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</div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Blakeslee%2C+J+P&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Blakeslee%2C+J+P&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Blakeslee%2C+J+P&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Blakeslee%2C+J+P&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=Blakeslee%2C+J+P&start=150" class="pagination-link " aria-label="Page 4" 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href="/search/astro-ph?searchtype=author&query=Lim%2C+S">Sungsoon Lim</a>, <a href="/search/astro-ph?searchtype=author&query=Peng%2C+E+W">Eric W. Peng</a>, <a href="/search/astro-ph?searchtype=author&query=C%C3%B4t%C3%A9%2C+P">Patrick C么t茅</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrarese%2C+L">Laura Ferrarese</a>, <a href="/search/astro-ph?searchtype=author&query=Roediger%2C+J+C">Joel C. Roediger</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+C">Chengze Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Spengler%2C+C">Chelsea Spengler</a>, <a href="/search/astro-ph?searchtype=author&query=Sola%2C+E">Elisabeth Sola</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P">Pierre-Alain Duc</a>, <a href="/search/astro-ph?searchtype=author&query=Sales%2C+L+V">Laura V. Sales</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Cuillandre%2C+J">Jean-Charles Cuillandre</a>, <a href="/search/astro-ph?searchtype=author&query=Durrell%2C+P+R">Patrick R. Durrell</a>, <a href="/search/astro-ph?searchtype=author&query=Emsellem%2C+E">Eric Emsellem</a>, <a href="/search/astro-ph?searchtype=author&query=Gwyn%2C+S+D+J">Stephen D. J. Gwyn</a>, <a href="/search/astro-ph?searchtype=author&query=Lan%C3%A7on%2C+A">Ariane Lan莽on</a>, <a href="/search/astro-ph?searchtype=author&query=Marleau%2C+F+R">Francine R. Marleau</a>, <a href="/search/astro-ph?searchtype=author&query=Mihos%2C+J+C">J. Christopher Mihos</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%BCller%2C+O">Oliver M眉ller</a>, <a href="/search/astro-ph?searchtype=author&query=Puzia%2C+T+H">Thomas H. Puzia</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">Rub茅n S谩nchez-Janssen</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.17049v1-abstract-short" style="display: inline;"> We present an analysis of the spatial distribution of globular cluster (GC) systems of 118 nearby early-type galaxies in the Next Generation Virgo Cluster Survey (NGVS) and Mass Assembly of early-Type GaLAxies with their fine Structures (MATLAS) survey programs, which both used MegaCam on the Canada-France-Hawaii Telescope. We describe the procedure used to select GC candidates and fit the spatial… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.17049v1-abstract-full').style.display = 'inline'; document.getElementById('2411.17049v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.17049v1-abstract-full" style="display: none;"> We present an analysis of the spatial distribution of globular cluster (GC) systems of 118 nearby early-type galaxies in the Next Generation Virgo Cluster Survey (NGVS) and Mass Assembly of early-Type GaLAxies with their fine Structures (MATLAS) survey programs, which both used MegaCam on the Canada-France-Hawaii Telescope. We describe the procedure used to select GC candidates and fit the spatial distributions of GCs to a two-dimensional S茅rsic function, which provides effective radii (half number radii) and S茅rsic indices, and estimate background contamination by adding a constant term to the S'ersic function. In cases where a neighboring galaxy affects the estimation of the GC spatial distribution in the target galaxy, we fit two 2D S茅rsic functions, simultaneously. We also investigate the color distributions of GCs in our sample by using Gaussian Mixture Modeling. For GC systems with bimodal color distributions, we divide the GCs into blue and red subgroups and fit their respective spatial distributions with S茅rsic functions. Finally, we measure the total number of GCs based on our fitted S茅rsic function, and calculate the GC specific frequency. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.17049v1-abstract-full').style.display = 'none'; document.getElementById('2411.17049v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">31 pages, 10 Figures (115 additional figures are available in the ApJS online Journal), 2 Tables, accepted for publication in ApJS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.16810">arXiv:2408.16810</a> <span> [<a href="https://arxiv.org/pdf/2408.16810">pdf</a>, <a href="https://arxiv.org/format/2408.16810">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> The TRGB-SBF Project. II. Resolving the Virgo Cluster with JWST </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Anand%2C+G+S">Gagandeep S. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Tully%2C+R+B">R. Brent Tully</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+Y">Yotam Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Shaya%2C+E+J">Edward J. Shaya</a>, <a href="/search/astro-ph?searchtype=author&query=Makarov%2C+D+I">Dmitry I. Makarov</a>, <a href="/search/astro-ph?searchtype=author&query=Makarova%2C+L+N">Lidia N. Makarova</a>, <a href="/search/astro-ph?searchtype=author&query=Chazov%2C+M+I">Maksim I. Chazov</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Jensen%2C+J+B">Joseph B. Jensen</a>, <a href="/search/astro-ph?searchtype=author&query=Kourkchi%2C+E">Ehsan Kourkchi</a>, <a href="/search/astro-ph?searchtype=author&query=Raimondo%2C+G">Gabriella Raimondo</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="2408.16810v1-abstract-short" style="display: inline;"> The Virgo Cluster is the nearest substantial cluster of galaxies to the Milky Way and a cornerstone of the extragalactic distance scale. Here, we present JWST/NIRCam observations that simultaneously cover the cores and halos of ten galaxies in and around the Virgo Cluster and are designed to perform simultaneous measurements of the tip of the red giant branch (TRGB) and surface brightness fluctuat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.16810v1-abstract-full').style.display = 'inline'; document.getElementById('2408.16810v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.16810v1-abstract-full" style="display: none;"> The Virgo Cluster is the nearest substantial cluster of galaxies to the Milky Way and a cornerstone of the extragalactic distance scale. Here, we present JWST/NIRCam observations that simultaneously cover the cores and halos of ten galaxies in and around the Virgo Cluster and are designed to perform simultaneous measurements of the tip of the red giant branch (TRGB) and surface brightness fluctuations (SBF). Seven of the targets are within the Virgo Cluster and where we are able to resolve some of the cluster's substructure, while an additional three provide important constraints on Virgo infall. The seven galaxies within Virgo itself all have SBF measurements from the Advanced Camera for Surveys Virgo Cluster Survey (ACSVCS). After adjusting the ACSVCS measurements for the offset from our new JWST TRGB measurements, we determine a distance to the Virgo Cluster of d $=$ 16.17 $\pm$ 0.25 (stat) $\pm$ 0.47 (sys) Mpc. The work presented here is part of a larger program to develop a Population II distance scale through the TRGB and SBF that is completely independent of the prominent Cepheid + Type Ia supernova ladder. The TRGB distances to the galaxies presented here, when combined with future SBF measurements, will provide a crucial step forward for determining whether or not systematic errors can explain the well-known "Hubble tension'' or if there is significant evidence for cracks in the $螞$CDM model. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.16810v1-abstract-full').style.display = 'none'; document.getElementById('2408.16810v1-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 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">submitted to ApJ. comments welcome and appreciated. program name has changed from Paper I's "The Population II Extragalactic Distance Scale" to "The TRGB-SBF Project"</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.03743">arXiv:2405.03743</a> <span> [<a href="https://arxiv.org/pdf/2405.03743">pdf</a>, <a href="https://arxiv.org/format/2405.03743">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The TRGB-SBF Project. I. A Tip of the Red Giant Branch Distance to the Fornax Cluster with JWST </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Anand%2C+G+S">Gagandeep S. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Tully%2C+R+B">R. Brent Tully</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+Y">Yotam Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Makarov%2C+D+I">Dmitry I. Makarov</a>, <a href="/search/astro-ph?searchtype=author&query=Makarova%2C+L+N">Lidia N. Makarova</a>, <a href="/search/astro-ph?searchtype=author&query=Jensen%2C+J+B">Joseph B. Jensen</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Kourkchi%2C+E">Ehsan Kourkchi</a>, <a href="/search/astro-ph?searchtype=author&query=Raimondo%2C+G">Gabriella Raimondo</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.03743v3-abstract-short" style="display: inline;"> Differences between the local value of the Hubble constant measured via the distance ladder versus the value inferred from the cosmic microwave background with the assumption of the standard $螞$CDM model have reached over 5$蟽$ significance. To determine if this discrepancy is due to new physics or more mundane systematic errors, it is essential to remove as many sources of systematic uncertainty a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.03743v3-abstract-full').style.display = 'inline'; document.getElementById('2405.03743v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.03743v3-abstract-full" style="display: none;"> Differences between the local value of the Hubble constant measured via the distance ladder versus the value inferred from the cosmic microwave background with the assumption of the standard $螞$CDM model have reached over 5$蟽$ significance. To determine if this discrepancy is due to new physics or more mundane systematic errors, it is essential to remove as many sources of systematic uncertainty as possible by developing high-precision distance ladders that are independent of the traditional Cepheid and Type Ia supernovae route. Here we present JWST observations of three early-type Fornax Cluster galaxies, the first of fourteen observations from a Cycle 2 JWST program. Our modest integration times allow us to measure highly precise tip of the red giant branch (TRGB) distances, and will also be used to perform measurements of Surface Brightness Fluctuations (SBF). From these three galaxies, we determine an average TRGB distance modulus to the Fornax Cluster of $渭$ = 31.424 $\pm$ 0.077 mag, or D = 19.3 $\pm$ 0.7 Mpc. With eleven more scheduled observations in nearby elliptical galaxies, our program will allow us set the zero point of the SBF scale to better than 2$\%$ for more distant measurements, charting a path towards a high-precision measurement of $H_{0}$ that is independent of the traditional Cepheid-SN Ia distance ladder. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.03743v3-abstract-full').style.display = 'none'; document.getElementById('2405.03743v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 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">14 pages, 9 figures, accepted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.16235">arXiv:2403.16235</a> <span> [<a href="https://arxiv.org/pdf/2403.16235">pdf</a>, <a href="https://arxiv.org/format/2403.16235">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The Next Generation Virgo Cluster Survey (NGVS). III. A Catalog of Surface Brightness Fluctuation Distances and the Three-Dimensional Distribution of Galaxies in the Virgo Cluster </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=C%C3%B4t%C3%A9%2C+P">Patrick C么t茅</a>, <a href="/search/astro-ph?searchtype=author&query=Raimondo%2C+G">Gabriella Raimondo</a>, <a href="/search/astro-ph?searchtype=author&query=Cuillandre%2C+J">Jean-Charles Cuillandre</a>, <a href="/search/astro-ph?searchtype=author&query=Durrell%2C+P+R">Patrick R. Durrell</a>, <a href="/search/astro-ph?searchtype=author&query=Gwyn%2C+S">Stephen Gwyn</a>, <a href="/search/astro-ph?searchtype=author&query=Hazra%2C+N">Nandini Hazra</a>, <a href="/search/astro-ph?searchtype=author&query=Peng%2C+E+W">Eric W. Peng</a>, <a href="/search/astro-ph?searchtype=author&query=Roediger%2C+J+C">Joel C. Roediger</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">R煤ben S谩nchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Kurzner%2C+M">Max Kurzner</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.16235v1-abstract-short" style="display: inline;"> The surface brightness fluctuation (SBF) method is a robust and efficient way of measuring distances to galaxies containing evolved stellar populations. Although many recent applications of the method have used space-based imaging, SBF remains a powerful technique for ground-based telescopes. Deep, wide-field imaging surveys with subarsecond seeing enable SBF measurements for numerous nearby galax… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.16235v1-abstract-full').style.display = 'inline'; document.getElementById('2403.16235v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.16235v1-abstract-full" style="display: none;"> The surface brightness fluctuation (SBF) method is a robust and efficient way of measuring distances to galaxies containing evolved stellar populations. Although many recent applications of the method have used space-based imaging, SBF remains a powerful technique for ground-based telescopes. Deep, wide-field imaging surveys with subarsecond seeing enable SBF measurements for numerous nearby galaxies. Using a preliminary calibration, Cantiello et al. (2018) presented SBF distances for 89 bright, mainly early-type galaxies observed in the Next Generation Virgo Cluster Survey (NGVS). Here, we present a refined calibration and SBF distances for 278 galaxies extending several magnitudes fainter than in previous work. The derived distances have uncertainties of 5-12\% depending on the properties of the individual galaxies, and our sample is more than three times larger than any previous SBF study of this region. Virgo has a famously complex structure with numerous subclusters, clouds and groups; we associate individual galaxies with the various substructures and map their three-dimensional spatial distribution. Curiously, subcluster A, centered around M87, appears to have two peaks in distance: the main peak at $\sim$16.5 Mpc and a smaller one at $\sim$19.4 Mpc. Subclusters B and C have distances of $\sim$15.8 Mpc. The W and W' groups form a filament-like structure, extending more than 15~Mpc behind the cluster with a commensurate velocity increase of $\sim$1000 \kms\ along its length. These measurements are a valuable resource for future studies of the relationship between galaxy properties and local environment within a dynamic and evolving region. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.16235v1-abstract-full').style.display = 'none'; document.getElementById('2403.16235v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">30 pages, 15 figures, Acccepted for publication on the ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.14847">arXiv:2403.14847</a> <span> [<a href="https://arxiv.org/pdf/2403.14847">pdf</a>, <a href="https://arxiv.org/format/2403.14847">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> NSCs from groups to clusters: A catalogue of dwarf galaxies in the Shapley Supercluster and the role of environment in galaxy nucleation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zanatta%2C+E+J+B">Emilio J. B. Zanatta</a>, <a href="/search/astro-ph?searchtype=author&query=Sanch%C3%A9z-Janssen%2C+R">Ruben Sanch茅z-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=de+Souza%2C+R+S">Rafael S. de Souza</a>, <a href="/search/astro-ph?searchtype=author&query=Chies-Santos%2C+A+L">Ana L. Chies-Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.14847v1-abstract-short" style="display: inline;"> Nuclear star clusters (NSCs) are dense star clusters located at the centre of galaxies spanning a wide range of masses and morphologies. Analysing NSC occupation statistics in different environments provides an invaluable window into investigating early conditions of high-density star formation and mass assembly in clusters and group galaxies. We use HST/ACS deep imaging to obtain a catalogue of d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.14847v1-abstract-full').style.display = 'inline'; document.getElementById('2403.14847v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.14847v1-abstract-full" style="display: none;"> Nuclear star clusters (NSCs) are dense star clusters located at the centre of galaxies spanning a wide range of masses and morphologies. Analysing NSC occupation statistics in different environments provides an invaluable window into investigating early conditions of high-density star formation and mass assembly in clusters and group galaxies. We use HST/ACS deep imaging to obtain a catalogue of dwarf galaxies in two galaxy clusters in the Shapley Supercluster: the central cluster Abell 3558 and the northern Abell 1736a. The Shapley region is an ideal laboratory to study nucleation as it stands as the highest mass concentration in the nearby Universe. We investigate the NSC occurrence in quiescent dwarf galaxies as faint as $M_{I} = -10$ mag and compare it with all other environments where nucleation data is available. We use galaxy cluster/group halo mass as a proxy for the environment and employ a Bayesian logistic regression framework to model the nucleation fraction ($f_{n}$) as a function of galaxy luminosity and environment. We find a notably high $f_n$ in Abell 3558: at $M_{I} \approx -13.1$ mag, half the galaxies in the cluster host NSCs. This is higher than in the Virgo and Fornax clusters but comparable to the Coma Cluster. On the other hand, the $f_n$ in Abell 1736a is relatively lower, comparable to groups in the Local Volume. We find that the probability of nucleation varies with galaxy luminosity remarkably similarly in galaxy clusters. These results reinforce previous findings of the important role of the environment in NSC formation/growth. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.14847v1-abstract-full').style.display = 'none'; document.getElementById('2403.14847v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 10 figures, accepted for publication in the MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.09926">arXiv:2403.09926</a> <span> [<a href="https://arxiv.org/pdf/2403.09926">pdf</a>, <a href="https://arxiv.org/format/2403.09926">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The Next Generation Virgo Cluster Survey (NGVS). XXVII.The Size and Structure of Globular Cluster Systems and their Connection to Dark Matter Halos </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lim%2C+S">Sungsoon Lim</a>, <a href="/search/astro-ph?searchtype=author&query=Peng%2C+E+W">Eric W. Peng</a>, <a href="/search/astro-ph?searchtype=author&query=C%C3%B4t%C3%A9%2C+P">Patrick C么t茅</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrarese%2C+L">Laura Ferrarese</a>, <a href="/search/astro-ph?searchtype=author&query=Roediger%2C+J+C">Joel C. Roediger</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+C">Chengze Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Spengler%2C+C">Chelsea Spengler</a>, <a href="/search/astro-ph?searchtype=author&query=Sola%2C+E">Elisabeth Sola</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P">Pierre-Alain Duc</a>, <a href="/search/astro-ph?searchtype=author&query=Sales%2C+L+V">Laura V. Sales</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Cuillandre%2C+J">Jean-Charles Cuillandre</a>, <a href="/search/astro-ph?searchtype=author&query=Durrell%2C+P+R">Patrick R. Durrell</a>, <a href="/search/astro-ph?searchtype=author&query=Emsellem%2C+E">Eric Emsellem</a>, <a href="/search/astro-ph?searchtype=author&query=Gwyn%2C+S+D+J">Stephen D. J. Gwyn</a>, <a href="/search/astro-ph?searchtype=author&query=Lan%C3%A7on%2C+A">Ariane Lan莽on</a>, <a href="/search/astro-ph?searchtype=author&query=Marleau%2C+F+R">Francine R. Marleau</a>, <a href="/search/astro-ph?searchtype=author&query=Mihos%2C+J+C">J. Christopher Mihos</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%BCller%2C+O">Oliver M眉ller</a>, <a href="/search/astro-ph?searchtype=author&query=Puzia%2C+T+H">Thomas H. Puzia</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">Rub茅n S谩nchez-Janssen</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.09926v1-abstract-short" style="display: inline;"> We study the size and structure of globular clusters (GC) systems of 118 early-type galaxies from the NGVS, MATLAS, and ACSVCS surveys. Fitting S茅rsic profiles, we investigate the relationship between effective radii of GC systems ($R_{e, \rm gc}$) and galaxy properties. GC systems are 2--4 times more extended than host galaxies across the entire stellar mass range of our sample (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.09926v1-abstract-full').style.display = 'inline'; document.getElementById('2403.09926v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.09926v1-abstract-full" style="display: none;"> We study the size and structure of globular clusters (GC) systems of 118 early-type galaxies from the NGVS, MATLAS, and ACSVCS surveys. Fitting S茅rsic profiles, we investigate the relationship between effective radii of GC systems ($R_{e, \rm gc}$) and galaxy properties. GC systems are 2--4 times more extended than host galaxies across the entire stellar mass range of our sample ($10^{8.3} < M_* < 10^{11.6}~M_{\odot}$). The relationship between $R_{e, \rm gc}$ and galaxy stellar mass exhibits a characteristic "knee" at a stellar mass of $M_p \simeq 10^{10.8}$, similar to galaxy $R_e$--stellar mass relationship. We present a new characterization of the traditional blue and red GC color sub-populations, describing them with respect to host galaxy $(g'-i')$ color ($螖_{gi}$): GCs with similar colors to their hosts have a "red" $螖_{gi}$, and those significantly bluer GCs have a "blue" $螖_{gi}$. The GC populations with red $螖_{gi}$, even in dwarf galaxies, are twice as extended as the stars, suggesting that formation or survival mechanisms favor the outer regions. We find a tight correlation between $R_{e, \rm gc}$ and the total number of GCs, with intrinsic scatter $\lesssim 0.1$ dex spanning two and three orders of magnitude in size and number, respectively. This holds for both red and blue subpopulations, albeit with different slopes. Assuming that $N_{GC, Total}$ correlates with $M_{200}$, we find that the red GC systems have effective radii of roughly 1-5\% $R_{\rm 200}$, while the blue GC systems in massive galaxies can have sizes as large as $\sim$10\% $R_{\rm 200}$. Environmental dependence on $R_{e, \rm gc}$ is also found, with lower density environments exhibiting more extended GC systems at fixed mass. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.09926v1-abstract-full').style.display = 'none'; document.getElementById('2403.09926v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages, 18 Figures, 3 tables, accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.05448">arXiv:2311.05448</a> <span> [<a href="https://arxiv.org/pdf/2311.05448">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1038/s41586-023-06650-z">10.1038/s41586-023-06650-z <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An evolutionary continuum from nucleated dwarf galaxies to star clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wang%2C+K">Kaixiang Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Peng%2C+E+W">Eric W. Peng</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+C">Chengze Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Mihos%2C+J+C">J. Christopher Mihos</a>, <a href="/search/astro-ph?searchtype=author&query=C%C3%B4t%C3%A9%2C+P">Patrick C么t茅</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrarese%2C+L">Laura Ferrarese</a>, <a href="/search/astro-ph?searchtype=author&query=Taylor%2C+M+A">Matthew A. Taylor</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Cuillandre%2C+J">Jean-Charles Cuillandre</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P">Pierre-Alain Duc</a>, <a href="/search/astro-ph?searchtype=author&query=Guhathakurta%2C+P">Puragra Guhathakurta</a>, <a href="/search/astro-ph?searchtype=author&query=Gwyn%2C+S">Stephen Gwyn</a>, <a href="/search/astro-ph?searchtype=author&query=Ko%2C+Y">Youkyung Ko</a>, <a href="/search/astro-ph?searchtype=author&query=Lan%C3%A7on%2C+A">Ariane Lan莽on</a>, <a href="/search/astro-ph?searchtype=author&query=Lim%2C+S">Sungsoon Lim</a>, <a href="/search/astro-ph?searchtype=author&query=MacArthur%2C+L+A">Lauren A. MacArthur</a>, <a href="/search/astro-ph?searchtype=author&query=Puzia%2C+T">Thomas Puzia</a>, <a href="/search/astro-ph?searchtype=author&query=Roediger%2C+J">Joel Roediger</a>, <a href="/search/astro-ph?searchtype=author&query=Sales%2C+L+V">Laura V. Sales</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">Rub茅n S谩nchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Spengler%2C+C">Chelsea Spengler</a>, <a href="/search/astro-ph?searchtype=author&query=Toloba%2C+E">Elisa Toloba</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+H">Hongxin Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhu%2C+M">Mingcheng Zhu</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.05448v1-abstract-short" style="display: inline;"> Systematic studies have revealed hundreds of ultra-compact dwarf galaxies (UCDs) in the nearby Universe. With half-light radii $r_h$ of approximately 10-100 parsecs and stellar masses $M_*$ $\approx$ $10^6-10^8$ solar masses, UCDs are among the densest known stellar systems. Although similar in appearance to massive globular clusters, the detection of extended stellar envelopes, complex star forma… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.05448v1-abstract-full').style.display = 'inline'; document.getElementById('2311.05448v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.05448v1-abstract-full" style="display: none;"> Systematic studies have revealed hundreds of ultra-compact dwarf galaxies (UCDs) in the nearby Universe. With half-light radii $r_h$ of approximately 10-100 parsecs and stellar masses $M_*$ $\approx$ $10^6-10^8$ solar masses, UCDs are among the densest known stellar systems. Although similar in appearance to massive globular clusters, the detection of extended stellar envelopes, complex star formation histories, elevated mass-to-light ratio, and supermassive black holes suggest that some UCDs are remnant nuclear star clusters of tidally-stripped dwarf galaxies, or even ancient compact galaxies. However, only a few objects have been found in the transient stage of tidal stripping, and this assumed evolutionary path has never been fully traced by observations. Here we show that 106 galaxies in the Virgo cluster have morphologies that are intermediate between normal, nucleated dwarf galaxies and single-component UCDs, revealing a continuum that fully maps this morphological transition, and fills the `size gap' between star clusters and galaxies. Their spatial distribution and redder color are also consistent with stripped satellite galaxies on their first few pericentric passages around massive galaxies. The `ultra-diffuse' tidal features around several of these galaxies directly show how UCDs are forming through tidal stripping, and that this evolutionary path can include an early phase as a nucleated ultra-diffuse galaxy (UDG). These UCDs represent substantial visible fossil remnants of ancient dwarf galaxies in galaxy clusters, and more low-mass remnants probably remain to be found. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.05448v1-abstract-full').style.display = 'none'; document.getElementById('2311.05448v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published in Nature. Accepted on September 15</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nature 623 (2023) 296-300 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.17085">arXiv:2310.17085</a> <span> [<a href="https://arxiv.org/pdf/2310.17085">pdf</a>, <a href="https://arxiv.org/format/2310.17085">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/stad3235">10.1093/mnras/stad3235 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Testing the Surface Brightness Fluctuation Method on Dwarf Galaxies in the COSMOS Field </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Foster%2C+L+M">Lauren M. Foster</a>, <a href="/search/astro-ph?searchtype=author&query=Taylor%2C+J+E">James E. Taylor</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.17085v1-abstract-short" style="display: inline;"> Dwarf galaxies are important tracers of small-scale cosmological structure, yet much of our knowledge about these systems comes from the limited sample of dwarf galaxies within the Local Group. To make a comprehensive inventory of dwarf populations in the local Universe, we require effective methods for deriving distance estimates for large numbers of faint, low surface brightness objects. Here we… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.17085v1-abstract-full').style.display = 'inline'; document.getElementById('2310.17085v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.17085v1-abstract-full" style="display: none;"> Dwarf galaxies are important tracers of small-scale cosmological structure, yet much of our knowledge about these systems comes from the limited sample of dwarf galaxies within the Local Group. To make a comprehensive inventory of dwarf populations in the local Universe, we require effective methods for deriving distance estimates for large numbers of faint, low surface brightness objects. Here we test the surface brightness fluctuation (SBF) method, traditionally applied to brighter early-type galaxies, on a sample of 20 nearby dwarf galaxies detected in the COSMOS field. These objects are partially resolved in HST ACS images, and have confirmed redshift distances in the range 17-130 Mpc. We discuss the many model choices required in applying the SBF method, and explore how these affect the final distance estimates. Amongst other variations on the method, when applying the SBF method, we alter the standard equation to include a term accounting for the power spectrum of the background, greatly improving our results. For the most robust modelling choices, we find a roughly Gaussian SBF signal that correlates linearly with distance out to distances of 50-100 Mpc, but with only a fraction of the power expected. At larger distances, there is excess power relative to that predicted, probably from undetected point sources. Overall, obtaining accurate SBF distances to faint, irregular galaxies remains challenging, but may yet prove possible with the inclusion of more information about galaxy properties and point source populations, and the use of more advanced techniques. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.17085v1-abstract-full').style.display = 'none'; document.getElementById('2310.17085v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 26 figures, accepted by MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.03116">arXiv:2307.03116</a> <span> [<a href="https://arxiv.org/pdf/2307.03116">pdf</a>, <a href="https://arxiv.org/format/2307.03116">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Surface Brightness Fluctuations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2307.03116v2-abstract-short" style="display: inline;"> The Surface Brightness Fluctuation (SBF) method is a powerful tool for determining distances to early-type galaxies. The method measures the intrinsic variance in a galaxy's surface brightness distribution to determine its distance with an accuracy of about 5%. Here, we discuss the mathematical formalism behind the SBF technique, its calibration, and the practicalities of how measurements are perf… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.03116v2-abstract-full').style.display = 'inline'; document.getElementById('2307.03116v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.03116v2-abstract-full" style="display: none;"> The Surface Brightness Fluctuation (SBF) method is a powerful tool for determining distances to early-type galaxies. The method measures the intrinsic variance in a galaxy's surface brightness distribution to determine its distance with an accuracy of about 5%. Here, we discuss the mathematical formalism behind the SBF technique, its calibration, and the practicalities of how measurements are performed. We review the various sources of uncertainties that affect the method and discuss how they can be minimized or controlled through careful observations and data analysis. The SBF technique has already been successfully applied to a large number of galaxies and used for deriving accurate constraints on the Hubble-Lema卯tre constant $H_0$. An approved JWST program will greatly reduce the systematic uncertainties by establishing a firm zero-point calibration using tip of the red giant branch (TRGB) distances. We summarize the existing results and discuss the excellent potential of the SBF method for improving the current constraints on $H_0$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.03116v2-abstract-full').style.display = 'none'; document.getElementById('2307.03116v2-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, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages - 2nd version with minor revisions</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.01863">arXiv:2307.01863</a> <span> [<a href="https://arxiv.org/pdf/2307.01863">pdf</a>, <a href="https://arxiv.org/format/2307.01863">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"> Comparing Globular Cluster System Properties with Host Galaxy Environment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hartman%2C+K">Kate Hartman</a>, <a href="/search/astro-ph?searchtype=author&query=Harris%2C+W+E">William E. Harris</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Ma%2C+C">Chung-Pei Ma</a>, <a href="/search/astro-ph?searchtype=author&query=Greene%2C+J+E">Jenny E. Greene</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2307.01863v1-abstract-short" style="display: inline;"> We present Hubble Space Telescope photometry in optical (F475X) and near-infrared (F110W) bands of the globular cluster (GC) systems of the inner halos of a sample of 15 massive elliptical galaxies. The targets are selected from the volume-limited MASSIVE survey, and chosen to sample a range of environments from sparsely populated groups to BCGs in dense clusters. We also present a quantitative mo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.01863v1-abstract-full').style.display = 'inline'; document.getElementById('2307.01863v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.01863v1-abstract-full" style="display: none;"> We present Hubble Space Telescope photometry in optical (F475X) and near-infrared (F110W) bands of the globular cluster (GC) systems of the inner halos of a sample of 15 massive elliptical galaxies. The targets are selected from the volume-limited MASSIVE survey, and chosen to sample a range of environments from sparsely populated groups to BCGs in dense clusters. We also present a quantitative model of the relation between (F475X - F110W) colour and cluster metallicity [M/H], using simulated GCs. Because much of the GC population in such galaxies is built up through accretion, the metallicity distribution of the GC systems might be expected to vary with galaxy environment. The photometry is used to create a completeness-corrected metallicity distribution for each galaxy in the sample, and to fit a double Gaussian curve to each histogram in order to model the two standard red and blue subpopulations. Finally, the properties of the GC metallicity distribution are correlated against galaxy environment. We find that almost no GCS properties and host galaxy environmental properties are correlated, with the exception of a weak but consistent correlation between blue fraction and nth-nearest neighbour surface density. The results suggest that the systemic properties of the GCS, at least in the inner to mid-halo regions, are influenced more strongly by the local environment at early times, rather than by the environmental properties we see today. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.01863v1-abstract-full').style.display = 'none'; document.getElementById('2307.01863v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 18 figures. Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.15170">arXiv:2306.15170</a> <span> [<a href="https://arxiv.org/pdf/2306.15170">pdf</a>, <a href="https://arxiv.org/ps/2306.15170">ps</a>, <a href="https://arxiv.org/format/2306.15170">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Gathering Galaxy Distances in Abundance with Roman Wide-Area Data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Hudson%2C+M+J">Michael J. Hudson</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrarese%2C+L">Laura Ferrarese</a>, <a href="/search/astro-ph?searchtype=author&query=Hazra%2C+N">Nandini Hazra</a>, <a href="/search/astro-ph?searchtype=author&query=Jensen%2C+J+B">Joseph B. Jensen</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=Raimondo%2C+G">Gabriella Raimondo</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.15170v2-abstract-short" style="display: inline;"> The extragalactic distance scale is fundamental to our understanding of astrophysics and cosmology. In recent years, the surface brightness fluctuation (SBF) method, applied in the near-IR, has proven especially powerful for measuring galaxy distances, first with HST and now with a new JWST program to calibrate the method directly from the tip of the red giant branch (TRGB). So far, however, the d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.15170v2-abstract-full').style.display = 'inline'; document.getElementById('2306.15170v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.15170v2-abstract-full" style="display: none;"> The extragalactic distance scale is fundamental to our understanding of astrophysics and cosmology. In recent years, the surface brightness fluctuation (SBF) method, applied in the near-IR, has proven especially powerful for measuring galaxy distances, first with HST and now with a new JWST program to calibrate the method directly from the tip of the red giant branch (TRGB). So far, however, the distances from space have been gathered slowly, one or two at a time. With the Roman Space Telescope, we have the opportunity to measure uniformly high-quality SBF distances to thousands of galaxies out to hundreds of Mpc. The impact of these data on cosmology and galaxy studies depends on the specifics of the survey, including the filter selection, exposure depth, and (especially) the sky coverage. While the baseline HLWAS survey in four filters plus the grism would yield useful data, the impact would be limited by the relatively small area. A more optimal approach would concentrate on the most efficient passband (F146), adopt an exposure time sufficient to measure good quality distances well out into the Hubble flow, and then maximize the sky coverage within the total time constraints. Grism observations over the same area can provide the needed information on redshifts and spectral energy distributions for compact sources, while colors for larger objects can be obtained from lower resolution surveys. The proposed plan will enable accurate determination of the physical properties of thousands of nearby galaxies, an independent measure of the Hubble constant $H_0$ with negligible statistical error, and competitive constraints on $S_8{\,=\,}蟽_8(惟_m/0.3)^{0.5}$. The resulting data set will be a phenomenal resource for a wide range of studies in astrophysics and cosmology. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.15170v2-abstract-full').style.display = 'none'; document.getElementById('2306.15170v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">5 pages; submitted to the call for Roman Core Community Survey white papers (revised version corrects a couple references)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.08043">arXiv:2210.08043</a> <span> [<a href="https://arxiv.org/pdf/2210.08043">pdf</a>, <a href="https://arxiv.org/format/2210.08043">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The MASSIVE Survey. XVIII. Deep Wide-Field $K$-band Photometry and Local Scaling Relations for Massive Early-Type Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Quenneville%2C+M+E">Matthew E. Quenneville</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Ma%2C+C">Chung-Pei Ma</a>, <a href="/search/astro-ph?searchtype=author&query=Greene%2C+J+E">Jenny E. Greene</a>, <a href="/search/astro-ph?searchtype=author&query=Gwyn%2C+S+D+J">Stephen D. J. Gwyn</a>, <a href="/search/astro-ph?searchtype=author&query=Ciccone%2C+S">Stephanie Ciccone</a>, <a href="/search/astro-ph?searchtype=author&query=Nyiri%2C+B">Blanka Nyiri</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="2210.08043v2-abstract-short" style="display: inline;"> We present wide-field, deep $K$-band photometry of 98 luminous early-type galaxies (ETGs) from the MASSIVE survey based on observations taken with the WIRCam instrument on the Canada-France-Hawaii Telescope. Using these images, we extract accurate total $K$-band luminosities ($L_K$) and half-light radii ($R_e$) for this sample of galaxies. We use these new values to explore the size-luminosity and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.08043v2-abstract-full').style.display = 'inline'; document.getElementById('2210.08043v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.08043v2-abstract-full" style="display: none;"> We present wide-field, deep $K$-band photometry of 98 luminous early-type galaxies (ETGs) from the MASSIVE survey based on observations taken with the WIRCam instrument on the Canada-France-Hawaii Telescope. Using these images, we extract accurate total $K$-band luminosities ($L_K$) and half-light radii ($R_e$) for this sample of galaxies. We use these new values to explore the size-luminosity and Faber-Jackson relations for massive ETGs. Within this volume-limited sample, we find clear evidence for curvature in both relations, indicating that the most luminous galaxies tend to have larger sizes and smaller velocity dispersions than expected from a simple power-law fit to less luminous galaxies. Our measured relations are qualitatively consistent with the most massive elliptical galaxies forming largely through dissipationless mergers. When the sample is separated into fast and slow rotators, we find the slow rotators to exhibit similar changes in slope with increasing $L_K$, suggesting that low-mass and high-mass slow rotators have different formation histories. The curvatures in the $R_e-L_K$ and $蟽-L_K$ relations cancel, leading to a relation between dynamical mass and luminosity that is well described by a single power-law: $R_e蟽^2 \propto {L_K}^b$ with $b \approx 1.2$. This is consistent with the tilt of the fundamental plane observed in lower mass elliptical galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.08043v2-abstract-full').style.display = 'none'; document.getElementById('2210.08043v2-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 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 7 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/2209.11238">arXiv:2209.11238</a> <span> [<a href="https://arxiv.org/pdf/2209.11238">pdf</a>, <a href="https://arxiv.org/format/2209.11238">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac94d8">10.3847/1538-4357/ac94d8 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Cosmicflows-4 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Tully%2C+R+B">R. Brent Tully</a>, <a href="/search/astro-ph?searchtype=author&query=Kourkchi%2C+E">Ehsan Kourkchi</a>, <a href="/search/astro-ph?searchtype=author&query=Courtois%2C+H+M">H茅l猫ne M. Courtois</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+G+S">Gagandeep S. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Brout%2C+D">Dillon Brout</a>, <a href="/search/astro-ph?searchtype=author&query=de+Jaeger%2C+T">Thomas de Jaeger</a>, <a href="/search/astro-ph?searchtype=author&query=Dupuy%2C+A">Alexandra Dupuy</a>, <a href="/search/astro-ph?searchtype=author&query=Guinet%2C+D">Daniel Guinet</a>, <a href="/search/astro-ph?searchtype=author&query=Howlett%2C+C">Cullan Howlett</a>, <a href="/search/astro-ph?searchtype=author&query=Jensen%2C+J+B">Joseph B. Jensen</a>, <a href="/search/astro-ph?searchtype=author&query=Pomar%C3%A8de%2C+D">Daniel Pomar猫de</a>, <a href="/search/astro-ph?searchtype=author&query=Rizzi%2C+L">Luca Rizzi</a>, <a href="/search/astro-ph?searchtype=author&query=Rubin%2C+D">David Rubin</a>, <a href="/search/astro-ph?searchtype=author&query=Said%2C+K">Khaled Said</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">Daniel Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Stahl%2C+B+E">Benjamin E. Stahl</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2209.11238v2-abstract-short" style="display: inline;"> With Cosmicflows-4, distances are compiled for 55,877 galaxies gathered into 38,065 groups. Eight methodologies are employed, with the largest numbers coming from the correlations between the photometric and kinematic properties of spiral galaxies (TF) and elliptical galaxies (FP). Supernovae that arise from degenerate progenitors (type Ia Sne) are an important overlapping component. Smaller contr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.11238v2-abstract-full').style.display = 'inline'; document.getElementById('2209.11238v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.11238v2-abstract-full" style="display: none;"> With Cosmicflows-4, distances are compiled for 55,877 galaxies gathered into 38,065 groups. Eight methodologies are employed, with the largest numbers coming from the correlations between the photometric and kinematic properties of spiral galaxies (TF) and elliptical galaxies (FP). Supernovae that arise from degenerate progenitors (type Ia Sne) are an important overlapping component. Smaller contributions come from distance estimates from the surface brightness fluctuations of elliptical galaxies and the luminosities and expansion rates of core collapse supernovae (SNII). Cepheid period-luminosity relation and tip of the red giant branch observations founded on local stellar parallax measurements along with the geometric maser distance to NGC 4258 provide the absolute scaling of distances. The assembly of galaxies into groups is an important feature of the study in facilitating overlaps between methodologies. Merging between multiple contributions within a methodology and between methodologies is carried out with Bayesian Markov chain Monte Carlo procedures. The final assembly of distances is compatible with a value of the Hubble constant of $H_0=74.6$ km s$^{-1}$ Mpc$^{-1}$ with the small statistical error of $\pm 0.8$ km s$^{-1}$ Mpc$^{-1}$ but a large potential systematic error of ~3 km s$^{-1}$ Mpc$^{-1}$. Peculiar velocities can be inferred from the measured distances. The interpretation of the field of peculiar velocities is complex because of large errors on individual components and invites analyses beyond the scope of this study. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.11238v2-abstract-full').style.display = 'none'; document.getElementById('2209.11238v2-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">38 pages, 24 figures. catalogs available at edd.ifa.hawaii.edu. Revised version, accepted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.09124">arXiv:2205.09124</a> <span> [<a href="https://arxiv.org/pdf/2205.09124">pdf</a>, <a href="https://arxiv.org/format/2205.09124">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/10.1051/0004-6361/202243390">10.1051/0004-6361/202243390 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A study of globular clusters in a lenticular galaxy in Hydra I from deep HST/ACS photometry </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hazra%2C+N">Nandini Hazra</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Raimondo%2C+G">Gabriella Raimondo</a>, <a href="/search/astro-ph?searchtype=author&query=Mirabile%2C+M">Marco Mirabile</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Branchesi%2C+M">Marica Branchesi</a>, <a href="/search/astro-ph?searchtype=author&query=Brocato%2C+E">Enzo Brocato</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2205.09124v1-abstract-short" style="display: inline;"> We take advantage of exquisitely deep optical imaging data from HST/ACS in the F475W ($g_{F475W}$) and F606W ($V_{F606W}$) bands, to study the properties of the globular cluster (GC) population in the intermediate mass lenticular galaxy PGC 087327, in the Hydra I galaxy cluster. We inspect the photometric (magnitudes and color) and morphometric (compactness, elongation, etc.) properties of sources… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.09124v1-abstract-full').style.display = 'inline'; document.getElementById('2205.09124v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.09124v1-abstract-full" style="display: none;"> We take advantage of exquisitely deep optical imaging data from HST/ACS in the F475W ($g_{F475W}$) and F606W ($V_{F606W}$) bands, to study the properties of the globular cluster (GC) population in the intermediate mass lenticular galaxy PGC 087327, in the Hydra I galaxy cluster. We inspect the photometric (magnitudes and color) and morphometric (compactness, elongation, etc.) properties of sources lying in an area of $\sim19\times19$ kpc centered on PGC 087327, and compare them with four neighbouring fields over the same HST/ACS mosaic. This allowed us to identify a list of GC candidates and to inspect their properties using a background decontamination method. Relative to the four comparison fields, PGC 087327 shows a robust overdensity of GCs, $N_{GC}=82\pm9$. At the estimated magnitude of the galaxy, this number implies a specific frequency of $S_N=1.8\pm0.7$. In spite of the short wavelength interval available with the $g_{F475W}$ and $V_{F606W}$ passbands, the color distribution shows a clear bimodality with a blue peak at $\langle g_{F475W}{-}V_{F606W} \rangle =0.47\pm0.05$ mag and a red peak at $\langle g_{F475W}{-}V_{F606W}\rangle =0.62\pm0.03$ mag. We also observe the typical steeper slope of the radial distribution of red GCs relative to blue ones. Thanks to the unique depth of the available data, we characterize the GC luminosity function (GCLF) well beyond the expected GCLF turn-over. We find $g^{TOM}_{F475W} = 26.54\pm0.10$ mag and $V^{TOM}_{F606W} = 26.08 \pm 0.09$ mag, which after calibration yields a distance of $D_{GCLF} = 56.7 \pm 4.3(statistical) \pm 5.2(systematic)$ Mpc. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.09124v1-abstract-full').style.display = 'none'; document.getElementById('2205.09124v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">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 666, A99 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.12060">arXiv:2204.12060</a> <span> [<a href="https://arxiv.org/pdf/2204.12060">pdf</a>, <a href="https://arxiv.org/format/2204.12060">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</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/ace04b">10.3847/1538-4357/ace04b <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Connecting Infrared Surface Brightness Fluctuation Distances to Type Ia Supernova Hosts: Testing the Top Rung of the Distance Ladder </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Garnavich%2C+P">Peter Garnavich</a>, <a href="/search/astro-ph?searchtype=author&query=Wood%2C+C+M">Charlotte M. Wood</a>, <a href="/search/astro-ph?searchtype=author&query=Milne%2C+P">Peter Milne</a>, <a href="/search/astro-ph?searchtype=author&query=Jensen%2C+J+B">Joseph B. Jensen</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+P+J">Peter J. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">Daniel Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Rose%2C+B">Benjamin Rose</a>, <a href="/search/astro-ph?searchtype=author&query=Brout%2C+D">Dillon Brout</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="2204.12060v2-abstract-short" style="display: inline;"> We compare infrared surface brightness fluctuation (IR SBF) distances measured in galaxies that have hosted type Ia supernovae (SNIa) to distances estimated from SNIa light curve fits. We show that the properties of SNIa found in IR SBF hosts are very different from those exploding in Cepheid calibrators, therefore, this is a direct test of systematic uncertainties on estimation of the Hubble cons… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.12060v2-abstract-full').style.display = 'inline'; document.getElementById('2204.12060v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.12060v2-abstract-full" style="display: none;"> We compare infrared surface brightness fluctuation (IR SBF) distances measured in galaxies that have hosted type Ia supernovae (SNIa) to distances estimated from SNIa light curve fits. We show that the properties of SNIa found in IR SBF hosts are very different from those exploding in Cepheid calibrators, therefore, this is a direct test of systematic uncertainties on estimation of the Hubble constant (Ho) using supernovae. The IR SBF results from Jensen et al. (2021; arXiv:2105.08299) provide a large and uniformly measured sample of IR SBF distances which we directly compare with distances to 25 SNIa host galaxies. We divide the Hubble flow SNIa into sub-samples that best match the divergent supernova properties seen in the IR SBF hosts and Cepheid hosts. We further divide the SNIa into a sample with light curve widths and host masses that are congruent to those found in the SBF-calibrated hosts. We refit the light curve stretch and color correlations with luminosity, and use these revised parameters to calibrate the Hubble flow supernovae with IR SBF calibrators. Relative to the Hubble flow, the average calibrator distance moduli vary by 0.03mag depending on the SNIa subsamples examined and this adds a 1.8% systematic uncertainty to our Hubble constant estimate. Based on the IR SBF calibrators, Ho=74.6$\pm$0.9(stat)$\pm$ 2.7(syst) km/s/Mpc, which is consistent with the Hubble constant derived from supernovae calibrated from Cepheid variables. We conclude that IR SBF provides reliable calibration of SNIa with a precision comparable to Cepheid calibrators, and with a significant saving in telescope time. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.12060v2-abstract-full').style.display = 'none'; document.getElementById('2204.12060v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 10 figures, 4 tables, accepted for publication in the Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.05318">arXiv:2204.05318</a> <span> [<a href="https://arxiv.org/pdf/2204.05318">pdf</a>, <a href="https://arxiv.org/ps/2204.05318">ps</a>, <a href="https://arxiv.org/format/2204.05318">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac63cf">10.3847/1538-4357/ac63cf <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Next Generation Virgo Cluster Survey. XXXIII. Stellar Population Gradients in the Virgo Cluster Core Globular Cluster System </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ko%2C+Y">Youkyung Ko</a>, <a href="/search/astro-ph?searchtype=author&query=Peng%2C+E+W">Eric W. Peng</a>, <a href="/search/astro-ph?searchtype=author&query=C%C3%B4t%C3%A9%2C+P">Patrick C么t茅</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrarese%2C+L">Laura Ferrarese</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+C">Chengze Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Longobardi%2C+A">Alessia Longobardi</a>, <a href="/search/astro-ph?searchtype=author&query=Lan%C3%A7on%2C+A">Ariane Lan莽on</a>, <a href="/search/astro-ph?searchtype=author&query=Mu%C3%B1oz%2C+R+P">Roberto P. Mu帽oz</a>, <a href="/search/astro-ph?searchtype=author&query=Puzia%2C+T+H">Thomas H. Puzia</a>, <a href="/search/astro-ph?searchtype=author&query=Alamo-Mart%C3%ADnez%2C+K+A">Karla A. Alamo-Mart铆nez</a>, <a href="/search/astro-ph?searchtype=author&query=Sales%2C+L+V">Laura V. Sales</a>, <a href="/search/astro-ph?searchtype=author&query=Ramos-Almendares%2C+F">Felipe Ramos-Almendares</a>, <a href="/search/astro-ph?searchtype=author&query=Abadi%2C+M+G">Mario G. Abadi</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+M+G">Myung Gyoon Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+H+S">Ho Seong Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=Caldwell%2C+N">Nelson Caldwell</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Boselli%2C+A">Alessandro Boselli</a>, <a href="/search/astro-ph?searchtype=author&query=Cuillandre%2C+J">Jean-Charles Cuillandre</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P">Pierre-Alain Duc</a>, <a href="/search/astro-ph?searchtype=author&query=Eyheramendy%2C+S">Susana Eyheramendy</a>, <a href="/search/astro-ph?searchtype=author&query=Guhathakurta%2C+P">Puragra Guhathakurta</a>, <a href="/search/astro-ph?searchtype=author&query=Gwyn%2C+S">Stephen Gwyn</a>, <a href="/search/astro-ph?searchtype=author&query=Jord%C3%A1n%2C+A">Andr茅s Jord谩n</a>, <a href="/search/astro-ph?searchtype=author&query=Lim%2C+S">Sungsoon Lim</a> , et al. (2 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2204.05318v1-abstract-short" style="display: inline;"> We present a study of the stellar populations of globular clusters (GCs) in the Virgo Cluster core with a homogeneous spectroscopic catalog of 692 GCs within a major axis distance $R_{\rm maj} = $ 840 kpc from M87. We investigate radial and azimuthal variations in the mean age, total metallicity, [Fe/H], and $伪$-element abundance, of blue (metal-poor) and red (metal-rich) GCs using their co-added… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.05318v1-abstract-full').style.display = 'inline'; document.getElementById('2204.05318v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.05318v1-abstract-full" style="display: none;"> We present a study of the stellar populations of globular clusters (GCs) in the Virgo Cluster core with a homogeneous spectroscopic catalog of 692 GCs within a major axis distance $R_{\rm maj} = $ 840 kpc from M87. We investigate radial and azimuthal variations in the mean age, total metallicity, [Fe/H], and $伪$-element abundance, of blue (metal-poor) and red (metal-rich) GCs using their co-added spectra. We find that the blue GCs have a steep radial gradient in [Z/H] within $R_{\rm maj} =$ 165 kpc, with roughly equal contributions from [Fe/H] and [$伪$/Fe], and flat gradients beyond. By contrast, the red GCs show a much shallower gradient in [Z/H], which is entirely driven by [Fe/H]. We use GC-tagged Illustris simulations to demonstrate an accretion scenario where more massive satellites (with more metal- and $伪$-rich GCs) sink further into the central galaxy than less massive ones, and where the gradient flattening occurs because of the low GC occupation fraction of low-mass dwarfs disrupted at larger distances. The dense environment around M87 may also cause the steep [$伪$/Fe] gradient of the blue GCs, mirroring what is seen in the dwarf galaxy population. The progenitors of red GCs have a narrower mass range than those of blue GCs, which makes their gradients shallower. We also explore spatial inhomogeneity in GC abundances, finding that the red GCs to the northwest of M87 are slightly more metal-rich. Future observations of GC stellar population gradients will be useful diagnostics of halo merger histories. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.05318v1-abstract-full').style.display = 'none'; document.getElementById('2204.05318v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 8 figures, 4 tables, accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.06142">arXiv:2203.06142</a> <span> [<a href="https://arxiv.org/pdf/2203.06142">pdf</a>, <a href="https://arxiv.org/format/2203.06142">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</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/10.1016/j.jheap.2022.04.002">10.1016/j.jheap.2022.04.002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Cosmology Intertwined: A Review of the Particle Physics, Astrophysics, and Cosmology Associated with the Cosmological Tensions and Anomalies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abdalla%2C+E">Elcio Abdalla</a>, <a href="/search/astro-ph?searchtype=author&query=Abell%C3%A1n%2C+G+F">Guillermo Franco Abell谩n</a>, <a href="/search/astro-ph?searchtype=author&query=Aboubrahim%2C+A">Amin Aboubrahim</a>, <a href="/search/astro-ph?searchtype=author&query=Agnello%2C+A">Adriano Agnello</a>, <a href="/search/astro-ph?searchtype=author&query=Akarsu%2C+O">Ozgur Akarsu</a>, <a href="/search/astro-ph?searchtype=author&query=Akrami%2C+Y">Yashar Akrami</a>, <a href="/search/astro-ph?searchtype=author&query=Alestas%2C+G">George Alestas</a>, <a href="/search/astro-ph?searchtype=author&query=Aloni%2C+D">Daniel Aloni</a>, <a href="/search/astro-ph?searchtype=author&query=Amendola%2C+L">Luca Amendola</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L+A">Luis A. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+R+I">Richard I. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Arendse%2C+N">Nikki Arendse</a>, <a href="/search/astro-ph?searchtype=author&query=Asgari%2C+M">Marika Asgari</a>, <a href="/search/astro-ph?searchtype=author&query=Ballardini%2C+M">Mario Ballardini</a>, <a href="/search/astro-ph?searchtype=author&query=Barger%2C+V">Vernon Barger</a>, <a href="/search/astro-ph?searchtype=author&query=Basilakos%2C+S">Spyros Basilakos</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+C">Ronaldo C. Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Battistelli%2C+E+S">Elia S. Battistelli</a>, <a href="/search/astro-ph?searchtype=author&query=Battye%2C+R">Richard Battye</a>, <a href="/search/astro-ph?searchtype=author&query=Benetti%2C+M">Micol Benetti</a>, <a href="/search/astro-ph?searchtype=author&query=Benisty%2C+D">David Benisty</a>, <a href="/search/astro-ph?searchtype=author&query=Berlin%2C+A">Asher Berlin</a>, <a href="/search/astro-ph?searchtype=author&query=de+Bernardis%2C+P">Paolo de Bernardis</a>, <a href="/search/astro-ph?searchtype=author&query=Berti%2C+E">Emanuele Berti</a>, <a href="/search/astro-ph?searchtype=author&query=Bidenko%2C+B">Bohdan Bidenko</a> , et al. (178 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="2203.06142v3-abstract-short" style="display: inline;"> In this paper we will list a few important goals that need to be addressed in the next decade, also taking into account the current discordances between the different cosmological probes, such as the disagreement in the value of the Hubble constant $H_0$, the $蟽_8$--$S_8$ tension, and other less statistically significant anomalies. While these discordances can still be in part the result of system… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.06142v3-abstract-full').style.display = 'inline'; document.getElementById('2203.06142v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.06142v3-abstract-full" style="display: none;"> In this paper we will list a few important goals that need to be addressed in the next decade, also taking into account the current discordances between the different cosmological probes, such as the disagreement in the value of the Hubble constant $H_0$, the $蟽_8$--$S_8$ tension, and other less statistically significant anomalies. While these discordances can still be in part the result of systematic errors, their persistence after several years of accurate analysis strongly hints at cracks in the standard cosmological scenario and the necessity for new physics or generalisations beyond the standard model. In this paper, we focus on the $5.0\,蟽$ tension between the {\it Planck} CMB estimate of the Hubble constant $H_0$ and the SH0ES collaboration measurements. After showing the $H_0$ evaluations made from different teams using different methods and geometric calibrations, we list a few interesting new physics models that could alleviate this tension and discuss how the next decade's experiments will be crucial. Moreover, we focus on the tension of the {\it Planck} CMB data with weak lensing measurements and redshift surveys, about the value of the matter energy density $惟_m$, and the amplitude or rate of the growth of structure ($蟽_8,f蟽_8$). We list a few interesting models proposed for alleviating this tension, and we discuss the importance of trying to fit a full array of data with a single model and not just one parameter at a time. Additionally, we present a wide range of other less discussed anomalies at a statistical significance level lower than the $H_0$--$S_8$ tensions which may also constitute hints towards new physics, and we discuss possible generic theoretical approaches that can collectively explain the non-standard nature of these signals.[Abridged] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.06142v3-abstract-full').style.display = 'none'; document.getElementById('2203.06142v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Contribution to Snowmass 2021. 224 pages, 27 figures. Accepted for publication in JHEAp</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> J. High En. Astrophys. 2204, 002 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.07241">arXiv:2201.07241</a> <span> [<a href="https://arxiv.org/pdf/2201.07241">pdf</a>, <a href="https://arxiv.org/format/2201.07241">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1007/s41114-022-00040-z">10.1007/s41114-022-00040-z <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Unveiling the Universe with Emerging Cosmological Probes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Moresco%2C+M">Michele Moresco</a>, <a href="/search/astro-ph?searchtype=author&query=Amati%2C+L">Lorenzo Amati</a>, <a href="/search/astro-ph?searchtype=author&query=Amendola%2C+L">Luca Amendola</a>, <a href="/search/astro-ph?searchtype=author&query=Birrer%2C+S">Simon Birrer</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Cimatti%2C+A">Andrea Cimatti</a>, <a href="/search/astro-ph?searchtype=author&query=Darling%2C+J">Jeremy Darling</a>, <a href="/search/astro-ph?searchtype=author&query=Della+Valle%2C+M">Massimo Della Valle</a>, <a href="/search/astro-ph?searchtype=author&query=Fishbach%2C+M">Maya Fishbach</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">Claudio Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Hamaus%2C+N">Nico Hamaus</a>, <a href="/search/astro-ph?searchtype=author&query=Holz%2C+D">Daniel Holz</a>, <a href="/search/astro-ph?searchtype=author&query=Izzo%2C+L">Luca Izzo</a>, <a href="/search/astro-ph?searchtype=author&query=Jimenez%2C+R">Raul Jimenez</a>, <a href="/search/astro-ph?searchtype=author&query=Lusso%2C+E">Elisabeta Lusso</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">Massimo Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Piedipalumbo%2C+E">Ester Piedipalumbo</a>, <a href="/search/astro-ph?searchtype=author&query=Pisani%2C+A">Alice Pisani</a>, <a href="/search/astro-ph?searchtype=author&query=Pourtsidou%2C+A">Alkistis Pourtsidou</a>, <a href="/search/astro-ph?searchtype=author&query=Pozzetti%2C+L">Lucia Pozzetti</a>, <a href="/search/astro-ph?searchtype=author&query=Quartin%2C+M">Miguel Quartin</a>, <a href="/search/astro-ph?searchtype=author&query=Risaliti%2C+G">Guido Risaliti</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">Piero Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Verde%2C+L">Licia Verde</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2201.07241v2-abstract-short" style="display: inline;"> The detection of the accelerated expansion of the Universe has been one of the major breakthroughs in modern cosmology. Several cosmological probes (CMB, SNe Ia, BAO) have been studied in depth to better understand the nature of the mechanism driving this acceleration, and they are being currently pushed to their limits, obtaining remarkable constraints that allowed us to shape the standard cosmol… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.07241v2-abstract-full').style.display = 'inline'; document.getElementById('2201.07241v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.07241v2-abstract-full" style="display: none;"> The detection of the accelerated expansion of the Universe has been one of the major breakthroughs in modern cosmology. Several cosmological probes (CMB, SNe Ia, BAO) have been studied in depth to better understand the nature of the mechanism driving this acceleration, and they are being currently pushed to their limits, obtaining remarkable constraints that allowed us to shape the standard cosmological model. In parallel to that, however, the percent precision achieved has recently revealed apparent tensions between measurements obtained from different methods. These are either indicating some unaccounted systematic effects, or are pointing toward new physics. Following the development of CMB, SNe, and BAO cosmology, it is critical to extend our selection of cosmological probes. Novel probes can be exploited to validate results, control or mitigate systematic effects, and, most importantly, to increase the accuracy and robustness of our results. This review is meant to provide a state-of-art benchmark of the latest advances in emerging beyond-standard cosmological probes. We present how several different methods can become a key resource for observational cosmology. In particular, we review cosmic chronometers, quasars, gamma-ray bursts, standard sirens, lensing time-delay with galaxies and clusters, cosmic voids, neutral hydrogen intensity mapping, surface brightness fluctuations, stellar ages of the oldest objects, secular redshift drift, and clustering of standard candles. The review describes the method, systematics, and results of each probe in a homogeneous way, giving the reader a clear picture of the available innovative methods that have been introduced in recent years and how to apply them. The review also discusses the potential synergies and complementarities between the various probes, exploring how they will contribute to the future of modern cosmology. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.07241v2-abstract-full').style.display = 'none'; document.getElementById('2201.07241v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Invited review article for Living Reviews in Relativity. Accepted version. 