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<button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.18015">arXiv:2412.18015</a> <span> [<a href="https://arxiv.org/pdf/2412.18015">pdf</a>, <a href="https://arxiv.org/format/2412.18015">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/10.1051/0004-6361/202452206">10.1051/0004-6361/202452206 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> VEGAS-SSS: An intra-group component in the globular cluster system of NGC 5018 group of galaxies using VST data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lonare%2C+P">Pratik Lonare</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Mirabile%2C+M">Marco Mirabile</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">Marilena Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">Marina Rejkuba</a>, <a href="/search/astro-ph?searchtype=author&query=Hilker%2C+M">Michael Hilker</a>, <a href="/search/astro-ph?searchtype=author&query=Habas%2C+R">Rebecca Habas</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">Enrichetta Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Hazra%2C+N">Nandini Hazra</a>, <a href="/search/astro-ph?searchtype=author&query=Riccio%2C+G">Gabriele Riccio</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="2412.18015v1-abstract-short" style="display: inline;"> Globular clusters (GCs) are fossil tracer of formation and evolution of galaxies and studying their properties provides crucial insights into past formation and interaction events. We study the properties of GC candidates in 1.25 $\times$ 1.03 sq. degrees area centred on NGC 5018 group of galaxies using deep, wide field and multi-band observations obtained with VST. We derived photometric catalogu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.18015v1-abstract-full').style.display = 'inline'; document.getElementById('2412.18015v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.18015v1-abstract-full" style="display: none;"> Globular clusters (GCs) are fossil tracer of formation and evolution of galaxies and studying their properties provides crucial insights into past formation and interaction events. We study the properties of GC candidates in 1.25 $\times$ 1.03 sq. degrees area centred on NGC 5018 group of galaxies using deep, wide field and multi-band observations obtained with VST. We derived photometric catalogues of compact and extended sources and identified GC candidates using a set of photometric and morphometric selection parameters. A GC candidates catalogue is inspected using a statistical background decontamination technique. The 2D distribution map of GC candidates reveals an overdensity of sources on brightest member of group, NGC 5018. No significant GC overdensities are observed in other bright galaxies of group. We report discovery of a candidate local nucleated LSB dwarf galaxy possibly in tidal interaction with NGC 5018. The 2D map also reveals an intra-group GC population aligning with bright galaxies and along intra-group light component. Radial density profile of GC candidates in NGC 5018 follows galaxy surface brightness profile. Colour profile of GC candidates centred on this galaxy shows no evidence of well-known colour bimodality, which is instead observed in intra-group population. From GC luminosity function (GCLF) analysis, we find a low specific frequency $S_{\!\rm N}=0.59 \pm 0.27$ for NGC 5018, consistent with previous results. This relatively low $S_{\!\rm N}$ and lack of colour bimodality might be due to a combination of observational data limitations and the post-merger status of NGC 5018, which might host a population of relatively young GCs. For intra-group GC population, we obtain a lower limit of $S_{\!\rm {N,gr}}\sim0.6$. Using GCLF as a distance indicator, we estimate that NGC 5018 is located $38.0 \pm 7.9$ Mpc away, consistent with values in the literature.. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.18015v1-abstract-full').style.display = 'none'; document.getElementById('2412.18015v1-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 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 694, A231 (2025) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.17672">arXiv:2412.17672</a> <span> [<a href="https://arxiv.org/pdf/2412.17672">pdf</a>, <a href="https://arxiv.org/format/2412.17672">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Euclid: Early Release Observations of diffuse stellar structures and globular clusters as probes of the mass assembly of galaxies in the Dorado group </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Urbano%2C+M">M. Urbano</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P+-">P. -A. Duc</a>, <a href="/search/astro-ph?searchtype=author&query=Saifollahi%2C+T">T. Saifollahi</a>, <a href="/search/astro-ph?searchtype=author&query=Sola%2C+E">E. Sola</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=Voggel%2C+K">K. Voggel</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=Bouy%2C+H">H. Bouy</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Carollo%2C+D">D. Carollo</a>, <a href="/search/astro-ph?searchtype=author&query=Cuillandre%2C+J+-">J. -C. Cuillandre</a>, <a href="/search/astro-ph?searchtype=author&query=Dimauro%2C+P">P. Dimauro</a>, <a href="/search/astro-ph?searchtype=author&query=Erwin%2C+P">P. Erwin</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=Habas%2C+R">R. Habas</a>, <a href="/search/astro-ph?searchtype=author&query=Hilker%2C+M">M. Hilker</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=Kluge%2C+M">M. Kluge</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=Liu%2C+Q">Q. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Marchal%2C+O">O. Marchal</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=Massari%2C+D">D. Massari</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%BCller%2C+O">O. M眉ller</a> , et al. (138 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2412.17672v1-abstract-short" style="display: inline;"> Deep surveys reveal tidal debris and associated compact stellar systems. Euclid's unique combination of capabilities (spatial resolution, depth, and wide sky coverage) will make it a groundbreaking tool for galactic archaeology in the local Universe, bringing low surface brightness (LSB) science into the era of large-scale astronomical surveys. Euclid's Early Release Observations (ERO) demonstrate… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.17672v1-abstract-full').style.display = 'inline'; document.getElementById('2412.17672v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.17672v1-abstract-full" style="display: none;"> Deep surveys reveal tidal debris and associated compact stellar systems. Euclid's unique combination of capabilities (spatial resolution, depth, and wide sky coverage) will make it a groundbreaking tool for galactic archaeology in the local Universe, bringing low surface brightness (LSB) science into the era of large-scale astronomical surveys. Euclid's Early Release Observations (ERO) demonstrate this potential with a field of view that includes several galaxies in the Dorado group. In this paper, we aim to derive from this image a mass assembly scenario for its main galaxies: NGC 1549, NGC 1553, and NGC 1546. We detect internal and external diffuse structures, and identify candidate globular clusters (GCs). By analysing the colours and distributions of the diffuse structures and candidate GCs, we can place constraints on the galaxies' mass assembly and merger histories. The results show that feature morphology, surface brightness, colours, and GC density profiles are consistent with galaxies that have undergone different merger scenarios. We classify NGC 1549 as a pure elliptical galaxy that has undergone a major merger. NGC 1553 appears to have recently transitioned from a late-type galaxy to early type, after a series of radial minor to intermediate mergers. NGC 1546 is a rare specimen of galaxy with an undisturbed disk and a prominent diffuse stellar halo, which we infer has been fed by minor mergers and then disturbed by the tidal effect from NGC 1553. Finally, we identify limitations specific to the observing conditions of this ERO, in particular stray light in the visible and persistence in the near-infrared bands. Once these issues are addressed and the extended emission from LSB objects is preserved by the data-processing pipeline, the Euclid Wide Survey will allow studies of the local Universe to be extended to statistical ensembles over a large part of the extragalactic sky. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.17672v1-abstract-full').style.display = 'none'; document.getElementById('2412.17672v1-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 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages, 20 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/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/2407.21620">arXiv:2407.21620</a> <span> [<a href="https://arxiv.org/pdf/2407.21620">pdf</a>, <a href="https://arxiv.org/format/2407.21620">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/10.1051/0004-6361/202451273">10.1051/0004-6361/202451273 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> VEGAS-SSS: Tracing Globular Cluster Populations in the Interacting NGC3640 Galaxy Group </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mirabile%2C+M">Marco Mirabile</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Lonare%2C+P">Pratik Lonare</a>, <a href="/search/astro-ph?searchtype=author&query=Ragusa%2C+R">Rossella Ragusa</a>, <a href="/search/astro-ph?searchtype=author&query=Paolillo%2C+M">Maurizio Paolillo</a>, <a href="/search/astro-ph?searchtype=author&query=Hazra%2C+N">Nandini Hazra</a>, <a href="/search/astro-ph?searchtype=author&query=La+Marca%2C+A">Antonio La