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</div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.11327">arXiv:2106.11327</a> <span> [<a href="https://arxiv.org/pdf/2106.11327">pdf</a>, <a href="https://arxiv.org/format/2106.11327">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/10.1093/mnras/stab1639">10.1093/mnras/stab1639 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Thermodynamic evolution of the $z=1.75$ galaxy cluster IDCS J1426.5+3508 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Andreon%2C+S">S. Andreon</a>, <a href="/search/astro-ph?searchtype=author&query=Romero%2C+C">C. Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Castagna%2C+F">F. Castagna</a>, <a href="/search/astro-ph?searchtype=author&query=Ragagnin%2C+A">A. Ragagnin</a>, <a href="/search/astro-ph?searchtype=author&query=Devlin%2C+M">M. Devlin</a>, <a href="/search/astro-ph?searchtype=author&query=Dicker%2C+S">S. Dicker</a>, <a href="/search/astro-ph?searchtype=author&query=Mason%2C+B">B. Mason</a>, <a href="/search/astro-ph?searchtype=author&query=Mroczkowski%2C+T">T. Mroczkowski</a>, <a href="/search/astro-ph?searchtype=author&query=Sarazin%2C+C">C. Sarazin</a>, <a href="/search/astro-ph?searchtype=author&query=Sievers%2C+J">J. Sievers</a>, <a href="/search/astro-ph?searchtype=author&query=Stanchfield%2C+S">S. Stanchfield</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2106.11327v2-abstract-short" style="display: inline;"> We present resolved thermodynamic profiles out to 500 kpc, about $r_{500}$, of the $z=1.75$ galaxy cluster IDCS J1426.5+3508 with 40 kpc resolution. Thanks to the combination of Sunyaev-Zel'dovich and X-ray datasets, IDCS J1426.5+3508 becomes the most distant cluster with resolved thermodynamic profiles. These are derived assuming a non-parametric pressure profile and a very flexible model for the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.11327v2-abstract-full').style.display = 'inline'; document.getElementById('2106.11327v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.11327v2-abstract-full" style="display: none;"> We present resolved thermodynamic profiles out to 500 kpc, about $r_{500}$, of the $z=1.75$ galaxy cluster IDCS J1426.5+3508 with 40 kpc resolution. Thanks to the combination of Sunyaev-Zel'dovich and X-ray datasets, IDCS J1426.5+3508 becomes the most distant cluster with resolved thermodynamic profiles. These are derived assuming a non-parametric pressure profile and a very flexible model for the electron density profile. The shape of the pressure profile is flatter than the universal pressure profile. The IDCS J1426.5+3508 temperature profile is increasing radially out to 500 kpc. To identify the possible future evolution of IDCS J1426.5+3508 , we compared it with its local descendants that numerical simulations show to be $0.65\pm0.12$ dex more massive. We found no evolution at 30 kpc, indicating a fine tuning between cooling and heating at small radii. At $30<r<300$ kpc, our observations show that entropy and heat must be deposited with little net gas transfer, while at 500 kpc the gas need to be replaced by a large amount of cold, lower entropy gas, consistent with theoretical expectation of a filamentary gas stream, which brings low entropy gas to 500 kpc and energy at even smaller radii. At $r \gtrsim 400$ kpc the polytropic index takes a low value, which indicates the presence of a large amount of non-thermal pressure. Our work also introduces a new definition of the evolutionary rate, which uses unscaled radii, unscaled thermodynamic quantities, and different masses at different redshifts to compare ancestors and descendants. It has the advantage of separating cluster evolution, dependence on mass, pseudo-evolution and returns a number with unique interpretation, unlike other definitions used in literature. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.11327v2-abstract-full').style.display = 'none'; document.getElementById('2106.11327v2-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 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">MNRAS, in press. In v2 we only corrected author affiliations and spelling</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2004.09555">arXiv:2004.09555</a> <span> [<a href="https://arxiv.org/pdf/2004.09555">pdf</a>, <a href="https://arxiv.org/format/2004.09555">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/ab8b5c">10.3847/1538-4365/ab8b5c <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MUSTANG-2 Galactic Plane Survey (MGPS90) pilot </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ginsburg%2C+A">Adam Ginsburg</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+L+D">L. D. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Dicker%2C+S">Simon Dicker</a>, <a href="/search/astro-ph?searchtype=author&query=Romero%2C+C">Charles Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Svoboda%2C+B">Brian Svoboda</a>, <a href="/search/astro-ph?searchtype=author&query=Devlin%2C+M">Mark Devlin</a>, <a href="/search/astro-ph?searchtype=author&query=Galv%C3%A1n-Madrid%2C+R">Roberto Galv谩n-Madrid</a>, <a href="/search/astro-ph?searchtype=author&query=Indebetouw%2C+R">Remy Indebetouw</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+H+B">Hauyu Baobab Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Mason%2C+B">Brian Mason</a>, <a href="/search/astro-ph?searchtype=author&query=Mroczkowski%2C+T">Tony Mroczkowski</a>, <a href="/search/astro-ph?searchtype=author&query=Armentrout%2C+W+P">W. P. Armentrout</a>, <a href="/search/astro-ph?searchtype=author&query=Bally%2C+J">John Bally</a>, <a href="/search/astro-ph?searchtype=author&query=Brogan%2C+C">Crystal Brogan</a>, <a href="/search/astro-ph?searchtype=author&query=Butterfield%2C+N">Natalie Butterfield</a>, <a href="/search/astro-ph?searchtype=author&query=Hunter%2C+T+R">Todd R. Hunter</a>, <a href="/search/astro-ph?searchtype=author&query=Reese%2C+E+D">Erik