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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/2410.19985">arXiv:2410.19985</a> <span> [<a href="https://arxiv.org/pdf/2410.19985">pdf</a>, <a href="https://arxiv.org/format/2410.19985">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 Galaxy Zoo Catalogs for the Galaxy And Mass Assembly (GAMA) Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B+W">Benne W. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Robertson%2C+C">Clayton Robertson</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+K">Kyle Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Pimbblet%2C+K+A">Kevin A. Pimbblet</a>, <a href="/search/astro-ph?searchtype=author&query=Casura%2C+S">Sarah Casura</a>, <a href="/search/astro-ph?searchtype=author&query=Sansom%2C+A+E">Anne E. Sansom</a>, <a href="/search/astro-ph?searchtype=author&query=Patel%2C+D">Divya Patel</a>, <a href="/search/astro-ph?searchtype=author&query=Butrum%2C+T">Trevor Butrum</a>, <a href="/search/astro-ph?searchtype=author&query=Glass%2C+D+H+W">David H. W. Glass</a>, <a href="/search/astro-ph?searchtype=author&query=Kelvin%2C+L">Lee Kelvin</a>, <a href="/search/astro-ph?searchtype=author&query=Baldry%2C+I+K">Ivan K. Baldry</a>, <a href="/search/astro-ph?searchtype=author&query=De+Propris%2C+R">Roberto De Propris</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S">Steven Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Masters%2C+K">Karen Masters</a>, <a href="/search/astro-ph?searchtype=author&query=Stone%2C+M">Maria Stone</a>, <a href="/search/astro-ph?searchtype=author&query=Hardin%2C+T">Tim Hardin</a>, <a href="/search/astro-ph?searchtype=author&query=Walmsley%2C+M">Mike Walmsley</a>, <a href="/search/astro-ph?searchtype=author&query=Liske%2C+J">Jochen Liske</a>, <a href="/search/astro-ph?searchtype=author&query=Adnan%2C+S+M+R">S M Rafee Adnan</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="2410.19985v1-abstract-short" style="display: inline;"> Galaxy Zoo is an online project to classify morphological features in extra-galactic imaging surveys with public voting. In this paper, we compare the classifications made for two different surveys, the Dark Energy Spectroscopic Instrument (DESI) imaging survey and a part of the Kilo-Degree Survey (KiDS), in the equatorial fields of the Galaxy And Mass Assembly (GAMA) survey. Our aim is to cross-v… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.19985v1-abstract-full').style.display = 'inline'; document.getElementById('2410.19985v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.19985v1-abstract-full" style="display: none;"> Galaxy Zoo is an online project to classify morphological features in extra-galactic imaging surveys with public voting. In this paper, we compare the classifications made for two different surveys, the Dark Energy Spectroscopic Instrument (DESI) imaging survey and a part of the Kilo-Degree Survey (KiDS), in the equatorial fields of the Galaxy And Mass Assembly (GAMA) survey. Our aim is to cross-validate and compare the classifications based on different imaging quality and depth. We find that generally the voting agrees globally but with substantial scatter i.e. substantial differences for individual galaxies. There is a notable higher voting fraction in favor of ``smooth'' galaxies in the DESI+\rev{\sc zoobot} classifications, most likely due to the difference between imaging depth. DESI imaging is shallower and slightly lower resolution than KiDS and the Galaxy Zoo images do not reveal details such as disk features \rev{and thus are missed in the {\sc zoobot} training sample}. \rev{We check against expert visual classifications and find good agreement with KiDS-based Galaxy Zoo voting.} We reproduce the results from Porter-Temple+ (2022), on the dependence of stellar mass, star-formation, and specific star-formation on the number of spiral arms. This shows that once corrected for redshift, the DESI Galaxy Zoo and KiDS Galaxy Zoo classifications agree well on population properties. The zoobot cross-validation increases confidence in its ability to compliment Galaxy Zoo classifications and its ability for transfer learning across surveys. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.19985v1-abstract-full').style.display = 'none'; document.getElementById('2410.19985v1-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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, 22 figures, 8 tables, accepted for publication in PASA</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.13503">arXiv:2405.13503</a> <span> [<a href="https://arxiv.org/pdf/2405.13503">pdf</a>, <a href="https://arxiv.org/format/2405.13503">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Euclid: Early Release Observations -- The intracluster light and intracluster globular clusters of the Perseus cluster </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kluge%2C+M">M. Kluge</a>, <a href="/search/astro-ph?searchtype=author&query=Hatch%2C+N+A">N. A. Hatch</a>, <a href="/search/astro-ph?searchtype=author&query=Montes%2C+M">M. Montes</a>, <a href="/search/astro-ph?searchtype=author&query=Golden-Marx%2C+J+B">J. B. Golden-Marx</a>, <a href="/search/astro-ph?searchtype=author&query=Gonzalez%2C+A+H">A. H. Gonzalez</a>, <a href="/search/astro-ph?searchtype=author&query=Cuillandre%2C+J+-">J. -C. Cuillandre</a>, <a href="/search/astro-ph?searchtype=author&query=Bolzonella%2C+M">M. Bolzonella</a>, <a href="/search/astro-ph?searchtype=author&query=Lan%C3%A7on%2C+A">A. Lan莽on</a>, <a href="/search/astro-ph?searchtype=author&query=Laureijs%2C+R">R. Laureijs</a>, <a href="/search/astro-ph?searchtype=author&query=Saifollahi%2C+T">T. Saifollahi</a>, <a href="/search/astro-ph?searchtype=author&query=Schirmer%2C+M">M. Schirmer</a>, <a href="/search/astro-ph?searchtype=author&query=Stone%2C+C">C. Stone</a>, <a href="/search/astro-ph?searchtype=author&query=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=Sorce%2C+J+G">J. G. Sorce</a>, <a href="/search/astro-ph?searchtype=author&query=Marleau%2C+F+R">F. R. Marleau</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P+-">P. -A. Duc</a>, <a href="/search/astro-ph?searchtype=author&query=Sola%2C+E">E. Sola</a>, <a href="/search/astro-ph?searchtype=author&query=Urbano%2C+M">M. Urbano</a>, <a href="/search/astro-ph?searchtype=author&query=Ahad%2C+S+L">S. L. Ahad</a>, <a href="/search/astro-ph?searchtype=author&query=Bah%C3%A9%2C+Y+M">Y. M. Bah茅</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S+P">S. P. Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Bellhouse%2C+C">C. Bellhouse</a>, <a href="/search/astro-ph?searchtype=author&query=Buitrago%2C+F">F. Buitrago</a>, <a href="/search/astro-ph?searchtype=author&query=Dimauro%2C+P">P. Dimauro</a> , et al. (163 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.13503v2-abstract-short" style="display: inline;"> We study the intracluster light (ICL) and intracluster globular clusters (ICGCs) in the nearby Perseus galaxy cluster using Euclid's EROs. By modelling the isophotal and iso-density contours, we mapped the distributions and properties of the ICL and ICGCs out to radii of 200-600 kpc (up to ~1/3 of the virial radius) from the brightest cluster galaxy (BCG). We find that the central 500 kpc hosts 70… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.13503v2-abstract-full').style.display = 'inline'; document.getElementById('2405.13503v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.13503v2-abstract-full" style="display: none;"> We study the intracluster light (ICL) and intracluster globular clusters (ICGCs) in the nearby Perseus galaxy cluster using Euclid's EROs. By modelling the isophotal and iso-density contours, we mapped the distributions and properties of the ICL and ICGCs out to radii of 200-600 kpc (up to ~1/3 of the virial radius) from the brightest cluster galaxy (BCG). We find that the central 500 kpc hosts 70000$\pm$2800 GCs and $1.7\times10^{12}$ L$_\odot$ of diffuse light from the BCG+ICL in the near-infrared H$_E$. This accounts for 38$\pm$6% of the cluster's total stellar luminosity within this radius. The ICL and ICGCs share a coherent spatial distribution, suggesting a common origin or that a common potential governs their distribution. Their contours on the largest scales (>200 kpc) are offset from the BCG's core westwards by 60 kpc towards several luminous cluster galaxies. This offset is opposite to the displacement observed in the gaseous intracluster medium. The radial surface brightness profile of the BCG+ICL is best described by a double S茅rsic model, with 68$\pm$4% of the H$_E$ light in the extended, outer component. The transition between these components occurs at ~60 kpc, beyond which the isophotes become increasingly elliptical and off-centred. The radial ICGC number density profile closely follows the BCG+ICL profile only beyond this 60 kpc radius, where we find an average of 60-80 GCs per $10^9$ M$_\odot$ of diffuse stellar mass. The BCG+ICL colour becomes increasingly blue with radius, consistent with the stellar populations in the ICL having subsolar metallicities [Fe/H] ~ -0.6 to -1.0. The colour of the ICL, and the specific frequency and luminosity function of the ICGCs suggest that the ICL+ICGCs were tidally stripped from the outskirts of massive satellites with masses of a few $\times10^{10}$ M$_\odot$, with an increasing contribution from dwarf galaxies at large radii. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.13503v2-abstract-full').style.display = 'none'; document.getElementById('2405.13503v2-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 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Paper submitted as part of the A&A special issue `Euclid on Sky', which contains Euclid key reference papers and first results from the Euclid Early Release Observations. 27 pages, 21 figures, 5 tables. Accepted for publication in A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.17225">arXiv:2306.17225</a> <span> [<a href="https://arxiv.org/pdf/2306.17225">pdf</a>, <a href="https://arxiv.org/format/2306.17225">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/ad17b8">10.3847/1538-4357/ad17b8 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Robust Study of High-Redshift Galaxies: Unsupervised Machine Learning for Characterising morphology with JWST up to z ~ 8 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Tohill%2C+C">Cl谩r-Br铆d Tohill</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S">Steven Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C">Christopher Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+L">Leonardo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Harvey%2C+T">Thomas Harvey</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+N">Nathan Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Austin%2C+D">Duncan Austin</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="2306.17225v2-abstract-short" style="display: inline;"> Galaxy morphologies provide valuable insights into their formation processes, tracing the spatial distribution of ongoing star formation and encoding signatures of dynamical interactions. While such information has been extensively investigated at low redshift, it is crucial to develop a robust system for characterising galaxy morphologies at earlier cosmic epochs. Relying solely on the nomenclatu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.17225v2-abstract-full').style.display = 'inline'; document.getElementById('2306.17225v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.17225v2-abstract-full" style="display: none;"> Galaxy morphologies provide valuable insights into their formation processes, tracing the spatial distribution of ongoing star formation and encoding signatures of dynamical interactions. While such information has been extensively investigated at low redshift, it is crucial to develop a robust system for characterising galaxy morphologies at earlier cosmic epochs. Relying solely on the nomenclature established for low-redshift galaxies risks introducing biases that hinder our understanding