Marca</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">Enrichetta Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">Marilena Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Mieske%2C+S">Steffen Mieske</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">Marina Rejkuba</a>, <a href="/search/astro-ph?searchtype=author&query=Hilker%2C+M">Michael Hilker</a>, <a href="/search/astro-ph?searchtype=author&query=Riccio%2C+G">Gabriele Riccio</a>, <a href="/search/astro-ph?searchtype=author&query=Habas%2C+R+A">Rebecca A. Habas</a>, <a href="/search/astro-ph?searchtype=author&query=Brocato%2C+E">Enzo Brocato</a>, <a href="/search/astro-ph?searchtype=author&query=Schipani%2C+P">Pietro Schipani</a>, <a href="/search/astro-ph?searchtype=author&query=Grado%2C+A">Aniello Grado</a>, <a href="/search/astro-ph?searchtype=author&query=Limatola%2C+L">Luca Limatola</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="2407.21620v1-abstract-short" style="display: inline;"> Globular clusters (GCs) are among the oldest stellar systems in the universe. As such, GCs population are valuable fossil tracers of galaxy formation and interaction history. We use the multi-band wide-field images obtained with the VST to study the properties of the GC population in an interacting pair of galaxies. We derived ugri photometry over $1.5x1.5deg^2$ centred on the galaxy group compose… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.21620v1-abstract-full').style.display = 'inline'; document.getElementById('2407.21620v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.21620v1-abstract-full" style="display: none;"> Globular clusters (GCs) are among the oldest stellar systems in the universe. As such, GCs population are valuable fossil tracers of galaxy formation and interaction history. We use the multi-band wide-field images obtained with the VST to study the properties of the GC population in an interacting pair of galaxies. We derived ugri photometry over $1.5x1.5deg^2$ centred on the galaxy group composed by two elliptical galaxies: NGC3640 and its fainter companion NGC3641. We studied the GC system properties from both the ugri and gri matched catalogs GC candidates were identified based on a combination of photometric properties (colors, magnitudes) and morphometric criteria (concentration index, elongation, FWHM), using sources with well-defined classifications from spectroscopic or imaging data available in the literature and numerical simulations as references. The selection criteria were also applied to empty fields to determine a statistical background correction for the number of identified GC candidates. The 2D density maps of GCs appear to align with the diffuse light patches resulting from merging events of the galaxies. The highest density peak of GCs is observed to be on NGC3641 rather than NGC3640, despite the latter being the more massive galaxy. The azimuthal averaged radial density profiles in both galaxies reveal that the GC population extends beyond the galaxy light profile and indicate the likely presence of an intra-group GC component. A color bimodality in (u-r) and (g-i) is observed for NGC3641, whereas NGC3640 shows a broad unimodal distribution. Analysis of the GC Luminosity Function indicates that both galaxies are roughly located at the same distance (~27Mpc). We provide an estimate of the total number of GCs, and determine the specific frequency for NGC3640, $S_N =2.0\pm0.6$, which aligns with expectations, while for NGC3641 we find a large $S_N=4.5\pm1.6$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.21620v1-abstract-full').style.display = 'none'; document.getElementById('2407.21620v1-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 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">37 pages, 23 figures, 13 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 691, A104 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.13502">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/2405.13496">arXiv:2405.13496</a> <span> [<a href="https://arxiv.org/pdf/2405.13496">pdf</a>, <a href="https://arxiv.org/format/2405.13496">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="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Euclid: Early Release Observations -- Programme overview and pipeline for compact- and diffuse-emission photometry </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=Bertin%2C+E">E. Bertin</a>, <a href="/search/astro-ph?searchtype=author&query=Bolzonella%2C+M">M. Bolzonella</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=Isani%2C+S">S. Isani</a>, <a href="/search/astro-ph?searchtype=author&query=Kluge%2C+M">M. Kluge</a>, <a href="/search/astro-ph?searchtype=author&query=Lai%2C+O">O. Lai</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=Lang%2C+D+A">D. A. Lang</a>, <a href="/search/astro-ph?searchtype=author&query=Laureijs%2C+R">R. Laureijs</a>, <a