D. Reese</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E">Erik Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Sarazin%2C+C">Craig Sarazin</a>, <a href="/search/astro-ph?searchtype=author&query=Shirley%2C+Y">Yancy Shirley</a>, <a href="/search/astro-ph?searchtype=author&query=Sievers%2C+J">Jonathan Sievers</a>, <a href="/search/astro-ph?searchtype=author&query=Stanchfield%2C+S">Sara Stanchfield</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="2004.09555v2-abstract-short" style="display: inline;"> We report the results of a pilot program for a Green Bank Telescope (GBT) MUSTANG Galactic Plane survey at 3 mm (90 GHz), MGPS90. The survey achieves a typical $1蟽$ depth of $1-2$ mJy beam$^{-1}$ with a 9" beam. We describe the survey parameters, quality assessment process, cataloging, and comparison with other data sets. We have identified 709 sources over seven observed fields selecting some of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.09555v2-abstract-full').style.display = 'inline'; document.getElementById('2004.09555v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2004.09555v2-abstract-full" style="display: none;"> We report the results of a pilot program for a Green Bank Telescope (GBT) MUSTANG Galactic Plane survey at 3 mm (90 GHz), MGPS90. The survey achieves a typical $1蟽$ depth of $1-2$ mJy beam$^{-1}$ with a 9" beam. We describe the survey parameters, quality assessment process, cataloging, and comparison with other data sets. We have identified 709 sources over seven observed fields selecting some of the most prominent millimeter-bright regions between $0掳< \ell < 50掳$ (total area $\approx 7.5 掳^2$). The majority of these sources have counterparts at other wavelengths. By applying flux selection criteria to these sources, we successfully recovered several known hypercompact HII (HCHII) regions, but did not confirm any new ones. We identify 126 sources that have mm-wavelength counterparts but do not have cm-wavelength counterparts and are therefore candidate HCHII regions; of these, 10 are morphologically compact and are strong candidates for new HCHII regions. Given the limited number of candidates in the extended area in this survey compared to the relatively large numbers seen in protoclusters W51 and W49, it appears that most HCHII regions exist within dense protoclusters. Comparing the counts of HCHII to ultracompact HII (UCHII) regions, we infer the HCHII region lifetime is 16-46% that of the UCHII region lifetime. We additionally separated the 3 mm emission into dust and free-free emission by comparing with archival 870 $渭$m and 20 cm data. In the selected pilot fields, most ($\gtrsim80$%) of the 3 mm emission comes from plasma, either through free-free or synchrotron emission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.09555v2-abstract-full').style.display = 'none'; document.getElementById('2004.09555v2-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 April, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 April, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to ApJS. Data publicly released, with links in paper. Reposted to fix missing figure labels</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1911.09236">arXiv:1911.09236</a> <span> [<a href="https://arxiv.org/pdf/1911.09236">pdf</a>, <a href="https://arxiv.org/format/1911.09236">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/10.1093/mnras/staa2330">10.1093/mnras/staa2330 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Active gas features in three HSC-SSP CAMIRA clusters revealed by high angular resolution analysis of MUSTANG-2 SZE and XXL X-ray observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Okabe%2C+N">Nobuhiro Okabe</a>, <a href="/search/astro-ph?searchtype=author&query=Dicker%2C+S">Simon Dicker</a>, <a href="/search/astro-ph?searchtype=author&query=Eckert%2C+D">Dominique Eckert</a>, <a href="/search/astro-ph?searchtype=author&query=Mroczkowski%2C+T">Tony Mroczkowski</a>, <a href="/search/astro-ph?searchtype=author&query=Gastaldello%2C+F">Fabio Gastaldello</a>, <a href="/search/astro-ph?searchtype=author&query=Lin%2C+Y">Yen-Ting Lin</a>, <a href="/search/astro-ph?searchtype=author&query=Devlin%2C+M">Mark Devlin</a>, <a href="/search/astro-ph?searchtype=author&query=Romero%2C+C+E">Charles E. Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Birkinshaw%2C+M">Mark Birkinshaw</a>, <a href="/search/astro-ph?searchtype=author&query=Sarazin%2C+C">Craig Sarazin</a>, <a href="/search/astro-ph?searchtype=author&query=Horellou%2C+C">Cathy Horellou</a>, <a href="/search/astro-ph?searchtype=author&query=Kitayama%2C+T">Tetsu Kitayama</a>, <a href="/search/astro-ph?searchtype=author&query=Umetsu%2C+K">Keiichi Umetsu</a>, <a href="/search/astro-ph?searchtype=author&query=Sereno%2C+M">Mauro Sereno</a>, <a href="/search/astro-ph?searchtype=author&query=Mason%2C+B+S">Brian S. Mason</a>, <a href="/search/astro-ph?searchtype=author&query=ZuHone%2C+J+A">John A. ZuHone</a>, <a href="/search/astro-ph?searchtype=author&query=Honda%2C+A">Ayaka Honda</a>, <a href="/search/astro-ph?searchtype=author&query=Akamatsu%2C+H">Hiroki Akamatsu</a>, <a href="/search/astro-ph?searchtype=author&query=Chiu%2C+I">I-Non Chiu</a>, <a href="/search/astro-ph?searchtype=author&query=Kohno%2C+K">Kotaro Kohno</a>, <a href="/search/astro-ph?searchtype=author&query=Lin%2C+K">Kai-Yang Lin</a>, <a href="/search/astro-ph?searchtype=author&query=Medezinski%2C+E">Elinor Medezinski</a>, <a href="/search/astro-ph?searchtype=author&query=Miyazaki%2C+S">Satoshi Miyazaki</a>, <a href="/search/astro-ph?searchtype=author&query=Mitsuishi%2C+I">Ikuyuki Mitsuishi</a>, <a href="/search/astro-ph?searchtype=author&query=Nishizawa%2C+A+J">Atsushi J. Nishizawa</a> , et al. (11 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1911.09236v2-abstract-short" style="display: inline;"> We present results from simultaneous modeling of high angular resolution GBT/MUSTANG-2 90 GHz Sunyaev-Zel'dovich effect (SZE) measurements and XMM-XXL X-ray images of three