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start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.17049">arXiv:2411.17049</a> <span> [<a href="https://arxiv.org/pdf/2411.17049">pdf</a>, <a href="https://arxiv.org/format/2411.17049">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 Spatial Distribution of Globular Cluster Systems in Early Type Galaxies: Estimation Procedure and Catalog of Properties for Globular Cluster Systems Observed with Deep Imaging Surveys </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lim%2C+S">Sungsoon Lim</a>, <a href="/search/astro-ph?searchtype=author&query=Peng%2C+E+W">Eric W. Peng</a>, <a href="/search/astro-ph?searchtype=author&query=C%C3%B4t%C3%A9%2C+P">Patrick C么t茅</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrarese%2C+L">Laura Ferrarese</a>, <a href="/search/astro-ph?searchtype=author&query=Roediger%2C+J+C">Joel C. Roediger</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+C">Chengze Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Spengler%2C+C">Chelsea Spengler</a>, <a href="/search/astro-ph?searchtype=author&query=Sola%2C+E">Elisabeth Sola</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P">Pierre-Alain Duc</a>, <a href="/search/astro-ph?searchtype=author&query=Sales%2C+L+V">Laura V. Sales</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Cuillandre%2C+J">Jean-Charles Cuillandre</a>, <a href="/search/astro-ph?searchtype=author&query=Durrell%2C+P+R">Patrick R. Durrell</a>, <a href="/search/astro-ph?searchtype=author&query=Emsellem%2C+E">Eric Emsellem</a>, <a href="/search/astro-ph?searchtype=author&query=Gwyn%2C+S+D+J">Stephen D. J. Gwyn</a>, <a href="/search/astro-ph?searchtype=author&query=Lan%C3%A7on%2C+A">Ariane Lan莽on</a>, <a href="/search/astro-ph?searchtype=author&query=Marleau%2C+F+R">Francine R. Marleau</a>, <a href="/search/astro-ph?searchtype=author&query=Mihos%2C+J+C">J. Christopher Mihos</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%BCller%2C+O">Oliver M眉ller</a>, <a href="/search/astro-ph?searchtype=author&query=Puzia%2C+T+H">Thomas H. Puzia</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">Rub茅n S谩nchez-Janssen</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.17049v1-abstract-short" style="display: inline;"> We present an analysis of the spatial distribution of globular cluster (GC) systems of 118 nearby early-type galaxies in the Next Generation Virgo Cluster Survey (NGVS) and Mass Assembly of early-Type GaLAxies with their fine Structures (MATLAS) survey programs, which both used MegaCam on the Canada-France-Hawaii Telescope. We describe the procedure used to select GC candidates and fit the spatial… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.17049v1-abstract-full').style.display = 'inline'; document.getElementById('2411.17049v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.17049v1-abstract-full" style="display: none;"> We present an analysis of the spatial distribution of globular cluster (GC) systems of 118 nearby early-type galaxies in the Next Generation Virgo Cluster Survey (NGVS) and Mass Assembly of early-Type GaLAxies with their fine Structures (MATLAS) survey programs, which both used MegaCam on the Canada-France-Hawaii Telescope. We describe the procedure used to select GC candidates and fit the spatial distributions of GCs to a two-dimensional S茅rsic function, which provides effective radii (half number radii) and S茅rsic indices, and estimate background contamination by adding a constant term to the S'ersic function. In cases where a neighboring galaxy affects the estimation of the GC spatial distribution in the target galaxy, we fit two 2D S茅rsic functions, simultaneously. We also investigate the color distributions of GCs in our sample by using Gaussian Mixture Modeling. For GC systems with bimodal color distributions, we divide the GCs into blue and red subgroups and fit their respective spatial distributions with S茅rsic functions. Finally, we measure the total number of GCs based on our fitted S茅rsic function, and calculate the GC specific frequency. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.17049v1-abstract-full').style.display = 'none'; document.getElementById('2411.17049v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">31 pages, 10 Figures (115 additional figures are available in the ApJS online Journal), 2 Tables, accepted for publication in ApJS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.06795">arXiv:2411.06795</a> <span> [<a href="https://arxiv.org/pdf/2411.06795">pdf</a>, <a href="https://arxiv.org/format/2411.06795">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/10.1051/0004-6361/202450143">10.1051/0004-6361/202450143 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Dwarf Galaxies in the MATLAS Survey: The satellite system of NGC474 under scrutiny with MUSE </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=M%C3%BCller%2C+O">Oliver M眉ller</a>, <a href="/search/astro-ph?searchtype=author&query=Marleau%2C+F+R">Francine R. Marleau</a>, <a href="/search/astro-ph?searchtype=author&query=Heesters%2C+N">Nick Heesters</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P">Pierre-Alain Duc</a>, <a href="/search/astro-ph?searchtype=author&query=Pawlowski%2C+M+S">Marcel S. Pawlowski</a>, <a href="/search/astro-ph?searchtype=author&query=Poulain%2C+M">M茅lina Poulain</a>, <a href="/search/astro-ph?searchtype=author&query=Habas%2C+R">Rebecca Habas</a>, <a href="/search/astro-ph?searchtype=author&query=Sola%2C+E">Elisabeth Sola</a>, <a href="/search/astro-ph?searchtype=author&query=Urbano%2C+M">Mathias Urbano</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+R">Rory Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Durrell%2C+P">Patrick Durrell</a>, <a href="/search/astro-ph?searchtype=author&query=Emsellem%2C+E">Eric Emsellem</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">Rub茅n S谩nchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Lim%2C+S">Sungsoon Lim</a>, <a href="/search/astro-ph?searchtype=author&query=Paudel%2C+S">Sanjaya Paudel</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.06795v1-abstract-short" style="display: inline;"> A recent study of the distribution of dwarf galaxies in the MATLAS sample in galaxy groups revealed an excess of flattened satellite structures, reminiscent of the co-rotating planes of dwarf galaxies discovered in the local Universe. If confirmed, this lends credence to the plane-of-satellite problem and further challenges the standard model of hierarchical structure formation. However, with only… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.06795v1-abstract-full').style.display = 'inline'; document.getElementById('2411.06795v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.06795v1-abstract-full" style="display: none;"> A recent study of the distribution of dwarf galaxies in the MATLAS sample in galaxy groups revealed an excess of flattened satellite structures, reminiscent of the co-rotating planes of dwarf galaxies discovered in the local Universe. If confirmed, this lends credence to the plane-of-satellite problem and further challenges the standard model of hierarchical structure formation. However, with only photometric data and no confirmation of the satellite membership, the study could not address the plane-of-satellite problem in full detail. Here we present spectroscopic follow-up observations of one of the most promising planes-of-satellites candidates in the MATLAS survey, the satellite system of NGC 474. Employing MUSE at the VLT and full spectrum fitting, we studied 13 dwarf galaxy candidates and confirmed nine to be members of the field around NGC 474. Measuring the stellar populations of all observed galaxies, we find that the MATLAS dwarfs have lower metallicities than the Local Group dwarfs at given luminosity. Two dwarf galaxies may form a pair of satellites based on their close projection and common velocity. Within the virial radius, we do not find a significant plane-of-satellites, however, there is a sub-population of six dwarf galaxies which seem to be anti-correlated in phase-space. Due to the low number of dwarf galaxies, this signal may arise by chance. With over 2000 dwarf galaxy candidates found in the MATLAS survey, this remains an intriguing data set to study the plane-of-satellites problem in a statistical fashion once more follow-up observations have been conducted. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.06795v1-abstract-full').style.display = 'none'; document.getElementById('2411.06795v1-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 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 8 figures, 2 tables. Accepted for publication in Astronomy & Astrophysics (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 693, A44 (2025) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.03311">arXiv:2408.03311</a> <span> [<a href="https://arxiv.org/pdf/2408.03311">pdf</a>, <a href="https://arxiv.org/format/2408.03311">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"> Dwarf Galaxies in the MATLAS Survey: Hubble Space Telescope Observations of the Globular Cluster Systems of 74 Ultra Diffuse Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Marleau%2C+F+R">Francine R. Marleau</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P">Pierre-Alain Duc</a>, <a href="/search/astro-ph?searchtype=author&query=Poulain%2C+M">Melina Poulain</a>, <a href="/search/astro-ph?searchtype=author&query=Mueller%2C+O">Oliver Mueller</a>, <a href="/search/astro-ph?searchtype=author&query=Lim%2C+S">Sungsoon Lim</a>, <a href="/search/astro-ph?searchtype=author&query=Durrell%2C+P+R">Patrick R. Durrell</a>, <a href="/search/astro-ph?searchtype=author&query=Habas%2C+R">Rebecca Habas</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez-Janssen%2C+R">Ruben Sanchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Paudel%2C+S">Sanjaya Paudel</a>, <a href="/search/astro-ph?searchtype=author&query=Fensch%2C+J">Jeremy Fensch</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="2408.03311v1-abstract-short" style="display: inline;"> Ultra diffuse galaxies, characterized by their low surface brightness and large physical size, constitute a subclass of dwarf galaxies that challenge our current understanding of galaxy formation and evolution. In this paper, we probe the properties of 74 UDGs, identified in the MATLAS survey, based on a comprehensive study of their globular cluster (GC) populations. We obtained high resolution HS… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.03311v1-abstract-full').style.display = 'inline'; document.getElementById('2408.03311v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.03311v1-abstract-full" style="display: none;"> Ultra diffuse galaxies, characterized by their low surface brightness and large physical size, constitute a subclass of dwarf galaxies that challenge our current understanding of galaxy formation and evolution. In this paper, we probe the properties of 74 UDGs, identified in the MATLAS survey, based on a comprehensive study of their globular cluster (GC) populations. We obtained high resolution HST imaging of these galaxies using the ACS F606W and F814W filters, allowing us to select GCs based on color and concentration index. After background subtraction and completeness correction, we calculate an overall total of 387 GCs. The number of GCs per galaxy ranges from 0 to 38, with the majority (64%) having low counts (0-2 GCs). On average, the more massive UDGs host a larger number of GCs. We find that our UDGs have specific frequencies (S_N) ranging from 0 to 91, with a small population (9%) with S_N > 30. The median S_N of our sample is similar to the one for the Perseus cluster UDGs, despite the fact that our UDGs are found in lower density environments. The S_N measurements for individual galaxies can extend beyond those found in Perseus, but remain below the values found for UDGs in the Virgo and Coma cluster. Based on a trending analysis of the S_N values with the host galaxy properties, we find trends with host galaxy size, roundness, color, and local density. For the UDGs with sufficiently high statistics, we study 2D density maps of the GC distributions, which show a variety of appearances: symmetric, asymmetric, off-center, and elongated. The UDGs with disturbed density maps also show disturbed stellar light morphologies. We further quantify the distribution by modeling it with a Sersic profile, finding R_{e,GC}/R_{e,gal} ~ 1.0, which indicates that the GCs follow the stellar light of the host galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.03311v1-abstract-full').style.display = 'none'; document.getElementById('2408.03311v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 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">20 pages, 17 figures, 2 tables, accepted for publication in A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.14356">arXiv:2407.14356</a> <span> [<a href="https://arxiv.org/pdf/2407.14356">pdf</a>, <a href="https://arxiv.org/format/2407.14356">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> </div> </div> <p class="title is-5 mathjax"> Atmosphyre: Modelling Atmospheric Chromatic Dispersion for Multi-Object Spectrographs </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Stephan%2C+J">J. Stephan</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">R. S谩nchez-Janssen</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="2407.14356v1-abstract-short" style="display: inline;"> The wavelength dependent refraction of light in the atmosphere causes the chromatic dispersion of a target on the focal plane of an instrument. This is known as atmospheric dispersion, with one of the consequences being wavelength dependent flux losses which are difficult to minimise, requiring analysis in both instrument design and operations. We present Atmosphyre, a novel python package develop… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.14356v1-abstract-full').style.display = 'inline'; document.getElementById('2407.14356v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.14356v1-abstract-full" style="display: none;"> The wavelength dependent refraction of light in the atmosphere causes the chromatic dispersion of a target on the focal plane of an instrument. This is known as atmospheric dispersion, with one of the consequences being wavelength dependent flux losses which are difficult to minimise, requiring analysis in both instrument design and operations. We present Atmosphyre, a novel python package developed to characterise the impact of atmospheric dispersion on a spectrograph, with a focus on fibre multi-object spectrographs (MOS) which will be at the forefront of ground-based astronomy for the next few decades. We show example simulations and provide recommendations for minimising fibre MOS flux losses. We conclude that the guiding wavelength should typically be bluer than the observing band mid-wavelength, around 25-45% of the way through the band. The aperture should be centred on this wavelength's location on the focal plane. This wavelength/position remains constant for all reasonable declinations and target hour angles. We also present an application of the package to MOSAIC, the ELT's multi-object spectrograph. We find that differential losses greater than 10% are unavoidable for 1h observations that are a) after a local hour angle of 2.5h, or b) at declinations below -60 degrees and above 10 degrees. We identify that the introduction of an atmospheric dispersion corrector (ADC) would result in the significant reduction of spectral distortions, a gain in survey speed for many observations, and enable the implementation of wider visible observing bands; as a result, there has been a proposal to adopt ADCs at a positioner level for MOSAIC. Future work includes adding field differential refraction to Atmosphyre, important for future wide-field multi-object spectrograph projects such as the proposed WST. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.14356v1-abstract-full').style.display = 'none'; document.getElementById('2407.14356v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 July, 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">10 pages, 6 figures, submitted to SPIE Astronomical Telescopes & Instrumentation, Ground-based and Airborne Instrumentation for Astronomy X (Conference 13096, Paper 219)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.14015">arXiv:2405.14015</a> <span> [<a href="https://arxiv.org/pdf/2405.14015">pdf</a>, <a href="https://arxiv.org/format/2405.14015">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/10.1051/0004-6361/202450851">10.1051/0004-6361/202450851 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Euclid preparation. LVIII. Detecting globular clusters in the Euclid survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Euclid+Collaboration"> Euclid Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Voggel%2C+K">K. Voggel</a>, <a href="/search/astro-ph?searchtype=author&query=Lan%C3%A7on%2C+A">A. Lan莽on</a>, <a href="/search/astro-ph?searchtype=author&query=Saifollahi%2C+T">T. Saifollahi</a>, <a href="/search/astro-ph?searchtype=author&query=Larsen%2C+S+S">S. S. Larsen</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">M. Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">M. Rejkuba</a>, <a href="/search/astro-ph?searchtype=author&query=Cuillandre%2C+J+-">J. -C. Cuillandre</a>, <a href="/search/astro-ph?searchtype=author&query=Hudelot%2C+P">P. Hudelot</a>, <a href="/search/astro-ph?searchtype=author&query=Nucita%2C+A+A">A. A. Nucita</a>, <a href="/search/astro-ph?searchtype=author&query=Urbano%2C+M">M. Urbano</a>, <a href="/search/astro-ph?searchtype=author&query=Romelli%2C+E">E. Romelli</a>, <a href="/search/astro-ph?searchtype=author&query=Raj%2C+M+A">M. A. Raj</a>, <a href="/search/astro-ph?searchtype=author&query=Schirmer%2C+M">M. Schirmer</a>, <a href="/search/astro-ph?searchtype=author&query=Tortora%2C+C">C. Tortora</a>, <a href="/search/astro-ph?searchtype=author&query=Abdurro%27uf"> Abdurro'uf</a>, <a href="/search/astro-ph?searchtype=author&query=Annibali%2C+F">F. Annibali</a>, <a href="/search/astro-ph?searchtype=author&query=Baes%2C+M">M. Baes</a>, <a href="/search/astro-ph?searchtype=author&query=Boldrini%2C+P">P. Boldrini</a>, <a href="/search/astro-ph?searchtype=author&query=Cabanac%2C+R">R. Cabanac</a>, <a href="/search/astro-ph?searchtype=author&query=Carollo%2C+D">D. Carollo</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C+J">C. J. Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P+-">P. -A. Duc</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+A+M+N">A. M. N. Ferguson</a>, <a href="/search/astro-ph?searchtype=author&query=Hunt%2C+L+K">L. K. Hunt</a> , et al. (248 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.14015v3-abstract-short" style="display: inline;"> Extragalactic globular clusters (EGCs) are an abundant and powerful tracer of galaxy dynamics and formation, and their own formation and evolution is also a matter of extensive debate. The compact nature of globular clusters means that they are hard to spatially resolve and thus study outside the Local Group. In this work we have examined how well EGCs will be detectable in images from the Euclid… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.14015v3-abstract-full').style.display = 'inline'; document.getElementById('2405.14015v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.14015v3-abstract-full" style="display: none;"> Extragalactic globular clusters (EGCs) are an abundant and powerful tracer of galaxy dynamics and formation, and their own formation and evolution is also a matter of extensive debate. The compact nature of globular clusters means that they are hard to spatially resolve and thus study outside the Local Group. In this work we have examined how well EGCs will be detectable in images from the Euclid telescope, using both simulated pre-launch images and the first early-release observations of the Fornax galaxy cluster. The Euclid Wide Survey will provide high-spatial resolution VIS imaging in the broad IE band as well as near-infrared photometry (YE, JE, and HE). We estimate that the galaxies within 100 Mpc in the footprint of the Euclid survey host around 830 000 EGCs of which about 350 000 are within the survey's detection limits. For about half of these EGCs, three infrared colours will be available as well. For any galaxy within 50Mpc the brighter half of its GC luminosity function will be detectable by the Euclid Wide Survey. The detectability of EGCs is mainly driven by the residual surface brightness of their host galaxy. We find that an automated machine-learning EGC-classification method based on real Euclid data of the Fornax galaxy cluster provides an efficient method to generate high purity and high completeness GC candidate catalogues. We confirm that EGCs are spatially resolved compared to pure point sources in VIS images of Fornax. Our analysis of both simulated and first on-sky data show that Euclid will increase the number of GCs accessible with high-resolution imaging substantially compared to previous surveys, and will permit the study of GCs in the outskirts of their hosts. Euclid is unique in enabling systematic studies of EGCs in a spatially unbiased and homogeneous manner and is primed to improve our understanding of many understudied aspects of GC astrophysics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.14015v3-abstract-full').style.display = 'none'; document.getElementById('2405.14015v3-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 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 693, A251 (2025) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.13502">arXiv:2405.13502</a> <span> [<a href="https://arxiv.org/pdf/2405.13502">pdf</a>, <a href="https://arxiv.org/format/2405.13502">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"> Euclid: Early Release Observations -- Dwarf galaxies in the Perseus galaxy cluster </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Marleau%2C+F+R">F. R. Marleau</a>, <a href="/search/astro-ph?searchtype=author&query=Cuillandre%2C+J+-">J. -C. Cuillandre</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">M. Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Carollo%2C+D">D. Carollo</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P+-">P. -A. Duc</a>, <a href="/search/astro-ph?searchtype=author&query=Habas%2C+R">R. Habas</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=Jablonka%2C+P">P. Jablonka</a>, <a href="/search/astro-ph?searchtype=author&query=Mirabile%2C+M">M. Mirabile</a>, <a href="/search/astro-ph?searchtype=author&query=Mondelin%2C+M">M. Mondelin</a>, <a href="/search/astro-ph?searchtype=author&query=Poulain%2C+M">M. Poulain</a>, <a href="/search/astro-ph?searchtype=author&query=Saifollahi%2C+T">T. Saifollahi</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">R. S谩nchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Sola%2C+E">E. Sola</a>, <a href="/search/astro-ph?searchtype=author&query=Urbano%2C+M">M. Urbano</a>, <a href="/search/astro-ph?searchtype=author&query=Z%C3%B6ller%2C+R">R. Z枚ller</a>, <a href="/search/astro-ph?searchtype=author&query=Bolzonella%2C+M">M. Bolzonella</a>, <a href="/search/astro-ph?searchtype=author&query=Lan%C3%A7on%2C+A">A. Lan莽on</a>, <a href="/search/astro-ph?searchtype=author&query=Laureijs%2C+R">R. Laureijs</a>, <a href="/search/astro-ph?searchtype=author&query=Marchal%2C+O">O. Marchal</a>, <a href="/search/astro-ph?searchtype=author&query=Schirmer%2C+M">M. Schirmer</a>, <a href="/search/astro-ph?searchtype=author&query=Stone%2C+C">C. Stone</a>, <a href="/search/astro-ph?searchtype=author&query=Boselli%2C+A">A. Boselli</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=Hatch%2C+N+A">N. A. Hatch</a> , et al. (171 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.13502v1-abstract-short" style="display: inline;"> We make use of the unprecedented depth, spatial resolution, and field of view of the Euclid Early Release Observations of the Perseus galaxy cluster to detect and characterise the dwarf galaxy population in this massive system. The Euclid high resolution VIS and combined VIS+NIR colour images were visually inspected and dwarf galaxy candidates were identified. Their morphologies, the presence of n… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.13502v1-abstract-full').style.display = 'inline'; document.getElementById('2405.13502v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.13502v1-abstract-full" style="display: none;"> We make use of the unprecedented depth, spatial resolution, and field of view of the Euclid Early Release Observations of the Perseus galaxy cluster to detect and characterise the dwarf galaxy population in this massive system. The Euclid high resolution VIS and combined VIS+NIR colour images were visually inspected and dwarf galaxy candidates were identified. Their morphologies, the presence of nuclei, and their globular cluster (GC) richness were visually assessed, complementing an automatic detection of the GC candidates. Structural and photometric parameters, including Euclid filter colours, were extracted from 2-dimensional fitting. Based on this analysis, a total of 1100 dwarf candidates were found across the image, with 638 appearing to be new identifications. The majority (96%) are classified as dwarf ellipticals, 53% are nucleated, 26% are GC-rich, and 6% show disturbed morphologies. A relatively high fraction of galaxies, 8%, are categorised as ultra-diffuse galaxies. The majority of the dwarfs follow the expected scaling relations. Globally, the GC specific frequency, S_N, of the Perseus dwarfs is intermediate between those measured in the Virgo and Coma clusters. While the dwarfs with the largest GC counts are found throughout the Euclid field of view, those located around the east-west strip, where most of the brightest cluster members are found, exhibit larger S_N values, on average. The spatial distribution of the dwarfs, GCs, and intracluster light show a main iso-density/isophotal centre displaced to the west of the bright galaxy light distribution. The ERO imaging of the Perseus cluster demonstrates the unique capability of Euclid to concurrently detect and characterise large samples of dwarfs, their nuclei, and their GC systems, allowing us to construct a detailed picture of the formation and evolution of galaxies