191 pages, 54 figures, 11 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.13699">arXiv:2111.13699</a> <span> [<a href="https://arxiv.org/pdf/2111.13699">pdf</a>, <a href="https://arxiv.org/format/2111.13699">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/ac58fd">10.3847/1538-4357/ac58fd <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MASSIVE Survey -- XVII. A Triaxial Orbit-based Determination of the Black Hole Mass and Intrinsic Shape of Elliptical Galaxy NGC 2693 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pilawa%2C+J+D">Jacob D. Pilawa</a>, <a href="/search/astro-ph?searchtype=author&query=Liepold%2C+C+M">Christopher M. Liepold</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade%2C+S+C+D">Silvana C. Delgado Andrade</a>, <a href="/search/astro-ph?searchtype=author&query=Walsh%2C+J+L">Jonelle L. Walsh</a>, <a href="/search/astro-ph?searchtype=author&query=Ma%2C+C">Chung-Pei Ma</a>, <a href="/search/astro-ph?searchtype=author&query=Quenneville%2C+M+E">Matthew E. Quenneville</a>, <a href="/search/astro-ph?searchtype=author&query=Greene%2C+J+E">Jenny E. Greene</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2111.13699v2-abstract-short" style="display: inline;"> We present a stellar dynamical mass measurement of a newly detected supermassive black hole (SMBH) at the center of the fast-rotating, massive elliptical galaxy NGC 2693 as part of the MASSIVE survey. We combine high signal-to-noise integral field spectroscopy (IFS) from the Gemini Multi-Object Spectrograph (GMOS) with wide-field data from the Mitchell Spectrograph at McDonald Observatory to extra… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.13699v2-abstract-full').style.display = 'inline'; document.getElementById('2111.13699v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.13699v2-abstract-full" style="display: none;"> We present a stellar dynamical mass measurement of a newly detected supermassive black hole (SMBH) at the center of the fast-rotating, massive elliptical galaxy NGC 2693 as part of the MASSIVE survey. We combine high signal-to-noise integral field spectroscopy (IFS) from the Gemini Multi-Object Spectrograph (GMOS) with wide-field data from the Mitchell Spectrograph at McDonald Observatory to extract and model stellar kinematics of NGC 2693 from the central $\sim 150$ pc out to $\sim2.5$ effective radii. Observations from Hubble Space Telescope (HST) WFC3 are used to determine the stellar light distribution. We perform fully triaxial Schwarzschild orbit modeling using the latest TriOS code and a Bayesian search in 6-D galaxy model parameter space to determine NGC 2693's SMBH mass ($M_\text{BH}$), stellar mass-to-light ratio, dark matter content, and intrinsic shape. We find $M_\text{BH} = \left(1.7\pm 0.4\right)\times 10^{9}\ M_\odot$ and a triaxial intrinsic shape with axis ratios $p=b/a=0.902 \pm 0.009$ and $q=c/a=0.721^{+0.011}_{-0.010}$, triaxiality parameter $T = 0.39 \pm 0.04$. In comparison, the best-fit orbit model in the axisymmetric limit and (cylindrical) Jeans anisotropic model of NGC 2693 prefer $M_\text{BH} = \left(2.4\pm 0.6\right)\times 10^{9}\ M_\odot$ and $M_\text{BH} = \left(2.9\pm 0.3\right)\times 10^{9}\ M_\odot$, respectively. Neither model can account for the non-axisymmetric stellar velocity features present in the IFS data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.13699v2-abstract-full').style.display = 'none'; document.getElementById('2111.13699v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 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">18 pages, 9 figures, 2 tables, accepted to ApJ 2022/02/24</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2110.11985">arXiv:2110.11985</a> <span> [<a href="https://arxiv.org/pdf/2110.11985">pdf</a>, <a href="https://arxiv.org/format/2110.11985">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/ac69ea">10.3847/1538-4357/ac69ea <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MASSIVE SURVEY XVI. The Stellar Initial Mass Function in the Center of MASSIVE Early-Type Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gu%2C+M">Meng Gu</a>, <a href="/search/astro-ph?searchtype=author&query=Greene%2C+J">Jenny Greene</a>, <a href="/search/astro-ph?searchtype=author&query=Newman%2C+A+B">Andrew B. Newman</a>, <a href="/search/astro-ph?searchtype=author&query=Kreisch%2C+C">Christina Kreisch</a>, <a href="/search/astro-ph?searchtype=author&query=Quenneville%2C+M">Matthew Quenneville</a>, <a href="/search/astro-ph?searchtype=author&query=Ma%2C+C">Chung-Pei Ma</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2110.11985v1-abstract-short" style="display: inline;"> The stellar initial mass function (IMF) is a fundamental property in the measurement of stellar masses and galaxy star formation histories. In this work we focus on the most massive galaxies in the nearby universe $\log(M_{\star}/M_{\odot})>11.2$. We obtain high quality Magellan/LDSS-3 long slit spectroscopy with a wide wavelength coverage of $0.4渭{\rm m}-1.01渭{\rm m}$ for 41 early-type galaxies (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.11985v1-abstract-full').style.display = 'inline'; document.getElementById('2110.11985v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.11985v1-abstract-full" style="display: none;"> The stellar initial mass function (IMF) is a fundamental property in the measurement of stellar masses and galaxy star formation histories. In this work we focus on the most massive galaxies in the nearby universe $\log(M_{\star}/M_{\odot})>11.2$. We obtain high quality Magellan/LDSS-3 long slit spectroscopy with a wide wavelength coverage of $0.4渭{\rm m}-1.01渭{\rm m}$ for 41 early-type galaxies (ETGs) in the MASSIVE survey, and derive high S/N spectra within an aperture of $R_{\rm e}/8$. Using detailed stellar synthesis models, we constrain the elemental abundances and stellar IMF of each galaxy through full spectral modeling. All the ETGs in our sample have an IMF that is steeper than a Milky Way (Kroupa) IMF. The best-fit IMF mismatch parameter, $伪_{\rm IMF}=(M/L)/(M/L)_{\rm MW}$, ranges from 1.12 to 3.05, with an average of $\langle 伪_{\rm IMF} \rangle=1.84$, suggesting that on average, the IMF is more bottom-heavy than Salpeter. Comparing the estimated stellar mass with the dynamical mass, we find that most galaxies have stellar masses smaller than their dynamical masses within the $1蟽$ uncertainty. We complement our sample with lower-mass galaxies from the literature, and confirm that $\log(伪_{\rm IMF})$ is positively correlated with $\log(蟽)$, $\log(M_{\star})$, and $\log(M_{\rm dyn})$. The IMF in the centers of more massive ETGs is more bottom-heavy. In addition, we find that $\log(伪_{\rm IMF})$ is positively correlated with both [Mg/Fe] and the estimated total metallicity [Z/H]. We find suggestive evidence that the effective stellar surface density $危_{\rm Kroupa}$ might be responsible for the variation of $伪_{\rm IMF}$. We conclude that $蟽$, [Mg/Fe] and [Z/H] are the primary drivers of the global stellar IMF variation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.11985v1-abstract-full').style.display = 'none'; document.getElementById('2110.11985v1-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 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 pages, 11 figures, submitted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.08299">arXiv:2105.08299</a> <span> [<a href="https://arxiv.org/pdf/2105.08299">pdf</a>, <a href="https://arxiv.org/format/2105.08299">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4365/ac01e7">10.3847/1538-4365/ac01e7 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Infrared Surface Brightness Fluctuation Distances for MASSIVE and Type Ia Supernova Host Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jensen%2C+J+B">Joseph B. Jensen</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Ma%2C+C">Chung-Pei Ma</a>, <a href="/search/astro-ph?searchtype=author&query=Milne%2C+P+A">Peter A. Milne</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+P+J">Peter J. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Garnavich%2C+P+M">Peter M. Garnavich</a>, <a href="/search/astro-ph?searchtype=author&query=Greene%2C+J+E">Jenny E. Greene</a>, <a href="/search/astro-ph?searchtype=author&query=Lucey%2C+J+R">John R. Lucey</a>, <a href="/search/astro-ph?searchtype=author&query=Phan%2C+A">Anh Phan</a>, <a href="/search/astro-ph?searchtype=author&query=Tully%2C+R+B">R. Brent Tully</a>, <a href="/search/astro-ph?searchtype=author&query=Wood%2C+C+M">Charlotte M. Wood</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2105.08299v1-abstract-short" style="display: inline;"> We measured high-quality surface brightness fluctuation (SBF) distances for a sample of 63 massive early-type galaxies using the WFC3/IR camera on the Hubble Space Telescope. The median uncertainty on the SBF distance measurements is 0.085 mag, or 3.9% in distance. Achieving this precision at distances of 50 to 100 Mpc required significant improvements to the SBF calibration and data analysis proc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.08299v1-abstract-full').style.display = 'inline'; document.getElementById('2105.08299v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.08299v1-abstract-full" style="display: none;"> We measured high-quality surface brightness fluctuation (SBF) distances for a sample of 63 massive early-type galaxies using the WFC3/IR camera on the Hubble Space Telescope. The median uncertainty on the SBF distance measurements is 0.085 mag, or 3.9% in distance. Achieving this precision at distances of 50 to 100 Mpc required significant improvements to the SBF calibration and data analysis procedures for WFC3/IR data. Forty-two of the galaxies are from the MASSIVE Galaxy Survey, a complete sample of massive galaxies within ~100 Mpc; the SBF distances for these will be used to improve the estimates of the stellar and central supermassive black hole masses in these galaxies. Twenty-four of the galaxies are Type Ia supernova hosts, useful for calibrating SN Ia distances for early-type galaxies and exploring possible systematic trends in the peak luminosities. Our results demonstrate that the SBF method is a powerful and versatile technique for measuring distances to galaxies with evolved stellar populations out to 100 Mpc and constraining the local value of the Hubble constant. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.08299v1-abstract-full').style.display = 'none'; document.getElementById('2105.08299v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astrophysical Journal Supplement Series; 22 pages, 7 figures, with 61 additional figures to be published as an online figure set</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2103.02123">arXiv:2103.02123</a> <span> [<a href="https://arxiv.org/pdf/2103.02123">pdf</a>, <a href="https://arxiv.org/format/2103.02123">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stab2348">10.1093/mnras/stab2348 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A high occurrence of nuclear star clusters in faint Coma galaxies, and the roles of mass and environment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zanatta%2C+E+J+B">Emilio J. B. Zanatta</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">Rub茅n S谩nchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Chies-Santos%2C+A+L">Ana L. Chies-Santos</a>, <a href="/search/astro-ph?searchtype=author&query=de+Souza%2C+R+S">Rafael S. de Souza</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2103.02123v2-abstract-short" style="display: inline;"> We use deep high resolution \textit{HST/ACS} imaging of two fields in the core of the Coma cluster to investigate the occurrence of nuclear star clusters (NSCs) in quiescent dwarf galaxies as faint as $M_{I} = -10$ mag. We employ a hierarchical Bayesian logistic regression framework to model the faint end of the nucleation fraction ($f_{n}$) as a function of both galaxy luminosity and environment.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.02123v2-abstract-full').style.display = 'inline'; document.getElementById('2103.02123v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.02123v2-abstract-full" style="display: none;"> We use deep high resolution \textit{HST/ACS} imaging of two fields in the core of the Coma cluster to investigate the occurrence of nuclear star clusters (NSCs) in quiescent dwarf galaxies as faint as $M_{I} = -10$ mag. We employ a hierarchical Bayesian logistic regression framework to model the faint end of the nucleation fraction ($f_{n}$) as a function of both galaxy luminosity and environment. We find that $f_n$ is remarkably high in Coma: at $M_{I} \approx -13$ mag half of the cluster dwarfs still host prominent NSCs. Comparison with dwarf systems in nearby clusters and groups shows that, within the uncertainties, the rate at which the probability of nucleation varies with galaxy luminosity is nearly universal. On the other hand, the fraction of nucleated galaxies at fixed luminosity does exhibit an environmental dependence. More massive environments feature higher nucleation fractions and fainter values of the half-nucleation luminosity, which roughly scales with host halo virial mass as $L_{I,f_{n50}} \propto \mathcal{M}_{200}^{-0.2}$. Our results reinforce the role of galaxy luminosity/mass as a major driver of the efficiency of NSC formation and also indicate a clear secondary dependence on the environment, hence paving the way to more refined theoretical models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.02123v2-abstract-full').style.display = 'none'; document.getElementById('2103.02123v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 11 figures, accepted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.02221">arXiv:2101.02221</a> <span> [<a href="https://arxiv.org/pdf/2101.02221">pdf</a>, <a href="https://arxiv.org/format/2101.02221">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</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/abe86a">10.3847/1538-4357/abe86a <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Hubble Constant from Infrared Surface Brightness Fluctuation Distances </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Jensen%2C+J+B">Joseph B. Jensen</a>, <a href="/search/astro-ph?searchtype=author&query=Ma%2C+C">Chung-Pei Ma</a>, <a href="/search/astro-ph?searchtype=author&query=Milne%2C+P+A">Peter A. Milne</a>, <a href="/search/astro-ph?searchtype=author&query=Greene%2C+J+E">Jenny E. Greene</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="2101.02221v2-abstract-short" style="display: inline;"> We present a measurement of the Hubble constant $H_0$ from surface brightness fluctuation (SBF) distances for 63 bright, mainly early-type galaxies out to 100 Mpc observed with the Wide Field Camera 3 Infrared Channel (WFC3/IR) on the Hubble Space Telescope (HST). The sample is drawn from several independent HST imaging programs using the F110W bandpass of WFC3/IR. The majority of galaxies are in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.02221v2-abstract-full').style.display = 'inline'; document.getElementById('2101.02221v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.02221v2-abstract-full" style="display: none;"> We present a measurement of the Hubble constant $H_0$ from surface brightness fluctuation (SBF) distances for 63 bright, mainly early-type galaxies out to 100 Mpc observed with the Wide Field Camera 3 Infrared Channel (WFC3/IR) on the Hubble Space Telescope (HST). The sample is drawn from several independent HST imaging programs using the F110W bandpass of WFC3/IR. The majority of galaxies are in the 50 to 80 Mpc range and come from the MASSIVE galaxy survey. The median statistical uncertainty on individual distance measurements is 4%. We construct the Hubble diagram with these IR SBF distances and constrain $H_0$ using {four} different treatments of the galaxy velocities. For the SBF zero point calibration, we use both the existing tie to Cepheid variables, updated for consistency with the latest determination of the distance to the Large Magellanic Cloud from detached eclipsing binaries, and a new tie to the tip of the red giant branch (TRGB) calibrated from the maser distance to NGC4258. These two SBF calibrations are consistent with each other and with theoretical predictions from stellar population models. From a weighted average of the Cepheid and TRGB calibrations, we derive $H_0=73.3{\,\pm\,}0.7{\,\pm\,}2.4$ km/s/Mpc, where the error bars reflect the statistical and systematic uncertainties. This result accords well with recent measurements of $H_0$ from Type~Ia supernovae, time delays in multiply lensed quasars, and water masers. The systematic uncertainty could be reduced to below 2% by calibrating the SBF method with precision TRGB distances for a statistical sample of massive early-type galaxies out to the Virgo cluster measured with the James Webb Space Telescope. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.02221v2-abstract-full').style.display = 'none'; document.getElementById('2101.02221v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 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">Replaced with version accepted to ApJ. 17 pages, including detailed Appendix on the Tip of the Red Giant Branch calibration; have added an additional peculiar velocity model to the analysis</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2021ApJ...911...65B </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.15275">arXiv:2007.15275</a> <span> [<a href="https://arxiv.org/pdf/2007.15275">pdf</a>, <a href="https://arxiv.org/format/2007.15275">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4365/abad91">10.3847/1538-4365/abad91 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Next Generation Virgo Cluster Survey. XXXIV. Ultra-Compact Dwarf (UCD) Galaxies in the Virgo Cluster </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Liu%2C+C">Chengze Liu</a>, <a href="/search/astro-ph?searchtype=author&query=C%C3%B4t%C3%A9%2C+P">Patrick C么t茅</a>, <a href="/search/astro-ph?searchtype=author&query=Peng%2C+E+W">Eric W. Peng</a>, <a href="/search/astro-ph?searchtype=author&query=Roediger%2C+J">Joel Roediger</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+H">Hongxin Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrarese%2C+L">Laura Ferrarese</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">Rub茅n S谩nchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Guhathakurta%2C+P">Puragra Guhathakurta</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+X">Xiaohu Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Jing%2C+Y">Yipeng Jing</a>, <a href="/search/astro-ph?searchtype=author&query=Alamo-Martinez%2C+K">Karla Alamo-Martinez</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Boselli%2C+A">Alessandro Boselli</a>, <a href="/search/astro-ph?searchtype=author&query=Cuilandre%2C+J">Jean-Charles Cuilandre</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P">Pierre-Alain Duc</a>, <a href="/search/astro-ph?searchtype=author&query=Durrell%2C+P">Patrick Durrell</a>, <a href="/search/astro-ph?searchtype=author&query=Gwyn%2C+S">Stephen Gwyn</a>, <a href="/search/astro-ph?searchtype=author&query=Jord%C3%A1n%2C+A">Andres Jord谩n</a>, <a href="/search/astro-ph?searchtype=author&query=Ko%2C+Y">Youkyung Ko</a>, <a href="/search/astro-ph?searchtype=author&query=Lan%C3%A7on%2C+A">Ariane Lan莽on</a>, <a href="/search/astro-ph?searchtype=author&query=Lim%2C+S">Sungsoon Lim</a>, <a href="/search/astro-ph?searchtype=author&query=Longobardi%2C+A">Alessia Longobardi</a>, <a href="/search/astro-ph?searchtype=author&query=Mei%2C+S">Simona Mei</a>, <a href="/search/astro-ph?searchtype=author&query=Mihos%2C+J+C">J. Christopher Mihos</a>, <a href="/search/astro-ph?searchtype=author&query=Munoz%2C+R">Roberto Munoz</a> , et al. (4 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2007.15275v1-abstract-short" style="display: inline;"> We present a study of ultra compact dwarf (UCD) galaxies in the Virgo cluster based mainly on imaging from the Next Generation Virgo Cluster Survey (NGVS). Using $\sim$100 deg$^{2}$ of $u^*giz$ imaging, we have identified more than 600 candidate UCDs, from the core of Virgo out to its virial radius. Candidates have been selected through a combination of magnitudes, ellipticities, colors, surface b… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.15275v1-abstract-full').style.display = 'inline'; document.getElementById('2007.15275v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.15275v1-abstract-full" style="display: none;"> We present a study of ultra compact dwarf (UCD) galaxies in the Virgo cluster based mainly on imaging from the Next Generation Virgo Cluster Survey (NGVS). Using $\sim$100 deg$^{2}$ of $u^*giz$ imaging, we have identified more than 600 candidate UCDs, from the core of Virgo out to its virial radius. Candidates have been selected through a combination of magnitudes, ellipticities, colors, surface brightnesses, half-light radii and, when available, radial velocities. Candidates were also visually validated from deep NGVS images. Subsamples of varying completeness and purity have been defined to explore the properties of UCDs and compare to those of globular clusters and the nuclei of dwarf galaxies with the aim of delineating the nature and origins of UCDs. From a surface density map, we find the UCDs to be mostly concentrated within Virgo's main subclusters, around its brightest galaxies. We identify several subsamples of UCDs -- i.e., the brightest, largest, and those with the most pronounced and/or asymmetric envelopes -- that could hold clues to the origin of UCDs and possible evolutionary links with dwarf nuclei. We find some evidence for such a connection from the existence of diffuse envelopes around some UCDs, and comparisons of radial distributions of UCDs and nucleated galaxies within the cluster. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.15275v1-abstract-full').style.display = 'none'; document.getElementById('2007.15275v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">70 pages, 24 figures, 6 tables, accepted for publication in ApJS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2001.11046">arXiv:2001.11046</a> <span> [<a href="https://arxiv.org/pdf/2001.11046">pdf</a>, <a href="https://arxiv.org/format/2001.11046">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/ab7016">10.3847/1538-4357/ab7016 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MASSIVE Survey XIV -- Stellar Velocity Profiles and Kinematic Misalignments from 200 pc to 20 kpc in Massive Early-type Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ene%2C+I">Irina Ene</a>, <a href="/search/astro-ph?searchtype=author&query=Ma%2C+C">Chung-Pei Ma</a>, <a href="/search/astro-ph?searchtype=author&query=Walsh%2C+J+L">Jonelle L. Walsh</a>, <a href="/search/astro-ph?searchtype=author&query=Greene%2C+J+E">Jenny E. Greene</a>, <a href="/search/astro-ph?searchtype=author&query=Thomas%2C+J">Jens Thomas</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2001.11046v1-abstract-short" style="display: inline;"> We use high spatial resolution stellar velocity maps from the Gemini GMOS integral-field spectrograph (IFS) and wide-field velocity maps from the McDonald Mitchell IFS to study the stellar velocity profiles and kinematic misalignments from $\sim 200$ pc to $\sim 20$ kpc in 20 early-type galaxies with stellar mass $M_* > 10^{11.7} M_\odot$ in the MASSIVE survey. While 80% of the galaxies have low s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.11046v1-abstract-full').style.display = 'inline'; document.getElementById('2001.11046v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2001.11046v1-abstract-full" style="display: none;"> We use high spatial resolution stellar velocity maps from the Gemini GMOS integral-field spectrograph (IFS) and wide-field velocity maps from the McDonald Mitchell IFS to study the stellar velocity profiles and kinematic misalignments from $\sim 200$ pc to $\sim 20$ kpc in 20 early-type galaxies with stellar mass $M_* > 10^{11.7} M_\odot$ in the MASSIVE survey. While 80% of the galaxies have low spins ($位< 0.1$) and low rotational velocities ($< 50$ km/s) in both the central region and the main body, we find a diverse range of velocity features and misalignment angles. For the 18 galaxies with measurable central kinematic axes, 10 have well aligned kinematic axis and photometric major axis, and the other 8 galaxies have misalignment angles that are distributed quite evenly from $15^\circ$ to the maximal value of $90^\circ$. There is a strong correlation between central kinematic misalignment and galaxy spin, where all 4 galaxies with significant spins have well aligned kinematic and photometric axes, but only 43% of the low-spin galaxies are well aligned. The central and main-body kinematic axes within a galaxy are not always aligned. When the two kinematic axes are aligned ($\sim 60$% of the cases), they are either also aligned with the photometric major axis or orthogonal to it. We find 13 galaxies to also exhibit noticeable local kinematic twists, and one galaxy to have a counter-rotating core. A diverse assembly history consisting of multiple gas-poor mergers of a variety of progenitor mass ratios and orbits is likely to be needed to account for the predominance of low spins and the wide range of central and main-body velocity features reported here for local massive ETGs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.11046v1-abstract-full').style.display = 'none'; document.getElementById('2001.11046v1-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 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in The Astrophysical Journal. 