rich galaxy clusters selected from the HSC-SSP Survey. The combination of high angular resolution SZE and X-ray imaging enables a spatially resolved multi-component analysis, which is crucial to understand complex distributions… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.09236v2-abstract-full').style.display = 'inline'; document.getElementById('1911.09236v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1911.09236v2-abstract-full" style="display: none;"> We present results from simultaneous modeling of high angular resolution GBT/MUSTANG-2 90 GHz Sunyaev-Zel'dovich effect (SZE) measurements and XMM-XXL X-ray images of three rich galaxy clusters selected from the HSC-SSP Survey. The combination of high angular resolution SZE and X-ray imaging enables a spatially resolved multi-component analysis, which is crucial to understand complex distributions of cluster gas properties. The targeted clusters have similar optical richnesses and redshifts, but exhibit different dynamical states in their member galaxy distributions: a single-peaked cluster, a double-peaked cluster, and a cluster belonging to a supercluster. A large-scale residual pattern in both regular Compton-parameter $y$ and X-ray surface brightness distributions is found in the single-peaked cluster, indicating a sloshing mode. The double-peaked cluster shows an X-ray remnant cool core between two SZE peaks associated with galaxy concentrations. The temperatures of the two peaks reach $\sim20-30$ keV in contrast to the cool core component of $\sim2$ keV, indicating a violent merger. The main SZE signal for the supercluster is elongated along a direction perpendicular to the major axis of the X-ray core, suggesting a minor merger before core passage. The $S_X$ and $y$ distributions are thus perturbed at some level, regardless of the optical properties. We find that the integrated Compton $y$ parameter and the temperature for the major merger are boosted from those expected by the weak-lensing mass and those for the other two clusters show no significant deviations, which is consistent with predictions of numerical simulations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.09236v2-abstract-full').style.display = 'none'; document.getElementById('1911.09236v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 August, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 November, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">36 pages, 25 figures, 5 tables; accepted for the 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/1908.09200">arXiv:1908.09200</a> <span> [<a href="https://arxiv.org/pdf/1908.09200">pdf</a>, <a href="https://arxiv.org/format/1908.09200">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/10.3847/1538-4357/ab6d70">10.3847/1538-4357/ab6d70 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Pressure profiles and mass estimates using high-resolution Sunyaev-Zel'dovich effect observations of Zwicky 3146 with MUSTANG-2 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Romero%2C+C+E">Charles E. Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Sievers%2C+J">Jonathan Sievers</a>, <a href="/search/astro-ph?searchtype=author&query=Ghirardini%2C+V">Vittorio Ghirardini</a>, <a href="/search/astro-ph?searchtype=author&query=Dicker%2C+S">Simon Dicker</a>, <a href="/search/astro-ph?searchtype=author&query=Giacintucci%2C+S">Simona Giacintucci</a>, <a href="/search/astro-ph?searchtype=author&query=Mroczkowski%2C+T">Tony Mroczkowski</a>, <a href="/search/astro-ph?searchtype=author&query=Mason%2C+B+S">Brian S. Mason</a>, <a href="/search/astro-ph?searchtype=author&query=Sarazin%2C+C">Craig Sarazin</a>, <a href="/search/astro-ph?searchtype=author&query=Devlin%2C+M">Mark Devlin</a>, <a href="/search/astro-ph?searchtype=author&query=Gaspari%2C+M">Massimo Gaspari</a>, <a href="/search/astro-ph?searchtype=author&query=Battaglia%2C+N">Nicholas Battaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Hilton%2C+M">Matthew Hilton</a>, <a href="/search/astro-ph?searchtype=author&query=Bulbul%2C+E">Esra Bulbul</a>, <a href="/search/astro-ph?searchtype=author&query=Lowe%2C+I">Ian Lowe</a>, <a href="/search/astro-ph?searchtype=author&query=Stanchfield%2C+S">Sara Stanchfield</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="1908.09200v1-abstract-short" style="display: inline;"> The galaxy cluster Zwicky 3146 is a sloshing cool core cluster at $z=0.291$ that in X-ray imaging does not appear to exhibit significant pressure substructure in the intracluster medium (ICM). The published $M_{500}$ values range between $3.88^{+0.62}_{-0.58}$ to $22.50 \pm 7.58 \times 10^{14}$ M$_{\odot}$, where ICM-based estimates with reported errors $<20$\% suggest that we should expect to fin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.09200v1-abstract-full').style.display = 'inline'; document.getElementById('1908.09200v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1908.09200v1-abstract-full" style="display: none;"> The galaxy cluster Zwicky 3146 is a sloshing cool core cluster at $z=0.291$ that in X-ray imaging does not appear to exhibit significant pressure substructure in the intracluster medium (ICM). The published $M_{500}$ values range between $3.88^{+0.62}_{-0.58}$ to $22.50 \pm 7.58 \times 10^{14}$ M$_{\odot}$, where ICM-based estimates with reported errors $<20$\% suggest that we should expect to find a mass between $6.53^{+0.44}_{-0.44} \times 10^{14}$ M$_{\odot}$ (from Planck, with an $8.4蟽$ detection) and $8.52^{+1.77}_{-1.47} \times 10^{14}$ M$_{\odot}$ (from ACT, with a $14蟽$ detection). This broad range of masses is suggestive that there is ample room for improvement for all methods. Here, we investigate the ability to estimate the mass of Zwicky 3146 via the Sunyaev-Zel'dovich (SZ) effect with data taken at 90 GHz by MUSTANG-2 to a noise level better than $15\ 渭$K at the center, and a cluster detection of $104蟽$. We derive a pressure profile from our SZ data which is in excellent agreement