of this new regime. In this paper, we employ variational auto-encoders to perform feature extraction on galaxies at z $>$ 2 using JWST/NIRCam data. Our sample comprises 6869 galaxies at z $>$ 2, including 255 galaxies z $>$ 5, which have been detected in both the CANDELS/HST fields and CEERS/JWST, ensuring reliable measurements of redshift, mass, and star formation rates. To address potential biases, we eliminate galaxy orientation and background sources prior to encoding the galaxy features, thereby constructing a physically meaningful feature space. We identify 11 distinct morphological classes that exhibit clear separation in various structural parameters, such as CAS-$M_{20}$, S茅rsic indices, specific star formation rates, and axis ratios. We observe a decline in the presence of spheroidal-type galaxies with increasing redshift, indicating a dominance of disk-like galaxies in the early universe. We demonstrate that conventional visual classification systems are inadequate for high-redshift morphology classification and advocate the need for a more detailed and refined classification scheme. Leveraging machine-extracted features, we propose a solution to this challenge and illustrate how our extracted clusters align with measured parameters, offering greater physical relevance compared to traditional methods. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.17225v2-abstract-full').style.display = 'none'; document.getElementById('2306.17225v2-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 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 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">29 pages, 17 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/2302.11482">arXiv:2302.11482</a> <span> [<a href="https://arxiv.org/pdf/2302.11482">pdf</a>, <a href="https://arxiv.org/format/2302.11482">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"> Exploring the Morphologies of High Redshift Galaxies with Machine Learning </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Tohill%2C+C">Cl谩r-Br铆d Tohill</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S">Steven Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C">Christopher Conselice</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2302.11482v1-abstract-short" style="display: inline;"> The morphology of a galaxy has been shown to encode the evolutionary history and correlates strongly with physical properties such as stellar mass, star formation rates and past merger events. While the majority of galaxies in the local universe can be classified on the Hubble sequence, little is known about the different types of galaxies we observe at high redshift. The irregular morphology of t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.11482v1-abstract-full').style.display = 'inline'; document.getElementById('2302.11482v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.11482v1-abstract-full" style="display: none;"> The morphology of a galaxy has been shown to encode the evolutionary history and correlates strongly with physical properties such as stellar mass, star formation rates and past merger events. While the majority of galaxies in the local universe can be classified on the Hubble sequence, little is known about the different types of galaxies we observe at high redshift. The irregular morphology of these galaxies makes visual classifications difficult, and with the future of astronomy consisting of many "Big Data" surveys we need an efficient, and unbiased classification system in place. In this work we explore the use of unsupervised machine learning techniques to preform feature extraction from galaxy images to separate high redshift galaxies into different morphological types based on the machine learning clusters. We expand on previous work by addressing observation biases such as the orientation, apparent size of the galaxies and noise before extracting features, thus reducing the number of clusters and forcing the network to learn meaningful features. We then compare the extracted clusters' physical properties, to investigate the separation between the groups. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.11482v1-abstract-full').style.display = 'none'; document.getElementById('2302.11482v1-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 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">5 pages, accepted for publication in Memorie della SAIt</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.05907">arXiv:2204.05907</a> <span> [<a href="https://arxiv.org/pdf/2204.05907">pdf</a>, <a href="https://arxiv.org/format/2204.05907">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> <span class="tag is-small is-grey 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/10.1051/0004-6361/202142935">10.1051/0004-6361/202142935 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galapagos-2/Galfitm/GAMA -- multi-wavelength measurement of galaxy structure: separating the properties of spheroid and disk components in modern surveys </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=H%C3%A4u%C3%9Fler%2C+B">Boris H盲u脽ler</a>, <a href="/search/astro-ph?searchtype=author&query=Vika%2C+M">Marina Vika</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S+P">Steven P. Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Johnston%2C+E+J">Evelyn J. Johnston</a>, <a href="/search/astro-ph?searchtype=author&query=Brough%2C+S">Sarah Brough</a>, <a href="/search/astro-ph?searchtype=author&query=Casura%2C+S">Sarah Casura</a>, <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B+W">Benne W. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Kelvin%2C+L+S">Lee S. Kelvin</a>, <a href="/search/astro-ph?searchtype=author&query=Popescu%2C+C">Cristina Popescu</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="2204.05907v1-abstract-short" style="display: inline;"> We present the capabilities of Galapagos--2 and Galfitm in the context of fitting 2-component profiles to galaxies, on the way to providing complete multi-band, multi-component fitting of large samples of galaxies in future surveys. We release both the code and the fit results to 234,239 objects from the DR3 of the Gama survey, a sample significantly deeper than previous works. We use stringent te… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.05907v1-abstract-full').style.display = 'inline'; document.getElementById('2204.05907v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.05907v1-abstract-full" style="display: none;"> We present the capabilities of Galapagos--2 and Galfitm in the context of fitting 2-component profiles to galaxies, on the way to providing complete multi-band, multi-component fitting of large samples of galaxies in future surveys. We release both the code and the fit results to 234,239 objects from the DR3 of the Gama survey, a sample significantly deeper than previous works. We use stringent tests on both simulated and real data, as well as comparison to public catalogues to evaluate the advantages of using multi-band over single-band data. We show that multi-band fitting using Galfitm provides significant advantages when trying to decompose galaxies into their individual constituents, as more data are being used, by effectively being able to use the colour information buried in the individual exposures to its advantage. Using simulated data, we find that multi-band fitting significantly reduces the deviations from real parameter values, allows component sizes and S茅rsic indices to be recovered more accurately, and, by design, constrains the band-to-band variations of these parameters to more physical values. On both simulated and real data, we confirm that the SEDs of the 2 main components can be recovered to fainter magnitudes compared to using single-band fitting, which tends to recover disks and bulges to - on average - have identical SEDs when the galaxies become too faint, instead of the different SEDs they truly have. By comparing our results to those provided by other fitting codes, we confirm that they agree in general, but measurement errors can be significantly reduced by using the multi-band tools developed by the MegaMorph project. We conclude that the multi-band fitting employed by Galapagos-2 and Galfitm significantly improves the accuracy of structural galaxy parameters and enables much larger samples to be be used in a scientific analysis. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.05907v1-abstract-full').style.display = 'none'; document.getElementById('2204.05907v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 April, 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">50 pages, 30 figures, accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 664, A92 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.08539">arXiv:2203.08539</a> <span> [<a href="https://arxiv.org/pdf/2203.08539">pdf</a>, <a href="https://arxiv.org/format/2203.08539">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/stac472">10.1093/mnras/stac472 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galaxy And Mass Assembly (GAMA): Data Release 4 and the z < 0.1 total and z < 0.08 morphological galaxy stellar mass functions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Driver%2C+S+P">Simon P. Driver</a>, <a href="/search/astro-ph?searchtype=author&query=Bellstedt%2C+S">Sabine Bellstedt</a>, <a href="/search/astro-ph?searchtype=author&query=Robotham%2C+A+S+G">Aaron S. G. Robotham</a>, <a href="/search/astro-ph?searchtype=author&query=Baldry%2C+I+K">Ivan K. Baldry</a>, <a href="/search/astro-ph?searchtype=author&query=Davies%2C+L+J">Luke J. Davies</a>, <a href="/search/astro-ph?searchtype=author&query=Liske%2C+J">Jochen Liske</a>, <a href="/search/astro-ph?searchtype=author&query=Obreschkow%2C+D">Danail Obreschkow</a>, <a href="/search/astro-ph?searchtype=author&query=Taylor%2C+E+N">Edward N. Taylor</a>, <a href="/search/astro-ph?searchtype=author&query=Wright%2C+A+H">Angus H. Wright</a>, <a href="/search/astro-ph?searchtype=author&query=Alpaslan%2C+M">Mehmet Alpaslan</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S+P">Steven P. Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+A+E">Amanda E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Bland-Hawthorn%2C+J">Joss Bland-Hawthorn</a>, <a href="/search/astro-ph?searchtype=author&query=Bilicki%2C+M">Maciej Bilicki</a>, <a href="/search/astro-ph?searchtype=author&query=Bravo%2C+M">Matias Bravo</a>, <a href="/search/astro-ph?searchtype=author&query=Brough%2C+S">Sarah Brough</a>, <a href="/search/astro-ph?searchtype=author&query=Casura%2C+S">Sarah Casura</a>, <a href="/search/astro-ph?searchtype=author&query=Cluver%2C+M+E">Michelle E. Cluver</a>, <a href="/search/astro-ph?searchtype=author&query=Colless%2C+M">Matthew Colless</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C+J">Christopher J. Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=Croom%2C+S+M">Scott M. Croom</a>, <a href="/search/astro-ph?searchtype=author&query=de+Jong%2C+J">Jelte de Jong</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Eugenio%2C+F">Franceso D'Eugenio</a>, <a href="/search/astro-ph?searchtype=author&query=De+Propris%2C+R">Roberto De Propris</a>, <a href="/search/astro-ph?searchtype=author&query=Dogruel%2C+B">Burak Dogruel</a> , et al. (45 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="2203.08539v1-abstract-short" style="display: inline;"> In Galaxy And Mass Assembly Data Release 4 (GAMA DR4), we make available our full spectroscopic redshift sample. This includes 248682 galaxy spectra, and, in combination with earlier surveys, results in 330542 redshifts across five sky regions covering ~250deg^2. The redshift density, is the highest available over such a sustained area, has exceptionally high completeness (95 per cent to r_KIDS=19… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.08539v1-abstract-full').style.display = 'inline'; document.getElementById('2203.08539v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.08539v1-abstract-full" style="display: none;"> In Galaxy And Mass Assembly Data Release 4 (GAMA DR4), we make available