href="/search/astro-ph?searchtype=author&query=Saifollahi%2C+T">T. Saifollahi</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=Abdurro%27uf"> Abdurro'uf</a>, <a href="/search/astro-ph?searchtype=author&query=Aghanim%2C+N">N. Aghanim</a>, <a href="/search/astro-ph?searchtype=author&query=Altieri%2C+B">B. Altieri</a>, <a href="/search/astro-ph?searchtype=author&query=Annibali%2C+F">F. Annibali</a>, <a href="/search/astro-ph?searchtype=author&query=Atek%2C+H">H. Atek</a>, <a href="/search/astro-ph?searchtype=author&query=Awad%2C+P">P. Awad</a>, <a href="/search/astro-ph?searchtype=author&query=Baes%2C+M">M. Baes</a>, <a href="/search/astro-ph?searchtype=author&query=Ba%C3%B1ados%2C+E">E. Ba帽ados</a>, <a href="/search/astro-ph?searchtype=author&query=Barrado%2C+D">D. Barrado</a>, <a href="/search/astro-ph?searchtype=author&query=Belladitta%2C+S">S. Belladitta</a>, <a href="/search/astro-ph?searchtype=author&query=Belokurov%2C+V">V. Belokurov</a> , et al. (240 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="2405.13496v1-abstract-short" style="display: inline;"> The Euclid ERO showcase Euclid's capabilities in advance of its main mission, targeting 17 astronomical objects, from galaxy clusters, nearby galaxies, globular clusters, to star-forming regions. A total of 24 hours observing time was allocated in the early months of operation, engaging the scientific community through an early public data release. We describe the development of the ERO pipeline t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.13496v1-abstract-full').style.display = 'inline'; document.getElementById('2405.13496v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.13496v1-abstract-full" style="display: none;"> The Euclid ERO showcase Euclid's capabilities in advance of its main mission, targeting 17 astronomical objects, from galaxy clusters, nearby galaxies, globular clusters, to star-forming regions. A total of 24 hours observing time was allocated in the early months of operation, engaging the scientific community through an early public data release. We describe the development of the ERO pipeline to create visually compelling images while simultaneously meeting the scientific demands within months of launch, leveraging a pragmatic, data-driven development strategy. The pipeline's key requirements are to preserve the image quality and to provide flux calibration and photometry for compact and extended sources. The pipeline's five pillars are: removal of instrumental signatures; astrometric calibration; photometric calibration; image stacking; and the production of science-ready catalogues for both the VIS and NISP instruments. We report a PSF with a full width at half maximum of 0.16" in the optical and 0.49" in the three NIR bands. Our VIS mean absolute flux calibration is accurate to about 1%, and 10% for NISP due to a limited calibration set; both instruments have considerable colour terms. The median depth is 25.3 and 23.2 AB mag with a SNR of 10 for galaxies, and 27.1 and 24.5 AB mag at an SNR of 5 for point sources for VIS and NISP, respectively. Euclid's ability to observe diffuse emission is exceptional due to its extended PSF nearly matching a pure diffraction halo, the best ever achieved by a wide-field, high-resolution imaging telescope. Euclid offers unparalleled capabilities for exploring the LSB Universe across all scales, also opening a new observational window in the NIR. Median surface-brightness levels of 29.9 and 28.3 AB mag per square arcsec are achieved for VIS and NISP, respectively, for detecting a 10 arcsec x 10 arcsec extended feature at the 1 sigma level. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.13496v1-abstract-full').style.display = 'none'; document.getElementById('2405.13496v1-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, 36 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/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/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/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/2107.09379">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/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/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/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> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1812.07346">arXiv:1812.07346</a> <span> [<a href="https://arxiv.org/pdf/1812.07346">pdf</a>, <a href="https://arxiv.org/format/1812.07346">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/10.1051/0004-6361/201834911">10.1051/0004-6361/201834911 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The ultra-diffuse galaxy NGC 1052-DF2 with MUSE: II. The population of DF2: stars, clusters and planetary nebulae </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Fensch%2C+J">Jeremy Fensch</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=Jerabkova%2C+T">Tereza Jerabkova</a>, <a