with that derived from X-ray data. From our SZ-derived pressure profiles, we infer $M_{500}$ and $M_{2500}$ via three methods -- $Y$-$M$ scaling relations, the virial theorem, and hydrostatic equilibrium -- where we employ X-ray constraints from \emph{XMM-Newton} on the electron density profile when assuming hydrostatic equilibrium. Depending on the model and estimation method, our $M_{500}$ estimates range from $6.23 \pm 0.59$ to $10.6 \pm 0.95 \times 10^{14}$ M$_{\odot}$, where our estimate from hydrostatic equilibrium, is $8.29^{+1.93}_{-1.24}$ ($\pm 19.1$\% stat) ${}^{+0.74}_{-0.68}$ ($\pm 8.6$\% sys, calibration) $\times 10^{14}$ M$_{\odot}$. Our fiducial mass, derived from a $Y$-$M$ relation is $8.16^{+0.44}_{-0.54}$ ($\pm 5.5$\% stat) ${}^{+0.46}_{-0.43}$ ($\pm 5.5$\% sys, $Y$-$M$) ${}^{+0.59}_{-0.55}$ ($\pm 7.0$\% sys, cal.) $\times 10^{14}$ M$_{\odot}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.09200v1-abstract-full').style.display = 'none'; document.getElementById('1908.09200v1-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 August, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">24 pages, 16 figures; submitted to ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2020 ApJ, 891, 90 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1905.05221">arXiv:1905.05221</a> <span> [<a href="https://arxiv.org/pdf/1905.05221">pdf</a>, <a href="https://arxiv.org/format/1905.05221">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/ab734a">10.3847/1538-4357/ab734a <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Confirmation of Enhanced Long Wavelength Dust Emission in OMC 2/3 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mason%2C+B">Brian Mason</a>, <a href="/search/astro-ph?searchtype=author&query=Dicker%2C+S">Simon Dicker</a>, <a href="/search/astro-ph?searchtype=author&query=Sadavoy%2C+S">Sarah Sadavoy</a>, <a href="/search/astro-ph?searchtype=author&query=Stanchfield%2C+S">Sara Stanchfield</a>, <a href="/search/astro-ph?searchtype=author&query=Mroczkowski%2C+T">Tony Mroczkowski</a>, <a href="/search/astro-ph?searchtype=author&query=Romero%2C+C">Charles Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Friesen%2C+R">Rachel Friesen</a>, <a href="/search/astro-ph?searchtype=author&query=Sarazin%2C+C">Craig Sarazin</a>, <a href="/search/astro-ph?searchtype=author&query=Sievers%2C+J">Jonathan Sievers</a>, <a href="/search/astro-ph?searchtype=author&query=Stanke%2C+T">Thomas Stanke</a>, <a href="/search/astro-ph?searchtype=author&query=Devlin%2C+M">Mark Devlin</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1905.05221v2-abstract-short" style="display: inline;"> Previous continuum observations from the MUSTANG camera on the Green Bank Telescope (GBT) of the nearby star-forming filament OMC 2/3 found elevated emission at 3.3 mm relative to shorter wavelength data. As a consequence, the inferred dust emissivity index obtained from modified black body dust spectra was considerably lower than what is typically measured on $\sim 0.1 \, {\rm pc}$ scales in near… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.05221v2-abstract-full').style.display = 'inline'; document.getElementById('1905.05221v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1905.05221v2-abstract-full" style="display: none;"> Previous continuum observations from the MUSTANG camera on the Green Bank Telescope (GBT) of the nearby star-forming filament OMC 2/3 found elevated emission at 3.3 mm relative to shorter wavelength data. As a consequence, the inferred dust emissivity index obtained from modified black body dust spectra was considerably lower than what is typically measured on $\sim 0.1 \, {\rm pc}$ scales in nearby molecular clouds. Here we present new observations of OMC 2/3 collected with the MUSTANG-2 camera on the GBT which confirm this elevated emission. We also present for the first time sensitive 1 cm observations made with the Ka-band receiver on the GBT which also show higher than expected emission. We use these observations--- along with Herschel, JCMT, Mambo, and GISMO data--- to assemble spectral energy distributions (SEDs) of a variety of structures in OMC 2/3 spanning the range $160 \, {\rm 渭m}$ to $1 \, {\rm cm}$. The data at 2 mm and shorter are generally consistent with a modified black body spectrum and a single value of $尾\sim 1.6$. The 3 mm and 1 cm data, however, lie well above such an SED. The spectrum of the long wavelength excess is inconsistent with both free-free emission and standard "Spinning Dust" models for Anomalous Microwave Emission (AME). The 3 mm and 1 cm data could be explained by a flatter dust emissivity at wavelengths shorter than 2 mm, potentially in concert with AME in some regions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.05221v2-abstract-full').style.display = 'none'; document.getElementById('1905.05221v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 February, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 May, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 8 figures, ApJ (in press)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2020 ApJ 893 13 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1903.03481">arXiv:1903.03481</a> <span> [<a href="https://arxiv.org/pdf/1903.03481">pdf</a>, <a href="https://arxiv.org/format/1903.03481">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ab0e7f">10.3847/1538-4357/ab0e7f <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MESAS Project: Long wavelength follow-up observations of Sirius A </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=White%2C+J+A">Jacob Aaron White</a>, <a href="/search/astro-ph?searchtype=author&query=Aufdenberg%2C+J">Jason Aufdenberg</a>, <a href="/search/astro-ph?searchtype=author&query=Boley%2C+A+C">Aaron C. Boley</a>, <a href="/search/astro-ph?searchtype=author&query=Devlin%2C+M">Mark Devlin</a>, <a href="/search/astro-ph?searchtype=author&query=Hauschildt%2C+P">Peter Hauschildt</a>, <a