our full spectroscopic redshift sample. This includes 248682 galaxy spectra, and, in combination with earlier surveys, results in 330542 redshifts across five sky regions covering ~250deg^2. The redshift density, is the highest available over such a sustained area, has exceptionally high completeness (95 per cent to r_KIDS=19.65mag), and is well suited for the study of galaxy mergers, galaxy groups, and the low redshift (z<0.25) galaxy population. DR4 includes 32 value-added tables or Data Management Units (DMUs) that provide a number of measured and derived data products including GALEX, ESO KiDS, ESO VIKING, WISE and Herschel Space Observatory imaging. Within this release, we provide visual morphologies for 15330 galaxies to z<0.08, photometric redshift estimates for all 18million objects to r_KIDS~25mag, and stellar velocity dispersions for 111830 galaxies. We conclude by deriving the total galaxy stellar mass function (GSMF) and its sub-division by morphological class (elliptical, compact-bulge and disc, diffuse-bulge and disc, and disc only). This extends our previous measurement of the total GSMF down to 10^6.75 M_sol h^-2_70 and we find a total stellar mass density of rho_*=(2.97+/-0.04)x10^8 M_sol h_70 Mpc^-3 or Omega_*=(2.17+/-0.03)x10^-3 h^-1_70. We conclude that at z<0.1, the Universe has converted 4.9+/-0.1 per cent of the baryonic mass implied by Big Bang Nucleosynthesis into stars that are gravitationally bound within the galaxy population. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.08539v1-abstract-full').style.display = 'none'; document.getElementById('2203.08539v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 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">Accepted for publication in MNRAS. GAMA Data Release 4 is available at: http://www.gama-survey.org/dr4/</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.14848">arXiv:2109.14848</a> <span> [<a href="https://arxiv.org/pdf/2109.14848">pdf</a>, <a href="https://arxiv.org/format/2109.14848">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"> A model-independent reconstruction of dark energy to very high redshift </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Moss%2C+A">Adam Moss</a>, <a href="/search/astro-ph?searchtype=author&query=Copeland%2C+E">Edmund Copeland</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S">Steven Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Clarke%2C+T">Thomas Clarke</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2109.14848v1-abstract-short" style="display: inline;"> We provide a model-independent reconstruction of dark energy from $z=0$ to $ \gtrsim 10^5$. We parameterise the model by a perfect fluid with a series of physically well-motivated bins in energy-density, such that the equation of state is always $-1 \le w \le 1$. Our method is capable of describing a range of theoretical models with smooth modifications to the expansion history. Combining the late… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.14848v1-abstract-full').style.display = 'inline'; document.getElementById('2109.14848v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.14848v1-abstract-full" style="display: none;"> We provide a model-independent reconstruction of dark energy from $z=0$ to $ \gtrsim 10^5$. We parameterise the model by a perfect fluid with a series of physically well-motivated bins in energy-density, such that the equation of state is always $-1 \le w \le 1$. Our method is capable of describing a range of theoretical models with smooth modifications to the expansion history. Combining the latest CMB, BAO, SN and local $H_0$ measurements, we obtain a large improvement of $螖蠂^2=41.3$ over LCDM, at the expense of 33 additional parameters in the fit, with dark energy contributing significantly between $z \sim 10^4 - 10^5$, and intriguingly with a sound speed $c_s^2 \sim 1/3$. A significant part of the $螖蠂^2$ improvement comes from \Planck\ + Atacama Cosmology Telescope (\textsc{Act}) data, alleviating tension between them within LCDM. We apply a correlation prior to penalise models with unnecessary degrees of freedom and find no preference for deviations from LCDM at late-times, but moderate Bayesian evidence of an early dark energy (EDE) component. Although the model has a large amount of freedom, it is unable to reduce $S_8 \equiv 蟽_8 (惟_\mathrm{c} / 0.3)^{0.5}$ below that of \lcdm, to bring about full concordance with large-scale structure data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.14848v1-abstract-full').style.display = 'none'; document.getElementById('2109.14848v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 pages, 3 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2103.17246">arXiv:2103.17246</a> <span> [<a href="https://arxiv.org/pdf/2103.17246">pdf</a>, <a href="https://arxiv.org/format/2103.17246">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/stab941">10.1093/mnras/stab941 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Recovering the origins of the lenticular galaxy NGC 3115 using multi-band imaging </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Buzzo%2C+M+L">Maria Luisa Buzzo</a>, <a href="/search/astro-ph?searchtype=author&query=Cortesi%2C+A">Arianna Cortesi</a>, <a href="/search/astro-ph?searchtype=author&query=Hernandez-Jimenez%2C+J+A">Jose A. Hernandez-Jimenez</a>, <a href="/search/astro-ph?searchtype=author&query=Coccato%2C+L">Lodovico Coccato</a>, <a href="/search/astro-ph?searchtype=author&query=Werle%2C+A">Ariel Werle</a>, <a href="/search/astro-ph?searchtype=author&query=Silva%2C+L+B+e">Leandro Beraldo e Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Grossi%2C+M">Marco Grossi</a>, <a href="/search/astro-ph?searchtype=author&query=Vika%2C+M">Marina Vika</a>, <a href="/search/astro-ph?searchtype=author&query=Barbosa%2C+C+E">Carlos Eduardo Barbosa</a>, <a href="/search/astro-ph?searchtype=author&query=Lucatelli%2C+G">Geferson Lucatelli</a>, <a href="/search/astro-ph?searchtype=author&query=Santana-Silva%2C+L">Luidhy