over a wide range of mass scales and environments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.13502v1-abstract-full').style.display = 'none'; document.getElementById('2405.13502v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">44 pages, 24 figures, 5 tables, paper submitted to A&A as part of the A&A special issue `Euclid on Sky', which contains Euclid key reference papers and first results from the Euclid Early Release Observations</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.13501">arXiv:2405.13501</a> <span> [<a href="https://arxiv.org/pdf/2405.13501">pdf</a>, <a href="https://arxiv.org/format/2405.13501">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"> Euclid: Early Release Observations -- Overview of the Perseus cluster and analysis of its luminosity and stellar mass functions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cuillandre%2C+J+-">J. -C. Cuillandre</a>, <a href="/search/astro-ph?searchtype=author&query=Bolzonella%2C+M">M. Bolzonella</a>, <a href="/search/astro-ph?searchtype=author&query=Boselli%2C+A">A. Boselli</a>, <a href="/search/astro-ph?searchtype=author&query=Marleau%2C+F+R">F. R. Marleau</a>, <a href="/search/astro-ph?searchtype=author&query=Mondelin%2C+M">M. Mondelin</a>, <a href="/search/astro-ph?searchtype=author&query=Sorce%2C+J+G">J. G. Sorce</a>, <a href="/search/astro-ph?searchtype=author&query=Stone%2C+C">C. Stone</a>, <a href="/search/astro-ph?searchtype=author&query=Buitrago%2C+F">F. Buitrago</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=George%2C+K">K. George</a>, <a href="/search/astro-ph?searchtype=author&query=Hatch%2C+N+A">N. A. Hatch</a>, <a href="/search/astro-ph?searchtype=author&query=Quilley%2C+L">L. Quilley</a>, <a href="/search/astro-ph?searchtype=author&query=Mannucci%2C+F">F. Mannucci</a>, <a href="/search/astro-ph?searchtype=author&query=Saifollahi%2C+T">T. Saifollahi</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">R. S谩nchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Tarsitano%2C+F">F. Tarsitano</a>, <a href="/search/astro-ph?searchtype=author&query=Tortora%2C+C">C. Tortora</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+X">X. Xu</a>, <a href="/search/astro-ph?searchtype=author&query=Bouy%2C+H">H. Bouy</a>, <a href="/search/astro-ph?searchtype=author&query=Gwyn%2C+S">S. Gwyn</a>, <a href="/search/astro-ph?searchtype=author&query=Kluge%2C+M">M. Kluge</a>, <a href="/search/astro-ph?searchtype=author&query=Lan%C3%A7on%2C+A">A. Lan莽on</a>, <a href="/search/astro-ph?searchtype=author&query=Laureijs%2C+R">R. Laureijs</a>, <a href="/search/astro-ph?searchtype=author&query=Schirmer%2C+M">M. Schirmer</a>, <a href="/search/astro-ph?searchtype=author&query=Abdurro%27uf"> Abdurro'uf</a> , et al. (177 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.13501v1-abstract-short" style="display: inline;"> The Euclid ERO programme targeted the Perseus cluster of galaxies, gathering deep data in the central region of the cluster over 0.7 square degree, corresponding to approximately 0.25 r_200. The data set reaches a point-source depth of IE=28.0 (YE, JE, HE = 25.3) AB magnitudes at 5 sigma with a 0.16" and 0.48" FWHM, and a surface brightness limit of 30.1 (29.2) mag per square arcsec. The exception… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.13501v1-abstract-full').style.display = 'inline'; document.getElementById('2405.13501v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.13501v1-abstract-full" style="display: none;"> The Euclid ERO programme targeted the Perseus cluster of galaxies, gathering deep data in the central region of the cluster over 0.7 square degree, corresponding to approximately 0.25 r_200. The data set reaches a point-source depth of IE=28.0 (YE, JE, HE = 25.3) AB magnitudes at 5 sigma with a 0.16" and 0.48" FWHM, and a surface brightness limit of 30.1 (29.2) mag per square arcsec. The exceptional depth and spatial resolution of this wide-field multi-band data enable the simultaneous detection and characterisation of both bright and low surface brightness galaxies, along with their globular cluster systems, from the optical to the NIR. This study advances beyond previous analyses of the cluster and enables a range of scientific investigations summarised here. We derive the luminosity and stellar mass functions (LF and SMF) of the Perseus cluster in the Euclid IE band, thanks to supplementary u,g,r,i,z and Halpha data from the CFHT. We adopt a catalogue of 1100 dwarf galaxies, detailed in the corresponding ERO paper. We identify all other sources in the Euclid images and obtain accurate photometric measurements using AutoProf or AstroPhot for 138 bright cluster galaxies, and SourceExtractor for half a million compact sources. Cluster membership for the bright sample is determined by calculating photometric redshifts with Phosphoros. Our LF and SMF are the deepest recorded for the Perseus cluster, highlighting the groundbreaking capabilities of the Euclid telescope. Both the LF and SMF fit a Schechter plus Gaussian model. The LF features a dip at M(IE)=-19 and a faint-end slope of alpha_S = -1.2 to -1.3. The SMF displays a low-mass-end slope of alpha_S = -1.2 to -1.35. These observed slopes are flatter than those predicted for dark matter halos in cosmological simulations, offering significant insights for models of galaxy formation and evolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.13501v1-abstract-full').style.display = 'none'; document.getElementById('2405.13501v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to A&A, 44 pages, 35 figures, Part of the A&A special issue `Euclid on Sky', which contains Euclid key reference papers and first results from the Euclid Early Release Observations</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.13500">arXiv:2405.13500</a> <span> [<a href="https://arxiv.org/pdf/2405.13500">pdf</a>, <a href="https://arxiv.org/format/2405.13500">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"> Euclid: Early Release Observations -- Globular clusters in the Fornax galaxy cluster, from dwarf galaxies to the intracluster field </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Saifollahi%2C+T">T. Saifollahi</a>, <a href="/search/astro-ph?searchtype=author&query=Voggel%2C+K">K. Voggel</a>, <a href="/search/astro-ph?searchtype=author&query=Lan%C3%A7on%2C+A">A. Lan莽on</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Raj%2C+M+A">M. A. Raj</a>, <a href="/search/astro-ph?searchtype=author&query=Cuillandre%2C+J+-">J. -C. Cuillandre</a>, <a href="/search/astro-ph?searchtype=author&query=Larsen%2C+S+S">S. S. Larsen</a>, <a href="/search/astro-ph?searchtype=author&query=Marleau%2C+F+R">F. R. Marleau</a>, <a href="/search/astro-ph?searchtype=author&query=Venhola%2C+A">A. Venhola</a>, <a href="/search/astro-ph?searchtype=author&query=Schirmer%2C+M">M. Schirmer</a>, <a href="/search/astro-ph?searchtype=author&query=Carollo%2C+D">D. Carollo</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P+-">P. -A. Duc</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+A+M+N">A. M. N. Ferguson</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=K%C3%BCmmel%2C+M">M. K眉mmel</a>, <a href="/search/astro-ph?searchtype=author&query=Laureijs%2C+R">R. Laureijs</a>, <a href="/search/astro-ph?searchtype=author&query=Marchal%2C+O">O. Marchal</a>, <a href="/search/astro-ph?searchtype=author&query=Nucita%2C+A+A">A. A. Nucita</a>, <a href="/search/astro-ph?searchtype=author&query=Peletier%2C+R+F">R. F. Peletier</a>, <a href="/search/astro-ph?searchtype=author&query=Poulain%2C+M">M. Poulain</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">M. Rejkuba</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">R. S谩nchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Urbano%2C+M">M. Urbano</a>, <a href="/search/astro-ph?searchtype=author&query=Abdurro%27uf"> Abdurro'uf</a>, <a href="/search/astro-ph?searchtype=author&query=Altieri%2C+B">B. Altieri</a> , et al. (174 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.13500v1-abstract-short" style="display: inline;"> We present an analysis of Euclid observations of a 0.5 deg$^2$ field in the central region of the Fornax galaxy cluster that were acquired during the performance verification phase. With these data, we investigate the potential of Euclid for identifying GCs at 20 Mpc, and validate the search methods using artificial GCs and known GCs within the field from the literature. Our analysis of artificial… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.13500v1-abstract-full').style.display = 'inline'; document.getElementById('2405.13500v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.13500v1-abstract-full" style="display: none;"> We present an analysis of Euclid observations of a 0.5 deg$^2$ field in the central region of the Fornax galaxy cluster that were acquired during the performance verification phase. With these data, we investigate the potential of Euclid for identifying GCs at 20 Mpc, and validate the search methods using artificial GCs and known GCs within the field from the literature. Our analysis of artificial GCs injected into the data shows that Euclid's data in $I_{\rm E}$ band is 80% complete at about $I_{\rm E} \sim 26.0$ mag ($M_{V\rm } \sim -5.0$ mag), and resolves GCs as small as $r_{\rm h} = 2.5$ pc. In the $I_{\rm E}$ band, we detect more than 95% of the known GCs from previous spectroscopic surveys and GC candidates of the ACS Fornax Cluster Survey, of which more than 80% are resolved. We identify more than 5000 new GC candidates within the field of view down to $I_{\rm E}$ mag, about 1.5 mag fainter than the typical GC luminosity function turn-over magnitude, and investigate their spatial distribution within the intracluster field. We then focus on the GC candidates around dwarf galaxies and investigate their numbers, stacked luminosity distribution and stacked radial distribution. While the overall GC properties are consistent with those in the literature, an interesting over-representation of relatively bright candidates is found within a small number of relatively GC-rich dwarf galaxies. Our work confirms the capabilities of Euclid data in detecting GCs and separating them from foreground and background contaminants at a distance of 20 Mpc, particularly for low-GC count systems such as dwarf galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.13500v1-abstract-full').style.display = 'none'; document.getElementById('2405.13500v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Paper submitted as part of the A&A special issue `Euclid on Sky', which contains Euclid key reference papers and first results from the Euclid Early Release Observations</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.12518">arXiv:2405.12518</a> <span> [<a href="https://arxiv.org/pdf/2405.12518">pdf</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> <p class="title is-5 mathjax"> WST -- Widefield Spectroscopic Telescope: Motivation, science drivers and top-level requirements for a new dedicated facility </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bacon%2C+R">Roland Bacon</a>, <a href="/search/astro-ph?searchtype=author&query=Maineiri%2C+V">Vincenzo Maineiri</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">Sofia Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Cimatti%2C+A">Andrea Cimatti</a>, <a href="/search/astro-ph?searchtype=author&query=Kneib%2C+J">Jean-Paul Kneib</a>, <a href="/search/astro-ph?searchtype=author&query=Brinchmann%2C+J">Jarle Brinchmann</a>, <a href="/search/astro-ph?searchtype=author&query=Ellis%2C+R">Richard Ellis</a>, <a href="/search/astro-ph?searchtype=author&query=Tolstoi%2C+E">Eline Tolstoi</a>, <a href="/search/astro-ph?searchtype=author&query=Smiljanic%2C+R">Rodolfo Smiljanic</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+V">Vanessa Hill</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+R">Richard Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Saez%2C+P+S">Paula Sanchez Saez</a>, <a href="/search/astro-ph?searchtype=author&query=Opitom%2C+C">Cyrielle Opitom</a>, <a href="/search/astro-ph?searchtype=author&query=Bryson%2C+I">Ian Bryson</a>, <a href="/search/astro-ph?searchtype=author&query=Dierickx%2C+P">Philippe Dierickx</a>, <a href="/search/astro-ph?searchtype=author&query=Garilli%2C+B">Bianca Garilli</a>, <a href="/search/astro-ph?searchtype=author&query=Gonzalez%2C+O">Oscar Gonzalez</a>, <a href="/search/astro-ph?searchtype=author&query=de+Jong%2C+R">Roelof de Jong</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+D">David Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Mieske%2C+S">Steffen Mieske</a>, <a href="/search/astro-ph?searchtype=author&query=Otarola%2C+A">Angel Otarola</a>, <a href="/search/astro-ph?searchtype=author&query=Schipani%2C+P">Pietro Schipani</a>, <a href="/search/astro-ph?searchtype=author&query=Travouillon%2C+T">Tony Travouillon</a>, <a href="/search/astro-ph?searchtype=author&query=Vernet%2C+J">Joel Vernet</a>, <a href="/search/astro-ph?searchtype=author&query=Bryant%2C+J">Julia Bryant</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="2405.12518v2-abstract-short" style="display: inline;"> In this paper, we describe the wide-field spectroscopic survey telescope (WST) project. WST is a 12-metre wide-field spectroscopic survey telescope with simultaneous operation of a large field-of-view (3 sq. degree), high-multiplex (20,000) multi-object spectrograph (MOS), with both a low and high-resolution modes, and a giant 3x3 arcmin2 integral field spectrograph (IFS). In scientific capability… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.12518v2-abstract-full').style.display = 'inline'; document.getElementById('2405.12518v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.12518v2-abstract-full" style="display: none;"> In this paper, we describe the wide-field spectroscopic survey telescope (WST) project. WST is a 12-metre wide-field spectroscopic survey telescope with simultaneous operation of a large field-of-view (3 sq. degree), high-multiplex (20,000) multi-object spectrograph (MOS), with both a low and high-resolution modes, and a giant 3x3 arcmin2 integral field spectrograph (IFS). In scientific capability, these specifications place WST far ahead of existing and planned facilities. In only 5 years of operation, the MOS would target 250 million galaxies and 25 million stars at low spectral resolution, plus 2 million stars at high resolution. Without need for pre-imaged targets, the IFS would deliver 4 billion spectra offering many serendipitous discoveries. 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 in synergy with future ground and space-based facilities. We show how it can address outstanding scientific questions in the areas of cosmology; galaxy assembly, evolution, and enrichment, including our own Milky Way; the origin of stars and planets; and time domain and multi-messenger astrophysics. WST's uniquely rich dataset may yield unforeseen discoveries in many of these areas. The telescope and instruments are designed as an integrated system and will mostly use existing technology, with the aim to minimise the carbon footprint and environmental impact. We will propose WST as the next European Southern Observatory (ESO) project after completion of the 39-metre ELT. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.12518v2-abstract-full').style.display = 'none'; document.getElementById('2405.12518v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 15 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/2403.16235">arXiv:2403.16235</a> <span> [<a href="https://arxiv.org/pdf/2403.16235">pdf</a>, <a href="https://arxiv.org/format/2403.16235">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 Next Generation Virgo Cluster Survey (NGVS). III. A Catalog of Surface Brightness Fluctuation Distances and the Three-Dimensional Distribution of Galaxies in the Virgo Cluster </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=C%C3%B4t%C3%A9%2C+P">Patrick C么t茅</a>, <a href="/search/astro-ph?searchtype=author&query=Raimondo%2C+G">Gabriella Raimondo</a>, <a href="/search/astro-ph?searchtype=author&query=Cuillandre%2C+J">Jean-Charles Cuillandre</a>, <a href="/search/astro-ph?searchtype=author&query=Durrell%2C+P+R">Patrick R. Durrell</a>, <a href="/search/astro-ph?searchtype=author&query=Gwyn%2C+S">Stephen Gwyn</a>, <a href="/search/astro-ph?searchtype=author&query=Hazra%2C+N">Nandini Hazra</a>, <a href="/search/astro-ph?searchtype=author&query=Peng%2C+E+W">Eric W. Peng</a>, <a href="/search/astro-ph?searchtype=author&query=Roediger%2C+J+C">Joel C. Roediger</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">R煤ben S谩nchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Kurzner%2C+M">Max Kurzner</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.16235v1-abstract-short" style="display: inline;"> The surface brightness fluctuation (SBF) method is a robust and efficient way of measuring distances to galaxies containing evolved stellar populations. Although many recent applications of the method have used space-based imaging, SBF remains a powerful technique for ground-based telescopes. Deep, wide-field imaging surveys with subarsecond seeing enable SBF measurements for numerous nearby galax… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.16235v1-abstract-full').style.display = 'inline'; document.getElementById('2403.16235v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.16235v1-abstract-full" style="display: none;"> The surface brightness fluctuation (SBF) method is a robust and efficient way of measuring distances to galaxies containing evolved stellar populations. Although many recent applications of the method have used space-based imaging, SBF remains a powerful technique for ground-based telescopes. Deep, wide-field imaging surveys with subarsecond seeing enable SBF measurements for numerous nearby galaxies. Using a preliminary calibration, Cantiello et al. (2018) presented SBF distances for 89 bright, mainly early-type galaxies observed in the Next Generation Virgo Cluster Survey (NGVS). Here, we present a refined calibration and SBF distances for 278 galaxies extending several magnitudes fainter than in previous work. The derived distances have uncertainties of 5-12\% depending on the properties of the individual galaxies, and our sample is more than three times larger than any previous SBF study of this region. Virgo has a famously complex structure with numerous subclusters, clouds and groups; we associate individual galaxies with the various substructures and map their three-dimensional spatial distribution. Curiously, subcluster A, centered around M87, appears to have two peaks in distance: the main peak at $\sim$16.5 Mpc and a smaller one at $\sim$19.4 Mpc. Subclusters B and C have distances of $\sim$15.8 Mpc. The W and W' groups form a filament-like structure, extending more than 15~Mpc behind the cluster with a commensurate velocity increase of $\sim$1000 \kms\ along its length. These measurements are a valuable resource for future studies of the relationship between galaxy properties and local environment within a dynamic and evolving region. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.16235v1-abstract-full').style.display = 'none'; document.getElementById('2403.16235v1-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 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">30 pages, 15 figures, Acccepted for publication on the 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/2403.14847">arXiv:2403.14847</a> <span> [<a href="https://arxiv.org/pdf/2403.14847">pdf</a>, <a href="https://arxiv.org/format/2403.14847">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"> NSCs from groups to clusters: A catalogue of dwarf galaxies in the Shapley Supercluster and the role of environment in galaxy nucleation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zanatta%2C+E+J+B">Emilio J. B. Zanatta</a>, <a href="/search/astro-ph?searchtype=author&query=Sanch%C3%A9z-Janssen%2C+R">Ruben Sanch茅z-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=de+Souza%2C+R+S">Rafael S. de Souza</a>, <a href="/search/astro-ph?searchtype=author&query=Chies-Santos%2C+A+L">Ana L. Chies-Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.14847v1-abstract-short" style="display: inline;"> Nuclear star clusters (NSCs) are dense star clusters located at the centre of galaxies spanning a wide range of masses and morphologies. Analysing NSC occupation statistics in different environments provides an invaluable window into investigating early conditions of high-density star formation and mass assembly in clusters and group galaxies. We use HST/ACS deep imaging to obtain a catalogue of d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.14847v1-abstract-full').style.display = 'inline'; document.getElementById('2403.14847v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.14847v1-abstract-full" style="display: none;"> Nuclear star clusters (NSCs) are dense star clusters located at the centre of galaxies spanning a wide range of masses and morphologies. Analysing NSC occupation statistics in different environments provides an invaluable window into investigating early conditions of high-density star formation and mass assembly in clusters and group galaxies. We use HST/ACS deep imaging to obtain a catalogue of dwarf galaxies in two galaxy clusters in the Shapley Supercluster: the central cluster Abell 3558 and the northern Abell 1736a. The Shapley region is an ideal laboratory to study nucleation as it stands as the highest mass concentration in the nearby Universe. We investigate the NSC occurrence in quiescent dwarf galaxies as faint as $M_{I} = -10$ mag and compare it with all other environments where nucleation data is available. We use galaxy cluster/group halo mass as a proxy for the environment and employ a Bayesian logistic regression framework to model the nucleation fraction ($f_{n}$) as a function of galaxy luminosity and environment. We find a notably high $f_n$ in Abell 3558: at $M_{I} \approx -13.1$ mag, half the galaxies in the cluster host NSCs. This is higher than in the Virgo and Fornax clusters but comparable to the Coma Cluster. On the other hand, the $f_n$ in Abell 1736a is relatively lower, comparable to groups in the Local Volume. We find that the probability of nucleation varies with galaxy luminosity remarkably similarly in galaxy clusters. These results reinforce previous findings of the important role of the environment in NSC formation/growth. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.14847v1-abstract-full').style.display = 'none'; document.getElementById('2403.14847v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 March, 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">20 pages, 10 figures, accepted for publication in the 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/2403.09926">arXiv:2403.09926</a> <span> [<a href="https://arxiv.org/pdf/2403.09926">pdf</a>, <a href="https://arxiv.org/format/2403.09926">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 Next Generation Virgo Cluster Survey (NGVS). XXVII.The Size and Structure of Globular Cluster Systems and their Connection to Dark Matter Halos </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lim%2C+S">Sungsoon Lim</a>, <a href="/search/astro-ph?searchtype=author&query=Peng%2C+E+W">Eric W. Peng</a>, <a href="/search/astro-ph?searchtype=author&query=C%C3%B4t%C3%A9%2C+P">Patrick C么t茅</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrarese%2C+L">Laura Ferrarese</a>, <a href="/search/astro-ph?searchtype=author&query=Roediger%2C+J+C">Joel C. Roediger</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+C">Chengze Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Spengler%2C+C">Chelsea Spengler</a>, <a href="/search/astro-ph?searchtype=author&query=Sola%2C+E">Elisabeth Sola</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P">Pierre-Alain Duc</a>, <a href="/search/astro-ph?searchtype=author&query=Sales%2C+L+V">Laura V. Sales</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Cuillandre%2C+J">Jean-Charles Cuillandre</a>, <a href="/search/astro-ph?searchtype=author&query=Durrell%2C+P+R">Patrick R. Durrell</a>, <a href="/search/astro-ph?searchtype=author&query=Emsellem%2C+E">Eric Emsellem</a>, <a href="/search/astro-ph?searchtype=author&query=Gwyn%2C+S+D+J">Stephen D. J. Gwyn</a>, <a href="/search/astro-ph?searchtype=author&query=Lan%C3%A7on%2C+A">Ariane Lan莽on</a>, <a href="/search/astro-ph?searchtype=author&query=Marleau%2C+F+R">Francine R. Marleau</a>, <a href="/search/astro-ph?searchtype=author&query=Mihos%2C+J+C">J. Christopher Mihos</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%BCller%2C+O">Oliver M眉ller</a>, <a href="/search/astro-ph?searchtype=author&query=Puzia%2C+T+H">Thomas H. Puzia</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">Rub茅n S谩nchez-Janssen</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.09926v1-abstract-short" style="display: inline;"> We study the size and structure of globular clusters (GC) systems of 118 early-type galaxies from the NGVS, MATLAS, and ACSVCS surveys. Fitting S茅rsic profiles, we investigate the relationship between effective radii of GC systems ($R_{e, \rm gc}$) and galaxy properties. GC systems are 2--4 times more extended than host galaxies across the entire stellar mass range of our sample (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.09926v1-abstract-full').style.display = 'inline'; document.getElementById('2403.09926v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.09926v1-abstract-full" style="display: none;"> We study the size and structure of globular clusters (GC) systems of 118 early-type galaxies from the NGVS, MATLAS, and ACSVCS surveys. Fitting S茅rsic profiles, we investigate the relationship between effective radii of GC systems ($R_{e, \rm gc}$) and galaxy properties. GC systems are 2--4 times more extended than host galaxies across the entire stellar mass range of our sample ($10^{8.3} < M_* < 10^{11.6}~M_{\odot}$). The relationship between $R_{e, \rm gc}$ and galaxy stellar mass exhibits a characteristic "knee" at a stellar mass of $M_p \simeq 10^{10.8}$, similar to galaxy $R_e$--stellar mass relationship. We present a new characterization of the traditional blue and red GC color sub-populations, describing them with respect to host galaxy $(g'-i')$ color ($螖_{gi}$): GCs with similar colors to their hosts have a "red" $螖_{gi}$, and those significantly bluer GCs have a "blue" $螖_{gi}$. The GC populations with red $螖_{gi}$, even in dwarf galaxies, are twice as extended as the stars, suggesting that formation or survival mechanisms favor the outer regions. We find a tight correlation between $R_{e, \rm gc}$ and the total number of GCs, with intrinsic scatter $\lesssim 0.1$ dex spanning two and three orders of magnitude in size and number, respectively. This holds for both red and blue subpopulations, albeit with different slopes. Assuming that $N_{GC, Total}$ correlates with $M_{200}$, we find that the red GC systems have effective radii of roughly 1-5\% $R_{\rm 200}$, while the blue GC systems in massive galaxies can have sizes as large as $\sim$10\% $R_{\rm 200}$. Environmental dependence on $R_{e, \rm gc}$ is also found, with lower density environments exhibiting more extended GC systems at fixed mass. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.09926v1-abstract-full').style.display = 'none'; document.getElementById('2403.09926v1-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 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">28 pages, 18 Figures, 3 tables, accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/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/2402.12033">arXiv:2402.12033</a> <span> [<a href="https://arxiv.org/pdf/2402.12033">pdf</a>, <a href="https://arxiv.org/format/2402.12033">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"> Constraining the stellar populations of ultra-diffuse galaxies in the MATLAS survey using spectral energy distribution fitting </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Buzzo%2C+M+L">Maria Luisa Buzzo</a>, <a href="/search/astro-ph?searchtype=author&query=Forbes%2C+D+A">Duncan A. Forbes</a>, <a href="/search/astro-ph?searchtype=author&query=Jarrett%2C+T+H">Thomas H. Jarrett</a>, <a href="/search/astro-ph?searchtype=author&query=Marleau%2C+F+R">Francine R. Marleau</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P">Pierre-Alain Duc</a>, <a href="/search/astro-ph?searchtype=author&query=Brodie%2C+J+P">Jean P. Brodie</a>, <a href="/search/astro-ph?searchtype=author&query=Romanowsky%2C+A+J">Aaron J. Romanowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Gannon%2C+J+S">Jonah S. Gannon</a>, <a href="/search/astro-ph?searchtype=author&query=Janssens%2C+S+R">Steven R. Janssens</a>, <a href="/search/astro-ph?searchtype=author&query=Pfeffer%2C+J">Joel Pfeffer</a>, <a href="/search/astro-ph?searchtype=author&query=Ferr%C3%A9-Mateu%2C+A">Anna Ferr茅-Mateu</a>, <a href="/search/astro-ph?searchtype=author&query=Haacke%2C+L">Lydia Haacke</a>, <a href="/search/astro-ph?searchtype=author&query=Couch%2C+W+J">Warrick J. Couch</a>, <a href="/search/astro-ph?searchtype=author&query=Lim%2C+S">Sungsoon Lim</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">Rub茅n S谩nchez-Janssen</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2402.12033v1-abstract-short" style="display: inline;"> We use spectral energy distribution (SED) fitting to place constraints on the stellar populations of 59 ultra-diffuse galaxies (UDGs) in the low-to-moderate density fields of the MATLAS survey. We use the routine PROSPECTOR, coupled with archival data in the optical from DECaLS, and near- and mid-infrared imaging from WISE, to recover the stellar masses, ages, metallicities and star formation time… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.12033v1-abstract-full').style.display = 'inline'; document.getElementById('2402.12033v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.12033v1-abstract-full" style="display: none;"> We use spectral energy distribution (SED) fitting to place constraints on the stellar populations of 59 ultra-diffuse galaxies (UDGs) in the low-to-moderate density fields of the MATLAS survey. We use the routine PROSPECTOR, coupled with archival data in the optical from DECaLS, and near- and mid-infrared imaging from WISE, to recover the stellar masses, ages, metallicities and star formation timescales of the UDGs. We find that a subsample of the UDGs lies within the scatter of the mass-metallicity relation (MZR) for local classical dwarfs. However, another subsample is more metal-poor, being consistent with the evolving MZR at high-redshift. We investigate UDG positioning trends in the mass-metallicity plane as a function of surface brightness, effective radius, axis ratio, local volume density, mass-weighted age, star formation timescale, globular cluster (GC) counts and GC specific frequency. We find that our sample of UDGs can be separated into two main classes. Class A: Comprised of UDGs with lower stellar masses, prolonged star formation histories (SFHs), more elongated, inhabiting less dense environments, hosting fewer GCs, younger, consistent with the classical dwarf MZR, and fainter. Class B: UDGs with higher stellar masses, rapid SFHs, rounder, inhabiting the densest of our probed environments, hosting on average the most numerous GC systems, older, consistent with the high-redshift MZR (i.e., consistent with early-quenching), and brighter. The combination of these properties suggests that UDGs of Class A are consistent with a `puffed-up dwarf' formation scenario, while UDGs of Class B seem to be better explained by `failed galaxy' scenarios. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.12033v1-abstract-full').style.display = 'none'; document.getElementById('2402.12033v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in MNRAS. 19 pages (+6 of appendices), 10 figures, 5 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/2311.05448">arXiv:2311.05448</a> <span> [<a href="https://arxiv.org/pdf/2311.05448">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1038/s41586-023-06650-z">10.1038/s41586-023-06650-z <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An evolutionary continuum from nucleated dwarf galaxies to star clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wang%2C+K">Kaixiang Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Peng%2C+E+W">Eric W. Peng</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+C">Chengze Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Mihos%2C+J+C">J. Christopher Mihos</a>, <a href="/search/astro-ph?searchtype=author&query=C%C3%B4t%C3%A9%2C+P">Patrick C么t茅</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrarese%2C+L">Laura Ferrarese</a>, <a href="/search/astro-ph?searchtype=author&query=Taylor%2C+M+A">Matthew A. Taylor</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Cuillandre%2C+J">Jean-Charles Cuillandre</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P">Pierre-Alain Duc</a>, <a href="/search/astro-ph?searchtype=author&query=Guhathakurta%2C+P">Puragra Guhathakurta</a>, <a href="/search/astro-ph?searchtype=author&query=Gwyn%2C+S">Stephen Gwyn</a>, <a href="/search/astro-ph?searchtype=author&query=Ko%2C+Y">Youkyung Ko</a>, <a href="/search/astro-ph?searchtype=author&query=Lan%C3%A7on%2C+A">Ariane Lan莽on</a>, <a href="/search/astro-ph?searchtype=author&query=Lim%2C+S">Sungsoon Lim</a>, <a href="/search/astro-ph?searchtype=author&query=MacArthur%2C+L+A">Lauren A. MacArthur</a>, <a href="/search/astro-ph?searchtype=author&query=Puzia%2C+T">Thomas Puzia</a>, <a href="/search/astro-ph?searchtype=author&query=Roediger%2C+J">Joel Roediger</a>, <a href="/search/astro-ph?searchtype=author&query=Sales%2C+L+V">Laura V. Sales</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">Rub茅n S谩nchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Spengler%2C+C">Chelsea Spengler</a>, <a href="/search/astro-ph?searchtype=author&query=Toloba%2C+E">Elisa Toloba</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+H">Hongxin Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhu%2C+M">Mingcheng 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="2311.05448v1-abstract-short" style="display: inline;"> Systematic studies have revealed hundreds of ultra-compact dwarf galaxies (UCDs) in the nearby Universe. With half-light radii $r_h$ of approximately 10-100 parsecs and stellar masses $M_*$ $\approx$ $10^6-10^8$ solar masses, UCDs are among the densest known stellar systems. Although similar in appearance to massive globular clusters, the detection of extended stellar envelopes, complex star forma… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.05448v1-abstract-full').style.display = 'inline'; document.getElementById('2311.05448v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.05448v1-abstract-full" style="display: none;"> Systematic studies have revealed hundreds of ultra-compact dwarf galaxies (UCDs) in the nearby Universe. With half-light radii $r_h$ of approximately 10-100 parsecs and stellar masses $M_*$ $\approx$ $10^6-10^8$ solar masses, UCDs are among the densest known stellar systems. Although similar in appearance to massive globular clusters, the detection of extended stellar envelopes, complex star formation histories, elevated mass-to-light ratio, and supermassive black holes suggest that some UCDs are remnant nuclear star clusters of tidally-stripped dwarf galaxies, or even ancient compact galaxies. However, only a few objects have been found in the transient stage of tidal stripping, and this assumed evolutionary path has never been fully traced by observations. Here we show that 106 galaxies in the Virgo cluster have morphologies that are intermediate between normal, nucleated dwarf galaxies and single-component UCDs, revealing a continuum that fully maps this morphological transition, and fills the `size gap' between star clusters and galaxies. Their spatial distribution and redder color are also consistent with stripped satellite galaxies on their first few pericentric passages around massive galaxies. The `ultra-diffuse' tidal features around several of these galaxies directly show how UCDs are forming through tidal stripping, and that this evolutionary path can include an early phase as a nucleated ultra-diffuse galaxy (UDG). These UCDs represent substantial visible fossil remnants of ancient dwarf galaxies in galaxy clusters, and more low-mass remnants probably remain to be found. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.05448v1-abstract-full').style.display = 'none'; document.getElementById('2311.05448v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published in Nature. Accepted on September 15</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nature 623 (2023) 296-300 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.08098">arXiv:2309.08098</a> <span> [<a href="https://arxiv.org/pdf/2309.08098">pdf</a>, <a href="https://arxiv.org/format/2309.08098">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnrasl/slad126">10.1093/mnrasl/slad126 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The creation of a massive UCD by tidal threshing from NGC 936 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Paudel%2C+S">Sanjaya Paudel</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P">Pierre-Alain Duc</a>, <a href="/search/astro-ph?searchtype=author&query=Lim%2C+S">Sungsoon Lim</a>, <a href="/search/astro-ph?searchtype=author&query=Poulain%2C+M">M茅lina Poulain</a>, <a href="/search/astro-ph?searchtype=author&query=Marleau%2C+F+R">Francine R. Marleau</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%BCller%2C+O">Oliver M眉ller</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">Rub茅n S谩nchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Habas%2C+R">Rebecca Habas</a>, <a href="/search/astro-ph?searchtype=author&query=Durrell%2C+P+R">Patrick R. Durrell</a>, <a href="/search/astro-ph?searchtype=author&query=Heesters%2C+N">Nick Heesters</a>, <a href="/search/astro-ph?searchtype=author&query=Chhatkuli%2C+D+N">Daya Nidhi Chhatkuli</a>, <a href="/search/astro-ph?searchtype=author&query=Yoon%2C+S">Suk-Jin Yoon</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="2309.08098v1-abstract-short" style="display: inline;"> We study a compact nucleus embedded in an early-type dwarf galaxy, MATLAS-167, which is in the process of disruption by the tidal force of the neighboring giant S0 galaxy, NGC 936, in a group environment. Using the imaging data of the MATLAS survey, we analyze the stellar tidal tail of MATLAS-167 and its central compact nucleus, designated as NGC 936_UCD. We find that NGC 936_UCD has a luminosity… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.08098v1-abstract-full').style.display = 'inline'; document.getElementById('2309.08098v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.08098v1-abstract-full" style="display: none;"> We study a compact nucleus embedded in an early-type dwarf galaxy, MATLAS-167, which is in the process of disruption by the tidal force of the neighboring giant S0 galaxy, NGC 936, in a group environment. Using the imaging data of the MATLAS survey, we analyze the stellar tidal tail of MATLAS-167 and its central compact nucleus, designated as NGC 936_UCD. We find that NGC 936_UCD has a luminosity of M$_{g}$ = $-$11.43$\pm$0.01 mag and a size of 66.5$\pm$17 pc, sharing the global properties of Ultra Compact Dwarf galaxies (UCDs) but significantly larger and brighter compared to the typical UCD populations observed in the Virgo cluster. By integrating the total luminosity of both the tidal stream and MATLAS-167, we estimate that the disrupted dwarf progenitor possesses a luminosity of M$_{g}$ = $-$15.92$\pm$0.06 mag, a typical bright dE luminosity. With the help of the optical spectrum observed by the SDSS survey, we derive the simple stellar population properties of NGC 936_UCD: a light-weighted age of 5.6$\pm$0.7 Gyr and metallicity of [Z/H] = $-$0.83$\pm$0.3 dex. Our findings suggest that tidal threshing is a possible formation mechanism of bright UCD populations in close proximity to giant galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.08098v1-abstract-full').style.display = 'none'; document.getElementById('2309.08098v1-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 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in 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/2305.04593">arXiv:2305.04593</a> <span> [<a href="https://arxiv.org/pdf/2305.04593">pdf</a>, <a href="https://arxiv.org/format/2305.04593">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/10.1051/0004-6361/202346441">10.1051/0004-6361/202346441 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Radial velocities and stellar population properties of 56 MATLAS dwarf galaxies observed with MUSE </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Heesters%2C+N">Nick Heesters</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%BCller%2C+O">Oliver M眉ller</a>, <a href="/search/astro-ph?searchtype=author&query=Marleau%2C+F+R">Francine R. Marleau</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P">Pierre-Alain Duc</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">Rub茅n S谩nchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Poulain%2C+M">M茅lina Poulain</a>, <a href="/search/astro-ph?searchtype=author&query=Habas%2C+R">Rebecca Habas</a>, <a href="/search/astro-ph?searchtype=author&query=Lim%2C+S">Sungsoon Lim</a>, <a href="/search/astro-ph?searchtype=author&query=Durrell%2C+P+R">Patrick R. Durrell</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2305.04593v1-abstract-short" style="display: inline;"> Dwarf galaxies have been extensively studied in the Local Group, in nearby groups, and selected clusters, giving us a robust picture of their global stellar and dynamical properties in particular locations in the Universe. Intense study of these properties has revealed correlations between them, including the well known universal stellar mass-metallicity relation. However, since dwarfs play a role… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.04593v1-abstract-full').style.display = 'inline'; document.getElementById('2305.04593v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.04593v1-abstract-full" style="display: none;"> Dwarf galaxies have been extensively studied in the Local Group, in nearby groups, and selected clusters, giving us a robust picture of their global stellar and dynamical properties in particular locations in the Universe. Intense study of these properties has revealed correlations between them, including the well known universal stellar mass-metallicity relation. However, since dwarfs play a role in a vast range of different environments, much can be learned about galaxy formation and evolution through extending the study of these objects to various locations. We present MUSE spectroscopy of a sample of 56 dwarf galaxies as a follow-up to the MATLAS survey in low-to-moderate density environments beyond the Local Volume. The dwarfs have stellar masses in the range of $M_{*}/M_{\odot}$ = 10$^{6.1}$-10$^{9.4}$ and show a distance range of D = 14-148 Mpc, the majority (75%) of which are located in the range targeted by the MATLAS survey (10-45 Mpc). We thus report a 75% (79% for dwarf ellipticals) success rate for the semi-automatic identification of dwarf galaxies in the MATLAS survey on the here presented subsample. Using pPXF full spectrum fitting, we determine their line-of-sight velocity and can match the majority of them with their massive host galaxy. Close inspection of their spectra reveals that ~30% show clear emission lines and thus star formation activity. We estimate their stellar population properties (age and metallicity) and compare our results with other works investigating Local Volume and cluster dwarf galaxies. We find that the dwarf galaxies presented in this work show a systematic offset from the stellar mass-metallicity relation towards lower metallicities at the same stellar mass. A similar deviation is present in other works in the stellar mass range probed in this work and might be attributed to the use of different methodologies for deriving the metallicity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.04593v1-abstract-full').style.display = 'none'; document.getElementById('2305.04593v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 15 figures, 1 table. Accepted for publication in Astronomy & Astrophysics, Abstract shortened due to arxiv abstract length requirements</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 676, A33 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.13046">arXiv:2304.13046</a> <span> [<a href="https://arxiv.org/pdf/2304.13046">pdf</a>, <a href="https://arxiv.org/format/2304.13046">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 Pristine Dwarf-Galaxy survey -- V. The edges of the dwarf galaxy Hercules </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Longeard%2C+N">Nicolas Longeard</a>, <a href="/search/astro-ph?searchtype=author&query=Jablonka%2C+P">Pascale Jablonka</a>, <a href="/search/astro-ph?searchtype=author&query=Battaglia%2C+G">Giuseppina Battaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Malhan%2C+K">Khyati Malhan</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+N">Nicolas Martin</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">Rub茅n S谩nchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Sestito%2C+F">Federico Sestito</a>, <a href="/search/astro-ph?searchtype=author&query=Starkenburg%2C+E">Else Starkenburg</a>, <a href="/search/astro-ph?searchtype=author&query=Venn%2C+K+A">Kim A. Venn</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="2304.13046v1-abstract-short" style="display: inline;"> We present a new spectroscopic study of the dwarf galaxy Hercules (d ~ 132 kpc) with data from the Anglo-Australian Telescope and its AAOmega spectrograph together with the Two Degree Field multi-object system to solve the conundrum that whether Hercules is tidally disrupting. We combine broadband photometry, proper motions from Gaia, and our Pristine narrow-band and metallicity-sensitive photomet… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.13046v1-abstract-full').style.display = 'inline'; document.getElementById('2304.13046v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.13046v1-abstract-full" style="display: none;"> We present a new spectroscopic study of the dwarf galaxy Hercules (d ~ 132 kpc) with data from the Anglo-Australian Telescope and its AAOmega spectrograph together with the Two Degree Field multi-object system to solve the conundrum that whether Hercules is tidally disrupting. We combine broadband photometry, proper motions from Gaia, and our Pristine narrow-band and metallicity-sensitive photometry to efficiently weed out the Milky Way contamination. Such cleaning is particularly critical in this kinematic regime, as both the transverse and heliocentric velocities of Milky Way populations overlap with Hercules. Thanks to this method, three new member stars are identified, including one at almost 10rh of the satellite. All three have velocities and metallicities consistent with that of the main body. Combining this new dataset with the entire literature cleaned out from contamination shows that Hercules does not exhibit a velocity gradient (d<v>/dX = 0.1+0.4/-0.2 km s-1 arcmin-1) and, as such, does not show evidence to undergo tidal disruption. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.13046v1-abstract-full').style.display = 'none'; document.getElementById('2304.13046v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.14375">arXiv:2302.14375</a> <span> [<a href="https://arxiv.org/pdf/2302.14375">pdf</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> </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/10.18727/0722-6691/5286">10.18727/0722-6691/5286 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The ESO's Extremely Large Telescope Working Groups </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Padovani%2C+P">Paolo Padovani</a>, <a href="/search/astro-ph?searchtype=author&query=Cirasuolo%2C+M">Michele Cirasuolo</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Burg%2C+R">Remco van der Burg</a>, <a href="/search/astro-ph?searchtype=author&query=Cantalloube%2C+F">Faustine Cantalloube</a>, <a href="/search/astro-ph?searchtype=author&query=George%2C+E">Elizabeth George</a>, <a href="/search/astro-ph?searchtype=author&query=Kasper%2C+M">Markus Kasper</a>, <a href="/search/astro-ph?searchtype=author&query=Leschinski%2C+K">Kieran Leschinski</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+C">Carlos Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Milli%2C+J">Julien Milli</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%B6hler%2C+S">Sabine M枚hler</a>, <a href="/search/astro-ph?searchtype=author&query=Neeser%2C+M">Mark Neeser</a>, <a href="/search/astro-ph?searchtype=author&query=Neichel%2C+B">Benoit Neichel</a>, <a href="/search/astro-ph?searchtype=author&query=Otarola%2C+A">Angel Otarola</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">Rub茅n S谩nchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Serra%2C+B">Benoit Serra</a>, <a href="/search/astro-ph?searchtype=author&query=Smette%2C+A">Alain Smette</a>, <a href="/search/astro-ph?searchtype=author&query=Valenti%2C+E">Elena Valenti</a>, <a href="/search/astro-ph?searchtype=author&query=Verinaud%2C+C">Christophe Verinaud</a>, <a href="/search/astro-ph?searchtype=author&query=Vernet%2C+J">Jo毛l Vernet</a>, <a href="/search/astro-ph?searchtype=author&query=Absil%2C+O">Olivier Absil</a>, <a href="/search/astro-ph?searchtype=author&query=Agapito%2C+G">Guido Agapito</a>, <a href="/search/astro-ph?searchtype=author&query=Andersen%2C+M">Morten Andersen</a>, <a href="/search/astro-ph?searchtype=author&query=Arcidiacono%2C+C">Carmelo Arcidiacono</a>, <a href="/search/astro-ph?searchtype=author&query=Arko%2C+M">Matej Arko</a>, <a href="/search/astro-ph?searchtype=author&query=Baudoz%2C+P">Pierre Baudoz</a> , et al. (60 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="2302.14375v1-abstract-short" style="display: inline;"> Since 2005 ESO has been working with its community and industry to develop an extremely large optical/infrared telescope. ESO's Extremely Large Telescope, or ELT for short, is a revolutionary ground-based telescope that will have a 39-metre main mirror and will be the largest visible and infrared light telescope in the world. To address specific topics that are needed for the science operations an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.14375v1-abstract-full').style.display = 'inline'; document.getElementById('2302.14375v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.14375v1-abstract-full" style="display: none;"> Since 2005 ESO has been working with its community and industry to develop an extremely large optical/infrared telescope. ESO's Extremely Large Telescope, or ELT for short, is a revolutionary ground-based telescope that will have a 39-metre main mirror and will be the largest visible and infrared light telescope in the world. To address specific topics that are needed for the science operations and calibrations of the telescope, thirteen specific working groups were created to coordinate the effort between ESO, the instrument consortia, and the wider community. We describe here the goals of these working groups as well as their achievements so far. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.14375v1-abstract-full').style.display = 'none'; document.getElementById('2302.14375v1-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 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">8 pages, 4 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Messenger, vol. 189, (December 2022) p. 23-30 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.12791">arXiv:2212.12791</a> <span> [<a href="https://arxiv.org/pdf/2212.12791">pdf</a>, <a href="https://arxiv.org/format/2212.12791">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> </div> </div> <p class="title is-5 mathjax"> CUBES: a UV spectrograph for the future </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Covino%2C+S">S. Covino</a>, <a href="/search/astro-ph?searchtype=author&query=Cristiani%2C+S">S. Cristiani</a>, <a href="/search/astro-ph?searchtype=author&query=Alcala%27%2C+J+M">J. M. Alcala'</a>, <a href="/search/astro-ph?searchtype=author&query=Alencar%2C+S+H+P">S. H. P. Alencar</a>, <a href="/search/astro-ph?searchtype=author&query=Balashev%2C+S+A">S. A. Balashev</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">B. Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=Bastian%2C+N">N. Bastian</a>, <a href="/search/astro-ph?searchtype=author&query=Battino%2C+U">U. Battino</a>, <a href="/search/astro-ph?searchtype=author&query=Bissell%2C+L">L. Bissell</a>, <a href="/search/astro-ph?searchtype=author&query=Bristow%2C+P">P. Bristow</a>, <a href="/search/astro-ph?searchtype=author&query=Calcines%2C+A">A. Calcines</a>, <a href="/search/astro-ph?searchtype=author&query=Calderone%2C+G">G. Calderone</a>, <a href="/search/astro-ph?searchtype=author&query=Cambianica%2C+P">P. Cambianica</a>, <a href="/search/astro-ph?searchtype=author&query=Carini%2C+R">R. Carini</a>, <a href="/search/astro-ph?searchtype=author&query=Carter%2C+B">B. Carter</a>, <a href="/search/astro-ph?searchtype=author&query=Cassisi%2C+S">S. Cassisi</a>, <a href="/search/astro-ph?searchtype=author&query=Castilho%2C+B+V">B. V. Castilho</a>, <a href="/search/astro-ph?searchtype=author&query=Cescutti%2C+G">G. Cescutti</a>, <a href="/search/astro-ph?searchtype=author&query=Christlieb%2C+N">N. Christlieb</a>, <a href="/search/astro-ph?searchtype=author&query=Cirami%2C+R">R. Cirami</a>, <a href="/search/astro-ph?searchtype=author&query=Conzelmann%2C+R">R. Conzelmann</a>, <a href="/search/astro-ph?searchtype=author&query=Coretti%2C+I">I. Coretti</a>, <a href="/search/astro-ph?searchtype=author&query=Cooke%2C+R">R. Cooke</a>, <a href="/search/astro-ph?searchtype=author&query=Cremonese%2C+G">G. Cremonese</a>, <a href="/search/astro-ph?searchtype=author&query=Cunha%2C+K">K. Cunha</a> , et al. (64 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="2212.12791v1-abstract-short" style="display: inline;"> In spite of the advent of extremely large telescopes in the UV/optical/NIR range, the current generation of 8-10m facilities is likely to remain competitive at ground-UV wavelengths for the foreseeable future. The Cassegrain U-Band Efficient Spectrograph (CUBES) has been designed to provide high-efficiency (>40%) observations in the near UV (305-400 nm requirement, 300-420 nm goal) at a spectral r… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.12791v1-abstract-full').style.display = 'inline'; document.getElementById('2212.12791v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.12791v1-abstract-full" style="display: none;"> In spite of the advent of extremely large telescopes in the UV/optical/NIR range, the current generation of 8-10m facilities is likely to remain competitive at ground-UV wavelengths for the foreseeable future. The Cassegrain U-Band Efficient Spectrograph (CUBES) has been designed to provide high-efficiency (>40%) observations in the near UV (305-400 nm requirement, 300-420 nm goal) at a spectral resolving power of R>20,000, although a lower-resolution, sky-limited mode of R ~ 7,000 is also planned. CUBES will offer new possibilities in many fields of astrophysics, providing access to key lines of stellar spectra: a tremendous diversity of iron-peak and heavy elements, lighter elements (in particular Beryllium) and light-element molecules (CO, CN, OH), as well as Balmer lines and the Balmer jump (particularly important for young stellar objects). The UV range is also critical in extragalactic studies: the circumgalactic medium of distant galaxies, the contribution of different types of sources to the cosmic UV background, the measurement of H2 and primordial Deuterium in a regime of relatively transparent intergalactic medium, and follow-up of explosive transients. The CUBES project completed a Phase A conceptual design in June 2021 and has now entered the Phase B dedicated to detailed design and construction. First science operations are planned for 2028. In this paper, we briefly describe the CUBES project development and goals, the main science cases, the instrument design and the project organization and management. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.12791v1-abstract-full').style.display = 'none'; document.getElementById('2212.12791v1-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 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">Proceedings for the HACK100 conference, Trieste, June 2022. arXiv admin note: substantial text overlap with arXiv:2208.01672</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.10593">arXiv:2212.10593</a> <span> [<a href="https://arxiv.org/pdf/2212.10593">pdf</a>, <a href="https://arxiv.org/format/2212.10593">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/stad198">10.1093/mnras/stad198 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The resolved chemical composition of the starburst dwarf galaxy CGCG007-025: Direct method versus photoionization model fitting </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez%2C+V">Vital Fern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Amor%C3%ADn%2C+R">Ricardo Amor铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez-Janssen%2C+R">Rub茅n Sanchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=del+Valle-Espinosa%2C+M+G">Macarena Garcia del Valle-Espinosa</a>, <a href="/search/astro-ph?searchtype=author&query=Papaderos%2C+P">Polychronis Papaderos</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2212.10593v1-abstract-short" style="display: inline;"> This work focuses on the gas chemical composition of CGCG007-025. This compact dwarf is undergoing a galaxy wide star forming burst, whose spatial behaviour has been observed by VLT/MUSE. We present a new line measurement library to treat almost 7800 voxels. The direct method chemical analysis is limited to 484 voxels with good detection of the $[SIII]$6312$\mathring{\mathrm{A}}$ temperature diagn… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.10593v1-abstract-full').style.display = 'inline'; document.getElementById('2212.10593v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.10593v1-abstract-full" style="display: none;"> This work focuses on the gas chemical composition of CGCG007-025. This compact dwarf is undergoing a galaxy wide star forming burst, whose spatial behaviour has been observed by VLT/MUSE. We present a new line measurement library to treat almost 7800 voxels. The direct method chemical analysis is limited to 484 voxels with good detection of the $[SIII]$6312$\mathring{\mathrm{A}}$ temperature diagnostic line. The recombination fluxes are corrected for stellar absorption via a population synthesis. Additionally, we discuss a new algorithm to fit photoionization models via neural networks. The 8 ionic abundances analyzed show a spatial normal distribution with a $蟽\sim0.1\,dex$, where only half this value can be explained by the uncertainty in the measurements. The oxygen abundance distribution is $12+log(O/H)=7.88\pm0.11$. The $T_{e}[SIII]$ and $ne[SII]$ are also normally distributed. However, in the central and brightest region, the $ne[SII]$ is almost thrice the mean galaxy value. This is also reflected in the extinction measurements. The ionization parameter has a distribution of $log(U) = -2.52^{0.17}_{0.19}$. The parameter spatial behaviour agrees with the $S^{2+}/S^{+}$ map. Finally, the discrepancies between the direct method and the photoionization model fitting are discussed. In the latter technique, we find that mixing lines with uneven uncertainty magnitudes can impact the accuracy of the results. In these fittings, we recommend overestimating the minimum flux uncertainty one order below the maximum line flux uncertainty. This provides a better match with the direct method. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.10593v1-abstract-full').style.display = 'none'; document.getElementById('2212.10593v1-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, 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">Minor revision of your manuscript is requested before it is reconsidered 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/2212.10585">arXiv:2212.10585</a> <span> [<a href="https://arxiv.org/pdf/2212.10585">pdf</a>, <a href="https://arxiv.org/format/2212.10585">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/stad1087">10.1093/mnras/stad1087 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Spatially-resolved chemodynamics of the starburst dwarf galaxy CGCG 007-025: Evidence for recent accretion of metal-poor gas </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=del+Valle-Espinosa%2C+M+G">M. G. del Valle-Espinosa</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez-Janssen%2C+R">R. Sanchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Amorin%2C+R">R. Amorin</a>, <a href="/search/astro-ph?searchtype=author&query=Fernandez%2C+V">V. Fernandez</a>, <a href="/search/astro-ph?searchtype=author&query=Almeida%2C+J+S">J. Sanchez Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Lorenzo%2C+B+G">B. Garcia Lorenzo</a>, <a href="/search/astro-ph?searchtype=author&query=Papaderos%2C+P">P. Papaderos</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2212.10585v2-abstract-short" style="display: inline;"> Nearby metal-poor starburst dwarf galaxies present a unique opportunity to probe the physics of high-density star formation with a detail and sensitivity unmatched by any observation of the high-z Universe. Here we present the first results from a chemodynamical study of the nearby, gas-rich starburst dwarf CGCG 007-025. We use VLT/MUSE integral field spectroscopy to characterise the properties of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.10585v2-abstract-full').style.display = 'inline'; document.getElementById('2212.10585v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.10585v2-abstract-full" style="display: none;"> Nearby metal-poor starburst dwarf galaxies present a unique opportunity to probe the physics of high-density star formation with a detail and sensitivity unmatched by any observation of the high-z Universe. Here we present the first results from a chemodynamical study of the nearby, gas-rich starburst dwarf CGCG 007-025. We use VLT/MUSE integral field spectroscopy to characterise the properties of the star-forming (SF) gas, from its metal content to its kinematics. The star formation rate (SFR) surface density presents a clumpy distribution, with the brightest knot hosting a 5 Myr young, Wolf-Rayet (WR) population (revealed by the presence of the characteristic 5808脜~WR bump). The ionised gas kinematics are dominated by disordered motions. A superposition of a narrow ($蟽\approx$ 50 km s$^{-1}$), intermediate (150 km s$^{-1}$) and broad (1000 km s$^{-1}$) kinematic components are needed to model the emission line profiles in the brightest SF region, suggesting the presence of energetic outflows from massive stars. The gas-phase metallicity of the galaxy spans 0.6 dex and displays a strong anti-correlation with SFR surface density, dropping to 12+log(O/H) = 7.7 in the central SF knot. The spatially-resolved BPTs indicates the gas is being ionised purely by SF processes. Finally, the anti-correlation between the SFR and the gas metallicity points out to accretion of metal-poor gas as the origin of the recent off-centre starburst, in which the infalling material ignites the SF episode. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.10585v2-abstract-full').style.display = 'none'; document.getElementById('2212.10585v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 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">15 pages, 11 figures, 1 table; published 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/2209.00040">arXiv:2209.00040</a> <span> [<a href="https://arxiv.org/pdf/2209.00040">pdf</a>, <a href="https://arxiv.org/format/2209.00040">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stac2491">10.1093/mnras/stac2491 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Near-infrared spectroscopy of embedded protostars in the massive metal-poor star-forming region NGC 346 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jones%2C+O+C">O. C. Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Reiter%2C+M">M. Reiter</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez-Janssen%2C+R">R. Sanchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+C+J">C. J. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Robertson%2C+C+S">C. S. Robertson</a>, <a href="/search/astro-ph?searchtype=author&query=Meixner%2C+M">M. Meixner</a>, <a href="/search/astro-ph?searchtype=author&query=Ochsendorf%2C+B">B. Ochsendorf</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2209.00040v1-abstract-short" style="display: inline;"> We present medium-resolution (R $\sim$ 4000) YJ, H \& K band spectroscopy of candidate young stellar objects (YSOs) in NGC~346, the most active star-formation region in the metal-poor (Z = 1/5 Z$_{\sun}$) Small Magellanic Cloud. The spectra were obtained with the KMOS (K-Band Multi Object Spectrograph) integral field instrument on the Very Large Telescope. From our initial sample of 18 candidate h… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.00040v1-abstract-full').style.display = 'inline'; document.getElementById('2209.00040v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.00040v1-abstract-full" style="display: none;"> We present medium-resolution (R $\sim$ 4000) YJ, H \& K band spectroscopy of candidate young stellar objects (YSOs) in NGC~346, the most active star-formation region in the metal-poor (Z = 1/5 Z$_{\sun}$) Small Magellanic Cloud. The spectra were obtained with the KMOS (K-Band Multi Object Spectrograph) integral field instrument on the Very Large Telescope. From our initial sample of 18 candidate high-mass YSOs previously identified from mid-IR photometry and radiative transfer model fits to their spectral energy distributions, approximately half were resolved into multiple components by our integral-field data. In total, we detect 30 continuum sources and extract reliable spectra for 12 of these objects. The spectra show various features including hydrogen recombination lines, and lines from H$_2$, He~{\sc i} and [Fe~{\sc ii}], which are indicative of accretion, discs and outflowing material in massive YSOs. We spectroscopically confirm the youthful nature of nine YSO candidates and identify two others as OB stars. All of the confirmed YSOs have Br$纬$ in emission, but no emission is seen from the CO bandhead, despite other disc tracers present in the spectra. He\,{\sc i}~1.083 $渭$m emission is also detected at appreciably higher rates than for the Galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.00040v1-abstract-full').style.display = 'none'; document.getElementById('2209.00040v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 6 figures. Accepted for publication 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/2208.01672">arXiv:2208.01672</a> <span> [<a href="https://arxiv.org/pdf/2208.01672">pdf</a>, <a href="https://arxiv.org/format/2208.01672">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="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> CUBES, the Cassegrain U-Band Efficient Spectrograph </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cristiani%2C+S">S. Cristiani</a>, <a href="/search/astro-ph?searchtype=author&query=Alcal%C3%A1%2C+J+M">J. M. Alcal谩</a>, <a href="/search/astro-ph?searchtype=author&query=Alencar%2C+S+H+P">S. H. P. Alencar</a>, <a href="/search/astro-ph?searchtype=author&query=Balashev%2C+S+A">S. A. Balashev</a>, <a href="/search/astro-ph?searchtype=author&query=Bastian%2C+N">N. Bastian</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">B. Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=Battino%2C+U">U. Battino</a>, <a href="/search/astro-ph?searchtype=author&query=Calcines%2C+A">A. Calcines</a>, <a href="/search/astro-ph?searchtype=author&query=Calderone%2C+G">G. Calderone</a>, <a href="/search/astro-ph?searchtype=author&query=Cambianica%2C+P">P. Cambianica</a>, <a href="/search/astro-ph?searchtype=author&query=Carini%2C+R">R. Carini</a>, <a href="/search/astro-ph?searchtype=author&query=Carter%2C+B">B. Carter</a>, <a href="/search/astro-ph?searchtype=author&query=Cassisi%2C+S">S. Cassisi</a>, <a href="/search/astro-ph?searchtype=author&query=Castilho%2C+B+V">B. V. Castilho</a>, <a href="/search/astro-ph?searchtype=author&query=Cescutti%2C+G">G. Cescutti</a>, <a href="/search/astro-ph?searchtype=author&query=Christlieb%2C+N">N. Christlieb</a>, <a href="/search/astro-ph?searchtype=author&query=Cirami%2C+R">R. Cirami</a>, <a href="/search/astro-ph?searchtype=author&query=Coretti%2C+I">I. Coretti</a>, <a href="/search/astro-ph?searchtype=author&query=Cooke%2C+R">R. Cooke</a>, <a href="/search/astro-ph?searchtype=author&query=Covino%2C+S">S. Covino</a>, <a href="/search/astro-ph?searchtype=author&query=Cremonese%2C+G">G. Cremonese</a>, <a href="/search/astro-ph?searchtype=author&query=Cunha%2C+K">K. Cunha</a>, <a href="/search/astro-ph?searchtype=author&query=Cupani%2C+G">G. Cupani</a>, <a href="/search/astro-ph?searchtype=author&query=da+Silva%2C+A+R">A. R. da Silva</a>, <a href="/search/astro-ph?searchtype=author&query=De+Caprio%2C+V">V. De Caprio</a> , et al. (52 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="2208.01672v1-abstract-short" style="display: inline;"> In the era of Extremely Large Telescopes, the current generation of 8-10m facilities are likely to remain competitive at ground-UV wavelengths for the foreseeable future. The Cassegrain U-Band Efficient Spectrograph (CUBES) has been designed to provide high-efficiency (>40%) observations in the near UV (305-400 nm requirement, 300-420 nm goal) at a spectral resolving power of R>20,000 (with a lowe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.01672v1-abstract-full').style.display = 'inline'; document.getElementById('2208.01672v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.01672v1-abstract-full" style="display: none;"> In the era of Extremely Large Telescopes, the current generation of 8-10m facilities are likely to remain competitive at ground-UV wavelengths for the foreseeable future. The Cassegrain U-Band Efficient Spectrograph (CUBES) has been designed to provide high-efficiency (>40%) observations in the near UV (305-400 nm requirement, 300-420 nm goal) at a spectral resolving power of R>20,000 (with a lower-resolution, sky-limited mode of R ~ 7,000). With the design focusing on maximizing the instrument throughput (ensuring a Signal to Noise Ratio (SNR) ~20 per high-resolution element at 313 nm for U ~18.5 mag objects in 1h of observations), it will offer new possibilities in many fields of astrophysics, providing access to key lines of stellar spectra: a tremendous diversity of iron-peak and heavy elements, lighter elements (in particular Beryllium) and light-element molecules (CO, CN, OH), as well as Balmer lines and the Balmer jump (particularly important for young stellar objects). The UV range is also critical in extragalactic studies: the circumgalactic medium of distant galaxies, the contribution of different types of sources to the cosmic UV background, the measurement of H2 and primordial Deuterium in a regime of relatively transparent intergalactic medium, and follow-up of explosive transients. The CUBES project completed a Phase A conceptual design in June 2021 and has now entered the detailed design and construction phase. First science operations are planned for 2028. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.01672v1-abstract-full').style.display = 'none'; document.getElementById('2208.01672v1-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">SPIE proceedings, SPIE Astronomical Telescopes + Instrumentation 2022, Montr茅al, Canada; 20 pages, 13 figures, 2 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.05318">arXiv:2204.05318</a> <span> [<a href="https://arxiv.org/pdf/2204.05318">pdf</a>, <a href="https://arxiv.org/ps/2204.05318">ps</a>, <a href="https://arxiv.org/format/2204.05318">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/ac63cf">10.3847/1538-4357/ac63cf <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Next Generation Virgo Cluster Survey. XXXIII. Stellar Population Gradients in the Virgo Cluster Core Globular Cluster System </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ko%2C+Y">Youkyung Ko</a>, <a href="/search/astro-ph?searchtype=author&query=Peng%2C+E+W">Eric W. Peng</a>, <a href="/search/astro-ph?searchtype=author&query=C%C3%B4t%C3%A9%2C+P">Patrick C么t茅</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrarese%2C+L">Laura Ferrarese</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+C">Chengze Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Longobardi%2C+A">Alessia Longobardi</a>, <a href="/search/astro-ph?searchtype=author&query=Lan%C3%A7on%2C+A">Ariane Lan莽on</a>, <a href="/search/astro-ph?searchtype=author&query=Mu%C3%B1oz%2C+R+P">Roberto P. Mu帽oz</a>, <a href="/search/astro-ph?searchtype=author&query=Puzia%2C+T+H">Thomas H. Puzia</a>, <a href="/search/astro-ph?searchtype=author&query=Alamo-Mart%C3%ADnez%2C+K+A">Karla A. Alamo-Mart铆nez</a>, <a href="/search/astro-ph?searchtype=author&query=Sales%2C+L+V">Laura V. Sales</a>, <a href="/search/astro-ph?searchtype=author&query=Ramos-Almendares%2C+F">Felipe Ramos-Almendares</a>, <a href="/search/astro-ph?searchtype=author&query=Abadi%2C+M+G">Mario G. Abadi</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+M+G">Myung Gyoon Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+H+S">Ho Seong Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Caldwell%2C+N">Nelson Caldwell</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Boselli%2C+A">Alessandro Boselli</a>, <a href="/search/astro-ph?searchtype=author&query=Cuillandre%2C+J">Jean-Charles Cuillandre</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P">Pierre-Alain Duc</a>, <a href="/search/astro-ph?searchtype=author&query=Eyheramendy%2C+S">Susana Eyheramendy</a>, <a href="/search/astro-ph?searchtype=author&query=Guhathakurta%2C+P">Puragra Guhathakurta</a>, <a href="/search/astro-ph?searchtype=author&query=Gwyn%2C+S">Stephen Gwyn</a>, <a href="/search/astro-ph?searchtype=author&query=Jord%C3%A1n%2C+A">Andr茅s Jord谩n</a>, <a href="/search/astro-ph?searchtype=author&query=Lim%2C+S">Sungsoon Lim</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="2204.05318v1-abstract-short" style="display: inline;"> We present a study of the stellar populations of globular clusters (GCs) in the Virgo Cluster core with a homogeneous spectroscopic catalog of 692 GCs within a major axis distance $R_{\rm maj} = $ 840 kpc from M87. We investigate radial and azimuthal variations in the mean age, total metallicity, [Fe/H], and $伪$-element abundance, of blue (metal-poor) and red (metal-rich) GCs using their co-added… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.05318v1-abstract-full').style.display = 'inline'; document.getElementById('2204.05318v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.05318v1-abstract-full" style="display: none;"> We present a study of the stellar populations of globular clusters (GCs) in the Virgo Cluster core with a homogeneous spectroscopic catalog of 692 GCs within a major axis distance $R_{\rm maj} = $ 840 kpc from M87. We investigate radial and azimuthal variations in the mean age, total metallicity, [Fe/H], and $伪$-element abundance, of blue (metal-poor) and red (metal-rich) GCs using their co-added spectra. We find that the blue GCs have a steep radial gradient in [Z/H] within $R_{\rm maj} =$ 165 kpc, with roughly equal contributions from [Fe/H] and [$伪$/Fe], and flat gradients beyond. By contrast, the red GCs show a much shallower gradient in [Z/H], which is entirely driven by [Fe/H]. We use GC-tagged Illustris simulations to demonstrate an accretion scenario where more massive satellites (with more metal- and $伪$-rich GCs) sink further into the central galaxy than less massive ones, and where the gradient flattening occurs because of the low GC occupation fraction of low-mass dwarfs disrupted at larger distances. The dense environment around M87 may also cause the steep [$伪$/Fe] gradient of the blue GCs, mirroring what is seen in the dwarf galaxy population. The progenitors of red GCs have a narrower mass range than those of blue GCs, which makes their gradients shallower. We also explore spatial inhomogeneity in GC abundances, finding that the red GCs to the northwest of M87 are slightly more metal-rich. Future observations of GC stellar population gradients will be useful diagnostics of halo merger histories. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.05318v1-abstract-full').style.display = 'none'; document.getElementById('2204.05318v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 8 figures, 4 tables, accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.02513">arXiv:2203.02513</a> <span> [<a href="https://arxiv.org/pdf/2203.02513">pdf</a>, <a href="https://arxiv.org/format/2203.02513">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/stac1516">10.1093/mnras/stac1516 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Pristine survey XVIII: C-19: Tidal debris of a dark matter-dominated globular cluster? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Errani%2C+R">Rapha毛l Errani</a>, <a href="/search/astro-ph?searchtype=author&query=Navarro%2C+J+F">Julio F. Navarro</a>, <a href="/search/astro-ph?searchtype=author&query=Ibata%2C+R">Rodrigo Ibata</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+N">Nicolas Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+Z">Zhen Yuan</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=Bonifacio%2C+P">Piercarlo Bonifacio</a>, <a href="/search/astro-ph?searchtype=author&query=Caffau%2C+E">Elisabetta Caffau</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez%2C+J+I+G">Jonay I. Gonz谩lez Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Malhan%2C+K">Khyati Malhan</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">Rub茅n S谩nchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Sestito%2C+F">Federico Sestito</a>, <a href="/search/astro-ph?searchtype=author&query=Starkenburg%2C+E">Else Starkenburg</a>, <a href="/search/astro-ph?searchtype=author&query=Thomas%2C+G+F">Guillaume F. Thomas</a>, <a href="/search/astro-ph?searchtype=author&query=Venn%2C+K+A">Kim A. Venn</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="2203.02513v2-abstract-short" style="display: inline;"> The recently discovered C-19 stellar stream is a collection of kinematically associated metal-poor stars in the halo of the Milky Way lacking an obvious progenitor. The stream spans an arc of ~15 degrees in the sky, and orbit-fitting suggests an apocentric distance of ~20 kpc and a pericentre of ~10 kpc. The narrow metallicity dispersion of stars with available spectra, together with light element… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.02513v2-abstract-full').style.display = 'inline'; document.getElementById('2203.02513v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.02513v2-abstract-full" style="display: none;"> The recently discovered C-19 stellar stream is a collection of kinematically associated metal-poor stars in the halo of the Milky Way lacking an obvious progenitor. The stream spans an arc of ~15 degrees in the sky, and orbit-fitting suggests an apocentric distance of ~20 kpc and a pericentre of ~10 kpc. The narrow metallicity dispersion of stars with available spectra, together with light element abundance variations, suggests a globular cluster (GC) origin. The observed metallicity ([Fe/H] ~ -3.4), however, is much lower than that of any known GC. In addition, the width and velocity dispersion of the stream are similar to those expected from disrupting dwarf galaxies, and substantially larger than the tidal debris of GCs able to disrupt on C-19's orbit. We propose here an unconventional model where the C-19 progenitor is a dark matter-dominated stellar system with GC-like abundance patterns. We use N-body simulations to show that the tidal disruption of a ~100 pc King-model stellar component embedded in a ~20 km/s cuspy cold dark matter halo yields debris consistent with C-19's observed width and velocity dispersion. The stellar component of the progenitor is fully disrupted, and is spread over two distinct streams; one corresponding to C-19 and another possibly hiding behind the Galactic plane. If such companion stream were found, it would suggest that dark matter-dominated dwarfs may also develop GC-like enrichment patterns, a finding that would inform our theoretical understanding of the formation of multiple populations in GCs and dwarf galaxies alike. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.02513v2-abstract-full').style.display = 'none'; document.getElementById('2203.02513v2-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 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 9 figures. minor edits to match accepted 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/2201.03862">arXiv:2201.03862</a> <span> [<a href="https://arxiv.org/pdf/2201.03862">pdf</a>, <a href="https://arxiv.org/format/2201.03862">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> </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/10.5281/zenodo.7195671">10.5281/zenodo.7195671 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Rubin-Euclid Derived Data Products: Initial Recommendations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Guy%2C+L+P">Leanne P. Guy</a>, <a href="/search/astro-ph?searchtype=author&query=Cuillandre%2C+J">Jean-Charles Cuillandre</a>, <a href="/search/astro-ph?searchtype=author&query=Bachelet%2C+E">Etienne Bachelet</a>, <a href="/search/astro-ph?searchtype=author&query=Banerji%2C+M">Manda Banerji</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">Franz E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Collett%2C+T">Thomas Collett</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=Eggl%2C+S">Siegfried Eggl</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+A">Annette Ferguson</a>, <a href="/search/astro-ph?searchtype=author&query=Fontana%2C+A">Adriano Fontana</a>, <a href="/search/astro-ph?searchtype=author&query=Heymans%2C+C">Catherine Heymans</a>, <a href="/search/astro-ph?searchtype=author&query=Hook%2C+I+M">Isobel M. Hook</a>, <a href="/search/astro-ph?searchtype=author&query=Aubourg%2C+%C3%89">脡ric Aubourg</a>, <a href="/search/astro-ph?searchtype=author&query=Aussel%2C+H">Herv茅 Aussel</a>, <a href="/search/astro-ph?searchtype=author&query=Bosch%2C+J">James Bosch</a>, <a href="/search/astro-ph?searchtype=author&query=Carry%2C+B">Benoit Carry</a>, <a href="/search/astro-ph?searchtype=author&query=Hoekstra%2C+H">Henk Hoekstra</a>, <a href="/search/astro-ph?searchtype=author&query=Kuijken%2C+K">Konrad Kuijken</a>, <a href="/search/astro-ph?searchtype=author&query=Lanusse%2C+F">Francois Lanusse</a>, <a href="/search/astro-ph?searchtype=author&query=Melchior%2C+P">Peter Melchior</a>, <a href="/search/astro-ph?searchtype=author&query=Mohr%2C+J">Joseph Mohr</a>, <a href="/search/astro-ph?searchtype=author&query=Moresco%2C+M">Michele Moresco</a>, <a href="/search/astro-ph?searchtype=author&query=Nakajima%2C+R">Reiko Nakajima</a>, <a href="/search/astro-ph?searchtype=author&query=Paltani%2C+S">St茅phane Paltani</a>, <a href="/search/astro-ph?searchtype=author&query=Troxel%2C+M">Michael Troxel</a> , et al. (95 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="2201.03862v2-abstract-short" style="display: inline;"> This report is the result of a joint discussion between the Rubin and Euclid scientific communities. The work presented in this report was focused on designing and recommending an initial set of Derived Data products (DDPs) that could realize the science goals enabled by joint processing. All interested Rubin and Euclid data rights holders were invited to contribute via an online discussion forum… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.03862v2-abstract-full').style.display = 'inline'; document.getElementById('2201.03862v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.03862v2-abstract-full" style="display: none;"> This report is the result of a joint discussion between the Rubin and Euclid scientific communities. The work presented in this report was focused on designing and recommending an initial set of Derived Data products (DDPs) that could realize the science goals enabled by joint processing. All interested Rubin and Euclid data rights holders were invited to contribute via an online discussion forum and a series of virtual meetings. Strong interest in enhancing science with joint DDPs emerged from across a wide range of astrophysical domains: Solar System, the Galaxy, the Local Volume, from the nearby to the primaeval Universe, and cosmology. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.03862v2-abstract-full').style.display = 'none'; document.getElementById('2201.03862v2-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 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Report of the Rubin-Euclid Derived Data Products Working Group, 78 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/2201.01310">arXiv:2201.01310</a> <span> [<a href="https://arxiv.org/pdf/2201.01310">pdf</a>, <a href="https://arxiv.org/ps/2201.01310">ps</a>, <a href="https://arxiv.org/format/2201.01310">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/stac2426">10.1093/mnras/stac2426 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Pristine survey -- XVI. The metallicity of 26 stellar streams around the Milky Way detected with the STREAMFINDER in Gaia EDR3 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Martin%2C+N+F">Nicolas F. Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Ibata%2C+R+A">Rodrigo A. Ibata</a>, <a href="/search/astro-ph?searchtype=author&query=Starkenburg%2C+E">Else Starkenburg</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+Z">Zhen Yuan</a>, <a href="/search/astro-ph?searchtype=author&query=Malhan%2C+K">Khyati Malhan</a>, <a href="/search/astro-ph?searchtype=author&query=Bellazzini%2C+M">Michele Bellazzini</a>, <a href="/search/astro-ph?searchtype=author&query=Viswanathan%2C+A">Akshara Viswanathan</a>, <a href="/search/astro-ph?searchtype=author&query=Aguado%2C+D">David Aguado</a>, <a href="/search/astro-ph?searchtype=author&query=Arentsen%2C+A">Anke Arentsen</a>, <a href="/search/astro-ph?searchtype=author&query=Bonifacio%2C+P">Piercarlo Bonifacio</a>, <a href="/search/astro-ph?searchtype=author&query=Carlberg%2C+R">Ray Carlberg</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez%2C+J+I+G">Jonay I. Gonz谩lez Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+V">Vanessa Hill</a>, <a href="/search/astro-ph?searchtype=author&query=Jablonka%2C+P">Pascale Jablonka</a>, <a href="/search/astro-ph?searchtype=author&query=Kordopatis%2C+G">Georges Kordopatis</a>, <a href="/search/astro-ph?searchtype=author&query=Lardo%2C+C">Carmela Lardo</a>, <a href="/search/astro-ph?searchtype=author&query=McConnachie%2C+A+W">Alan W. McConnachie</a>, <a href="/search/astro-ph?searchtype=author&query=Navarro%2C+J">Julio Navarro</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">Rub茅n S谩nchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Sestito%2C+F">Federico Sestito</a>, <a href="/search/astro-ph?searchtype=author&query=Thomas%2C+G+F">Guillaume F. Thomas</a>, <a href="/search/astro-ph?searchtype=author&query=Venn%2C+K+A">Kim A. Venn</a>, <a href="/search/astro-ph?searchtype=author&query=Vitali%2C+S">Sara Vitali</a>, <a href="/search/astro-ph?searchtype=author&query=Voggel%2C+K+T">Karina T. Voggel</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2201.01310v2-abstract-short" style="display: inline;"> We use the photometric metallicities provided by the panoramic Pristine survey to study the veracity and derive the metallicities of the numerous stellar streams found by the application of the STREAMFINDER algorithm to the Gaia EDR3 data. All 26 streams present in Pristine show a clear metallicity distribution function, which provides an independent check of the reality of these structures, suppo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.01310v2-abstract-full').style.display = 'inline'; document.getElementById('2201.01310v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.01310v2-abstract-full" style="display: none;"> We use the photometric metallicities provided by the panoramic Pristine survey to study the veracity and derive the metallicities of the numerous stellar streams found by the application of the STREAMFINDER algorithm to the Gaia EDR3 data. All 26 streams present in Pristine show a clear metallicity distribution function, which provides an independent check of the reality of these structures, supporting the reliability of STREAMFINDER in finding streams and the power of Pristine to measure precise metallicities. We further present 6 candidate structures with coherent phase-space and metallicity signals that are very likely streams. The majority of studied streams are very metal-poor (14 structures with [Fe/H]<-2.0) and include 3 systems with [Fe/H]<-2.9 (C-11, C-19, and C-20). These streams could be the closest debris of low-luminosity dwarf galaxies or may have originated from globular clusters of significantly lower metallicity than any known current Milky Way globular cluster. Our study shows that the promise of the Gaia data for Galactic Archeology studies can be substantially strengthened by quality photometric metallicities, allowing us to peer back into the earliest epochs of the formation of our Galaxy and its stellar halo constituents. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.01310v2-abstract-full').style.display = 'none'; document.getElementById('2201.01310v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages, 29 figures, accepted for publication in MNRAS. Updated version has only minor changes compared to initial submission. The metallicity of most streams have marginally changed in the updated 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/2111.14491">arXiv:2111.14491</a> <span> [<a href="https://arxiv.org/pdf/2111.14491">pdf</a>, <a href="https://arxiv.org/format/2111.14491">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/10.1051/0004-6361/202142012">10.1051/0004-6361/202142012 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> HI observations of the MATLAS dwarf and ultra-diffuse galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Poulain%2C+M">Melina Poulain</a>, <a href="/search/astro-ph?searchtype=author&query=Marleau%2C+F+R">Francine R. Marleau</a>, <a href="/search/astro-ph?searchtype=author&query=Habas%2C+R">Rebecca Habas</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P">Pierre-Alain Duc</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez-Janssen%2C+R">Ruben Sanchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Durrell%2C+P+R">Patrick R. Durrell</a>, <a href="/search/astro-ph?searchtype=author&query=Paudel%2C+S">Sanjaya Paudel</a>, <a href="/search/astro-ph?searchtype=author&query=Mueller%2C+O">Oliver Mueller</a>, <a href="/search/astro-ph?searchtype=author&query=Lim%2C+S">Sungsoon Lim</a>, <a href="/search/astro-ph?searchtype=author&query=Bilek%2C+M">Michal Bilek</a>, <a href="/search/astro-ph?searchtype=author&query=Fensch%2C+J">Jeremy Fensch</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="2111.14491v1-abstract-short" style="display: inline;"> The presence of HI gas in galaxies is inextricably linked to their morphology and evolution. This paper aims to understand the HI content of the already identified 2210 dwarfs located in the low-to-moderate density environments of the MATLAS deep imaging survey. We combine the HI observations from the ATLAS$^{3D}$ survey, with the extragalactic HI sources from the ALFALFA survey, to extract the HI… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.14491v1-abstract-full').style.display = 'inline'; document.getElementById('2111.14491v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.14491v1-abstract-full" style="display: none;"> The presence of HI gas in galaxies is inextricably linked to their morphology and evolution. This paper aims to understand the HI content of the already identified 2210 dwarfs located in the low-to-moderate density environments of the MATLAS deep imaging survey. We combine the HI observations from the ATLAS$^{3D}$ survey, with the extragalactic HI sources from the ALFALFA survey, to extract the HI line width, velocity and mass of the MATLAS dwarfs. From the 1773 dwarfs in our sample with available HI observations, 8% (145) have an HI line detection. The majority of the dwarfs show irregular morphology, while 29% (42) are ellipticals, the largest sample of HI-bearing dwarf ellipticals (dEs) to date. Of the HI dwarf sample, 2% (3) are ultra-diffuse galaxies (UDGs), 12% have a transition-type morphology, 5% are tidal dwarf candidates, and 10% appear to be disrupted objects. In our optically selected sample, 9.5% of the dEs, 7% of the UDGs and 10% of the classical dwarfs are HI-bearing. The HI-bearing dwarfs have on average bluer colors than the dwarfs without detected HI. We find relations between the stellar and HI masses, gas fraction, color and absolute magnitude consistent with previous studies of dwarfs probing similar masses and environments. For 79% of the dwarfs identified as satellites of massive early-type galaxies, we find that the HI mass increases with the projected distance to the host. Using the HI line width, we estimate dynamical masses and find that 5% (7) of the dwarfs are dark matter deficient. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.14491v1-abstract-full').style.display = 'none'; document.getElementById('2111.14491v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 14 figures, 1 table. Accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 659, A14 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2110.13783">arXiv:2110.13783</a> <span> [<a href="https://arxiv.org/pdf/2110.13783">pdf</a>, <a href="https://arxiv.org/format/2110.13783">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"> Extragalactic globular clusters with Euclid and other wide surveys </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lan%C3%A7on%2C+A">Ariane Lan莽on</a>, <a href="/search/astro-ph?searchtype=author&query=Larsen%2C+S">S. Larsen</a>, <a href="/search/astro-ph?searchtype=author&query=Voggel%2C+K">K. Voggel</a>, <a href="/search/astro-ph?searchtype=author&query=Cuillandre%2C+J+-">J. -C. Cuillandre</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P+-">P. -A. Duc</a>, <a href="/search/astro-ph?searchtype=author&query=Chantereau%2C+W">W. Chantereau</a>, <a href="/search/astro-ph?searchtype=author&query=Jain%2C+R">R. Jain</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">R. S谩nchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">M. Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">M. Rejkuba</a>, <a href="/search/astro-ph?searchtype=author&query=Marleau%2C+F">F. Marleau</a>, <a href="/search/astro-ph?searchtype=author&query=Saifollahi%2C+T">T. Saifollahi</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C">C. Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=Hunt%2C+L">L. Hunt</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+A+M+N">A. M. N. Ferguson</a>, <a href="/search/astro-ph?searchtype=author&query=Lagadec%2C+E">E. Lagadec</a>, <a href="/search/astro-ph?searchtype=author&query=C%C3%B4t%C3%A9%2C+P">P. C么t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="2110.13783v1-abstract-short" style="display: inline;"> Globular clusters play a role in many areas of astrophysics, ranging from stellar physics to cosmology. New ground-based optical surveys complemented by observations from space-based telescopes with unprecedented near-infrared capabilities will help us solve the puzzles of their formation histories. In this context, the Wide Survey of the Euclid space mission will provide red and near-infrared dat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.13783v1-abstract-full').style.display = 'inline'; document.getElementById('2110.13783v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.13783v1-abstract-full" style="display: none;"> Globular clusters play a role in many areas of astrophysics, ranging from stellar physics to cosmology. New ground-based optical surveys complemented by observations from space-based telescopes with unprecedented near-infrared capabilities will help us solve the puzzles of their formation histories. In this context, the Wide Survey of the Euclid space mission will provide red and near-infrared data over about 15000 square degrees of the sky. Combined with optical photometry from the ground, it will allow us to construct a global picture of the globular cluster populations in both dense and tenuous environments out to tens of megaparsecs. The homogeneous photometry of these data sets will rejuvenate stellar population studies that depend on precise spectral energy distributions. We provide a brief overview of these perspectives. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.13783v1-abstract-full').style.display = 'none'; document.getElementById('2110.13783v1-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 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">4 pages, 1 figure. Proceedings of an oral contribution to Session 23 "Wide Field Photometric Surveys II" of the 2021 meeting of SF2A (Soci茅t茅 Fran莽aise d'Astronomie et d'Astrophysique), June 9, 2021. Reviewed by the proceedings editors and the Euclid Consortium editorial board</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.13173">arXiv:2109.13173</a> <span> [<a href="https://arxiv.org/pdf/2109.13173">pdf</a>, <a href="https://arxiv.org/format/2109.13173">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/10.1051/0004-6361/202141432">10.1051/0004-6361/202141432 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Ultra diffuse galaxies in the MATLAS low-to-moderate density fields </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Marleau%2C+F+R">Francine R. Marleau</a>, <a href="/search/astro-ph?searchtype=author&query=Habas%2C+R">Rebecca Habas</a>, <a href="/search/astro-ph?searchtype=author&query=Poulain%2C+M">Melina Poulain</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P">Pierre-Alain Duc</a>, <a href="/search/astro-ph?searchtype=author&query=Mueller%2C+O">Oliver Mueller</a>, <a href="/search/astro-ph?searchtype=author&query=Lim%2C+S">Sungsoon Lim</a>, <a href="/search/astro-ph?searchtype=author&query=Durrell%2C+P+R">Patrick R. Durrell</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez-Janssen%2C+R">Ruben Sanchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Paudel%2C+S">Sanjaya Paudel</a>, <a href="/search/astro-ph?searchtype=author&query=Ahad%2C+S+L">Syeda Lammim Ahad</a>, <a href="/search/astro-ph?searchtype=author&query=Chougule%2C+A">Abhishek Chougule</a>, <a href="/search/astro-ph?searchtype=author&query=Bilek%2C+M">Michal Bilek</a>, <a href="/search/astro-ph?searchtype=author&query=Fensch%2C+J">Jeremy Fensch</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2109.13173v1-abstract-short" style="display: inline;"> Recent advances in deep dedicated imaging surveys over the past decade have uncovered a surprisingly large number of extremely faint low surface brightness galaxies with large physical sizes called ultra diffuse galaxies (UDGs) in clusters and, more recently, in lower density environments. As part of the MATLAS survey, a deep imaging large program at the Canada-France-Hawaii Telescope (CFHT), our… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.13173v1-abstract-full').style.display = 'inline'; document.getElementById('2109.13173v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.13173v1-abstract-full" style="display: none;"> Recent advances in deep dedicated imaging surveys over the past decade have uncovered a surprisingly large number of extremely faint low surface brightness galaxies with large physical sizes called ultra diffuse galaxies (UDGs) in clusters and, more recently, in lower density environments. As part of the MATLAS survey, a deep imaging large program at the Canada-France-Hawaii Telescope (CFHT), our team has identified 2210 dwarf galaxies, 59 (~3%) of which qualify as UDGs. Averaging over the survey area, we find ~0.4 UDG per square degree. They are found in a range of low to moderate density environments, although 61% of the sample fall within the virial radii of groups. Based on a detailed analysis of their photometric and structural properties, we find that the MATLAS UDGs do not show significant differences from the traditional dwarfs, except from the predefined size and surface brightness cut. Their median color is as red as the one measured in galaxy clusters, albeit with a narrower color range. The majority of the UDGs are visually classified as dwarf ellipticals with log stellar masses of ~6.5-8.7. The fraction of nucleated UDGs (~34%) is roughly the same as the nucleated fraction of the traditional dwarfs. Only five (~8%) UDGs show signs of tidal disruption and only two are tidal dwarf galaxy candidates. A study of globular cluster (GC) candidates selected in the CFHT images finds no evidence of a higher GC specific frequency S_N for UDGs than for classical dwarfs, contrary to what is found in most clusters. The UDG halo-to-stellar mass ratio distribution, as estimated from the GC counts, peaks at roughly the same value as for the traditional dwarfs, but spans the smaller range of ~10-2000. We interpret these results to mean that the large majority of the field-to-group UDGs do not have a different formation scenario than traditional dwarfs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.13173v1-abstract-full').style.display = 'none'; document.getElementById('2109.13173v1-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 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">32 pages, 25 figures, 3 tables, accepted in A&A; All data including images may be queried from the MATLAS web project: http://obas-matlas.u-strasbg.fr/WP/?page_id=825</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2108.10189">arXiv:2108.10189</a> <span> [<a href="https://arxiv.org/pdf/2108.10189">pdf</a>, <a href="https://arxiv.org/format/2108.10189">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/10.1051/0004-6361/202141184">10.1051/0004-6361/202141184 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Flattened structures of dwarf satellites around massive host galaxies in the MATLAS low-to-moderate density fields </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Heesters%2C+N">N. Heesters</a>, <a href="/search/astro-ph?searchtype=author&query=Habas%2C+R">R. Habas</a>, <a href="/search/astro-ph?searchtype=author&query=Marleau%2C+F+R">F. R. Marleau</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%BCller%2C+O">O. M眉ller</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P+-">P. -A. Duc</a>, <a href="/search/astro-ph?searchtype=author&query=Poulain%2C+M">M. Poulain</a>, <a href="/search/astro-ph?searchtype=author&query=Durrell%2C+P">P. Durrell</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">R. S谩nchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Paudel%2C+S">S. Paudel</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="2108.10189v1-abstract-short" style="display: inline;"> It was first observed in the 1970s that the dwarf galaxies surrounding our Milky Way, so-called satellites, appear to be arranged in a thin, vast plane. Similar discoveries have been made around additional galaxies in the local Universe such as Andromeda, Centaurus A, and potentially M83. In the specific cases with available kinematic data, the dwarf satellites also appear to preferentially co-orb… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.10189v1-abstract-full').style.display = 'inline'; document.getElementById('2108.10189v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.10189v1-abstract-full" style="display: none;"> It was first observed in the 1970s that the dwarf galaxies surrounding our Milky Way, so-called satellites, appear to be arranged in a thin, vast plane. Similar discoveries have been made around additional galaxies in the local Universe such as Andromeda, Centaurus A, and potentially M83. In the specific cases with available kinematic data, the dwarf satellites also appear to preferentially co-orbit their massive host galaxy. Planes of satellites are rare in the lambda cold dark matter ($螞$CDM) paradigm, although they may be a natural consequence of projection effects. Such a phase-space correlation, however, remains difficult to explain. In this work we analyzed the 2D spatial distribution of 2210 dwarf galaxies around early-type galaxies (ETGs) in the low-to-medium density fields of the "Mass Assembly of early-Type GaLAxies with their fine Structures" (MATLAS) survey. Under the assumption that the dwarfs are satellite members of the central massive ETG, we identified flattened structures using both a variation in the Hough transform and total least square (TLS) fitting. In 119 satellite systems, we find 31 statistically significant flattened dwarf structures using a combination of both methods with subsequent Monte Carlo (MC) simulations with random data. The vast majority of these dwarf structures lie within the estimated virial radii of the massive host. The major axes of these systems are aligned better than 30掳 with the estimated orientation of the large-scale structure in nine (50%) cases. Additional distance measurements and future kinematic studies will be required to confirm the planar nature of these structures and to determine if they are corotating systems. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.10189v1-abstract-full').style.display = 'none'; document.getElementById('2108.10189v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 August, 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, 15 figures, Accepted for publication in Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 654, A161 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.10849">arXiv:2107.10849</a> <span> [<a href="https://arxiv.org/pdf/2107.10849">pdf</a>, <a href="https://arxiv.org/format/2107.10849">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/stac1827">10.1093/mnras/stac1827 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Pristine Dwarf-Galaxy survey -- IV. Probing the outskirts of the dwarf galaxy Bo枚tes I </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Longeard%2C+N">Nicolas Longeard</a>, <a href="/search/astro-ph?searchtype=author&query=Jablonka%2C+P">Pascale Jablonka</a>, <a href="/search/astro-ph?searchtype=author&query=Arentsen%2C+A">Anke Arentsen</a>, <a href="/search/astro-ph?searchtype=author&query=Thomas%2C+G+F">Guillaume F. Thomas</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=Carlberg%2C+R+G">Raymond G. Carlberg</a>, <a href="/search/astro-ph?searchtype=author&query=Lucchesi%2C+R">Romain Lucchesi</a>, <a href="/search/astro-ph?searchtype=author&query=Malhan%2C+K">Khyati Malhan</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+N">Nicolas Martin</a>, <a href="/search/astro-ph?searchtype=author&query=McConnachie%2C+A+W">Alan W. McConnachie</a>, <a href="/search/astro-ph?searchtype=author&query=Navarro%2C+J+F">Julio F. Navarro</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">Rub茅n S谩nchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Sestito%2C+F">Federico Sestito</a>, <a href="/search/astro-ph?searchtype=author&query=Starkenburg%2C+E">Else Starkenburg</a>, <a href="/search/astro-ph?searchtype=author&query=Yuan%2C+Z">Zhen 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="2107.10849v3-abstract-short" style="display: inline;"> We present a new spectroscopic study of the dwarf galaxy Bootes I (Boo I) with data from the Anglo-Australian Telescope and its AAOmega spectrograph together with the Two Degree Field multi-object system. We observed 36 high-probability Boo I stars selected using Gaia Early Data Release 3 proper motions and photometric metallicities from the Pristine survey. Out of those, 27 are found to be Boo I'… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.10849v3-abstract-full').style.display = 'inline'; document.getElementById('2107.10849v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.10849v3-abstract-full" style="display: none;"> We present a new spectroscopic study of the dwarf galaxy Bootes I (Boo I) with data from the Anglo-Australian Telescope and its AAOmega spectrograph together with the Two Degree Field multi-object system. We observed 36 high-probability Boo I stars selected using Gaia Early Data Release 3 proper motions and photometric metallicities from the Pristine survey. Out of those, 27 are found to be Boo I's stars, resulting in an excellent success rate of 75% at finding new members. Our analysis uses a new pipeline developed to estimate radial velocities and equivalent widths of the calcium triplet lines from Gaussian and Voigt line profile fits. The metallicities of 16 members are derived, including 3 extremely metal-poor stars ([Fe/H] < -3.0), which translates into a success rate of 25% at finding them with the combination of Pristine and Gaia. Using the large spatial extent of our new members that spans up to 4.1 half-light radii and spectroscopy from the literature, we find a systemic velocity gradient of 0.40 +/- 0.10 km/s/arcmin and a small but resolved metallicity gradient of -0.008 +/- 0.003 dex/arcmin. Finally, we show that Boo I is more elongated than previously thought with an ellipticity of epsilon = 0.68 +/- 0.15. Its velocity and metallicity gradients as well as its elongation suggest that Boo I may have been affected by tides, a result supported by direct dynamical modelling. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.10849v3-abstract-full').style.display = 'none'; document.getElementById('2107.10849v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2021. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.09379">arXiv:2107.09379</a> <span> [<a href="https://arxiv.org/pdf/2107.09379">pdf</a>, <a href="https://arxiv.org/format/2107.09379">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/stab2092">10.1093/mnras/stab2092 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Structure and morphology of the MATLAS dwarf galaxies and their central nuclei </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Poulain%2C+M">Melina Poulain</a>, <a href="/search/astro-ph?searchtype=author&query=Marleau%2C+F+R">Francine R. Marleau</a>, <a href="/search/astro-ph?searchtype=author&query=Habas%2C+R">Rebecca Habas</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P">Pierre-Alain Duc</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez-Janssen%2C+R">Ruben Sanchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Durrell%2C+P+R">Patrick R. Durrell</a>, <a href="/search/astro-ph?searchtype=author&query=Paudel%2C+S">Sanjaya Paudel</a>, <a href="/search/astro-ph?searchtype=author&query=Ahad%2C+S+L">Syeda Lammim Ahad</a>, <a href="/search/astro-ph?searchtype=author&query=Chougule%2C+A">Abhishek Chougule</a>, <a href="/search/astro-ph?searchtype=author&query=Mueller%2C+O">Oliver Mueller</a>, <a href="/search/astro-ph?searchtype=author&query=Lim%2C+S">Sungsoon Lim</a>, <a href="/search/astro-ph?searchtype=author&query=Bilek%2C+M">Michal Bilek</a>, <a href="/search/astro-ph?searchtype=author&query=Fensch%2C+J">Jeremy Fensch</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="2107.09379v2-abstract-short" style="display: inline;"> We present a photometric study of the dwarf galaxy population in the low to moderate density environments of the MATLAS (Mass Assembly of early-Type gaLAxies with their fine Structures) deep imaging survey. The sample consists of 2210 dwarfs, including 508 nucleated. We define a nucleus as a compact source that is close to the galaxy photocentre (within 0.5 $R_e$) which is also the brightest such… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.09379v2-abstract-full').style.display = 'inline'; document.getElementById('2107.09379v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.09379v2-abstract-full" style="display: none;"> We present a photometric study of the dwarf galaxy population in the low to moderate density environments of the MATLAS (Mass Assembly of early-Type gaLAxies with their fine Structures) deep imaging survey. The sample consists of 2210 dwarfs, including 508 nucleated. We define a nucleus as a compact source that is close to the galaxy photocentre (within 0.5 $R_e$) which is also the brightest such source within the galaxy's effective radius. The morphological analysis is performed using a 2D surface brightness profile modelling on the g-band images of both the galaxies and nuclei. Our study reveals that, for similar luminosities, the MATLAS dwarfs show ranges in the distribution of structural properties comparable to cluster (Virgo and Fornax) dwarfs and a range of sizes comparable to the Local Group and Local Volume dwarfs. Colour measurements using the r- and i-band images indicate that the dwarfs in low and moderate density environments are as red as cluster dwarfs on average. The observed similarities between dwarf ellipticals in vastly different environments imply that dEs are not uniquely the product of morphological transformation due to ram-pressure stripping and galaxy harassment in high density environments. We measure that the dwarf nuclei are located predominantly in massive, bright and round dwarfs and observe fewer nuclei in dwarfs with a faint centre and a small size. The colour of the galaxy nucleus shows no clear relation to the colour of the dwarf, in agreement with the migration and wet migration nucleus formation scenarios. The catalogues of the MATLAS dwarfs photometric and structural properties are provided. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.09379v2-abstract-full').style.display = 'none'; document.getElementById('2107.09379v2-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, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 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">19 pages, 15 figures, 4 tables. v2: table and text changes to match the published version 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/2105.04569">arXiv:2105.04569</a> <span> [<a href="https://arxiv.org/pdf/2105.04569">pdf</a>, <a href="https://arxiv.org/format/2105.04569">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/abffcf">10.3847/1538-4357/abffcf <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Fresh Insights on the Kinematics of M49's Globular Cluster System with MMT/Hectospec Spectroscopy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Taylor%2C+M+A">Matthew A. Taylor</a>, <a href="/search/astro-ph?searchtype=author&query=Ko%2C+Y">Youkyung Ko</a>, <a href="/search/astro-ph?searchtype=author&query=C%C3%B4t%C3%A9%2C+P">Patrick C么t茅</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrarese%2C+L">Laura Ferrarese</a>, <a href="/search/astro-ph?searchtype=author&query=Peng%2C+E+W">Eric W. Peng</a>, <a href="/search/astro-ph?searchtype=author&query=Zabludoff%2C+A">Ann Zabludoff</a>, <a href="/search/astro-ph?searchtype=author&query=Roediger%2C+J">Joel Roediger</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">Rub茅n S谩nchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Hendel%2C+D">David Hendel</a>, <a href="/search/astro-ph?searchtype=author&query=Chilingarian%2C+I">Igor Chilingarian</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+C">Chengze Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Spengler%2C+C">Chelsea Spengler</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+H">Hongxin Zhang</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="2105.04569v1-abstract-short" style="display: inline;"> We present the first results of an MMT/Hectospec campaign to measure the kinematics of globular clusters (GCs) around M49 -- the brightest galaxy in the Virgo galaxy cluster, which dominates the Virgo B subcluster. The data include kinematic tracers beyond 95 kpc (~5.2 effective radii) for M49 for the first time, enabling us to achieve three key insights reported here. First, beyond ~20'-30' (~100… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.04569v1-abstract-full').style.display = 'inline'; document.getElementById('2105.04569v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.04569v1-abstract-full" style="display: none;"> We present the first results of an MMT/Hectospec campaign to measure the kinematics of globular clusters (GCs) around M49 -- the brightest galaxy in the Virgo galaxy cluster, which dominates the Virgo B subcluster. The data include kinematic tracers beyond 95 kpc (~5.2 effective radii) for M49 for the first time, enabling us to achieve three key insights reported here. First, beyond ~20'-30' (~100-150 kpc), the GC kinematics sampled along the minor photometric axis of M49 become increasingly hotter, indicating a transition from GCs related to M49 to those representing the Virgo B intra-cluster medium. Second, there is an anomaly in the line-of-sight radial velocity dispersion ($蟽_{r,los}$) profile in an annulus ~10-15' (~50-90 kpc) from M49 in which the kinematics cool by $螖蟽_{r,los}~150$ km s$^{-1}$ relative to those in- or outward. The kinematic fingerprint of a previous accretion event is hinted at in projected phase-space, and we isolate GCs that both give rise to this feature, and are spatially co-located with two prominent stellar shells in the halo of M49. Third, we find a subsample of GCs with velocities representative of the dwarf galaxy VCC1249 that is currently interacting with M49. The spatial distribution of these GCs closely resembles the morphology of VCC1249's isophotes, indicating that several of these GCs are likely in the act of being stripped from the dwarf during its passage through M49's halo. Taken together, these results point toward the opportunity of witnessing on-going giant halo assembly in the depths of a cluster environment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.04569v1-abstract-full').style.display = 'none'; document.getElementById('2105.04569v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 May, 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">14 pages, 9 figures, accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2103.02123">arXiv:2103.02123</a> <span> [<a href="https://arxiv.org/pdf/2103.02123">pdf</a>, <a href="https://arxiv.org/format/2103.02123">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/stab2348">10.1093/mnras/stab2348 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A high occurrence of nuclear star clusters in faint Coma galaxies, and the roles of mass and environment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zanatta%2C+E+J+B">Emilio J. B. Zanatta</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">Rub茅n S谩nchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Chies-Santos%2C+A+L">Ana L. Chies-Santos</a>, <a href="/search/astro-ph?searchtype=author&query=de+Souza%2C+R+S">Rafael S. de Souza</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</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="2103.02123v2-abstract-short" style="display: inline;"> We use deep high resolution \textit{HST/ACS} imaging of two fields in the core of the Coma cluster to investigate the occurrence of nuclear star clusters (NSCs) in quiescent dwarf galaxies as faint as $M_{I} = -10$ mag. We employ a hierarchical Bayesian logistic regression framework to model the faint end of the nucleation fraction ($f_{n}$) as a function of both galaxy luminosity and environment.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.02123v2-abstract-full').style.display = 'inline'; document.getElementById('2103.02123v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.02123v2-abstract-full" style="display: none;"> We use deep high resolution \textit{HST/ACS} imaging of two fields in the core of the Coma cluster to investigate the occurrence of nuclear star clusters (NSCs) in quiescent dwarf galaxies as faint as $M_{I} = -10$ mag. We employ a hierarchical Bayesian logistic regression framework to model the faint end of the nucleation fraction ($f_{n}$) as a function of both galaxy luminosity and environment. We find that $f_n$ is remarkably high in Coma: at $M_{I} \approx -13$ mag half of the cluster dwarfs still host prominent NSCs. Comparison with dwarf systems in nearby clusters and groups shows that, within the uncertainties, the rate at which the probability of nucleation varies with galaxy luminosity is nearly universal. On the other hand, the fraction of nucleated galaxies at fixed luminosity does exhibit an environmental dependence. More massive environments feature higher nucleation fractions and fainter values of the half-nucleation luminosity, which roughly scales with host halo virial mass as $L_{I,f_{n50}} \propto \mathcal{M}_{200}^{-0.2}$. Our results reinforce the role of galaxy luminosity/mass as a major driver of the efficiency of NSC formation and also indicate a clear secondary dependence on the environment, hence paving the way to more refined theoretical models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.02123v2-abstract-full').style.display = 'none'; document.getElementById('2103.02123v2-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 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 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">15 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/2101.10659">arXiv:2101.10659</a> <span> [<a href="https://arxiv.org/pdf/2101.10659">pdf</a>, <a href="https://arxiv.org/format/2101.10659">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/ac2831">10.3847/1538-4357/ac2831 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Dwarf galaxies in the MATLAS survey: Hubble Space Telescope observations of the globular cluster system in the ultra-diffuse galaxy MATLAS-2019 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=M%C3%BCller%2C+O">Oliver M眉ller</a>, <a href="/search/astro-ph?searchtype=author&query=Durrell%2C+P+R">Patrick R. Durrell</a>, <a href="/search/astro-ph?searchtype=author&query=Marleau%2C+F+R">Francine R. Marleau</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P">Pierre-Alain Duc</a>, <a href="/search/astro-ph?searchtype=author&query=Lim%2C+S">Sungsoon Lim</a>, <a href="/search/astro-ph?searchtype=author&query=Posti%2C+L">Lorenzo Posti</a>, <a href="/search/astro-ph?searchtype=author&query=Agnello%2C+A">Adriano Agnello</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">R煤ben S谩nchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Poulain%2C+M">M茅lina Poulain</a>, <a href="/search/astro-ph?searchtype=author&query=Habas%2C+R">Rebecca Habas</a>, <a href="/search/astro-ph?searchtype=author&query=Emsellem%2C+E">Eric Emsellem</a>, <a href="/search/astro-ph?searchtype=author&query=Paudel%2C+S">Sanjaya Paudel</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Burg%2C+R+F+J">Remco F. J. van der Burg</a>, <a href="/search/astro-ph?searchtype=author&query=Fensch%2C+J">J茅r茅my Fensch</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2101.10659v2-abstract-short" style="display: inline;"> Ultra-diffuse galaxies (UDGs) are very low-surface brightness galaxies with large effective radii. Spectroscopic measurements of a few UDGs have revealed a low dark matter content, based on the internal motion of stars or globular clusters (GCs). This is in contrast to the large number of GCs found for these systems, from which it would be expected to correspond to a large dark matter halo mass. H… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.10659v2-abstract-full').style.display = 'inline'; document.getElementById('2101.10659v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.10659v2-abstract-full" style="display: none;"> Ultra-diffuse galaxies (UDGs) are very low-surface brightness galaxies with large effective radii. Spectroscopic measurements of a few UDGs have revealed a low dark matter content, based on the internal motion of stars or globular clusters (GCs). This is in contrast to the large number of GCs found for these systems, from which it would be expected to correspond to a large dark matter halo mass. Here we present HST+ACS observations for the UDG MATLAS-2019 in the NGC5846 group. Using the F606W and F814W filters, we trace the GC population two magnitudes below the peak of the GC luminosity function (GCLF). Employing Bayesian considerations, we identify 26+-6 GCs associated with the dwarf, yielding a large specific frequency of S_N=58+-14. We use the turnover of the GCLF to derive a distance of 21+-2 Mpc, which is consistent with the NGC5846 group of galaxies. Due to the superior image quality of the HST, we are able to resolve the GCs and measure their sizes, which are consistent with the sizes of GCs around Local Group galaxies. Using the linear relation between the total mass of galaxies and of GCs, we derive a halo mass of 0.9(+-0.2) *10^11 M_solar (M_solar/L_solar>1000). The high abundance of GCs, together with the small uncertainties, make MATLAS-2019 one of the most extreme UDGs, which likely sets an upper limit of the number of GCs for UDGs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.10659v2-abstract-full').style.display = 'none'; document.getElementById('2101.10659v2-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 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 10 figures, 1 table, accepted for publication in APJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.08393">arXiv:2012.08393</a> <span> [<a href="https://arxiv.org/pdf/2012.08393">pdf</a>, <a href="https://arxiv.org/format/2012.08393">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> </div> </div> <p class="title is-5 mathjax"> MOSAIC: the high-multiplex and multi-IFU spectrograph for the ELT </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">Rub茅n S谩nchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Hammer%2C+F">Francois Hammer</a>, <a href="/search/astro-ph?searchtype=author&query=Morris%2C+S">Simon Morris</a>, <a href="/search/astro-ph?searchtype=author&query=Cuby%2C+J">Jean-Gabriel Cuby</a>, <a href="/search/astro-ph?searchtype=author&query=Kaper%2C+L">Lex Kaper</a>, <a href="/search/astro-ph?searchtype=author&query=Steinmetz%2C+M">Matthias Steinmetz</a>, <a href="/search/astro-ph?searchtype=author&query=Afonso%2C+J">Jose Afonso</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">Beatriz Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=Bergin%2C+E">Edwin Bergin</a>, <a href="/search/astro-ph?searchtype=author&query=Finoguenov%2C+A">Alexis Finoguenov</a>, <a href="/search/astro-ph?searchtype=author&query=Gallego%2C+J">Jes煤s Gallego</a>, <a href="/search/astro-ph?searchtype=author&query=Kassin%2C+S">Susan Kassin</a>, <a href="/search/astro-ph?searchtype=author&query=Miller%2C+C">Christopher Miller</a>, <a href="/search/astro-ph?searchtype=author&query=%C3%96stlin%2C+G">Goran 脰stlin</a>, <a href="/search/astro-ph?searchtype=author&query=Pentericci%2C+L">Laura Pentericci</a>, <a href="/search/astro-ph?searchtype=author&query=Schaerer%2C+D">Daniel Schaerer</a>, <a href="/search/astro-ph?searchtype=author&query=Ziegler%2C+B">Bodo Ziegler</a>, <a href="/search/astro-ph?searchtype=author&query=Chemla%2C+F">Fanny Chemla</a>, <a href="/search/astro-ph?searchtype=author&query=Dalton%2C+G">Gavin Dalton</a>, <a href="/search/astro-ph?searchtype=author&query=De+Frondat%2C+F">Fatima De Frondat</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+C">Chris Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Mignant%2C+D+L">David Le Mignant</a>, <a href="/search/astro-ph?searchtype=author&query=Puech%2C+M">Mathieu Puech</a>, <a href="/search/astro-ph?searchtype=author&query=Rodrigues%2C+M">Myriam Rodrigues</a>, <a href="/search/astro-ph?searchtype=author&query=Taburet%2C+S">Sylvestre Taburet</a> , et al. (18 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2012.08393v1-abstract-short" style="display: inline;"> MOSAIC is the planned multi-object spectrograph for the 39m Extremely Large Telescope (ELT). Conceived as a multi-purpose instrument, it offers both high multiplex and multi-IFU capabilities at a range of intermediate to high spectral resolving powers in the visible and the near-infrared. MOSAIC will enable unique spectroscopic surveys of the faintest sources, from the oldest stars in the Galaxy a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.08393v1-abstract-full').style.display = 'inline'; document.getElementById('2012.08393v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.08393v1-abstract-full" style="display: none;"> MOSAIC is the planned multi-object spectrograph for the 39m Extremely Large Telescope (ELT). Conceived as a multi-purpose instrument, it offers both high multiplex and multi-IFU capabilities at a range of intermediate to high spectral resolving powers in the visible and the near-infrared. MOSAIC will enable unique spectroscopic surveys of the faintest sources, from the oldest stars in the Galaxy and beyond to the first populations of galaxies that completed the reionisation of the Universe--while simultaneously opening up a wide discovery space. In this contribution we present the status of the instrument ahead of Phase B, showcasing the key science cases as well as introducing the updated set of top level requirements and the adopted architecture. The high readiness level will allow MOSAIC to soon enter the construction phase, with the goal to provide the ELT community with a world-class MOS capability as soon as possible after the telescope first light. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.08393v1-abstract-full').style.display = 'none'; document.getElementById('2012.08393v1-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, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to SPIE</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.03960">arXiv:2012.03960</a> <span> [<a href="https://arxiv.org/pdf/2012.03960">pdf</a>, <a href="https://arxiv.org/format/2012.03960">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stab1783">10.1093/mnras/stab1783 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Pristine survey -- XII: Gemini-GRACES chemo-dynamical study of newly discovered extremely metal-poor stars in the Galaxy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kielty%2C+C+L">Collin L. Kielty</a>, <a href="/search/astro-ph?searchtype=author&query=Venn%2C+K+A">Kim A. Venn</a>, <a href="/search/astro-ph?searchtype=author&query=Sestito%2C+F">Federico Sestito</a>, <a href="/search/astro-ph?searchtype=author&query=Starkenburg%2C+E">Else Starkenburg</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+N+F">Nicolas F. Martin</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=Arentsen%2C+A">Anke Arentsen</a>, <a href="/search/astro-ph?searchtype=author&query=Fabbro%2C+S">S茅bastien Fabbro</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez%2C+J+I+G">Jonay I. Gonz谩lez Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+V">Vanessa Hill</a>, <a href="/search/astro-ph?searchtype=author&query=Jablonka%2C+P">Pascale Jablonka</a>, <a href="/search/astro-ph?searchtype=author&query=Lardo%2C+C">Carmela Lardo</a>, <a href="/search/astro-ph?searchtype=author&query=Mashonkina%2C+L+I">Lyudmila I. Mashonkina</a>, <a href="/search/astro-ph?searchtype=author&query=Navarro%2C+J+F">Julio F. Navarro</a>, <a href="/search/astro-ph?searchtype=author&query=Sneden%2C+C">Chris Sneden</a>, <a href="/search/astro-ph?searchtype=author&query=Thomas%2C+G+F">Guillaume F. Thomas</a>, <a href="/search/astro-ph?searchtype=author&query=Youakim%2C+K">Kris Youakim</a>, <a href="/search/astro-ph?searchtype=author&query=Bialek%2C+S">Spencer Bialek</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">Rub茅n S谩nchez-Janssen</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="2012.03960v2-abstract-short" style="display: inline;"> High-resolution optical spectra of 30 metal-poor stars selected from the \Pristine\ survey are presented, based on observations taken with the Gemini Observatory GRACES spectrograph. Stellar parameters \teff and \logg are determined using a Gaia DR2 colour-temperature calibration and surface gravity from the Stefan-Boltzmann equation. GRACES spectra are used to determine chemical abundances (or up… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.03960v2-abstract-full').style.display = 'inline'; document.getElementById('2012.03960v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.03960v2-abstract-full" style="display: none;"> High-resolution optical spectra of 30 metal-poor stars selected from the \Pristine\ survey are presented, based on observations taken with the Gemini Observatory GRACES spectrograph. Stellar parameters \teff and \logg are determined using a Gaia DR2 colour-temperature calibration and surface gravity from the Stefan-Boltzmann equation. GRACES spectra are used to determine chemical abundances (or upper-limits) for 20 elements (Li, O, Na, Mg, K, Ca, Ti, Sc, Cr, Mn, Fe, Ni, Cu, Zn, Y, Zr, Ba, La, Nd, Eu). These stars are confirmed to be metal-poor ([Fe/H]$<-2.5$), with higher precision than from earlier medium-resolution analyses. The chemistry for most targets is similar to other extremely metal-poor stars in the Galactic halo. Three stars near [Fe/H]$=-3.0$ have unusually low Ca and high Mg, suggestive of contributions from few SN~II where alpha-element formation through hydrostatic nucleosynthesis was more efficient. Three new carbon-enhanced metal-poor stars are also identified (two CEMP-s and one potential CEMP-no star) when our chemical abundances are combined with carbon from previous medium-resolution analyses. The GRACES spectra also provide precision radial velocities ($蟽_{\rm RV}\le0.2$km\,s$^{-1}$) for dynamical orbit calculations with the Gaia DR2 proper motions. Most of our targets are dynamically associated with the Galactic halo; however, five stars with [Fe/H]$<-3$ have planar-like orbits, including one retrograde star. Another five stars are dynamically consistent with the Gaia-Sequoia accretion event; three have typical halo [$伪$/Fe] ratios for their metallicities, whereas two are [Mg/Fe]-deficient, and one is a new CEMP-s candidate. These results are discussed in terms of the formation and early chemical evolution of the Galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.03960v2-abstract-full').style.display = 'none'; document.getElementById('2012.03960v2-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 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 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">18 pages, 15 figures plus additional figures and tables in the appendix. MNRAS accepted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2011.03549">arXiv:2011.03549</a> <span> [<a href="https://arxiv.org/pdf/2011.03549">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <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/10.18727/0722-6691/5220">10.18727/0722-6691/5220 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MOSAIC on the ELT: high-multiplex spectroscopy to unravel the physics of stars and galaxies from the dark ages to the present-day </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hammer%2C+F">F. Hammer</a>, <a href="/search/astro-ph?searchtype=author&query=Morris%2C+S">S. Morris</a>, <a href="/search/astro-ph?searchtype=author&query=Cuby%2C+J+G">J. G. Cuby</a>, <a href="/search/astro-ph?searchtype=author&query=Kaper%2C+L">L. Kaper</a>, <a href="/search/astro-ph?searchtype=author&query=Steinmetz%2C+M">M. Steinmetz</a>, <a href="/search/astro-ph?searchtype=author&query=Afonso%2C+J">J. Afonso</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuy%2C+B">B. Barbuy</a>, <a href="/search/astro-ph?searchtype=author&query=Bergin%2C+E">E. Bergin</a>, <a href="/search/astro-ph?searchtype=author&query=Finogenov%2C+A">A. Finogenov</a>, <a href="/search/astro-ph?searchtype=author&query=Gallego%2C+J">J. Gallego</a>, <a href="/search/astro-ph?searchtype=author&query=Kassin%2C+S">S. Kassin</a>, <a href="/search/astro-ph?searchtype=author&query=Miller%2C+C">C. Miller</a>, <a href="/search/astro-ph?searchtype=author&query=Ostlin%2C+G">G. Ostlin</a>, <a href="/search/astro-ph?searchtype=author&query=Penterricci%2C+L">L. Penterricci</a>, <a href="/search/astro-ph?searchtype=author&query=Schaerer%2C+D">D. Schaerer</a>, <a href="/search/astro-ph?searchtype=author&query=Ziegler%2C+B">B. Ziegler</a>, <a href="/search/astro-ph?searchtype=author&query=Chemla%2C+F">F. Chemla</a>, <a href="/search/astro-ph?searchtype=author&query=Dalton%2C+G">G. Dalton</a>, <a href="/search/astro-ph?searchtype=author&query=De+Frondat%2C+F">F. De Frondat</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+C">C. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Mignant%2C+D+L">D. Le Mignant</a>, <a href="/search/astro-ph?searchtype=author&query=Puech%2C+M">M. Puech</a>, <a href="/search/astro-ph?searchtype=author&query=Rodrigues%2C+M">M. Rodrigues</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez-Janssen%2C+R">R. Sanchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Taburet%2C+S">S. Taburet</a> , et al. (14 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="2011.03549v2-abstract-short" style="display: inline;"> The powerful combination of the cutting-edge multi-object spectrograph MOSAIC with the world largest telescope, the ELT, will allow us to probe deeper into the Universe than was possible. MOSAIC is an extremely efficient instrument in providing spectra for the numerous faint sources in the Universe, including the very first galaxies and sources of cosmic reionization. MOSAIC has a high multiplex i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.03549v2-abstract-full').style.display = 'inline'; document.getElementById('2011.03549v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.03549v2-abstract-full" style="display: none;"> The powerful combination of the cutting-edge multi-object spectrograph MOSAIC with the world largest telescope, the ELT, will allow us to probe deeper into the Universe than was possible. MOSAIC is an extremely efficient instrument in providing spectra for the numerous faint sources in the Universe, including the very first galaxies and sources of cosmic reionization. MOSAIC has a high multiplex in the NIR and in the VIS, in addition to multi-Integral Field Units (Multi-IFUs) in NIR. As such it is perfectly suited to carry out an inventory of dark matter (from rotation curves) and baryons in the cool-warm gas phases in galactic haloes at z=3-4. MOSAIC will enable detailed maps of the intergalactic medium at z=3, the evolutionary history of dwarf galaxies during a Hubble time, the chemistry directly measured from stars up to several Mpc. Finally, it will measure all faint features seen in cluster gravitational lenses or in streams surrounding nearby galactic halos, providing MOSAIC to be a powerful instrument with an extremely large space of discoveries. The preliminary design of MOSAIC is expected to begin next year, and its level of readiness is already high, given the instrumental studies made by the team. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.03549v2-abstract-full').style.display = 'none'; document.getElementById('2011.03549v2-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 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 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">8 pages, 4 Figures, Pre-edited version, to appear in the ESO Messenger No.182 - Quarter 1 2021 - Version identical to the Edited one</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.15275">arXiv:2007.15275</a> <span> [<a href="https://arxiv.org/pdf/2007.15275">pdf</a>, <a href="https://arxiv.org/format/2007.15275">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/abad91">10.3847/1538-4365/abad91 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Next Generation Virgo Cluster Survey. XXXIV. Ultra-Compact Dwarf (UCD) Galaxies in the Virgo Cluster </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Liu%2C+C">Chengze Liu</a>, <a href="/search/astro-ph?searchtype=author&query=C%C3%B4t%C3%A9%2C+P">Patrick C么t茅</a>, <a href="/search/astro-ph?searchtype=author&query=Peng%2C+E+W">Eric W. Peng</a>, <a href="/search/astro-ph?searchtype=author&query=Roediger%2C+J">Joel Roediger</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+H">Hongxin Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrarese%2C+L">Laura Ferrarese</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">Rub茅n S谩nchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Guhathakurta%2C+P">Puragra Guhathakurta</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+X">Xiaohu Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Jing%2C+Y">Yipeng Jing</a>, <a href="/search/astro-ph?searchtype=author&query=Alamo-Martinez%2C+K">Karla Alamo-Martinez</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Boselli%2C+A">Alessandro Boselli</a>, <a href="/search/astro-ph?searchtype=author&query=Cuilandre%2C+J">Jean-Charles Cuilandre</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P">Pierre-Alain Duc</a>, <a href="/search/astro-ph?searchtype=author&query=Durrell%2C+P">Patrick Durrell</a>, <a href="/search/astro-ph?searchtype=author&query=Gwyn%2C+S">Stephen Gwyn</a>, <a href="/search/astro-ph?searchtype=author&query=Jord%C3%A1n%2C+A">Andres Jord谩n</a>, <a href="/search/astro-ph?searchtype=author&query=Ko%2C+Y">Youkyung Ko</a>, <a href="/search/astro-ph?searchtype=author&query=Lan%C3%A7on%2C+A">Ariane Lan莽on</a>, <a href="/search/astro-ph?searchtype=author&query=Lim%2C+S">Sungsoon Lim</a>, <a href="/search/astro-ph?searchtype=author&query=Longobardi%2C+A">Alessia Longobardi</a>, <a href="/search/astro-ph?searchtype=author&query=Mei%2C+S">Simona Mei</a>, <a href="/search/astro-ph?searchtype=author&query=Mihos%2C+J+C">J. Christopher Mihos</a>, <a href="/search/astro-ph?searchtype=author&query=Munoz%2C+R">Roberto Munoz</a> , et al. (4 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2007.15275v1-abstract-short" style="display: inline;"> We present a study of ultra compact dwarf (UCD) galaxies in the Virgo cluster based mainly on imaging from the Next Generation Virgo Cluster Survey (NGVS). Using $\sim$100 deg$^{2}$ of $u^*giz$ imaging, we have identified more than 600 candidate UCDs, from the core of Virgo out to its virial radius. Candidates have been selected through a combination of magnitudes, ellipticities, colors, surface b… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.15275v1-abstract-full').style.display = 'inline'; document.getElementById('2007.15275v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.15275v1-abstract-full" style="display: none;"> We present a study of ultra compact dwarf (UCD) galaxies in the Virgo cluster based mainly on imaging from the Next Generation Virgo Cluster Survey (NGVS). Using $\sim$100 deg$^{2}$ of $u^*giz$ imaging, we have identified more than 600 candidate UCDs, from the core of Virgo out to its virial radius. Candidates have been selected through a combination of magnitudes, ellipticities, colors, surface brightnesses, half-light radii and, when available, radial velocities. Candidates were also visually validated from deep NGVS images. Subsamples of varying completeness and purity have been defined to explore the properties of UCDs and compare to those of globular clusters and the nuclei of dwarf galaxies with the aim of delineating the nature and origins of UCDs. From a surface density map, we find the UCDs to be mostly concentrated within Virgo's main subclusters, around its brightest galaxies. We identify several subsamples of UCDs -- i.e., the brightest, largest, and those with the most pronounced and/or asymmetric envelopes -- that could hold clues to the origin of UCDs and possible evolutionary links with dwarf nuclei. We find some evidence for such a connection from the existence of diffuse envelopes around some UCDs, and comparisons of radial distributions of UCDs and nucleated galaxies within the cluster. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.15275v1-abstract-full').style.display = 'none'; document.getElementById('2007.15275v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 July, 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">70 pages, 24 figures, 6 tables, accepted for publication in ApJS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.10565">arXiv:2007.10565</a> <span> [<a href="https://arxiv.org/pdf/2007.10565">pdf</a>, <a href="https://arxiv.org/format/2007.10565">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/aba433">10.3847/1538-4357/aba433 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Next Generation Virgo Cluster Survey (NGVS). XXX. Ultra-Diffuse Galaxies and their Globular Cluster Systems </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lim%2C+S">Sungsoon Lim</a>, <a href="/search/astro-ph?searchtype=author&query=C%C3%B4t%C3%A9%2C+P">Patrick C么t茅</a>, <a href="/search/astro-ph?searchtype=author&query=Peng%2C+E+W">Eric W. Peng</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrarese%2C+L">Laura Ferrarese</a>, <a href="/search/astro-ph?searchtype=author&query=Roediger%2C+J+C">Joel C. Roediger</a>, <a href="/search/astro-ph?searchtype=author&query=Durrell%2C+P+R">Patrick R. Durrell</a>, <a href="/search/astro-ph?searchtype=author&query=Mihos%2C+J+C">J. Christopher Mihos</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+K">Kaixiang Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Gwyn%2C+S+D+J">S. D. J. Gwyn</a>, <a href="/search/astro-ph?searchtype=author&query=Cuillandre%2C+J">Jean-Charles Cuillandre</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+C">Chengze Liu</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">Rub茅n S谩nchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Toloba%2C+E">Elisa Toloba</a>, <a href="/search/astro-ph?searchtype=author&query=Sales%2C+L+V">Laura V. Sales</a>, <a href="/search/astro-ph?searchtype=author&query=Guhathakurta%2C+P">Puragra Guhathakurta</a>, <a href="/search/astro-ph?searchtype=author&query=Lan%C3%A7on%2C+A">Ariane Lan莽on</a>, <a href="/search/astro-ph?searchtype=author&query=Puzia%2C+T+H">Thomas H. Puzia</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="2007.10565v1-abstract-short" style="display: inline;"> We present a study of ultra-diffuse galaxies (UDGs) in the Virgo Cluster based on deep imaging from the Next Generation Virgo Cluster Survey (NGVS). Applying a new definition for the UDG class based on galaxy scaling relations, we define samples of 44 and 26 UDGs using expansive and restrictive selection criteria, respectively. Our UDG sample includes objects that are significantly fainter than pr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.10565v1-abstract-full').style.display = 'inline'; document.getElementById('2007.10565v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.10565v1-abstract-full" style="display: none;"> We present a study of ultra-diffuse galaxies (UDGs) in the Virgo Cluster based on deep imaging from the Next Generation Virgo Cluster Survey (NGVS). Applying a new definition for the UDG class based on galaxy scaling relations, we define samples of 44 and 26 UDGs using expansive and restrictive selection criteria, respectively. Our UDG sample includes objects that are significantly fainter than previously known UDGs: i.e., more than half are fainter than $\langle渭\rangle_e \sim27.5$ mag arcsec$^{-2}$. The UDGs in Virgo's core region show some evidence for being structurally distinct from "normal" dwarf galaxies, but this separation disappears when considering the full sample of galaxies throughout the cluster. UDGs are more centrally concentrated in their spatial distribution than other Virgo galaxies of similar luminosity, while their morphologies demonstrate that at least some UDGs owe their diffuse nature to physical processes---such as tidal interactions or low-mass mergers---that are at play within the cluster environment. The globular cluster (GC) systems of Virgo UDGs have a wide range in specific frequency ($S_N$), with a higher mean $S_N$ than "normal" Virgo dwarfs, but a lower mean $S_N$ than Coma UDGs at fixed luminosity. Their GCs are predominantly blue, with a small contribution from red clusters in the more massive UDGs. The combined GC luminosity function is consistent with those observed in dwarf galaxies, showing no evidence of being anomalously luminous. The diversity in their morphologies and their GC properties suggests no single process has given rise to all objects within the UDG class. Based on the available evidence, we conclude that UDGs are simply those systems that occupy the extended tails of the galaxy size and surface brightness distributions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.10565v1-abstract-full').style.display = 'none'; document.getElementById('2007.10565v1-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 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">31 pages, 16 figures, 4 tables, accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2006.08641">arXiv:2006.08641</a> <span> [<a href="https://arxiv.org/pdf/2006.08641">pdf</a>, <a href="https://arxiv.org/format/2006.08641">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/staa1661">10.1093/mnras/staa1661 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Pristine Inner Galaxy Survey (PIGS) II: Uncovering the most metal-poor populations in the inner Milky Way </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Arentsen%2C+A">Anke Arentsen</a>, <a href="/search/astro-ph?searchtype=author&query=Starkenburg%2C+E">Else Starkenburg</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+N+F">Nicolas F. Martin</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=Zucker%2C+D+B">Daniel B. Zucker</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+C+A">Carlos Allende Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+V">Vanessa Hill</a>, <a href="/search/astro-ph?searchtype=author&query=Venn%2C+K+A">Kim. A. Venn</a>, <a href="/search/astro-ph?searchtype=author&query=Carlberg%2C+R+G">Raymond G. Carlberg</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez%2C+J+I+G">Jonay I. Gonz谩lez Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Mashonkina%2C+L+I">Lyudmila I. Mashonkina</a>, <a href="/search/astro-ph?searchtype=author&query=Navarro%2C+J+F">Julio F. Navarro</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">Rub茅n S谩nchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Schultheis%2C+M">Mathias Schultheis</a>, <a href="/search/astro-ph?searchtype=author&query=Thomas%2C+G+F">Guillaume F. Thomas</a>, <a href="/search/astro-ph?searchtype=author&query=Youakim%2C+K">Kris Youakim</a>, <a href="/search/astro-ph?searchtype=author&query=Lewis%2C+G+F">Geraint F. Lewis</a>, <a href="/search/astro-ph?searchtype=author&query=Simpson%2C+J+D">Jeffrey D. Simpson</a>, <a href="/search/astro-ph?searchtype=author&query=Wan%2C+Z">Zhen Wan</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R+E">Roger E. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Geisler%2C+D">Doug Geisler</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Connell%2C+J+E">Julia E. O'Connell</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2006.08641v1-abstract-short" style="display: inline;"> Metal-poor stars are important tools for tracing the early history of the Milky Way, and for learning about the first generations of stars. Simulations suggest that the oldest metal-poor stars are to be found in the inner Galaxy. Typical bulge surveys, however, lack low metallicity ([Fe/H] < -1.0) stars because the inner Galaxy is predominantly metal-rich. The aim of the Pristine Inner Galaxy Surv… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.08641v1-abstract-full').style.display = 'inline'; document.getElementById('2006.08641v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2006.08641v1-abstract-full" style="display: none;"> Metal-poor stars are important tools for tracing the early history of the Milky Way, and for learning about the first generations of stars. Simulations suggest that the oldest metal-poor stars are to be found in the inner Galaxy. Typical bulge surveys, however, lack low metallicity ([Fe/H] < -1.0) stars because the inner Galaxy is predominantly metal-rich. The aim of the Pristine Inner Galaxy Survey (PIGS) is to study the metal-poor and very metal-poor (VMP, [Fe/H] < -2.0) stars in this region. In PIGS, metal-poor targets for spectroscopic follow-up are selected from metallicity-sensitive CaHK photometry from the CFHT. This work presents the ~250 deg^2 photometric survey as well as intermediate-resolution spectroscopic follow-up observations for ~8000 stars using AAOmega on the AAT. The spectra are analysed using two independent tools: ULySS with an empirical spectral library, and FERRE with a library of synthetic spectra. The comparison between the two methods enables a robust determination of the stellar parameters and their uncertainties. We present a sample of 1300 VMP stars -- the largest sample of VMP stars in the inner Galaxy to date. Additionally, our spectroscopic dataset includes ~1700 horizontal branch stars, which are useful metal-poor standard candles. We furthermore show that PIGS photometry selects VMP stars with unprecedented efficiency: 86%/80% (lower/higher extinction) of the best candidates satisfy [Fe/H] < -2.0, as do 80%/63% of a larger, less strictly selected sample. We discuss future applications of this unique dataset that will further our understanding of the chemical and dynamical evolution of the innermost regions of our Galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.08641v1-abstract-full').style.display = 'none'; document.getElementById('2006.08641v1-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, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted for publication in MNRAS, 17 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/2006.04606">arXiv:2006.04606</a> <span> [<a href="https://arxiv.org/pdf/2006.04606">pdf</a>, <a href="https://arxiv.org/format/2006.04606">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/10.1051/0004-6361/202038351">10.1051/0004-6361/202038351 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A spectroscopic study of MATLAS-2019 with MUSE: an ultra-diffuse galaxy with an excess of old globular clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=M%C3%BCller%2C+O">Oliver M眉ller</a>, <a href="/search/astro-ph?searchtype=author&query=Marleau%2C+F+R">Francine R. Marleau</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P">Pierre-Alain Duc</a>, <a href="/search/astro-ph?searchtype=author&query=Habas%2C+R">Rebecca Habas</a>, <a href="/search/astro-ph?searchtype=author&query=Fensch%2C+J">J茅r茅my Fensch</a>, <a href="/search/astro-ph?searchtype=author&query=Emsellem%2C+E">Eric Emsellem</a>, <a href="/search/astro-ph?searchtype=author&query=Poulain%2C+M">M茅lina Poulain</a>, <a href="/search/astro-ph?searchtype=author&query=Lim%2C+S">Sungsoon Lim</a>, <a href="/search/astro-ph?searchtype=author&query=Agnello%2C+A">Adriano Agnello</a>, <a href="/search/astro-ph?searchtype=author&query=Durrell%2C+P">Patrick Durrell</a>, <a href="/search/astro-ph?searchtype=author&query=Paudel%2C+S">Sanjaya Paudel</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">Rub茅n S谩nchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Burg%2C+R+F+J">Remco F. J. van der Burg</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2006.04606v1-abstract-short" style="display: inline;"> The MATLAS deep imaging survey has uncovered a plethora of dwarf galaxies in the low density environment it has mapped. A fraction of them are unusually extended and have a low-surface brightness. Among these so-called ultra-diffuse galaxies, a few seem to host an excess of globular clusters. With the integral-field unit spectrograph MUSE we have observed one of these galaxies - MATLAS J15052031+0… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.04606v1-abstract-full').style.display = 'inline'; document.getElementById('2006.04606v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2006.04606v1-abstract-full" style="display: none;"> The MATLAS deep imaging survey has uncovered a plethora of dwarf galaxies in the low density environment it has mapped. A fraction of them are unusually extended and have a low-surface brightness. Among these so-called ultra-diffuse galaxies, a few seem to host an excess of globular clusters. With the integral-field unit spectrograph MUSE we have observed one of these galaxies - MATLAS J15052031+0148447 (MATLAS-2019) - located towards the nearby group NGC 5846 and measured its systemic velocity,age, and metallicity, and that of its globular clusters candidates. For the stellar body of MATLAS-2019 we derive a metallicity of -1.33+0.19-0.01 dex and an age of 11.2+1.8-0.8 Gyr. For some of the individual GCs and the stacked GC population, we derive consistent ages and metallicities. From the 11 confirmed globular clusters and using a Markov Chain Monte Carlo approach we derived a dynamical mass-to-light ratio of 4.2+8.6-3.4M/L. This is at the lower end of the luminosity-mass scaling relation defined by the Local Group dwarf galaxies. Furthermore, we couldn't confirm nor reject the possibility of a rotational component of the GC system. If present, this would further modify the inferred mass. Follow-up observations of the globular cluster population and of the stellar body of the galaxy are needed to assess whether this galaxy is lacking dark matter like it was suggested for the pair of dwarf galaxies in the field of NGC 1052, or if this is a miss-interpretation arising from systematic uncertainties of the method commonly used for these systems and the large uncertainties of the individual globular cluster velocities. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.04606v1-abstract-full').style.display = 'none'; document.getElementById('2006.04606v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 9 figures, 2 tables, accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 640, A106 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2005.05976">arXiv:2005.05976</a> <span> [<a href="https://arxiv.org/pdf/2005.05976">pdf</a>, <a href="https://arxiv.org/format/2005.05976">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/stab604">10.1093/mnras/stab604 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Pristine Dwarf-Galaxy survey -- III. Revealing the nature of the Milky Way globular cluster Sagittarius II </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Longeard%2C+N">Nicolas Longeard</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+N">Nicolas Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Ibata%2C+R">Rodrigo Ibata</a>, <a href="/search/astro-ph?searchtype=author&query=Starkenburg%2C+E">Else Starkenburg</a>, <a href="/search/astro-ph?searchtype=author&query=Jablonka%2C+P">Pascale Jablonka</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=Carlberg%2C+R+G">Raymond G. Carlberg</a>, <a href="/search/astro-ph?searchtype=author&query=C%C3%B4t%C3%A9%2C+P">Patrick C么t茅</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez%2C+J+I+G">Jonay I. Gonz谩lez Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Lucchesi%2C+R">Romain Lucchesi</a>, <a href="/search/astro-ph?searchtype=author&query=Malhan%2C+K">Khyati Malhan</a>, <a href="/search/astro-ph?searchtype=author&query=Navarro%2C+J+F">Julio F. Navarro</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">Rub茅n S谩nchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Thomas%2C+G+F">Guillaume F. Thomas</a>, <a href="/search/astro-ph?searchtype=author&query=Venn%2C+K">Kim Venn</a>, <a href="/search/astro-ph?searchtype=author&query=McConnachie%2C+A+W">Alan W. McConnachie</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="2005.05976v1-abstract-short" style="display: inline;"> We present a new spectroscopic study of the faint Milky Way satellite Sagittarius II. Using multi-object spectroscopy from the Fibre Large Array Multi Element Spectrograph, we supplement the dataset of Longeard et al. (2020) with 47 newly observed stars, 19 of which are identified as members of the satellite. These additional member stars are used to put tighter constraints on the dynamics and the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.05976v1-abstract-full').style.display = 'inline'; document.getElementById('2005.05976v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2005.05976v1-abstract-full" style="display: none;"> We present a new spectroscopic study of the faint Milky Way satellite Sagittarius II. Using multi-object spectroscopy from the Fibre Large Array Multi Element Spectrograph, we supplement the dataset of Longeard et al. (2020) with 47 newly observed stars, 19 of which are identified as members of the satellite. These additional member stars are used to put tighter constraints on the dynamics and the metallicity properties of the system. We find a low velocity dispersion of SgrII v = 1.7 +/- 0.5 km s-1, in agreement with the dispersion of Milky Way globular clusters of similar luminosity. We confirm the very metal-poor nature of the satellite ([Fe/H]_SgrII = -2.23 +/- 0.07) and find that the metallicity dispersion of Sgr II is not resolved, reaching only 0.20 at the 95% confidence limit. No star with a metallicity below -2.5 is confidently detected. Therefore, despite the unusually large size of the system (rh = 35.5 +1.4-1.2 pc), we conclude that Sgr II is an old and metal-poor globular cluster of the Milky Way. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.05976v1-abstract-full').style.display = 'none'; document.getElementById('2005.05976v1-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 May, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2020. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2005.01532">arXiv:2005.01532</a> <span> [<a href="https://arxiv.org/pdf/2005.01532">pdf</a>, <a href="https://arxiv.org/format/2005.01532">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/staa1261">10.1093/mnras/staa1261 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Next Generation Fornax Survey (NGFS): VII. A MUSE view of the nuclear star clusters in Fornax dwarf galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Johnston%2C+E+J">Evelyn J. Johnston</a>, <a href="/search/astro-ph?searchtype=author&query=Puzia%2C+T+H">Thomas H. Puzia</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=Eigenthaler%2C+P">Paul Eigenthaler</a>, <a href="/search/astro-ph?searchtype=author&query=Galaz%2C+G">Gaspar Galaz</a>, <a href="/search/astro-ph?searchtype=author&query=H%C3%A4u%C3%9Fler%2C+B">Boris H盲u脽ler</a>, <a href="/search/astro-ph?searchtype=author&query=Mora%2C+M+D">Marcelo D. Mora</a>, <a href="/search/astro-ph?searchtype=author&query=Ordenes-Brice%C3%B1o%2C+Y">Yasna Ordenes-Brice帽o</a>, <a href="/search/astro-ph?searchtype=author&query=Rong%2C+Y">Yu Rong</a>, <a href="/search/astro-ph?searchtype=author&query=Spengler%2C+C">Chelsea Spengler</a>, <a href="/search/astro-ph?searchtype=author&query=Vogt%2C+F">Fr茅d茅ric Vogt</a>, <a href="/search/astro-ph?searchtype=author&query=C%C3%B4t%C3%A9%2C+P">Patrick C么t茅</a>, <a href="/search/astro-ph?searchtype=author&query=Grebel%2C+E+K">Eva K. Grebel</a>, <a href="/search/astro-ph?searchtype=author&query=Hilker%2C+M">Michael Hilker</a>, <a href="/search/astro-ph?searchtype=author&query=Mieske%2C+S">Steffen Mieske</a>, <a href="/search/astro-ph?searchtype=author&query=Miller%2C+B">Bryan Miller</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">Ruben S谩nchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Taylor%2C+M+A">Matthew A. Taylor</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+H">Hong-Xin Zhang</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="2005.01532v1-abstract-short" style="display: inline;"> Clues to the formation and evolution of Nuclear Star Clusters (NSCs) lie in their stellar populations. However, these structures are often very faint compared to their host galaxy, and spectroscopic analysis of NSCs is hampered by contamination of light from the rest of the system. With the introduction of wide-field IFU spectrographs, new techniques have been developed to model the light from dif… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.01532v1-abstract-full').style.display = 'inline'; document.getElementById('2005.01532v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2005.01532v1-abstract-full" style="display: none;"> Clues to the formation and evolution of Nuclear Star Clusters (NSCs) lie in their stellar populations. However, these structures are often very faint compared to their host galaxy, and spectroscopic analysis of NSCs is hampered by contamination of light from the rest of the system. With the introduction of wide-field IFU spectrographs, new techniques have been developed to model the light from different components within galaxies, making it possible to cleanly extract the spectra of the NSCs and study their properties with minimal contamination from the light of the rest of the galaxy. This work presents the analysis of the NSCs in a sample of 12 dwarf galaxies in the Fornax Cluster observed with MUSE. Analysis of the stellar populations and star-formation histories reveal that all the NSCs show evidence of multiple episodes of star formation, indicating that they have built up their mass further since their initial formation. The NSCs were found to have systematically lower metallicities than their host galaxies, which is consistent with a scenario for mass-assembly through mergers with infalling globular clusters, while the presence of younger stellar populations and gas emission in the core of two galaxies is indicative of in-situ star formation. We conclude that the NSCs in these dwarf galaxies likely originated as globular clusters that migrated to the core of the galaxy which have built up their mass mainly through mergers with other infalling clusters, with gas-inflow leading to in-situ star formation playing a secondary role. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.01532v1-abstract-full').style.display = 'none'; document.getElementById('2005.01532v1-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 May, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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, 13 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/2001.01670">arXiv:2001.01670</a> <span> [<a href="https://arxiv.org/pdf/2001.01670">pdf</a>, <a href="https://arxiv.org/format/2001.01670">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ab64e9">10.3847/1538-4357/ab64e9 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Strikingly Metal-Rich Halo of the Sombrero Galaxy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R+E">Roger E. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Goudfrooij%2C+P">Paul Goudfrooij</a>, <a href="/search/astro-ph?searchtype=author&query=Correnti%2C+M">Matteo Correnti</a>, <a href="/search/astro-ph?searchtype=author&query=Gnedin%2C+O+Y">Oleg Y. Gnedin</a>, <a href="/search/astro-ph?searchtype=author&query=Harris%2C+W+E">William E. Harris</a>, <a href="/search/astro-ph?searchtype=author&query=Chandar%2C+R">Rupali Chandar</a>, <a href="/search/astro-ph?searchtype=author&query=Puzia%2C+T+H">Thomas H. Puzia</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez-Janssen%2C+R">Ruben Sanchez-Janssen</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="2001.01670v2-abstract-short" style="display: inline;"> The nature of the Sombrero galaxy (M 104 = NGC 4594) has remained elusive despite many observational studies at a variety of wavelengths. Here we present Hubble Space Telescope imaging of two fields at $\sim$16 and 33 kpc along the minor axis to examine stellar metallicity gradients in the extended spheroid. We use this imaging, extending more than 2 mag below the tip of the red giant branch (TRGB… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.01670v2-abstract-full').style.display = 'inline'; document.getElementById('2001.01670v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2001.01670v2-abstract-full" style="display: none;"> The nature of the Sombrero galaxy (M 104 = NGC 4594) has remained elusive despite many observational studies at a variety of wavelengths. Here we present Hubble Space Telescope imaging of two fields at $\sim$16 and 33 kpc along the minor axis to examine stellar metallicity gradients in the extended spheroid. We use this imaging, extending more than 2 mag below the tip of the red giant branch (TRGB), in combination with artificial star tests to forward model observed color-magnitude diagrams (CMDs), measuring metallicity distribution functions (MDFs) at different radii along the minor axis. An important and unexpected result is that the halo of the Sombrero is strikingly metal-rich: even the outer field, located at $\sim$17 effective radii of the bulge, has a median metallicity [Z/H]$\sim$-0.15 and the fraction of stars with [Z/H]<-1.0 is negligible. This is unprecedented among massive galaxy halos studied to date, even among giant ellipticals. We find significant radial metallicity gradients, characterized by an increase in the fraction of metal-poor stars with radius and a gradient in median metallicity of $\sim$-0.01 dex/kpc. The density profile is well fit by power laws with slopes that exhibit a dependence on metallicity, with flatter slopes for more metal-poor stars. We discuss our results in the context of recent stellar MDF studies of other nearby galaxies and potential formation scenarios for the Sombrero galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.01670v2-abstract-full').style.display = 'none'; document.getElementById('2001.01670v2-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 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 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">ApJ accepted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1911.08491">arXiv:1911.08491</a> <span> [<a href="https://arxiv.org/pdf/1911.08491">pdf</a>, <a href="https://arxiv.org/ps/1911.08491">ps</a>, <a href="https://arxiv.org/format/1911.08491">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnrasl/slaa022">10.1093/mnrasl/slaa022 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Pristine survey X: a large population of low-metallicity stars permeates the Galactic disk </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sestito%2C+F">Federico Sestito</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+N+F">Nicolas F. Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Starkenburg%2C+E">Else Starkenburg</a>, <a href="/search/astro-ph?searchtype=author&query=Arentsen%2C+A">Anke Arentsen</a>, <a href="/search/astro-ph?searchtype=author&query=Ibata%2C+R+A">Rodrigo A. Ibata</a>, <a href="/search/astro-ph?searchtype=author&query=Longeard%2C+N">Nicolas Longeard</a>, <a href="/search/astro-ph?searchtype=author&query=Kielty%2C+C">Collin Kielty</a>, <a href="/search/astro-ph?searchtype=author&query=Youakim%2C+K">Kristopher Youakim</a>, <a href="/search/astro-ph?searchtype=author&query=Venn%2C+K+A">Kim A. Venn</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=Carlberg%2C+R+G">Raymond G. Carlberg</a>, <a href="/search/astro-ph?searchtype=author&query=Hernandez%2C+J+I+G">Jonay I. Gonzalez Hernandez</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+V">Vanessa Hill</a>, <a href="/search/astro-ph?searchtype=author&query=Jablonka%2C+P">Pascale Jablonka</a>, <a href="/search/astro-ph?searchtype=author&query=Kordopatis%2C+G">Georges Kordopatis</a>, <a href="/search/astro-ph?searchtype=author&query=Malhan%2C+K">Khyati Malhan</a>, <a href="/search/astro-ph?searchtype=author&query=Navarro%2C+J+F">Julio F. Navarro</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez-Janssen%2C+R">Ruben Sanchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Thomas%2C+G">Guillame Thomas</a>, <a href="/search/astro-ph?searchtype=author&query=Tolstoy%2C+E">Eline Tolstoy</a>, <a href="/search/astro-ph?searchtype=author&query=Wilson%2C+T+G">Thomas G. Wilson</a>, <a href="/search/astro-ph?searchtype=author&query=Palicio%2C+P+A">Pedro Alonso Palicio</a>, <a href="/search/astro-ph?searchtype=author&query=Bialek%2C+S">Spencer Bialek</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia-Dias%2C+R">Rafael Garcia-Dias</a>, <a href="/search/astro-ph?searchtype=author&query=Lucchesi%2C+R">Romain Lucchesi</a> , et al. (4 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1911.08491v1-abstract-short" style="display: inline;"> The orbits of the least chemically enriched stars open a window on the formation of our Galaxy when it was still in its infancy. The common picture is that these low-metallicity stars are distributed as an isotropic, pressure-supported component since these stars were either accreted from the early building blocks of the assembling Milky Way, or were later brought by the accretion of faint dwarf g… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.08491v1-abstract-full').style.display = 'inline'; document.getElementById('1911.08491v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1911.08491v1-abstract-full" style="display: none;"> The orbits of the least chemically enriched stars open a window on the formation of our Galaxy when it was still in its infancy. The common picture is that these low-metallicity stars are distributed as an isotropic, pressure-supported component since these stars were either accreted from the early building blocks of the assembling Milky Way, or were later brought by the accretion of faint dwarf galaxies. Combining the metallicities and radial velocities from the Pristine and LAMOST surveys and Gaia DR2 parallaxes and proper motions for an unprecedented large and unbiased sample of very metal-poor stars at $[Fe/H]\leq-2.5$ we show that this picture is incomplete. This sample shows strong statistical evidence (at the $5.0蟽$ level) of asymmetry in their kinematics, favouring prograde motion. Moreover, we find that $31\%$ of the stars that currently reside in the disk do not venture outside of the disk plane throughout their orbit. The discovery of this population implies that a significant fraction of stars with iron abundances $[Fe/H]\leq-2.5$ formed within or concurrently with the Milky Way disk and that the history of the disk was quiet enough to allow them to retain their disk-like orbital properties. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.08491v1-abstract-full').style.display = 'none'; document.getElementById('1911.08491v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 November, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to MNRAS letter, 5 pages with 1 figure. Appendices A and B with 3 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1911.00021">arXiv:1911.00021</a> <span> [<a href="https://arxiv.org/pdf/1911.00021">pdf</a>, <a href="https://arxiv.org/format/1911.00021">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/10.1051/0004-6361/201936048">10.1051/0004-6361/201936048 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Simulating MOS science on the ELT: Ly$伪$ forest tomography </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Japelj%2C+J">J. Japelj</a>, <a href="/search/astro-ph?searchtype=author&query=Laigle%2C+C">C. Laigle</a>, <a href="/search/astro-ph?searchtype=author&query=Puech%2C+M">M. Puech</a>, <a href="/search/astro-ph?searchtype=author&query=Pichon%2C+C">C. Pichon</a>, <a href="/search/astro-ph?searchtype=author&query=Rahmani%2C+H">H. Rahmani</a>, <a href="/search/astro-ph?searchtype=author&query=Dubois%2C+Y">Y. Dubois</a>, <a href="/search/astro-ph?searchtype=author&query=Devriendt%2C+J+E+G">J. E. G. Devriendt</a>, <a href="/search/astro-ph?searchtype=author&query=Petitjean%2C+P">P. Petitjean</a>, <a href="/search/astro-ph?searchtype=author&query=Hammer%2C+F">F. Hammer</a>, <a href="/search/astro-ph?searchtype=author&query=Gendron%2C+E">E. Gendron</a>, <a href="/search/astro-ph?searchtype=author&query=Kaper%2C+L">L. Kaper</a>, <a href="/search/astro-ph?searchtype=author&query=Morris%2C+S">S. Morris</a>, <a href="/search/astro-ph?searchtype=author&query=Pirzkal%2C+N">N. Pirzkal</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">R. S谩nchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Slyz%2C+A">A. Slyz</a>, <a href="/search/astro-ph?searchtype=author&query=Vergani%2C+S+D">S. D. Vergani</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+Y">Y. Yang</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1911.00021v2-abstract-short" style="display: inline;"> Mapping of the large-scale structure through cosmic time has numerous applications in the studies of cosmology and galaxy evolution. At $z > 2$, the structure can be traced by the neutral intergalactic medium (IGM) by way of observing the Ly$伪$, forest towards densely-sampled lines-of-sight of bright background sources, such as quasars and star forming galaxies. We investigate the scientific poten… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.00021v2-abstract-full').style.display = 'inline'; document.getElementById('1911.00021v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1911.00021v2-abstract-full" style="display: none;"> Mapping of the large-scale structure through cosmic time has numerous applications in the studies of cosmology and galaxy evolution. At $z > 2$, the structure can be traced by the neutral intergalactic medium (IGM) by way of observing the Ly$伪$, forest towards densely-sampled lines-of-sight of bright background sources, such as quasars and star forming galaxies. We investigate the scientific potential of MOSAIC, a planned multi-object spectrograph on the European Extremely Large Telescope (ELT), for the 3D mapping of the IGM at $z \gtrsim 3$. We simulate a survey of $3 \lesssim z \lesssim 4$ galaxies down to a limiting magnitude of $m_{r}\sim 25.5$ mag in an area of 1 degree$^2$ in the sky. Galaxies and their spectra (including the line-of-sight Ly$伪$ absorption) are taken from the lightcone extracted from the Horizon-AGN cosmological hydrodynamical simulation. The quality of the reconstruction of the original density field is studied for different spectral resolutions and signal-to-noise ratios of the spectra. We demonstrate that the minimum $S/N$ (per resolution element) of the faintest galaxies that such survey has to reach is $S/N = 4$. We show that a survey with such sensitivity enables a robust extraction of cosmic filaments and the detection of the theoretically-predicted galaxy stellar mass and star-formation rate gradients towards filaments. By simulating the realistic performance of MOSAIC we obtain $S/N(T_{\rm obs}, R, m_{r})$ scaling relations. We estimate that $\lesssim 35~(65)$ nights of observation time are required to carry out the survey with the instrument's high multiplex mode and with the spectral resolution of $R=1000~(2000)$. A survey with a MOSAIC-concept instrument on the ELT is found to enable the mapping of the IGM at $z > 3$ on Mpc scales, and as such will be complementary to and competitive with other planned IGM tomography surveys. [abridged] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.00021v2-abstract-full').style.display = 'none'; document.getElementById('1911.00021v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 November, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 31 October, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages, accepted to A&A; language edited</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 632, A94 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1910.13462">arXiv:1910.13462</a> <span> [<a href="https://arxiv.org/pdf/1910.13462">pdf</a>, <a href="https://arxiv.org/format/1910.13462">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/stz3045">10.1093/mnras/stz3045 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Newly discovered dwarf galaxies in the MATLAS low density fields </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Habas%2C+R">Rebecca Habas</a>, <a href="/search/astro-ph?searchtype=author&query=Marleau%2C+F+R">Francine R. Marleau</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P">Pierre-Alain Duc</a>, <a href="/search/astro-ph?searchtype=author&query=Durrell%2C+P+R">Patrick R. Durrell</a>, <a href="/search/astro-ph?searchtype=author&query=Paudel%2C+S">Sanjaya Paudel</a>, <a href="/search/astro-ph?searchtype=author&query=Poulain%2C+M">M茅lina Poulain</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">Rub茅n S谩nchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Sreejith%2C+S">Sreevarsha Sreejith</a>, <a href="/search/astro-ph?searchtype=author&query=Ramasawmy%2C+J">Joanna Ramasawmy</a>, <a href="/search/astro-ph?searchtype=author&query=Stemock%2C+B">Bryson Stemock</a>, <a href="/search/astro-ph?searchtype=author&query=Leach%2C+C">Christopher Leach</a>, <a href="/search/astro-ph?searchtype=author&query=Cuillandre%2C+J">Jean-Charles Cuillandre</a>, <a href="/search/astro-ph?searchtype=author&query=Gwyn%2C+S">Stephen Gwyn</a>, <a href="/search/astro-ph?searchtype=author&query=Agnello%2C+A">Adriano Agnello</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%ADlek%2C+M">Michal B铆lek</a>, <a href="/search/astro-ph?searchtype=author&query=Fensch%2C+J">J茅r茅my Fensch</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%BCller%2C+O">Oliver M眉ller</a>, <a href="/search/astro-ph?searchtype=author&query=Peng%2C+E+W">Eric W. Peng</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Burg%2C+R+F+J">Remco F. J. van der Burg</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="1910.13462v2-abstract-short" style="display: inline;"> We present the photometric properties of 2210 newly identified dwarf galaxy candidates in the MATLAS fields. The Mass Assembly of early Type gaLAxies with their fine Structures (MATLAS) deep imaging survey mapped $\sim$142 deg$^2$ of the sky around nearby isolated early type galaxies using MegaCam on the Canada-France-Hawaii Telescope, reaching surface brightnesses of $\sim$ 28.5 - 29 in the g-ban… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.13462v2-abstract-full').style.display = 'inline'; document.getElementById('1910.13462v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1910.13462v2-abstract-full" style="display: none;"> We present the photometric properties of 2210 newly identified dwarf galaxy candidates in the MATLAS fields. The Mass Assembly of early Type gaLAxies with their fine Structures (MATLAS) deep imaging survey mapped $\sim$142 deg$^2$ of the sky around nearby isolated early type galaxies using MegaCam on the Canada-France-Hawaii Telescope, reaching surface brightnesses of $\sim$ 28.5 - 29 in the g-band. The dwarf candidates were identified through a direct visual inspection of the images and by visually cleaning a sample selected using a partially automated approach, and were morphologically classified at the time of identification. Approximately 75% of our candidates are dEs, indicating that a large number of early type dwarfs also populate low density environments, and 23.2% are nucleated. Distances were determined for 13.5% of our sample using pre-existing $z_{spec}$ measurements and HI detections. We confirm the dwarf nature for 99% of this sub-sample based on a magnitude cut $M_g$ = -18. Additionally, most of these ($\sim$90%) have relative velocities suggesting that they form a satellite population around nearby massive galaxies rather than an isolated field sample. Assuming that the candidates over the whole survey are satellites of the nearby galaxies, we demonstrate that the MATLAS dwarfs follow the same scaling relations as dwarfs in the Local Group as well as the Virgo and Fornax clusters. We also find that the nucleated fraction increases with $M_g$, and find evidence of a morphology-density relation for dwarfs around isolated massive galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.13462v2-abstract-full').style.display = 'none'; document.getElementById('1910.13462v2-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 December, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 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">21 pages, 16 figures, 1 table. Accepted for publication in MNRAS; minor corrections to the text, and updated Figures 8 and 9 to match published version</span> </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> </ul> </nav> <div class="is-hidden-tablet">  <span 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