href="/search/astro-ph?searchtype=author&query=Hughes%2C+A+G">Anna G. Hughes</a>, <a href="/search/astro-ph?searchtype=author&query=Hughes%2C+A+M">A. Meredith Hughes</a>, <a href="/search/astro-ph?searchtype=author&query=Mason%2C+B">Brian Mason</a>, <a href="/search/astro-ph?searchtype=author&query=Matthews%2C+B">Brenda Matthews</a>, <a href="/search/astro-ph?searchtype=author&query=Mo%C3%B3r%2C+A">Attila Mo贸r</a>, <a href="/search/astro-ph?searchtype=author&query=Mroczkowski%2C+T">Tony Mroczkowski</a>, <a href="/search/astro-ph?searchtype=author&query=Romero%2C+C">Charles Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Sievers%2C+J">Jonathan Sievers</a>, <a href="/search/astro-ph?searchtype=author&query=Stanchfield%2C+S">Sara Stanchfield</a>, <a href="/search/astro-ph?searchtype=author&query=Tapia%2C+F">Francisco Tapia</a>, <a href="/search/astro-ph?searchtype=author&query=Wilner%2C+D+J">David J. Wilner</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="1903.03481v1-abstract-short" style="display: inline;"> Modeling the submillimeter to centimeter emission of stars is challenging due to a lack of sensitive observations at these long wavelengths. We launched an ongoing campaign to obtain new observations entitled Measuring the Emission of Stellar Atmospheres at Submillimeter/millimeter wavelengths (MESAS). Here we present ALMA, GBT, and VLA observations of Sirius A, the closest main-sequence A-type st… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.03481v1-abstract-full').style.display = 'inline'; document.getElementById('1903.03481v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1903.03481v1-abstract-full" style="display: none;"> Modeling the submillimeter to centimeter emission of stars is challenging due to a lack of sensitive observations at these long wavelengths. We launched an ongoing campaign to obtain new observations entitled Measuring the Emission of Stellar Atmospheres at Submillimeter/millimeter wavelengths (MESAS). Here we present ALMA, GBT, and VLA observations of Sirius A, the closest main-sequence A-type star, that span from 1.4 to 9.0 millimeters. These observations complement our previous millimeter data on Sirius A and are entirely consistent with the PHOENIX stellar atmosphere models constructed to explain them. We note that accurate models of long wavelength emission from stars are essential not only to understand fundamental stellar processes, but also to determine the presence of dusty debris in spatially unresolved observations of circumstellar disks. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.03481v1-abstract-full').style.display = 'none'; document.getElementById('1903.03481v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 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">7 pages, 1 figure, 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/1901.02476">arXiv:1901.02476</a> <span> [<a href="https://arxiv.org/pdf/1901.02476">pdf</a>, <a href="https://arxiv.org/format/1901.02476">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201833385">10.1051/0004-6361/201833385 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Dust opacity variations in the pre-stellar core L1544 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chacon-Tanarro%2C+A">A. Chacon-Tanarro</a>, <a href="/search/astro-ph?searchtype=author&query=Pineda%2C+J+E">J. E. Pineda</a>, <a href="/search/astro-ph?searchtype=author&query=Caselli%2C+P">P. Caselli</a>, <a href="/search/astro-ph?searchtype=author&query=Bizzocchi%2C+L">L. Bizzocchi</a>, <a href="/search/astro-ph?searchtype=author&query=Gutermuth%2C+R+A">R. A. Gutermuth</a>, <a href="/search/astro-ph?searchtype=author&query=Mason%2C+B+S">B. S. Mason</a>, <a href="/search/astro-ph?searchtype=author&query=Gomez-Ruiz%2C+A+I">A. I. Gomez-Ruiz</a>, <a href="/search/astro-ph?searchtype=author&query=Harju%2C+J">J. Harju</a>, <a href="/search/astro-ph?searchtype=author&query=Devlin%2C+M">M. Devlin</a>, <a href="/search/astro-ph?searchtype=author&query=Dicker%2C+S+R">S. R. Dicker</a>, <a href="/search/astro-ph?searchtype=author&query=Mroczkowski%2C+T">T. Mroczkowski</a>, <a href="/search/astro-ph?searchtype=author&query=Romero%2C+C+E">C. E. Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Sievers%2C+J">J. Sievers</a>, <a href="/search/astro-ph?searchtype=author&query=Stanchfield%2C+S">S. Stanchfield</a>, <a href="/search/astro-ph?searchtype=author&query=Offner%2C+S">S. Offner</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez-Arguelles%2C+D">D. Sanchez-Arguelles</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="1901.02476v1-abstract-short" style="display: inline;"> Context: The study of dust emission at millimeter wavelengths is important to shed light on the dust properties and physical structure of pre-stellar cores, the initial conditions in the process of star and planet formation. Aims: Using two new continuum facilities, AzTEC at the LMT and MUSTANG-2 at the GBO, we aim to detect changes in the optical properties of dust grains as a function of radius… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.02476v1-abstract-full').style.display = 'inline'; document.getElementById('1901.02476v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1901.02476v1-abstract-full" style="display: none;"> Context: The study of dust emission at millimeter wavelengths is important to shed light on the dust properties and physical structure of pre-stellar cores, the initial conditions in the process of star and planet formation. Aims: Using two new continuum facilities, AzTEC at the LMT and MUSTANG-2 at the GBO, we aim to detect changes in the optical properties of dust grains as a function of radius for the well-known pre-stellar core L1544. Methods: We determine the emission profiles at 1.1 and 3.3 mm and examine whether they can be reproduced in terms of the current best physical models for L1544. We also make use of various tools to determine the radial distributions of the density, temperature, and the dust opacity in a self-consistent manner. Results: We find that our observations cannot be reproduced without invoking opacity variations. With the new data, new temperature and density profiles, as well as opacity variations across the core, have been derived. The opacity changes are consistent with the expected variations between uncoagulated bare grains, toward the outer regions of the core, and grains with thick ice mantles, toward the core center. A simple analytical grain growth model predicts the presence of grains of ~3-4 um within the central 2000 au for the new density profile. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.02476v1-abstract-full').style.display = 'none'; document.getElementById('1901.02476v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 January, 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">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 623, A118 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1709.03318">arXiv:1709.03318</a> <span> [<a href="https://arxiv.org/pdf/1709.03318">pdf</a>, <a href="https://arxiv.org/format/1709.03318">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"> MERGHERS: An SZ-selected cluster survey with MeerKAT </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Knowles%2C+K">Kenda Knowles</a>, <a href="/search/astro-ph?searchtype=author&query=Baker%2C+A">Andrew Baker</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+K">Kaustuv Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Bharadwaj%2C+V">Vijaysarathi Bharadwaj</a>, <a href="/search/astro-ph?searchtype=author&query=Deane%2C+R">Roger Deane</a>, <a href="/search/astro-ph?searchtype=author&query=Devlin%2C+M">Mark Devlin</a>, <a href="/search/astro-ph?searchtype=author&query=Dicker%2C+S">Simon Dicker</a>, <a href="/search/astro-ph?searchtype=author&query=de+Gasperin%2C+F">Francesco de Gasperin</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrari%2C+C">Chiara Ferrari</a>, <a href="/search/astro-ph?searchtype=author&query=Hilton%2C+M">Matt Hilton</a>, <a href="/search/astro-ph?searchtype=author&query=Hughes%2C+J+P">John P. Hughes</a>, <a href="/search/astro-ph?searchtype=author&query=Intema%2C+H+T">Huib T. Intema</a>, <a href="/search/astro-ph?searchtype=author&query=Makhathini%2C+S">Sphesihle Makhathini</a>, <a href="/search/astro-ph?searchtype=author&query=Moodley%2C+K">Kavilan Moodley</a>, <a href="/search/astro-ph?searchtype=author&query=Oozeer%2C+N">Nadeem Oozeer</a>, <a href="/search/astro-ph?searchtype=author&query=Pfrommer%2C+C">Christoph Pfrommer</a>, <a href="/search/astro-ph?searchtype=author&query=Sievers%2C+J">Jonathan Sievers</a>, <a href="/search/astro-ph?searchtype=author&query=Sikhosana%2C+S+P">Sinenhlanhla P. Sikhosana</a>, <a href="/search/astro-ph?searchtype=author&query=Smirnov%2C+O">Oleg Smirnov</a>, <a href="/search/astro-ph?searchtype=author&query=Sommer%2C+M+W">Martin W. Sommer</a>, <a href="/search/astro-ph?searchtype=author&query=Stanchfield%2C+S">Sara Stanchfield</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Heyden%2C+K">Kurt van der Heyden</a>, <a href="/search/astro-ph?searchtype=author&query=Zwart%2C+J+T+L">Jonathan T. L. Zwart</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="1709.03318v1-abstract-short" style="display: inline;"> The MeerKAT telescope will be one of the most sensitive radio arrays in the pre-SKA era. Here we discuss a low-frequency SZ-selected cluster survey with MeerKAT, the MeerKAT Extended Relics, Giant Halos, and Extragalactic Radio Sources (MERGHERS) survey. The primary goal of this survey is to detect faint signatures of diffuse cluster emission, specifically radio halos and relics. SZ-selected clust… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1709.03318v1-abstract-full').style.display = 'inline'; document.getElementById('1709.03318v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1709.03318v1-abstract-full" style="display: none;"> The MeerKAT telescope will be one of the most sensitive radio arrays in the pre-SKA era. Here we discuss a low-frequency SZ-selected cluster survey with MeerKAT, the MeerKAT Extended Relics, Giant Halos, and Extragalactic Radio Sources (MERGHERS) survey. The primary goal of this survey is to detect faint signatures of diffuse cluster emission, specifically radio halos and relics. SZ-selected cluster samples offer a homogeneous, mass-limited set of targets out to higher redshift than X-ray samples. MeerKAT is sensitive enough to detect diffuse radio emission at the faint levels expected in low-mass and high-redshift clusters, thereby enabling radio halo and relic formation theories to be tested with a larger statistical sample over a significantly expanded phase space. Complementary multiwavelength follow-up observations will provide a more complete picture of any clusters found to host diffuse emission, thereby enhancing the scientific return of the MERGHERS survey. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1709.03318v1-abstract-full').style.display = 'none'; document.getElementById('1709.03318v1-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 September, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">12 pages, 3 figures, proceedings from MeerKAT Science: On the Pathway to the SKA, 25-27 May, 2016</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1409.7084">arXiv:1409.7084</a> <span> [<a href="https://arxiv.org/pdf/1409.7084">pdf</a>, <a href="https://arxiv.org/format/1409.7084">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1142/S2251171714400017">10.1142/S2251171714400017 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Next Generation BLAST Experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Galitzki%2C+N">Nicholas Galitzki</a>, <a href="/search/astro-ph?searchtype=author&query=Ade%2C+P+A+R">Peter A. R. Ade</a>, <a href="/search/astro-ph?searchtype=author&query=Angil%C3%A8%2C+F+E">Francesco E. Angil猫</a>, <a href="/search/astro-ph?searchtype=author&query=Ashton%2C+P">Peter Ashton</a>, <a