerregaard Sillassen</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+S">Shuowen Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Magdis%2C+G+E">Georgios E. Magdis</a>, <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">Emanuele Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Weaver%2C+J+R">John R. Weaver</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">Raphael Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Kokorev%2C+V">Vasily Kokorev</a>, <a href="/search/astro-ph?searchtype=author&query=Valentino%2C+F">Francesco Valentino</a>, <a href="/search/astro-ph?searchtype=author&query=Finoguenov%2C+A">Alexis Finoguenov</a>, <a href="/search/astro-ph?searchtype=author&query=Shuntov%2C+M">Marko Shuntov</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%B3mez-Guijarro%2C+C">Carlos G贸mez-Guijarro</a>, <a href="/search/astro-ph?searchtype=author&query=Coogan%2C+R">Rosemary Coogan</a>, <a href="/search/astro-ph?searchtype=author&query=Greve%2C+T+R">Thomas R. Greve</a>, <a href="/search/astro-ph?searchtype=author&query=Toft%2C+S">Sune Toft</a>, <a href="/search/astro-ph?searchtype=author&query=Sese%2C+D+B">David B. Sese</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="2209.05895v1-abstract-short" style="display: inline;"> We report a galaxy group candidate HPC1001 at $z\approx3.7$ in the COSMOS field. This structure was selected as a high galaxy overdensity at $z>3$ in the COSMOS2020 catalog. It contains ten candidate members, of which eight are assembled in a $10''\times10''$ area with the highest sky density among known protoclusters and groups at $z>3$. Four out of ten sources were also detected at 1.2$~$mm with… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.05895v1-abstract-full').style.display = 'inline'; document.getElementById('2209.05895v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.05895v1-abstract-full" style="display: none;"> We report a galaxy group candidate HPC1001 at $z\approx3.7$ in the COSMOS field. This structure was selected as a high galaxy overdensity at $z>3$ in the COSMOS2020 catalog. It contains ten candidate members, of which eight are assembled in a $10''\times10''$ area with the highest sky density among known protoclusters and groups at $z>3$. Four out of ten sources were also detected at 1.2$~$mm with Atacama Large Millimeter Array continuum observations. Photometric redshifts, measured by four independent methods, fall within a narrow range of $3.5<z<3.9$ and with a weighted average of $z=3.65\pm0.07$. The integrated far-IR-to-radio spectral energy distribution yields a total UV and IR star formation rate ${\rm SFR}\approx 900~M_{\odot}~yr^{-1}$. We also estimated a halo mass of $\sim10^{13}~M_\odot$ for the structure, which at this redshift is consistent with potential cold gas inflow. Remarkably, the most massive member has a specific star formation rate and dust to stellar mass ratio of $M_{\rm dust}/M_{*}$ that are both significantly lower than that of star-forming galaxies at this redshift, suggesting that HPC1001 could be a $z\approx3.7$ galaxy group in maturing phase. If confirmed, this would be the earliest structure in maturing phase to date, and an ideal laboratory to study the formation of the earliest quiescent galaxies as well as cold gas accretion in dense environments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.05895v1-abstract-full').style.display = 'none'; document.getElementById('2209.05895v1-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 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">A&A Letter in press</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 665, L7 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.07909">arXiv:2205.07909</a> <span> [<a href="https://arxiv.org/pdf/2205.07909">pdf</a>, <a href="https://arxiv.org/format/2205.07909">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/10.1051/0004-6361/202142843">10.1051/0004-6361/202142843 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Starbursts with suppressed velocity dispersion revealed in a forming cluster at z=2.51 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Xiao%2C+M">Mengyuan Xiao</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+T">Tao Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Elbaz%2C+D">David Elbaz</a>, <a href="/search/astro-ph?searchtype=author&query=Iono%2C+D">Daisuke Iono</a>, <a href="/search/astro-ph?searchtype=author&query=Lu%2C+X">Xing Lu</a>, <a href="/search/astro-ph?searchtype=author&query=Bing%2C+L">Longji Bing</a>, <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">Emanuele Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Magnelli%2C+B">Benjamin Magnelli</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%B3mez-Guijarro%2C+C">Carlos G贸mez-Guijarro</a>, <a href="/search/astro-ph?searchtype=author&query=Bournaud%2C+F">Frederic Bournaud</a>, <a href="/search/astro-ph?searchtype=author&query=Gu%2C+Q">Qiusheng Gu</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+S">Shuowen Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Valentino%2C+F">Francesco Valentino</a>, <a href="/search/astro-ph?searchtype=author&query=Zanella%2C+A">Anita Zanella</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">Raphael Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+S">Sergio Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G">Gabriel Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Kohno%2C+K">Kotaro Kohno</a>, <a href="/search/astro-ph?searchtype=author&query=Schreiber%2C+C">Corentin Schreiber</a>, <a href="/search/astro-ph?searchtype=author&query=Ciesla%2C+L">Laure Ciesla</a>, <a href="/search/astro-ph?searchtype=author&query=Yu%2C+X">Xiaoling Yu</a>, <a href="/search/astro-ph?searchtype=author&query=Okumura%2C+K">Koryo Okumura</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="2205.07909v1-abstract-short" style="display: inline;"> One of the most prominent features of galaxy clusters is the presence of a dominant population of massive ellipticals in their cores. Stellar archaeology suggests that these gigantic beasts assembled most of their stars in the early Universe via starbursts. However, the role of dense environments and their detailed physical mechanisms in triggering starburst activities remain unknown. Here we repo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.07909v1-abstract-full').style.display = 'inline'; document.getElementById('2205.07909v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.07909v1-abstract-full" style="display: none;"> One of the most prominent features of galaxy clusters is the presence of a dominant population of massive ellipticals in their cores. Stellar archaeology suggests that these gigantic beasts assembled most of their stars in the early Universe via starbursts. However, the role of dense environments and their detailed physical mechanisms in triggering starburst activities remain unknown. Here we report spatially resolved Atacama Large Millimeter/submillimeter Array (ALMA) observations of the CO $J= 3-2$ emission line, with a resolution of about 2.5 kiloparsecs, toward a forming galaxy cluster core with starburst galaxies at $z=2.51$. In contrast to starburst galaxies in the field often associated with galaxy mergers or highly turbulent gaseous disks, our observations show that the two starbursts in the cluster exhibit dynamically cold (rotation-dominated) gas-rich disks. Their gas disks have extremely low velocity dispersion ($蟽_{\mathrm{0}} \sim 20-30$ km s$^{-1}$), which is three times lower than their field counterparts at similar redshifts. The high gas fraction and suppressed velocity dispersion yield gravitationally unstable gas disks, which enables highly efficient star formation. The suppressed velocity dispersion, likely induced by the accretion of corotating and coplanar cold gas, might serve as an essential avenue to trigger starbursts in massive halos at high redshifts. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.07909v1-abstract-full').style.display = 'none'; document.getElementById('2205.07909v1-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 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">19 pages, 14 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 664, A63 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.02208">arXiv:2203.02208</a> <span> [<a href="https://arxiv.org/pdf/2203.02208">pdf</a>, <a href="https://arxiv.org/format/2203.02208">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/10.1051/0004-6361/202142333">10.1051/0004-6361/202142333 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The 700 ks Chandra Spiderweb Field I: evidence for widespread nuclear activity in the Protocluster </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Tozzi%2C+P">P. Tozzi</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=Pannella%2C+M">M. Pannella</a>, <a href="/search/astro-ph?searchtype=author&query=Fiore%2C+F">F. Fiore</a>, <a href="/search/astro-ph?searchtype=author&query=Miley%2C+G">G. Miley</a>, <a href="/search/astro-ph?searchtype=author&query=Nonino%2C+M">M. Nonino</a>, <a href="/search/astro-ph?searchtype=author&query=Rottgering%2C+H+J+A">H. J. A. Rottgering</a>, <a href="/search/astro-ph?searchtype=author&query=Strazzullo%2C+V">V. Strazzullo</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+C+S">C. S. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Borgani%2C+S">S. Borgani</a>, <a href="/search/astro-ph?searchtype=author&query=Calabro%27%2C+A">A. Calabro'</a>, <a href="/search/astro-ph?searchtype=author&query=Carilli%2C+C">C. Carilli</a>, <a href="/search/astro-ph?searchtype=author&query=Dannerbauer%2C+H">H. Dannerbauer</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Mascolo%2C+L">L. Di Mascolo</a>, <a href="/search/astro-ph?searchtype=author&query=Feruglio%2C+C">C. Feruglio</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">R. Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+S">S. Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+A">A. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Mroczkowski%2C+T">T. Mroczkowski</a>, <a href="/search/astro-ph?searchtype=author&query=Norman%2C+C">C. Norman</a>, <a href="/search/astro-ph?searchtype=author&query=Rasia%2C+E">E. Rasia</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Saro%2C+A">A. Saro</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="2203.02208v2-abstract-short" style="display: inline;"> (Abridged) We present an analysis of the 700 ks Chandra ACIS-S observation of the field around the Spiderweb Galaxy at z=2.156, focusing on the nuclear activity in the associated large-scale environment. We identify unresolved X-ray sources down to flux limits of 1.3X10^{-16} and 3.9X10^{-16} erg/s/cm^2 in the soft and hard band, respectively. We search for counterparts in the optical, NIR and sub… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.02208v2-abstract-full').style.display = 'inline'; document.getElementById('2203.02208v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.02208v2-abstract-full" style="display: none;"> (Abridged) We present an analysis of the 700 ks Chandra ACIS-S observation of the field around the Spiderweb Galaxy at z=2.156, focusing on the nuclear activity in the associated large-scale environment. We identify unresolved X-ray sources down to flux limits of 1.3X10^{-16} and 3.9X10^{-16} erg/s/cm^2 in the soft and hard band, respectively. We search for counterparts in the optical, NIR and submm bands to identify X-ray sources belonging to the protocluster. We detect 107 X-ray unresolved sources within 5 arcmin (corresponding to 2.5 Mpc) of J1140-2629, among which 13 have optical counterparts with spectroscopic redshift 2.11<z<2.20, and 1 source with photometric redshift consistent with this range. Our X-ray spectral analysis shows that their intrinsic spectral slope is consistent with an average <螕>~1.84+-0.04. The best-fit intrinsic absorption for 5 protocluster X-ray members is N_H>10^{23} cm^{-2}, while other 6 have upper limits of the order of fewX10^{22} cm^{-2}. Two sources can only be fitted with very flat 螕<=1, and are therefore considered Compton-thick candidates. Their 0.5-10 keV rest frame luminosities are larger than 2X10^{43} erg/s, significantly greater than X-ray luminosities expected from star formation activity. The X-ray luminosity function of AGN in the volume associated to the Spiderweb protocluster in the range 10^{43}<L_X<10^{44.5} erg/s, is at least 10 times higher than that in the field at the same redshift and significantly flatter. The X-ray AGN fraction is measured to be (25.5+-4.5)% in the stellar mass range log(M*/M_sun)>10.5, corresponding to an enhancement of 6.0^{+9.0}_{-3.0} with respect to the COSMOS field at comparable redshifts and stellar mass range. We conclude that the galaxy population in the Spiderweb Protocluster is characterized by enhanced X-ray nuclear activity triggered by environmental effects on Mpc scales. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.02208v2-abstract-full').style.display = 'none'; document.getElementById('2203.02208v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">Astronomy & Astrophysics. Minor changes in this version. Version accepted 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 662, A54 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2202.03715">arXiv:2202.03715</a> <span> [<a href="https://arxiv.org/pdf/2202.03715">pdf</a>, <a href="https://arxiv.org/format/2202.03715">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/ac531f">10.3847/2041-8213/ac531f <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Evidence for Cold-stream to Hot-accretion Transition as Traced by Ly伪 Emission from Groups and Clusters at 2 < z < 3.3 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">E. Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Rich%2C+R+M">R. M. Rich</a>, <a href="/search/astro-ph?searchtype=author&query=Valentino%2C+F">F. Valentino</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+S">S. Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Delvecchio%2C+I">I. Delvecchio</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+D">D. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Strazzullo%2C+V">V. Strazzullo</a>, <a href="/search/astro-ph?searchtype=author&query=Neill%2C+J">J. Neill</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">R. Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Finoguenov%2C+A">A. Finoguenov</a>, <a href="/search/astro-ph?searchtype=author&query=Bournaud%2C+F">F. Bournaud</a>, <a href="/search/astro-ph?searchtype=author&query=Elbaz%2C+D">D. Elbaz</a>, <a href="/search/astro-ph?searchtype=author&query=Kalita%2C+B+S">B. S. Kalita</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Sullivan%2C+D">D. O'Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+T">T. Wang</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="2202.03715v2-abstract-short" style="display: inline;"> We present Keck Cosmic Web Imager (KCWI) observations of giant Lya halos surrounding 9 galaxy groups and clusters at 2<z<3.3, including five new detections and one upper limit. We find observational evidence for the cold-stream to hot-accretion transition predicted by theory by measuring a decrease in the ratio between the spatially extended Lya luminosity and the expected baryonic accretion rate… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.03715v2-abstract-full').style.display = 'inline'; document.getElementById('2202.03715v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.03715v2-abstract-full" style="display: none;"> We present Keck Cosmic Web Imager (KCWI) observations of giant Lya halos surrounding 9 galaxy groups and clusters at 2<z<3.3, including five new detections and one upper limit. We find observational evidence for the cold-stream to hot-accretion transition predicted by theory by measuring a decrease in the ratio between the spatially extended Lya luminosity and the expected baryonic accretion rate (BAR), with increasing elongation above the transition mass Mstream). This implies a modulation of the share of BAR that remains cold diminishing quasi-linearly (logarithmic slope of 0.97+-0.19, 5 sigma significance) with the halo to Mstream mass ratio. The integrated star-formation rates (SFRs) and AGN bolometric luminosities display a potentially consistent decrease, albeit significant only at 2.6 sigma and 1.3 sigma, respectively. The higher scatter in these tracers suggests the Lya emission might be mostly a direct product of cold accretion in these structures rather than indirect, mediated by outflows and photo-ionization from SFR and AGNs; this is also supported by energetics considerations. Below Mstream (cold-stream regime) we measure LLya/BAR=10^{40.51+-0.16}~erg/s/Msun*yr, consistent with predictions, and SFR/BAR=10^{-0.54+-0.23}: on average 30_{-10}^{+20}% of the cold streams go into stars. Above Mstream (hot-accretion regime), LLya is set by Mstream (within 0.2~dex scatter in our sample), independent of the halo mass but rising tenfold from z=2 to 3. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.03715v2-abstract-full').style.display = 'none'; document.getElementById('2202.03715v2-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 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 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">ApJ Letters</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal Letters, Volume 926, Issue 2, id.L21, 7 pp. 2022 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.09068">arXiv:2201.09068</a> <span> [<a href="https://arxiv.org/pdf/2201.09068">pdf</a>, <a href="https://arxiv.org/format/2201.09068">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/stac3450">10.1093/mnras/stac3450 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Massive quiescent galaxies at $z\sim3$: a comparison of selection, stellar population and structural properties with simulation predictions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lustig%2C+P">Peter Lustig</a>, <a href="/search/astro-ph?searchtype=author&query=Strazzullo%2C+V">Veronica Strazzullo</a>, <a href="/search/astro-ph?searchtype=author&query=Remus%2C+R">Rhea-Silvia Remus</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Eugenio%2C+C">Chiara D'Eugenio</a>, <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">Emanuele Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Burkert%2C+A">Andreas Burkert</a>, <a href="/search/astro-ph?searchtype=author&query=De+Lucia%2C+G">Gabriella De Lucia</a>, <a href="/search/astro-ph?searchtype=author&query=Delvecchio%2C+I">Ivan Delvecchio</a>, <a href="/search/astro-ph?searchtype=author&query=Dolag%2C+K">Klaus Dolag</a>, <a href="/search/astro-ph?searchtype=author&query=Fontanot%2C+F">Fabio Fontanot</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">Raphael Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Mohr%2C+J+J">Joseph J. Mohr</a>, <a href="/search/astro-ph?searchtype=author&query=Onodera%2C+M">Masato Onodera</a>, <a href="/search/astro-ph?searchtype=author&query=Pannella%2C+M">Maurilio Pannella</a>, <a href="/search/astro-ph?searchtype=author&query=Pillepich%2C+A">Annalisa Pillepich</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="2201.09068v2-abstract-short" style="display: inline;"> We study stellar population and structural properties of massive $\log(M_{\star} / M_{\odot}) >11$ galaxies at $z\sim 2.7$ in the Magneticum and IllustrisTNG hydrodynamical simulations and GAEA semi-analytic model. We find stellar mass functions broadly consistent with observations, with no scarcity of massive, quiescent galaxies at $z\sim 2.7$, but with a higher quiescent galaxy fraction at high… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.09068v2-abstract-full').style.display = 'inline'; document.getElementById('2201.09068v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.09068v2-abstract-full" style="display: none;"> We study stellar population and structural properties of massive $\log(M_{\star} / M_{\odot}) >11$ galaxies at $z\sim 2.7$ in the Magneticum and IllustrisTNG hydrodynamical simulations and GAEA semi-analytic model. We find stellar mass functions broadly consistent with observations, with no scarcity of massive, quiescent galaxies at $z\sim 2.7$, but with a higher quiescent galaxy fraction at high masses in IllustrisTNG. Average ages of simulated quiescent galaxies are between $\sim 0.8$ and 1.0 Gyr, older by a factor $\sim 2$ than observed in spectroscopically-confirmed quiescent galaxies at similar redshift. Besides being potentially indicative of limitations of simulations in reproducing observed star formation histories, this discrepancy may also reflect limitations in the estimation of observed ages. We investigate the purity of simulated UVJ rest-frame color-selected massive quiescent samples with photometric uncertainties typical of deep surveys (e.g., COSMOS). We find evidence for significant contamination (up to 60 percent) by dusty star-forming galaxies in the UVJ region that is typically populated by older quiescent sources. Furthermore, the completeness of UVJ-selected quiescent samples at this redshift may be reduced by 30 percent due to a high fraction of young quiescent galaxies not entering the UVJ quiescent region. Massive, quiescent galaxies in simulations have on average lower angular momenta and higher projected axis ratios and concentrations than star-forming counterparts. Average sizes of simulated quiescent galaxies are broadly consistent with observations within the uncertainties. The average size ratio of quiescent and star-forming galaxies in the probed mass range is formally consistent with observations, although this result is partly affected by poor statistics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.09068v2-abstract-full').style.display = 'none'; document.getElementById('2201.09068v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 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">23 pages, 9 figures. Submitted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.08926">arXiv:2109.08926</a> <span> [<a href="https://arxiv.org/pdf/2109.08926">pdf</a>, <a href="https://arxiv.org/format/2109.08926">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="Earth and Planetary Astrophysics">astro-ph.EP</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/ac2829">10.3847/1538-4357/ac2829 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Panspermia in a Milky Way-like Galaxy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">Raphael Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Hong%2C+S+E">Sungwook E. Hong</a>, <a href="/search/astro-ph?searchtype=author&query=Snaith%2C+O">Owain Snaith</a>, <a href="/search/astro-ph?searchtype=author&query=Hong%2C+S">Sungryong Hong</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="2109.08926v1-abstract-short" style="display: inline;"> We study the process of panspermia in Milky Way-like galaxies by modeling the probability of successful travel of organic compounds between stars harboring potentially habitable planets. To this end, we apply the modified habitability recipe of Gobat & Hong (2016) to a model galaxy from the MUGS suite of zoom-in cosmological simulations. We find that, unlike habitability, which only occupies narro… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.08926v1-abstract-full').style.display = 'inline'; document.getElementById('2109.08926v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.08926v1-abstract-full" style="display: none;"> We study the process of panspermia in Milky Way-like galaxies by modeling the probability of successful travel of organic compounds between stars harboring potentially habitable planets. To this end, we apply the modified habitability recipe of Gobat & Hong (2016) to a model galaxy from the MUGS suite of zoom-in cosmological simulations. We find that, unlike habitability, which only occupies narrow dynamic range over the entire galaxy, the panspermia probability can vary be orders of magnitude between the inner ($R, b = 1-4 {\rm kpc}$) and outer disk. However, only a small fraction of star particles have very large values of panspermia probability and, consequently, the fraction of star particles where the panspermia process is more effective than prebiotic evolution is much lower than from na茂ve expectations based on the ratio between panspermia probability and natural habitability. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.08926v1-abstract-full').style.display = 'none'; document.getElementById('2109.08926v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 18 figures, ApJ 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/2109.03842">arXiv:2109.03842</a> <span> [<a href="https://arxiv.org/pdf/2109.03842">pdf</a>, <a href="https://arxiv.org/format/2109.03842">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202141417">10.1051/0004-6361/202141417 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The effect of active galactic nuclei on the cold interstellar medium in distant star-forming galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Valentino%2C+F">Francesco Valentino</a>, <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">Emanuele Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Puglisi%2C+A">Annagrazia Puglisi</a>, <a href="/search/astro-ph?searchtype=author&query=Magdis%2C+G+E">Georgios E. Magdis</a>, <a href="/search/astro-ph?searchtype=author&query=Kokorev%2C+V">Vasily Kokorev</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+D">Daizhong Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Madden%2C+S+C">Suzanne C. Madden</a>, <a href="/search/astro-ph?searchtype=author&query=Gomez-Guijarro%2C+C">Carlos Gomez-Guijarro</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+M">Min-Young Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Cortzen%2C+I">Isabella Cortzen</a>, <a href="/search/astro-ph?searchtype=author&query=Circosta%2C+C">Chiara Circosta</a>, <a href="/search/astro-ph?searchtype=author&query=Delvecchio%2C+I">Ivan Delvecchio</a>, <a href="/search/astro-ph?searchtype=author&query=Mullaney%2C+J+R">James R. Mullaney</a>, <a href="/search/astro-ph?searchtype=author&query=Gao%2C+Y">Yu Gao</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">Raphael Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Aravena%2C+M">Manuel Aravena</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+S">Shuowen Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Fujimoto%2C+S">Seiji Fujimoto</a>, <a href="/search/astro-ph?searchtype=author&query=Silverman%2C+J+D">John D. Silverman</a>, <a href="/search/astro-ph?searchtype=author&query=Dannerbauer%2C+H">Helmut Dannerbauer</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="2109.03842v1-abstract-short" style="display: inline;"> In the framework of a systematic ALMA study of IR-selected main-sequence and starburst galaxies at z~1-1.7 at typical ~1" resolution, we report on the effects of mid-IR- and X-ray-detected active galactic nuclei (AGN) on the reservoirs and excitation of molecular gas in a sample of 55 objects. We find detectable nuclear activity in ~30% of the sample. The presence of dusty tori influences the IR S… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.03842v1-abstract-full').style.display = 'inline'; document.getElementById('2109.03842v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.03842v1-abstract-full" style="display: none;"> In the framework of a systematic ALMA study of IR-selected main-sequence and starburst galaxies at z~1-1.7 at typical ~1" resolution, we report on the effects of mid-IR- and X-ray-detected active galactic nuclei (AGN) on the reservoirs and excitation of molecular gas in a sample of 55 objects. We find detectable nuclear activity in ~30% of the sample. The presence of dusty tori influences the IR SED of galaxies, as highlighted by the strong correlation among the AGN contribution to the total IR luminosity budget (fAGN = LIR,AGN/LIR), its hard X-ray emission, and the Rayleigh-Jeans to mid-IR (S1.2mm/S24um) observed color, with consequences on the empirical SFR estimates. Nevertheless, we find only marginal effects of AGN on the CO (J=2,4,5,7) or neutral carbon ([CI](1-0), [CI](2-1)) line luminosities and on the derived molecular gas excitation as gauged by line ratios and the full SLEDs. The [CI] and CO emission up to J=5,7 thus primarily traces the properties of the host in typical IR luminous galaxies. However, we highlight the existence of a large variety of line luminosities and ratios despite the homogeneous selection. In particular, we find a sparse group of AGN-dominated sources with the highest LIR,AGN/LIR,SFR ratios, >3, that are more luminous in CO(5-4) than what is predicted by the L'CO(5-4)-LIR,SFR relation, which might be the result of the nuclear activity. For the general population, our findings translate into AGN having minimal effects on quantities such as gas and dust fractions and SFEs. If anything, we find hints of a marginal tendency of AGN hosts to be compact at far-IR wavelengths and to display 1.8x larger dust optical depths. In general, this is consistent with a marginal impact of the nuclear activity on the gas reservoirs and star formation in average star-forming AGN hosts with LIR>5e11 Lsun, typically underrepresented in surveys of quasars and SMGs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.03842v1-abstract-full').style.display = 'none'; document.getElementById('2109.03842v1-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 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 10 figures + Appendix, accepted in A&A on August 28th, 2021. The data compilation will be available on Vizier. (Minor) updates for the AGN population with respect to the data release of Valentino et al. 2020, A&A, 641, 155. For an early access, please contact the corresponding author. Abstract slightly modified to adjust to arXiv's requirements</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 654, A165 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.03305">arXiv:2109.03305</a> <span> [<a href="https://arxiv.org/pdf/2109.03305">pdf</a>, <a href="https://arxiv.org/format/2109.03305">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/10.1051/0004-6361/202142168">10.1051/0004-6361/202142168 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CLASH-VLT: Abell~S1063. Cluster assembly history and spectroscopic catalogue </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">A. Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Biviano%2C+A">A. Biviano</a>, <a href="/search/astro-ph?searchtype=author&query=Annunziatella%2C+M">M. Annunziatella</a>, <a href="/search/astro-ph?searchtype=author&query=Girardi%2C+M">M. Girardi</a>, <a href="/search/astro-ph?searchtype=author&query=Sartoris%2C+B">B. Sartoris</a>, <a href="/search/astro-ph?searchtype=author&query=Nonino%2C+M">M. Nonino</a>, <a href="/search/astro-ph?searchtype=author&query=Brescia%2C+M">M. Brescia</a>, <a href="/search/astro-ph?searchtype=author&query=Riccio%2C+G">G. Riccio</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Balestra%2C+I">I. Balestra</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=De+Lucia%2C+G">G. De Lucia</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">R. Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Seitz%2C+S">S. Seitz</a>, <a href="/search/astro-ph?searchtype=author&query=Tozzi%2C+P">P. Tozzi</a>, <a href="/search/astro-ph?searchtype=author&query=Scodeggio%2C+M">M. Scodeggio</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Angora%2C+G">G. Angora</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">P. Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Borgani%2C+S">S. Borgani</a>, <a href="/search/astro-ph?searchtype=author&query=Demarco%2C+R">R. Demarco</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">M. Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Strazzullo%2C+V">V. Strazzullo</a>, <a href="/search/astro-ph?searchtype=author&query=Tortorelli%2C+L">L. Tortorelli</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="2109.03305v2-abstract-short" style="display: inline;"> Using the CLASH-VLT survey, we assembled an unprecedented sample of 1234 spectroscopically confirmed members in Abell~S1063, finding a dynamically complex structure at z_cl=0.3457 with a velocity dispersion 蟽_v=1380 -32 +26 km s^-1. We investigate cluster environmental and dynamical effects by analysing the projected phase-space diagram and the orbits as a function of galaxy spectral properties. W… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.03305v2-abstract-full').style.display = 'inline'; document.getElementById('2109.03305v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.03305v2-abstract-full" style="display: none;"> Using the CLASH-VLT survey, we assembled an unprecedented sample of 1234 spectroscopically confirmed members in Abell~S1063, finding a dynamically complex structure at z_cl=0.3457 with a velocity dispersion 蟽_v=1380 -32 +26 km s^-1. We investigate cluster environmental and dynamical effects by analysing the projected phase-space diagram and the orbits as a function of galaxy spectral properties. We classify cluster galaxies according to the presence and strength of the [OII] emission line, the strength of the H$未$ absorption line, and colours. We investigate the relationship between the spectral classes of galaxies and their position in the projected phase-space diagram. We analyse separately red and blue galaxy orbits. By correlating the observed positions and velocities with the projected phase-space constructed from simulations, we constrain the accretion redshift of galaxies with different spectral types. Passive galaxies are mainly located in the virialised region, while emission-line galaxies are outside r_200, and are accreted later into the cluster. Emission-lines and post-starbursts show an asymmetric distribution in projected phase-space within r_200, with the first being prominent at Delta_v/sigma <~-1.5$, and the second at Delta_v/ sigma >~ 1.5, suggesting that backsplash galaxies lie at large positive velocities. We find that low-mass passive galaxies are accreted in the cluster before the high-mass ones. This suggests that we observe as passives only the low-mass galaxies accreted early in the cluster as blue galaxies, that had the time to quench their star formation. We also find that red galaxies move on more radial orbits than blue galaxies. This can be explained if infalling galaxies can remain blue moving on tangential orbits. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.03305v2-abstract-full').style.display = 'none'; document.getElementById('2109.03305v2-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 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, 28 figures, 3 tables, Accepted for publication in Astronomy and Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 656, A147 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2102.11752">arXiv:2102.11752</a> <span> [<a href="https://arxiv.org/pdf/2102.11752">pdf</a>, <a href="https://arxiv.org/format/2102.11752">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/stab559">10.1093/mnras/stab559 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Feedback Factory: Multiple faint radio-jets detected in a cluster at z=2 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kalita%2C+B+S">Boris S. Kalita</a>, <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">Emanuele Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Coogan%2C+R+T">Rosemary T. Coogan</a>, <a href="/search/astro-ph?searchtype=author&query=Delvecchio%2C+I">Ivan Delvecchio</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">Raphael Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Valentino%2C+F">Francesco Valentino</a>, <a href="/search/astro-ph?searchtype=author&query=Strazzullo%2C+V">Veronica Strazzullo</a>, <a href="/search/astro-ph?searchtype=author&query=Tremou%2C+E">Evangelia Tremou</a>, <a href="/search/astro-ph?searchtype=author&query=Elbaz%2C+D">David Elbaz</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%B3mez-Guijarro%2C+C">Carlos G贸mez-Guijarro</a>, <a href="/search/astro-ph?searchtype=author&query=Finoguenov%2C+A">Alexis Finoguenov</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2102.11752v1-abstract-short" style="display: inline;"> We report the detection of multiple faint radio sources, that we identify as AGN-jets, within CLJ1449+0856 at z=2 using 3 GHz VLA observations. We study the effects of radio-jet based kinetic feedback at high redshifts, which has been found to be crucial in low redshift clusters to explain the observed thermodynamic properties of their ICM. We investigate this interaction at an epoch featuring hig… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.11752v1-abstract-full').style.display = 'inline'; document.getElementById('2102.11752v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2102.11752v1-abstract-full" style="display: none;"> We report the detection of multiple faint radio sources, that we identify as AGN-jets, within CLJ1449+0856 at z=2 using 3 GHz VLA observations. We study the effects of radio-jet based kinetic feedback at high redshifts, which has been found to be crucial in low redshift clusters to explain the observed thermodynamic properties of their ICM. We investigate this interaction at an epoch featuring high levels of AGN activity and a transitional phase of ICM in regards to the likelihood of residual cold-gas accretion. We measure a total flux of $\rm 30.6 \pm 3.3~渭Jy$ from the 6 detected jets. Their power contribution is estimated to be $1.2 ~(\pm 0.6)~ \times 10^{44} ~\rm ergs~ s^{-1}$, although this value could be up to $4.7 ~ \times 10^{44} ~\rm ergs~ s^{-1}$. This is a factor $\sim 0.25 - 1.0$ of the previously estimated instantaneous energy injection into the ICM of CLJ1449+0856 from AGN outflows and star formation, that have already been found to be sufficient in globally offsetting the cooling flows in the cluster core. In line with the already detected abundance of star formation, this mode of feedback being distributed over multiple sites, contrary to a single central source observed at low redshifts, points to accretion of gas into the cluster centre. This also suggests a 'steady state' of the cluster featuring non cool-core like behaviour. Finally, we also examine the TIR-radio luminosity ratio for the known sample of galaxies within the cluster core and find that dense environments do not have any serious consequence on the compliance of galaxies to the IR-radio correlation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.11752v1-abstract-full').style.display = 'none'; document.getElementById('2102.11752v1-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 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2021. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.07724">arXiv:2101.07724</a> <span> [<a href="https://arxiv.org/pdf/2101.07724">pdf</a>, <a href="https://arxiv.org/format/2101.07724">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/10.1051/0004-6361/202039577">10.1051/0004-6361/202039577 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multiwavelength dissection of a massive heavily dust-obscured galaxy and its blue companion at z $\sim $2 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hamed%2C+M">M. Hamed</a>, <a href="/search/astro-ph?searchtype=author&query=Ciesla%2C+L">L. Ciesla</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%A9thermin%2C+M">M. B茅thermin</a>, <a href="/search/astro-ph?searchtype=author&query=Ma%C5%82ek%2C+K">K. Ma艂ek</a>, <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">E. Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Sargent%2C+M+T">M. T. Sargent</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">R. Gobat</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="2101.07724v1-abstract-short" style="display: inline;"> In this work we study a system of two galaxies, Astarte and Adonis, at z $\sim $2 when the Universe was undergoing its peak of star formation activity. Astarte is a dusty star-forming galaxy at the massive-end of the main sequence (MS) and Adonis is a less-massive, bright in ultraviolet (UV), companion galaxy with an optical spectroscopic redshift. We analyse the physical properties of this system… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.07724v1-abstract-full').style.display = 'inline'; document.getElementById('2101.07724v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.07724v1-abstract-full" style="display: none;"> In this work we study a system of two galaxies, Astarte and Adonis, at z $\sim $2 when the Universe was undergoing its peak of star formation activity. Astarte is a dusty star-forming galaxy at the massive-end of the main sequence (MS) and Adonis is a less-massive, bright in ultraviolet (UV), companion galaxy with an optical spectroscopic redshift. We analyse the physical properties of this system, and probe the gas mass of Astarte with its ALMA CO emission, to investigate whether this ultra-massive galaxy is quenching or not. We use CIGALE - a spectral energy distribution modeling code - to derive the key physical properties of Astarte and Adonis, mainly their star formation rates (SFRs), stellar masses, and dust luminosities. We inspect the variation of the physical parameters depending on the assumed dust attenuation law. We also estimate the molecular gas mass of Astarte from its CO emission, using different $伪_{CO}$ and transition ratios ($r_{31}$) and discuss the implication of the various assumptions on the gas mass derivation. We find that Astarte exhibits a MS-like star formation activity, while Adonis is undergoing a strong starburst (SB) phase. The molecular gas mass of Astarte is far below the gas fraction of typical star-forming galaxies at z=2. This low gas content and high SFR, result in a depletion time of $0.22\pm0.07$ Gyrs, slightly shorter than what is expected for a MS galaxy at this redshift. The CO luminosity versus the total IR luminosity suggests a MS-like activity assuming a galactic conversion factor and a low transition ratio. The SFR of Astarte is of the same order using different attenuation laws, unlike its stellar mass that increases using shallow attenuation laws. We discuss these properties and suggest that Astarte might be experiencing a recent decrease of star formation activity and is quenching through the MS following a SB epoch. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.07724v1-abstract-full').style.display = 'none'; document.getElementById('2101.07724v1-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 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 7 figures, accepted for publication in A&A. Abstract abridged for arXiv submission</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 646, A127 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.04700">arXiv:2101.04700</a> <span> [<a href="https://arxiv.org/pdf/2101.04700">pdf</a>, <a href="https://arxiv.org/format/2101.04700">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/10.1051/0004-6361/202039280">10.1051/0004-6361/202039280 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Interstellar Medium of Quiescent Galaxies and its Evolution With Time </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Magdis%2C+G+E">Georgios E. Magdis</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">R. Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Valentino%2C+F">F. Valentino</a>, <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">E. Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Zanella%2C+A">A. Zanella</a>, <a href="/search/astro-ph?searchtype=author&query=Kokorev%2C+V">V. Kokorev</a>, <a href="/search/astro-ph?searchtype=author&query=Toft%2C+S">S. Toft</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+S">S. Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Whitaker%2C+K">K. Whitaker</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="2101.04700v1-abstract-short" style="display: inline;"> We characterise the basic far-IR (FIR) properties and the gas mass fraction of massive (<log(M*/Msun)> ~ 11.0) quiescent galaxies (QGs) and explore how these evolve from z = 2.0 to the present day. We use robust, multi-wavelength (mid- to far-IR and sub-millimetre to radio) stacking ensembles of homogeneously selected and mass complete samples of log(M*/Msun) > 10.8 QGs. We find that the dust to s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.04700v1-abstract-full').style.display = 'inline'; document.getElementById('2101.04700v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.04700v1-abstract-full" style="display: none;"> We characterise the basic far-IR (FIR) properties and the gas mass fraction of massive (<log(M*/Msun)> ~ 11.0) quiescent galaxies (QGs) and explore how these evolve from z = 2.0 to the present day. We use robust, multi-wavelength (mid- to far-IR and sub-millimetre to radio) stacking ensembles of homogeneously selected and mass complete samples of log(M*/Msun) > 10.8 QGs. We find that the dust to stellar mass ratio (Md/M*) rises steeply as a function of redshift up to z~1.0 and then remains flat at least out to z = 2.0. Using Md as a proxy of gas mass (Mgas), we find a similar trend for the evolution of the gas mass fraction (fgas) with z > 1.0 QGs having fgas ~ 7.0% (for solar metallicity). This fgas is 3 - 10 times lower than that of normal star forming galaxies (SFGs) at their corresponding redshift but ~3 and ~10 times larger compared to that of z = 0.5 and local QGs. Furthermore, the inferred gas depletion time scales are comparable to that of local SFGs and systematically longer than that of main sequence galaxies at their corresponding redshifts. Our analysis also reveals that the average dust temperature (Td) of massive QGs remains roughly constant (< Td > = 21.0 \pm 2.0K) at least out to z ~ 2.0 and is substantially colder (~ 10K) compared to that of z > 0 SFGs. This motivated us to construct and release a redshift-invariant template IR SED, that we use to make predictions for ALMA observations and to explore systematic effects in the Mgas estimates of massive, high-z QGs. Finally, we discuss how a simple model that considers progenitor-bias can effectively reproduce the observed evolution of Md/M* and fgas. Our results indicate universal initial interstellar medium conditions for quenched galaxies and a large degree of uniformity in their internal processes across cosmic time. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.04700v1-abstract-full').style.display = 'none'; document.getElementById('2101.04700v1-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 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication 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 647, A33 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.02767">arXiv:2012.02767</a> <span> [<a href="https://arxiv.org/pdf/2012.02767">pdf</a>, <a href="https://arxiv.org/format/2012.02767">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/10.1051/0004-6361/202040067">10.1051/0004-6361/202040067 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> HST grism spectroscopy of z~3 massive quiescent galaxies: Approaching the metamorphosis </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=D%27Eugenio%2C+C">C. D'Eugenio</a>, <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">E. Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">R. Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Strazzullo%2C+V">V. Strazzullo</a>, <a href="/search/astro-ph?searchtype=author&query=Lustig%2C+P">P. Lustig</a>, <a href="/search/astro-ph?searchtype=author&query=Delvecchio%2C+I">I. Delvecchio</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+S">S. Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Cimatti%2C+A">A. Cimatti</a>, <a href="/search/astro-ph?searchtype=author&query=Onodera%2C+M">M. Onodera</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="2012.02767v2-abstract-short" style="display: inline;"> Tracing the emergence of the massive quiescent galaxy (QG) population requires the build-up of reliable quenched samples. We present Hubble Space Telescope WFC3/G141 grism spectra of 10 quiescent galaxy candidates selected at $2.5<z<3.5$ in the COSMOS field. Spectroscopic confirmation for the whole sample is obtained within 1-3 orbits based on the presence of strong spectral breaks and Balmer abso… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.02767v2-abstract-full').style.display = 'inline'; document.getElementById('2012.02767v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.02767v2-abstract-full" style="display: none;"> Tracing the emergence of the massive quiescent galaxy (QG) population requires the build-up of reliable quenched samples. We present Hubble Space Telescope WFC3/G141 grism spectra of 10 quiescent galaxy candidates selected at $2.5<z<3.5$ in the COSMOS field. Spectroscopic confirmation for the whole sample is obtained within 1-3 orbits based on the presence of strong spectral breaks and Balmer absorption lines. Combining their spectra with optical to near-IR photometry, star-forming solutions are formally rejected for the entire sample. Broad spectral indices are consistent with the presence of young A-type stars, which implies that the last major episode of star formation has taken place no earlier than $\sim$300-800 Myr prior to observation. Marginalising over three different slopes of the dust attenuation curve, we obtain short mass-weighted ages and an average peak star formation rate of SFR$\sim10^3$ M$_{\odot}$ yr$^{-1}$ at $z_{formation}\sim3.5$. Despite mid- and far-IR data are too shallow to determine the obscured SFR on a galaxy-by-galaxy basis, the mean stack emission from 3GHz data constrains the level of residual obscured SFR to be globally below 50 M$_{\odot}$ yr$^{-1}$, hence three times below the scatter of the coeval main sequence. Alternatively, the very same radio detection suggests a widespread radio-mode feedback by active galactic nuclei (AGN) four times stronger than in z$\sim$1.8 massive QGs. This is accompanied by a 30% fraction of X-ray luminous AGN with a black hole accretion rate per unit SFR enhanced by a factor of $\sim30$ with respect to similarly massive QGs at lower redshift. The average compact, high S茅rsic index morphologies of our galaxies, coupled with their young mass-weighted ages, suggest that the mechanisms responsible for the development of a spheroidal component might be concomitant with (or preceding) those causing their quenching. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.02767v2-abstract-full').style.display = 'none'; document.getElementById('2012.02767v2-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 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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. 28 pages, 16 figures + additional plots in appendix A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 653, A32 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.02766">arXiv:2012.02766</a> <span> [<a href="https://arxiv.org/pdf/2012.02766">pdf</a>, <a href="https://arxiv.org/format/2012.02766">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/staa3766">10.1093/mnras/staa3766 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Compact, bulge dominated structures of spectroscopically confirmed quiescent galaxies at z~3 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lustig%2C+P">Peter Lustig</a>, <a href="/search/astro-ph?searchtype=author&query=Strazzullo%2C+V">Veronica Strazzullo</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Eugenio%2C+C">Chiara D'Eugenio</a>, <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">Emanuele Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Pannella%2C+M">Maurilio Pannella</a>, <a href="/search/astro-ph?searchtype=author&query=Renzini%2C+A">Alvio Renzini</a>, <a href="/search/astro-ph?searchtype=author&query=Cimatti%2C+A">Andrea Cimatti</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">Raphael Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+S">Shuowen Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Mohr%2C+J+J">Joseph J. Mohr</a>, <a href="/search/astro-ph?searchtype=author&query=Onodera%2C+M">Masato Onodera</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="2012.02766v1-abstract-short" style="display: inline;"> We study structural properties of spectroscopically confirmed massive quiescent galaxies at $z\approx 3$ with one of the first sizeable samples of such sources, made of ten $10.8<\log(M_{\star}/M_{\odot})<11.3$ galaxies at $2.4 < z < 3.2$ in the COSMOS field whose redshifts and quiescence are confirmed by HST grism spectroscopy. Although affected by a weak bias toward younger stellar populations,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.02766v1-abstract-full').style.display = 'inline'; document.getElementById('2012.02766v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.02766v1-abstract-full" style="display: none;"> We study structural properties of spectroscopically confirmed massive quiescent galaxies at $z\approx 3$ with one of the first sizeable samples of such sources, made of ten $10.8<\log(M_{\star}/M_{\odot})<11.3$ galaxies at $2.4 < z < 3.2$ in the COSMOS field whose redshifts and quiescence are confirmed by HST grism spectroscopy. Although affected by a weak bias toward younger stellar populations, this sample is deemed to be largely representative of the majority of the most massive and thus intrinsically rarest quiescent sources at this cosmic time. We rely on targeted HST/WFC3 observations and fit S茅rsic profiles to the galaxy surface brightness distributions at $\approx 4000$ angstrom restframe. We find typically high S茅rsic indices and axis ratios (medians $\approx 4.5$ and $0.73$, respectively) suggesting that, at odds with some previous results, the first massive quiescent galaxies may largely be already bulge-dominated systems. We measure compact galaxy sizes with an average of $\approx 1.4$kpc at $\log(M_{\star}/M_{\odot})\approx 11.2$, in good agreement with the extrapolation at the highest masses of previous determinations of the stellar mass - size relation of quiescent galaxies, and of its redshift evolution, from photometrically selected samples at lower and similar redshifts. This work confirms the existence of a population of compact, bulge dominated, massive, quiescent sources at $z\approx 3$, providing one of the first statistical estimates of their structural properties, and further constraining the early formation and evolution of the first quiescent galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.02766v1-abstract-full').style.display = 'none'; document.getElementById('2012.02766v1-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 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">19 pages, 10 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/2011.10547">arXiv:2011.10547</a> <span> [<a href="https://arxiv.org/pdf/2011.10547">pdf</a>, <a href="https://arxiv.org/format/2011.10547">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/10.1051/0004-6361/202039593">10.1051/0004-6361/202039593 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The evolution of the gas fraction of quiescent galaxies modeled as a consequence of their creation rate </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">Raphael Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Magdis%2C+G">Georgios Magdis</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Eugenio%2C+C">Chiara D'Eugenio</a>, <a href="/search/astro-ph?searchtype=author&query=Valentino%2C+F">Francesco Valentino</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2011.10547v1-abstract-short" style="display: inline;"> We discuss the evolution of the interstellar medium of quiescent galaxies, currently emerging from recent analyses, with the help of a simple model based on well-established empirical relations such as the stellar mass functions and the main sequence of star formation. This model is meant to describe observed quantities without making specific assumptions on the nature of quenching processes, but… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.10547v1-abstract-full').style.display = 'inline'; document.getElementById('2011.10547v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.10547v1-abstract-full" style="display: none;"> We discuss the evolution of the interstellar medium of quiescent galaxies, currently emerging from recent analyses, with the help of a simple model based on well-established empirical relations such as the stellar mass functions and the main sequence of star formation. This model is meant to describe observed quantities without making specific assumptions on the nature of quenching processes, but relying on their observable consequences. We find that the high gas fractions seen or suggested at high redshift in quiescent galaxies, and their apparent mild evolution at early times, can be mostly attributed to a progenitor effect where recently quenched galaxies with ~10% gas fractions dominate the quiescent galaxy population until z~1. In the same context, the much lower gas and dust fractions measured in local early-type galaxies are interpreted as the product of the steady depletion of their interstellar medium on a ~2 Gyr timescale, coupled with a higher fraction of more gas-exhaustive events. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.10547v1-abstract-full').style.display = 'none'; document.getElementById('2011.10547v1-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 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 pages, 5 figures, 2 tables (including appendices). Accepted for publication in Astronomy & Astrophysics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2006.12521">arXiv:2006.12521</a> <span> [<a href="https://arxiv.org/pdf/2006.12521">pdf</a>, <a href="https://arxiv.org/format/2006.12521">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/10.1051/0004-6361/202038322">10.1051/0004-6361/202038322 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CO emission in distant galaxies on and above the main sequence </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Valentino%2C+F">Francesco Valentino</a>, <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">Emanuele Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Puglisi%2C+A">Annagrazia Puglisi</a>, <a href="/search/astro-ph?searchtype=author&query=Magdis%2C+G+E">Georgios E. Magdis</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+D">Daizhong Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Kokorev%2C+V">Vasily Kokorev</a>, <a href="/search/astro-ph?searchtype=author&query=Cortzen%2C+I">Isabella Cortzen</a>, <a href="/search/astro-ph?searchtype=author&query=Madden%2C+S+C">Suzanne C. Madden</a>, <a href="/search/astro-ph?searchtype=author&query=Aravena%2C+M">Manuel Aravena</a>, <a href="/search/astro-ph?searchtype=author&query=Gomez-Guijarro%2C+C">Carlos Gomez-Guijarro</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+M">Min-Young Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Floc%27h%2C+E+L">Emeric Le Floc'h</a>, <a href="/search/astro-ph?searchtype=author&query=Gao%2C+Y">Yu Gao</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">Raphael Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Bournaud%2C+F">Frederic Bournaud</a>, <a href="/search/astro-ph?searchtype=author&query=Dannerbauer%2C+H">Helmut Dannerbauer</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+S">Shuowen Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M+E">Mark E. Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Kartaltepe%2C+J+S">Jeyhan S. Kartaltepe</a>, <a href="/search/astro-ph?searchtype=author&query=Sanders%2C+D">David Sanders</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="2006.12521v1-abstract-short" style="display: inline;"> We present the detection of multiple CO line transitions with ALMA in a few tens of infrared-selected galaxies on and above the main sequence at z=1.1-1.7. We reliably detected the emission of CO(5-4), CO(2-1), and CO(7-6)+[CI](2-1) in 50, 33, and 13 galaxies, respectively, and we complemented this information with available CO(4-3) and [CI](1-0) fluxes for part of the sample, and modeling of the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.12521v1-abstract-full').style.display = 'inline'; document.getElementById('2006.12521v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2006.12521v1-abstract-full" style="display: none;"> We present the detection of multiple CO line transitions with ALMA in a few tens of infrared-selected galaxies on and above the main sequence at z=1.1-1.7. We reliably detected the emission of CO(5-4), CO(2-1), and CO(7-6)+[CI](2-1) in 50, 33, and 13 galaxies, respectively, and we complemented this information with available CO(4-3) and [CI](1-0) fluxes for part of the sample, and modeling of the optical-to-mm SEDs. We retrieve a quasi-linear relation between LIR and CO(5-4) or CO(7-6) for main-sequence galaxies and starbursts, corroborating the hypothesis that these transitions can be used as SFR tracers. We find the CO excitation to steadily increase as a function of the star formation efficiency, the mean intensity of the radiation field warming the dust, the surface density of SFR, and, less distinctly, with the distance from the main sequence. This adds to the tentative evidence for higher excitation of the CO+[CI] SLED of starbursts relative to that for main-sequence objects, where the dust opacities play a minor role in shaping the high-J CO transitions in our sample. However, the distinction between the average SLED of upper main-sequence and starburst galaxies is blurred, driven by a wide variety of intrinsic shapes. LVG radiative transfer modeling demonstrates the existence of a highly excited component that elevates the CO SLED of high-redshift main-sequence and starbursting galaxies above the typical values observed in the disk of the Milky Way. This excited component is dense and it encloses ~50% of the total molecular gas mass in main-sequence objects. We interpret the observed trends involving the CO excitation as mainly driven by a combination of large SFRs and compact sizes, naturally connected with enhanced dense molecular gas fractions and higher dust and gas temperatures, due to increasing UV radiation fields, cosmic ray rates, and dust/gas coupling. [Abridged] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.12521v1-abstract-full').style.display = 'none'; document.getElementById('2006.12521v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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, 9 figures + Appendix, accepted in A&A. The data compilation will be released as a .fits table on the journal's website. For an early access, please contact the corresponding author. The plots of spectra and far-infrared SEDs will be available on the journal's website and temporarily at this link: https://bit.ly/spectra_and_seds_valentino_2020c</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 641, A155 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2006.11089">arXiv:2006.11089</a> <span> [<a href="https://arxiv.org/pdf/2006.11089">pdf</a>, <a href="https://arxiv.org/format/2006.11089">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/10.1051/0004-6361/202038700">10.1051/0004-6361/202038700 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Three Lyman-alpha emitting filaments converging to a massive galaxy group at z=2.91: discussing the case for cold gas infall </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">E. Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Valentino%2C+F">F. Valentino</a>, <a href="/search/astro-ph?searchtype=author&query=Rich%2C+R+M">R. M. Rich</a>, <a href="/search/astro-ph?searchtype=author&query=Neill%2C+J+D">J. D. Neill</a>, <a href="/search/astro-ph?searchtype=author&query=Gronke%2C+M">M. Gronke</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Sullivan%2C+D">D. O'Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=Elbaz%2C+D">D. Elbaz</a>, <a href="/search/astro-ph?searchtype=author&query=Bournaud%2C+F">F. Bournaud</a>, <a href="/search/astro-ph?searchtype=author&query=Finoguenov%2C+A">A. Finoguenov</a>, <a href="/search/astro-ph?searchtype=author&query=Marchal%2C+A">A. Marchal</a>, <a href="/search/astro-ph?searchtype=author&query=Delvecchio%2C+I">I. Delvecchio</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+S">S. Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+D">D. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Calabro%2C+A">A. Calabro</a>, <a href="/search/astro-ph?searchtype=author&query=Coogan%2C+R">R. Coogan</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Eugenio%2C+C">C. D'Eugenio</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">R. Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Kalita%2C+B+S">B. S. Kalita</a>, <a href="/search/astro-ph?searchtype=author&query=Laursen%2C+P">P. Laursen</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+D+C">D. C. Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Puglisi%2C+A">A. Puglisi</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">E. Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Strazzullo%2C+V">V. Strazzullo</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+T">T. Wang</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="2006.11089v2-abstract-short" style="display: inline;"> We have discovered a 300kpc-wide giant Lya nebula centered on the massive galaxy group RO-1001 at z=2.91 in the COSMOS field. Keck Cosmic Web Imager observations reveal three cold gas filaments converging into the center of the potential well of its ~4x10^13Msun dark matter halo, hosting 1200Msun/yr of star formation as probed by ALMA and NOEMA observations. The nebula morphological and kinematics… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.11089v2-abstract-full').style.display = 'inline'; document.getElementById('2006.11089v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2006.11089v2-abstract-full" style="display: none;"> We have discovered a 300kpc-wide giant Lya nebula centered on the massive galaxy group RO-1001 at z=2.91 in the COSMOS field. Keck Cosmic Web Imager observations reveal three cold gas filaments converging into the center of the potential well of its ~4x10^13Msun dark matter halo, hosting 1200Msun/yr of star formation as probed by ALMA and NOEMA observations. The nebula morphological and kinematics properties and the prevalence of blueshifted components in the Lya spectra are consistent with a scenario of gas accretion. The upper limits on AGN activity and overall energetics favor gravity as the primary Lya powering source and infall as the main source of gas flows to the system. Although interpretational difficulties remain, with outflows and likely also photoionization with ensuing recombination still playing a role, this finding provides arguably an ideal environment to quantitatively test models of cold gas accretion and galaxy feeding inside an actively star-forming massive halo at high redshift. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.11089v2-abstract-full').style.display = 'none'; document.getElementById('2006.11089v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">20 pages, 12 figures, 3 tables. Accepted for publication in A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2003.04342">arXiv:2003.04342</a> <span> [<a href="https://arxiv.org/pdf/2003.04342">pdf</a>, <a href="https://arxiv.org/format/2003.04342">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/10.3847/2041-8213/ab7a96">10.3847/2041-8213/ab7a96 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Typical Massive Quiescent Galaxy at z$\sim$3 is a Post-starburst </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=D%27Eugenio%2C+C">C. D'Eugenio</a>, <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">E. Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">R. Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Strazzullo%2C+V">V. Strazzullo</a>, <a href="/search/astro-ph?searchtype=author&query=Lustig%2C+P">P. Lustig</a>, <a href="/search/astro-ph?searchtype=author&query=Delvecchio%2C+I">I. Delvecchio</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+S">S. Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Puglisi%2C+A">A. Puglisi</a>, <a href="/search/astro-ph?searchtype=author&query=Calabr%C3%B3%2C+A">A. Calabr贸</a>, <a href="/search/astro-ph?searchtype=author&query=Mancini%2C+C">C. Mancini</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">M. Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Cimatti%2C+A">A. Cimatti</a>, <a href="/search/astro-ph?searchtype=author&query=Onodera%2C+M">M. Onodera</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2003.04342v1-abstract-short" style="display: inline;"> We have obtained spectroscopic confirmation with Hubble Space Telescope WFC3/G141 of a first sizeable sample of nine quiescent galaxies at 2.4<z<3.3. Their average near-UV/optical rest-frame spectrum is characterized by low attenuation (Av$\sim$0.6 mag) and a strong Balmer break, larger than the 4000 A break, corresponding to a fairly young age of $\sim$300 Myr. This formally classifies a substant… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.04342v1-abstract-full').style.display = 'inline'; document.getElementById('2003.04342v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2003.04342v1-abstract-full" style="display: none;"> We have obtained spectroscopic confirmation with Hubble Space Telescope WFC3/G141 of a first sizeable sample of nine quiescent galaxies at 2.4<z<3.3. Their average near-UV/optical rest-frame spectrum is characterized by low attenuation (Av$\sim$0.6 mag) and a strong Balmer break, larger than the 4000 A break, corresponding to a fairly young age of $\sim$300 Myr. This formally classifies a substantial fraction of classically selected quiescent galaxies at z $\sim$ 3 as post-starbursts, marking their convergence to the quenching epoch. The rapid spectral evolution with respect to z $\sim$ 1.5 quiescent galaxies is not matched by an increase of residual star-formation, as judged from the weak detection of [O II]3727A emission, pointing to a flattening of the steep increase in gas fractions previously seen from z $\sim$ 0 to 1.8. However, radio 3GHz stacked emission implies either much stronger dust-obscured star formation or substantial further evolution in radio-mode AGN activity with respect to z $\sim$ 1.5. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.04342v1-abstract-full').style.display = 'none'; document.getElementById('2003.04342v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 March, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 4 figures. To appear on ApJ 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/2001.03641">arXiv:2001.03641</a> <span> [<a href="https://arxiv.org/pdf/2001.03641">pdf</a>, <a href="https://arxiv.org/format/2001.03641">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/10.1051/0004-6361/201936727">10.1051/0004-6361/201936727 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A hyper luminous starburst at z=4.72 magnified by a lensing galaxy pair at z=1.48 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ciesla%2C+L">L. Ciesla</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%A9thermin%2C+M">M. B茅thermin</a>, <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">E. Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Richard%2C+J">J. Richard</a>, <a href="/search/astro-ph?searchtype=author&query=Diaz-Santos%2C+T">T. Diaz-Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Sargent%2C+M+T">M. T. Sargent</a>, <a href="/search/astro-ph?searchtype=author&query=Elbaz%2C+D">D. Elbaz</a>, <a href="/search/astro-ph?searchtype=author&query=Boquien%2C+M">M. Boquien</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+T">T. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Schreiber%2C+C">C. Schreiber</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+C">C. Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Zabl%2C+J">J. Zabl</a>, <a href="/search/astro-ph?searchtype=author&query=Fraser%2C+M">M. Fraser</a>, <a href="/search/astro-ph?searchtype=author&query=Aravena%2C+M">M. Aravena</a>, <a href="/search/astro-ph?searchtype=author&query=Assef%2C+R+J">R. J. Assef</a>, <a href="/search/astro-ph?searchtype=author&query=Baker%2C+A+J">A. J. Baker</a>, <a href="/search/astro-ph?searchtype=author&query=Beelen%2C+A">A. Beelen</a>, <a href="/search/astro-ph?searchtype=author&query=Boselli%2C+A">A. Boselli</a>, <a href="/search/astro-ph?searchtype=author&query=Bournaud%2C+F">F. Bournaud</a>, <a href="/search/astro-ph?searchtype=author&query=Burgarella%2C+D">D. Burgarella</a>, <a href="/search/astro-ph?searchtype=author&query=Charmandaris%2C+V">V. Charmandaris</a>, <a href="/search/astro-ph?searchtype=author&query=C%C3%B4t%C3%A9%2C+P">P. C么t茅</a>, <a href="/search/astro-ph?searchtype=author&query=Epinat%2C+B">B. Epinat</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrarese%2C+L">L. Ferrarese</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">R. Gobat</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="2001.03641v1-abstract-short" style="display: inline;"> [Abridged] We discovered in the Herschel Reference Survey an extremely bright IR source with $S_{500}$~120mJy (Red Virgo 4 - RV4). Based on IRAM/EMIR and IRAM/NOEMA detections of the CO(5-4), CO(4-3), and [CI] lines, RV4 is located at z=4.724, yielding a total observed L$_{IR}$ of 1.1+/-0.6x0$^{14}$L$_{\odot}$. At the position of the Herschel emission, three blobs are detected with the VLA at 10cm… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.03641v1-abstract-full').style.display = 'inline'; document.getElementById('2001.03641v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2001.03641v1-abstract-full" style="display: none;"> [Abridged] We discovered in the Herschel Reference Survey an extremely bright IR source with $S_{500}$~120mJy (Red Virgo 4 - RV4). Based on IRAM/EMIR and IRAM/NOEMA detections of the CO(5-4), CO(4-3), and [CI] lines, RV4 is located at z=4.724, yielding a total observed L$_{IR}$ of 1.1+/-0.6x0$^{14}$L$_{\odot}$. At the position of the Herschel emission, three blobs are detected with the VLA at 10cm. The CO(5-4) line detection of each blob confirms that they are at the same redshift with the same line width, indicating that they are multiple images of the same source. In Spitzer and deep optical observations, two sources, High-z Lens 1 (HL1) West and HL1 East, are detected at the center of the three VLA/NOEMA blobs. These two sources are placed at z=1.48 with XSHOOTER spectra, suggesting that they could be merging and gravitationally lensing the emission of RV4. HL1 is the second most distant lens known to date in strong lensing systems. The Einstein radius of the lensing system is 2.2"+/-0.2 (20kpc). The high redshift of HL1 and the large Einstein radius are highly unusual for a strong lensing system. We present the ISM properties of the background source RV4. Different estimates of the gas depletion time yield low values suggesting that RV4 is a SB galaxy. Among all high-z SMGs, this source exhibits one of the lowest L$_{[CI]}$ to L$_{IR}$ ratios, 3.2+/-0.9x10$^{-6}$, suggesting an extremely short gas tdepl of only 14+/-5Myr. It also shows a relatively high L$_{[CI]}$ to L$_{CO(4-3)}$ ratio (0.7+/-0.2) and low L$_{CO(5-4)}$ to L$_{IR}$ ratio (only ~50% of the value expected for normal galaxies) hinting a low density of gas. Finally, we discuss that the short tdepl of RV4 can be explained by either a very high SFE, which is difficult to reconcile with major mergers simulations of high-z galaxies, or a rapid decrease of SF, which would bias the estimate of tdepl toward low value. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.03641v1-abstract-full').style.display = 'none'; document.getElementById('2001.03641v1-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 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">14 pages, 15 figures, accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 635, A27 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1907.12136">arXiv:1907.12136</a> <span> [<a href="https://arxiv.org/pdf/1907.12136">pdf</a>, <a href="https://arxiv.org/ps/1907.12136">ps</a>, <a href="https://arxiv.org/format/1907.12136">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/stz2099">10.1093/mnras/stz2099 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A contribution of star-forming clumps and accreting satellites to the mass assembly of z ~ 2 galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zanella%2C+A">A. Zanella</a>, <a href="/search/astro-ph?searchtype=author&query=Floc%27h%2C+E+L">E. Le Floc'h</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+C+M">C. M. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">E. Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Bernhard%2C+E">E. Bernhard</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">R. Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Strazzullo%2C+V">V. Strazzullo</a>, <a href="/search/astro-ph?searchtype=author&query=Valentino%2C+F">F. Valentino</a>, <a href="/search/astro-ph?searchtype=author&query=Cibinel%2C+A">A. Cibinel</a>, <a href="/search/astro-ph?searchtype=author&query=Almeida%2C+J+S">J. S谩nchez Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Kohandel%2C+M">M. Kohandel</a>, <a href="/search/astro-ph?searchtype=author&query=Fensch%2C+J">J. Fensch</a>, <a href="/search/astro-ph?searchtype=author&query=Behrendt%2C+M">M. Behrendt</a>, <a href="/search/astro-ph?searchtype=author&query=Burkert%2C+A">A. Burkert</a>, <a href="/search/astro-ph?searchtype=author&query=Onodera%2C+M">M. Onodera</a>, <a href="/search/astro-ph?searchtype=author&query=Bournaud%2C+F">F. Bournaud</a>, <a href="/search/astro-ph?searchtype=author&query=Scholtz%2C+J">J. Scholtz</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="1907.12136v1-abstract-short" style="display: inline;"> We investigate the contribution of clumps and satellites to the galaxy mass assembly. We analyzed spatially-resolved Hubble Space Telescope observations (imaging and slitless spectroscopy) of 53 star-forming galaxies at z ~ 1 - 3. We created continuum and emission line maps and pinpointed residual "blobs" detected after subtracting the galaxy disk. Those were separated into compact (unresolved) an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1907.12136v1-abstract-full').style.display = 'inline'; document.getElementById('1907.12136v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1907.12136v1-abstract-full" style="display: none;"> We investigate the contribution of clumps and satellites to the galaxy mass assembly. We analyzed spatially-resolved Hubble Space Telescope observations (imaging and slitless spectroscopy) of 53 star-forming galaxies at z ~ 1 - 3. We created continuum and emission line maps and pinpointed residual "blobs" detected after subtracting the galaxy disk. Those were separated into compact (unresolved) and extended (resolved) components. Extended components have sizes ~ 2 kpc and comparable stellar mass and age as the galaxy disks, whereas the compact components are 1.5 dex less massive and 0.4 dex younger than the disks. Furthermore the extended blobs are typically found at larger distances from the galaxy barycenter than the compact ones. Prompted by these observations and by the comparison with simulations, we suggest that compact blobs are in-situ formed clumps, whereas the extended ones are accreting satellites. Clumps and satellites enclose respectively ~ 20% and ~< 80% of the galaxy stellar mass, ~ 30% and ~ 20% of its star formation rate. Considering the compact blobs, we statistically estimated that massive clumps (Mstar >~ 10^9 Msun) have lifetimes of ~ 650 Myr, and the less massive ones (10^8 < Mstar < 10^9 Msun) of ~ 145 Myr. This supports simulations predicting long-lived clumps (lifetime > 100 Myr). Finally, ~< 30% (13%) of our sample galaxies are undergoing single (multiple) merger(s), they have a projected separation ~< 10 kpc, and the typical mass ratio of our satellites is 1:5 (but ranges between 1:10 and 1:1), in agreement with literature results for close pair galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1907.12136v1-abstract-full').style.display = 'none'; document.getElementById('1907.12136v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 July, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">20 pages (plus appendix), 8 figures, 2 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/1907.10985">arXiv:1907.10985</a> <span> [<a href="https://arxiv.org/pdf/1907.10985">pdf</a>, <a href="https://arxiv.org/format/1907.10985">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201935862">10.1051/0004-6361/201935862 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Sunyaev-Zel'dovich detection of the galaxy cluster Cl J1449+0856 at z = 1.99: the pressure profile in uv space </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">R. Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">E. Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Coogan%2C+R+T">R. T. Coogan</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+A+M+C+L">A. M. C. Le Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Bournaud%2C+F">F. Bournaud</a>, <a href="/search/astro-ph?searchtype=author&query=Melin%2C+J+-">J. -B. Melin</a>, <a href="/search/astro-ph?searchtype=author&query=Riechers%2C+D+A">D. A. Riechers</a>, <a href="/search/astro-ph?searchtype=author&query=Sargent%2C+M">M. Sargent</a>, <a href="/search/astro-ph?searchtype=author&query=Valentino%2C+F">F. Valentino</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+H+S">H. S. Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Finoguenov%2C+A">A. Finoguenov</a>, <a href="/search/astro-ph?searchtype=author&query=Strazzullo%2C+V">V. Strazzullo</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="1907.10985v1-abstract-short" style="display: inline;"> We present Atacama Large Millimetre Array and Atacama Compact Array observations of the Sunyaev-Zel'dovich effect in the z = 2 galaxy cluster Cl J1449+0856, an X-ray-detected progenitor of typical massive clusters in the present day Universe. While in a cleaned but otherwise untouched 92 GHz map of this cluster, little to no negative signal is visible, careful subtraction of known sub-millimetre e… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1907.10985v1-abstract-full').style.display = 'inline'; document.getElementById('1907.10985v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1907.10985v1-abstract-full" style="display: none;"> We present Atacama Large Millimetre Array and Atacama Compact Array observations of the Sunyaev-Zel'dovich effect in the z = 2 galaxy cluster Cl J1449+0856, an X-ray-detected progenitor of typical massive clusters in the present day Universe. While in a cleaned but otherwise untouched 92 GHz map of this cluster, little to no negative signal is visible, careful subtraction of known sub-millimetre emitters in the uv plane reveals a decrement at 5$蟽$ significance. The total signal is -190$\pm$36 $渭$Jy, with a peak offset by 5"-9" ($\sim$50 kpc) from both the X-ray centroid and the still-forming brightest cluster galaxy. A comparison of the recovered uv-amplitude profile of the decrement with different pressure models allows us to derive total mass constraints consistent with the $\sim$6$\times$10$^{13}$ M$_{\odot}$ estimated from X-ray data. Moreover, we find no strong evidence for a deviation of the pressure profile with respect to local galaxy clusters, although a slight tension at small-to-intermediate spatial scales suggests a flattened central profile, opposite to what seen in a cool core and possibly an AGN-related effect. This analysis of the lowest mass single SZ detection so far illustrates the importance of interferometers when observing the SZ effect in high-redshift clusters, the cores of which cannot be considered quiescent, such that careful subtraction of galaxy emission is necessary. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1907.10985v1-abstract-full').style.display = 'none'; document.getElementById('1907.10985v1-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, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">11 pages, 6 figures (+appendices); accepted for publication in Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 629, A104 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1905.02958">arXiv:1905.02958</a> <span> [<a href="https://arxiv.org/pdf/1905.02958">pdf</a>, <a href="https://arxiv.org/format/1905.02958">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/ab1f92">10.3847/2041-8213/ab1f92 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Main Sequence at $z \sim 1.3$ contains a sizable fraction of galaxies with compact star formation sizes: a new population of early post-starbursts? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Puglisi%2C+A">A. Puglisi</a>, <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">E. Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+D">D. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Bournaud%2C+F">F. Bournaud</a>, <a href="/search/astro-ph?searchtype=author&query=Silverman%2C+J+D">J. D. Silverman</a>, <a href="/search/astro-ph?searchtype=author&query=Circosta%2C+C">C. Circosta</a>, <a href="/search/astro-ph?searchtype=author&query=Calabr%C3%B2%2C+A">A. Calabr貌</a>, <a href="/search/astro-ph?searchtype=author&query=Aravena%2C+M">M. Aravena</a>, <a href="/search/astro-ph?searchtype=author&query=Cibinel%2C+A">A. Cibinel</a>, <a href="/search/astro-ph?searchtype=author&query=Dannerbauer%2C+H">H. Dannerbauer</a>, <a href="/search/astro-ph?searchtype=author&query=Delvecchio%2C+I">I. Delvecchio</a>, <a href="/search/astro-ph?searchtype=author&query=Elbaz%2C+D">D. Elbaz</a>, <a href="/search/astro-ph?searchtype=author&query=Gao%2C+Y">Y. Gao</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">R. Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+S">S. Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Floc%27h%2C+E+L">E. Le Floc'h</a>, <a href="/search/astro-ph?searchtype=author&query=Magdis%2C+G+E">G. E. Magdis</a>, <a href="/search/astro-ph?searchtype=author&query=Mancini%2C+C">C. Mancini</a>, <a href="/search/astro-ph?searchtype=author&query=Riechers%2C+D+A">D. A. Riechers</a>, <a href="/search/astro-ph?searchtype=author&query=Rodighiero%2C+G">G. Rodighiero</a>, <a href="/search/astro-ph?searchtype=author&query=Sargent%2C+M">M. Sargent</a>, <a href="/search/astro-ph?searchtype=author&query=Valentino%2C+F">F. Valentino</a>, <a href="/search/astro-ph?searchtype=author&query=Zanisi%2C+L">L. Zanisi</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="1905.02958v1-abstract-short" style="display: inline;"> ALMA measurements for 93 $Herschel$-selected galaxies at $1.1 \leqslant z \leqslant 1.7$ in COSMOS reveal a sizable ($>29$\%) population with compact star formation (SF) sizes, lying on average $> \times 3.6$ below the optical stellar mass ($M_{\star}$)-size relation of disks. This sample widely spans the star-forming Main Sequence (MS), having… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.02958v1-abstract-full').style.display = 'inline'; document.getElementById('1905.02958v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1905.02958v1-abstract-full" style="display: none;"> ALMA measurements for 93 $Herschel$-selected galaxies at $1.1 \leqslant z \leqslant 1.7$ in COSMOS reveal a sizable ($>29$\%) population with compact star formation (SF) sizes, lying on average $> \times 3.6$ below the optical stellar mass ($M_{\star}$)-size relation of disks. This sample widely spans the star-forming Main Sequence (MS), having $10^{8} \leqslant M_{\star} \leqslant 10^{11.5} \ M_{\odot}$ and $20 \leqslant SFR \leqslant 680 \ M_{\odot} \rm yr^{-1}$. The 32 size measurements and 61 upper limits are measured on ALMA images that combine observations of CO(5-4), CO(4-3), CO(2-1) and $位_{\rm obs} \sim 1.1-1.3 \ \rm mm$ continuum, all tracing the star-forming molecular gas. These compact galaxies have instead normally extended $K_{band}$ sizes, suggesting strong specific $SFR$ gradients. Compact galaxies comprise the $50\pm18 \%$ of MS galaxies at $M_{\star} > 10^{11} M_{\odot}$. This is not expected in standard bi-modal scenarios where MS galaxies are mostly steadily-growing extended disks. We suggest that compact MS objects are early post-starburst galaxies in which the merger-driven boost of SF has subsided. They retain their compact SF size until either further gas accretion restores pre-merger galaxy-wide SF, or until becoming quenched. The fraction of merger-affected SF inside the MS seems thus larger than anticipated and might reach $\sim 50$\% at the highest $M_{\star}$. The presence of large galaxies above the MS demonstrates an overall poor correlation between galaxy SF size and specific $SFR$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.02958v1-abstract-full').style.display = 'none'; document.getElementById('1905.02958v1-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 May, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">7 pages, 5 figures. Accepted for publication in ApJ 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/1901.06390">arXiv:1901.06390</a> <span> [<a href="https://arxiv.org/pdf/1901.06390">pdf</a>, <a href="https://arxiv.org/format/1901.06390">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/stz409">10.1093/mnras/stz409 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Suppressed CO emission and high G/D ratios in z=2 galaxies with sub-solar gas-phase metallicity </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Coogan%2C+R+T">R. T. Coogan</a>, <a href="/search/astro-ph?searchtype=author&query=Sargent%2C+M+T">M. T. Sargent</a>, <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">E. Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Valentino%2C+F">F. Valentino</a>, <a href="/search/astro-ph?searchtype=author&query=Strazzullo%2C+V">V. Strazzullo</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%A9thermin%2C+M">M. B茅thermin</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">R. Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+D">D. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Magdis%2C+G">G. Magdis</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="1901.06390v1-abstract-short" style="display: inline;"> We study a population of significantly sub-solar enrichment galaxies at z=1.99, to investigate how molecular gas, dust and star-formation relate in low-metallicity galaxies at the peak epoch of star-formation. We target our sample with several deep ALMA and VLA datasets, and find no individual detections of CO[4-3], CO[1-0] or dust, in stark contrast to the $>$60% detection rate expected for solar… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.06390v1-abstract-full').style.display = 'inline'; document.getElementById('1901.06390v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1901.06390v1-abstract-full" style="display: none;"> We study a population of significantly sub-solar enrichment galaxies at z=1.99, to investigate how molecular gas, dust and star-formation relate in low-metallicity galaxies at the peak epoch of star-formation. We target our sample with several deep ALMA and VLA datasets, and find no individual detections of CO[4-3], CO[1-0] or dust, in stark contrast to the $>$60% detection rate expected for solar-enrichment galaxies with these MS Halpha SFRs. We find that both low and high density molecular gas (traced by CO[1-0] and CO[4-3] respectively) are affected by the low enrichment, showing sample average (stacked) luminosity deficits $>$0.5-0.7 dex below expectations. This is particularly pertinent for the use of high-J CO emission as a proxy of instantaneous star-formation rate. Our individual galaxy data and stacked constraints point to a strong inverse dependence $\propto Z^纬$ of gas-to-dust ratios (G/D) and CO-to-H$_{2}$ conversion factors (aco) on metallicity at z$\sim$2, with $纬_{\rm G/D}<$-2.2 and $纬_{伪_{\rm CO}}<$-0.8, respectively. We quantify the importance of comparing G/D and aco vs. metallicity trends from the literature on a common, suitably normalised metallicity scale. When accounting for systematic offsets between different metallicity scales, our z$\sim$2 constraints on these scaling relations are consistent with the corresponding relations for local galaxies. However, among those local relations, we favour those with a steep/double power-law dependence of G/D on metallicity. Finally, we discuss the implications of these findings for (a) gas mass measurements for sub-M$^{*}$ galaxies, and (b) efforts to identify the characteristic galaxy mass scale contributing most to the comoving molecular gas density at z=2. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.06390v1-abstract-full').style.display = 'none'; document.getElementById('1901.06390v1-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 January, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">15 pages, 5 figures, 3 tables. Accepted for publication in Monthly Notices of the Royal Astronomical Society</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1901.05013">arXiv:1901.05013</a> <span> [<a href="https://arxiv.org/pdf/1901.05013">pdf</a>, <a href="https://arxiv.org/format/1901.05013">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/10.1051/0004-6361/201834522">10.1051/0004-6361/201834522 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Deciphering an evolutionary sequence of merger stages in infrared-luminous starburst galaxies at z ~ 0.7 </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Daddi%2C+E">Emanuele Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Puglisi%2C+A">Annagrazia Puglisi</a>, <a href="/search/astro-ph?searchtype=author&query=Oliva%2C+E">Ernesto Oliva</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">Raphael Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Cassata%2C+P">Paolo Cassata</a>, <a href="/search/astro-ph?searchtype=author&query=Amor%C3%ADn%2C+R">Ricardo Amor铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Arimoto%2C+N">Nobuo Arimoto</a>, <a href="/search/astro-ph?searchtype=author&query=Boquien%2C+M">M茅d茅ric Boquien</a>, <a href="/search/astro-ph?searchtype=author&query=Carraro%2C+R">Rosamaria Carraro</a>, <a href="/search/astro-ph?searchtype=author&query=Delvecchio%2C+I">Ivan Delvecchio</a>, <a href="/search/astro-ph?searchtype=author&query=Ibar%2C+E">Eduardo Ibar</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+S">Shuowen Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Juneau%2C+S">St茅phanie Juneau</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+D">Daizhong Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Onodera%2C+M">Masato Onodera</a>, <a href="/search/astro-ph?searchtype=author&query=Mannucci%2C+F">Filippo Mannucci</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1nez%2C+H+M">Hugo M茅ndez Hern谩nez</a>, <a href="/search/astro-ph?searchtype=author&query=Rodighiero%2C+G">Giulia Rodighiero</a>, <a href="/search/astro-ph?searchtype=author&query=Valentino%2C+F">Francesco Valentino</a>, <a href="/search/astro-ph?searchtype=author&query=Zanella%2C+A">Anita Zanella</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="1901.05013v1-abstract-short" style="display: inline;"> Based on optical/near-IR Magellan FIRE spectra of 25 starburst galaxies at 0.5 < z < 0.9, Calabr貌 et al.(2018) showed that their attenuation properties can be explained by a single-parameter sequence of total obscurations ranging from A(V)=2 to A(V)=30 towards the starburst core centers in a mixed stars and dust configuration. We investigate here the origin of this sequence for the same sample. We… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.05013v1-abstract-full').style.display = 'inline'; document.getElementById('1901.05013v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1901.05013v1-abstract-full" style="display: none;"> Based on optical/near-IR Magellan FIRE spectra of 25 starburst galaxies at 0.5 < z < 0.9, Calabr貌 et al.