href="/search/astro-ph?searchtype=author&query=Emsellem%2C+E">Eric Emsellem</a>, <a href="/search/astro-ph?searchtype=author&query=Zanella%2C+A">Anita Zanella</a>, <a href="/search/astro-ph?searchtype=author&query=Agnello%2C+A">Adriano Agnello</a>, <a href="/search/astro-ph?searchtype=author&query=Hilker%2C+M">Michael Hilker</a>, <a href="/search/astro-ph?searchtype=author&query=Mueller%2C+O">Oliver Mueller</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">Marina Rejkuba</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=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=Marleau%2C+F+R">Francine R. Marleau</a>, <a href="/search/astro-ph?searchtype=author&query=Peng%2C+E">Eric Peng</a>, <a href="/search/astro-ph?searchtype=author&query=Janssen%2C+R+S">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="1812.07346v2-abstract-short" style="display: inline;"> NGC 1052-DF2, an ultra diffuse galaxy (UDG), has been the subject of intense debate. Its alleged absence of dark matter, and the brightness and number excess of its globular clusters (GCs) at an initially assumed distance of 20Mpc, suggested a new formation channel for UDGs. We present the first systematic spectroscopic analysis of both the stellar body and the GCs (six of which were previously kn… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.07346v2-abstract-full').style.display = 'inline'; document.getElementById('1812.07346v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1812.07346v2-abstract-full" style="display: none;"> NGC 1052-DF2, an ultra diffuse galaxy (UDG), has been the subject of intense debate. Its alleged absence of dark matter, and the brightness and number excess of its globular clusters (GCs) at an initially assumed distance of 20Mpc, suggested a new formation channel for UDGs. We present the first systematic spectroscopic analysis of both the stellar body and the GCs (six of which were previously known, and one newly confirmed member) of this galaxy using MUSE@VLT. Even though NGC 1052-DF2 does not show any spatially extended emission lines we report the discovery of three planetary nebulae (PNe). We conduct full spectral fitting on the UDG and the stacked spectra of all GCs. The UDG's stellar population is old, 8.9$\pm$1.5 Gyr, metal-poor, with [M/H] = $-$1.07$\pm$0.12 with little or no $伪$-enrichment. The stacked spectrum of all GCs indicates a similar age of 8.9$\pm$1.8 Gyr, but lower metallicity, with [M/H] = $-$1.63$\pm$0.09, and similarly low $伪$-enrichment. There is no evidence for a variation of age and metallicity in the GC population with the available spectra. The significantly more metal-rich stellar body with respect to its associated GCs, the age of the population, its metallicity and alpha enrichment, are all in line with other dwarf galaxies. NGC 1052-DF2 thus falls on the same empirical mass-metallicity relation as other dwarfs, for the full distance range assumed in the literature. We find that both debated distance estimates (13 and 20 Mpc) are similarly likely, given the three discovered PNe. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.07346v2-abstract-full').style.display = 'none'; document.getElementById('1812.07346v2-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 January, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 December, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 7 figures, accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 625, A77 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1812.07345">arXiv:1812.07345</a> <span> [<a href="https://arxiv.org/pdf/1812.07345">pdf</a>, <a href="https://arxiv.org/format/1812.07345">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/10.1051/0004-6361/201834909">10.1051/0004-6361/201834909 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The ultra-diffuse galaxy NGC 1052-DF2 with MUSE: I. Kinematics of the stellar body </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Emsellem%2C+E">Eric Emsellem</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">Jeremy Fensch</a>, <a href="/search/astro-ph?searchtype=author&query=Jerabkova%2C+T">Tereza Jerabkova</a>, <a href="/search/astro-ph?searchtype=author&query=Zanella%2C+A">Anita Zanella</a>, <a href="/search/astro-ph?searchtype=author&query=Agnello%2C+A">Adriano Agnello</a>, <a href="/search/astro-ph?searchtype=author&query=Hilker%2C+M">Michael Hilker</a>, <a href="/search/astro-ph?searchtype=author&query=Mueller%2C+O">Oliver Mueller</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">Marina Rejkuba</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=Habas%2C+R">Rebecca Habas</a>, <a href="/search/astro-ph?searchtype=author&query=Lelli%2C+F">Federico Lelli</a>, <a href="/search/astro-ph?searchtype=author&query=Lim%2C+S">Sungsoon Lim</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=Peng%2C+E">Eric Peng</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="1812.07345v3-abstract-short" style="display: inline;"> The so-called ultra-diffuse galaxy NGC~1052-DF2 was announced to be a galaxy lacking dark matter based on a spectroscopic study of its constituent globular clusters. Here we present the first spectroscopic analysis of the stellar body of this galaxy using the MUSE integral-field spectrograph at the (ESO) Very Large Telescope. The MUSE datacube simultaneously provides DF2's stellar velocity field a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.07345v3-abstract-full').style.display = 'inline'; document.getElementById('1812.07345v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1812.07345v3-abstract-full" style="display: none;"> The so-called ultra-diffuse galaxy NGC~1052-DF2 was announced to be a galaxy lacking dark matter based on a spectroscopic study of its constituent globular clusters. Here we present the first spectroscopic analysis of the stellar body of this galaxy using the MUSE integral-field spectrograph at the (ESO) Very Large Telescope. The MUSE datacube simultaneously provides DF2's stellar velocity field and systemic velocities for seven globular clusters (GCs). We further discovered three planetary nebulae (PNe) that are likely part of this galaxy. While five of the clusters had velocities measured in the literature, we were able to confirm the membership of two more candidates through precise radial velocity measurements, which increases the measured specific frequency of GCs in DF2. The mean velocity of the diffuse stellar body, 1792.9$^{-1.8}_{+1.4}$~\kms, is consistent with the mean globular cluster velocity. We detect a weak but significant velocity gradient within the stellar body, with a kinematic axis close to the photometric major-axis, making it a prolate-like rotator. We estimate a velocity dispersion from the clusters and PNe of $蟽_{\mathrm{int}}=10.6^{+3.9}_{-2.3}$~\kms. The velocity dispersion $蟽_{\rm{DF2}\star}$(\re) for the stellar body within one effective radius is $10.8^{-4.0}_{+3.2}$~\kms. Considering various sources of systemic uncertainties this central value varies between 5 and 13~\kms, and we conservatively report a 95\% confidence upper limit to the dispersion within one \re\ of 21~\kms. We provide updated mass estimates based on these dispersions corresponding to the different distances to NGC~1052-DF2 that have been reported in the recent literature. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.07345v3-abstract-full').style.display = 'none'; document.getElementById('1812.07345v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 December, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 5 figures, Accepted for publication in A&A. Publisher ready version: minor language editing</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1712.09857">arXiv:1712.09857</a> <span> [<a href="https://arxiv.org/pdf/1712.09857">pdf</a>, <a href="https://arxiv.org/format/1712.09857">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/sty005">10.1093/mnras/sty005 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galaxy Evolution in the Cluster Abell 85: New Insights from the Dwarf Population </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=Fadda%2C+D">Dario Fadda</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=Biviano%2C+A">Andrea Biviano</a>, <a href="/search/astro-ph?searchtype=author&query=Durret%2C+F">Florence Durret</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1712.09857v1-abstract-short" style="display: inline;"> We present the first results of a new spectroscopic survey of the cluster Abell 85 targeting 1466 candidate cluster members within the central $\sim$1 deg$^2$ of the cluster and having magnitudes $m_r < 20.5$ using VIMOS/VLT and HYDRA/WIYN. A total of 520 galaxies are confirmed as either relaxed cluster members or part of an infalling population. A significant fraction are low mass; the median ste… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1712.09857v1-abstract-full').style.display = 'inline'; document.getElementById('1712.09857v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1712.09857v1-abstract-full" style="display: none;"> We present the first results of a new spectroscopic survey of the cluster Abell 85 targeting 1466 candidate cluster members within the central $\sim$1 deg$^2$ of the cluster and having magnitudes $m_r < 20.5$ using VIMOS/VLT and HYDRA/WIYN. A total of 520 galaxies are confirmed as either relaxed cluster members or part of an infalling population. A significant fraction are low mass; the median stellar mass of the sample is $10^{9.6} M_{\odot} $, and 25% have stellar masses below $10^9 M_{\odot}$ (i.e. 133 dwarf galaxies). We also identify seven active galactic nuclei (AGN), four of which reside in dwarf host galaxies. We probe the evolution of star formation rates, based on H$伪$ emission and continuum modeling, as a function of both mass and environment. We