href="/search/astro-ph?searchtype=author&query=Beall%2C+J+A">James A. Beall</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+D">Dan Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Bradford%2C+K+J">Kristi J. Bradford</a>, <a href="/search/astro-ph?searchtype=author&query=Che%2C+G">George Che</a>, <a href="/search/astro-ph?searchtype=author&query=Cho%2C+H">Hsiao-Mei Cho</a>, <a href="/search/astro-ph?searchtype=author&query=Devlin%2C+M+J">Mark J. Devlin</a>, <a href="/search/astro-ph?searchtype=author&query=Dober%2C+B+J">Bradley J. Dober</a>, <a href="/search/astro-ph?searchtype=author&query=Fissel%2C+L+M">Laura M. Fissel</a>, <a href="/search/astro-ph?searchtype=author&query=Fukui%2C+Y">Yasuo Fukui</a>, <a href="/search/astro-ph?searchtype=author&query=Gao%2C+J">Jiansong Gao</a>, <a href="/search/astro-ph?searchtype=author&query=Groppi%2C+C+E">Christopher E. Groppi</a>, <a href="/search/astro-ph?searchtype=author&query=Hillbrand%2C+S">Seth Hillbrand</a>, <a href="/search/astro-ph?searchtype=author&query=Hilton%2C+G+C">Gene C. Hilton</a>, <a href="/search/astro-ph?searchtype=author&query=Hubmayr%2C+J">Johannes Hubmayr</a>, <a href="/search/astro-ph?searchtype=author&query=Irwin%2C+K+D">Kent D. Irwin</a>, <a href="/search/astro-ph?searchtype=author&query=Klein%2C+J">Jeffrey Klein</a>, <a href="/search/astro-ph?searchtype=author&query=Van+Lanen%2C+J">Jeff Van Lanen</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+D">Dale Li</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Z">Zhi-Yun Li</a>, <a href="/search/astro-ph?searchtype=author&query=Lourie%2C+N+P">Nathan P. Lourie</a>, <a href="/search/astro-ph?searchtype=author&query=Mani%2C+H">Hamdi Mani</a> , et al. (16 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1409.7084v2-abstract-short" style="display: inline;"> The Balloon-borne Large Aperture Submillimeter Telescope for Polarimetry (BLASTPol) was a suborbital experiment designed to map magnetic fields in order to study their role in star formation processes. BLASTPol made detailed polarization maps of a number of molecular clouds during its successful flights from Antarctica in 2010 and 2012. We present the next-generation BLASTPol instrument (BLAST-TNG… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1409.7084v2-abstract-full').style.display = 'inline'; document.getElementById('1409.7084v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1409.7084v2-abstract-full" style="display: none;"> The Balloon-borne Large Aperture Submillimeter Telescope for Polarimetry (BLASTPol) was a suborbital experiment designed to map magnetic fields in order to study their role in star formation processes. BLASTPol made detailed polarization maps of a number of molecular clouds during its successful flights from Antarctica in 2010 and 2012. We present the next-generation BLASTPol instrument (BLAST-TNG) that will build off the success of the previous experiment and continue its role as a unique instrument and a test bed for new technologies. With a 16-fold increase in mapping speed, BLAST-TNG will make larger and deeper maps. Major improvements include a 2.5 m carbon fiber mirror that is 40% wider than the BLASTPol mirror and ~3000 polarization sensitive detectors. BLAST-TNG will observe in three bands at 250, 350, and 500 microns. The telescope will serve as a pathfinder project for microwave kinetic inductance detector (MKID) technology, as applied to feedhorn coupled submillimeter detector arrays. The liquid helium cooled cryostat will have a 28-day hold time and will utilize a closed-cycle $^3$He refrigerator to cool the detector arrays to 270 mK. This will enable a detailed mapping of more targets with higher polarization resolution than any other submillimeter experiment to date. BLAST-TNG will also be the first balloon-borne telescope to offer shared risk observing time to the community. This paper outlines the motivation for the project and the instrumental design. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1409.7084v2-abstract-full').style.display = 'none'; document.getElementById('1409.7084v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 November, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 September, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Journal of Astronomical Instrumentation, Vol. 3, No. 2 (2014) 1440001 (16 pages) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1407.3756">arXiv:1407.3756</a> <span> [<a href="https://arxiv.org/pdf/1407.3756">pdf</a>, <a href="https://arxiv.org/format/1407.3756">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1117/12.2054419">10.1117/12.2054419 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The next-generation BLASTPol experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dober%2C+B">Bradley Dober</a>, <a href="/search/astro-ph?searchtype=author&query=Ade%2C+P+A+R">Peter A. R. Ade</a>, <a href="/search/astro-ph?searchtype=author&query=Ashton%2C+P">Peter Ashton</a>, <a href="/search/astro-ph?searchtype=author&query=Angil%C3%A8%2C+F+E">Francesco E. Angil猫</a>, <a href="/search/astro-ph?searchtype=author&query=Beall%2C+J+A">James A. Beall</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+D">Dan Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Bradford%2C+K+J">Kristi J. Bradford</a>, <a href="/search/astro-ph?searchtype=author&query=Che%2C+G">George Che</a>, <a href="/search/astro-ph?searchtype=author&query=Cho%2C+H">Hsiao-Mei Cho</a>, <a href="/search/astro-ph?searchtype=author&query=Devlin%2C+M+J">Mark J. Devlin</a>, <a href="/search/astro-ph?searchtype=author&query=Fissel%2C+L+M">Laura M. Fissel</a>, <a href="/search/astro-ph?searchtype=author&query=Fukui%2C+Y">Yasuo Fukui</a>, <a href="/search/astro-ph?searchtype=author&query=Galitzki%2C+N">Nicholas Galitzki</a>, <a href="/search/astro-ph?searchtype=author&query=Gao%2C+J">Jiansong Gao</a>, <a href="/search/astro-ph?searchtype=author&query=Groppi%2C+C+E">Christopher E. Groppi</a>, <a href="/search/astro-ph?searchtype=author&query=Hillbrand%2C+S">Seth