15 pages, 7 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/2001.08753">arXiv:2001.08753</a> <span> [<a href="https://arxiv.org/pdf/2001.08753">pdf</a>, <a href="https://arxiv.org/format/2001.08753">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/ab6f71">10.3847/1538-4357/ab6f71 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MASSIVE Survey -- XV. A Stellar Dynamical Mass Measurement of the Supermassive Black Hole in Massive Elliptical Galaxy NGC 1453 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Liepold%2C+C+M">Christopher M. Liepold</a>, <a href="/search/astro-ph?searchtype=author&query=Quenneville%2C+M+E">Matthew E. Quenneville</a>, <a href="/search/astro-ph?searchtype=author&query=Ma%2C+C">Chung-Pei Ma</a>, <a href="/search/astro-ph?searchtype=author&query=Walsh%2C+J+L">Jonelle L. Walsh</a>, <a href="/search/astro-ph?searchtype=author&query=McConnell%2C+N+J">Nicholas J. McConnell</a>, <a href="/search/astro-ph?searchtype=author&query=Greene%2C+J+E">Jenny E. Greene</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2001.08753v2-abstract-short" style="display: inline;"> We present a new stellar dynamical mass measurement ($M_\mathrm{BH}$) of the supermassive black hole (SMBH) in NGC 1453, a fast-rotating massive elliptical galaxy in the MASSIVE survey. We measure stellar kinematics in 135 spatial bins in the central 1.5 kpc by 2 kpc region of the galaxy using high signal-to-noise ($S/N \sim 130$) spectra from the Gemini-North GMOS integral-field spectrograph (IFS… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.08753v2-abstract-full').style.display = 'inline'; document.getElementById('2001.08753v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2001.08753v2-abstract-full" style="display: none;"> We present a new stellar dynamical mass measurement ($M_\mathrm{BH}$) of the supermassive black hole (SMBH) in NGC 1453, a fast-rotating massive elliptical galaxy in the MASSIVE survey. We measure stellar kinematics in 135 spatial bins in the central 1.5 kpc by 2 kpc region of the galaxy using high signal-to-noise ($S/N \sim 130$) spectra from the Gemini-North GMOS integral-field spectrograph (IFS). Combining with wide-field IFS kinematics out to $\sim 3$ effective radii and stellar light distributions from Hubble Space Telescope (HST) WFC3 images, we perform Schwarzschild orbit-based mass modeling in the axisymmetric limit to constrain the mass components in NGC 1453. The best-fit black hole mass is $M_\mathrm{BH} =(2.9 \pm 0.4) 10^9 M_\odot$; the mass models without a central black hole are excluded at the $8.7蟽$ level. The NGC 1453 black hole lies within the intrinsic scatter of the SMBH and galaxy scaling relations, unlike three other galaxies hosting $\gtrsim 10^{10} M_\odot$ SMBHs in the MASSIVE sample. The high-$S/N$ GMOS spectra enable us to determine 8 moments of the Gauss-Hermite expansion of the line-of-sight velocity distributions (LOSVDs), which are used as constraints in the orbit modeling. The stellar orbits in the mass models are further constrained to produce negligible $h_9$ through $h_{12}$ to minimize spurious behavior in the LOSVDs. We show that truncating the series at $h_4$, as was often done in prior work, leads to a much weaker constraint on the inferred $M_\mathrm{BH}$ for NGC 1453. Furthermore, we discuss precautions and modifications that are needed to achieve axisymmetry in triaxial orbit codes that use the Schwarzschild method to sample the start space of stellar orbits in triaxial gravitational potentials. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.08753v2-abstract-full').style.display = 'none'; document.getElementById('2001.08753v2-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 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in The Astrophysical Journal. 22 pages, 12 figures; References updated</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1909.09196">arXiv:1909.09196</a> <span> [<a href="https://arxiv.org/pdf/1909.09196">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Strategic Scientific Plan for Gemini Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">J. P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Adamson%2C+A">A. Adamson</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+C">C. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%ADaz%2C+R">R. D铆az</a>, <a href="/search/astro-ph?searchtype=author&query=Miller%2C+B">B. Miller</a>, <a href="/search/astro-ph?searchtype=author&query=Peck%2C+A">A. Peck</a>, <a href="/search/astro-ph?searchtype=author&query=Rutten%2C+R">R. Rutten</a>, <a href="/search/astro-ph?searchtype=author&query=Sivo%2C+G">G. Sivo</a>, <a href="/search/astro-ph?searchtype=author&query=Thomas-Osip%2C+J">J. Thomas-Osip</a>, <a href="/search/astro-ph?searchtype=author&query=Boroson%2C+T">T. Boroson</a>, <a href="/search/astro-ph?searchtype=author&query=Carrasco%2C+R">R. Carrasco</a>, <a href="/search/astro-ph?searchtype=author&query=Dennihy%2C+E">E. Dennihy</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%ADaz%2C+M">M. D铆az</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrarese%2C+L">L. Ferrarese</a>, <a href="/search/astro-ph?searchtype=author&query=Green%2C+R">R. Green</a>, <a href="/search/astro-ph?searchtype=author&query=Hirst%2C+P">P. Hirst</a>, <a href="/search/astro-ph?searchtype=author&query=Hwang%2C+N">N. Hwang</a>, <a href="/search/astro-ph?searchtype=author&query=J%C3%B8rgensen%2C+I">I. J酶rgensen</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+H">H. Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kleinman%2C+S">S. Kleinman</a>, <a href="/search/astro-ph?searchtype=author&query=Labrie%2C+K">K. Labrie</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+T">T. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lotz%2C+J">J. Lotz</a>, <a href="/search/astro-ph?searchtype=author&query=Leggett%2C+S">S. Leggett</a>, <a href="/search/astro-ph?searchtype=author&query=Medina%2C+L">L. Medina</a> , et al. (8 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1909.09196v1-abstract-short" style="display: inline;"> We present the Strategic Scientific Plan (SSP) for the direction and activities of the Gemini Observatory in the 2020s. The overarching goal is to ensure that Gemini best uses the available resources to serve the needs of its international user community throughout the coming decade. The actionable items fall into three general categories: (1) preserving Gemini's current facilities and strengths;… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.09196v1-abstract-full').style.display = 'inline'; document.getElementById('1909.09196v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1909.09196v1-abstract-full" style="display: none;"> We present the Strategic Scientific Plan (SSP) for the direction and activities of the Gemini Observatory in the 2020s. The overarching goal is to ensure that Gemini best uses the available resources to serve the needs of its international user community throughout the coming decade. The actionable items fall into three general categories: (1) preserving Gemini's current facilities and strengths; (2) developing instrumentation and software systems, including data pipelines, to enable new scientific capabilities that build on those strengths; (3) strategizing how visiting instruments can deliver additional valuable capabilities. We provide a high-level timeline (schematically illustrated in one figure) for the main developments discussed in this SSP. The schedule is ambitious, but in light of the recent Gemini in the Era of Multi-Messenger Astronomy (GEMMA) award from the NSF, the plan becomes achievable. Lists of milestones are given for gauging progress. As these milestones are reached and new instruments become available, some current instruments will need to be retired; we make recommendations in this regard. The final section concludes by reemphasizing the importance of a strong partnership committed to the needs of all members. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.09196v1-abstract-full').style.display = 'none'; document.getElementById('1909.09196v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Basic version with minimal illustration, 30 pages with 4 figures. For richly illustrated versions with the same textual content, see: http://www.gemini.edu/news/gemini-strategic-scientific-plan</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1904.08929">arXiv:1904.08929</a> <span> [<a href="https://arxiv.org/pdf/1904.08929">pdf</a>, <a href="https://arxiv.org/format/1904.08929">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/ab1f04">10.3847/1538-4357/ab1f04 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MASSIVE Survey XIII -- Spatially Resolved Stellar Kinematics in the Central 1 kpc of 20 Massive Elliptical Galaxies with the GMOS-North Integral-Field Spectrograph </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ene%2C+I">Irina Ene</a>, <a href="/search/astro-ph?searchtype=author&query=Ma%2C+C">Chung-Pei Ma</a>, <a href="/search/astro-ph?searchtype=author&query=McConnell%2C+N+J">Nicholas J. McConnell</a>, <a href="/search/astro-ph?searchtype=author&query=Walsh%2C+J+L">Jonelle L. Walsh</a>, <a href="/search/astro-ph?searchtype=author&query=Kempski%2C+P">Philipp Kempski</a>, <a href="/search/astro-ph?searchtype=author&query=Greene%2C+J+E">Jenny E. Greene</a>, <a href="/search/astro-ph?searchtype=author&query=Thomas%2C+J">Jens Thomas</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1904.08929v2-abstract-short" style="display: inline;"> We use observations from the GEMINI-N/GMOS integral-field spectrograph (IFS) to obtain spatially resolved stellar kinematics of the central $\sim 1$ kpc of 20 early-type galaxies (ETGs) with stellar masses greater than $10^{11.7} M_\odot$ in the MASSIVE survey. Together with observations from the wide-field Mitchell IFS at McDonald Observatory in our earlier work, we obtain unprecedentedly detaile… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.08929v2-abstract-full').style.display = 'inline'; document.getElementById('1904.08929v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1904.08929v2-abstract-full" style="display: none;"> We use observations from the GEMINI-N/GMOS integral-field spectrograph (IFS) to obtain spatially resolved stellar kinematics of the central $\sim 1$ kpc of 20 early-type galaxies (ETGs) with stellar masses greater than $10^{11.7} M_\odot$ in the MASSIVE survey. Together with observations from the wide-field Mitchell IFS at McDonald Observatory in our earlier work, we obtain unprecedentedly detailed kinematic maps of local massive ETGs, covering a scale of $\sim 0.1-30$ kpc. The high ($\sim 120$) signal-to-noise of the GMOS spectra enable us to obtain two-dimensional maps of the line-of-sight velocity, velocity dispersion $蟽$, as well as the skewness $h_3$ and kurtosis $h_4$ of the stellar velocity distributions. All but one galaxy in the sample have $蟽(R)$ profiles that increase towards the center, whereas the slope of $蟽(R)$ at one effective radius ($R_e$) can be of either sign. The $h_4$ is generally positive, with 14 of the 20 galaxies having positive $h_4$ within the GMOS aperture and 18 having positive $h_4$ within $1 R_e$. The positive $h_4$ and rising $蟽(R)$ towards small radii are indicative of a central black hole and velocity anisotropy. We demonstrate the constraining power of the data on the mass distributions in ETGs by applying Jeans anisotropic modeling (JAM) to NGC~1453, the most regular fast rotator in the sample. Despite the limitations of JAM, we obtain a clear $蠂^2$ minimum in black hole mass, stellar mass-to-light ratio, velocity anisotropy parameters, and the circular velocity of the dark matter halo. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.08929v2-abstract-full').style.display = 'none'; document.getElementById('1904.08929v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 May, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1904.06909">arXiv:1904.06909</a> <span> [<a href="https://arxiv.org/pdf/1904.06909">pdf</a>, <a href="https://arxiv.org/ps/1904.06909">ps</a>, <a href="https://arxiv.org/format/1904.06909">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/ab12d9">10.3847/1538-4357/ab12d9 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The ACS Fornax Cluster Survey. III. Globular Cluster Specific Frequencies of Early-Type Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Yiqing Liu</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=Jord%C3%A1n%2C+A">Andr茅s Jord谩n</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=C%C3%B4t%C3%A9%2C+P">Patrick C么t茅</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrarese%2C+L">Laura Ferrarese</a>, <a href="/search/astro-ph?searchtype=author&query=Puzia%2C+T+H">Thomas H. Puzia</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1904.06909v1-abstract-short" style="display: inline;"> The globular cluster (GC) specific frequency ($S_N$), defined as the number of GCs per unit galactic luminosity, represents the efficiency of GC formation (and survival) compared to field stars. Despite the naive expectation that star cluster formation should scale directly with star formation, this efficiency varies widely across galaxies. To explore this variation we measure the z-band GC specif… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.06909v1-abstract-full').style.display = 'inline'; document.getElementById('1904.06909v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1904.06909v1-abstract-full" style="display: none;"> The globular cluster (GC) specific frequency ($S_N$), defined as the number of GCs per unit galactic luminosity, represents the efficiency of GC formation (and survival) compared to field stars. Despite the naive expectation that star cluster formation should scale directly with star formation, this efficiency varies widely across galaxies. To explore this variation we measure the z-band GC specific frequency ($S_{N,z}$) for 43 early-type galaxies (ETGs) from the Hubble Space Telescope (HST)/Advanced Camera for Surveys (ACS) Fornax Cluster Survey. Combined with the homogenous measurements of $S_{N,z}$ in 100 ETGs from the HST/ACS Virgo Cluster Survey from Peng et al. (2008), we investigate the dependence of $S_{N,z}$ on mass and environment over a range of galaxy properties. We find that $S_{N,z}$ behaves similarly in the two galaxy clusters, despite the clusters' order-of-magnitude difference in mass density. The $S_{N,z}$ is low in intermediate-mass ETGs ($-20<M_z<-23$), and increases with galaxy luminosity. It is elevated at low masses, on average, but with a large scatter driven by galaxies in dense environments. The densest environments with the strongest tidal forces appear to strip the GC systems of low-mass galaxies. However, in low-mass galaxies that are not in strong tidal fields, denser environments correlate with enhanced GC formation efficiencies. Normalizing by inferred halo masses, the GC mass fraction, $畏=(3.36\pm0.2)\times10^{-5}$, is constant for ETGs with stellar masses $\mathcal{M}_\star \lesssim 3\times10^{10}M_\odot$, in agreement with previous studies. The lack of correlation between the fraction of GCs and the nuclear light implies only a weak link between the infall of GCs and the formation of nuclei. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.06909v1-abstract-full').style.display = 'none'; document.getElementById('1904.06909v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 7 figures, 6 tables; accepted by ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1903.08884">arXiv:1903.08884</a> <span> [<a href="https://arxiv.org/pdf/1903.08884">pdf</a>, <a href="https://arxiv.org/format/1903.08884">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/stz871">10.1093/mnras/stz871 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MASSIVE survey - XI. What drives the molecular gas properties of early-type galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+A">Timothy A. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Greene%2C+J+E">Jenny E. Greene</a>, <a href="/search/astro-ph?searchtype=author&query=Ma%2C+C">Chung-Pei Ma</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Dawson%2C+J+M">James M. Dawson</a>, <a href="/search/astro-ph?searchtype=author&query=Pandya%2C+V">Viraj Pandya</a>, <a href="/search/astro-ph?searchtype=author&query=Veale%2C+M">Melanie Veale</a>, <a href="/search/astro-ph?searchtype=author&query=Zabel%2C+N">Nikki Zabel</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="1903.08884v1-abstract-short" style="display: inline;"> In this paper we study the molecular gas content of a representative sample of 67 of the most massive early-type galaxies in the local universe, drawn uniformly from the MASSIVE survey. We present new IRAM-30m telescope observations of 30 of these galaxies, allowing us to probe the molecular gas content of the entire sample to a fixed molecular-to-stellar mass fraction of 0.1%. The total detection… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.08884v1-abstract-full').style.display = 'inline'; document.getElementById('1903.08884v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1903.08884v1-abstract-full" style="display: none;"> In this paper we study the molecular gas content of a representative sample of 67 of the most massive early-type galaxies in the local universe, drawn uniformly from the MASSIVE survey. We present new IRAM-30m telescope observations of 30 of these galaxies, allowing us to probe the molecular gas content of the entire sample to a fixed molecular-to-stellar mass fraction of 0.1%. The total detection rate in this representative sample is 25$^{+5.9}_{-4.4}$%, and by combining the MASSIVE and ATLAS$^{\rm 3D}$ molecular gas surveys we find a joint detection rate of 22.4$^{+2.4}_{-2.1}$%. This detection rate seems to be independent of galaxy mass, size, position on the fundamental plane, and local environment. We show here for the first time that true slow rotators can host molecular gas reservoirs, but the rate at which they do so is significantly lower than for fast-rotators. Objects with a higher velocity dispersion at fixed mass (a higher kinematic bulge fraction) are less likely to have detectable molecular gas, and where gas does exist, have lower molecular gas fractions. In addition, satellite galaxies in dense environments have $\approx$0.6 dex lower molecular gas-to-stellar mass ratios than isolated objects. In order to interpret these results we created a toy model, which we use to constrain the origin of the gas in these systems. We are able to derive an independent estimate of the gas-rich merger rate in the low-redshift universe. These gas rich mergers appear to dominate the supply of gas to ETGs, but stellar mass loss, hot halo cooling and transformation of spiral galaxies also play a secondary role. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.08884v1-abstract-full').style.display = 'none'; document.getElementById('1903.08884v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 March, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">19 pages, 12 figures, accepted by MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1903.08184">arXiv:1903.08184</a> <span> [<a href="https://arxiv.org/pdf/1903.08184">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Probing the Time Domain with High Spatial Resolution </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">J. P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Rodney%2C+S+A">S. A. Rodney</a>, <a href="/search/astro-ph?searchtype=author&query=Lotz%2C+J+M">J. M. Lotz</a>, <a href="/search/astro-ph?searchtype=author&query=Sivo%2C+G">G. Sivo</a>, <a href="/search/astro-ph?searchtype=author&query=Sivanandam%2C+S">S. Sivanandam</a>, <a href="/search/astro-ph?searchtype=author&query=Andersen%2C+M">M. Andersen</a>, <a href="/search/astro-ph?searchtype=author&query=Carrasco%2C+R">R. Carrasco</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrarese%2C+L">L. Ferrarese</a>, <a href="/search/astro-ph?searchtype=author&query=Foley%2C+R+J">R. J. Foley</a>, <a href="/search/astro-ph?searchtype=author&query=Goodsell%2C+S">S. Goodsell</a>, <a href="/search/astro-ph?searchtype=author&query=Hirst%2C+P">P. Hirst</a>, <a href="/search/astro-ph?searchtype=author&query=Jensen%2C+J+B">J. B. Jensen</a>, <a href="/search/astro-ph?searchtype=author&query=Kelly%2C+P+L">P. L. Kelly</a>, <a href="/search/astro-ph?searchtype=author&query=Kaurov%2C+A+A">A. A. Kaurov</a>, <a href="/search/astro-ph?searchtype=author&query=Lemoine-Busserolle%2C+M">M. Lemoine-Busserolle</a>, <a href="/search/astro-ph?searchtype=author&query=Miller%2C+B+W">B. W. Miller</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Meara%2C+J">J. O'Meara</a>, <a href="/search/astro-ph?searchtype=author&query=Roe%2C+H">H. Roe</a>, <a href="/search/astro-ph?searchtype=author&query=Schwamb%2C+M+E">M. E. Schwamb</a>, <a href="/search/astro-ph?searchtype=author&query=Scharw%C3%A4chter%2C+J">J. Scharw盲chter</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="1903.08184v1-abstract-short" style="display: inline;"> Two groundbreaking new facilities will commence operations early in the 2020s and thereafter define much of the broad landscape of US optical-infrared astronomy in the remaining decade. The Large Synoptic Survey Telescope (LSST), perched atop Cerro Pachon in the Chilean Andes, will revolutionize the young field of Time Domain Astronomy through its wide-field, multi-band optical imaging survey. At… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.08184v1-abstract-full').style.display = 'inline'; document.getElementById('1903.08184v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1903.08184v1-abstract-full" style="display: none;"> Two groundbreaking new facilities will commence operations early in the 2020s and thereafter define much of the broad landscape of US optical-infrared astronomy in the remaining decade. The Large Synoptic Survey Telescope (LSST), perched atop Cerro Pachon in the Chilean Andes, will revolutionize the young field of Time Domain Astronomy through its wide-field, multi-band optical imaging survey. At the same time, the James Webb Space Telescope (JWST), orbiting at the Sun-Earth L2 Lagrange point, will provide stunningly high-resolution views of selected targets from the red end of the optical spectrum to the mid-infrared. However, the spatial resolution of the LSST observations will be limited by atmospheric seeing, while JWST will be limited in its time-domain capabilities. This paper highlights the scientific opportunities lying between these two landmark missions, i.e., science enabled by systems capable of astronomical observations with both high cadence in the time domain and high resolution in the spatial domain. The opportunities range from constraining the late phases of stellar evolution in nearby resolved populations to constraining dark matter distributions and cosmology using lensed transient sources. We describe a system that can deliver the required capabilities. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.08184v1-abstract-full').style.display = 'none'; document.getElementById('1903.08184v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 March, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">Science white paper submitted to Astro2020</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1903.04553">arXiv:1903.04553</a> <span> [<a href="https://arxiv.org/pdf/1903.04553">pdf</a>, <a href="https://arxiv.org/ps/1903.04553">ps</a>, <a href="https://arxiv.org/format/1903.04553">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Gravity and Light: Combining Gravitational Wave and Electromagnetic Observations in the 2020s </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Foley%2C+R+J">R. J. Foley</a>, <a href="/search/astro-ph?searchtype=author&query=Alexander%2C+K+D">K. D. Alexander</a>, <a href="/search/astro-ph?searchtype=author&query=Andreoni%2C+I">I. Andreoni</a>, <a href="/search/astro-ph?searchtype=author&query=Arcavi%2C+I">I. Arcavi</a>, <a href="/search/astro-ph?searchtype=author&query=Auchettl%2C+K">K. Auchettl</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+J">J. Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Baym%2C+G">G. Baym</a>, <a href="/search/astro-ph?searchtype=author&query=Bellm%2C+E+C">E. C. Bellm</a>, <a href="/search/astro-ph?searchtype=author&query=Beloborodov%2C+A+M">A. M. Beloborodov</a>, <a href="/search/astro-ph?searchtype=author&query=Blagorodnova%2C+N">N. Blagorodnova</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">J. P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Brady%2C+P+R">P. R. Brady</a>, <a href="/search/astro-ph?searchtype=author&query=Branchesi%2C+M">M. Branchesi</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+J+S">J. S. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Butler%2C+N">N. Butler</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">M. Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Chornock%2C+R">R. Chornock</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+D+O">D. O. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Cooke%2C+J">J. Cooke</a>, <a href="/search/astro-ph?searchtype=author&query=Coppejans%2C+D+L">D. L. Coppejans</a>, <a href="/search/astro-ph?searchtype=author&query=Corsi%2C+A">A. Corsi</a>, <a href="/search/astro-ph?searchtype=author&query=Couch%2C+S+M">S. M. Couch</a>, <a href="/search/astro-ph?searchtype=author&query=Coughlin%2C+M+W">M. W. Coughlin</a>, <a href="/search/astro-ph?searchtype=author&query=Coulter%2C+D+A">D. A. Coulter</a>, <a href="/search/astro-ph?searchtype=author&query=Cowperthwaite%2C+P+S">P. S. Cowperthwaite</a> , et al. (88 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="1903.04553v1-abstract-short" style="display: inline;"> As of today, we have directly detected exactly one source in both gravitational waves (GWs) and electromagnetic (EM) radiation, the binary neutron star merger GW170817, its associated gamma-ray burst GRB170817A, and the subsequent kilonova SSS17a/AT 2017gfo. Within ten years, we will detect hundreds of events, including new classes of events such as neutron-star-black-hole mergers, core-collapse s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.04553v1-abstract-full').style.display = 'inline'; document.getElementById('1903.04553v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1903.04553v1-abstract-full" style="display: none;"> As of today, we have directly detected exactly one source in both gravitational waves (GWs) and electromagnetic (EM) radiation, the binary neutron star merger GW170817, its associated gamma-ray burst GRB170817A, and the subsequent kilonova SSS17a/AT 2017gfo. Within ten years, we will detect hundreds of events, including new classes of events such as neutron-star-black-hole mergers, core-collapse supernovae, and almost certainly something completely unexpected. As we build this sample, we will explore exotic astrophysical topics ranging from nucleosynthesis, stellar evolution, general relativity, high-energy astrophysics, nuclear matter, to cosmology. The discovery potential is extraordinary, and investments in this area will yield major scientific breakthroughs. Here we outline some of the most exciting scientific questions that can be answered by combining GW and EM observations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.04553v1-abstract-full').style.display = 'none'; document.getElementById('1903.04553v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 March, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">submitted to Astro2020</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1901.01271">arXiv:1901.01271</a> <span> [<a href="https://arxiv.org/pdf/1901.01271">pdf</a>, <a href="https://arxiv.org/format/1901.01271">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/ab01e3">10.3847/1538-4357/ab01e3 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MASSIVE Survey - XII Connecting Stellar Populations of Early-Type Galaxies to Kinematics and Environment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Greene%2C+J+E">Jenny E Greene</a>, <a href="/search/astro-ph?searchtype=author&query=Veale%2C+M">Melanie Veale</a>, <a href="/search/astro-ph?searchtype=author&query=Ma%2C+C">Chung-Pei Ma</a>, <a href="/search/astro-ph?searchtype=author&query=Thomas%2C+J">Jens Thomas</a>, <a href="/search/astro-ph?searchtype=author&query=Quenneville%2C+M+E">Matthew E. Quenneville</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Walsh%2C+J+L">Jonelle L. Walsh</a>, <a href="/search/astro-ph?searchtype=author&query=Goulding%2C+A">Andrew Goulding</a>, <a href="/search/astro-ph?searchtype=author&query=Ito%2C+J">Jennifer Ito</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1901.01271v1-abstract-short" style="display: inline;"> We measure the stellar populations as a function of radius for 90 early-type galaxies (ETGs) in the MASSIVE survey, a volume-limited integral-field spectroscopic (IFS) galaxy survey targeting all northern-sky ETGs with absolute K-band magnitude M_K < -25.3 mag, or stellar mass M* 4x10^11 M_sun, within 108 Mpc. We are able to measure reliable stellar population parameters for individual galaxies ou… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.01271v1-abstract-full').style.display = 'inline'; document.getElementById('1901.01271v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1901.01271v1-abstract-full" style="display: none;"> We measure the stellar populations as a function of radius for 90 early-type galaxies (ETGs) in the MASSIVE survey, a volume-limited integral-field spectroscopic (IFS) galaxy survey targeting all northern-sky ETGs with absolute K-band magnitude M_K < -25.3 mag, or stellar mass M* 4x10^11 M_sun, within 108 Mpc. We are able to measure reliable stellar population parameters for individual galaxies out to 10-20 kpc (1-3 R_e) depending on the galaxy. Focusing on ~R_e (~10 kpc), we find significant correlations between the abundance ratios, sigma, and M* at large radius, but we also find that the abundance ratios saturate in the highest-mass bin. We see a strong correlation between the kurtosis of the line of sight velocity distribution (h4) and the stellar population parameters beyond R_e. Galaxies with higher radial anisotropy appear to be older, with metal-poorer stars and enhanced [alpha/Fe]. We suggest that the higher radial anisotropy may derive from more accretion of small satellites. Finally, we see some evidence for correlations between environmental metrics (measured locally and on >5 Mpc scales) and the stellar populations, as expected if satellites are quenched earlier in denser environments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.01271v1-abstract-full').style.display = 'none'; document.getElementById('1901.01271v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 January, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 7 figures, Appendix not included here due to size constraints. Posted after responding to referee's comments</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1812.01019">arXiv:1812.01019</a> <span> [<a href="https://arxiv.org/pdf/1812.01019">pdf</a>, <a href="https://arxiv.org/format/1812.01019">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/aaf4fd">10.3847/1538-4357/aaf4fd <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Next Generation Virgo Cluster Survey. XXIII. Fundamentals of nuclear star clusters over seven decades in galaxy mass </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=C%C3%B4t%C3%A9%2C+P">P. C么t茅</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrarese%2C+L">L. Ferrarese</a>, <a href="/search/astro-ph?searchtype=author&query=Peng%2C+E+W">E. W. Peng</a>, <a href="/search/astro-ph?searchtype=author&query=Roediger%2C+J">J. Roediger</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">J. P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Emsellem%2C+E">E. Emsellem</a>, <a href="/search/astro-ph?searchtype=author&query=Puzia%2C+T+H">T. H. Puzia</a>, <a href="/search/astro-ph?searchtype=author&query=Spengler%2C+C">C. Spengler</a>, <a href="/search/astro-ph?searchtype=author&query=Taylor%2C+J">J. Taylor</a>, <a href="/search/astro-ph?searchtype=author&query=%C3%81lamo-Mart%C3%ADnez%2C+K+A">K. A. 脕lamo-Mart铆nez</a>, <a href="/search/astro-ph?searchtype=author&query=Boselli%2C+A">A. Boselli</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">M. Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Cuillandre%2C+J+-">J. -C. Cuillandre</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P+-">P. -A. Duc</a>, <a href="/search/astro-ph?searchtype=author&query=Durrell%2C+P">P. Durrell</a>, <a href="/search/astro-ph?searchtype=author&query=Gwyn%2C+S">S. Gwyn</a>, <a href="/search/astro-ph?searchtype=author&query=MacArthur%2C+L+A">L. A. MacArthur</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=Lim%2C+S">S. Lim</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+C">C. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Mei%2C+S">S. Mei</a>, <a href="/search/astro-ph?searchtype=author&query=Miller%2C+B">B. Miller</a>, <a href="/search/astro-ph?searchtype=author&query=Mu%C3%B1oz%2C+R">R. Mu帽oz</a>, <a href="/search/astro-ph?searchtype=author&query=Mihos%2C+J+C">J. C. Mihos</a> , et al. (3 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1812.01019v1-abstract-short" style="display: inline;"> Using deep, high resolution optical imaging from the Next Generation Virgo Cluster Survey we study the properties of nuclear star clusters (NSCs) in a sample of nearly 400 quiescent galaxies in the core of Virgo with stellar masses $10^{5}\lesssim M_{*}/M_{\odot} \lesssim10^{12}$. The nucleation fraction reaches a peak value $f_{n}\approx90\%$ for $M_{*} \approx 10^{9} M_{\odot}$ galaxies and decl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.01019v1-abstract-full').style.display = 'inline'; document.getElementById('1812.01019v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1812.01019v1-abstract-full" style="display: none;"> Using deep, high resolution optical imaging from the Next Generation Virgo Cluster Survey we study the properties of nuclear star clusters (NSCs) in a sample of nearly 400 quiescent galaxies in the core of Virgo with stellar masses $10^{5}\lesssim M_{*}/M_{\odot} \lesssim10^{12}$. The nucleation fraction reaches a peak value $f_{n}\approx90\%$ for $M_{*} \approx 10^{9} M_{\odot}$ galaxies and declines for both higher and lower masses, but nuclei populate galaxies as small as $M_{*} \approx5\times10^{5} M_{\odot}$. Comparison with literature data for nearby groups and clusters shows that at the low-mass end nucleation is more frequent in denser environments. The NSC mass function peaks at $M_{NSC}\approx7\times10^{5} M_{\odot}$, a factor 3-4 times larger than the turnover mass for globular clusters (GCs). We find a nonlinear relation between the stellar masses of NSCs and of their host galaxies, with a mean nucleus-to-galaxy mass ratio that drops to $M_{NSC}/M_{*}\approx3.6\times10^{-3}$ for $M_{*} \approx 5\times10^{9} M_{\odot}$ galaxies. Nuclei in both more and less massive galaxies are much more prominent: $M_{NSC}\propto M_{*}^{0.46}$ at the low-mass end, where nuclei are nearly 50% as massive as their hosts. We measure an intrinsic scatter in NSC masses at fixed galaxy stellar mass of 0.4 dex, which we interpret as evidence that the process of NSC growth is significantly stochastic. At low galaxy masses we find a close connection between NSCs and GC systems, including a very similar occupation distribution and comparable total masses. We discuss these results in the context of current dissipative and dissipationless models of NSC formation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.01019v1-abstract-full').style.display = 'none'; document.getElementById('1812.01019v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 December, 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">ApJ accepted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1808.02176">arXiv:1808.02176</a> <span> [<a href="https://arxiv.org/pdf/1808.02176">pdf</a>, <a href="https://arxiv.org/ps/1808.02176">ps</a>, <a href="https://arxiv.org/format/1808.02176">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"> Independent Analysis of the Distance to NGC1052-DF2 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1808.02176v2-abstract-short" style="display: inline;"> The conclusion that the diffuse galaxy NGC1052-DF2 is deficient in dark matter depends critically on the distance, as noted in the original publication and subsequent works. The results of our preliminary assessment of the SBF distance have already been referenced on the web. Here we present the details of a more careful analysis, supply some context, and comment on the remaining uncertainty. </span> <span class="abstract-full has-text-grey-dark mathjax" id="1808.02176v2-abstract-full" style="display: none;"> The conclusion that the diffuse galaxy NGC1052-DF2 is deficient in dark matter depends critically on the distance, as noted in the original publication and subsequent works. The results of our preliminary assessment of the SBF distance have already been referenced on the web. Here we present the details of a more careful analysis, supply some context, and comment on the remaining uncertainty. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.02176v2-abstract-full').style.display = 'none'; document.getElementById('1808.02176v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 August, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 August, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">2 pages, accepted by Research Notes of the American Astronomical Society; text is a bit laconic because of the RNAAS word limit</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1807.08750">arXiv:1807.08750</a> <span> [<a href="https://arxiv.org/pdf/1807.08750">pdf</a>, <a href="https://arxiv.org/format/1807.08750">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/aad3d2">10.3847/1538-4357/aad3d2 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Next Generation Virgo Cluster Survey (NGVS) XXXI. The kinematics of intra-cluster globular clusters in the core of the Virgo cluster </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Longobardi%2C+A">Alessia Longobardi</a>, <a href="/search/astro-ph?searchtype=author&query=Peng%2C+E+W">Eric W. Peng</a>, <a href="/search/astro-ph?searchtype=author&query=C%C3%B4t%C3%A9%2C+P">Patrick C么t茅</a>, <a href="/search/astro-ph?searchtype=author&query=Mihos%2C+J+C">J. Christopher Mihos</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrarese%2C+L">Laura Ferrarese</a>, <a href="/search/astro-ph?searchtype=author&query=Puzia%2C+T+H">Thomas H. Puzia</a>, <a href="/search/astro-ph?searchtype=author&query=Lan%C3%A7on%2C+A">Ariane Lan莽on</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+H">Hong-Xin Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Mu%C3%B1oz%2C+R+P">Roberto P. Mu帽oz</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Guhathakurta%2C+P">Puragra Guhathakurta</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=S%C3%A1nchez-Janssen%2C+R">R煤ben S谩nchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Toloba%2C+E">Elisa Toloba</a>, <a href="/search/astro-ph?searchtype=author&query=Jord%C3%A1n%2C+A">Andr茅s Jord谩n</a>, <a href="/search/astro-ph?searchtype=author&query=Eyheramendy%2C+S">Susana Eyheramendy</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+D+J">Stephen D. J. Gwyn</a>, <a href="/search/astro-ph?searchtype=author&query=Boselli%2C+A">Alessandro Boselli</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P">Pierre-Alain Duc</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+C">Chengze Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Alamo-Mart%C3%ADnez%2C+K">Karla Alamo-Mart铆nez</a>, <a href="/search/astro-ph?searchtype=author&query=Powalka%2C+M">Mathieu Powalka</a>, <a href="/search/astro-ph?searchtype=author&query=Lim%2C+S">Sungsoon Lim</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1807.08750v1-abstract-short" style="display: inline;"> Intra-cluster (IC) populations are expected to be a natural result of the hierarchical assembly of clusters, yet their low space densities make them difficult to detect and study. We present the first definitive kinematic detection of an IC population of globular clusters (GCs) in the Virgo cluster, around the central galaxy, M87. This study focuses on the Virgo core for which the combination of N… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.08750v1-abstract-full').style.display = 'inline'; document.getElementById('1807.08750v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1807.08750v1-abstract-full" style="display: none;"> Intra-cluster (IC) populations are expected to be a natural result of the hierarchical assembly of clusters, yet their low space densities make them difficult to detect and study. We present the first definitive kinematic detection of an IC population of globular clusters (GCs) in the Virgo cluster, around the central galaxy, M87. This study focuses on the Virgo core for which the combination of NGVS photometry and follow-up spectroscopy allows us to reject foreground star contamination and explore GC kinematics over the full Virgo dynamical range. The GC kinematics changes gradually with galactocentric distance, decreasing in mean velocity and increasing in velocity dispersion, eventually becoming indistinguishable from the kinematics of Virgo dwarf galaxies at $\mathrm{R>320\, kpc}$. By kinematically tagging M87 halo and intra-cluster GCs we find that 1) the M87 halo has a smaller fraction ($52\pm3\%$) of blue clusters with respect to the IC counterpart ($77\pm10\%$), 2) the $(g'-r')_{0}$ vs $(i'-z')_{0}$ color-color diagrams reveal a galaxy population that is redder than the IC population that may be due to a different composition in chemical abundance and progenitor mass, and 3) the ICGC distribution is shallower and more extended than the M87 GCs, yet still centrally concentrated. The ICGC specific frequency, $S_{N,\mathrm{ICL}}=10.2\pm4.8$, is consistent with what is observed for the population of quenched, low-mass galaxies within 1~Mpc from the cluster's center. The IC population at Virgo's center is thus consistent with being an accreted component from low-mass galaxies tidally stripped or disrupted through interactions, with a total mass of $\mathrm{M_{ICL,tot}=10.8\pm0.1\times10^{11}M_{\odot}}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.08750v1-abstract-full').style.display = 'none'; document.getElementById('1807.08750v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 July, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">31 pages, 13 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/1806.05425">arXiv:1806.05425</a> <span> [<a href="https://arxiv.org/pdf/1806.05425">pdf</a>, <a href="https://arxiv.org/ps/1806.05425">ps</a>, <a href="https://arxiv.org/format/1806.05425">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/aacb81">10.3847/1538-4357/aacb81 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Globular Cluster Systems of Ultra-Diffuse Galaxies in the Coma Cluster </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lim%2C+S">Sungsoon Lim</a>, <a href="/search/astro-ph?searchtype=author&query=Peng%2C+E+W">Eric W. Peng</a>, <a href="/search/astro-ph?searchtype=author&query=Cote%2C+P">Patrick Cote</a>, <a href="/search/astro-ph?searchtype=author&query=Sales%2C+L+V">Laura V. Sales</a>, <a href="/search/astro-ph?searchtype=author&query=Brok%2C+M+d">Mark den Brok</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Guhathakurta%2C+P">Puragra Guhathakurta</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1806.05425v1-abstract-short" style="display: inline;"> Ultra-diffuse galaxies (UDGs) are unusual galaxies with low luminosities, similar to classical dwarf galaxies, but sizes up to $\sim\!5$ larger than expected for their mass. Some UDGs have large populations of globular clusters (GCs), something unexpected in galaxies with such low stellar density and mass. We have carried out a comprehensive study of GCs in both UDGs and classical dwarf galaxies a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.05425v1-abstract-full').style.display = 'inline'; document.getElementById('1806.05425v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1806.05425v1-abstract-full" style="display: none;"> Ultra-diffuse galaxies (UDGs) are unusual galaxies with low luminosities, similar to classical dwarf galaxies, but sizes up to $\sim\!5$ larger than expected for their mass. Some UDGs have large populations of globular clusters (GCs), something unexpected in galaxies with such low stellar density and mass. We have carried out a comprehensive study of GCs in both UDGs and classical dwarf galaxies at comparable stellar masses using HST observations of the Coma cluster. We present new imaging for 33 Dragonfly UDGs with the largest effective radii ($>2$ kpc), and additionally include 15 UDGs and 54 classical dwarf galaxies from the HST/ACS Coma Treasury Survey and the literature. Out of a total of 48 UDGs, 27 have statistically significant GC systems, and 11 have candidate nuclear star clusters. The GC specific frequency ($S_N$) varies dramatically, with the mean $S_N$ being higher for UDGs than for classical dwarfs. At constant stellar mass, galaxies with larger sizes (or lower surface brightnesses) have higher $S_N$, with the trend being stronger at higher stellar mass. At lower stellar masses, UDGs tend to have higher $S_N$ when closer to the center of the cluster, i.e., in denser environments. The fraction of UDGs with a nuclear star cluster also depends on environment, varying from $\sim\!40$\% in the cluster core, where it is slightly lower than the nucleation fraction of classical dwarfs, to $\lesssim20\%$ in the outskirts. Collectively, we observe an unmistakable diversity in the abundance of GCs, and this may point to multiple formation routes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.05425v1-abstract-full').style.display = 'none'; document.getElementById('1806.05425v1-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 June, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 10 figures, 2 tables, accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1802.06814">arXiv:1802.06814</a> <span> [<a href="https://arxiv.org/pdf/1802.06814">pdf</a>, <a href="https://arxiv.org/format/1802.06814">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/aaae63">10.3847/1538-4357/aaae63 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Next Generation Virgo Cluster Survey (NGVS). XXXII:~Search for a Globular Cluster Substructure in the Virgo Galaxy Cluster Core </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Powalka%2C+M">Mathieu Powalka</a>, <a href="/search/astro-ph?searchtype=author&query=Puzia%2C+T+H">Thomas H. Puzia</a>, <a href="/search/astro-ph?searchtype=author&query=Lan%C3%A7on%2C+A">Ariane Lan莽on</a>, <a href="/search/astro-ph?searchtype=author&query=Peng%2C+A+L+E+W">Alessia Longobardi Eric W. Peng</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P">Pierre-Alain Duc</a>, <a href="/search/astro-ph?searchtype=author&query=Alamo-Mart%C3%ADnez%2C+K">Karla Alamo-Mart铆nez</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=C%C3%B4t%C3%A9%2C+P">Patrick C么t茅</a>, <a href="/search/astro-ph?searchtype=author&query=Cuillandre%2C+J">Jean-Charles Cuillandre</a>, <a href="/search/astro-ph?searchtype=author&query=Durrell%2C+P">Patrick Durrell</a>, <a href="/search/astro-ph?searchtype=author&query=Eigenthaler%2C+P">Paul Eigenthaler</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrarese%2C+L">Laura Ferrarese</a>, <a href="/search/astro-ph?searchtype=author&query=Guhathakurta%2C+P">Puragra Guhathakurta</a>, <a href="/search/astro-ph?searchtype=author&query=Gwyn%2C+S+D+J">S. D. J. Gwyn</a>, <a href="/search/astro-ph?searchtype=author&query=Hudelot%2C+P">Patrick Hudelot</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+C">Chengze Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Mei%2C+S">Simona Mei</a>, <a href="/search/astro-ph?searchtype=author&query=Mu%C3%B1oz%2C+R+P">Roberto P. Mu帽oz</a>, <a href="/search/astro-ph?searchtype=author&query=Roediger%2C+J">Joel Roediger</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">Rub茅n S谩nchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Toloba%2C+E">Elisa Toloba</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+H">Hongxin Zhang</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1802.06814v1-abstract-short" style="display: inline;"> Substructure in globular cluster (GC) populations around large galaxies is expected in galaxy formation scenarios that involve accretion or merger events, and it has been searched for using direct associations between GCs and structure in the diffuse galaxy light, or with GC kinematics. Here, we present a search for candidate substructures in the GC population around the Virgo cD galaxy M87 throug… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.06814v1-abstract-full').style.display = 'inline'; document.getElementById('1802.06814v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1802.06814v1-abstract-full" style="display: none;"> Substructure in globular cluster (GC) populations around large galaxies is expected in galaxy formation scenarios that involve accretion or merger events, and it has been searched for using direct associations between GCs and structure in the diffuse galaxy light, or with GC kinematics. Here, we present a search for candidate substructures in the GC population around the Virgo cD galaxy M87 through the analysis of the spatial distribution of the GC colors.~The study is based on a sample of $\sim\!1800$ bright GCs with high-quality $u,g,r,i,z,K_s$ photometry, selected to ensure a low contamination by foreground stars or background galaxies.~The spectral energy distributions of the GCs are associated with formal estimates of age and metallicity, which are representative of its position in a 4-D color-space relative to standard single stellar population models.~Dividing the sample into broad bins based on the relative formal ages, we observe inhomogeneities which reveal signatures of GC substructures.