(2018) showed that their attenuation properties can be explained by a single-parameter sequence of total obscurations ranging from A(V)=2 to A(V)=30 towards the starburst core centers in a mixed stars and dust configuration. We investigate here the origin of this sequence for the same sample. We show that total attenuations anti-correlate with the starburst sizes in radio (3 GHz) with a significance larger than 5sigma and a scatter of 0.26 dex. More obscured and compact starbursts also show enhanced N2 (=[NII]/Halpha) ratios and larger line velocity widths that we attribute to an increasing shock contribution toward later merger phases, driven by deeper gravitational potential wells at the coalescence. Additionally, the attenuation is also linked to the equivalent width (EW) of hydrogen recombination lines, which is sensitive to the luminosity weighted age of the relatively unobscured stellar populations. Overall, the correlations among A(V), radio size, line width, N2 and EW of Balmer/Paschen lines converge towards suggesting an evolutionary sequence of merger stages: all of these quantities are likely to be good time-tracers of the merger phenomenon, and their large spanned range appears to be characteristic of the different merger phases. Half of our sample at higher obscurations have radio sizes approximately 3 times smaller than early type galaxies at the same redshift, suggesting that, in analogy with local Ultraluminous Infrared galaxies (ULIRGs), these cores cannot be directly forming elliptical galaxies. Finally, we detect mid-IR AGN torus for half of our sample and additional X-ray emission for 6 starbursts; intriguingly, the latter have systematically more compact sizes, suggestive of emerging AGNs towards later merger stages, possibly precursors of a later QSO phase. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.05013v1-abstract-full').style.display = 'none'; document.getElementById('1901.05013v1-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 January, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">30 pages, 21 figures and 2 tables. Accepted for publication to A&A. The key result is in Fig. 3, while a Cartoon of the merger sequence is shown in Fig. 9</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 623, A64 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1810.10558">arXiv:1810.10558</a> <span> [<a href="https://arxiv.org/pdf/1810.10558">pdf</a>, <a href="https://arxiv.org/format/1810.10558">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/aaeb2c">10.3847/2041-8213/aaeb2c <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Revealing environmental dependence of molecular gas content in a distant X-ray cluster at z=2.51 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wang%2C+T">Tao Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Elbaz%2C+D">David Elbaz</a>, <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">Emanuele Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+D">Daizhong Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Kodama%2C+T">Tadayuki Kodama</a>, <a href="/search/astro-ph?searchtype=author&query=Tanaka%2C+I">Ichi Tanaka</a>, <a href="/search/astro-ph?searchtype=author&query=Schreiber%2C+C">Corentin Schreiber</a>, <a href="/search/astro-ph?searchtype=author&query=Zanella%2C+A">Anita Zanella</a>, <a href="/search/astro-ph?searchtype=author&query=Valentino%2C+F">Francesco Valentino</a>, <a href="/search/astro-ph?searchtype=author&query=Sargent%2C+M">Mark Sargent</a>, <a href="/search/astro-ph?searchtype=author&query=Kohno%2C+K">Kotaro Kohno</a>, <a href="/search/astro-ph?searchtype=author&query=Xiao%2C+M">Mengyuan Xiao</a>, <a href="/search/astro-ph?searchtype=author&query=Pannella%2C+M">Maurilio Pannella</a>, <a href="/search/astro-ph?searchtype=author&query=Ciesla%2C+L">Laure Ciesla</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">Raphael Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Koyama%2C+Y">Yusei Koyama</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="1810.10558v1-abstract-short" style="display: inline;"> We present a census of the molecular gas properties of galaxies in the most distant known X-ray cluster, CLJ1001, at z=2.51, using deep observations of CO(1-0) with JVLA. In total 14 cluster members with $M_{*} > 10^{10.5} M_{\odot}$ are detected, including all the massive star-forming members within the virial radius, providing the largest galaxy sample in a single cluster at $z > 2$ with CO(1-0)… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1810.10558v1-abstract-full').style.display = 'inline'; document.getElementById('1810.10558v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1810.10558v1-abstract-full" style="display: none;"> We present a census of the molecular gas properties of galaxies in the most distant known X-ray cluster, CLJ1001, at z=2.51, using deep observations of CO(1-0) with JVLA. In total 14 cluster members with $M_{*} > 10^{10.5} M_{\odot}$ are detected, including all the massive star-forming members within the virial radius, providing the largest galaxy sample in a single cluster at $z > 2$ with CO(1-0) measurements. We find a large variety in the gas content of these cluster galaxies, which is correlated with their relative positions (or accretion states), with those closer to the cluster core being increasingly gas-poor. Moreover, despite their low gas content, the galaxies in the cluster center exhibit an elevated star formation efficiency (SFE=SFR/$M_{\rm gas}$) compared to field galaxies, suggesting that the suppression on the SFR is likely delayed compared to that on the gas content. Their gas depletion time is around $t_{\rm dep} \sim 400$ Myrs, comparable to the cluster dynamical time. This implies that they will likely consume all their gas within a single orbit around the cluster center, and form a passive cluster core by $z\sim2$. This result is one of the first direct pieces of evidence for the influence of environment on the gas reservoirs and SFE of $z > 2$ cluster galaxies, thereby providing new insights into the rapid formation and quenching of the most massive galaxies in the early universe. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1810.10558v1-abstract-full').style.display = 'none'; document.getElementById('1810.10558v1-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 October, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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 ApJ 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/1808.10331">arXiv:1808.10331</a> <span> [<a href="https://arxiv.org/pdf/1808.10331">pdf</a>, <a href="https://arxiv.org/format/1808.10331">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/sty2394">10.1093/mnras/sty2394 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The [C II] emission as a molecular gas mass tracer in galaxies at low and high redshift </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zanella%2C+A">A. Zanella</a>, <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">E. Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Magdis%2C+G">G. Magdis</a>, <a href="/search/astro-ph?searchtype=author&query=Santos%2C+T+D">T. Diaz Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Cormier%2C+D">D. Cormier</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+D">D. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Cibinel%2C+A">A. Cibinel</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">R. Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">M. Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Sargent%2C+M">M. Sargent</a>, <a href="/search/astro-ph?searchtype=author&query=Popping%2C+G">G. Popping</a>, <a href="/search/astro-ph?searchtype=author&query=Madden%2C+S+C">S. C. Madden</a>, <a href="/search/astro-ph?searchtype=author&query=Bethermin%2C+M">M. Bethermin</a>, <a href="/search/astro-ph?searchtype=author&query=Hughes%2C+T+M">T. M. Hughes</a>, <a href="/search/astro-ph?searchtype=author&query=Valentino%2C+F">F. Valentino</a>, <a href="/search/astro-ph?searchtype=author&query=Rujopakarn%2C+W">W. Rujopakarn</a>, <a href="/search/astro-ph?searchtype=author&query=Pannella%2C+M">M. Pannella</a>, <a href="/search/astro-ph?searchtype=author&query=Bournaud%2C+F">F. Bournaud</a>, <a href="/search/astro-ph?searchtype=author&query=Walter%2C+F">F. Walter</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+T">T. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Elbaz%2C+D">D. Elbaz</a>, <a href="/search/astro-ph?searchtype=author&query=Coogan%2C+R+T">R. T. Coogan</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="1808.10331v1-abstract-short" style="display: inline;"> We present ALMA Band 9 observations of the [C II]158um emission for a sample of 10 main-sequence galaxies at redshift z ~ 2, with typical stellar masses (log M*/Msun ~ 10.0 - 10.9) and star formation rates (~ 35 - 115 Msun/yr). Given the strong and well understood evolution of the interstellar medium from the present to z = 2, we investigate the behaviour of the [C II] emission and empirically ide… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.10331v1-abstract-full').style.display = 'inline'; document.getElementById('1808.10331v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1808.10331v1-abstract-full" style="display: none;"> We present ALMA Band 9 observations of the [C II]158um emission for a sample of 10 main-sequence galaxies at redshift z ~ 2, with typical stellar masses (log M*/Msun ~ 10.0 - 10.9) and star formation rates (~ 35 - 115 Msun/yr). Given the strong and well understood evolution of the interstellar medium from the present to z = 2, we investigate the behaviour of the [C II] emission and empirically identify its primary driver. We detect [C II] from six galaxies (four secure, two tentative) and estimate ensemble averages including non detections. The [C II]-to-infrared luminosity ratio (L[C II]/LIR) of our sample is similar to that of local main-sequence galaxies (~ 2 x 10^-3), and ~ 10 times higher than that of starbursts. The [C II] emission has an average spatial extent of 4 - 7 kpc, consistent with the optical size. Complementing our sample with literature data, we find that the [C II] luminosity correlates with galaxies' molecular gas mass, with a mean absolute deviation of 0.2 dex and without evident systematics: the [C II]-to-H2 conversion factor (alpha_[C II] ~ 30 Msun/Lsun) is largely independent of galaxies' depletion time, metallicity, and redshift. [C II] seems therefore a convenient tracer to estimate galaxies' molecular gas content regardless of their starburst or main-sequence nature, and extending to metal-poor galaxies at low and high redshifts. The dearth of [C II] emission reported for z > 6 - 7 galaxies might suggest either a high star formation efficiency or a small fraction of UV light from star formation reprocessed by dust. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.10331v1-abstract-full').style.display = 'none'; document.getElementById('1808.10331v1-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 August, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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 MNRAS. 28 pages, including 12 figures, 5 tables, 3 appendices</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1807.04350">arXiv:1807.04350</a> <span> [<a href="https://arxiv.org/pdf/1807.04350">pdf</a>, <a href="https://arxiv.org/format/1807.04350">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/10.3847/2041-8213/aad33e">10.3847/2041-8213/aad33e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Near-infrared emission lines in starburst galaxies at 0.5 < z < 0.9 : Discovery of a merger sequence of extreme obscurations </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Daddi%2C+E">Emanuele Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Cassata%2C+P">Paolo Cassata</a>, <a href="/search/astro-ph?searchtype=author&query=Onodera%2C+M">Masato Onodera</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">Raphael Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Puglisi%2C+A">Annagrazia Puglisi</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+S">Shuowen Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+D">Daizhong Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Amor%C3%ADn%2C+R">Ricardo Amor铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Arimoto%2C+N">Nobuo Arimoto</a>, <a href="/search/astro-ph?searchtype=author&query=Boquien%2C+M">M茅d茅ric Boquien</a>, <a href="/search/astro-ph?searchtype=author&query=Carraro%2C+R">Rosamaria Carraro</a>, <a href="/search/astro-ph?searchtype=author&query=Elbaz%2C+D">David Elbaz</a>, <a href="/search/astro-ph?searchtype=author&query=Ibar%2C+E">Eduardo Ibar</a>, <a href="/search/astro-ph?searchtype=author&query=Juneau%2C+S">St茅phanie Juneau</a>, <a href="/search/astro-ph?searchtype=author&query=Mannucci%2C+F">Filippo Mannucci</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1nez%2C+H+M">Hugo M茅ndez Hern谩nez</a>, <a href="/search/astro-ph?searchtype=author&query=Oliva%2C+E">Ernesto Oliva</a>, <a href="/search/astro-ph?searchtype=author&query=Rodighiero%2C+G">Giulia Rodighiero</a>, <a href="/search/astro-ph?searchtype=author&query=Valentino%2C+F+M">Francesco M. Valentino</a>, <a href="/search/astro-ph?searchtype=author&query=Zanella%2C+A">Anita Zanella</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1807.04350v1-abstract-short" style="display: inline;"> We obtained optical/near-IR rest-frame Magellan FIRE spectra (including Pa$尾$ and Pa$纬$) of 25 starburst galaxies at 0.5<z<0.9, with average star formation rates (SFR) x7 above the Main Sequence (MS). We find that Paschen-to-Balmer line ratios saturate around a constant value corresponding to $A_{\rm V}\sim$2-3 mag, while line to IR luminosity ratios suggest a large range of more extreme obscurati… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.04350v1-abstract-full').style.display = 'inline'; document.getElementById('1807.04350v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1807.04350v1-abstract-full" style="display: none;"> We obtained optical/near-IR rest-frame Magellan FIRE spectra (including Pa$尾$ and Pa$纬$) of 25 starburst galaxies at 0.5<z<0.9, with average star formation rates (SFR) x7 above the Main Sequence (MS). We find that Paschen-to-Balmer line ratios saturate around a constant value corresponding to $A_{\rm V}\sim$2-3 mag, while line to IR luminosity ratios suggest a large range of more extreme obscurations and appear to be uncorrelated to the former. This behavior is not consistent with standard attenuation laws derived for local and distant galaxies, while being remarkably consistent with observations of starburst cores in which young stars and dust are homogeneously mixed. This model implies $A_{\rm V}=$2-30 mag attenuation to the center of starburst cores, with a median of ~9 mag (a factor of 4000). X-ray hardness ratios for 6 AGNs in our sample and column densities derived from observed dust masses and radio sizes independently confirm this level of attenuation. In these conditions observed optical/near-IR emission comes from surface regions, while inner starburst cores are invisible. We thus attribute the high [NII]/H$伪$ ratios to widespread shocks from accretion, turbulence and dynamic disturbances rather than to AGNs. The large range of optical depths demonstrates that substantial diversity is present within the starburst population, possibly connected to different merger phases or progenitor properties. The majority of our targets are, in fact, morphologically classified as mergers. We argue that the extreme obscuration provides in itself smoking gun evidence of their merger origin, and a powerful tool for identifying mergers at even higher redshifts. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.04350v1-abstract-full').style.display = 'none'; document.getElementById('1807.04350v1-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 July, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">ApJ Letters in press; the key result is in Figure 4 (left)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1806.06856">arXiv:1806.06856</a> <span> [<a href="https://arxiv.org/pdf/1806.06856">pdf</a>, <a href="https://arxiv.org/format/1806.06856">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/10.3847/1538-4357/aacd10">10.3847/1538-4357/aacd10 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Deciphering the activity and quiescence of high-redshift cluster environments: ALMA observations of ClJ1449+0856 at z=2 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Strazzullo%2C+V">V. Strazzullo</a>, <a href="/search/astro-ph?searchtype=author&query=Coogan%2C+R+T">R. T. Coogan</a>, <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">E. Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Sargent%2C+M+T">M. T. Sargent</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">R. Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Valentino%2C+F">F. Valentino</a>, <a href="/search/astro-ph?searchtype=author&query=Bethermin%2C+M">M. Bethermin</a>, <a href="/search/astro-ph?searchtype=author&query=Pannella%2C+M">M. Pannella</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">M. Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Renzini%2C+A">A. Renzini</a>, <a href="/search/astro-ph?searchtype=author&query=Arimoto%2C+N">N. Arimoto</a>, <a href="/search/astro-ph?searchtype=author&query=Cimatti%2C+A">A. Cimatti</a>, <a href="/search/astro-ph?searchtype=author&query=Dannerbauer%2C+H">H. Dannerbauer</a>, <a href="/search/astro-ph?searchtype=author&query=Finoguenov%2C+A">A. Finoguenov</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+D">D. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Onodera%2C+M">M. Onodera</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="1806.06856v1-abstract-short" style="display: inline;"> We present ALMA observations of the 870$渭$m continuum and CO(4-3) line emission in the core of the galaxy cluster ClJ1449+0856 at z=2, a NIR-selected, X-ray detected system in the mass range of typical progenitors of today's massive clusters. The 870$渭$m map reveals six F$_{870渭m}$ > 0.5 mJy sources spread over an area of 0.07 arcmin$^2$, giving an overdensity of a factor ~10 (6) with respect to b… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.06856v1-abstract-full').style.display = 'inline'; document.getElementById('1806.06856v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1806.06856v1-abstract-full" style="display: none;"> We present ALMA observations of the 870$渭$m continuum and CO(4-3) line emission in the core of the galaxy cluster ClJ1449+0856 at z=2, a NIR-selected, X-ray detected system in the mass range of typical progenitors of today's massive clusters. The 870$渭$m map reveals six F$_{870渭m}$ > 0.5 mJy sources spread over an area of 0.07 arcmin$^2$, giving an overdensity of a factor ~10 (6) with respect to blank field counts down to F$_{870渭m}$ > 1 (0.5) mJy. On the other hand, deep CO(4-3) follow-up confirms membership of three of these sources, but suggests that the remaining three, including the brightest 870$渭$m sources in the field (F$_{870渭m}\gtrsim$2 mJy), are likely interlopers. The measurement of 870$渭$m continuum and CO(4-3) line fluxes at the positions of previously-known cluster members provides a deep probe of dusty star formation occurring in the core of this high-redshift structure, adding up to a total SFR~700$\pm$100 M$_{\odot}$/yr and yielding an integrated star formation rate density of ~10$^4$ M$_{\odot}$/yr/Mpc$^3$, five orders of magnitude larger than in the field at the same epoch, due to the concentration of star-forming galaxies in the small volume of the dense cluster core. The combination of these observations with previously available HST imaging highlights the presence in this same volume of a population of galaxies with already suppressed star formation. This diverse composition of galaxy populations in ClJ1449+0856 is especially highlighted at the very cluster center, where a complex assembly of quiescent and star-forming sources is likely forming the future Brightest Cluster Galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.06856v1-abstract-full').style.display = 'none'; document.getElementById('1806.06856v1-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 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">11 pages, 6 figures, ApJ in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1805.09789">arXiv:1805.09789</a> <span> [<a href="https://arxiv.org/pdf/1805.09789">pdf</a>, <a href="https://arxiv.org/format/1805.09789">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/sty1446">10.1093/mnras/sty1446 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Merger driven star-formation activity in Cl J1449+0856 at z=1.99 as seen by ALMA and JVLA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Coogan%2C+R+T">R. T. Coogan</a>, <a href="/search/astro-ph?searchtype=author&query=Daddi%2C+E">E. Daddi</a>, <a href="/search/astro-ph?searchtype=author&query=Sargent%2C+M+T">M. T. Sargent</a>, <a href="/search/astro-ph?searchtype=author&query=Strazzullo%2C+V">V. Strazzullo</a>, <a href="/search/astro-ph?searchtype=author&query=Valentino%2C+F">F. Valentino</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">R. Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Magdis%2C+G">G. Magdis</a>, <a href="/search/astro-ph?searchtype=author&query=Bethermin%2C+M">M. Bethermin</a>, <a href="/search/astro-ph?searchtype=author&query=Pannella%2C+M">M. Pannella</a>, <a href="/search/astro-ph?searchtype=author&query=Onodera%2C+M">M. Onodera</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+D">D. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Cimatti%2C+A">A. Cimatti</a>, <a href="/search/astro-ph?searchtype=author&query=Dannerbauer%2C+H">H. Dannerbauer</a>, <a href="/search/astro-ph?searchtype=author&query=Carollo%2C+M">M. Carollo</a>, <a href="/search/astro-ph?searchtype=author&query=Renzini%2C+A">A. Renzini</a>, <a href="/search/astro-ph?searchtype=author&query=Tremou%2C+E">E. Tremou</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="1805.09789v1-abstract-short" style="display: inline;"> We use ALMA and JVLA observations of the galaxy cluster Cl J1449+0856 at z=1.99, in order to study how dust-obscured star-formation, ISM content and AGN activity are linked to environment and galaxy interactions during the crucial phase of high-z cluster assembly. We present detections of multiple transitions of $^{12}$CO, as well as dust continuum emission detections from 11 galaxies in the core… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.09789v1-abstract-full').style.display = 'inline'; document.getElementById('1805.09789v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1805.09789v1-abstract-full" style="display: none;"> We use ALMA and JVLA observations of the galaxy cluster Cl J1449+0856 at z=1.99, in order to study how dust-obscured star-formation, ISM content and AGN activity are linked to environment and galaxy interactions during the crucial phase of high-z cluster assembly. We present detections of multiple transitions of $^{12}$CO, as well as dust continuum emission detections from 11 galaxies in the core of Cl J1449+0856. We measure the gas excitation properties, star-formation rates, gas consumption timescales and gas-to-stellar mass ratios for the galaxies. We find evidence for a large fraction of galaxies with highly-excited molecular gas, contributing $>$50% to the total SFR in the cluster core. We compare these results with expectations for field galaxies, and conclude that environmental influences have strongly enhanced the fraction of excited galaxies in this cluster. We find a dearth of molecular gas in the galaxies' gas reservoirs, implying a high star-formation efficiency (SFE) in the cluster core, and find short gas depletion timescales $蟿$<0.1-0.4 Gyrs for all galaxies. Interestingly, we do not see evidence for increased specific star-formation rates (sSFRs) in the cluster galaxies, despite their high SFEs and gas excitations. We find evidence for a large number of mergers in the cluster core, contributing a large fraction of the core's total star-formation compared with expectations in the field. We conclude that the environmental impact on the galaxy excitations is linked to the high rate of galaxy mergers, interactions and active galactic nuclei in the cluster core. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.09789v1-abstract-full').style.display = 'none'; document.getElementById('1805.09789v1-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 May, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">29 pages, 15 figures, 7 tables + Appendix. 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/1803.02375">arXiv:1803.02375</a> <span> [<a href="https://arxiv.org/pdf/1803.02375">pdf</a>, <a href="https://arxiv.org/format/1803.02375">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/sty617">10.1093/mnras/sty617 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Kormendy Relation of Galaxies in the Frontier Fields Clusters: Abell S1063 and MACS J1149.5+2223 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Tortorelli%2C+L">Luca Tortorelli</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">Amata Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Paolillo%2C+M">Maurizio Paolillo</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">Piero Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Gargiulo%2C+A">Adriana Gargiulo</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">Raphael Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Balestra%2C+I">Italo Balestra</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=Annunziatella%2C+M">Marianna Annunziatella</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">Claudio Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Lombardi%2C+M">Marco Lombardi</a>, <a href="/search/astro-ph?searchtype=author&query=Nonino%2C+M">Mario Nonino</a>, <a href="/search/astro-ph?searchtype=author&query=Rettura%2C+A">Alessandro Rettura</a>, <a href="/search/astro-ph?searchtype=author&query=Sartoris%2C+B">Barbara Sartoris</a>, <a href="/search/astro-ph?searchtype=author&query=Strazzullo%2C+V">Veronica Strazzullo</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="1803.02375v1-abstract-short" style="display: inline;"> We analyse the Kormendy relations (KRs) of the two Frontier Fields clusters, Abell S1063, at z = 0.348, and MACS J1149.5+2223, at z = 0.542, exploiting very deep Hubble Space Telescope photometry and VLT/MUSE integral field spectroscopy. With this novel dataset, we are able to investigate how the KR parameters depend on the cluster galaxy sample selection and how this affects studies of galaxy evo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1803.02375v1-abstract-full').style.display = 'inline'; document.getElementById('1803.02375v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1803.02375v1-abstract-full" style="display: none;"> We analyse the Kormendy relations (KRs) of the two Frontier Fields clusters, Abell S1063, at z = 0.348, and MACS J1149.5+2223, at z = 0.542, exploiting very deep Hubble Space Telescope photometry and VLT/MUSE integral field spectroscopy. With this novel dataset, we are able to investigate how the KR parameters depend on the cluster galaxy sample selection and how this affects studies of galaxy evolution based on the KR. We define and compare four different galaxy samples according to: (a) S茅rsic indices: early-type ('ETG'), (b) visual inspection: 'ellipticals', (c) colours: 'red', (d) spectral properties: 'passive'. The classification is performed for a complete sample of galaxies with m$_{\textit{F814W}} \le$ 22.5 ABmag (M$_{*}$ $\gtrsim 10^{10.0}$ M$_{\odot}$). To derive robust galaxy structural parameters, we use two methods: (1) an iterative estimate of structural parameters using images of increasing size, in order to deal with closely separated galaxies and (2) different background estimations, to deal with the Intracluster light contamination. The comparison between the KRs obtained from the different samples suggests that the sample selection could affect the estimate of the best-fitting KR parameters. The KR built with ETGs is fully consistent with the one obtained for ellipticals and passive. On the other hand, the KR slope built on the red sample is only marginally consistent with those obtained with the other samples. We also release the photometric catalogue with structural parameters for the galaxies included in the present analysis. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1803.02375v1-abstract-full').style.display = 'none'; document.getElementById('1803.02375v1-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 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">23 pages, 18 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/1801.06546">arXiv:1801.06546</a> <span> [<a href="https://arxiv.org/pdf/1801.06546">pdf</a>, <a href="https://arxiv.org/format/1801.06546">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/sty175">10.1093/mnras/sty175 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Kinematics of the SN Refsdal host revealed by MUSE: a regularly rotating spiral galaxy at z~1.5 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Di+Teodoro%2C+E+M">E. M. Di Teodoro</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Fraternali%2C+F">F. Fraternali</a>, <a href="/search/astro-ph?searchtype=author&query=Gobat%2C+R">R. Gobat</a>, <a href="/search/astro-ph?searchtype=author&query=Karman%2C+W">W. Karman</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">A. Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Balestra%2C+I">I. Balestra</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+I">K. I. Caputi</a>, <a href="/search/astro-ph?searchtype=author&query=Lombardi%2C+M">M. Lombardi</a>, <a href="/search/astro-ph?searchtype=author&query=Suyu%2C+S+H">S. H. Suyu</a>, <a href="/search/astro-ph?searchtype=author&query=Treu%2C+T">T. Treu</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="1801.06546v2-abstract-short" style="display: inline;"> We use Multi Unit Spectroscopic Explorer (MUSE) observations of the galaxy cluster MACS J1149.5+2223 to explore the kinematics of the grand-design spiral galaxy Sp1149 hosting the SN Refsdal. Sp1149 lies at $z\simeq1.49$, has a stellar mass $M_*\simeq5\times10^9 \, \mathrm{M_\odot}$, a star-formation rate $\mathrm{SFR} \simeq1-6 \, \mathrm{M_\odot/yr}$ and represents a likely progenitor of a Milky… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.06546v2-abstract-full').style.display = 'inline'; document.getElementById('1801.06546v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1801.06546v2-abstract-full" style="display: none;"> We use Multi Unit Spectroscopic Explorer (MUSE) observations of the galaxy cluster MACS J1149.5+2223 to explore the kinematics of the grand-design spiral galaxy Sp1149 hosting the SN Refsdal. Sp1149 lies at $z\simeq1.49$, has a stellar mass $M_*\simeq5\times10^9 \, \mathrm{M_\odot}$, a star-formation rate $\mathrm{SFR} \simeq1-6 \, \mathrm{M_\odot/yr}$ and represents a likely progenitor of a Milky-Way-like galaxy. All the four multiple images of Sp1149 in our data show strong OII-line emissions pointing to a clear rotation pattern. We take advantage of the gravitational lensing magnification effect ($\simeq 4 \times$) on the OII emission of the least distorted image to fit 3D kinematic models to the MUSE data-cube and derive the rotation curve and the velocity dispersion profile of Sp1149. We find that the rotation curve steeply rises, peaks at $R\simeq1$ kpc and then (initially) declines and flattens to an average $V_\mathrm{flat} = 128^{+29}_{-19}$ km/s. The shape of the rotation curve is well determined but the actual value of $V_\mathrm{flat}$ is quite uncertain because of the nearly face-on configuration of the galaxy. The intrinsic velocity dispersion due to gas turbulence is almost constant across the entire disc with an average of $27\pm5$ km/s. This value is consistent with $z=0$ measurements in the ionized gas component and a factor 2-4 lower than other estimates in different galaxies at similar redshifts. The average stellar-to-total mass fraction is of the order of one fifth. Our kinematic analysis returns the picture of a regular star-forming, mildly turbulent, rotation-dominated ($V / 蟽\simeq5$) spiral galaxy in a 4 Gyr old Universe. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.06546v2-abstract-full').style.display = 'none'; document.getElementById('1801.06546v2-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 February, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 January, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">10 pages, 5 figures. Accepted for publication in MNRAS</span> </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=Gobat%2C+R&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Gobat%2C+R&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Gobat%2C+R&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Gobat%2C+R&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </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> 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