Hillbrand</a>, <a href="/search/astro-ph?searchtype=author&query=Hilton%2C+G+C">Gene C. Hilton</a>, <a href="/search/astro-ph?searchtype=author&query=Hubmayr%2C+J">Johannes Hubmayr</a>, <a href="/search/astro-ph?searchtype=author&query=Irwin%2C+K+D">Kent D. Irwin</a>, <a href="/search/astro-ph?searchtype=author&query=Klein%2C+J">Jeffrey Klein</a>, <a href="/search/astro-ph?searchtype=author&query=Van+Lanen%2C+J">Jeff Van Lanen</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+D">Dale Li</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Z">Zhi-Yun Li</a>, <a href="/search/astro-ph?searchtype=author&query=Lourie%2C+N+P">Nathan P. Lourie</a>, <a href="/search/astro-ph?searchtype=author&query=Mani%2C+H">Hamdi Mani</a> , et al. (14 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1407.3756v1-abstract-short" style="display: inline;"> The Balloon-borne Large Aperture Submillimeter Telescope for Polarimetry (BLASTPol) is a suborbital mapping experiment designed to study the role magnetic fields play in star formation. BLASTPol has had two science flights from McMurdo Station, Antarctica in 2010 and 2012. These flights have produced thousands of polarization vectors at 250, 350 and 500 microns in several molecular cloud targets.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1407.3756v1-abstract-full').style.display = 'inline'; document.getElementById('1407.3756v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1407.3756v1-abstract-full" style="display: none;"> The Balloon-borne Large Aperture Submillimeter Telescope for Polarimetry (BLASTPol) is a suborbital mapping experiment designed to study the role magnetic fields play in star formation. BLASTPol has had two science flights from McMurdo Station, Antarctica in 2010 and 2012. These flights have produced thousands of polarization vectors at 250, 350 and 500 microns in several molecular cloud targets. We present the design, specifications, and progress towards the next-generation BLASTPol experiment (BLAST-TNG). BLAST-TNG will fly a 40% larger diameter primary mirror, with almost 8 times the number of polarization-sensitive detectors resulting in a factor of 16 increase in mapping speed. With a spatial resolution of 22 arcseconds and four times the field of view of BLASTPol, BLAST-TNG will bridge the angular scales between Planck's low resolution all-sky maps and ALMA's ultra-high resolution narrow fields. The new receiver has a larger cryogenics volume, allowing for a 28 day hold time. BLAST-TNG employs three arrays of Microwave Kinetic Inductance Detectors (MKIDs) with 30% fractional bandwidth at 250, 350 and 500 microns. In this paper, we will present the new BLAST-TNG instrument and science objectives. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1407.3756v1-abstract-full').style.display = 'none'; document.getElementById('1407.3756v1-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 July, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 6 figures. Presented at SPIE Ground-based and Airborne Telescopes V, June 23, 2014. To be published in Proceedings of SPIE Volume 9145</span> </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg> <a href="https://info.arxiv.org/help/contact.html"> Contact</a> </li> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>subscribe to arXiv mailings</title><desc>Click here to subscribe</desc><path d="M476 3.2L12.5 270.6c-18.1 10.4-15.8 35.6 2.2 43.2L121 358.4l287.3-253.2c5.5-4.9 13.3 2.6 8.6 8.3L176 407v80.5c0 23.6 28.5 32.9 42.5 15.8L282 426l124.6 52.2c14.2 6 30.4-2.9 33-18.2l72-432C515 7.8 493.3-6.8 476 3.2z"/></svg> <a href="https://info.arxiv.org/help/subscribe"> Subscribe</a> </li> </ul> </div> </div> </div>   <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/license/index.html">Copyright</a></li> <li><a href="https://info.arxiv.org/help/policies/privacy_policy.html">Privacy Policy</a></li> </ul> </div> <div class="column sorry-app-links"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/web_accessibility.html">Web Accessibility Assistance</a></li> <li> <p class="help"> <a class="a11y-main-link" href="https://status.arxiv.org" target="_blank">arXiv Operational Status <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 256 512" class="icon filter-dark_grey" role="presentation"><path d="M224.3 273l-136 136c-9.4 9.4-24.6 9.4-33.9 0l-22.6-22.6c-9.4-9.4-9.4-24.6 0-33.9l96.4-96.4-96.4-96.4c-9.4-9.4-9.4-24.6 0-33.9L54.3 103c9.4-9.4 24.6-9.4 33.9 0l136 136c9.5 9.4 9.5 24.6.1 34z"/></svg></a><br> Get status notifications via <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/email/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg>email</a> or <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/slack/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 448 512" class="icon filter-black" role="presentation"><path d="M94.12 315.1c0 25.9-21.16 47.06-47.06 47.06S0 341 0 315.1c0-25.9 21.16-47.06 47.06-47.06h47.06v47.06zm23.72 0c0-25.9 21.16-47.06 47.06-47.06s47.06 21.16 47.06 47.06v117.84c0 25.9-21.16 47.06-47.06 47.06s-47.06-21.16-47.06-47.06V315.1zm47.06-188.98c-25.9 0-47.06-21.16-47.06-47.06S139 32 164.9 32s47.06 21.16 47.06 47.06v47.06H164.9zm0 23.72c25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06H47.06C21.16 243.96 0 222.8 0 196.9s21.16-47.06 47.06-47.06H164.9zm188.98 47.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06h-47.06V196.9zm-23.72 0c0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06V79.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06V196.9zM283.1 385.88c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06v-47.06h47.06zm0-23.72c-25.9 0-47.06-21.16-47.06-47.06 0-25.9 21.16-47.06 47.06-47.06h117.84c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06H283.1z"/></svg>slack</a> </p> </li> </ul> </div> </div> </div>  </div> </footer> <script src="https://static.arxiv.org/static/base/1.0.0a5/js/member_acknowledgement.js"></script> </body> </html>

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