Santana-Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S">Steven Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Debattista%2C+V+P">Victor P. Debattista</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=Overzier%2C+R">Roderik Overzier</a>, <a href="/search/astro-ph?searchtype=author&query=Romanowsky%2C+A+J">Aaron J. Romanowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrari%2C+F">Fabricio Ferrari</a>, <a href="/search/astro-ph?searchtype=author&query=Brodie%2C+J+P">Jean P. Brodie</a>, <a href="/search/astro-ph?searchtype=author&query=de+Oliveira%2C+C+M">Claudia Mendes de Oliveira</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="2103.17246v1-abstract-short" style="display: inline;"> A detailed study of the morphology of lenticular galaxies is an important way to understand how this type of galaxy formed and evolves over time. Decomposing a galaxy into its components (disc, bulge, bar, ...) allows recovering the colour gradients present in each system, its star formation history, and its assembly history. We use GALFITM to perform a multi-wavelength structural decomposition of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.17246v1-abstract-full').style.display = 'inline'; document.getElementById('2103.17246v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.17246v1-abstract-full" style="display: none;"> A detailed study of the morphology of lenticular galaxies is an important way to understand how this type of galaxy formed and evolves over time. Decomposing a galaxy into its components (disc, bulge, bar, ...) allows recovering the colour gradients present in each system, its star formation history, and its assembly history. We use GALFITM to perform a multi-wavelength structural decomposition of the closest lenticular galaxy, NGC 3115, resulting in the description of its stellar light into several main components: a bulge, a thin disc, a thick disc and also evidence of a bar. We report the finding of central bluer stellar populations in the bulge, as compared to the colour of the galaxy outskirts, indicating either the presence of an Active Galactic Nucleus (AGN) and/or recent star formation activity. From the spectral energy distribution results, we show that the galaxy has a low luminosity AGN component, but even excluding the effect of the nuclear activity, the bulge is still bluer than the outer-regions of the galaxy, revealing a recent episode of star formation. Based on all of the derived properties, we propose a scenario for the formation of NGC 3115 consisting of an initial gas-rich merger, followed by accretions and feedback that quench the galaxy, until a recent encounter with the companion KK084 that reignited the star formation in the bulge, provoked a core displacement in NGC 3115 and generated spiral-like features. This result is consistent with the two-phase formation scenario, proposed in previous studies of this galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.17246v1-abstract-full').style.display = 'none'; document.getElementById('2103.17246v1-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 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">Accepted for publication in MNRAS: 22 pages, 15 figures, 7 tables, 1 appendix</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2102.08414">arXiv:2102.08414</a> <span> [<a href="https://arxiv.org/pdf/2102.08414">pdf</a>, <a href="https://arxiv.org/format/2102.08414">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="Computer Vision and Pattern Recognition">cs.CV</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/stab2093">10.1093/mnras/stab2093 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galaxy Zoo DECaLS: Detailed Visual Morphology Measurements from Volunteers and Deep Learning for 314,000 Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Walmsley%2C+M">Mike Walmsley</a>, <a href="/search/astro-ph?searchtype=author&query=Lintott%2C+C">Chris Lintott</a>, <a href="/search/astro-ph?searchtype=author&query=Geron%2C+T">Tobias Geron</a>, <a href="/search/astro-ph?searchtype=author&query=Kruk%2C+S">Sandor Kruk</a>, <a href="/search/astro-ph?searchtype=author&query=Krawczyk%2C+C">Coleman Krawczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Willett%2C+K+W">Kyle W. Willett</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S">Steven Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Kelvin%2C+L+S">Lee S. Kelvin</a>, <a href="/search/astro-ph?searchtype=author&query=Fortson%2C+L">Lucy Fortson</a>, <a href="/search/astro-ph?searchtype=author&query=Gal%2C+Y">Yarin Gal</a>, <a href="/search/astro-ph?searchtype=author&query=Keel%2C+W">William Keel</a>, <a href="/search/astro-ph?searchtype=author&query=Masters%2C+K+L">Karen L. Masters</a>, <a href="/search/astro-ph?searchtype=author&query=Mehta%2C+V">Vihang Mehta</a>, <a href="/search/astro-ph?searchtype=author&query=Simmons%2C+B+D">Brooke D. Simmons</a>, <a href="/search/astro-ph?searchtype=author&query=Smethurst%2C+R">Rebecca Smethurst</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+L">Lewis Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Baeten%2C+E+M">Elisabeth M. Baeten</a>, <a href="/search/astro-ph?searchtype=author&query=Macmillan%2C+C">Christine Macmillan</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="2102.08414v2-abstract-short" style="display: inline;"> We present Galaxy Zoo DECaLS: detailed visual morphological classifications for Dark Energy Camera Legacy Survey images of galaxies within the SDSS DR8 footprint. Deeper DECaLS images (r=23.6 vs. r=22.2 from SDSS) reveal spiral arms, weak bars, and tidal features not previously visible in SDSS imaging. To best exploit the greater depth of DECaLS images, volunteers select from a new set of answers… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.08414v2-abstract-full').style.display = 'inline'; document.getElementById('2102.08414v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2102.08414v2-abstract-full" style="display: none;"> We present Galaxy Zoo DECaLS: detailed visual morphological classifications for Dark Energy Camera Legacy Survey images of galaxies within the SDSS DR8 footprint. Deeper DECaLS images (r=23.6 vs. r=22.2 from SDSS) reveal spiral arms, weak bars, and tidal features not previously visible in SDSS imaging. To best exploit the greater depth of DECaLS images, volunteers select from a new set of answers designed to improve our sensitivity to mergers and bars. Galaxy Zoo volunteers provide 7.5 million individual classifications over 314,000 galaxies. 