find that more star forming galaxies are observed at larger clustercentric distances, while infalling galaxies show evidence for recently enhanced star forming activity. Main sequence galaxies, defined by their continuum star formation rates, show different evolutionary behavior based on their mass. At the low mass end, the galaxies have had their star formation recently quenched, while more massive galaxies show no significant change. The timescales probed here favor fast quenching mechanisms, such as ram-pressure stripping. Galaxies within the green valley, defined similarly, do not show evidence of quenching. Instead, the low mass galaxies maintain their levels of star forming activity, while the more massive galaxies have experienced a recent burst. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1712.09857v1-abstract-full').style.display = 'none'; document.getElementById('1712.09857v1-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 December, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 10 figures, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1411.3844">arXiv:1411.3844</a> <span> [<a href="https://arxiv.org/pdf/1411.3844">pdf</a>, <a href="https://arxiv.org/format/1411.3844">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/10.1051/0004-6361/201629832">10.1051/0004-6361/201629832 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Infrared signature of active massive black holes in nearby dwarf 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=Clancy%2C+D">Dominic Clancy</a>, <a href="/search/astro-ph?searchtype=author&query=Habas%2C+R">Rebecca Habas</a>, <a href="/search/astro-ph?searchtype=author&query=Bianconi%2C+M">Matteo Bianconi</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="1411.3844v3-abstract-short" style="display: inline;"> We investigate the possible presence of active galactic nuclei (AGN) in dwarf galaxies and other nearby galaxies to identify candidates for follow-up confirmation and dynamical mass measurements. We use the Wide-field Infrared Survey Explorer (WISE) All-Sky Release Source Catalog and examine the infrared colours of a sample of dwarf galaxies and other nearby galaxies in order to identify both unob… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1411.3844v3-abstract-full').style.display = 'inline'; document.getElementById('1411.3844v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1411.3844v3-abstract-full" style="display: none;"> We investigate the possible presence of active galactic nuclei (AGN) in dwarf galaxies and other nearby galaxies to identify candidates for follow-up confirmation and dynamical mass measurements. We use the Wide-field Infrared Survey Explorer (WISE) All-Sky Release Source Catalog and examine the infrared colours of a sample of dwarf galaxies and other nearby galaxies in order to identify both unobscured and obscured candidate AGN by applying the infrared colour diagnostic. Stellar masses of galaxies are obtained using a combination of three independent methods. Black hole masses are estimated using the bolometric luminosity of the AGN candidates and computed for three cases of the bolometric-to-Eddington luminosity ratio. We identify 303 candidate AGN, of which 276 were subsequently found to have been independently identified as AGN via other methods. The remaining 9% require follow-up observations for confirmation. The activity is detected in galaxies with stellar masses from ~ 10^6 to 10^9 solar masses; assuming the candidates are AGN, the black hole masses are estimated to be ~ 10^3 - 10^6 solar masses, adopting L_bol = 0.1 L_Edd. The black hole masses probed are several orders of magnitude smaller than previously reported for centrally located massive black holes. We examine the stellar mass versus black hole mass relationship in this low galaxy mass regime. We find that it is consistent with the existing relation extending linearly (in log-log space) into the lower mass regime. These findings suggest that CMBH are present in low-mass galaxies and in the Local Universe, and provide new impetus for follow-up dynamical studies of quiescent black holes in local dwarf galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1411.3844v3-abstract-full').style.display = 'none'; document.getElementById('1411.3844v3-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 July, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 November, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 9 figures, 4 tables, accepted for publication in Astronomy & Astrophysics. The first version of this paper appeared on astro-ph in 2014 (arXiv:1411.3844). The new version includes 3 new tables, 1 new figure and updated discussion</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astronomy & Astrophysics, 602, 28 (2017) </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path 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