~The most significant of these is a spatial overdensity of GCs with relatively young age labels, of diameter $\sim\!0.1$\,deg ($\sim\!30\,$kpc), located to the south of M87.~The significance of this detection is larger than about 5$蟽$ after accounting for estimates of random and systematic errors.~Surprisingly, no large Virgo galaxy is present in this area, that could potentially host these GCs.~But candidate substructures in the M87 halo with equally elusive hosts have been described based on kinematic studies in the past.~The number of GC spectra available around M87 is currently insufficient to clarify the nature of the new candidate substructure. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.06814v1-abstract-full').style.display = 'none'; document.getElementById('1802.06814v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 February, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 6 figures, Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1802.05526">arXiv:1802.05526</a> <span> [<a href="https://arxiv.org/pdf/1802.05526">pdf</a>, <a href="https://arxiv.org/format/1802.05526">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/aab043">10.3847/1538-4357/aab043 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Next Generation Virgo Cluster Survey (NGVS). XVIII. Measurement and Calibration of Surface Brightness Fluctuation Distances for Bright Galaxies in Virgo (and Beyond) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">J. P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrarese%2C+L">L. Ferrarese</a>, <a href="/search/astro-ph?searchtype=author&query=Cote%2C+P">P. Cote</a>, <a href="/search/astro-ph?searchtype=author&query=Roediger%2C+J+C">J. C. Roediger</a>, <a href="/search/astro-ph?searchtype=author&query=Raimondo%2C+G">G. Raimondo</a>, <a href="/search/astro-ph?searchtype=author&query=Peng%2C+E+W">E. W. Peng</a>, <a href="/search/astro-ph?searchtype=author&query=Gwyn%2C+S">S. Gwyn</a>, <a href="/search/astro-ph?searchtype=author&query=Durrell%2C+P+R">P. R. Durrell</a>, <a href="/search/astro-ph?searchtype=author&query=Cuillandre%2C+J+C">J. C. Cuillandre</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1802.05526v1-abstract-short" style="display: inline;"> We describe a program to measure surface brightness fluctuation (SBF) distances to galaxies observed in the Next Generation Virgo Cluster Survey (NGVS), a photometric imaging survey covering $104~deg^2$ of the Virgo cluster in the ${u}^*,g,i,z$ bandpasses with the Canada-France Hawaii Telescope. We describe the selection of the sample galaxies, the procedures for measuring the apparent $i$-band SB… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.05526v1-abstract-full').style.display = 'inline'; document.getElementById('1802.05526v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1802.05526v1-abstract-full" style="display: none;"> We describe a program to measure surface brightness fluctuation (SBF) distances to galaxies observed in the Next Generation Virgo Cluster Survey (NGVS), a photometric imaging survey covering $104~deg^2$ of the Virgo cluster in the ${u}^*,g,i,z$ bandpasses with the Canada-France Hawaii Telescope. We describe the selection of the sample galaxies, the procedures for measuring the apparent $i$-band SBF magnitude $\bar{i}$, and the calibration of the absolute $\bar{M}_i$ as a function of observed stellar population properties. The multi-band NGVS data set provides multiple options for calibrating the SBF distances, and we explore various calibrations involving individual color indices as well as combinations of two different colors. Within the color range of the present sample, the two-color calibrations do not significantly improve the scatter with respect to wide-baseline, single-color calibrations involving $u^{*}$. We adopt the ${u}^*{-}z$ calibration as reference for the present galaxy sample, with an observed scatter of 0.11 mag. For a few cases that lack good ${u}^*$ photometry, we use an alternative relation based on a combination of $g{-}i$ and $g{-}z$ colors, with only a slightly larger observed scatter of 0.12 mag. The agreement of our measurements with the best existing distance estimates provides confidence that our measurements are accurate. We present a preliminary catalog of distances for 89 galaxies brighter than $B_T\approx13.0$ mag within the survey footprint, including members of the background M and W Clouds at roughly twice the distance of the main body of the Virgo cluster. The extension of the present work to fainter and bluer galaxies is in progress. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.05526v1-abstract-full').style.display = 'none'; document.getElementById('1802.05526v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 February, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">ApJ accepted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1802.00014">arXiv:1802.00014</a> <span> [<a href="https://arxiv.org/pdf/1802.00014">pdf</a>, <a href="https://arxiv.org/format/1802.00014">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/sty1649">10.1093/mnras/sty1649 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MASSIVE Survey - X. Misalignment between Kinematic and Photometric Axes and Intrinsic Shapes of Massive Early-Type Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ene%2C+I">Irina Ene</a>, <a href="/search/astro-ph?searchtype=author&query=Ma%2C+C">Chung-Pei Ma</a>, <a href="/search/astro-ph?searchtype=author&query=Veale%2C+M">Melanie Veale</a>, <a href="/search/astro-ph?searchtype=author&query=Greene%2C+J+E">Jenny E. Greene</a>, <a href="/search/astro-ph?searchtype=author&query=Thomas%2C+J">Jens Thomas</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Foster%2C+C">Caroline Foster</a>, <a href="/search/astro-ph?searchtype=author&query=Walsh%2C+J+L">Jonelle L. Walsh</a>, <a href="/search/astro-ph?searchtype=author&query=Ito%2C+J">Jennifer Ito</a>, <a href="/search/astro-ph?searchtype=author&query=Goulding%2C+A+D">Andy D. Goulding</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1802.00014v2-abstract-short" style="display: inline;"> We use spatially resolved two-dimensional stellar velocity maps over a $107"\times 107"$ field of view to investigate the kinematic features of 90 early-type galaxies above stellar mass $10^{11.5}M_\odot$ in the MASSIVE survey. We measure the misalignment angle $唯$ between the kinematic and photometric axes and identify local features such as velocity twists and kinematically distinct components.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.00014v2-abstract-full').style.display = 'inline'; document.getElementById('1802.00014v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1802.00014v2-abstract-full" style="display: none;"> We use spatially resolved two-dimensional stellar velocity maps over a $107"\times 107"$ field of view to investigate the kinematic features of 90 early-type galaxies above stellar mass $10^{11.5}M_\odot$ in the MASSIVE survey. We measure the misalignment angle $唯$ between the kinematic and photometric axes and identify local features such as velocity twists and kinematically distinct components. We find 46% of the sample to be well aligned ($唯< 15^{\circ}$), 33% misaligned, and 21% without detectable rotation (non-rotators). Only 24% of the sample are fast rotators, the majority of which (91%) are aligned, whereas 57% of the slow rotators are misaligned with a nearly flat distribution of $唯$ from $15^{\circ}$ to $90^{\circ}$. 11 galaxies have $唯\gtrsim 60^{\circ}$ and thus exhibit minor-axis ("prolate") rotation in which the rotation is preferentially around the photometric major axis. Kinematic misalignments occur more frequently for lower galaxy spin or denser galaxy environments. Using the observed misalignment and ellipticity distributions, we infer the intrinsic shape distribution of our sample and find that MASSIVE slow rotators are consistent with being mildly triaxial, with mean axis ratios of $b/a=0.88$ and $c/a=0.65$. In terms of local kinematic features, 51% of the sample exhibit kinematic twists of larger than $20^{\circ}$, and 2 galaxies have kinematically distinct components. The frequency of misalignment and the broad distribution of $唯$ reported here suggest that the most massive early-type galaxies are mildly triaxial, and that formation processes resulting in kinematically misaligned slow rotators such as gas-poor mergers occur frequently in this mass range. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.00014v2-abstract-full').style.display = 'none'; document.getElementById('1802.00014v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 June, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 31 January, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1801.08245">arXiv:1801.08245</a> <span> [<a href="https://arxiv.org/pdf/1801.08245">pdf</a>, <a href="https://arxiv.org/format/1801.08245">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/aab1f3">10.3847/1538-4357/aab1f3 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MASSIVE Survey IX: Photometric Analysis of 35 High Mass Early-Type Galaxies with HST WFC3/IR </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Goullaud%2C+C+F">Charles F. Goullaud</a>, <a href="/search/astro-ph?searchtype=author&query=Jensen%2C+J+B">Joseph B. Jensen</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Ma%2C+C">Chung-Pei Ma</a>, <a href="/search/astro-ph?searchtype=author&query=Greene%2C+J+E">Jenny E. Greene</a>, <a href="/search/astro-ph?searchtype=author&query=Thomas%2C+J">Jens Thomas</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1801.08245v2-abstract-short" style="display: inline;"> We present near-infrared observations of 35 of the most massive early-type galaxies in the local universe. The observations were made using the infrared channel of the Hubble Space Telescope Wide Field Camera 3 in the F110W (1.1 $渭$m) filter. We measured surface brightness profiles and elliptical isophotal fit parameters from the nuclear regions out to a radius of ~10 kpc in most cases. We find th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.08245v2-abstract-full').style.display = 'inline'; document.getElementById('1801.08245v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1801.08245v2-abstract-full" style="display: none;"> We present near-infrared observations of 35 of the most massive early-type galaxies in the local universe. The observations were made using the infrared channel of the Hubble Space Telescope Wide Field Camera 3 in the F110W (1.1 $渭$m) filter. We measured surface brightness profiles and elliptical isophotal fit parameters from the nuclear regions out to a radius of ~10 kpc in most cases. We find that 37% (13) of the galaxies in our sample have isophotal position angle rotations greater than 20 degrees over the radial range imaged by WFC3/IR, which is often due to the presence of neighbors or multiple nuclei. Most galaxies in our sample are significantly rounder near the center than in the outer regions. This sample contains six fast rotators and 28 slow rotators. We find that all fast rotators are either disky or show no measurable deviation from purely elliptical isophotes. Among slow rotators, significantly disky and boxy galaxies occur with nearly equal frequency. The galaxies in our sample often exhibit changing isophotal shapes, sometimes showing both significantly disky and boxy isophotes at different radii. The fact that parameters vary widely between galaxies and within individual galaxies is evidence that these massive galaxies have complicated formation histories, and some of them have experienced recent mergers and have not fully relaxed. These data demonstrate the value of high spatial resolution IR imaging of galaxies and provide measurements necessary for determining stellar masses, dynamics, and black hole masses in high mass galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.08245v2-abstract-full').style.display = 'none'; document.getElementById('1801.08245v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 February, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 January, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">31 pages, 39 figures, accepted for publication in the Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1801.06080">arXiv:1801.06080</a> <span> [<a href="https://arxiv.org/pdf/1801.06080">pdf</a>, <a href="https://arxiv.org/ps/1801.06080">ps</a>, <a href="https://arxiv.org/format/1801.06080">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/aaad64">10.3847/2041-8213/aaad64 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Precise Distance to the Host Galaxy of the Binary Neutron Star Merger GW170817 Using Surface Brightness Fluctuations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Jensen%2C+J+B">J. B. Jensen</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">J. P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Berger%2C+E">E. Berger</a>, <a href="/search/astro-ph?searchtype=author&query=Levan%2C+A+J">A. J. Levan</a>, <a href="/search/astro-ph?searchtype=author&query=Tanvir%2C+N+R">N. R. Tanvir</a>, <a href="/search/astro-ph?searchtype=author&query=Raimondo%2C+G">G. Raimondo</a>, <a href="/search/astro-ph?searchtype=author&query=Brocato%2C+E">E. Brocato</a>, <a href="/search/astro-ph?searchtype=author&query=Alexander%2C+K+D">K. D. Alexander</a>, <a href="/search/astro-ph?searchtype=author&query=Blanchard%2C+P+K">P. K. Blanchard</a>, <a href="/search/astro-ph?searchtype=author&query=Branchesi%2C+M">M. Branchesi</a>, <a href="/search/astro-ph?searchtype=author&query=Cano%2C+Z">Z. Cano</a>, <a href="/search/astro-ph?searchtype=author&query=Chornock%2C+R">R. Chornock</a>, <a href="/search/astro-ph?searchtype=author&query=Covino%2C+S">S. Covino</a>, <a href="/search/astro-ph?searchtype=author&query=Cowperthwaite%2C+P+S">P. S. Cowperthwaite</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Avanzo%2C+P">P. D'Avanzo</a>, <a href="/search/astro-ph?searchtype=author&query=Eftekhari%2C+T">T. Eftekhari</a>, <a href="/search/astro-ph?searchtype=author&query=Fong%2C+W">W. Fong</a>, <a href="/search/astro-ph?searchtype=author&query=Fruchter%2C+A+S">A. S. Fruchter</a>, <a href="/search/astro-ph?searchtype=author&query=Grado%2C+A">A. Grado</a>, <a href="/search/astro-ph?searchtype=author&query=Hjorth%2C+J">J. Hjorth</a>, <a href="/search/astro-ph?searchtype=author&query=Holz%2C+D+E">D. E. Holz</a>, <a href="/search/astro-ph?searchtype=author&query=Lyman%2C+J+D">J. D. Lyman</a>, <a href="/search/astro-ph?searchtype=author&query=Mandel%2C+I">I. Mandel</a>, <a href="/search/astro-ph?searchtype=author&query=Margutti%2C+R">R. Margutti</a> , et al. (3 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1801.06080v2-abstract-short" style="display: inline;"> The joint detection of gravitational waves and electromagnetic radiation from the binary neutron star (BNS) merger GW170817 has provided unprecedented insight into a wide range of physical processes: heavy element synthesis via the $r$-process; the production of relativistic ejecta; the equation of state of neutron stars and the nature of the merger remnant; the binary coalescence timescale; and a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.06080v2-abstract-full').style.display = 'inline'; document.getElementById('1801.06080v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1801.06080v2-abstract-full" style="display: none;"> The joint detection of gravitational waves and electromagnetic radiation from the binary neutron star (BNS) merger GW170817 has provided unprecedented insight into a wide range of physical processes: heavy element synthesis via the $r$-process; the production of relativistic ejecta; the equation of state of neutron stars and the nature of the merger remnant; the binary coalescence timescale; and a measurement of the Hubble constant via the "standard siren" technique. In detail, all of these results depend on the distance to the host galaxy of the merger event, NGC4993. In this paper we measure the surface brightness fluctuation (SBF) distance to NGC4993 in the F110W and F160W passbands of the Wide Field Camera 3 Infrared Channel on the Hubble Space Telescope (HST). For the preferred F110W passband we derive a distance modulus of $m{-}M=33.05\pm0.08\pm0.10$ mag, or a linear distance $d=40.7\pm1.4\pm1.9$ Mpc (random and systematic errors, respectively); a virtually identical result is obtained from the F160W data. This is the most precise distance to NGC4993 available to date. Combining our distance measurement with the corrected recession velocity of NGC4993 implies a Hubble constant $H_0=71.9\pm 7.1~km~s^{-1}~Mpc^{-1}$. A comparison of our result to the GW-inferred value of $H_0$ indicates a binary orbital inclination of $i\,{\gtrsim}\,137~掳$. The SBF technique can be applied to early-type host galaxies of BNS mergers to ${\sim\,}100$ Mpc with HST and possibly as far as ${\sim\,}300$ Mpc with the James Webb Space Telescope, thereby helping to break the inherent distance-inclination degeneracy of the GW signals at distances where many future BNS mergers are likely to be detected. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.06080v2-abstract-full').style.display = 'none'; document.getElementById('1801.06080v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 February, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 January, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">ApJ Letters in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1711.00750">arXiv:1711.00750</a> <span> [<a href="https://arxiv.org/pdf/1711.00750">pdf</a>, <a href="https://arxiv.org/format/1711.00750">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/10.1051/0004-6361/201730649">10.1051/0004-6361/201730649 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> VEGAS-SSS II: Comparing the globular cluster systems in NGC3115 and NGC1399 using VEGAS and FDS survey data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Abrusco%2C+R">Raffaele D'Abrusco</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">Marilena Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Paolillo%2C+M">Maurizio Paolillo</a>, <a href="/search/astro-ph?searchtype=author&query=Capaccioli%2C+M">Massimo Capaccioli</a>, <a href="/search/astro-ph?searchtype=author&query=Limatola%2C+L">Luca Limatola</a>, <a href="/search/astro-ph?searchtype=author&query=Grado%2C+A">Aniello Grado</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">Enrica Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Raimondo%2C+G">Gabriella Raimondo</a>, <a href="/search/astro-ph?searchtype=author&query=Napolitano%2C+N">Nicola Napolitano</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Brocato%2C+E">Enzo Brocato</a>, <a href="/search/astro-ph?searchtype=author&query=Forbes%2C+D+A">Duncan A. Forbes</a>, <a href="/search/astro-ph?searchtype=author&query=Hilker%2C+M">Michael Hilker</a>, <a href="/search/astro-ph?searchtype=author&query=Mieske%2C+S">Steffen Mieske</a>, <a href="/search/astro-ph?searchtype=author&query=Peletier%2C+R">Reynier Peletier</a>, <a href="/search/astro-ph?searchtype=author&query=van+de+Ven%2C+G">Glenn van de Ven</a>, <a href="/search/astro-ph?searchtype=author&query=Schipani%2C+P">Pietro Schipani</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="1711.00750v1-abstract-short" style="display: inline;"> We analyze the globular cluster (GC) systems in two very different galaxies, N3115 and N1399. With the papers of this series, we aim at highlighting common and different properties in the GC systems in galaxies covering a wide range of parameter space. We compare the GCs in N3115 and N1399 as derived from the analysis of u, g, and i band images taken with the VST telescope as part of the VEGAS and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1711.00750v1-abstract-full').style.display = 'inline'; document.getElementById('1711.00750v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1711.00750v1-abstract-full" style="display: none;"> We analyze the globular cluster (GC) systems in two very different galaxies, N3115 and N1399. With the papers of this series, we aim at highlighting common and different properties in the GC systems in galaxies covering a wide range of parameter space. We compare the GCs in N3115 and N1399 as derived from the analysis of u, g, and i band images taken with the VST telescope as part of the VEGAS and FDS surveys. We selected GC candidates using as reference the morpho-photometric and color properties of confirmed GCs. The surface density of GCs in N3115 reveal a morphology similar to the profile of field stars; the same is true when blue and red GCs are taken separately. The GC maps for N1399 are richer in structure and confirm the existence of an intracluster GC component. We confirm the presence of a spatial offset in the N1399 GC centroid and find that the centroid of the GCs for N3115 coincides well with the galaxy center. Both GC systems show unambiguous color bimodality in g-i and u-i. The azimuthal average of the radial density profiles in both galaxies reveals a larger spatial extent for the total GCs population with respect to the galaxy surface brightness profile. As for the specific frequency of GCs, Sn, we find it is a factor of two higher in N1399 than for N3115. By inspecting the radial behavior of the specific frequency, Sn(<r), for the total, blue, and red GCs, we find notable similarities between the trends for red GCs in the two targets. In spite of extremely different host environments, the red GCs in both cases appear closely linked to the light distribution of field stars. Blue GCs extend to larger galactocentric scales than red GCs, marking a significant difference between the two galaxies: the blue/red GCs and field stellar components of N3115 appear well thermalized with each other and the blue GCs in N1399 appear to fade into an unrelaxed intracluster GC population. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1711.00750v1-abstract-full').style.display = 'none'; document.getElementById('1711.00750v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 November, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">25 pages, 18 figures, Astronomy and Astrophysics (accepted)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 611, A93 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1710.01322">arXiv:1710.01322</a> <span> [<a href="https://arxiv.org/pdf/1710.01322">pdf</a>, <a href="https://arxiv.org/ps/1710.01322">ps</a>, <a href="https://arxiv.org/format/1710.01322">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/aa8f44">10.3847/1538-4357/aa8f44 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Specific Frequencies and Luminosity Profiles of Cluster Galaxies and Intracluster Light in Abell 1689 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Alamo-Mart%C3%ADnez%2C+K+A">K. A. Alamo-Mart铆nez</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">J. P. Blakeslee</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1710.01322v1-abstract-short" style="display: inline;"> We present magnitudes and profile fits for 180 galaxies in the central field of the massive lensing cluster Abell 1689 using very deep imaging with the ACS/HST in the F814W bandpass. Previous work revealed an exceptionally large number of globular clusters (GCs) in A1689 and mapped their number density distribution. We decompose this number density map into GCs associated with individual cluster g… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1710.01322v1-abstract-full').style.display = 'inline'; document.getElementById('1710.01322v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1710.01322v1-abstract-full" style="display: none;"> We present magnitudes and profile fits for 180 galaxies in the central field of the massive lensing cluster Abell 1689 using very deep imaging with the ACS/HST in the F814W bandpass. Previous work revealed an exceptionally large number of globular clusters (GCs) in A1689 and mapped their number density distribution. We decompose this number density map into GCs associated with individual cluster galaxies and ICGCs (intracluster globular clusters) associated with the intracluster light (ICL). In all, we measure GC specific frequencies $S_N$ for 33 cluster members and the ICL. The relation between $S_N$ and galaxy magnitude is consistent with the trend observed in Virgo, although some intermediate luminosity galaxies scatter to $S_N>10$. We estimate the ICL makes up 11% of the starlight in this field, whereas the ICGCs account for $\sim\,$35% of the GCs, both consistent with predictions from simulations. Galaxies with higher $S_N$ values tend to be rounder, and there is a marginally significant trend of decreasing $S_N$ with increasing specific angular momenta $位_R$. We also reevaluate the GC population in the A2744 Frontier Field, for which fewer than one-tenth as many GCs have been detected because of its larger distance. Finally, our core-S茅rsic fit to the light profile of the A1689 BCG implies a break radius of 3.8kpc, among the largest known; we discuss implications of the sizable core and extensive GC population for the supermassive black hole in light of scaling relations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1710.01322v1-abstract-full').style.display = 'none'; document.getElementById('1710.01322v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 October, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in 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/1708.00870">arXiv:1708.00870</a> <span> [<a href="https://arxiv.org/pdf/1708.00870">pdf</a>, <a href="https://arxiv.org/format/1708.00870">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stx2717">10.1093/mnras/stx2717 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MASSIVE Survey - VIII. Stellar Velocity Dispersion Profiles and Environmental Dependence of Early-Type Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Veale%2C+M">Melanie Veale</a>, <a href="/search/astro-ph?searchtype=author&query=Ma%2C+C">Chung-Pei Ma</a>, <a href="/search/astro-ph?searchtype=author&query=Greene%2C+J+E">Jenny E. Greene</a>, <a href="/search/astro-ph?searchtype=author&query=Thomas%2C+J">Jens Thomas</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Walsh%2C+J+L">Jonelle L. Walsh</a>, <a href="/search/astro-ph?searchtype=author&query=Ito%2C+J">Jennifer Ito</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="1708.00870v2-abstract-short" style="display: inline;"> We measure the radial profiles of the stellar velocity dispersions, $蟽(R)$, for 90 early-type galaxies (ETGs) in the MASSIVE survey, a volume-limited integral-field spectroscopic (IFS) galaxy survey targeting all northern-sky ETGs with absolute $K$-band magnitude $M_K < -25.3$ mag, or stellar mass $M_* > 4 \times 10^{11} M_\odot$, within 108 Mpc. Our wide-field 107" $\times$ 107" IFS data cover ra… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1708.00870v2-abstract-full').style.display = 'inline'; document.getElementById('1708.00870v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1708.00870v2-abstract-full" style="display: none;"> We measure the radial profiles of the stellar velocity dispersions, $蟽(R)$, for 90 early-type galaxies (ETGs) in the MASSIVE survey, a volume-limited integral-field spectroscopic (IFS) galaxy survey targeting all northern-sky ETGs with absolute $K$-band magnitude $M_K < -25.3$ mag, or stellar mass $M_* > 4 \times 10^{11} M_\odot$, within 108 Mpc. Our wide-field 107" $\times$ 107" IFS data cover radii as large as 40 kpc, for which we quantify separately the inner (2 kpc) and outer (20 kpc) logarithmic slopes $纬_{\rm inner}$ and $纬_{\rm outer}$ of $蟽(R)$. While $纬_{\rm inner}$ is mostly negative, of the 56 galaxies with sufficient radial coverage to determine $纬_{\rm outer}$ we find 36% to have rising outer dispersion profiles, 30% to be flat within the uncertainties, and 34% to be falling. The fraction of galaxies with rising outer profiles increases with $M_*$ and in denser galaxy environment, with 10 of the 11 most massive galaxies in our sample having flat or rising dispersion profiles. The strongest environmental correlations are with local density and halo mass, but a weaker correlation with large-scale density also exists. The average $纬_{\rm outer}$ is similar for brightest group galaxies, satellites, and isolated galaxies in our sample. We find a clear positive correlation between the gradients of the outer dispersion profile and the gradients of the velocity kurtosis $h_4$. Altogether, our kinematic results suggest that the increasing fraction of rising dispersion profiles in the most massive ETGs are caused (at least in part) by variations in the total mass profiles rather than in the velocity anisotropy alone. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1708.00870v2-abstract-full').style.display = 'none'; document.getElementById('1708.00870v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 October, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 August, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted/in press, 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/1706.04194">arXiv:1706.04194</a> <span> [<a href="https://arxiv.org/pdf/1706.04194">pdf</a>, <a href="https://arxiv.org/format/1706.04194">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/aa77b1">10.3847/1538-4357/aa77b1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Next Generation Virgo cluster Survey (NGVS). XXVI. The issues of photometric age and metallicity estimates for globular clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Powalka%2C+M">Mathieu Powalka</a>, <a href="/search/astro-ph?searchtype=author&query=Lan%C3%A7on%2C+A">Ariane Lan莽on</a>, <a href="/search/astro-ph?searchtype=author&query=Puzia%2C+T+H">Thomas H. Puzia</a>, <a href="/search/astro-ph?searchtype=author&query=Peng%2C+E+W">Eric W. Peng</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+C">Chengze Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Mu%C3%B1oz%2C+R+P">Roberto P. Mu帽oz</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=C%C3%B4t%C3%A9%2C+P">Patrick C么t茅</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrarese%2C+L">Laura Ferrarese</a>, <a href="/search/astro-ph?searchtype=author&query=Roediger%2C+J">Joel Roediger</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Janssen%2C+R">R煤ben S谩nchez-Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+H">Hongxin Zhang</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=Cuillandre%2C+J">Jean-Charles Cuillandre</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P">Pierre-Alain Duc</a>, <a href="/search/astro-ph?searchtype=author&query=Guhathakurta%2C+P">Puragra Guhathakurta</a>, <a href="/search/astro-ph?searchtype=author&query=Gwyn%2C+S+D+J">S. D. J. Gwyn</a>, <a href="/search/astro-ph?searchtype=author&query=Hudelot%2C+P">Patrick Hudelot</a>, <a href="/search/astro-ph?searchtype=author&query=Mei%2C+S">Simona Mei</a>, <a href="/search/astro-ph?searchtype=author&query=Toloba%2C+E">Elisa Toloba</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1706.04194v1-abstract-short" style="display: inline;"> Large samples of globular clusters (GC) with precise multi-wavelength photometry are becoming increasingly available and can be used to constrain the formation history of galaxies. We present the results of an analysis of Milky Way (MW) and Virgo core GCs based on five optical-near-infrared colors and ten synthetic stellar population models. For the MW GCs, the models tend to agree on photometric… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1706.04194v1-abstract-full').style.display = 'inline'; document.getElementById('1706.04194v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1706.04194v1-abstract-full" style="display: none;"> Large samples of globular clusters (GC) with precise multi-wavelength photometry are becoming increasingly available and can be used to constrain the formation history of galaxies. We present the results of an analysis of Milky Way (MW) and Virgo core GCs based on five optical-near-infrared colors and ten synthetic stellar population models. For the MW GCs, the models tend to agree on photometric ages and metallicities, with values similar to those obtained with previous studies. When used with Virgo core GCs, for which photometry is provided by the Next Generation Virgo cluster Survey (NGVS), the same models generically return younger ages. This is a consequence of the systematic differences observed between the locus occupied by Virgo core GCs and models in panchromatic color space. Only extreme fine-tuning of the adjustable parameters available to us can make the majority of the best-fit ages old. Although we cannot exclude that the formation history of the Virgo core may lead to more conspicuous populations of relatively young GCs than in other environments, we emphasize that the intrinsic properties of the Virgo GCs are likely to differ systematically from those assumed in the models. Thus, the large wavelength coverage and photometric quality of modern GC samples, such as used here, is not by itself sufficient to better constrain the GC formation histories. Models matching the environment-dependent characteristics of GCs in multi-dimensional color space are needed to improve the situation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1706.04194v1-abstract-full').style.display = 'none'; document.getElementById('1706.04194v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 June, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 12 figures, Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1703.08573">arXiv:1703.08573</a> <span> [<a href="https://arxiv.org/pdf/1703.08573">pdf</a>, <a href="https://arxiv.org/format/1703.08573">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stx1639">10.1093/mnras/stx1639 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MASSIVE Survey - VII. The Relationship of Angular Momentum, Stellar Mass and Environment of Early-Type Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Veale%2C+M">Melanie Veale</a>, <a href="/search/astro-ph?searchtype=author&query=Ma%2C+C">Chung-Pei Ma</a>, <a href="/search/astro-ph?searchtype=author&query=Greene%2C+J+E">Jenny E. Greene</a>, <a href="/search/astro-ph?searchtype=author&query=Thomas%2C+J">Jens Thomas</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=McConnell%2C+N">Nicholas McConnell</a>, <a href="/search/astro-ph?searchtype=author&query=Walsh%2C+J+L">Jonelle L. Walsh</a>, <a href="/search/astro-ph?searchtype=author&query=Ito%2C+J">Jennifer Ito</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1703.08573v2-abstract-short" style="display: inline;"> We analyse the environmental properties of 370 local early-type galaxies (ETGs) in the MASSIVE and ATLAS3D surveys, two complementary volume-limited integral-field spectroscopic (IFS) galaxy surveys spanning absolute $K$-band magnitude $-21.5 > M_K > -26.6$, or stellar mass $8 \times 10^{9} < M_* < 2 \times 10^{12} M_\odot$. We find these galaxies to reside in a diverse range of environments measu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.08573v2-abstract-full').style.display = 'inline'; document.getElementById('1703.08573v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1703.08573v2-abstract-full" style="display: none;"> We analyse the environmental properties of 370 local early-type galaxies (ETGs) in the MASSIVE and ATLAS3D surveys, two complementary volume-limited integral-field spectroscopic (IFS) galaxy surveys spanning absolute $K$-band magnitude $-21.5 > M_K > -26.6$, or stellar mass $8 \times 10^{9} < M_* < 2 \times 10^{12} M_\odot$. We find these galaxies to reside in a diverse range of environments measured by four methods: group membership (whether a galaxy is a brightest group/cluster galaxy, satellite, or isolated), halo mass, large-scale mass density (measured over a few Mpc), and local mass density (measured within the $N$th neighbour). The spatially resolved IFS stellar kinematics provide robust measurements of the spin parameter $位_e$ and enable us to examine the relationship among $位_e$, $M_*$, and galaxy environment. We find a strong correlation between $位_e$ and $M_*$, where the average $位_e$ decreases from $\sim 0.4$ to below 0.1 with increasing mass, and the fraction of slow rotators $f_{\rm slow}$ increases from $\sim 10$% to 90%. We show for the first time that at fixed $M_*$, there are almost no trends between galaxy spin and environment; the apparent kinematic morphology-density relation for ETGs is therefore primarily driven by $M_*$ and is accounted for by the joint correlations between $M_*$ and spin, and between $M_*$ and environment. A possible exception is that the increased $f_{\rm slow}$ at high local density is slightly more than expected based only on these joint correlations. Our results suggest that the physical processes responsible for building up the present-day stellar masses of massive galaxies are also very efficient at reducing their spin, in any environment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.08573v2-abstract-full').style.display = 'none'; document.getElementById('1703.08573v2-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 June, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 March, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1701.08772">arXiv:1701.08772</a> <span> [<a href="https://arxiv.org/pdf/1701.08772">pdf</a>, <a href="https://arxiv.org/format/1701.08772">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/aa5ebc">10.3847/1538-4357/aa5ebc <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MASSIVE Survey VI: The Spatial Distribution and Kinematics of Warm Ionized Gas in the Most Massive Local Early-type Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pandya%2C+V">Viraj Pandya</a>, <a href="/search/astro-ph?searchtype=author&query=Greene%2C+J+E">Jenny E. Greene</a>, <a href="/search/astro-ph?searchtype=author&query=Ma%2C+C">Chung-Pei Ma</a>, <a href="/search/astro-ph?searchtype=author&query=Veale%2C+M">Melanie Veale</a>, <a href="/search/astro-ph?searchtype=author&query=Ene%2C+I">Irina Ene</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+A">Timothy A. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Goulding%2C+A+D">Andy D. Goulding</a>, <a href="/search/astro-ph?searchtype=author&query=McConnell%2C+N+J">Nicholas J. McConnell</a>, <a href="/search/astro-ph?searchtype=author&query=Nyland%2C+K">Kristina Nyland</a>, <a href="/search/astro-ph?searchtype=author&query=Thomas%2C+J">Jens Thomas</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="1701.08772v1-abstract-short" style="display: inline;"> We present the first systematic investigation of the existence, spatial distribution, and kinematics of warm ionized gas as traced by the [O II] 3727AA emission line in 74 of the most massive galaxies in the local Universe. All of our galaxies have deep integral field spectroscopy from the volume- and magnitude-limited MASSIVE survey of early-type galaxies with stellar mass log(M_*/M_sun) > 11.5 (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1701.08772v1-abstract-full').style.display = 'inline'; document.getElementById('1701.08772v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1701.08772v1-abstract-full" style="display: none;"> We present the first systematic investigation of the existence, spatial distribution, and kinematics of warm ionized gas as traced by the [O II] 3727AA emission line in 74 of the most massive galaxies in the local Universe. All of our galaxies have deep integral field spectroscopy from the volume- and magnitude-limited MASSIVE survey of early-type galaxies with stellar mass log(M_*/M_sun) > 11.5 (M_K < -25.3 mag) and distance D < 108 Mpc. Of the 74 galaxies in our sample, we detect warm ionized gas in 28, which yields a global detection fraction of 38\pm6% down to a typical [O II] equivalent width limit of 2AA. MASSIVE fast rotators are more likely to have gas than MASSIVE slow rotators with detection fractions of 80\pm10% and 28\pm6%, respectively. The spatial extents span a wide range of radii (0.6 - 18.2 kpc; 0.1 - 4R_e), and the gas morphologies are diverse, with 17/28 = 61\pm9% being centrally concentrated, 8/28 = 29\pm9% exhibiting clear rotation out to several kpc, and 3/28 = 11\pm6% being extended but patchy. Three out of four fast rotators show kinematic alignment between the stars and gas, whereas the two slow rotators with robust kinematic measurements available exhibit kinematic misalignment. Our inferred warm ionized gas masses are roughly ~10^5M_sun. The emission line ratios and radial equivalent width profiles are generally consistent with excitation of the gas by the old underlying stellar population. We explore different gas origin scenarios for MASSIVE galaxies and find that a variety of physical processes are likely at play, including internal gas recycling, cooling out of the hot gaseous halo, and gas acquired via mergers. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1701.08772v1-abstract-full').style.display = 'none'; document.getElementById('1701.08772v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 January, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">Re-submitted to ApJ after addressing referee report; main body is 14 pages with 6 figures; with appendices, total of 24 pages and 14 figures; comments welcome</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1701.04845">arXiv:1701.04845</a> <span> [<a href="https://arxiv.org/pdf/1701.04845">pdf</a>, <a href="https://arxiv.org/format/1701.04845">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/10.3847/1538-4357/836/1/67">10.3847/1538-4357/836/1/67 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galactic Dark Matter Halos and Globular Cluster Populations. III: Extension to Extreme Environments </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Harris%2C+W+E">William E. Harris</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Harris%2C+G+L+H">Gretchen L. H. Harris</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1701.04845v1-abstract-short" style="display: inline;"> The total mass M_GCS in the globular cluster (GC) system of a galaxy is empirically a near-constant fraction of the total mass M_h = M_bary + M_dark of the galaxy, across a range of 10^5 in galaxy mass. This trend is radically unlike the strongly nonlinear behavior of total stellar mass M_star versus M_h. We discuss extensions of this trend to two more extreme situations: (a) entire clusters of ga… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1701.04845v1-abstract-full').style.display = 'inline'; document.getElementById('1701.04845v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1701.04845v1-abstract-full" style="display: none;"> The total mass M_GCS in the globular cluster (GC) system of a galaxy is empirically a near-constant fraction of the total mass M_h = M_bary + M_dark of the galaxy, across a range of 10^5 in galaxy mass. This trend is radically unlike the strongly nonlinear behavior of total stellar mass M_star versus M_h. We discuss extensions of this trend to two more extreme situations: (a) entire clusters of galaxies, and (b) the Ultra-Diffuse Galaxies (UDGs) recently discovered in Coma and elsewhere. Our calibration of the ratio 畏_M = M_GCS / M_h from normal galaxies, accounting for new revisions in the adopted mass-to-light ratio for GCs, now gives 畏_M = 2.9 \times 10^{-5} as the mean absolute mass fraction. We find that the same ratio appears valid for galaxy clusters and UDGs. Estimates of 畏_M in the four clusters we examine tend to be slightly higher than for individual galaxies, butmore data and better constraints on the mean GC mass in such systems are needed to determine if this difference is significant. We use the constancy of 畏_M to estimate total masses for several individual cases; for example, the total mass of the Milky Way is calculated to be M_h = 1.1 \times 10^{12} M_sun. Physical explanations for the uniformity of 畏_M are still descriptive, but point to a picture in which massive, dense star clusters in their formation stages were relatively immune to the feedback that more strongly influenced lower-density regions where most stars form. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1701.04845v1-abstract-full').style.display = 'none'; document.getElementById('1701.04845v1-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 January, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">In press for Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1611.03561">arXiv:1611.03561</a> <span> [<a href="https://arxiv.org/pdf/1611.03561">pdf</a>, <a href="https://arxiv.org/format/1611.03561">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/10.3847/1538-4357/834/1/66">10.3847/1538-4357/834/1/66 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> THE NEXT GENERATION VIRGO CLUSTER SURVEY. XIV. Shell feature early-type dwarf galaxies in the Virgo cluster </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=Smith%2C+R">Rory Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P">Pierre-Alain Duc</a>, <a href="/search/astro-ph?searchtype=author&query=C%C3%B4t%C3%A9%2C+P">Patrick C么t茅</a>, <a href="/search/astro-ph?searchtype=author&query=Cuillandre%2C+J">Jean-Charles Cuillandre</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrarese%2C+L">Laura Ferrarese</a>, <a href="/search/astro-ph?searchtype=author&query=Blakeslee%2C+J+P">John P. Blakeslee</a>, <a href="/search/astro-ph?searchtype=author&query=Boselli%2C+A">Alessandro Boselli</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">Michele Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Gwyn%2C+S+D+J">S. D. J. Gwyn</a>, <a href="/search/astro-ph?searchtype=author&query=Guhathakurta%2C+P">Puragra Guhathakurta</a>, <a href="/search/astro-ph?searchtype=author&query=Mei%2C+S">Simona Mei</a>, <a href="/search/astro-ph?searchtype=author&query=Mihos%2C+J+C">J. Christopher Mihos</a>, <a href="/search/astro-ph?searchtype=author&query=Peng%2C+E+W">Eric W. Peng</a>, <a href="/search/astro-ph?searchtype=author&query=Powalka%2C+M">Mathieu Powalka</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=Toloba%2C+E">Elisa Toloba</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+H">Hongxin Zhang</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1611.03561v1-abstract-short" style="display: inline;"> The Next Generation Virgo Cluster Survey is a deep (with a $2蟽$ detection limit $渭_g$ = 29~mag~arcsec$^{-2}$ in the $g-$band) optical panchromatic survey targeting the Virgo cluster from its core to virial radius, for a total areal coverage of 104 square degrees. As such, the survey is well suited for the study of galaxies' outskirts, haloes and low surface brightness features that arise from dyna… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.03561v1-abstract-full').style.display = 'inline'; document.getElementById('1611.03561v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1611.03561v1-abstract-full" style="display: none;"> The Next Generation Virgo Cluster Survey is a deep (with a $2蟽$ detection limit $渭_g$ = 29~mag~arcsec$^{-2}$ in the $g-$band) optical panchromatic survey targeting the Virgo cluster from its core to virial radius, for a total areal coverage of 104 square degrees. As such, the survey is well suited for the study of galaxies' outskirts, haloes and low surface brightness features that arise from dynamical interactions within the cluster environment. We report the discovery of extremely faint ($渭_g$ $>$ 25 mag arcsec$^{-2}$) shells in three Virgo cluster early-type dwarf galaxies, VCC~1361, VCC~1447 and VCC~1668. Among them, VCC~1447 has an absolute magnitude M$_{g}$ = -11.71 mag and is {\it the least massive galaxy with a shell system discovered to date}. We present a detailed study of these low surface brightness features. We detect between three and four shells in each of our galaxies. Within the uncertainties, we find no evidence of a color difference between the galaxy main body and shell features. The observed arcs of the shells are located upto several effective radii of the galaxies. We further explore the origin of these low surface brightness features with the help of idealized numerical simulations. We find that a near equal mass merger is best able to reproduce the main properties of the shells, including their quite symmetric appearance and their alignment along the major axis of the galaxy. The simulations provide support for a formation scenario in which a recent merger, between two near-equal mass, gas-free dwarf galaxies forms the observed shell systems. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.03561v1-abstract-full').style.display = 'none'; document.getElementById('1611.03561v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 November, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, Accepted to ApJ</span> </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous 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