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</div> <div class="control"> <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=Gallazzi%2C+A&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Gallazzi%2C+A&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Gallazzi%2C+A&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Gallazzi%2C+A&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/2408.12442">arXiv:2408.12442</a> <span> [<a href="https://arxiv.org/pdf/2408.12442">pdf</a>, <a href="https://arxiv.org/format/2408.12442">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> From Halos to Galaxies. VI. Improved halo mass estimation for SDSS groups and measurement of the halo mass function </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zhao%2C+D">Dingyi Zhao</a>, <a href="/search/astro-ph?searchtype=author&query=Peng%2C+Y">Yingjie Peng</a>, <a href="/search/astro-ph?searchtype=author&query=Jing%2C+Y">Yipeng Jing</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+X">Xiaohu Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Ho%2C+L+C">Luis C. Ho</a>, <a href="/search/astro-ph?searchtype=author&query=Renzini%2C+A">Alvio Renzini</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A+R">Anna R. Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Lyu%2C+C">Cheqiu Lyu</a>, <a href="/search/astro-ph?searchtype=author&query=Maiolino%2C+R">Roberto Maiolino</a>, <a href="/search/astro-ph?searchtype=author&query=Dou%2C+J">Jing Dou</a>, <a href="/search/astro-ph?searchtype=author&query=Gao%2C+Z">Zeyu Gao</a>, <a href="/search/astro-ph?searchtype=author&query=Gu%2C+Q">Qiusheng Gu</a>, <a href="/search/astro-ph?searchtype=author&query=Mannucci%2C+F">Filippo Mannucci</a>, <a href="/search/astro-ph?searchtype=author&query=Mo%2C+H">Houjun Mo</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+B">Bitao Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+E">Enci Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+K">Kai Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+Y">Yu-Chen Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+B">Bingxiao Xu</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+F">Feng Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Zhu%2C+X">Xingye Zhu</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.12442v1-abstract-short" style="display: inline;"> In $螞$CDM cosmology, galaxies form and evolve in their host dark matter (DM) halos. Halo mass is crucial for understanding the halo-galaxy connection. The abundance matching (AM) technique has been widely used to derive the halo masses of galaxy groups. However, quenching of the central galaxy can decouple the coevolution of its stellar mass and DM halo mass. Different halo assembly histories can… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.12442v1-abstract-full').style.display = 'inline'; document.getElementById('2408.12442v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.12442v1-abstract-full" style="display: none;"> In $螞$CDM cosmology, galaxies form and evolve in their host dark matter (DM) halos. Halo mass is crucial for understanding the halo-galaxy connection. The abundance matching (AM) technique has been widely used to derive the halo masses of galaxy groups. However, quenching of the central galaxy can decouple the coevolution of its stellar mass and DM halo mass. Different halo assembly histories can also result in significantly different final stellar mass of the central galaxies. These processes can introduce substantial uncertainties in the halo masses derived from the AM method, particularly leading to a systematic bias between groups with star-forming centrals (blue groups) and passive centrals (red groups). To improve, we developed a new machine learning (ML) algorithm that accounts for these effects and is trained on simulations. Our results show that the ML method eliminates the systematic bias in the derived halo masses for blue and red groups and is, on average, $\sim1/3$ more accurate than the AM method. With careful calibration of observable quantities from simulations and observations from SDSS, we apply our ML model to the SDSS Yang et al. groups to derive their halo masses down to $10^{11.5}\mathrm{M_\odot}$ or even lower. The derived SDSS group halo mass function agrees well with the theoretical predictions, and the derived stellar-to-halo mass relations for both red and blue groups matches well with those obtained from direct weak lensing measurements. These new halo mass estimates enable more accurate investigation of the galaxy-halo connection and the role of the halos in galaxy evolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.12442v1-abstract-full').style.display = 'none'; document.getElementById('2408.12442v1-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 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 9 figures. Submitted to ApJ, comments welcome!</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.07749">arXiv:2408.07749</a> <span> [<a href="https://arxiv.org/pdf/2408.07749">pdf</a>, <a href="https://arxiv.org/format/2408.07749">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"> From Halos to Galaxies. X: Decoding Galaxy SEDs with Physical Priors and Accurate Star Formation History Reconstruction </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gao%2C+Z">Zeyu Gao</a>, <a href="/search/astro-ph?searchtype=author&query=Peng%2C+Y">Yingjie Peng</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+K">Kai Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Ho%2C+L+C">Luis C. Ho</a>, <a href="/search/astro-ph?searchtype=author&query=Renzini%2C+A">Alvio Renzini</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A+R">Anna R. Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Mannucci%2C+F">Filippo Mannucci</a>, <a href="/search/astro-ph?searchtype=author&query=Mo%2C+H">Houjun Mo</a>, <a href="/search/astro-ph?searchtype=author&query=Jing%2C+Y">Yipeng Jing</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+X">Xiaohu Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+E">Enci Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhao%2C+D">Dingyi Zhao</a>, <a href="/search/astro-ph?searchtype=author&query=Dou%2C+J">Jing Dou</a>, <a href="/search/astro-ph?searchtype=author&query=Gu%2C+Q">Qiusheng Gu</a>, <a href="/search/astro-ph?searchtype=author&query=Lyu%2C+C">Cheqiu Lyu</a>, <a href="/search/astro-ph?searchtype=author&query=Maiolino%2C+R">Roberto Maiolino</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+B">Bitao Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+Y">Yu-Chen Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+B">Bingxiao Xu</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+F">Feng Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Zhu%2C+X">Xingye Zhu</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.07749v1-abstract-short" style="display: inline;"> The spectral energy distribution (SED) of galaxies is essential for deriving fundamental properties like stellar mass and star formation history (SFH). However, conventional methods, including both parametric and non-parametric approaches, often fail to accurately recover the observed cosmic star formation rate (SFR) density due to oversimplified or unrealistic assumptions about SFH and their inab… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.07749v1-abstract-full').style.display = 'inline'; document.getElementById('2408.07749v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.07749v1-abstract-full" style="display: none;"> The spectral energy distribution (SED) of galaxies is essential for deriving fundamental properties like stellar mass and star formation history (SFH). However, conventional methods, including both parametric and non-parametric approaches, often fail to accurately recover the observed cosmic star formation rate (SFR) density due to oversimplified or unrealistic assumptions about SFH and their inability to account for the complex SFH variations across different galaxy populations. To address this issue, we introduce a novel approach that improves galaxy broad-band SED analysis by incorporating physical priors derived from hydrodynamical simulations. Tests using IllustrisTNG simulations demonstrate that our method can reliably determine galaxy physical properties from broad-band photometry, including stellar mass within 0.05 dex, current SFR within 0.3 dex, and fractional stellar formation time within 0.2 dex, with a negligible fraction of catastrophic failures. When applied to the SDSS main photometric galaxy sample with spectroscopic redshift, our estimates of stellar mass and SFR are consistent with the widely-used MPA-JHU and GSWLC catalogs. Notably, using the derived SFHs of individual SDSS galaxies, we estimate the cosmic SFR density and stellar mass density with remarkable consistency to direct observations up to $z \sim 6$. This marks the first time SFHs derived from SEDs can accurately match observations. Consequently, our method can reliably recover observed spectral indices such as $\rm D_{\rm n}(4000)$ and $\rm H未_{\rm A}$ by synthesizing the full spectra of galaxies using the estimated SFHs and metal enrichment histories, relying solely on broad-band photometry as input. Furthermore, this method is extremely computationally efficient compared to conventional approaches. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.07749v1-abstract-full').style.display = 'none'; document.getElementById('2408.07749v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 12 figures. Submitted to ApJ, comments welcome!</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.10974">arXiv:2407.10974</a> <span> [<a href="https://arxiv.org/pdf/2407.10974">pdf</a>, <a href="https://arxiv.org/format/2407.10974">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/stae1739">10.1093/mnras/stae1739 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Age and metal gradients in massive quiescent galaxies at $0.6 \lesssim z \lesssim 1.0$: implications for quenching and assembly histories </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+C+M">Chloe M. Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Kriek%2C+M">Mariska Kriek</a>, <a href="/search/astro-ph?searchtype=author&query=Beverage%2C+A+G">Aliza G. Beverage</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Wel%2C+A">Arjen van der Wel</a>, <a href="/search/astro-ph?searchtype=author&query=Bezanson%2C+R">Rachel Bezanson</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Eugenio%2C+F">Francesco D'Eugenio</a>, <a href="/search/astro-ph?searchtype=author&query=Franx%2C+M">Marijn Franx</a>, <a href="/search/astro-ph?searchtype=author&query=Pi%C3%B1a%2C+P+E+M">Pavel E. Mancera Pi帽a</a>, <a href="/search/astro-ph?searchtype=author&query=Nersesian%2C+A">Angelos Nersesian</a>, <a href="/search/astro-ph?searchtype=author&query=Slob%2C+M">Martje Slob</a>, <a href="/search/astro-ph?searchtype=author&query=Suess%2C+K+A">Katherine A. Suess</a>, <a href="/search/astro-ph?searchtype=author&query=van+Dokkum%2C+P+G">Pieter G. van Dokkum</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+P">Po-Feng Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">Anna Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Zibetti%2C+S">Stefano Zibetti</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.10974v2-abstract-short" style="display: inline;"> We present spatially resolved, simple stellar population equivalent ages, stellar metallicities, and abundance ratios for 456 massive ($10.3\lesssim\log(\mathrm{M}_*/\mathrm{M}_\odot)\lesssim11.8$) quiescent galaxies at $0.6\lesssim z\lesssim1.0$ from the Large Early Galaxy Astrophysics Census, derived using full-spectrum models. Typically, we find flat age and [Mg/Fe] gradients, and negative [Fe/… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.10974v2-abstract-full').style.display = 'inline'; document.getElementById('2407.10974v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.10974v2-abstract-full" style="display: none;"> We present spatially resolved, simple stellar population equivalent ages, stellar metallicities, and abundance ratios for 456 massive ($10.3\lesssim\log(\mathrm{M}_*/\mathrm{M}_\odot)\lesssim11.8$) quiescent galaxies at $0.6\lesssim z\lesssim1.0$ from the Large Early Galaxy Astrophysics Census, derived using full-spectrum models. Typically, we find flat age and [Mg/Fe] gradients, and negative [Fe/H] gradients, implying iron-rich cores. We also estimate intrinsic [Fe/H] gradients via forward modelling. We examine the observed gradients in three age bins. Younger quiescent galaxies typically have negative [Fe/H] gradients and positive age gradients, possibly indicating a recent central starburst. Additionally, this finding suggests that photometrically measured flat colour gradients in young quiescent galaxies are the result of the positive age and negative metallicity gradients cancelling each other. For older quiescent galaxies, the age gradients become flat and [Fe/H] gradients weaken, though remain negative. Thus, negative colour gradients at older ages are likely driven by metallicity gradients. The diminishing age gradient may result from the starburst fading. Furthermore, the persistence of the [Fe/H] gradients may suggest that the outskirts are simultaneously built up by mergers with lower metallicity satellites. On the other hand, the gradients could be inherited from the star-forming phase, in which case mergers may not be needed to explain our findings. This work illustrates the need for resolved spectroscopy, instead of just photometry, to measure stellar population gradients. Extending these measurements to higher redshift is imperative for understanding how stellar populations in quiescent galaxies are assembled over cosmic time. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.10974v2-abstract-full').style.display = 'none'; document.getElementById('2407.10974v2-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 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 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">Accepted for publication in MNRAS; minor typesetting corrections after copyediting</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> MN-24-1137-MJ </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.06264">arXiv:2407.06264</a> <span> [<a href="https://arxiv.org/pdf/2407.06264">pdf</a>, <a href="https://arxiv.org/format/2407.06264">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1117/12.3018977">10.1117/12.3018977 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> SHARP -- A near-IR multi-mode spectrograph conceived for MORFEO@ELT </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Saracco%2C+P">P. Saracco</a>, <a href="/search/astro-ph?searchtype=author&query=Conconi%2C+P">P. Conconi</a>, <a href="/search/astro-ph?searchtype=author&query=Arcidiacono%2C+C">C. Arcidiacono</a>, <a href="/search/astro-ph?searchtype=author&query=Portaluri%2C+E">E. Portaluri</a>, <a href="/search/astro-ph?searchtype=author&query=Mahmoodzadeh%2C+H">H. Mahmoodzadeh</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Orazi%2C+V">V. D'Orazi</a>, <a href="/search/astro-ph?searchtype=author&query=Fedele%2C+D">D. Fedele</a>, <a href="/search/astro-ph?searchtype=author&query=Gargiulo%2C+A">A. Gargiulo</a>, <a href="/search/astro-ph?searchtype=author&query=Vanzella%2C+E">E. Vanzella</a>, <a href="/search/astro-ph?searchtype=author&query=Franzetti%2C+P">P. Franzetti</a>, <a href="/search/astro-ph?searchtype=author&query=Arosio%2C+I">I. Arosio</a>, <a href="/search/astro-ph?searchtype=author&query=Barbalini%2C+L">L. Barbalini</a>, <a href="/search/astro-ph?searchtype=author&query=Lops%2C+G">G. Lops</a>, <a href="/search/astro-ph?searchtype=author&query=Molinari%2C+E">E. Molinari</a>, <a href="/search/astro-ph?searchtype=author&query=Cascone%2C+E">E. Cascone</a>, <a href="/search/astro-ph?searchtype=author&query=Cianniello%2C+V">V. Cianniello</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Auria%2C+D">D. D'Auria</a>, <a href="/search/astro-ph?searchtype=author&query=De+Caprio%2C+V">V. De Caprio</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Antonio%2C+I">I. Di Antonio</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Francesco%2C+B">B. Di Francesco</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Rico%2C+G">G. Di Rico</a>, <a href="/search/astro-ph?searchtype=author&query=Eredia%2C+C">C. Eredia</a>, <a href="/search/astro-ph?searchtype=author&query=Fumana%2C+M">M. Fumana</a>, <a href="/search/astro-ph?searchtype=author&query=Greggio%2C+D">D. Greggio</a>, <a href="/search/astro-ph?searchtype=author&query=Rodeghiero%2C+G">G. Rodeghiero</a> , et al. (28 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="2407.06264v3-abstract-short" style="display: inline;"> The Extremely Large Telescopes (ELTs), thanks to their large apertures and cutting-edge Multi-Conjugate Adaptive Optics (MCAO) systems, promise to deliver sharper and deeper data even than the JWST. SHARP is a concept study for a near-IR (0.95-2.45 $渭$m) spectrograph conceived to fully exploit the collecting area and the angular resolution of the upcoming generation of ELTs. In particular, SHARP i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.06264v3-abstract-full').style.display = 'inline'; document.getElementById('2407.06264v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.06264v3-abstract-full" style="display: none;"> The Extremely Large Telescopes (ELTs), thanks to their large apertures and cutting-edge Multi-Conjugate Adaptive Optics (MCAO) systems, promise to deliver sharper and deeper data even than the JWST. SHARP is a concept study for a near-IR (0.95-2.45 $渭$m) spectrograph conceived to fully exploit the collecting area and the angular resolution of the upcoming generation of ELTs. In particular, SHARP is designed for the 2nd port of MORFEO@ELT. Composed of a Multi-Object Spectrograph, NEXUS, and a multi-Integral Field Unit, VESPER, MORFEO-SHARP will deliver high angular ($\sim$30 mas) and spectral (R$\simeq$300, 2000, 6000, 17000) resolution, outperforming NIRSpec@JWST (100 mas). SHARP will enable studies of the nearby Universe and the early Universe in unprecedented detail. NEXUS is fed by a configurable slit system deploying up to 30 slits with $\sim$2.4 arcsec length and adjustable width, over a field of about 1.2"$\times$1.2" (35 mas/pix). Each slit is fed by an inversion prism able to rotate by an arbitrary angle the field that can be seen by the slit. VESPER is composed of 12 probes of 1.7"$\times$1.5" each (spaxel 31 mas) probing a field 24"$\times$70". SHARP is conceived to exploit the ELTs apertures reaching the faintest flux and the sharpest angular resolution by joining the sensitivity of NEXUS and the high spatial sampling of VESPER to MORFEO capabilities. This article provides an overview of the scientific design drivers, their solutions, and the resulting optical design of the instrument achieving the required optical performance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.06264v3-abstract-full').style.display = 'none'; document.getElementById('2407.06264v3-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 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">Proceedings of the SPIE Astronomical Telescopes and Instrumentation 2024, Volume 13096, Paper No. 130965I, 11 pp, 11 figs</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.03409">arXiv:2407.03409</a> <span> [<a href="https://arxiv.org/pdf/2407.03409">pdf</a>, <a href="https://arxiv.org/format/2407.03409">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"> From Halos to Galaxies. IX. Estimate of Halo Assembly History for SDSS Galaxy Groups </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lyu%2C+C">Cheqiu Lyu</a>, <a href="/search/astro-ph?searchtype=author&query=Peng%2C+Y">Yingjie Peng</a>, <a href="/search/astro-ph?searchtype=author&query=Jing%2C+Y">Yipeng Jing</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+X">Xiaohu Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Ho%2C+L+C">Luis C. Ho</a>, <a href="/search/astro-ph?searchtype=author&query=Renzini%2C+A">Alvio Renzini</a>, <a href="/search/astro-ph?searchtype=author&query=Zhao%2C+D">Dingyi Zhao</a>, <a href="/search/astro-ph?searchtype=author&query=Mannucci%2C+F">Filippo Mannucci</a>, <a href="/search/astro-ph?searchtype=author&query=Mo%2C+H">Houjun Mo</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+K">Kai Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+B">Bitao Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+B">Bingxiao Xu</a>, <a href="/search/astro-ph?searchtype=author&query=Dou%2C+J">Jing Dou</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A+R">Anna R. Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Gu%2C+Q">Qiusheng Gu</a>, <a href="/search/astro-ph?searchtype=author&query=Maiolino%2C+R">Roberto Maiolino</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+E">Enci Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+F">Feng Yuan</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="2407.03409v1-abstract-short" style="display: inline;"> The properties of the galaxies are tightly connected to their host halo mass and halo assembly history. Accurate measurement of the halo assembly history in observation is challenging but crucial to the understanding of galaxy formation and evolution. The stellar-to-halo mass ratio ($M_*/M_{\mathrm{h}}$) for the centrals has often been used to indicate the halo assembly time $t_{\mathrm{h,50}}$ of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.03409v1-abstract-full').style.display = 'inline'; document.getElementById('2407.03409v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.03409v1-abstract-full" style="display: none;"> The properties of the galaxies are tightly connected to their host halo mass and halo assembly history. Accurate measurement of the halo assembly history in observation is challenging but crucial to the understanding of galaxy formation and evolution. The stellar-to-halo mass ratio ($M_*/M_{\mathrm{h}}$) for the centrals has often been used to indicate the halo assembly time $t_{\mathrm{h,50}}$ of the group, where $t_{\mathrm{h,50}}$ is the lookback time at which a halo has assembled half of its present-day virial mass. Using mock data from the semi-analytic models, we find that $M_*/M_{\mathrm{h}}$ shows a significant scatter with $t_{\mathrm{h,50}}$, with a strong systematic difference between the group with a star-forming central (blue group) and passive central (red group). To improve the accuracy, we develop machine-learning models to estimate $t_{\mathrm{h,50}}$ for galaxy groups using only observable quantities in the mocks. Since star-formation quenching will decouple the co-growth of the dark matter and baryon, we train our models separately for blue and red groups. Our models have successfully recovered $t_{\mathrm{h,50}}$, within an accuracy of $\sim$ 1.09 Gyr. With careful calibrations of individual observable quantities in the mocks with SDSS observations, we apply the trained models to the SDSS Yang et al. groups and derive the $t_{\mathrm{h,50}}$ for each group for the first time. The derived SDSS $t_{\mathrm{h,50}}$ distributions are in good agreement with that in the mocks, in particular for blue groups. The derived halo assembly history, together with the halo mass, make an important step forward in studying the halo-galaxy connections in observation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.03409v1-abstract-full').style.display = 'none'; document.getElementById('2407.03409v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">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">18 pages, 7 figures. Accepted by ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.11748">arXiv:2406.11748</a> <span> [<a href="https://arxiv.org/pdf/2406.11748">pdf</a>, <a href="https://arxiv.org/format/2406.11748">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"> Retrieval of the physical parameters of galaxies from WEAVE-StePS-like data using machine learning </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Angthopo%2C+J">J. Angthopo</a>, <a href="/search/astro-ph?searchtype=author&query=Granett%2C+B+R">B. R. Granett</a>, <a href="/search/astro-ph?searchtype=author&query=La+Barbera%2C+F">F. La Barbera</a>, <a href="/search/astro-ph?searchtype=author&query=Longhetti%2C+M">M. Longhetti</a>, <a href="/search/astro-ph?searchtype=author&query=Iovino%2C+A">A. Iovino</a>, <a href="/search/astro-ph?searchtype=author&query=Fossati%2C+M">M. Fossati</a>, <a href="/search/astro-ph?searchtype=author&query=Ditrani%2C+F+R">F. R. Ditrani</a>, <a href="/search/astro-ph?searchtype=author&query=Costantin%2C+L">L. Costantin</a>, <a href="/search/astro-ph?searchtype=author&query=Zibetti%2C+S">S. Zibetti</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">A. Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Bl%C3%A1zquez%2C+P">P. S谩nchez-Bl谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Tortora%2C+C">C. Tortora</a>, <a href="/search/astro-ph?searchtype=author&query=Spiniello%2C+C">C. Spiniello</a>, <a href="/search/astro-ph?searchtype=author&query=Poggianti%2C+B">B. Poggianti</a>, <a href="/search/astro-ph?searchtype=author&query=Vazdekis%2C+A">A. Vazdekis</a>, <a href="/search/astro-ph?searchtype=author&query=Balcells%2C+M">M. Balcells</a>, <a href="/search/astro-ph?searchtype=author&query=Bardelli%2C+S">S. Bardelli</a>, <a href="/search/astro-ph?searchtype=author&query=Benn%2C+C+R">C. R. Benn</a>, <a href="/search/astro-ph?searchtype=author&query=Bianconi%2C+M">M. Bianconi</a>, <a href="/search/astro-ph?searchtype=author&query=Bolzonella%2C+M">M. Bolzonella</a>, <a href="/search/astro-ph?searchtype=author&query=Busarello%2C+G">G. Busarello</a>, <a href="/search/astro-ph?searchtype=author&query=Cassar%C3%A0%2C+L+P">L. P. Cassar脿</a>, <a href="/search/astro-ph?searchtype=author&query=Corsini%2C+E+M">E. M. Corsini</a>, <a href="/search/astro-ph?searchtype=author&query=Cucciati%2C+O">O. Cucciati</a>, <a href="/search/astro-ph?searchtype=author&query=Dalton%2C+G">G. Dalton</a> , et al. (24 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="2406.11748v1-abstract-short" style="display: inline;"> The WHT Enhanced Area Velocity Explorer (WEAVE) is a new, massively multiplexing spectrograph. This new instrument will be exploited to obtain high S/N spectra of $\sim$25000 galaxies at intermediate redshifts for the WEAVE Stellar Population Survey (WEAVE-StePS). We test machine learning methods for retrieving the key physical parameters of galaxies from WEAVE-StePS-like spectra using both photom… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.11748v1-abstract-full').style.display = 'inline'; document.getElementById('2406.11748v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.11748v1-abstract-full" style="display: none;"> The WHT Enhanced Area Velocity Explorer (WEAVE) is a new, massively multiplexing spectrograph. This new instrument will be exploited to obtain high S/N spectra of $\sim$25000 galaxies at intermediate redshifts for the WEAVE Stellar Population Survey (WEAVE-StePS). We test machine learning methods for retrieving the key physical parameters of galaxies from WEAVE-StePS-like spectra using both photometric and spectroscopic information at various S/Ns and redshifts. We simulated $\sim$105000 galaxy spectra assuming SFH with an exponentially declining star formation rate, covering a wide range of ages, stellar metallicities, sSFRs, and dust extinctions. We then evaluated the ability of the random forest and KNN algorithms to correctly predict such parameters assuming no measurement errors. We checked how much the predictive ability deteriorates for different S/Ns and redshifts, finding that both algorithms still accurately estimate the ages and metallicities with low bias. The dispersion varies from 0.08-0.16 dex for ages and 0.11-0.25 dex for metallicity, depending on the redshift and S/N. For dust attenuation, we find a similarly low bias and dispersion. For the sSFR, we find a very good constraining power for star-forming galaxies, log sSFR$\gtrsim$ -11, where the bias is $\sim$ 0.01 dex and the dispersion is $\sim$ 0.10 dex. For more quiescent galaxies, with log sSFR$\lesssim$ -11, we find a higher bias, 0.61-0.86 dex, and a higher dispersion, $\sim$ 0.4 dex, for different S/Ns and redshifts. Generally, we find that the RF outperforms the KNN. Finally, the retrieved sSFR was used to successfully classify galaxies as part of the blue cloud, green valley, or red sequence. We demonstrate that machine learning algorithms can accurately estimate the physical parameters of simulated galaxies even at relatively low S/N=10 per angstrom spectra with available ancillary photometric information. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.11748v1-abstract-full').style.display = 'none'; document.getElementById('2406.11748v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 10 + 2 figures, 4 tables, accepted 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/2403.05398">arXiv:2403.05398</a> <span> [<a href="https://arxiv.org/pdf/2403.05398">pdf</a>, <a href="https://arxiv.org/format/2403.05398">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> The Wide-field Spectroscopic Telescope (WST) Science White Paper </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mainieri%2C+V">Vincenzo Mainieri</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+R+I">Richard I. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Brinchmann%2C+J">Jarle Brinchmann</a>, <a href="/search/astro-ph?searchtype=author&query=Cimatti%2C+A">Andrea Cimatti</a>, <a href="/search/astro-ph?searchtype=author&query=Ellis%2C+R+S">Richard S. Ellis</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+V">Vanessa Hill</a>, <a href="/search/astro-ph?searchtype=author&query=Kneib%2C+J">Jean-Paul Kneib</a>, <a href="/search/astro-ph?searchtype=author&query=McLeod%2C+A+F">Anna F. McLeod</a>, <a href="/search/astro-ph?searchtype=author&query=Opitom%2C+C">Cyrielle Opitom</a>, <a href="/search/astro-ph?searchtype=author&query=Roth%2C+M+M">Martin M. Roth</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez-Saez%2C+P">Paula Sanchez-Saez</a>, <a href="/search/astro-ph?searchtype=author&query=Smiljanic%2C+R">Rodolfo Smiljanic</a>, <a href="/search/astro-ph?searchtype=author&query=Tolstoy%2C+E">Eline Tolstoy</a>, <a href="/search/astro-ph?searchtype=author&query=Bacon%2C+R">Roland Bacon</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">Sofia Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Adamo%2C+A">Angela Adamo</a>, <a href="/search/astro-ph?searchtype=author&query=Annibali%2C+F">Francesca Annibali</a>, <a href="/search/astro-ph?searchtype=author&query=Arevalo%2C+P">Patricia Arevalo</a>, <a href="/search/astro-ph?searchtype=author&query=Audard%2C+M">Marc Audard</a>, <a href="/search/astro-ph?searchtype=author&query=Barsanti%2C+S">Stefania Barsanti</a>, <a href="/search/astro-ph?searchtype=author&query=Battaglia%2C+G">Giuseppina Battaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Aran%2C+A+M+B">Amelia M. Bayo Aran</a>, <a href="/search/astro-ph?searchtype=author&query=Belfiore%2C+F">Francesco Belfiore</a>, <a href="/search/astro-ph?searchtype=author&query=Bellazzini%2C+M">Michele Bellazzini</a>, <a href="/search/astro-ph?searchtype=author&query=Bellini%2C+E">Emilio Bellini</a> , et al. (192 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="2403.05398v2-abstract-short" style="display: inline;"> The Wide-field Spectroscopic Telescope (WST) is proposed as a new facility dedicated to the efficient delivery of spectroscopic surveys. This white paper summarises the initial concept as well as the corresponding science cases. WST will feature simultaneous operation of a large field-of-view (3 sq. degree), a high multiplex (20,000) multi-object spectrograph (MOS) and a giant 3x3 sq. arcmin integ… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.05398v2-abstract-full').style.display = 'inline'; document.getElementById('2403.05398v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.05398v2-abstract-full" style="display: none;"> The Wide-field Spectroscopic Telescope (WST) is proposed as a new facility dedicated to the efficient delivery of spectroscopic surveys. This white paper summarises the initial concept as well as the corresponding science cases. WST will feature simultaneous operation of a large field-of-view (3 sq. degree), a high multiplex (20,000) multi-object spectrograph (MOS) and a giant 3x3 sq. arcmin integral field spectrograph (IFS). In scientific capability these requirements place WST far ahead of existing and planned facilities. Given the current investment in deep imaging surveys and noting the diagnostic power of spectroscopy, WST will fill a crucial gap in astronomical capability and work synergistically with future ground and space-based facilities. This white paper shows that WST can address outstanding scientific questions in the areas of cosmology; galaxy assembly, evolution, and enrichment, including our own Milky Way; origin of stars and planets; time domain and multi-messenger astrophysics. WST's uniquely rich dataset will deliver unforeseen discoveries in many of these areas. The WST Science Team (already including more than 500 scientists worldwide) is open to the all astronomical community. To register in the WST Science Team please visit https://www.wstelescope.com/for-scientists/participate <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.05398v2-abstract-full').style.display = 'none'; document.getElementById('2403.05398v2-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 April, 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">194 pages, 66 figures. Comments are welcome (wstelescope@gmail.com)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.07335">arXiv:2401.07335</a> <span> [<a href="https://arxiv.org/pdf/2401.07335">pdf</a>, <a href="https://arxiv.org/format/2401.07335">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/10.1093/mnras/stae178">10.1093/mnras/stae178 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> On the maximum age resolution achievable through stellar population synthesis models </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zibetti%2C+S">Stefano Zibetti</a>, <a href="/search/astro-ph?searchtype=author&query=Rossi%2C+E">Edoardo Rossi</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A+R">Anna R. Gallazzi</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="2401.07335v1-abstract-short" style="display: inline;"> As the reconstruction of the star-formation histories (SFH) of galaxies from spectroscopic data becomes increasingly popular, we explore the best age resolution achievable with stellar population synthesis (SPS) models, relying on different constraints: broad-band colours, absorption indices, a combination of the two, and the full spectrum. We perform idealized experiments on SPS models and show t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.07335v1-abstract-full').style.display = 'inline'; document.getElementById('2401.07335v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.07335v1-abstract-full" style="display: none;"> As the reconstruction of the star-formation histories (SFH) of galaxies from spectroscopic data becomes increasingly popular, we explore the best age resolution achievable with stellar population synthesis (SPS) models, relying on different constraints: broad-band colours, absorption indices, a combination of the two, and the full spectrum. We perform idealized experiments on SPS models and show that the minimum resolvable relative duration of a star-formation episode (time difference between 10% and 90% of the stellar mass formed divided by the median age) is never better than 0.4, even when using spectra with signal-to-noise ratio (SNR) larger than 100 per AA. Typically, the best relative age resolution ranges between 0.4 and 0.7 over most of the age-metallicity plane, corresponding to minimum bin sizes for SFH sampling between 0.15 and 0.25 dex. This resolution makes the spectroscopic exploration of distant galaxies mandatory in order to reconstruct the early phases of galaxies' SFHs. We show that spectroscopy with SNR $\gtrsim$ 2/AA is essential for good age resolution. Remarkably, using the full spectrum does not prove significantly more effective than relying on absorption indices, especially at SNR $\lesssim$ 20/AA. We discuss the physical origins of the age resolution trends as a function of age and metallicity, and identify the presence of maxima in age resolution (i.e. minima in measurable relative time duration) at the characteristic ages that correspond to quick time variations in spectral absorption features. We connect these maxima to bumps commonly observed in reconstructed SFHs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.07335v1-abstract-full').style.display = 'none'; document.getElementById('2401.07335v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 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">Accepted for publication on MNRAS - 16 pages</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.18000">arXiv:2310.18000</a> <span> [<a href="https://arxiv.org/pdf/2310.18000">pdf</a>, <a href="https://arxiv.org/format/2310.18000">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"> Less is less: photometry alone cannot predict the observed spectral indices of $z\sim1$ galaxies from the LEGA-C spectroscopic survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Nersesian%2C+A">Angelos Nersesian</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Wel%2C+A">Arjen van der Wel</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">Anna Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Leja%2C+J">Joel Leja</a>, <a href="/search/astro-ph?searchtype=author&query=Bezanson%2C+R">Rachel Bezanson</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+E+F">Eric F. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Eugenio%2C+F">Francesco D'Eugenio</a>, <a href="/search/astro-ph?searchtype=author&query=de+Graaff%2C+A">Anna de Graaff</a>, <a href="/search/astro-ph?searchtype=author&query=Kaushal%2C+Y">Yasha Kaushal</a>, <a href="/search/astro-ph?searchtype=author&query=Martorano%2C+M">Marco Martorano</a>, <a href="/search/astro-ph?searchtype=author&query=Maseda%2C+M">Michael Maseda</a>, <a href="/search/astro-ph?searchtype=author&query=Zibetti%2C+S">Stefano Zibetti</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.18000v1-abstract-short" style="display: inline;"> We test whether we can predict optical spectra from deep-field photometry of distant galaxies. Our goal is to perform a comparison in data space, highlighting the differences between predicted and observed spectra. The Large Early Galaxy Astrophysics Census (LEGA-C) provides high-quality optical spectra of thousands of galaxies at redshift $0.6<z<1$. Broad-band photometry of the same galaxies, dra… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.18000v1-abstract-full').style.display = 'inline'; document.getElementById('2310.18000v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.18000v1-abstract-full" style="display: none;"> We test whether we can predict optical spectra from deep-field photometry of distant galaxies. Our goal is to perform a comparison in data space, highlighting the differences between predicted and observed spectra. The Large Early Galaxy Astrophysics Census (LEGA-C) provides high-quality optical spectra of thousands of galaxies at redshift $0.6<z<1$. Broad-band photometry of the same galaxies, drawn from the recent COSMOS2020 catalog, is used to predict the optical spectra with the spectral energy distribution (SED) fitting code Prospector and the MILES stellar library. The observed and predicted spectra are compared in terms of two age and metallicity-sensitive absorption features (H$未_\mathrm{A}$ and Fe4383). The global bimodality of star-forming and quiescent galaxies in photometric space is recovered with the model spectra. But the presence of a systematic offset in the Fe4383 line strength and the weak correlation between the observed and modeled line strength imply that accurate age or metallicity determinations cannot be inferred from photometry alone. For now we caution that photometry-based estimates of stellar population properties are determined mostly by the modeling approach and not the physical properties of galaxies, even when using the highest-quality photometric datasets and state-of-the-art fitting techniques. When exploring a new physical parameter space (i.e. redshift or galaxy mass) high-quality spectroscopy is always needed to inform the analysis of photometry. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.18000v1-abstract-full').style.display = 'none'; document.getElementById('2310.18000v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 October, 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">13 pages, 8 figures, accepted 26 October 2023</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.12966">arXiv:2309.12966</a> <span> [<a href="https://arxiv.org/pdf/2309.12966">pdf</a>, <a href="https://arxiv.org/format/2309.12966">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> INSPIRE: INvestigating Stellar Population In RElics V. A catalogue of ultra-compact massive galaxies outside the local Universe and their degree of relicness </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Spiniello%2C+C">C. Spiniello</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Ago%2C+G">G. D'Ago</a>, <a href="/search/astro-ph?searchtype=author&query=Coccato%2C+L">L. Coccato</a>, <a href="/search/astro-ph?searchtype=author&query=Hartke%2C+J">J. Hartke</a>, <a href="/search/astro-ph?searchtype=author&query=Tortora%2C+C">C. Tortora</a>, <a href="/search/astro-ph?searchtype=author&query=Ferr%C3%A9-Mateu%2C+A">A. Ferr茅-Mateu</a>, <a href="/search/astro-ph?searchtype=author&query=Pulsoni%2C+C">C. Pulsoni</a>, <a href="/search/astro-ph?searchtype=author&query=Cappellari%2C+M">M. Cappellari</a>, <a href="/search/astro-ph?searchtype=author&query=Maksymowicz-Maciata%2C+M">M. Maksymowicz-Maciata</a>, <a href="/search/astro-ph?searchtype=author&query=Arnaboldi%2C+M">M. Arnaboldi</a>, <a href="/search/astro-ph?searchtype=author&query=Bevacqua%2C+D">D. Bevacqua</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">A. Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Hunt%2C+L+K">L. K. Hunt</a>, <a href="/search/astro-ph?searchtype=author&query=La+Barbera%2C+F">F. La Barbera</a>, <a href="/search/astro-ph?searchtype=author&query=Mart%C3%ADn-Navarro%2C+I">I. Mart铆n-Navarro</a>, <a href="/search/astro-ph?searchtype=author&query=Napolitano%2C+N+R">N. R. Napolitano</a>, <a href="/search/astro-ph?searchtype=author&query=Radovich%2C+M">M. Radovich</a>, <a href="/search/astro-ph?searchtype=author&query=Saracco%2C+P">P. Saracco</a>, <a href="/search/astro-ph?searchtype=author&query=Scognamiglio%2C+D">D. Scognamiglio</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">M. Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Zibetti%2C+S">S. Zibetti</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2309.12966v2-abstract-short" style="display: inline;"> This paper presents the third data release of the INvestigating Stellar Population In RElics (INSPIRE) project, comprising 52 ultra-compact massive galaxies (UCMGs) observed with the X-Shooter spectrograph. We measure integrated stellar velocity dispersion, [Mg/Fe] abundances, ages, and metallicities for all the INSPIRE objects. We thus infer star formation histories and confirm the existence of a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.12966v2-abstract-full').style.display = 'inline'; document.getElementById('2309.12966v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.12966v2-abstract-full" style="display: none;"> This paper presents the third data release of the INvestigating Stellar Population In RElics (INSPIRE) project, comprising 52 ultra-compact massive galaxies (UCMGs) observed with the X-Shooter spectrograph. We measure integrated stellar velocity dispersion, [Mg/Fe] abundances, ages, and metallicities for all the INSPIRE objects. We thus infer star formation histories and confirm the existence of a degree of relicness (DoR), defined in terms of the fraction of stellar mass formed by $z=2$, the time at which a galaxy has assembled 75\% of its mass, and the final assembly time. Objects with a high DoR assembled their stellar mass at early epochs, while low-DoR objects show a non-negligible fraction of later-formed populations and hence a spread in ages and metallicities. A higher DoR correlates with larger [Mg/Fe], super-solar metallicity, and larger velocity dispersion values. The 52 UMCGs span a large range of DoR from 0.83 to 0.06, with 38 of them having formed more than 75\% of their mass by $z=2$. Of these, nine are extreme relics (DoR$>0.7$), since they formed the totality ($>99\%$) of their stellar mass by redshift $z=2$. The remaining 14 UCMGs cannot be considered relics, as they are characterised by more extended star formation histories. With INSPIRE, we built the first sizeable sample of relics outside the local Universe, up to $z\sim0.4$, increasing the number of confirmed relics by a factor of $>10$, and opening up an important window to explain the mass assembly of massive galaxies in the high-z Universe. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.12966v2-abstract-full').style.display = 'none'; document.getElementById('2309.12966v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 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">accepted for publication on MNRAS, 20 pages, 15 figures, 3 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.08681">arXiv:2308.08681</a> <span> [<a href="https://arxiv.org/pdf/2308.08681">pdf</a>, <a href="https://arxiv.org/format/2308.08681">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"> Stars, gas, and star formation of distant post-starburst galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wu%2C+P">Po-Feng Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Bezanson%2C+R">Rachel Bezanson</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Eugenio%2C+F">Francesco D'Eugenio</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A+R">Anna R. Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Greene%2C+J+E">Jenny E. Greene</a>, <a href="/search/astro-ph?searchtype=author&query=Maseda%2C+M+V">Michael V. Maseda</a>, <a href="/search/astro-ph?searchtype=author&query=Suess%2C+K+A">Katherine A. Suess</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Wel%2C+A">Arjen van der Wel</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2308.08681v1-abstract-short" style="display: inline;"> We present a comprehensive multi-wavelength study of 5 poststarburst galaxies with $M_\ast > 10^{11} M_\odot$ at $z\sim 0.7$, examining their stars, gas, and current and past star-formation activities. Using optical images from the Subaru telescope and Hubble Space Telescope, we observe a high incidence of companion galaxies and low surface brightness tidal features, indicating that quenching is c… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.08681v1-abstract-full').style.display = 'inline'; document.getElementById('2308.08681v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.08681v1-abstract-full" style="display: none;"> We present a comprehensive multi-wavelength study of 5 poststarburst galaxies with $M_\ast > 10^{11} M_\odot$ at $z\sim 0.7$, examining their stars, gas, and current and past star-formation activities. Using optical images from the Subaru telescope and Hubble Space Telescope, we observe a high incidence of companion galaxies and low surface brightness tidal features, indicating that quenching is closely related to interactions between galaxies. From optical spectra provided by the LEGA-C survey, we model the stellar continuum to derive the star-formation histories and show that the stellar masses of progenitors ranging from $2\times10^9 M_\odot$ to $10^{11} M_\odot$, undergoing a burst of star formation several hundred million years prior to observation, with a decay time scale of $\sim100$ million years. Our ALMA observations detect CO(2-1) emission in four galaxies, with the molecular gas spreading over up to $>1"$, or $\sim10$ kpc, with a mass of up to $\sim2 \times10^{10} M_\odot$. However, star-forming regions are unresolved by either the slit spectra or 3~GHz continuum observed by the Very Large Array. Comparisons between the star-formation rates and gas masses, and the sizes of CO emission and star-forming regions suggest a low star-forming efficiency. We show that the star-formation rates derived from IR and radio luminosities with commonly-used calibrations tend to overestimate the true values because of the prodigious amount of radiation from old stars and the contribution from AGN, as the optical spectra reveal weak AGN-driven outflows. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.08681v1-abstract-full').style.display = 'none'; document.getElementById('2308.08681v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted by ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.03441">arXiv:2308.03441</a> <span> [<a href="https://arxiv.org/pdf/2308.03441">pdf</a>, <a href="https://arxiv.org/format/2308.03441">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 elemental abundances of quiescent galaxies in the LEGA-C survey: the (non-)evolution of [伪/Fe] from z = 0.75 to z = 0 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bevacqua%2C+D">Davide Bevacqua</a>, <a href="/search/astro-ph?searchtype=author&query=Saracco%2C+P">Paolo Saracco</a>, <a href="/search/astro-ph?searchtype=author&query=La+Barbera%2C+F">Francesco La Barbera</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Ago%2C+G">Giuseppe D'Ago</a>, <a href="/search/astro-ph?searchtype=author&query=de+Propris%2C+R">Roberto de Propris</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreras%2C+I">Ignacio Ferreras</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">Anna Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Pasquali%2C+A">Anna Pasquali</a>, <a href="/search/astro-ph?searchtype=author&query=Spiniello%2C+C">Chiara Spiniello</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2308.03441v1-abstract-short" style="display: inline;"> We measure the [$伪$/Fe] abundances for 183 quiescent galaxies at z = 0.60 - 0.75 with stellar masses ranging 10.4 \leq log10 10.4 $\leq$ log10 (M$_*$ /M$_\odot$) $\leq$ 11.6 selected from the LEGA-C survey. We estimate [$伪$/Fe] from the ratio of the spectral indices Mgb ($位 \sim 5177$ 脜) and Fe4383, compared to predictions of simple stellar population models. We find that 91% of quiescents in our… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.03441v1-abstract-full').style.display = 'inline'; document.getElementById('2308.03441v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.03441v1-abstract-full" style="display: none;"> We measure the [$伪$/Fe] abundances for 183 quiescent galaxies at z = 0.60 - 0.75 with stellar masses ranging 10.4 \leq log10 10.4 $\leq$ log10 (M$_*$ /M$_\odot$) $\leq$ 11.6 selected from the LEGA-C survey. We estimate [$伪$/Fe] from the ratio of the spectral indices Mgb ($位 \sim 5177$ 脜) and Fe4383, compared to predictions of simple stellar population models. We find that 91% of quiescents in our sample have supersolar [$伪$/Fe], with an average value of [$伪$/Fe] = +0.24 $\pm$ 0.01. We find no significant correlation between [$伪$/Fe] and stellar metallicity, mass, velocity dispersion, and average formation time. Galaxies that formed the bulk of their stellar mass on time scales shorter than 1 Gyr follow the same [$伪$/Fe] distribution as those which formed on longer time scales. In comparison to local early-type galaxies and to stacked spectra of quiescent galaxies at z = 0.38 and z = 0.07, we find that the average [$伪$/Fe] has not changed between z = 0.75 and the present time. Our work shows that the vast majority of massive quiescent galaxies at z $\sim$ 0.7 are $伪$-enhanced, and that no detectable evolution of the average [$伪$/Fe] has taken place over the last $\sim$ 6.5 Gyr. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.03441v1-abstract-full').style.display = 'none'; document.getElementById('2308.03441v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 10 figures, 2 tables, 1 appendix</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.02635">arXiv:2308.02635</a> <span> [<a href="https://arxiv.org/pdf/2308.02635">pdf</a>, <a href="https://arxiv.org/format/2308.02635">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/10.1051/0004-6361/202346563">10.1051/0004-6361/202346563 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Stellar metallicity from optical and UV spectral indices: Test case for WEAVE-StePS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ditrani%2C+F+R">F. R. Ditrani</a>, <a href="/search/astro-ph?searchtype=author&query=Longhetti%2C+M">M. Longhetti</a>, <a href="/search/astro-ph?searchtype=author&query=La+Barbera%2C+F">F. La Barbera</a>, <a href="/search/astro-ph?searchtype=author&query=Iovino%2C+A">A. Iovino</a>, <a href="/search/astro-ph?searchtype=author&query=Costantin%2C+L">L. Costantin</a>, <a href="/search/astro-ph?searchtype=author&query=Zibetti%2C+S">S. Zibetti</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">A. Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Fossati%2C+M">M. Fossati</a>, <a href="/search/astro-ph?searchtype=author&query=Angthopo%2C+J">J. Angthopo</a>, <a href="/search/astro-ph?searchtype=author&query=Ascasibar%2C+Y">Y. Ascasibar</a>, <a href="/search/astro-ph?searchtype=author&query=Poggianti%2C+B">B. Poggianti</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Bl%C3%A1zquez%2C+P">P. S谩nchez-Bl谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Balcells%2C+M">M. Balcells</a>, <a href="/search/astro-ph?searchtype=author&query=Bianconi%2C+M">M. Bianconi</a>, <a href="/search/astro-ph?searchtype=author&query=Bolzonella%2C+M">M. Bolzonella</a>, <a href="/search/astro-ph?searchtype=author&query=Cassar%C3%A0%2C+L+P">L. P. Cassar脿</a>, <a href="/search/astro-ph?searchtype=author&query=Cucciati%2C+O">O. Cucciati</a>, <a href="/search/astro-ph?searchtype=author&query=Dalton%2C+G">G. Dalton</a>, <a href="/search/astro-ph?searchtype=author&query=Ferr%C3%A9-Mateu%2C+A">A. Ferr茅-Mateu</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa-Benito%2C+R">R. Garc铆a-Benito</a>, <a href="/search/astro-ph?searchtype=author&query=Granett%2C+B">B. Granett</a>, <a href="/search/astro-ph?searchtype=author&query=Gullieuszik%2C+M">M. Gullieuszik</a>, <a href="/search/astro-ph?searchtype=author&query=Ikhsanova%2C+A">A. Ikhsanova</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+S">S. Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Knapen%2C+J+H">J. H. Knapen</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="2308.02635v1-abstract-short" style="display: inline;"> The upcoming generation of optical spectrographs on four meter-class telescopes, with their huge multiplexing capabilities, excellent spectral resolution, and unprecedented wavelength coverage, will provide high-quality spectra for thousands of galaxies. These data will allow us to examine of the stellar population properties at intermediate redshift, an epoch that remains unexplored by large and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.02635v1-abstract-full').style.display = 'inline'; document.getElementById('2308.02635v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.02635v1-abstract-full" style="display: none;"> The upcoming generation of optical spectrographs on four meter-class telescopes, with their huge multiplexing capabilities, excellent spectral resolution, and unprecedented wavelength coverage, will provide high-quality spectra for thousands of galaxies. These data will allow us to examine of the stellar population properties at intermediate redshift, an epoch that remains unexplored by large and deep surveys. We assess our capability to retrieve the mean stellar metallicity in galaxies at different redshifts and S/N, while simultaneously exploiting the UV and optical rest-frame wavelength coverage. The work is based on a comprehensive library of spectral templates of stellar populations, covering a wide range of age and metallicity values and built assuming various SFHs. We simulated realistic observations of a large sample of galaxies carried out with WEAVE at the WHT at different redshifts and S/N values. We measured all the reliable indices on the simulated spectra and on the comparison library. We then adopted a Bayesian approach to obtain the probability distribution of stellar metallicity. The analysis of the spectral indices has shown how some mid-UV indices can provide reliable constraints on stellar metallicity, along with optical indicators. The analysis of the mock observations has shown that even at S/N=10, the metallicity can be derived within 0.3 dex, in particular, for stellar populations older than 2 Gyr. Our results are in good agreement with other theoretical and observational works in the literature and show how the UV indicators can be advantageous in constraining metallicities. This is very promising for the upcoming surveys carried out with new, highly multiplexed, large-field spectrographs, such as StePS at the WEAVE and 4MOST, which will provide spectra of thousands of galaxies covering large spectral ranges at relatively high S/N. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.02635v1-abstract-full').style.display = 'none'; document.getElementById('2308.02635v1-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 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 14 figures. Submitted 31/03/2023, Accepted 20/07/2023</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 677, A93 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.08120">arXiv:2306.08120</a> <span> [<a href="https://arxiv.org/pdf/2306.08120">pdf</a>, <a href="https://arxiv.org/format/2306.08120">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/stad1821">10.1093/mnras/stad1821 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The large molecular gas fraction of post-starburst galaxies at z > 1 </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=Valentino%2C+F">F. Valentino</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">A. Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Belli%2C+S">S. Belli</a>, <a href="/search/astro-ph?searchtype=author&query=Magdis%2C+G">G. Magdis</a>, <a href="/search/astro-ph?searchtype=author&query=Bolamperti%2C+A">A. Bolamperti</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.08120v1-abstract-short" style="display: inline;"> Post-starburst galaxies are sources that had the last major episode of star formation about 1 Gyr before the epoch of the observations and are on their way to quiescence. It is important to study such galaxies at redshift z > 1, during their main quenching phase, and estimate their molecular gas content to constrain the processes responsible for the cessation of star formation. We present CO(3-2)… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.08120v1-abstract-full').style.display = 'inline'; document.getElementById('2306.08120v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.08120v1-abstract-full" style="display: none;"> Post-starburst galaxies are sources that had the last major episode of star formation about 1 Gyr before the epoch of the observations and are on their way to quiescence. It is important to study such galaxies at redshift z > 1, during their main quenching phase, and estimate their molecular gas content to constrain the processes responsible for the cessation of star formation. We present CO(3-2) ALMA observations of two massive (Mstar ~ 5 x 10^10 Msun) post-starburst galaxies at z > 1. We measure their molecular gas fraction to be f_H2 = M_H2/Mstar ~ 8% - 16%, consistent with z < 1 post-starburst galaxies from the literature. The star formation efficiency of our targets is ~ 10x lower than that of star-forming galaxies at similar redshift, and they are outliers of the f_H2 - specific star formation rate (sSFR) relation of star-forming galaxies, as they have larger f_H2 than expected given their sSFR. The gas fraction of post-starbursts from our sample and the literature correlates with the Dn4000 spectral index, a proxy of the stellar population age. This suggests that their gas content decreases after the last major burst of star formation. Finally, one of our targets is undergoing a major merger phase with two highly star-forming companions. This hints at a picture where a perturber event (e.g., major merger) quenches star formation without completely removing the molecular gas. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.08120v1-abstract-full').style.display = 'none'; document.getElementById('2306.08120v1-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 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">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/2304.12343">arXiv:2304.12343</a> <span> [<a href="https://arxiv.org/pdf/2304.12343">pdf</a>, <a href="https://arxiv.org/format/2304.12343">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 Gas-Phase Mass--Metallicity Relation for Massive Galaxies at $z\sim0.7$ with the LEGA-C Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lewis%2C+Z+J">Zach J. Lewis</a>, <a href="/search/astro-ph?searchtype=author&query=Andrews%2C+B+H">Brett H. Andrews</a>, <a href="/search/astro-ph?searchtype=author&query=Bezanson%2C+R">Rachel Bezanson</a>, <a href="/search/astro-ph?searchtype=author&query=Maseda%2C+M">Michael Maseda</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+E+F">Eric F. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Dav%C3%A9%2C+R">Romeel Dav茅</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Eugenio%2C+F">Francesco D'Eugenio</a>, <a href="/search/astro-ph?searchtype=author&query=Franx%2C+M">Marijn Franx</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">Anna Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=de+Graaff%2C+A">Anna de Graaff</a>, <a href="/search/astro-ph?searchtype=author&query=Kaushal%2C+Y">Yasha Kaushal</a>, <a href="/search/astro-ph?searchtype=author&query=Nersesian%2C+A">Angelos Nersesian</a>, <a href="/search/astro-ph?searchtype=author&query=Newman%2C+J+A">Jeffrey A. Newman</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Wel%2C+A">Arjen van der Wel</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+P">Po-Feng Wu</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2304.12343v1-abstract-short" style="display: inline;"> The massive end of the gas-phase mass--metallicity relation (MZR) is a sensitive probe of active galactic nuclei (AGN) feedback that is a crucial but highly uncertain component of galaxy evolution models. In this paper, we extend the $z\sim0.7$ MZR by $\sim$0.5 dex up to log$(M_\star/\textrm{M}_\odot)\sim11.1$. We use extremely deep VLT VIMOS spectra from the Large Early Galaxy Astrophysics Census… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.12343v1-abstract-full').style.display = 'inline'; document.getElementById('2304.12343v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.12343v1-abstract-full" style="display: none;"> The massive end of the gas-phase mass--metallicity relation (MZR) is a sensitive probe of active galactic nuclei (AGN) feedback that is a crucial but highly uncertain component of galaxy evolution models. In this paper, we extend the $z\sim0.7$ MZR by $\sim$0.5 dex up to log$(M_\star/\textrm{M}_\odot)\sim11.1$. We use extremely deep VLT VIMOS spectra from the Large Early Galaxy Astrophysics Census (LEGA-C) survey to measure metallicities for 145 galaxies. The LEGA-C MZR matches the normalization of the $z\sim0.8$ DEEP2 MZR where they overlap, so we combine the two to create an MZR spanning from 9.3 to 11.1 log$(M_\star/\textrm{M}_\odot)$. The LEGA-C+DEEP2 MZR at $z\sim0.7$ is offset to slightly lower metallicities (0.05-0.13 dex) than the $z\sim0$ MZR, but it otherwise mirrors the established power law rise at low/intermediate stellar masses and asymptotic flattening at high stellar masses. We compare the LEGA-C+DEEP2 MZR to the MZR from two cosmological simulations (IllustrisTNG and SIMBA), which predict qualitatively different metallicity trends for high-mass galaxies. This comparison highlights that our extended MZR provides a crucial observational constraint for galaxy evolution models in a mass regime where the MZR is very sensitive to choices about the implementation of AGN feedback. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.12343v1-abstract-full').style.display = 'none'; document.getElementById('2304.12343v1-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 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 4 figures, 1 table</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.05520">arXiv:2303.05520</a> <span> [<a href="https://arxiv.org/pdf/2303.05520">pdf</a>, <a href="https://arxiv.org/format/2303.05520">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"> Evolution in the orbital structure of quiescent galaxies from MAGPI, LEGA-C and SAMI surveys: direct evidence for merger-driven growth over the last 7 Gy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=D%27Eugenio%2C+F">Francesco D'Eugenio</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Wel%2C+A">Arjen van der Wel</a>, <a href="/search/astro-ph?searchtype=author&query=Piotrowska%2C+J+M">Joanna M. Piotrowska</a>, <a href="/search/astro-ph?searchtype=author&query=Bezanson%2C+R">Rachel Bezanson</a>, <a href="/search/astro-ph?searchtype=author&query=Taylor%2C+E+N">Edward N. Taylor</a>, <a href="/search/astro-ph?searchtype=author&query=van+de+Sande%2C+J">Jesse van de Sande</a>, <a href="/search/astro-ph?searchtype=author&query=Baker%2C+W+M">William M. Baker</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+E+F">Eric F. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Bellstedt%2C+S">Sabine Bellstedt</a>, <a href="/search/astro-ph?searchtype=author&query=Bland-Hawthorn%2C+J">Joss Bland-Hawthorn</a>, <a href="/search/astro-ph?searchtype=author&query=Bluck%2C+A+F+L">Asa F. L. Bluck</a>, <a href="/search/astro-ph?searchtype=author&query=Brough%2C+S">Sarah Brough</a>, <a href="/search/astro-ph?searchtype=author&query=Bryant%2C+J+J">Julia J. Bryant</a>, <a href="/search/astro-ph?searchtype=author&query=Colless%2C+M">Matthew Colless</a>, <a href="/search/astro-ph?searchtype=author&query=Cortese%2C+L">Luca Cortese</a>, <a href="/search/astro-ph?searchtype=author&query=Croom%2C+S+M">Scott M. Croom</a>, <a href="/search/astro-ph?searchtype=author&query=Derkenne%2C+C">Caro Derkenne</a>, <a href="/search/astro-ph?searchtype=author&query=van+Dokkum%2C+P">Pieter van Dokkum</a>, <a href="/search/astro-ph?searchtype=author&query=Fisher%2C+D">Deanne Fisher</a>, <a href="/search/astro-ph?searchtype=author&query=Foster%2C+C">Caroline Foster</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">Anna Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=de+Graaff%2C+A">Anna de Graaff</a>, <a href="/search/astro-ph?searchtype=author&query=Groves%2C+B">Brent Groves</a>, <a href="/search/astro-ph?searchtype=author&query=van+Houdt%2C+J">Josha van Houdt</a>, <a href="/search/astro-ph?searchtype=author&query=Lagos%2C+C+d+P">Claudia del P. Lagos</a> , et al. (15 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="2303.05520v1-abstract-short" style="display: inline;"> We present the first study of spatially integrated higher-order stellar kinematics over cosmic time. We use deep rest-frame optical spectroscopy of quiescent galaxies at redshifts z=0.05, 0.3 and 0.8 from the SAMI, MAGPI and LEGA-C surveys to measure the excess kurtosis $h_4$ of the stellar velocity distribution, the latter parametrised as a Gauss-Hermite series. Conservatively using a redshift-in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.05520v1-abstract-full').style.display = 'inline'; document.getElementById('2303.05520v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.05520v1-abstract-full" style="display: none;"> We present the first study of spatially integrated higher-order stellar kinematics over cosmic time. We use deep rest-frame optical spectroscopy of quiescent galaxies at redshifts z=0.05, 0.3 and 0.8 from the SAMI, MAGPI and LEGA-C surveys to measure the excess kurtosis $h_4$ of the stellar velocity distribution, the latter parametrised as a Gauss-Hermite series. Conservatively using a redshift-independent cut in stellar mass ($M_\star = 10^{11}\,{\rm M}_\odot$), and matching the stellar-mass distributions of our samples, we find 7 $蟽$ evidence of $h_4$ increasing with cosmic time, from a median value of 0.019$\pm$0.002 at z=0.8 to 0.059$\pm$0.004 at z=0.06. Alternatively, we use a physically motivated sample selection, based on the mass distribution of the progenitors of local quiescent galaxies as inferred from numerical simulations; in this case, we find 10 $蟽$ evidence. This evolution suggests that, over the last 7 Gyr, there has been a gradual decrease in the rotation-to-dispersion ratio and an increase in the radial anisotropy of the stellar velocity distribution, qualitatively consistent with accretion of gas-poor satellites. These findings demonstrate that massive galaxies continue to accrete mass and increase their dispersion support after becoming quiescent. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.05520v1-abstract-full').style.display = 'none'; document.getElementById('2303.05520v1-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, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 9 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/2303.04157">arXiv:2303.04157</a> <span> [<a href="https://arxiv.org/pdf/2303.04157">pdf</a>, <a href="https://arxiv.org/format/2303.04157">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"> Different higher-order kinematics between star-forming and quiescent galaxies based on the SAMI, MAGPI and LEGA-C surveys </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=D%27Eugenio%2C+F">Francesco D'Eugenio</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Wel%2C+A">Arjen van der Wel</a>, <a href="/search/astro-ph?searchtype=author&query=Derkenne%2C+C">Caro Derkenne</a>, <a href="/search/astro-ph?searchtype=author&query=van+Houdt%2C+J">Josha van Houdt</a>, <a href="/search/astro-ph?searchtype=author&query=Bezanson%2C+R">Rachel Bezanson</a>, <a href="/search/astro-ph?searchtype=author&query=Taylor%2C+E+N">Edward N. Taylor</a>, <a href="/search/astro-ph?searchtype=author&query=van+de+Sande%2C+J">Jesse van de Sande</a>, <a href="/search/astro-ph?searchtype=author&query=Baker%2C+W+M">William M. Baker</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+E+F">Eric F. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Bland-Hawthorn%2C+J">Joss Bland-Hawthorn</a>, <a href="/search/astro-ph?searchtype=author&query=Bluck%2C+A+F+L">Asa F. L. Bluck</a>, <a href="/search/astro-ph?searchtype=author&query=Brough%2C+S">Sarah Brough</a>, <a href="/search/astro-ph?searchtype=author&query=Bryant%2C+J+J">Julia J. Bryant</a>, <a href="/search/astro-ph?searchtype=author&query=Colless%2C+M">Matthew Colless</a>, <a href="/search/astro-ph?searchtype=author&query=Cortese%2C+L">Luca Cortese</a>, <a href="/search/astro-ph?searchtype=author&query=Croom%2C+S+M">Scott M. Croom</a>, <a href="/search/astro-ph?searchtype=author&query=van+Dokkum%2C+P">Pieter van Dokkum</a>, <a href="/search/astro-ph?searchtype=author&query=Fisher%2C+D">Deanne Fisher</a>, <a href="/search/astro-ph?searchtype=author&query=Foster%2C+C">Caroline Foster</a>, <a href="/search/astro-ph?searchtype=author&query=Fraser-McKelvie%2C+A">Amelia Fraser-McKelvie</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">Anna Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=de+Graaff%2C+A">Anna de Graaff</a>, <a href="/search/astro-ph?searchtype=author&query=Groves%2C+B">Brent Groves</a>, <a href="/search/astro-ph?searchtype=author&query=Lagos%2C+C+d+P">Claudia del P. Lagos</a>, <a href="/search/astro-ph?searchtype=author&query=Looser%2C+T+J">Tobias J. Looser</a> , et al. (16 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.04157v1-abstract-short" style="display: inline;"> We present the first statistical study of spatially integrated non-Gaussian stellar kinematics spanning 7 Gyr in cosmic time. We use deep, rest-frame optical spectroscopy of massive galaxies (stellar mass $M_\star > 10^{10.5} {\rm M}_\odot$) at redshifts z = 0.05, 0.3 and 0.8 from the SAMI, MAGPI and LEGA-C surveys, to measure the excess kurtosis $h_4$ of the stellar velocity distribution, the lat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.04157v1-abstract-full').style.display = 'inline'; document.getElementById('2303.04157v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.04157v1-abstract-full" style="display: none;"> We present the first statistical study of spatially integrated non-Gaussian stellar kinematics spanning 7 Gyr in cosmic time. We use deep, rest-frame optical spectroscopy of massive galaxies (stellar mass $M_\star > 10^{10.5} {\rm M}_\odot$) at redshifts z = 0.05, 0.3 and 0.8 from the SAMI, MAGPI and LEGA-C surveys, to measure the excess kurtosis $h_4$ of the stellar velocity distribution, the latter parametrised as a Gauss-Hermite series. We find that at all redshifts where we have large enough samples, $h_4$ anti-correlates with the ratio between rotation and dispersion, highlighting the physical connection between these two kinematic observables. In addition, and independently from the anti-correlation with rotation-to-dispersion ratio, we also find a correlation between $h_4$ and $M_\star$, potentially connected to the assembly history of galaxies. In contrast, after controlling for mass, we find no evidence of independent correlation between $h_4$ and aperture velocity dispersion or galaxy size. These results hold for both star-forming and quiescent galaxies. For quiescent galaxies, $h_4$ also correlates with projected shape, even after controlling for the rotation-to-dispersion ratio. At any given redshift, star-forming galaxies have lower $h_4$ compared to quiescent galaxies, highlighting the link between kinematic structure and star-forming activity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.04157v1-abstract-full').style.display = 'none'; document.getElementById('2303.04157v1-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 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">26 pages, 15 figures Accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.10936">arXiv:2302.10936</a> <span> [<a href="https://arxiv.org/pdf/2302.10936">pdf</a>, <a href="https://arxiv.org/format/2302.10936">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/acbefa">10.3847/1538-4357/acbefa <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An Atlas of Color-selected Quiescent Galaxies at $z>3$ in Public $JWST$ Fields </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=Brammer%2C+G">Gabriel Brammer</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=Kokorev%2C+V">Vasily Kokorev</a>, <a href="/search/astro-ph?searchtype=author&query=Fujimoto%2C+S">Seiji Fujimoto</a>, <a href="/search/astro-ph?searchtype=author&query=Jespersen%2C+C+K">Christian Kragh Jespersen</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=Weaver%2C+J+R">John R. Weaver</a>, <a href="/search/astro-ph?searchtype=author&query=Ito%2C+K">Kei Ito</a>, <a href="/search/astro-ph?searchtype=author&query=Tanaka%2C+M">Masayuki Tanaka</a>, <a href="/search/astro-ph?searchtype=author&query=Ilbert%2C+O">Olivier Ilbert</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=Whitaker%2C+K+E">Katherine E. Whitaker</a>, <a href="/search/astro-ph?searchtype=author&query=Faisst%2C+A+L">Andreas L. Faisst</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">Anna Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Gillman%2C+S">Steven Gillman</a>, <a href="/search/astro-ph?searchtype=author&query=Gimenez-Arteaga%2C+C">Clara Gimenez-Arteaga</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=Kubo%2C+M">Mariko Kubo</a>, <a href="/search/astro-ph?searchtype=author&query=Heintz%2C+K+E">Kasper E. Heintz</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">Michaela Hirschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Oesch%2C+P">Pascal Oesch</a>, <a href="/search/astro-ph?searchtype=author&query=Onodera%2C+M">Masato Onodera</a>, <a href="/search/astro-ph?searchtype=author&query=Rizzo%2C+F">Francesca Rizzo</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+M">Minju Lee</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="2302.10936v1-abstract-short" style="display: inline;"> We present the results of a systematic search for candidate quiescent galaxies in the distant Universe in eleven $JWST$ fields with publicly available observations collected during the first three months of operations and covering an effective sky area of $\sim145$ arcmin$^2$. We homogeneously reduce the new $JWST$ data and combine them with existing observations from the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.10936v1-abstract-full').style.display = 'inline'; document.getElementById('2302.10936v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.10936v1-abstract-full" style="display: none;"> We present the results of a systematic search for candidate quiescent galaxies in the distant Universe in eleven $JWST$ fields with publicly available observations collected during the first three months of operations and covering an effective sky area of $\sim145$ arcmin$^2$. We homogeneously reduce the new $JWST$ data and combine them with existing observations from the $Hubble\,Space\,Telescope$. We select a robust sample of $\sim80$ candidate quiescent and quenching galaxies at $3 < z < 5$ using two methods: (1) based on their rest-frame $UVJ$ colors, and (2) a novel quantitative approach based on Gaussian Mixture Modeling of the $NUV-U$, $U-V$, and $V-J$ rest-frame color space, which is more sensitive to recently quenched objects. We measure comoving number densities of massive ($M_\star\geq 10^{10.6} M_\odot$) quiescent galaxies consistent with previous estimates relying on ground-based observations, after homogenizing the results in the literature with our mass and redshift intervals. However, we find significant field-to-field variations of the number densities up to a factor of $2-3$, highlighting the effect of cosmic variance and suggesting the presence of overdensities of red quiescent galaxies at $z>3$, as it could be expected for highly clustered massive systems. Importantly, $JWST$ enables the robust identification of quenching/quiescent galaxy candidates at lower masses and higher redshifts than before, challenging standard formation scenarios. All data products, including the literature compilation, are made publicly available. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.10936v1-abstract-full').style.display = 'none'; document.getElementById('2302.10936v1-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 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 6 Figures + Appendix. Accepted for publication in ApJ on Feb, 9. Data release: - Reduced HST+JWST mosaics + photometric catalogs and Eazy-py modeling: https://erda.ku.dk/archives/7166d013c1ca1371aac3c57b9e73190d/published-archive.html - Supplementary material and tables: https://zenodo.org/record/7614908#.Y-4ZruzMLmE - MAST: https://doi.org/10.17909/g3nt-a370 - See also Gould et al. 2023</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.07366">arXiv:2302.07366</a> <span> [<a href="https://arxiv.org/pdf/2302.07366">pdf</a>, <a href="https://arxiv.org/format/2302.07366">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/10.1051/0004-6361/202245361">10.1051/0004-6361/202245361 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> WEAVE-StePS. A stellar population survey using WEAVE at WHT </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Iovino%2C+A">A. Iovino</a>, <a href="/search/astro-ph?searchtype=author&query=Poggianti%2C+B+M">B. M. Poggianti</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">A. Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Longhetti%2C+M">M. Longhetti</a>, <a href="/search/astro-ph?searchtype=author&query=Bolzonella%2C+M">M. Bolzonella</a>, <a href="/search/astro-ph?searchtype=author&query=Busarello%2C+G">G. Busarello</a>, <a href="/search/astro-ph?searchtype=author&query=Gullieuszik%2C+M">M. Gullieuszik</a>, <a href="/search/astro-ph?searchtype=author&query=LaBarbera%2C+F">F. LaBarbera</a>, <a href="/search/astro-ph?searchtype=author&query=Merluzzi%2C+P">P. Merluzzi</a>, <a href="/search/astro-ph?searchtype=author&query=Morelli%2C+L">L. Morelli</a>, <a href="/search/astro-ph?searchtype=author&query=Tortora%2C+C">C. Tortora</a>, <a href="/search/astro-ph?searchtype=author&query=Vergani%2C+D">D. Vergani</a>, <a href="/search/astro-ph?searchtype=author&query=Zibetti%2C+S">S. Zibetti</a>, <a href="/search/astro-ph?searchtype=author&query=Haines%2C+C+P">C. P. Haines</a>, <a href="/search/astro-ph?searchtype=author&query=Costantin%2C+L">L. Costantin</a>, <a href="/search/astro-ph?searchtype=author&query=Ditrani%2C+F+R">F. R. Ditrani</a>, <a href="/search/astro-ph?searchtype=author&query=Pozzetti%2C+L">L. Pozzetti</a>, <a href="/search/astro-ph?searchtype=author&query=Angthopo%2C+J">J. Angthopo</a>, <a href="/search/astro-ph?searchtype=author&query=Balcells%2C+M">M. Balcells</a>, <a href="/search/astro-ph?searchtype=author&query=Bardelli%2C+S">S. Bardelli</a>, <a href="/search/astro-ph?searchtype=author&query=Benn%2C+C+R">C. R. Benn</a>, <a href="/search/astro-ph?searchtype=author&query=Bianconi%2C+M">M. Bianconi</a>, <a href="/search/astro-ph?searchtype=author&query=Cassar%C3%A0%2C+L+P">L. P. Cassar脿</a>, <a href="/search/astro-ph?searchtype=author&query=Corsini%2C+E+M">E. M. Corsini</a>, <a href="/search/astro-ph?searchtype=author&query=Cucciati%2C+O">O. Cucciati</a> , et al. (22 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2302.07366v1-abstract-short" style="display: inline;"> The upcoming new generation of optical spectrographs on four-meter-class telescopes will provide valuable opportunities for forthcoming galaxy surveys through their huge multiplexing capabilities, excellent spectral resolution, and unprecedented wavelength coverage. WEAVE is a new wide-field spectroscopic facility mounted on the 4.2 m William Herschel Telescope in La Palma. WEAVE-StePS is one of t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.07366v1-abstract-full').style.display = 'inline'; document.getElementById('2302.07366v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.07366v1-abstract-full" style="display: none;"> The upcoming new generation of optical spectrographs on four-meter-class telescopes will provide valuable opportunities for forthcoming galaxy surveys through their huge multiplexing capabilities, excellent spectral resolution, and unprecedented wavelength coverage. WEAVE is a new wide-field spectroscopic facility mounted on the 4.2 m William Herschel Telescope in La Palma. WEAVE-StePS is one of the five extragalactic surveys that will use WEAVE during its first five years of operations. It will observe galaxies using WEAVE MOS (~950 fibres across a field of view of ~3 deg2 on the sky) in low-resolution mode (R~5000, spanning the wavelength range 3660-9590 AA). WEAVE-StePS will obtain high-quality spectra (S/N ~ 10 per AA at R~5000) for a magnitude-limited (I_AB = 20.5) sample of ~25,000 galaxies, the majority selected at z>=0.3. The survey goal is to provide precise spectral measurements in the crucial interval that bridges the gap between LEGA-C and SDSS data. The wide area coverage of ~25 deg2 will enable us to observe galaxies in a variety of environments. The ancillary data available in each observed field (including X-ray coverage, multi-narrow-band photometry and spectroscopic redshift information) will provide an environmental characterisation for each observed galaxy. This paper presents the science case of WEAVE-StePS, the fields to be observed, the parent catalogues used to define the target sample, and the observing strategy chosen after a forecast of the expected performance of the instrument for our typical targets. WEAVE-StePS will go back further in cosmic time than SDSS, extending its reach to encompass more than ~6 Gyr, nearly half of the age of the Universe. The spectral and redshift range covered by WEAVE-StePS will open a new observational window by continuously tracing the evolutionary path of galaxies in the largely unexplored intermediate-redshift range. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.07366v1-abstract-full').style.display = 'none'; document.getElementById('2302.07366v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 9 figures, A&A in press</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 672, A87 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.05453">arXiv:2302.05453</a> <span> [<a href="https://arxiv.org/pdf/2302.05453">pdf</a>, <a href="https://arxiv.org/format/2302.05453">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/10.1051/0004-6361/202245542">10.1051/0004-6361/202245542 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> INSPIRE: INvestigating Stellar Population In RElics III. Second data release (DR2): testing the systematics on the stellar velocity dispersion </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=D%27Ago%2C+G">G. D'Ago</a>, <a href="/search/astro-ph?searchtype=author&query=Spiniello%2C+C">C. Spiniello</a>, <a href="/search/astro-ph?searchtype=author&query=Coccato%2C+L">L. Coccato</a>, <a href="/search/astro-ph?searchtype=author&query=Tortora%2C+C">C. Tortora</a>, <a href="/search/astro-ph?searchtype=author&query=La+Barbera%2C+F">F. La Barbera</a>, <a href="/search/astro-ph?searchtype=author&query=Arnaboldi%2C+M">M. Arnaboldi</a>, <a href="/search/astro-ph?searchtype=author&query=Bevacqua%2C+D">D. Bevacqua</a>, <a href="/search/astro-ph?searchtype=author&query=Ferr%C3%A9-Mateu%2C+A">A. Ferr茅-Mateu</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">A. Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Hartke%2C+J">J. Hartke</a>, <a href="/search/astro-ph?searchtype=author&query=Hunt%2C+L+K">L. K. Hunt</a>, <a href="/search/astro-ph?searchtype=author&query=Mart%C3%ADn-Navarro%2C+I">I. Mart铆n-Navarro</a>, <a href="/search/astro-ph?searchtype=author&query=Napolitano%2C+N+R">N. R. Napolitano</a>, <a href="/search/astro-ph?searchtype=author&query=Pulsoni%2C+C">C. Pulsoni</a>, <a href="/search/astro-ph?searchtype=author&query=Radovich%2C+M">M. Radovich</a>, <a href="/search/astro-ph?searchtype=author&query=Saracco%2C+P">P. Saracco</a>, <a href="/search/astro-ph?searchtype=author&query=Scognamiglio%2C+D">D. Scognamiglio</a>, <a href="/search/astro-ph?searchtype=author&query=Zibetti%2C+S">S. Zibetti</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2302.05453v1-abstract-short" style="display: inline;"> This is the second data release (DR2) of the INvestigating Stellar Population In RElics (INSPIRE) project, comprising 21 new systems with observations completed before March 2022. For each system, we release four one-dimensional (1D) spectra to the ESO Science Archive, one spectrum for each arm of the X-Shooter spectrograph. In this paper, we focus on the line-of-sight velocity distribution, measu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.05453v1-abstract-full').style.display = 'inline'; document.getElementById('2302.05453v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.05453v1-abstract-full" style="display: none;"> This is the second data release (DR2) of the INvestigating Stellar Population In RElics (INSPIRE) project, comprising 21 new systems with observations completed before March 2022. For each system, we release four one-dimensional (1D) spectra to the ESO Science Archive, one spectrum for each arm of the X-Shooter spectrograph. In this paper, we focus on the line-of-sight velocity distribution, measuring integrated stellar velocity dispersions from the spectra, and assessing their robustness and the associated uncertainties. For each of the 21 new systems, we systematically investigated the effect of the parameters and set-ups of the full spectral fitting on the stellar velocity dispersion ($蟽$) measurements. In particular, we tested how $蟽$ changes when several parameters of the fit as well as the resolution and spectral coverage of the input spectra are varied. We found that the effect that causes the largest systematic uncertainties on $蟽$ is the wavelength range used for the fit, especially for spectra with a lower signal-to-noise ratio (S/N $\leq$ 30). When using blue wavelengths (UVB arm) one generally underestimates the velocity dispersion (by $\sim$15 km/s). The values obtained from the near-IR (NIR) arm present a larger scatter because the quality of the spectra is lower. We finally compared our results with those in literature, finding a very good agreement overall. Joining results obtained in DR1 with those presented here, INSPIRE contains 40 ultra-compact massive galaxies, corresponding to 75% of the whole survey. By plotting these systems in a stellar mass-velocity dispersion diagram, we identify at least four highly reliable relic candidates among the new systems. Their velocity dispersion is larger than that of normal-sized galaxies of similar stellar mass. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.05453v1-abstract-full').style.display = 'none'; document.getElementById('2302.05453v1-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 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication, and in press on A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 672, A17 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.03981">arXiv:2212.03981</a> <span> [<a href="https://arxiv.org/pdf/2212.03981">pdf</a>, <a href="https://arxiv.org/format/2212.03981">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stad557">10.1093/mnras/stad557 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The wide-field, multiplexed, spectroscopic facility WEAVE: Survey design, overview, and simulated implementation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jin%2C+S">Shoko Jin</a>, <a href="/search/astro-ph?searchtype=author&query=Trager%2C+S+C">Scott C. Trager</a>, <a href="/search/astro-ph?searchtype=author&query=Dalton%2C+G+B">Gavin B. Dalton</a>, <a href="/search/astro-ph?searchtype=author&query=Aguerri%2C+J+A+L">J. Alfonso L. Aguerri</a>, <a href="/search/astro-ph?searchtype=author&query=Drew%2C+J+E">J. E. Drew</a>, <a href="/search/astro-ph?searchtype=author&query=Falc%C3%B3n-Barroso%2C+J">Jes煤s Falc贸n-Barroso</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%A4nsicke%2C+B+T">Boris T. G盲nsicke</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+V">Vanessa Hill</a>, <a href="/search/astro-ph?searchtype=author&query=Iovino%2C+A">Angela Iovino</a>, <a href="/search/astro-ph?searchtype=author&query=Pieri%2C+M+M">Matthew M. Pieri</a>, <a href="/search/astro-ph?searchtype=author&query=Poggianti%2C+B+M">Bianca M. Poggianti</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+D+J+B">D. J. B. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">Antonella Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Abrams%2C+D+C">Don Carlos Abrams</a>, <a href="/search/astro-ph?searchtype=author&query=Aguado%2C+D+S">David S. Aguado</a>, <a href="/search/astro-ph?searchtype=author&query=Antoja%2C+T">Teresa Antoja</a>, <a href="/search/astro-ph?searchtype=author&query=Arag%C3%B3n-Salamanca%2C+A">Alfonso Arag贸n-Salamanca</a>, <a href="/search/astro-ph?searchtype=author&query=Ascasibar%2C+Y">Yago Ascasibar</a>, <a href="/search/astro-ph?searchtype=author&query=Babusiaux%2C+C">Carine Babusiaux</a>, <a href="/search/astro-ph?searchtype=author&query=Balcells%2C+M">Marc Balcells</a>, <a href="/search/astro-ph?searchtype=author&query=Barrena%2C+R">R. Barrena</a>, <a href="/search/astro-ph?searchtype=author&query=Battaglia%2C+G">Giuseppina Battaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Belokurov%2C+V">Vasily Belokurov</a>, <a href="/search/astro-ph?searchtype=author&query=Bensby%2C+T">Thomas Bensby</a>, <a href="/search/astro-ph?searchtype=author&query=Bonifacio%2C+P">Piercarlo Bonifacio</a> , et al. (190 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2212.03981v2-abstract-short" style="display: inline;"> WEAVE, the new wide-field, massively multiplexed spectroscopic survey facility for the William Herschel Telescope, will see first light in late 2022. WEAVE comprises a new 2-degree field-of-view prime-focus corrector system, a nearly 1000-multiplex fibre positioner, 20 individually deployable 'mini' integral field units (IFUs), and a single large IFU. These fibre systems feed a dual-beam spectrogr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.03981v2-abstract-full').style.display = 'inline'; document.getElementById('2212.03981v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.03981v2-abstract-full" style="display: none;"> WEAVE, the new wide-field, massively multiplexed spectroscopic survey facility for the William Herschel Telescope, will see first light in late 2022. WEAVE comprises a new 2-degree field-of-view prime-focus corrector system, a nearly 1000-multiplex fibre positioner, 20 individually deployable 'mini' integral field units (IFUs), and a single large IFU. These fibre systems feed a dual-beam spectrograph covering the wavelength range 366$-$959\,nm at $R\sim5000$, or two shorter ranges at $R\sim20\,000$. After summarising the design and implementation of WEAVE and its data systems, we present the organisation, science drivers and design of a five- to seven-year programme of eight individual surveys to: (i) study our Galaxy's origins by completing Gaia's phase-space information, providing metallicities to its limiting magnitude for $\sim$3 million stars and detailed abundances for $\sim1.5$ million brighter field and open-cluster stars; (ii) survey $\sim0.4$ million Galactic-plane OBA stars, young stellar objects and nearby gas to understand the evolution of young stars and their environments; (iii) perform an extensive spectral survey of white dwarfs; (iv) survey $\sim400$ neutral-hydrogen-selected galaxies with the IFUs; (v) study properties and kinematics of stellar populations and ionised gas in $z<0.5$ cluster galaxies; (vi) survey stellar populations and kinematics in $\sim25\,000$ field galaxies at $0.3\lesssim z \lesssim 0.7$; (vii) study the cosmic evolution of accretion and star formation using $>1$ million spectra of LOFAR-selected radio sources; (viii) trace structures using intergalactic/circumgalactic gas at $z>2$. Finally, we describe the WEAVE Operational Rehearsals using the WEAVE Simulator. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.03981v2-abstract-full').style.display = 'none'; document.getElementById('2212.03981v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 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">41 pages, 27 figures, accepted for publication by MNRAS; updated version including information on individual grants in a revised Acknowledgements section, corrections to the affiliation list, and an updated references list</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.06194">arXiv:2203.06194</a> <span> [<a href="https://arxiv.org/pdf/2203.06194">pdf</a>, <a href="https://arxiv.org/format/2203.06194">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac4e18">10.3847/1538-4357/ac4e18 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> LEGA-C: analysis of dynamical masses from ionized gas and stellar kinematics at z~0.8 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Straatman%2C+C+M+S">Caroline M. S. Straatman</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Wel%2C+A">Arjen van der Wel</a>, <a href="/search/astro-ph?searchtype=author&query=van+Houdt%2C+J">Josha van Houdt</a>, <a href="/search/astro-ph?searchtype=author&query=Bezanson%2C+R">Rachel Bezanson</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+E+F">Eric F. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=van+Dokkum%2C+P">Pieter van Dokkum</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Eugenio%2C+F">Francesco D'Eugenio</a>, <a href="/search/astro-ph?searchtype=author&query=Franx%2C+M">Marijn Franx</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">Anna Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=de+Graaff%2C+A">Anna de Graaff</a>, <a href="/search/astro-ph?searchtype=author&query=Maseda%2C+M">Michael Maseda</a>, <a href="/search/astro-ph?searchtype=author&query=Meidt%2C+S+E">Sharon E. Meidt</a>, <a href="/search/astro-ph?searchtype=author&query=Muzzin%2C+A">Adam Muzzin</a>, <a href="/search/astro-ph?searchtype=author&query=Sobral%2C+D">David Sobral</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+P">Po-Feng Wu</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="2203.06194v1-abstract-short" style="display: inline;"> We compare dynamical mass estimates based on spatially extended stellar and ionized gas kinematics ($\mathrm{M_{dyn,*}}$ and $\mathrm{M_{dyn,eml}}$, respectively) of 157 star forming galaxies at $0.6\leq z<1$. Compared to $z\sim0$, these galaxies have enhanced star formation rates, with stellar feedback likely affecting the dynamics of the gas. We use LEGA-C DR3, the highest redshift dataset provi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.06194v1-abstract-full').style.display = 'inline'; document.getElementById('2203.06194v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.06194v1-abstract-full" style="display: none;"> We compare dynamical mass estimates based on spatially extended stellar and ionized gas kinematics ($\mathrm{M_{dyn,*}}$ and $\mathrm{M_{dyn,eml}}$, respectively) of 157 star forming galaxies at $0.6\leq z<1$. Compared to $z\sim0$, these galaxies have enhanced star formation rates, with stellar feedback likely affecting the dynamics of the gas. We use LEGA-C DR3, the highest redshift dataset providing sufficiently deep measurements of a $K_s-$band limited sample. For $\mathrm{M_{dyn,*}}$ we use Jeans Anisotropic Multi-Gaussian Expansion models. For $\mathrm{M_{dyn,eml}}$ we first fit a custom model of a rotating exponential disk with uniform dispersion, whose light is projected through a slit and corrected for beam smearing. We then apply an asymmetric drift correction based on assumptions common in the literature to the fitted kinematic components to obtain the circular velocity, assuming hydrostatic equilibrium. Within the half-light radius, $\mathrm{M_{dyn,eml}}$ is on average lower than $\mathrm{M_{dyn,*}}$, with a mean offset of $-0.15\pm0.016$ dex and galaxy-to-galaxy scatter of $0.19$ dex, reflecting the combined random uncertainty. While data of higher spatial resolution are needed to understand this small offset, it supports the assumption that the galaxy-wide ionized gas kinematics do not predominantly originate from disruptive events such as star formation driven outflows. However, a similar agreement can be obtained without modeling from the integrated emission line dispersions for axis ratios $q<0.8$. This suggests that our current understanding of gas kinematics is not sufficient to efficiently apply asymmetric drift corrections to improve dynamical mass estimates compared to observations lacking the $S/N$ required for spatially extended dynamics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.06194v1-abstract-full').style.display = 'none'; document.getElementById('2203.06194v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">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">19 pages, 7 figures, accepted for publication by 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/2203.04979">arXiv:2203.04979</a> <span> [<a href="https://arxiv.org/pdf/2203.04979">pdf</a>, <a href="https://arxiv.org/format/2203.04979">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/aca677">10.3847/1538-4357/aca677 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> REQUIEM-2D: A diversity of formation pathways in a sample of spatially-resolved massive quiescent galaxies at z~2 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Akhshik%2C+M">Mohammad Akhshik</a>, <a href="/search/astro-ph?searchtype=author&query=Whitaker%2C+K+E">Katherine E. Whitaker</a>, <a href="/search/astro-ph?searchtype=author&query=Leja%2C+J">Joel Leja</a>, <a href="/search/astro-ph?searchtype=author&query=Richard%2C+J">Johan Richard</a>, <a href="/search/astro-ph?searchtype=author&query=Spilker%2C+J+S">Justin S. Spilker</a>, <a href="/search/astro-ph?searchtype=author&query=Song%2C+M">Mimi Song</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G">Gabriel Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Bezanson%2C+R">Rachel Bezanson</a>, <a href="/search/astro-ph?searchtype=author&query=Ebeling%2C+H">Harald Ebeling</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A+R">Anna R. Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Mahler%2C+G">Guillaume Mahler</a>, <a href="/search/astro-ph?searchtype=author&query=Mowla%2C+L+A">Lamiya A. Mowla</a>, <a href="/search/astro-ph?searchtype=author&query=Nelson%2C+E+J">Erica J. Nelson</a>, <a href="/search/astro-ph?searchtype=author&query=Pacifici%2C+C">Camilla Pacifici</a>, <a href="/search/astro-ph?searchtype=author&query=Sharon%2C+K">Keren Sharon</a>, <a href="/search/astro-ph?searchtype=author&query=Toft%2C+S">Sune Toft</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+C+C">Christina C. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Wright%2C+L">Lillian Wright</a>, <a href="/search/astro-ph?searchtype=author&query=Zabl%2C+J">Johannes Zabl</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="2203.04979v1-abstract-short" style="display: inline;"> REQUIEM-2D (REsolving QUIEscent Magnified galaxies with 2D grism spectroscopy) is comprised of a sample of 8 massive ($\log M_*/M_\odot > 10.6$) strongly lensed quiescent galaxies at $z\sim2$. REQUIEM-2D combines the natural magnification from strong gravitational lensing with the high spatial-resolution grism spectroscopy of \emph{Hubble Space Telescope} through a spectrophotometric fit to study… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.04979v1-abstract-full').style.display = 'inline'; document.getElementById('2203.04979v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.04979v1-abstract-full" style="display: none;"> REQUIEM-2D (REsolving QUIEscent Magnified galaxies with 2D grism spectroscopy) is comprised of a sample of 8 massive ($\log M_*/M_\odot > 10.6$) strongly lensed quiescent galaxies at $z\sim2$. REQUIEM-2D combines the natural magnification from strong gravitational lensing with the high spatial-resolution grism spectroscopy of \emph{Hubble Space Telescope} through a spectrophotometric fit to study spatially resolved stellar populations. We show that quiescent galaxies in the REQUIEM-2D survey have diverse formation histories manifesting as a gradient in stellar ages, including examples of (1) a younger central region supporting outside-in formation, (2) flat age gradients that show evidence for both spatially-uniform early formation or inside-out quenching, and (3) regions at a fixed radial distance having different ages (such asymmetries cannot be recovered when averaging stellar population measurements azimuthally). The typical dust attenuation curve for the REQUIEM-2D galaxies is constrained to be steeper than Calzetti's law in the UV and generally consistent with $A_V<1$. Combined together and accounting for the different physical radial distances and formation time-scales, we find that the REQUIEM-2D galaxies that formed earlier in the universe exhibit slow and uniform growth in their inner core, whereas the galaxies that formed later have rapid inner growth in their inner core with younger ages relative to the outskirts. These results challenge the currently accepted paradigm of how massive quiescent galaxies form, where the earliest galaxies are thought to form most rapidly. Significantly larger samples close to the epoch of formation with similar data quality and higher spectral resolution are required to validate this finding. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.04979v1-abstract-full').style.display = 'none'; document.getElementById('2203.04979v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">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">Submitted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2202.03975">arXiv:2202.03975</a> <span> [<a href="https://arxiv.org/pdf/2202.03975">pdf</a>, <a href="https://arxiv.org/format/2202.03975">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/stac370">10.1093/mnras/stac370 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Stellar mass as the "glocal" driver of galaxies' stellar population properties </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zibetti%2C+S">Stefano Zibetti</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A+R">Anna R. Gallazzi</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="2202.03975v1-abstract-short" style="display: inline;"> The properties of the stellar populations in a galaxy are known to correlate with the amount and the distribution of stellar mass. We take advantage of the maps of light-weighted mean stellar age Agewr and metallicity Z*wr for a sample of 362 galaxies from the integral-field spectroscopic survey CALIFA (summing up to >600,000 individual regions of approximately 1 kpc linear size), produced in our… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.03975v1-abstract-full').style.display = 'inline'; document.getElementById('2202.03975v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.03975v1-abstract-full" style="display: none;"> The properties of the stellar populations in a galaxy are known to correlate with the amount and the distribution of stellar mass. We take advantage of the maps of light-weighted mean stellar age Agewr and metallicity Z*wr for a sample of 362 galaxies from the integral-field spectroscopic survey CALIFA (summing up to >600,000 individual regions of approximately 1 kpc linear size), produced in our previous works, to investigate how these local properties react to the local stellar-mass surface density mu* and to the global total stellar mass M* and mean stellar-mass surface density <mu>e. We establish the existence of i) a dual mu*-Agewr relation, resulting in a young sequence and an old ridge, and ii) a mu*-Z*wr relation, overall independent of the age of the regions. The global mass parameters (M* and, possibly secondarily, <mu>e) determine the distribution of mu* in a galaxy and set the maximum attainable mu*, which increases with M*. M* affects the shape and normalization of the local relations up to a threshold mass of $\sim 10^{10.3}$ MSun, above which they remain unchanged. We conclude that stellar mass is a "glocal" (i.e. simultaneously global and local) driver of the stellar population properties. We consider how the local and global mass-age and mass-metallicity relations are connected, and in particular discuss how it is possible, from a single local relation, to produce two different global mass-metallicity relations for quiescent and star-forming galaxies respectively, as reported in the literature. Structural differences in these two classes of galaxies are key to explain the duality in global scaling relations and appear as essential in modelling the baryonic cycle of galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.03975v1-abstract-full').style.display = 'none'; document.getElementById('2202.03975v1-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 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">Accepted for publication on 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/2112.08372">arXiv:2112.08372</a> <span> [<a href="https://arxiv.org/pdf/2112.08372">pdf</a>, <a href="https://arxiv.org/format/2112.08372">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/ac4419">10.3847/1538-4357/ac4419 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The LEGA-C of nature and nurture in stellar populations of galaxies at z~0.6-1.0: D4000 and H-delta reveal different assembly histories for quiescent galaxies in different environments </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sobral%2C+D">David Sobral</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Wel%2C+A">Arjen van der Wel</a>, <a href="/search/astro-ph?searchtype=author&query=Bezanson%2C+R">Rachel Bezanson</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+E">Eric Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Muzzin%2C+A">Adam Muzzin</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Eugenio%2C+F">Francesco D'Eugenio</a>, <a href="/search/astro-ph?searchtype=author&query=Darvish%2C+B">Behnam Darvish</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">Anna Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+P">Po-Feng Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Maseda%2C+M">Michael Maseda</a>, <a href="/search/astro-ph?searchtype=author&query=Matthee%2C+J">Jorryt Matthee</a>, <a href="/search/astro-ph?searchtype=author&query=Paulino-Afonso%2C+A">Ana Paulino-Afonso</a>, <a href="/search/astro-ph?searchtype=author&query=Straatman%2C+C">Caroline Straatman</a>, <a href="/search/astro-ph?searchtype=author&query=van+Dokkum%2C+P">Pieter van Dokkum</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2112.08372v1-abstract-short" style="display: inline;"> Galaxy evolution is driven by a variety of physical processes which are predicted to proceed at different rates for different dark matter haloes and environments across cosmic times. A record of this evolution is preserved in galaxy stellar populations, which we can access using absorption-line spectroscopy. Here we explore the large LEGA-C survey (DR3) to investigate the role of the environment a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.08372v1-abstract-full').style.display = 'inline'; document.getElementById('2112.08372v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.08372v1-abstract-full" style="display: none;"> Galaxy evolution is driven by a variety of physical processes which are predicted to proceed at different rates for different dark matter haloes and environments across cosmic times. A record of this evolution is preserved in galaxy stellar populations, which we can access using absorption-line spectroscopy. Here we explore the large LEGA-C survey (DR3) to investigate the role of the environment and stellar mass on stellar populations at z~0.6-1.0 in the COSMOS field. Leveraging the statistical power and depth of LEGA-C, we reveal significant gradients in D4000 and H-delta equivalent widths (EWs) distributions over the stellar mass vs environment 2D spaces for the massive galaxy population (M>10^10 M$_{\odot}$) at z~0.6-1.0. D4000 and H-delta EWs primarily depend on stellar mass, but they also depend on environment at fixed stellar mass. By splitting the sample into centrals and satellites, and in terms of star-forming galaxies and quiescent galaxies, we reveal that the significant environmental trends of D4000 and H-delta EW when controlling for stellar mass are driven by quiescent galaxies. Regardless of being centrals or satellites, star-forming galaxies reveal D4000 and H-delta EWs which depend strongly on their stellar mass and are completely independent of the environment at 0.6<z<1.0. The environmental trends seen for satellite galaxies are fully driven by the trends that hold only for quiescent galaxies, combined with the strong environmental dependency of the quiescent fraction at fixed stellar mass. Our results are consistent with recent predictions from simulations that point towards massive galaxies forming first in over-densities or the most compact dark matter haloes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.08372v1-abstract-full').style.display = 'none'; document.getElementById('2112.08372v1-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 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApJ. 18 pages, 9 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2110.00009">arXiv:2110.00009</a> <span> [<a href="https://arxiv.org/pdf/2110.00009">pdf</a>, <a href="https://arxiv.org/format/2110.00009">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac2bfe">10.3847/1538-4357/ac2bfe <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Ubiquitous [OII] Emission in Quiescent Galaxies at z ~ 0.85 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Maseda%2C+M+V">Michael V. Maseda</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Wel%2C+A">Arjen van der Wel</a>, <a href="/search/astro-ph?searchtype=author&query=Franx%2C+M">Marijn Franx</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+E+F">Eric F. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Bezanson%2C+R">Rachel Bezanson</a>, <a href="/search/astro-ph?searchtype=author&query=Muzzin%2C+A">Adam Muzzin</a>, <a href="/search/astro-ph?searchtype=author&query=Sobral%2C+D">David Sobral</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Eugenio%2C+F">Francesco D'Eugenio</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">Anna Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=de+Graaff%2C+A">Anna de Graaff</a>, <a href="/search/astro-ph?searchtype=author&query=Leja%2C+J">Joel Leja</a>, <a href="/search/astro-ph?searchtype=author&query=Straatman%2C+C">Caroline Straatman</a>, <a href="/search/astro-ph?searchtype=author&query=Whitaker%2C+K+E">Katherine E. Whitaker</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+C+C">Christina C. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+P">Po-Feng Wu</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2110.00009v1-abstract-short" style="display: inline;"> Using deep rest-frame optical spectroscopy from the Large Early Galaxy Astrophysical Census (LEGA-C) survey, conducted using VIMOS on the ESO Very Large Telescope, we systematically search for low-ionization [OII] 3726,3729 emission in the spectra of a mass-complete sample of z~0.85 galaxies. Intriguingly, we find that 59 percent of UVJ-quiescent (i.e. non star-forming) galaxies in the sample have… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.00009v1-abstract-full').style.display = 'inline'; document.getElementById('2110.00009v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.00009v1-abstract-full" style="display: none;"> Using deep rest-frame optical spectroscopy from the Large Early Galaxy Astrophysical Census (LEGA-C) survey, conducted using VIMOS on the ESO Very Large Telescope, we systematically search for low-ionization [OII] 3726,3729 emission in the spectra of a mass-complete sample of z~0.85 galaxies. Intriguingly, we find that 59 percent of UVJ-quiescent (i.e. non star-forming) galaxies in the sample have ionized gas, as traced by [OII] emission, detected above our completeness limit of 1.5 Angstroms. The median stacked spectrum of the lowest equivalent width quiescent galaxies also shows [OII] emission. The overall fraction of sources with [OII] above our equivalent width limit is comparable to what we find in the low-redshift Universe from GAMA and MASSIVE, except perhaps at the highest stellar masses (log Mstar/Msol > 11.5). However, stacked spectra for the individual low-equivalent width systems uniquely indicates ubiquitous [OII] emission in the higher-z LEGA-C sample, with typical [OII] luminosities per unit stellar mass that are a factor of 3 larger than the lower-z GAMA sample. Star formation in these otherwise quiescent galaxies could play a role in producing the [OII] emission at higher-z, although it is unlikely to provide the bulk of the ionizing photons. More work is required to fully quantify the contributions of evolved stellar populations or active galactic nuclei to the observed spectra. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.00009v1-abstract-full').style.display = 'none'; document.getElementById('2110.00009v1-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, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">ApJ accepted: 16 pages, 11 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2108.10455">arXiv:2108.10455</a> <span> [<a href="https://arxiv.org/pdf/2108.10455">pdf</a>, <a href="https://arxiv.org/format/2108.10455">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/ac20d6">10.3847/1538-3881/ac20d6 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Towards precise galaxy evolution: a comparison between spectral indices of $z\sim1$ galaxies in the IllustrisTNG simulation and the LEGA-C survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wu%2C+P">Po-Feng Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Nelson%2C+D">Dylan Nelson</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Wel%2C+A">Arjen van der Wel</a>, <a href="/search/astro-ph?searchtype=author&query=Pillepich%2C+A">Annalisa Pillepich</a>, <a href="/search/astro-ph?searchtype=author&query=Zibetti%2C+S">Stefano Zibetti</a>, <a href="/search/astro-ph?searchtype=author&query=Bezanson%2C+R">Rachel Bezanson</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Eugenio%2C+F">Francesco D'Eugenio</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">Anna Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Pacifici%2C+C">Camilla Pacifici</a>, <a href="/search/astro-ph?searchtype=author&query=Straatman%2C+C+M+S">Caroline M. S. Straatman</a>, <a href="/search/astro-ph?searchtype=author&query=Bari%C5%A1i%C4%87%2C+I">Ivana Bari拧i膰</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+E+F">Eric F. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Maseda%2C+M+V">Michael V. Maseda</a>, <a href="/search/astro-ph?searchtype=author&query=Muzzin%2C+A">Adam Muzzin</a>, <a href="/search/astro-ph?searchtype=author&query=Sobral%2C+D">David Sobral</a>, <a href="/search/astro-ph?searchtype=author&query=Whitaker%2C+K+E">Katherine E. 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="2108.10455v2-abstract-short" style="display: inline;"> We present the first comparison of observed stellar continuum spectra of high-redshift galaxies and mock galaxy spectra generated from hydrodynamical simulations. The mock spectra are produced from the IllustrisTNG TNG100 simulation combined with stellar population models and take into account dust attenuation and realistic observational effects (aperture effects and noise). We compare the simulat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.10455v2-abstract-full').style.display = 'inline'; document.getElementById('2108.10455v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.10455v2-abstract-full" style="display: none;"> We present the first comparison of observed stellar continuum spectra of high-redshift galaxies and mock galaxy spectra generated from hydrodynamical simulations. The mock spectra are produced from the IllustrisTNG TNG100 simulation combined with stellar population models and take into account dust attenuation and realistic observational effects (aperture effects and noise). We compare the simulated $D_n4000$ and EW(H$未$) of galaxies with $10.5 \leq \log(M_\ast/M_\odot) \leq 11.5$ at $0.6 \leq z \leq 1.0$ to the observed distributions from the LEGA-C survey. TNG100 globally reproduces the observed distributions of spectral indices, implying that the age distribution of galaxies in TNG100 is generally realistic. Yet there are small but significant differences. For old galaxies, TNG100 shows small $D_n4000$ when compared to LEGA-C, while LEGA-C galaxies have larger EW(H$未$) at fixed $D_n4000$. There are several possible explanations: 1) LEGA-C galaxies have overall older ages combined with small contributions (a few percent in mass) from younger ($<1$~Gyr) stars, while TNG100 galaxies may not have such young sub-populations; 2) the spectral mismatch could be due to systematic uncertainties in the stellar population models used to convert stellar ages and metallicities to observables. In conclusion, the latest cosmological galaxy formation simulations broadly reproduce the global age distribution of galaxies at $z\sim1$ and, at the same time, the high quality of the latest observed and simulated datasets help constrain stellar population synthesis models as well as the physical models underlying the simulations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.10455v2-abstract-full').style.display = 'none'; document.getElementById('2108.10455v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 12 figures, accepted by AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2108.08142">arXiv:2108.08142</a> <span> [<a href="https://arxiv.org/pdf/2108.08142">pdf</a>, <a href="https://arxiv.org/format/2108.08142">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac1f29">10.3847/1538-4357/ac1f29 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Stellar Dynamical Models for 797 $z\sim 0.8$ Galaxies from LEGA-C </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=van+Houdt%2C+J">Josha van Houdt</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Wel%2C+A">Arjen van der Wel</a>, <a href="/search/astro-ph?searchtype=author&query=Bezanson%2C+R">Rachel Bezanson</a>, <a href="/search/astro-ph?searchtype=author&query=Franx%2C+M">Marijn Franx</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Eugenio%2C+F">Francesco D'Eugenio</a>, <a href="/search/astro-ph?searchtype=author&query=Barisic%2C+I">Ivana Barisic</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+E+F">Eric F. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">Anna Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=de+Graaff%2C+A">Anna de Graaff</a>, <a href="/search/astro-ph?searchtype=author&query=Maseda%2C+M+V">Michael V. Maseda</a>, <a href="/search/astro-ph?searchtype=author&query=Pacifici%2C+C">Camilla Pacifici</a>, <a href="/search/astro-ph?searchtype=author&query=van+de+Sande%2C+J">Jesse van de Sande</a>, <a href="/search/astro-ph?searchtype=author&query=Sobral%2C+D">David Sobral</a>, <a href="/search/astro-ph?searchtype=author&query=Straatman%2C+C">Caroline Straatman</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+P">Po-Feng Wu</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2108.08142v1-abstract-short" style="display: inline;"> We present spatially resolved stellar kinematics for 797 $z=0.6-1$ galaxies selected from the LEGA-C survey and construct axisymmetric Jeans models to quantify their dynamical mass and degree of rotational support. The survey is $K_s$-band selected, irrespective of color or morphological type, and allows for a first assessment of the stellar dynamical structure of the general $L^*$ galaxy populati… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.08142v1-abstract-full').style.display = 'inline'; document.getElementById('2108.08142v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.08142v1-abstract-full" style="display: none;"> We present spatially resolved stellar kinematics for 797 $z=0.6-1$ galaxies selected from the LEGA-C survey and construct axisymmetric Jeans models to quantify their dynamical mass and degree of rotational support. The survey is $K_s$-band selected, irrespective of color or morphological type, and allows for a first assessment of the stellar dynamical structure of the general $L^*$ galaxy population at large lookback time. Using light profiles from Hubble Space Telescope imaging as a tracer, our approach corrects for observational effects (seeing convolution and slit geometry), and uses well-informed priors on inclination, anisotropy and a non-luminous mass component. Tabulated data include total mass estimates in a series of spherical apertures (1, 5, and 10 kpc; 1$\times$ and 2$\times$\re), as well as rotational velocities, velocity dispersions and anisotropy. We show that almost all star-forming galaxies and $\sim$50\% of quiescent galaxies are rotation-dominated, with deprojected $V/蟽\sim1-2$. Revealing the complexity in galaxy evolution, we find that the most massive star-forming galaxies are among the most rotation-dominated, and the most massive quiescent galaxies among the least rotation-dominated galaxies. These measurements set a new benchmark for studying galaxy evolution, using stellar dynamical structure for galaxies at large lookback time. Together with the additional information on stellar population properties from the LEGA-C spectra, the dynamical mass and $V/蟽$ measurements presented here create new avenues for studying galaxy evolution at large lookback time. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.08142v1-abstract-full').style.display = 'none'; document.getElementById('2108.08142v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApJ. Data table will be published with journal article and is now available upon request</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2108.00744">arXiv:2108.00744</a> <span> [<a href="https://arxiv.org/pdf/2108.00744">pdf</a>, <a href="https://arxiv.org/format/2108.00744">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4365/ac1356">10.3847/1538-4365/ac1356 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Large Early Galaxy Astrophysics Census (LEGA-C) Data Release 3: 3000 High-Quality Spectra of $K_s$-selected galaxies at $z>0.6$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=van+der+Wel%2C+A">Arjen van der Wel</a>, <a href="/search/astro-ph?searchtype=author&query=Bezanson%2C+R">Rachel Bezanson</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Eugenio%2C+F">Francesco D'Eugenio</a>, <a href="/search/astro-ph?searchtype=author&query=Straatman%2C+C">Caroline Straatman</a>, <a href="/search/astro-ph?searchtype=author&query=Franx%2C+M">Marijn Franx</a>, <a href="/search/astro-ph?searchtype=author&query=van+Houdt%2C+J">Josha van Houdt</a>, <a href="/search/astro-ph?searchtype=author&query=Maseda%2C+M+V">Michael V. Maseda</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">Anna Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+P">Po-Feng Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Pacifici%2C+C">Camilla Pacifici</a>, <a href="/search/astro-ph?searchtype=author&query=Barisic%2C+I">Ivana Barisic</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=Munoz-Mateos%2C+J+C">Juan Carlos Munoz-Mateos</a>, <a href="/search/astro-ph?searchtype=author&query=Vervalcke%2C+S">Sarah Vervalcke</a>, <a href="/search/astro-ph?searchtype=author&query=Zibetti%2C+S">Stefano Zibetti</a>, <a href="/search/astro-ph?searchtype=author&query=Sobral%2C+D">David Sobral</a>, <a href="/search/astro-ph?searchtype=author&query=de+Graaff%2C+A">Anna de Graaff</a>, <a href="/search/astro-ph?searchtype=author&query=Calhau%2C+J">Joao Calhau</a>, <a href="/search/astro-ph?searchtype=author&query=Kaushal%2C+Y">Yasha Kaushal</a>, <a href="/search/astro-ph?searchtype=author&query=Muzzin%2C+A">Adam Muzzin</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+E+F">Eric F. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=van+Dokkum%2C+P+G">Pieter G. van Dokkum</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2108.00744v1-abstract-short" style="display: inline;"> We present the third and final data release of the Large Early Galaxy Astrophysics Census (LEGA-C), an ESO/VLT public spectroscopic survey targeting $0.6 < z < 1.0$, Ks-selected galaxies. The data release contains 3528 spectra with measured stellar velocity dispersions and stellar population properties, a 25-fold increase in sample size compared to previous work. This $K_s$-selected sample probes… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.00744v1-abstract-full').style.display = 'inline'; document.getElementById('2108.00744v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.00744v1-abstract-full" style="display: none;"> We present the third and final data release of the Large Early Galaxy Astrophysics Census (LEGA-C), an ESO/VLT public spectroscopic survey targeting $0.6 < z < 1.0$, Ks-selected galaxies. The data release contains 3528 spectra with measured stellar velocity dispersions and stellar population properties, a 25-fold increase in sample size compared to previous work. This $K_s$-selected sample probes the galaxy population down to $\sim0.3 L^*$, for all colors and morphological types. Along with the spectra we publish a value-added catalog with stellar and ionized gas velocity dispersions, stellar absorption line indices, emission line fluxes and equivalent widths, complemented with structural parameters measured from HST/ACS imaging. With its combination of high precision and large sample size, LEGA-C provides a new benchmark for galaxy evolution studies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.00744v1-abstract-full').style.display = 'none'; document.getElementById('2108.00744v1-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 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApJS. Data available at http://archive.eso.org/cms/eso-archive-news/Third-and-final-release-of-the-Large-Early-Galaxy-Census-LEGA-C-Spectroscopic-Public-Survey-published.html or https://users.ugent.be/\string~avdrwel/research.html\#legac</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.01054">arXiv:2107.01054</a> <span> [<a href="https://arxiv.org/pdf/2107.01054">pdf</a>, <a href="https://arxiv.org/format/2107.01054">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/stac705">10.1093/mnras/stac705 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The LEGA-C and SAMI Galaxy Surveys: Quiescent Stellar Populations and the Mass-Size Plane across 6 Gyr </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Barone%2C+T+M">Tania M. Barone</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Eugenio%2C+F">Francesco D'Eugenio</a>, <a href="/search/astro-ph?searchtype=author&query=Scott%2C+N">Nicholas Scott</a>, <a href="/search/astro-ph?searchtype=author&query=Colless%2C+M">Matthew Colless</a>, <a href="/search/astro-ph?searchtype=author&query=Vaughan%2C+S+P">Sam P. Vaughan</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Wel%2C+A">Arjen van der Wel</a>, <a href="/search/astro-ph?searchtype=author&query=Fraser-McKelvie%2C+A">Amelia Fraser-McKelvie</a>, <a href="/search/astro-ph?searchtype=author&query=de+Graaff%2C+A">Anna de Graaff</a>, <a href="/search/astro-ph?searchtype=author&query=van+de+Sande%2C+J">Jesse van de Sande</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+P">Po-Feng Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Bezanson%2C+R">Rachel Bezanson</a>, <a href="/search/astro-ph?searchtype=author&query=Brough%2C+S">Sarah Brough</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+E">Eric Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Croom%2C+S+M">Scott M. Croom</a>, <a href="/search/astro-ph?searchtype=author&query=Cortese%2C+L">Luca Cortese</a>, <a href="/search/astro-ph?searchtype=author&query=Driver%2C+S">Simon Driver</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A+R">Anna R. Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Muzzin%2C+A">Adam Muzzin</a>, <a href="/search/astro-ph?searchtype=author&query=Sobral%2C+D">David Sobral</a>, <a href="/search/astro-ph?searchtype=author&query=Bland-Hawthorn%2C+J">Joss Bland-Hawthorn</a>, <a href="/search/astro-ph?searchtype=author&query=Bryant%2C+J+J">Julia J. Bryant</a>, <a href="/search/astro-ph?searchtype=author&query=Goodwin%2C+M">Michael Goodwin</a>, <a href="/search/astro-ph?searchtype=author&query=Lawrence%2C+J+S">Jon S. Lawrence</a>, <a href="/search/astro-ph?searchtype=author&query=Lorente%2C+N+P+F">Nuria P. F. Lorente</a>, <a href="/search/astro-ph?searchtype=author&query=Owers%2C+M+S">Matt S. Owers</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="2107.01054v2-abstract-short" style="display: inline;"> We investigate the change in mean stellar population age and metallicity ([Z/H]) scaling relations for quiescent galaxies from intermediate redshift ($0.60\leq z\leq0.76$) using the LEGA-C Survey, to low redshift ($0.014\leq z\leq0.10$) using the SAMI Galaxy Survey. We find that, similarly to their low-redshift counterparts, the stellar metallicity of quiescent galaxies at $0.60\leq z\leq 0.76$ cl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.01054v2-abstract-full').style.display = 'inline'; document.getElementById('2107.01054v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.01054v2-abstract-full" style="display: none;"> We investigate the change in mean stellar population age and metallicity ([Z/H]) scaling relations for quiescent galaxies from intermediate redshift ($0.60\leq z\leq0.76$) using the LEGA-C Survey, to low redshift ($0.014\leq z\leq0.10$) using the SAMI Galaxy Survey. We find that, similarly to their low-redshift counterparts, the stellar metallicity of quiescent galaxies at $0.60\leq z\leq 0.76$ closely correlates with $M_*/R_\mathrm{e}$ (a proxy for the gravitational potential or escape velocity), in that galaxies with deeper potential wells are more metal-rich. This supports the hypothesis that the relation arises due to the gravitational potential regulating the retention of metals, by determining the escape velocity required by metal-rich stellar and supernova ejecta to escape the system and avoid being recycled into later stellar generations. On the other hand, we find no correlation between stellar age and $M_*/R_\mathrm{e}^2$ (stellar mass surface density $危$) in the LEGA-C sample, despite this being a strong relation at low redshift. We consider this change in the age--$危$ relation in the context of the redshift evolution of the star-forming and quiescent populations in the mass--size plane, and find our results can be explained as a consequence of galaxies forming more compactly at higher redshifts, and remaining compact throughout their evolution. Furthermore, galaxies appear to quench at a characteristic surface density that decreases with decreasing redshift. The $z\sim 0$ age--$危$ relation is therefore a result of building up the quiescent and star-forming populations with galaxies that formed at a range of redshifts and so a range of surface densities. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.01054v2-abstract-full').style.display = 'none'; document.getElementById('2107.01054v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 11 figures, accepted 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/2106.08338">arXiv:2106.08338</a> <span> [<a href="https://arxiv.org/pdf/2106.08338">pdf</a>, <a href="https://arxiv.org/format/2106.08338">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac0ae3">10.3847/1538-4357/ac0ae3 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An exquisitely deep view of quenching galaxies through the gravitational lens: Stellar population, morphology, and ionized gas </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Man%2C+A+W+S">Allison W. S. Man</a>, <a href="/search/astro-ph?searchtype=author&query=Zabl%2C+J">Johannes Zabl</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=Richard%2C+J">Johan Richard</a>, <a href="/search/astro-ph?searchtype=author&query=Toft%2C+S">Sune Toft</a>, <a href="/search/astro-ph?searchtype=author&query=Stockmann%2C+M">Mikkel Stockmann</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A+R">Anna R. Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Zibetti%2C+S">Stefano Zibetti</a>, <a href="/search/astro-ph?searchtype=author&query=Ebeling%2C+H">Harald Ebeling</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2106.08338v1-abstract-short" style="display: inline;"> This work presents an in-depth analysis of four gravitationally lensed red galaxies at z = 1.6-3.2. The sources are magnified by factors of 2.7-30 by foreground clusters, enabling spectral and morphological measurements that are otherwise challenging. Our sample extends below the characteristic mass of the stellar mass function and is thus more representative of the quiescent galaxy population at… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.08338v1-abstract-full').style.display = 'inline'; document.getElementById('2106.08338v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.08338v1-abstract-full" style="display: none;"> This work presents an in-depth analysis of four gravitationally lensed red galaxies at z = 1.6-3.2. The sources are magnified by factors of 2.7-30 by foreground clusters, enabling spectral and morphological measurements that are otherwise challenging. Our sample extends below the characteristic mass of the stellar mass function and is thus more representative of the quiescent galaxy population at z > 1 than previous spectroscopic studies. We analyze deep VLT/X-SHOOTER spectra and multi-band Hubble Space Telescope photometry that cover the rest-frame UV-to-optical regime. The entire sample resembles stellar disks as inferred from lensing-reconstructed images. Through stellar population synthesis analysis we infer that the targets are young (median age = 0.1-1.2 Gyr) and formed 80% of their stellar masses within 0.07-0.47 Gyr. Mg II $位位2796,2803$ absorption is detected across the sample. Blue-shifted absorption and/or redshifted emission of Mg II is found in the two youngest sources, indicative of a galactic-scale outflow of warm ($T\sim10^{4}$ K) gas. The [O III] $\lambda5007$ luminosity is higher for the two young sources (median age less than 0.4 Gyr) than the two older ones, perhaps suggesting a decline in nuclear activity as quenching proceeds. Despite high-velocity ($v\approx1500$ km s$^{-1}$) galactic-scale outflows seen in the most recently quenched galaxies, warm gas is still present to some extent long after quenching. Altogether our results indicate that star formation quenching at high redshift must have been a rapid process (< 1 Gyr) that does not synchronize with bulge formation or complete gas removal. Substantial bulge growth is required if they are to evolve into the metal-rich cores of present-day slow-rotators. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.08338v1-abstract-full').style.display = 'none'; document.getElementById('2106.08338v1-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 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in the Astrophysical Journal. 37 pages, 20 figures, 10 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.13368">arXiv:2105.13368</a> <span> [<a href="https://arxiv.org/pdf/2105.13368">pdf</a>, <a href="https://arxiv.org/format/2105.13368">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/stab1562">10.1093/mnras/stab1562 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Imprint of Cosmic Web Quenching on Central Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Winkel%2C+N">Nico Winkel</a>, <a href="/search/astro-ph?searchtype=author&query=Pasquali%2C+A">Anna Pasquali</a>, <a href="/search/astro-ph?searchtype=author&query=Kraljic%2C+K">Katarina Kraljic</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+R">Rory Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A+R">Anna R. Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Jackson%2C+T+M">Thomas M. Jackson</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2105.13368v1-abstract-short" style="display: inline;"> We investigate how cosmic web environment impacts the average properties of central galaxies in the Sloan Digital Sky Survey (SDSS). We analyse how the average specific star-formation rate, stellar age, metallicity and element abundance ratio [$伪$/Fe] of SDSS central galaxies depend on distance from the cosmic web nodes, walls and filaments identified by DisPerSE. In our approach we control for ga… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.13368v1-abstract-full').style.display = 'inline'; document.getElementById('2105.13368v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.13368v1-abstract-full" style="display: none;"> We investigate how cosmic web environment impacts the average properties of central galaxies in the Sloan Digital Sky Survey (SDSS). We analyse how the average specific star-formation rate, stellar age, metallicity and element abundance ratio [$伪$/Fe] of SDSS central galaxies depend on distance from the cosmic web nodes, walls and filaments identified by DisPerSE. In our approach we control for galaxy stellar mass and local density differentiated between field and group environment. Our results confirm the known trend whereby galaxies exhibit lower specific star-formation rates with decreasing distance to the cosmic web features. Furthermore, we show that centrals closer to either nodes, walls or filaments are on average older, metal richer and $伪$-enhanced compared to their equal mass counterparts at larger distances. The identified property gradients appear to have the same amplitude for central galaxies in the field as for those in groups. Our findings support a cosmic web quenching that stems from nurture effects, such as ram pressure stripping and strangulation, and/or nature effects linked to the intrinsic properties of the cosmic web. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.13368v1-abstract-full').style.display = 'none'; document.getElementById('2105.13368v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 7 figures, 4 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/2104.08295">arXiv:2104.08295</a> <span> [<a href="https://arxiv.org/pdf/2104.08295">pdf</a>, <a href="https://arxiv.org/ps/2104.08295">ps</a>, <a href="https://arxiv.org/format/2104.08295">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/10.1093/mnras/stab1213">10.1093/mnras/stab1213 <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 mass-metallicity relations from the VANDELS survey and the GAEA Semi-Analytic model </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Fontanot%2C+F">Fabio Fontanot</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=Talia%2C+M">Margherita Talia</a>, <a href="/search/astro-ph?searchtype=author&query=Mannucci%2C+F">Filippo Mannucci</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">Marco Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Cresci%2C+G">Giovanni Cresci</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=Gallazzi%2C+A">Anna Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">Michaela Hirschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">Laura Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Xie%2C+L">Lizhi Xie</a>, <a href="/search/astro-ph?searchtype=author&query=Amorin%2C+R">Ricardo Amorin</a>, <a href="/search/astro-ph?searchtype=author&query=Bolzonella%2C+M">Micol Bolzonella</a>, <a href="/search/astro-ph?searchtype=author&query=Bongiorno%2C+A">Angela Bongiorno</a>, <a href="/search/astro-ph?searchtype=author&query=Cucciati%2C+O">Olga Cucciati</a>, <a href="/search/astro-ph?searchtype=author&query=Cullen%2C+F">Fergus Cullen</a>, <a href="/search/astro-ph?searchtype=author&query=Fynbo%2C+J+P+U">Johan P. U. Fynbo</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N">Nimish Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Hibon%2C+P">Pascale Hibon</a>, <a href="/search/astro-ph?searchtype=author&query=McLure%2C+R+J">Ross J. McLure</a>, <a href="/search/astro-ph?searchtype=author&query=Pozzetti%2C+L">Lucia Pozzetti</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2104.08295v2-abstract-short" style="display: inline;"> In this work, we study the evolution of the mass-metallicity relations (MZRs) as predicted by the GAlaxy Evolution and Assembly (GAEA) semi-analytic model. We contrast these predictions with recent results from the VANDELS survey, that allows us to expand the accessible redshift range for the stellar MZR up to $z\sim3.5$. We complement our study by considering the evolution of the gas-phase MZR in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.08295v2-abstract-full').style.display = 'inline'; document.getElementById('2104.08295v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2104.08295v2-abstract-full" style="display: none;"> In this work, we study the evolution of the mass-metallicity relations (MZRs) as predicted by the GAlaxy Evolution and Assembly (GAEA) semi-analytic model. We contrast these predictions with recent results from the VANDELS survey, that allows us to expand the accessible redshift range for the stellar MZR up to $z\sim3.5$. We complement our study by considering the evolution of the gas-phase MZR in the same redshift range. We show that GAEA is able to reproduce the observed evolution of the $z<3.5$ gas-phase MZR and $z<0.7$ stellar MZR, while it overpredicts the stellar metallicity at $z\sim3.5$. Furthermore, GAEA also reproduces the so-called fundamental metallicity relation (FMR) between gas-phase metallicity, stellar mass and star formation rate (SFR). In particular, the gas-phase FMR in GAEA is already in place at $z\sim5$ and shows almost no evolution at lower redshift. GAEA predicts the existence of a stellar FMR, that is, however, characterized by a relevant redshift evolution, although its shape follows closely the gas-phase FMR. We also report additional unsolved tensions between model and data: the overall normalization of the predicted MZR agrees with observations only within $\sim$0.1 dex; the largest discrepancies are seen at $z\sim3.5$ where models tend to slightly overpredict observed metallicities; the slope of the predicted MZR at fixed SFR is too steep below a few ${\rm M}_\odot\ {\rm yr}^{-1}$. Finally, we provide model predictions for the evolution of the MZRs at higher redshifts, that would be useful in the context of future surveys, like those that will be performed with JWST. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.08295v2-abstract-full').style.display = 'none'; document.getElementById('2104.08295v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 8 figures, MNRAS accepted, replaced to match the published version</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2103.12086">arXiv:2103.12086</a> <span> [<a href="https://arxiv.org/pdf/2103.12086">pdf</a>, <a href="https://arxiv.org/format/2103.12086">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/10.1051/0004-6361/202140856">10.1051/0004-6361/202140856 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> INSPIRE: INvestigating Stellar Population In RElics II. First Data Release (DR1) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Spiniello%2C+C">C. Spiniello</a>, <a href="/search/astro-ph?searchtype=author&query=Tortora%2C+C">C. Tortora</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Ago%2C+G">G. D'Ago</a>, <a href="/search/astro-ph?searchtype=author&query=Coccato%2C+L">L. Coccato</a>, <a href="/search/astro-ph?searchtype=author&query=La+Barbera%2C+F">F. La Barbera</a>, <a href="/search/astro-ph?searchtype=author&query=Ferr%C3%A9-Mateu%2C+A">A. Ferr茅-Mateu</a>, <a href="/search/astro-ph?searchtype=author&query=Pulsoni%2C+C">C. Pulsoni</a>, <a href="/search/astro-ph?searchtype=author&query=Arnaboldi%2C+M">M. Arnaboldi</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">A. Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Hunt%2C+L">L. Hunt</a>, <a href="/search/astro-ph?searchtype=author&query=Napolitano%2C+N+R">N. R. Napolitano</a>, <a href="/search/astro-ph?searchtype=author&query=Radovich%2C+M">M. Radovich</a>, <a href="/search/astro-ph?searchtype=author&query=Scognamiglio%2C+D">D. Scognamiglio</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">M. Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Zibetti%2C+S">S. Zibetti</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2103.12086v2-abstract-short" style="display: inline;"> The INvestigating Stellar Population In RElics is an on-going project targeting 52 ultra-compact massive galaxies at 0.1<z<0.5 with the X-Shooter@VLT spectrograph (XSH). These objects are the perfect candidates to be 'relics', massive red-nuggets formed at high-z (z>2) through a short and intense star formation burst, that evolved passively and undisturbed until the present-day. Relics provide a u… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.12086v2-abstract-full').style.display = 'inline'; document.getElementById('2103.12086v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.12086v2-abstract-full" style="display: none;"> The INvestigating Stellar Population In RElics is an on-going project targeting 52 ultra-compact massive galaxies at 0.1<z<0.5 with the X-Shooter@VLT spectrograph (XSH). These objects are the perfect candidates to be 'relics', massive red-nuggets formed at high-z (z>2) through a short and intense star formation burst, that evolved passively and undisturbed until the present-day. Relics provide a unique opportunity to study the mechanisms of star formation at high-z. In this paper, we present the first INSPIRE Data Release, comprising 19 systems with observations completed in 2020. We use the methods already presented in the INSPIRE Pilot, but revisiting the 1D spectral extraction. For these 19 systems, we obtain an estimate of the stellar velocity dispersion, fitting separately the two UVB and VIS XSH arms at their original resolution. We estimate [Mg/Fe] abundances via line-index strength and mass-weighted integrated stellar ages and metallicities with full spectral fitting on the combined spectrum. Ages are generally old, in agreement with the photometric ones, and metallicities are almost always super-solar, confirming the mass-metallicity relation. The [Mg/Fe] ratio is also larger than solar for the great majority of the galaxies, as expected. We find that 10 objects have formed more than 75% of their stellar mass (M*) within 3 Gyr from the Big Bang and classify them as relics. Among these, we identify 4 galaxies which had already fully assembled their M* by that time. They are therefore `extreme relics' of the ancient Universe. The INSPIRE DR1 catalogue of 10 known relics to-date augment by a factor of 3.3 the total number of confirmed relics, also enlarging the redshift window. It is therefore the largest publicly available collection. Thanks to the larger number of systems, we can also better quantify the existence of a 'degree of relicness', already hinted at the Pilot Paper. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.12086v2-abstract-full').style.display = 'none'; document.getElementById('2103.12086v2-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 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">(Abstract abridged) 21 pages, 12 figures and 5 tables in the main body, plus 3 figure and 1 table in the appendix, accepted for publication on A&A. The associated data are available via the ESO Phase 3 Science Portal</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 654, A136 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.05935">arXiv:2012.05935</a> <span> [<a href="https://arxiv.org/pdf/2012.05935">pdf</a>, <a href="https://arxiv.org/format/2012.05935">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/abce66">10.3847/1538-4357/abce66 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Fundamental Plane of Massive Quiescent Galaxies at z~2 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Stockmann%2C+M">Mikkel Stockmann</a>, <a href="/search/astro-ph?searchtype=author&query=J%C3%B8rgensen%2C+I">Inger J酶rgensen</a>, <a href="/search/astro-ph?searchtype=author&query=Toft%2C+S">Sune Toft</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C+J">Christopher J. Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=Faisst%2C+A">Andreas Faisst</a>, <a href="/search/astro-ph?searchtype=author&query=Margalef-Bentabol%2C+B">Berta Margalef-Bentabol</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">Anna Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Zibetti%2C+S">Stefano Zibetti</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=G%C3%B3mez-Guijarro%2C+C">Carlos G贸mez-Guijarro</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">Michaela Hirschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Lagos%2C+C+D">Claudia D. Lagos</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=Zabl%2C+J">Johannes Zabl</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="2012.05935v1-abstract-short" style="display: inline;"> We examine the Fundamental Plane (FP) and mass-to-light ratio ($M/L$) scaling relations using the largest sample of massive quiescent galaxies at $1.5<z<2.5$ to date. The FP ($r_{e}, 蟽_{e}, I_{e}$) is established using $19$ $UVJ$ quiescent galaxies from COSMOS with $Hubble$ $Space$ $Telescope$ $(HST)$ $H_{F160W}$ rest-frame optical sizes and X-shooter absorption line measured stellar velocity disp… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.05935v1-abstract-full').style.display = 'inline'; document.getElementById('2012.05935v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.05935v1-abstract-full" style="display: none;"> We examine the Fundamental Plane (FP) and mass-to-light ratio ($M/L$) scaling relations using the largest sample of massive quiescent galaxies at $1.5<z<2.5$ to date. The FP ($r_{e}, 蟽_{e}, I_{e}$) is established using $19$ $UVJ$ quiescent galaxies from COSMOS with $Hubble$ $Space$ $Telescope$ $(HST)$ $H_{F160W}$ rest-frame optical sizes and X-shooter absorption line measured stellar velocity dispersions. For a very massive, ${\rm{log}}(M_{\ast}/M_{\odot})>11.26$, subset of 8 quiescent galaxies at $z>2$, from Stockmann et al. (2020), we show that they cannot passively evolve to the local Coma cluster relation alone and must undergo significant structural evolution to mimic the sizes of local massive galaxies. The evolution of the FP and $M/L$ scaling relations, from $z=2$ to present-day, for this subset are consistent with passive aging of the stellar population and minor merger structural evolution into the most massive galaxies in the Coma cluster and other massive elliptical galaxies from the MASSIVE Survey. Modeling the luminosity evolution from minor merger added stellar populations favors a history of merging with "dry" quiescent galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.05935v1-abstract-full').style.display = 'none'; document.getElementById('2012.05935v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 December, 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">17 pages, 6 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2011.05347">arXiv:2011.05347</a> <span> [<a href="https://arxiv.org/pdf/2011.05347">pdf</a>, <a href="https://arxiv.org/format/2011.05347">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/10.1051/0004-6361/202038936">10.1051/0004-6361/202038936 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> INSPIRE: INvestigating Stellar Population In RElics -- I. Survey presentation and pilot program </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Spiniello%2C+C">C. Spiniello</a>, <a href="/search/astro-ph?searchtype=author&query=Tortora%2C+C">C. Tortora</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Ago%2C+G">G. D'Ago</a>, <a href="/search/astro-ph?searchtype=author&query=Coccato%2C+L">L. Coccato</a>, <a href="/search/astro-ph?searchtype=author&query=La+Barbera%2C+F">F. La Barbera</a>, <a href="/search/astro-ph?searchtype=author&query=Ferr%C3%A9-Mateu%2C+A">A. Ferr茅-Mateu</a>, <a href="/search/astro-ph?searchtype=author&query=Napolitano%2C+N+R">N. R. Napolitano</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">M. Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Scognamiglio%2C+D">D. Scognamiglio</a>, <a href="/search/astro-ph?searchtype=author&query=Arnaboldi%2C+M">M. Arnaboldi</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">A. Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Hunt%2C+L">L. Hunt</a>, <a href="/search/astro-ph?searchtype=author&query=Moehler%2C+S">S. Moehler</a>, <a href="/search/astro-ph?searchtype=author&query=Radovich%2C+M">M. Radovich</a>, <a href="/search/astro-ph?searchtype=author&query=Zibetti%2C+S">S. Zibetti</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2011.05347v2-abstract-short" style="display: inline;"> Massive ETGs are thought to form through a two-phase process. At early times, an intense and fast starburst forms blue and disk-dominated galaxies. After quenching, the remaining structures become red, compact and massive, i.e., 'red nuggets'. Then, a time-extended second phase which is dominated by mergers, causes structural evolution and size growth. Given the stochastic nature of mergers, a sma… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.05347v2-abstract-full').style.display = 'inline'; document.getElementById('2011.05347v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.05347v2-abstract-full" style="display: none;"> Massive ETGs are thought to form through a two-phase process. At early times, an intense and fast starburst forms blue and disk-dominated galaxies. After quenching, the remaining structures become red, compact and massive, i.e., 'red nuggets'. Then, a time-extended second phase which is dominated by mergers, causes structural evolution and size growth. Given the stochastic nature of mergers, a small fraction of red nuggets survives, without any interaction, massive and compact until today: relic galaxies. Since this fraction depends on the processes dominating the size growth, counting relics at low-z is a valuable way to disentangle between different galaxy evolution models. In this paper, we introduce the INvestigating Stellar Population In RElics (INSPIRE) Project, that aims at spectroscopically confirming and fully characterizing a large number of relics at 0.1<z<0.5. We focus here on the first results based on a pilot program targeting three systems, representative of the whole sample. For these, we extract 1D optical spectra over an aperture comprising ~30 % of the galaxies light, and obtain line-of-sight integrated stellar velocity and velocity dispersion. We also infer the stellar [$伪$/Fe] abundance from line-index measurements and mass-weighted age and metallicity from full-spectral fitting with single stellar population models. Two galaxies have large integrated stellar velocity dispersion values, confirming their massive nature. They are populated by stars with super-solar metallicity and [$伪$/Fe]. Both objects have formed >80 % of their stellar mass within a short (0.5 - 1.0 Gyrs) initial star formation episode occurred only ~1 Gyr after the Big Bang. The third galaxy has a more extended star formation history and a lower velocity dispersion. Thus we confirm two out of three candidates as relics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.05347v2-abstract-full').style.display = 'none'; document.getElementById('2011.05347v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 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">19 pages, 14 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 646, A28 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2010.04733">arXiv:2010.04733</a> <span> [<a href="https://arxiv.org/pdf/2010.04733">pdf</a>, <a href="https://arxiv.org/format/2010.04733">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/10.1093/mnras/stab265">10.1093/mnras/stab265 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galaxy evolution across environments as probed by the ages, stellar metallicities and [alpha/Fe] of central and satellite galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A+R">Anna R. Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Pasquali%2C+A">Anna Pasquali</a>, <a href="/search/astro-ph?searchtype=author&query=Zibetti%2C+S">Stefano Zibetti</a>, <a href="/search/astro-ph?searchtype=author&query=La+Barbera%2C+F">Francesco La Barbera</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2010.04733v2-abstract-short" style="display: inline;"> We explore how the star formation and metal enrichment histories of present-day galaxies have been affected by environment combining stellar population parameter estimates and group environment characterization for SDSS DR7. We compare stellar ages, stellar metallicities and element abundance ratios [alpha/Fe] of satellite and central galaxies, as a function of their stellar and host group halo ma… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.04733v2-abstract-full').style.display = 'inline'; document.getElementById('2010.04733v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.04733v2-abstract-full" style="display: none;"> We explore how the star formation and metal enrichment histories of present-day galaxies have been affected by environment combining stellar population parameter estimates and group environment characterization for SDSS DR7. We compare stellar ages, stellar metallicities and element abundance ratios [alpha/Fe] of satellite and central galaxies, as a function of their stellar and host group halo mass, controlling for the current star formation rate and for the infall epoch. We confirm that below log(Mstar/Msun)=10.5 satellites are older and metal-richer than equally-massive central galaxies. On the contrary, we do not detect any difference in their [alpha/Fe]: this depends primarily on stellar mass and not on group hierarchy nor host halo mass. We also find that the differences in the median age and metallicity of satellites and centrals at stellar mass below 10^{10.5}Msun are largely due to the higher fraction of passive galaxies among satellites and as a function of halo mass. We argue that the observed trends at low masses reveal the action of satellite-specific environmental effects in a `delayed-then-rapid' fashion. When accounting for the varying quiescent fraction, small residual excess in age, metallicity and [alpha/Fe] emerge for satellites dominated by old stellar populations and residing in halos more massive than 10^{14}Msun, compared to equally-massive central galaxies. This excess in age, metallicity and [alpha/Fe] pertain to ancient infallers, i.e. satellites that have accreted onto the current halo more than 5 Gyr ago. This result points to the action of environment in the early phases of star formation in galaxies located close to cosmic density peaks. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.04733v2-abstract-full').style.display = 'none'; document.getElementById('2010.04733v2-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 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted for publication on MNRAS, minor revisions after referee report, 24 pages, 12 figures, 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/2007.00663">arXiv:2007.00663</a> <span> [<a href="https://arxiv.org/pdf/2007.00663">pdf</a>, <a href="https://arxiv.org/format/2007.00663">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/staa1937">10.1093/mnras/staa1937 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Inverse stellar population age gradients of post-starburst galaxies at z=0.8 with LEGA-C </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=D%27Eugenio%2C+F">Francesco D'Eugenio</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Wel%2C+A">Arjen van der Wel</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+P">Po-Feng Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Barone%2C+T+M">Tania M. Barone</a>, <a href="/search/astro-ph?searchtype=author&query=van+Houdt%2C+J">Josha van Houdt</a>, <a href="/search/astro-ph?searchtype=author&query=Bezanson%2C+R">Rachel Bezanson</a>, <a href="/search/astro-ph?searchtype=author&query=Straatman%2C+C+M+S">Caroline M. S. Straatman</a>, <a href="/search/astro-ph?searchtype=author&query=Pacifici%2C+C">Camilla Pacifici</a>, <a href="/search/astro-ph?searchtype=author&query=Muzzin%2C+A">Adam Muzzin</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">Anna Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Wild%2C+V">Vivienne Wild</a>, <a href="/search/astro-ph?searchtype=author&query=Sobral%2C+D">David Sobral</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+E+F">Eric F. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Zibetti%2C+S">Stefano Zibetti</a>, <a href="/search/astro-ph?searchtype=author&query=Mowla%2C+L">Lamiya Mowla</a>, <a href="/search/astro-ph?searchtype=author&query=Franx%2C+M">Marijn Franx</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2007.00663v1-abstract-short" style="display: inline;"> We use deep, spatially resolved spectroscopy from the LEGA-C Survey to study radial variations in the stellar population of 17 spectroscopically-selected post-starburst (PSB) galaxies. We use spectral fitting to measure two Lick indices, $H未_A$ and $Fe4383$, and find that, on average, PSB galaxies have radially decreasing $H未_A$ and increasing $Fe4383$ profiles. In contrast, a control sample of qu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.00663v1-abstract-full').style.display = 'inline'; document.getElementById('2007.00663v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.00663v1-abstract-full" style="display: none;"> We use deep, spatially resolved spectroscopy from the LEGA-C Survey to study radial variations in the stellar population of 17 spectroscopically-selected post-starburst (PSB) galaxies. We use spectral fitting to measure two Lick indices, $H未_A$ and $Fe4383$, and find that, on average, PSB galaxies have radially decreasing $H未_A$ and increasing $Fe4383$ profiles. In contrast, a control sample of quiescent, non-PSB galaxies in the same mass range shows outwardly increasing $H未_A$ and decreasing $Fe4383$. The observed gradients are weak ($\approx-0.2$ 脜/$R_e$), mainly due to seeing convolution. A two-SSP model suggests intrinsic gradients are as strong as observed in local PSB galaxies ($\approx -0.8$ 脜$/R_e$). We interpret these results in terms of inside-out growth (for the bulk of the quiescent population) vs star formation occurring last in the centre (for PSB galaxies). At $z\approx0.8$, central starbursts are often the result of gas-rich mergers, as evidenced by the high fraction of PSB galaxies with disturbed morphologies and tidal features (40%). Our results provide additional evidence for multiple paths to quiescence: a standard path, associated with inside-out disc formation and with gradually decreasing star-formation activity, without fundamental structural transformation, and a fast path, associated with centrally-concentrated starbursts, leaving an inverse age gradient and smaller half-light radius. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.00663v1-abstract-full').style.display = 'none'; document.getElementById('2007.00663v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 9 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2003.02347">arXiv:2003.02347</a> <span> [<a href="https://arxiv.org/pdf/2003.02347">pdf</a>, <a href="https://arxiv.org/format/2003.02347">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </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/10.1051/0004-6361/202037879">10.1051/0004-6361/202037879 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> On the connection between galactic downsizing and the most fundamental galactic scaling relations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Spitoni%2C+E">E. Spitoni</a>, <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">F. Calura</a>, <a href="/search/astro-ph?searchtype=author&query=Mignoli%2C+M">M. Mignoli</a>, <a href="/search/astro-ph?searchtype=author&query=Gilli%2C+R">R. Gilli</a>, <a href="/search/astro-ph?searchtype=author&query=Aguirre%2C+V+S">V. Silva Aguirre</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">A. Gallazzi</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="2003.02347v2-abstract-short" style="display: inline;"> In their evolution, star-forming galaxies are known to follow scaling relations between some fundamental physical quantities, such as the mass-metallicity and the main sequence relations. We aim at studying the evolution of galaxies that, at a given redshift, lie simultaneously on the mass-metallicity and main sequence relations (MZR, MSR). To this aim, we use the analytical, 'leaky-box' chemical… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.02347v2-abstract-full').style.display = 'inline'; document.getElementById('2003.02347v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2003.02347v2-abstract-full" style="display: none;"> In their evolution, star-forming galaxies are known to follow scaling relations between some fundamental physical quantities, such as the mass-metallicity and the main sequence relations. We aim at studying the evolution of galaxies that, at a given redshift, lie simultaneously on the mass-metallicity and main sequence relations (MZR, MSR). To this aim, we use the analytical, 'leaky-box' chemical evolution model of Spitoni et al. (2017), in which galaxy evolution is described by an infall timescale $蟿$ and a wind efficiency $位$. We provide a detailed analysis of the temporal evolution of galactic metallicity, stellar mass, mass-weighted age and gas fraction. The evolution of the galaxies lying on the MZR and MSR at $z\sim0.1$ suggests that the average infall time-scale in two different bins of stellar masses ($M_{\star}<10^{10} M_{\odot}$ and $M_{\star}>10^{10} M_{\odot}$) decreases with decreasing redshift. This means that at each redshift, only the youngest galaxies can be assembled on the shortest timescales and still belong to the star-forming MSR. In the lowest mass bin, a decrease of the median $蟿$ is accompanied by an increase of the median $位$ value. This implies that systems which have formed at more recent times will need to eject a larger amount of mass to keep their metallicity at low values. Another important result is that galactic downsizing, as traced by the age-mass relation, is naturally recovered by imposing that local galaxies lie on both the MZR and MSR. Finally, we study the evolution of the hosts of C$_{\rm IV}$ -selected AGN, which at $z\sim 2$ follow a flat MZR, as found by Mignoli et al. (2019). If we impose that these systems lie on the MSR, at lower redshifts we find an 'inverted' MZR, meaning that some additional processes must be at play in their evolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.02347v2-abstract-full').style.display = 'none'; document.getElementById('2003.02347v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 August, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 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">Accepted for publication in Astronomy and Astrophysics (A&A), 20 pages, 26 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 642, A113 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2001.02695">arXiv:2001.02695</a> <span> [<a href="https://arxiv.org/pdf/2001.02695">pdf</a>, <a href="https://arxiv.org/format/2001.02695">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/ab7241">10.3847/2041-8213/ab7241 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Stellar Kinematics and Environment at z~0.8 in the LEGA-C Survey: Massive, Slow-Rotators are Built First in Overdense Environments </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cole%2C+J">Justin Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Bezanson%2C+R">Rachel Bezanson</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Wel%2C+A">Arjen van der Wel</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+E">Eric Bell</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Eugenio%2C+F">Francesco D'Eugenio</a>, <a href="/search/astro-ph?searchtype=author&query=Franx%2C+M">Marijn Franx</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">Anna Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=van+Houdt%2C+J">Josha van Houdt</a>, <a href="/search/astro-ph?searchtype=author&query=Muzzin%2C+A">Adam Muzzin</a>, <a href="/search/astro-ph?searchtype=author&query=Pacifici%2C+C">Camilla Pacifici</a>, <a href="/search/astro-ph?searchtype=author&query=van+de+Sande%2C+J">Jesse van de Sande</a>, <a href="/search/astro-ph?searchtype=author&query=Sobral%2C+D">David Sobral</a>, <a href="/search/astro-ph?searchtype=author&query=Straatman%2C+C">Caroline Straatman</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+P">Po-Feng Wu</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2001.02695v1-abstract-short" style="display: inline;"> In this letter, we investigate the impact of environment on integrated and spatially-resolved stellar kinematics of a sample of massive, quiescent galaxies at intermediate redshift ($0.6<z<1.0$). For this analysis, we combine photometric and spectroscopic parameters from the UltraVISTA and Large Early Galaxy Astrophysics Census (LEGA-C) surveys in the COSMOS field and environmental measurements. W… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.02695v1-abstract-full').style.display = 'inline'; document.getElementById('2001.02695v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2001.02695v1-abstract-full" style="display: none;"> In this letter, we investigate the impact of environment on integrated and spatially-resolved stellar kinematics of a sample of massive, quiescent galaxies at intermediate redshift ($0.6<z<1.0$). For this analysis, we combine photometric and spectroscopic parameters from the UltraVISTA and Large Early Galaxy Astrophysics Census (LEGA-C) surveys in the COSMOS field and environmental measurements. We analyze the trends with overdensity (1+$未$) on the rotational support of quiescent galaxies and find no universal trends at either fixed mass or fixed stellar velocity dispersion. This is consistent with previous studies of the local Universe; rotational support of massive galaxies depends primarily on stellar mass. We highlight two populations of massive galaxies ($\log M_\star/M_\odot\geq11$) that deviate from the average mass relation. First, the most massive galaxies in the most under-dense regions ($(1+未)\leq1$) exhibit elevated rotational support. Similarly, at the highest masses ($\log M_\star/M_\odot\geq11.25$) the range in rotational support is significant in all but the densest regions. This corresponds to an increasing slow-rotator fraction such that only galaxies in the densest environments ($(1+未)\geq3.5$) are primarily (90$\pm$10\%) slow-rotators.This effect is not seen at fixed velocity dispersion, suggesting minor merging as the driving mechanism: only in the densest regions have the most massive galaxies experienced significant minor merging, building stellar mass and diminishing rotation without significantly affecting the central stellar velocity dispersion. In the local Universe, most massive galaxies are slow-rotators, regardless of environment, suggesting minor merging occurs at later cosmic times $(z\lesssim0.6)$ in all but the most dense environments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.02695v1-abstract-full').style.display = 'none'; document.getElementById('2001.02695v1-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 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">10 pages, 5 figures, submitted to 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/1912.06522">arXiv:1912.06522</a> <span> [<a href="https://arxiv.org/pdf/1912.06522">pdf</a>, <a href="https://arxiv.org/format/1912.06522">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/stz3556">10.1093/mnras/stz3556 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The frequency of very young galaxies in the local Universe: II. The view from SDSS spectra </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mamon%2C+G+A">Gary A. Mamon</a>, <a href="/search/astro-ph?searchtype=author&query=Trevisan%2C+M">Marina Trevisan</a>, <a href="/search/astro-ph?searchtype=author&query=Thuan%2C+T+X">Trinh X. Thuan</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">Anna Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Dav%C3%A9%2C+R">Romeel Dav茅</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="1912.06522v2-abstract-short" style="display: inline;"> Only a handful of galaxies in the local Universe appear to be very young. We estimate the fraction of very young galaxies (VYGs), defined as those with more than half their stellar masses formed within the last Gyr. We fit non-parametric star formation histories (SFHs) to ~280 000 galaxy spectra from a flux- and volume-limited subsample of the Main Galaxy Sample (MGS) of the SDSS, which is also co… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1912.06522v2-abstract-full').style.display = 'inline'; document.getElementById('1912.06522v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1912.06522v2-abstract-full" style="display: none;"> Only a handful of galaxies in the local Universe appear to be very young. We estimate the fraction of very young galaxies (VYGs), defined as those with more than half their stellar masses formed within the last Gyr. We fit non-parametric star formation histories (SFHs) to ~280 000 galaxy spectra from a flux- and volume-limited subsample of the Main Galaxy Sample (MGS) of the SDSS, which is also complete in mass-to-light ratio, thus properly accounting for passive galaxies of a given mass. The VYG fractions decrease with increasing galaxy stellar mass, from ~50% at $m = 10^8\,\rm M_\odot$ to ~0.1% at $m = 10^{11.5}\,\rm M_\odot$, with differences of up to 1 dex between the different spectral models used to estimate the SFH and on how we treat aperture effects. But old stellar populations may hide in our VYGs despite our conservative VYG sample built with galaxies that are globally bluer than within the region viewed by the SDSS fibre. The VYG fractions versus mass decrease more gradually compared to the Tweed et al. predictions using analytical and semi-analytical models of galaxy formation, but agree better with the SIMBA hydrodynamical simulation. These discrepancies highlight the usefulness of VYGs in constraining the strong uncertainties in both galaxy formation models and spectral modelling of galaxy SFHs. Given the lognormal cosmic SFH, these mean VYG fractions suggest that galaxies with $m > 10^8\,\rm M_\odot$ undergo at most 4 major starbursts on average. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1912.06522v2-abstract-full').style.display = 'none'; document.getElementById('1912.06522v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 March, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 December, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">Published version, consolidated with Erratum on caption of Table A1 (the table is for all 404 931 galaxies in the Clean sample, not just those that are candidate VYGs according to at least one spectral model). New is in green and omitted is in strikeout-red</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> MNRAS 492, 1791-1811 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1912.03683">arXiv:1912.03683</a> <span> [<a href="https://arxiv.org/pdf/1912.03683">pdf</a>, <a href="https://arxiv.org/format/1912.03683">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ab5fd9">10.3847/1538-4357/ab5fd9 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The colors and sizes of recently quenched galaxies: a result of compact starburst before quenching </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wu%2C+P">Po-Feng Wu</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Wel%2C+A">Arjen van der Wel</a>, <a href="/search/astro-ph?searchtype=author&query=Bezanson%2C+R">Rachel Bezanson</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">Anna Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Pacifici%2C+C">Camilla Pacifici</a>, <a href="/search/astro-ph?searchtype=author&query=Straatman%2C+C+M+S">Caroline M. S. Straatman</a>, <a href="/search/astro-ph?searchtype=author&query=Barisic%2C+I">Ivana Barisic</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+E+F">Eric F. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Chauke%2C+P">Priscilla Chauke</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Eugenio%2C+F">Francesco D'Eugenio</a>, <a href="/search/astro-ph?searchtype=author&query=Franx%2C+M">Marijn Franx</a>, <a href="/search/astro-ph?searchtype=author&query=Muzzin%2C+A">Adam Muzzin</a>, <a href="/search/astro-ph?searchtype=author&query=Sobral%2C+D">David Sobral</a>, <a href="/search/astro-ph?searchtype=author&query=van+Houdt%2C+J">Josha van Houdt</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="1912.03683v1-abstract-short" style="display: inline;"> We analyze the colors and sizes of 32 quiescent (UVJ-selected) galaxies with strong Balmer absorption ($\mbox{EW}(H未) \geq 4$脜) at $z\sim0.8$ drawn from DR2 of the LEGA-C survey to test the hypothesis that these galaxies experienced compact, central starbursts before quenching. These recently quenched galaxies, usually referred to as post-starburst galaxies, span a wide range of colors and we find… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1912.03683v1-abstract-full').style.display = 'inline'; document.getElementById('1912.03683v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1912.03683v1-abstract-full" style="display: none;"> We analyze the colors and sizes of 32 quiescent (UVJ-selected) galaxies with strong Balmer absorption ($\mbox{EW}(H未) \geq 4$脜) at $z\sim0.8$ drawn from DR2 of the LEGA-C survey to test the hypothesis that these galaxies experienced compact, central starbursts before quenching. These recently quenched galaxies, usually referred to as post-starburst galaxies, span a wide range of colors and we find a clear correlation between color and half-light radius, such that bluer galaxies are smaller. We build simple toy models to explain this correlation: a normal star-forming disk plus a central, compact starburst component. Bursts with exponential decay timescale of $\sim$~100 Myr that produce $\sim10\%$ to more than 100\% of the pre-existing masses can reproduce the observed correlation. More significant bursts also produce bluer and smaller descendants. Our findings imply that when galaxies shut down star formation rapidly, they generally had experienced compact, starburst events and that the large, observed spread in sizes and colors mostly reflects a variety of burst strengths. Recently quenched galaxies should have younger stellar ages in the centers; multi-wavelength data with high spatial resolution are required to reveal the age gradient. Highly dissipative processes should be responsible for this type of formation history. While determining the mechanisms for individual galaxies is challenging, some recently quenched galaxies show signs of gravitational interactions, suggesting that mergers are likely an important mechanism in triggering the rapid shut-down of star-formation activities at $z\sim0.8$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1912.03683v1-abstract-full').style.display = 'none'; document.getElementById('1912.03683v1-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 December, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">16 pages, 8 figures, 1 table, accepted by ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1912.01619">arXiv:1912.01619</a> <span> [<a href="https://arxiv.org/pdf/1912.01619">pdf</a>, <a href="https://arxiv.org/format/1912.01619">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ab5af4">10.3847/1538-4357/ab5af4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> X-shooter Spectroscopy and HST Imaging of 15 Ultra Massive Quiescent Galaxies at $z\gtrsim2$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Stockmann%2C+M">Mikkel Stockmann</a>, <a href="/search/astro-ph?searchtype=author&query=Toft%2C+S">Sune Toft</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">Anna Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Zibetti%2C+S">Stefano Zibetti</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C+J">Christopher J. Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=Margalef-Bentabol%2C+B">Berta Margalef-Bentabol</a>, <a href="/search/astro-ph?searchtype=author&query=Zabl%2C+J">Johannes Zabl</a>, <a href="/search/astro-ph?searchtype=author&query=J%C3%B8rgensen%2C+I">Inger J酶rgensen</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=G%C3%B3mez-Guijarro%2C+C">Carlos G贸mez-Guijarro</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=Brammer%2C+G+B">Gabriel B. Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Ceverino%2C+D">Daniel Ceverino</a>, <a href="/search/astro-ph?searchtype=author&query=Cortzen%2C+I">Isabella Cortzen</a>, <a href="/search/astro-ph?searchtype=author&query=Davidzon%2C+I">Iary Davidzon</a>, <a href="/search/astro-ph?searchtype=author&query=Demarco%2C+R">Richardo Demarco</a>, <a href="/search/astro-ph?searchtype=author&query=Faisst%2C+A">Andreas Faisst</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">Michaela Hirschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Krogager%2C+J">Jens-Kristian Krogager</a>, <a href="/search/astro-ph?searchtype=author&query=Lagos%2C+C+D">Claudia D. Lagos</a>, <a href="/search/astro-ph?searchtype=author&query=Man%2C+A+W+S">Allison W. S. Man</a>, <a href="/search/astro-ph?searchtype=author&query=Mundy%2C+C+J">Carl J. Mundy</a>, <a href="/search/astro-ph?searchtype=author&query=Peng%2C+Y">Yingjie Peng</a>, <a href="/search/astro-ph?searchtype=author&query=Selsing%2C+J">Jonatan Selsing</a>, <a href="/search/astro-ph?searchtype=author&query=Steinhardt%2C+C+L">Charles L. Steinhardt</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="1912.01619v1-abstract-short" style="display: inline;"> We present a detailed analysis of a large sample of spectroscopically confirmed ultra-massive quiescent galaxies (${\rm{log}}(M_{\ast}/M_{\odot})\sim11.5$) at $z\gtrsim2$. This sample comprises 15 galaxies selected in the COSMOS and UDS fields by their bright K-band magnitudes and followed up with VLT/X-shooter spectroscopy and HST/WFC3 $H_{F160W}$ imaging. These observations allow us to unambiguo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1912.01619v1-abstract-full').style.display = 'inline'; document.getElementById('1912.01619v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1912.01619v1-abstract-full" style="display: none;"> We present a detailed analysis of a large sample of spectroscopically confirmed ultra-massive quiescent galaxies (${\rm{log}}(M_{\ast}/M_{\odot})\sim11.5$) at $z\gtrsim2$. This sample comprises 15 galaxies selected in the COSMOS and UDS fields by their bright K-band magnitudes and followed up with VLT/X-shooter spectroscopy and HST/WFC3 $H_{F160W}$ imaging. These observations allow us to unambiguously confirm their redshifts ascertain their quiescent nature and stellar ages, and to reliably assess their internal kinematics and effective radii. We find that these galaxies are compact, consistent with the high mass end of the mass-size relation for quiescent galaxies at $z=2$. Moreover, the distribution of the measured stellar velocity dispersions of the sample is consistent with the most massive local early-type galaxies from the MASSIVE Survey showing that evolution in these galaxies, is dominated by changes in size. The HST images reveal, as surprisingly high, that $40\ \%$ of the sample have tidal features suggestive of mergers and companions in close proximity, including three galaxies experiencing ongoing major mergers. The absence of velocity dispersion evolution from $z=2$ to $0$, coupled with a doubling of the stellar mass, with a factor of four size increase and the observed disturbed stellar morphologies support dry minor mergers as the primary drivers of the evolution of the massive quiescent galaxies over the last 10 billion years. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1912.01619v1-abstract-full').style.display = 'none'; document.getElementById('1912.01619v1-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 December, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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, 10 figures, accepted in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1910.06236">arXiv:1910.06236</a> <span> [<a href="https://arxiv.org/pdf/1910.06236">pdf</a>, <a href="https://arxiv.org/ps/1910.06236">ps</a>, <a href="https://arxiv.org/format/1910.06236">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/10.1051/0004-6361/201936413">10.1051/0004-6361/201936413 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The CALIFA view on stellar angular momentum across the Hubble sequence </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Falc%C3%B3n-Barroso%2C+J">J. Falc贸n-Barroso</a>, <a href="/search/astro-ph?searchtype=author&query=van+de+Ven%2C+G">G. van de Ven</a>, <a href="/search/astro-ph?searchtype=author&query=Lyubenova%2C+M">M. Lyubenova</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%A9ndez-Abreu%2C+J">J. M茅ndez-Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aguerri%2C+J+A+L">J. A. L. Aguerri</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa-Lorenzo%2C+B">B. Garc铆a-Lorenzo</a>, <a href="/search/astro-ph?searchtype=author&query=Bekerait%C3%A9%2C+S">S. Bekerait茅</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez%2C+S+F">S. F. S谩nchez</a>, <a href="/search/astro-ph?searchtype=author&query=Husemann%2C+B">B. Husemann</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa-Benito%2C+R">R. Garc铆a-Benito</a>, <a href="/search/astro-ph?searchtype=author&query=Delgado%2C+R+M+G">R. M. Gonz谩lez Delgado</a>, <a href="/search/astro-ph?searchtype=author&query=Mast%2C+D">D. Mast</a>, <a href="/search/astro-ph?searchtype=author&query=Walcher%2C+C+J">C. J. Walcher</a>, <a href="/search/astro-ph?searchtype=author&query=Zibetti%2C+S">S. Zibetti</a>, <a href="/search/astro-ph?searchtype=author&query=Zhu%2C+L">L. Zhu</a>, <a href="/search/astro-ph?searchtype=author&query=Barrera-Ballesteros%2C+J+K">J. K. Barrera-Ballesteros</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Bl%C3%A1zquez%2C+P">P. S谩nchez-Bl谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Singh%2C+R">R. Singh</a>, <a href="/search/astro-ph?searchtype=author&query=Bosch%2C+R+C+E+v+d">R. C. E. van den Bosch</a>, <a href="/search/astro-ph?searchtype=author&query=Wild%2C+V">V. Wild</a>, <a href="/search/astro-ph?searchtype=author&query=Bland-Hawthorn%2C+J">J. Bland-Hawthorn</a>, <a href="/search/astro-ph?searchtype=author&query=Fernandes%2C+R+C">R. Cid Fernandes</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lorenzo-C%C3%A1ceres%2C+A">A. de Lorenzo-C谩ceres</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">A. Gallazzi</a> , et al. (10 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1910.06236v1-abstract-short" style="display: inline;"> [Abridged] We present the apparent stellar angular momentum of 300 galaxies across the Hubble sequence, using integral-field spectroscopic data from the CALIFA survey. Adopting the same $位_\mathrm{R}$ parameter previously used to distinguish between slow and fast rotating early-type (elliptical and lenticular) galaxies, we show that spiral galaxies as expected are almost all fast rotators. Given t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.06236v1-abstract-full').style.display = 'inline'; document.getElementById('1910.06236v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1910.06236v1-abstract-full" style="display: none;"> [Abridged] We present the apparent stellar angular momentum of 300 galaxies across the Hubble sequence, using integral-field spectroscopic data from the CALIFA survey. Adopting the same $位_\mathrm{R}$ parameter previously used to distinguish between slow and fast rotating early-type (elliptical and lenticular) galaxies, we show that spiral galaxies as expected are almost all fast rotators. Given the extent of our data, we provide relations for $位_\mathrm{R}$ measured in different apertures, including conversions to long-slit 1D apertures. Our sample displays a wide range of $位_\mathrm{Re}$ values, consistent with previous IFS studies. The fastest rotators are dominated by relatively massive and highly star-forming Sb galaxies, which preferentially reside in the main star-forming sequence. These galaxies reach $位_\mathrm{Re}$ values of $\sim$0.85, are the largest galaxies at a given mass, and display some of the strongest stellar population gradients. Compared to the population of S0 galaxies, our findings suggest that fading may not be the dominant mechanism transforming spirals into lenticulars. Interestingly, we find that $位_\mathrm{Re}$ decreases for late-type Sc and Sd spiral galaxies, with values than in occasions puts them in the slow-rotator regime. While for some of them this can be explained by their irregular morphologies and/or face-on configurations, others are edge-on systems with no signs of significant dust obscuration. The latter are typically at the low-mass end, but this does not explain their location in the classical ($V/蟽$,$\varepsilon$) and ($位_\mathrm{Re}$,$\varepsilon$) diagrams. Our initial investigations, based on dynamical models, suggest that these are dynamically hot disks, probably influenced by the observed important fraction of dark matter within R$_\mathrm{e}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.06236v1-abstract-full').style.display = 'none'; document.getElementById('1910.06236v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 October, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 7 figures, A&A accepted</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 632, A59 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1910.01647">arXiv:1910.01647</a> <span> [<a href="https://arxiv.org/pdf/1910.01647">pdf</a>, <a href="https://arxiv.org/format/1910.01647">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/10.1051/0004-6361/201936550">10.1051/0004-6361/201936550 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A few StePS forward in unveiling the complexity of galaxy evolution: light-weighted stellar ages of intermediate redshift galaxies with WEAVE </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Costantin%2C+L">L. Costantin</a>, <a href="/search/astro-ph?searchtype=author&query=Iovino%2C+A">A. Iovino</a>, <a href="/search/astro-ph?searchtype=author&query=Zibetti%2C+S">S. Zibetti</a>, <a href="/search/astro-ph?searchtype=author&query=Longhetti%2C+M">M. Longhetti</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">A. Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Mercurio%2C+A">A. Mercurio</a>, <a href="/search/astro-ph?searchtype=author&query=Lonoce%2C+I">I. Lonoce</a>, <a href="/search/astro-ph?searchtype=author&query=Balcells%2C+M">M. Balcells</a>, <a href="/search/astro-ph?searchtype=author&query=Bolzonella%2C+M">M. Bolzonella</a>, <a href="/search/astro-ph?searchtype=author&query=Busarello%2C+G">G. Busarello</a>, <a href="/search/astro-ph?searchtype=author&query=Dalton%2C+G">G. Dalton</a>, <a href="/search/astro-ph?searchtype=author&query=Ferr%C3%A9-Mateu%2C+A">A. Ferr茅-Mateu</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa-Benito%2C+R">R. Garc铆a-Benito</a>, <a href="/search/astro-ph?searchtype=author&query=Gargiulo%2C+A">A. Gargiulo</a>, <a href="/search/astro-ph?searchtype=author&query=Haines%2C+C">C. Haines</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+S">S. Jin</a>, <a href="/search/astro-ph?searchtype=author&query=La+Barbera%2C+F">F. La Barbera</a>, <a href="/search/astro-ph?searchtype=author&query=McGee%2C+S">S. McGee</a>, <a href="/search/astro-ph?searchtype=author&query=Merluzzi%2C+P">P. Merluzzi</a>, <a href="/search/astro-ph?searchtype=author&query=Morelli%2C+L">L. Morelli</a>, <a href="/search/astro-ph?searchtype=author&query=Murphy%2C+D+N+A">D. N. A. Murphy</a>, <a href="/search/astro-ph?searchtype=author&query=de+Arriba%2C+L+P">L. Peralta de Arriba</a>, <a href="/search/astro-ph?searchtype=author&query=Pizzella%2C+A">A. Pizzella</a>, <a href="/search/astro-ph?searchtype=author&query=Poggianti%2C+B+M">B. M. Poggianti</a>, <a href="/search/astro-ph?searchtype=author&query=Pozzetti%2C+L">L. Pozzetti</a> , et al. (7 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="1910.01647v1-abstract-short" style="display: inline;"> The upcoming new generation of optical spectrographs on four-meter-class telescopes will provide invaluable information for reconstructing the history of star formation in individual galaxies up to redshifts of about 0.7. We aim at defining simple but robust and meaningful physical parameters that can be used to trace the coexistence of widely diverse stellar components: younger stellar population… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.01647v1-abstract-full').style.display = 'inline'; document.getElementById('1910.01647v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1910.01647v1-abstract-full" style="display: none;"> The upcoming new generation of optical spectrographs on four-meter-class telescopes will provide invaluable information for reconstructing the history of star formation in individual galaxies up to redshifts of about 0.7. We aim at defining simple but robust and meaningful physical parameters that can be used to trace the coexistence of widely diverse stellar components: younger stellar populations superimposed on the bulk of older ones. We produce spectra of galaxies closely mimicking data from the forthcoming Stellar Populations at intermediate redshifts Survey (StePS), a survey that uses the WEAVE spectrograph on the William Herschel Telescope. First, we assess our ability to reliably measure both ultraviolet and optical spectral indices in galaxies of different spectral types for typically expected signal-to-noise levels. Then, we analyze such mock spectra with a Bayesian approach, deriving the probability density function of r- and u-band light-weighted ages as well as of their difference. We find that the ultraviolet indices significantly narrow the uncertainties in estimating the r- and u-band light-weighted ages and their difference in individual galaxies. These diagnostics, robustly retrievable for large galaxy samples even when observed at moderate signal-to-noise ratios, allow us to identify secondary episodes of star formation up to an age of ~0.1 Gyr for stellar populations older than ~1.5 Gyr, pushing up to an age of ~1 Gyr for stellar populations older than ~5 Gyr. The difference between r-band and u-band light-weighted ages is shown to be a powerful diagnostic to characterize and constrain extended star-formation histories and the presence of young stellar populations on top of older ones. This parameter can be used to explore the interplay between different galaxy star-formation histories and physical parameters such as galaxy mass, size, morphology, and environment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.01647v1-abstract-full').style.display = 'none'; document.getElementById('1910.01647v1-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 October, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">18 pages, 20 figures, accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 632, A9 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1909.10721">arXiv:1909.10721</a> <span> [<a href="https://arxiv.org/pdf/1909.10721">pdf</a>, <a href="https://arxiv.org/ps/1909.10721">ps</a>, <a href="https://arxiv.org/format/1909.10721">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/ab4ff3">10.3847/2041-8213/ab4ff3 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Stellar Velocity Dispersion of a Massive Quenching Galaxy at z=4.01 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Tanaka%2C+M">Masayuki Tanaka</a>, <a href="/search/astro-ph?searchtype=author&query=Valentino%2C+F">Francesco Valentino</a>, <a href="/search/astro-ph?searchtype=author&query=Toft%2C+S">Sune Toft</a>, <a href="/search/astro-ph?searchtype=author&query=Onodera%2C+M">Masato Onodera</a>, <a href="/search/astro-ph?searchtype=author&query=Shimakawa%2C+R">Rhythm Shimakawa</a>, <a href="/search/astro-ph?searchtype=author&query=Ceverino%2C+D">Daniel Ceverino</a>, <a href="/search/astro-ph?searchtype=author&query=Faisst%2C+A+L">Andreas L. Faisst</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">Anna Gallazzi</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=Kubo%2C+M">Mariko Kubo</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=Steinhardt%2C+C+L">Charles L. Steinhardt</a>, <a href="/search/astro-ph?searchtype=author&query=Stockmann%2C+M">Mikkel Stockmann</a>, <a href="/search/astro-ph?searchtype=author&query=Yabe%2C+K">Kiyoto Yabe</a>, <a href="/search/astro-ph?searchtype=author&query=Zabl%2C+J">Johannes Zabl</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="1909.10721v2-abstract-short" style="display: inline;"> We present the first stellar velocity dispersion measurement of a massive quenching galaxy at z=4.01. The galaxy is first identified as a massive z>~4 galaxy with suppressed star formation from photometric redshifts based on deep multi-band data in the UKIDSS Ultra Deep Survey field. A follow-up spectroscopic observation with MOSFIRE on Keck revealed strong multiple absorption features, which are… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.10721v2-abstract-full').style.display = 'inline'; document.getElementById('1909.10721v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1909.10721v2-abstract-full" style="display: none;"> We present the first stellar velocity dispersion measurement of a massive quenching galaxy at z=4.01. The galaxy is first identified as a massive z>~4 galaxy with suppressed star formation from photometric redshifts based on deep multi-band data in the UKIDSS Ultra Deep Survey field. A follow-up spectroscopic observation with MOSFIRE on Keck revealed strong multiple absorption features, which are identified as Balmer absorption lines, giving a secure redshift of z=4.01. Thanks to the high S/N of the spectrum, we are able to estimate the stellar velocity dispersion, sigma=268+/-59 km/s. This velocity dispersion is consistent with that of massive galaxies today, implying no significant evolution in stellar velocity dispersion over the last 12 Gyr. Based on an upper limit on its physical size from deep optical images (r_eff<1.3 kpc), we find that its dynamical mass is consistent with the stellar mass inferred from photometry. Furthermore, the galaxy is located on the mass fundamental plane extrapolated from lower redshift galaxies. Combining all these results, we find that the velocity dispersion does not significantly evolve with redshift, although the size and mass of massive quenched galaxies do. This suggests that the mass in the core of massive galaxies does not evolve significantly, while most of the mass growth occurs in the outskirts of the galaxies, which also increases the size. This picture is consistent with a two-phase formation scenario in which mass and size growth is due to accretion in the outskirts of galaxies via mergers. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.10721v2-abstract-full').style.display = 'none'; document.getElementById('1909.10721v2-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 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published in the Astrophysical Journal letters. Fixed an error in dynamical mass</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJL, 885 (2019), L34 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1909.10540">arXiv:1909.10540</a> <span> [<a href="https://arxiv.org/pdf/1909.10540">pdf</a>, <a href="https://arxiv.org/format/1909.10540">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ab64dc">10.3847/1538-4357/ab64dc <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Quiescent galaxies 1.5 billion years after the Big Bang and their progenitors </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=Tanaka%2C+M">Masayuki Tanaka</a>, <a href="/search/astro-ph?searchtype=author&query=Davidzon%2C+I">Iary Davidzon</a>, <a href="/search/astro-ph?searchtype=author&query=Toft%2C+S">Sune Toft</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=Stockmann%2C+M">Mikkel Stockmann</a>, <a href="/search/astro-ph?searchtype=author&query=Onodera%2C+M">Masato Onodera</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G">Gabriel Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Ceverino%2C+D">Daniel Ceverino</a>, <a href="/search/astro-ph?searchtype=author&query=Faisst%2C+A+L">Andreas L. Faisst</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">Anna Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Hayward%2C+C+C">Christopher C. Hayward</a>, <a href="/search/astro-ph?searchtype=author&query=Ilbert%2C+O">Olivier Ilbert</a>, <a href="/search/astro-ph?searchtype=author&query=Kubo%2C+M">Mariko Kubo</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=Selsing%2C+J">Jonatan Selsing</a>, <a href="/search/astro-ph?searchtype=author&query=Shimakawa%2C+R">Rhythm Shimakawa</a>, <a href="/search/astro-ph?searchtype=author&query=Sparre%2C+M">Martin Sparre</a>, <a href="/search/astro-ph?searchtype=author&query=Steinhardt%2C+C">Charles Steinhardt</a>, <a href="/search/astro-ph?searchtype=author&query=Yabe%2C+K">Kiyoto Yabe</a>, <a href="/search/astro-ph?searchtype=author&query=Zabl%2C+J">Johannes Zabl</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="1909.10540v2-abstract-short" style="display: inline;"> We report two secure ($z=3.775, 4.012$) and one tentative ($z\approx3.767$) spectroscopic confirmations of massive and quiescent galaxies through $K$-band observations with Keck/MOSFIRE and VLT/X-Shooter. The stellar continuum emission, the absence of strong nebular emission lines and the lack of significant far-infrared detections confirm the passive nature of these objects, disfavoring the alter… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.10540v2-abstract-full').style.display = 'inline'; document.getElementById('1909.10540v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1909.10540v2-abstract-full" style="display: none;"> We report two secure ($z=3.775, 4.012$) and one tentative ($z\approx3.767$) spectroscopic confirmations of massive and quiescent galaxies through $K$-band observations with Keck/MOSFIRE and VLT/X-Shooter. The stellar continuum emission, the absence of strong nebular emission lines and the lack of significant far-infrared detections confirm the passive nature of these objects, disfavoring the alternative solution of low-redshift dusty star-forming interlopers. We derive stellar masses of $\mathrm{log}(M_{\star}/M_\odot)\sim11$ and ongoing star formation rates placing these galaxies $\gtrsim 1-2$ dex below the main sequence at their redshifts. The adopted parametrization of the star formation history suggests that these sources experienced a strong ($\langle \rm SFR \rangle \sim 1200-3500\,M_\odot\,\mathrm{yr}^{-1}$) and short ($\sim 50$ Myr) burst of star formation, peaking $\sim 150-500$ Myr before the time of observation, all properties reminiscent of the characteristics of sub-millimeter galaxies (SMGs) at $z>4$. We investigate this connection by comparing the comoving number densities and the properties of these two populations. We find a fair agreement only with the deepest sub-mm surveys detecting not only the most extreme starbursts, but also more normal galaxies. We support these findings by further exploring the Illustris-TNG cosmological simulation, retrieving populations of both fully quenched massive galaxies at $z\sim3-4$ and SMGs at $z\sim4-5$, with number densities and properties in agreement with the observations at $z\sim3$, but in increasing tension at higher redshift. Nevertheless, as suggested by the observations, not all the progenitors of quiescent galaxies at these redshifts shine as bright SMGs in their past and, similarly, not all bright SMGs quench by $z\sim3$, both fractions depending on the threshold assumed to define the SMGs themselves. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.10540v2-abstract-full').style.display = 'none'; document.getElementById('1909.10540v2-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 December, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages (+appendix), 11 figures, accepted for publication in the Astrophysical Journal (ApJ). This work comes with a companion letter by Tanaka, Valentino, Toft et al. 2019, ApJL, 885, L34</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1909.01133">arXiv:1909.01133</a> <span> [<a href="https://arxiv.org/pdf/1909.01133">pdf</a>, <a href="https://arxiv.org/format/1909.01133">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/stz2573">10.1093/mnras/stz2573 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Oxygen yields as a constraint on feedback processes in galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lara-Lopez%2C+M+A">Maritza A. Lara-Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=De+Rossi%2C+M+E">Maria Emilia De Rossi</a>, <a href="/search/astro-ph?searchtype=author&query=Pilyugin%2C+L+S">Leonid S. Pilyugin</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">Anna Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Hughes%2C+T+M">Thomas M. Hughes</a>, <a href="/search/astro-ph?searchtype=author&query=Zinchenko%2C+I+A">Igor A. Zinchenko</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="1909.01133v2-abstract-short" style="display: inline;"> We study the interplay between several properties determined from Optical and a combination of Optical/Radio measurements, such as the effective Oxygen yield (y_eff), the star formation efficiency, gas metallicity, depletion time, gas fraction, and baryonic mass(M_bar), among others. We use spectroscopic data from the SDSS survey, and HI information from the ALFALFA survey to build a statistically… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.01133v2-abstract-full').style.display = 'inline'; document.getElementById('1909.01133v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1909.01133v2-abstract-full" style="display: none;"> We study the interplay between several properties determined from Optical and a combination of Optical/Radio measurements, such as the effective Oxygen yield (y_eff), the star formation efficiency, gas metallicity, depletion time, gas fraction, and baryonic mass(M_bar), among others. We use spectroscopic data from the SDSS survey, and HI information from the ALFALFA survey to build a statistically significant sample of more than 5,000 galaxies. Furthermore, we complement our analysis with data from the GASS and COLD GASS surveys, and with a sample of star-forming galaxies from the Virgo cluster. Additionally, we have compared our results with predictions from the EAGLE simulations, finding a very good agreement when using the high-resolution run. We explore in detail the M_bar-y_eff relation, finding a bimodal trend that can be separated when the stellar age of galaxies is considered. On one hand, y_eff increases with M_bar for young galaxies(log(t_r) < 9.2 yr), while y_eff shows an anti-correlation with M_bar for older galaxies (log(t_r) > 9.4 yr). While a correlation between M_bar and y_eff has been observed and studied before, mainly for samples of dwarfs and irregular galaxies, their anti-correlated counterpart for massive galaxies has not been previously reported. The EAGLE simulations indicate that AGN feedback must have played an important role in their history by quenching their star formation rate, whereas low mass galaxies would have been affected by a combination of outflows and infall of gas. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.01133v2-abstract-full').style.display = 'none'; document.getElementById('1909.01133v2-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 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">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/1906.02209">arXiv:1906.02209</a> <span> [<a href="https://arxiv.org/pdf/1906.02209">pdf</a>, <a href="https://arxiv.org/format/1906.02209">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/stz3205">10.1093/mnras/stz3205 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Insights into formation scenarios of massive Early-Type galaxies from spatially resolved stellar population analysis in CALIFA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zibetti%2C+S">Stefano Zibetti</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A+R">Anna R. Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">Michaela Hirschmann</a>, <a href="/search/astro-ph?searchtype=author&query=Consolandi%2C+G">Guido Consolandi</a>, <a href="/search/astro-ph?searchtype=author&query=Falc%C3%B3n-Barroso%2C+J">Jes煤s Falc贸n-Barroso</a>, <a href="/search/astro-ph?searchtype=author&query=van+de+Ven%2C+G">Glenn van de Ven</a>, <a href="/search/astro-ph?searchtype=author&query=Lyubenova%2C+M">Mariya Lyubenova</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="1906.02209v2-abstract-short" style="display: inline;"> We perform spatially resolved stellar population analysis for a sample of 69 early-type galaxies (ETGs) from the CALIFA integral field spectroscopic survey, including 48 ellipticals and 21 S0's. We generate and quantitatively characterize profiles of light-weighted mean stellar age and metallicity within $\lesssim 2R_e$, as a function of radius and stellar-mass surface density $渭_*$. We study in d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.02209v2-abstract-full').style.display = 'inline'; document.getElementById('1906.02209v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1906.02209v2-abstract-full" style="display: none;"> We perform spatially resolved stellar population analysis for a sample of 69 early-type galaxies (ETGs) from the CALIFA integral field spectroscopic survey, including 48 ellipticals and 21 S0's. We generate and quantitatively characterize profiles of light-weighted mean stellar age and metallicity within $\lesssim 2R_e$, as a function of radius and stellar-mass surface density $渭_*$. We study in detail the dependence of profiles on galaxies' global properties, including velocity dispersion $蟽_e$, stellar mass, morphology. ETGs are universally characterized by strong, negative metallicity gradients ($\sim -0.3\,\text{dex}$ per $R_e$) within $1\,R_e$, which flatten out moving towards larger radii. A quasi-universal local $渭_*$-metallicity relation emerges, which displays a residual systematic dependence on $蟽_e$, whereby higher $蟽_e$ implies higher metallicity at fixed $渭_*$. Age profiles are typically U-shaped, with minimum around $0.4\,R_e$, asymptotic increase to maximum ages beyond $\sim 1.5\,R_e$, and an increase towards the centre. The depth of the minimum and the central increase anti-correlate with $蟽_e$. A possible qualitative interpretation of these observations is a two-phase scenario. In the first phase, dissipative collapse occurs in the inner $1\,R_e$, establishing a negative metallicity gradient. The competition between the outside-in quenching due to feedback-driven winds and some form of inside-out quenching, possibly caused by central AGN feedback or dynamical heating, determines the U-shaped age profiles. In the second phase, the accretion of ex-situ stars from quenched and low-metallicity satellites shapes the flatter stellar population profiles in the outer regions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.02209v2-abstract-full').style.display = 'none'; document.getElementById('1906.02209v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 November, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 June, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted version to appear in MNRAS. Improved discussion with respect to original submission and additional tests included</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1905.07541">arXiv:1905.07541</a> <span> [<a href="https://arxiv.org/pdf/1905.07541">pdf</a>, <a href="https://arxiv.org/format/1905.07541">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ab164d">10.3847/1538-4357/ab164d <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Rejuvenation in $z\sim0.8$ quiescent galaxies in LEGA-C </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chauke%2C+P">Priscilla Chauke</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Wel%2C+A">Arjen van der Wel</a>, <a href="/search/astro-ph?searchtype=author&query=Pacifici%2C+C">Camilla Pacifici</a>, <a href="/search/astro-ph?searchtype=author&query=Bezanson%2C+R">Rachel Bezanson</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+P">Po-Feng Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Gallazzi%2C+A">Anna Gallazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Straatman%2C+C">Caroline Straatman</a>, <a href="/search/astro-ph?searchtype=author&query=Franx%2C+M">Marijn Franx</a>, <a href="/search/astro-ph?searchtype=author&query=Bari%C5%A1i%C4%87%2C+I">Ivana Bari拧i膰</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+E+F">Eric F. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=van+Houdt%2C+J">Josha van Houdt</a>, <a href="/search/astro-ph?searchtype=author&query=Maseda%2C+M+V">Michael V. Maseda</a>, <a href="/search/astro-ph?searchtype=author&query=Muzzin%2C+A">Adam Muzzin</a>, <a href="/search/astro-ph?searchtype=author&query=Sobral%2C+D">David Sobral</a>, <a href="/search/astro-ph?searchtype=author&query=Spilker%2C+J">Justin Spilker</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="1905.07541v1-abstract-short" style="display: inline;"> We use reconstructed star-formation histories (SFHs) of quiescent galaxies at $z=0.6-1$ in the LEGA-C survey to identify secondary star-formation episodes that, after an initial period of quiescence, moved the galaxies back to the star-forming main sequence (blue cloud). $16\pm3$\% of the $z\sim0.8$ quiescent population has experienced such rejuvenation events in the redshift range $0.7<z<1.5$ aft… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.07541v1-abstract-full').style.display = 'inline'; document.getElementById('1905.07541v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1905.07541v1-abstract-full" style="display: none;"> We use reconstructed star-formation histories (SFHs) of quiescent galaxies at $z=0.6-1$ in the LEGA-C survey to identify secondary star-formation episodes that, after an initial period of quiescence, moved the galaxies back to the star-forming main sequence (blue cloud). $16\pm3$\% of the $z\sim0.8$ quiescent population has experienced such rejuvenation events in the redshift range $0.7<z<1.5$ after reaching quiescence at some earlier time. On average, these galaxies first became quiescent at $z=1.2$, and those that rejuvenated, remained quiescent for $\sim1$Gyr before their secondary SF episode which lasted $\sim0.7$Gyr. The stellar mass attributed to rejuvenation is on average 10\% of the galaxy stellar mass, with rare instances of an increase of more than a factor 2. Overall, rejuvenation events only contribute $\sim2$\% of the total stellar mass in $z\sim0.8$ quiescent galaxies and we conclude that rejuvenation is not an important evolutionary channel when considering the growth of the red sequence. However, our results complicate the interpretation of galaxy demographics in color space: the galaxies with rejuvenation events tend to lie in the so-called `green valley', yet their progenitors were quiescent at $z\sim2$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.07541v1-abstract-full').style.display = 'none'; document.getElementById('1905.07541v1-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 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">14 pages, 8 figures, accepted by ApJ</span> </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a 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