140,000 galaxies receive at least 30 classifications, sufficient to accurately measure detailed morphology like bars, and the remainder receive approximately 5. All classifications are used to train an ensemble of Bayesian convolutional neural networks (a state-of-the-art deep learning method) to predict posteriors for the detailed morphology of all 314,000 galaxies. When measured against confident volunteer classifications, the networks are approximately 99% accurate on every question. Morphology is a fundamental feature of every galaxy; our human and machine classifications are an accurate and detailed resource for understanding how galaxies evolve. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.08414v2-abstract-full').style.display = 'none'; document.getElementById('2102.08414v2-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 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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 by MNRAS July '21. Open access DOI below. Data at https://doi.org/10.5281/zenodo.4196266. Code at https://www.github.com/mwalmsley/zoobot. Docs at https://zoobot.readthedocs.io/. Interactive viewer at https://share.streamlit.io/mwalmsley/galaxy-poster/gz_decals_mike_walmsley.py</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.09081">arXiv:2012.09081</a> <span> [<a href="https://arxiv.org/pdf/2012.09081">pdf</a>, <a href="https://arxiv.org/format/2012.09081">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div 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/ac033c">10.3847/1538-4357/ac033c <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Quantifying Non-parametric Structure of High-redshift Galaxies with Deep Learning </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Tohill%2C+C">C. Tohill</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+L">L. Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C+J">C. J. Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S+P">S. P. Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrari%2C+F">F. Ferrari</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2012.09081v3-abstract-short" style="display: inline;"> At high redshift, due to both observational limitations and the variety of galaxy morphologies in the early universe, measuring galaxy structure can be challenging. Non-parametric measurements such as the CAS system have thus become an important tool due to both their model-independent nature and their utility as a straightforward computational process. Recently, convolutional neural networks (CNN… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.09081v3-abstract-full').style.display = 'inline'; document.getElementById('2012.09081v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.09081v3-abstract-full" style="display: none;"> At high redshift, due to both observational limitations and the variety of galaxy morphologies in the early universe, measuring galaxy structure can be challenging. Non-parametric measurements such as the CAS system have thus become an important tool due to both their model-independent nature and their utility as a straightforward computational process. Recently, convolutional neural networks (CNNs) have been shown to be adept at image analysis, and are beginning to supersede traditional measurements of visual morphology and model-based structural parameters. In this work, we take a further step by extending CNNs to measure well known non-parametric structural quantities: concentration ($C$) and asymmetry ($A$). We train CNNs to predict $C$ and $A$ from individual images of $\sim 150,000$ galaxies at $0 < z < 7$ in the CANDELS fields, using Bayesian hyperparameter optimisation to select suitable network architectures. Our resulting networks accurately reproduce measurements compared with standard algorithms. Furthermore, using simulated images, we show that our networks are more stable than the standard algorithms at low signal-to-noise. While both approaches suffer from similar systematic biases with redshift, these remain small out to $z \sim 7$. Once trained, measurements with our networks are $> 10^3$ times faster than previous methods. Our approach is thus able to reproduce standard measures of non-parametric morphologies and shows the potential of employing neural networks to provide superior results in substantially less time. This will be vital for making best use of the large and complex datasets provided by upcoming galaxy surveys, such as Euclid and Rubin-LSST. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.09081v3-abstract-full').style.display = 'none'; document.getElementById('2012.09081v3-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 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 13 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/2009.09493">arXiv:2009.09493</a> <span> [<a href="https://arxiv.org/pdf/2009.09493">pdf</a>, <a href="https://arxiv.org/format/2009.09493">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/abb612">10.3847/1538-3881/abb612 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galaxy And Mass Assembly: A Comparison between Galaxy-Galaxy Lens Searches in KiDS/GAMA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Knabel%2C+S">Shawn Knabel</a>, <a href="/search/astro-ph?searchtype=author&query=Steele%2C+R+L">Rebecca L. Steele</a>, <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B+W">Benne W. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Bridge%2C+J+S">Joanna S. Bridge</a>, <a href="/search/astro-ph?searchtype=author&query=Jacques%2C+A">Alice Jacques</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A">Andrew Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S+P">Steven P. Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+M+J+I">Michael J. I. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Brough%2C+S">Sarah Brough</a>, <a href="/search/astro-ph?searchtype=author&query=Kelvin%2C+L+S">Lee S. Kelvin</a>, <a href="/search/astro-ph?searchtype=author&query=Bilicki%2C+M">Maciej Bilicki</a>, <a href="/search/astro-ph?searchtype=author&query=Kielkopf%2C+J">John Kielkopf</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="2009.09493v1-abstract-short" style="display: inline;"> Strong gravitational lenses are a rare and instructive type of astronomical object. Identification has long relied on serendipity, but different strategies -- such as mixed spectroscopy of multiple galaxies along the line of sight, machine learning algorithms, and citizen science -- have been employed to identify these objects as new imaging surveys become available. We report on the comparison… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.09493v1-abstract-full').style.display = 'inline'; document.getElementById('2009.09493v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.09493v1-abstract-full" style="display: none;"> Strong gravitational lenses are a rare and instructive type of astronomical object. Identification has long relied on serendipity, but different strategies -- such as mixed spectroscopy of multiple galaxies along the line of sight, machine learning algorithms, and citizen science -- have been employed to identify these objects as new imaging surveys become available. We report on the comparison between spectroscopic, machine learning, and citizen science identification of galaxy-galaxy lens candidates from independently constructed lens catalogs in the common survey area of the equatorial fields of the GAMA survey. In these, we have the opportunity to compare high-completeness spectroscopic identifications against high-fidelity imaging from the Kilo Degree Survey (KiDS) used for both machine learning and citizen science lens searches. We find that the three methods -- spectroscopy, machine learning, and citizen science -- identify 47, 47, and 13 candidates respectively in the 180 square degrees surveyed. These identifications barely overlap, with only two identified by both citizen science and machine learning. We have traced this discrepancy to inherent differences in the selection functions of each of the three methods, either within their parent samples (i.e. citizen science focuses on low-redshift) or inherent to the method (i.e. machine learning is limited by its training sample and prefers well-separated features, while spectroscopy requires sufficient flux from lensed features to lie within the fiber). These differences manifest as separate samples in estimated Einstein radius, lens stellar mass, and lens redshift. The combined sample implies a lens candidate sky-density $\sim0.59$ deg$^{-2}$ and can inform the construction of a training set spanning a wider mass-redshift space. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.09493v1-abstract-full').style.display = 'none'; document.getElementById('2009.09493v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">22 figures, 6 tables, accepted for publication in The Astronomical 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/2006.10450">arXiv:2006.10450</a> <span> [<a href="https://arxiv.org/pdf/2006.10450">pdf</a>, <a href="https://arxiv.org/format/2006.10450">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"> Galaxy Zoo Builder: Four Component Photometric decomposition of Spiral Galaxies Guided by Citizen Science </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lingard%2C+T+K">Timothy K. Lingard</a>, <a href="/search/astro-ph?searchtype=author&query=Masters%2C+K+L">Karen L. Masters</a>, <a href="/search/astro-ph?searchtype=author&query=Krawczyk%2C+C">Coleman Krawczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Lintott%2C+C">Chris Lintott</a>, <a href="/search/astro-ph?searchtype=author&query=Kruk%2C+S">Sandor Kruk</a>, <a href="/search/astro-ph?searchtype=author&query=Simmons%2C+B">Brooke Simmons</a>, <a href="/search/astro-ph?searchtype=author&query=Simpson%2C+R">Robert Simpson</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S">Steven Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Nichol%2C+R+C">Robert C. Nichol</a>, <a href="/search/astro-ph?searchtype=author&query=Baeten%2C+E">Elisabeth Baeten</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2006.10450v2-abstract-short" style="display: inline;"> Multi-component modelling of galaxies is a valuable tool in the effort to quantitatively understand galaxy evolution, yet the use of the technique is plagued by issues of convergence, model selection and parameter degeneracies. These issues limit its application over large samples to the simplest models, with complex models being applied only to very small samples. We attempt to resolve this dilem… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.10450v2-abstract-full').style.display = 'inline'; document.getElementById('2006.10450v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2006.10450v2-abstract-full" style="display: none;"> Multi-component modelling of galaxies is a valuable tool in the effort to quantitatively understand galaxy evolution, yet the use of the technique is plagued by issues of convergence, model selection and parameter degeneracies. These issues limit its application over large samples to the simplest models, with complex models being applied only to very small samples. We attempt to resolve this dilemma of "quantity or quality" by developing a novel framework, built inside the Zooniverse citizen science platform, to enable the crowdsourcing of model creation for Sloan Digitial Sky Survey galaxies. We have applied the method, including a final algorithmic optimisation step, on a test sample of 198 galaxies, and examine the robustness of this new method. We also compare it to automated fitting pipelines, demonstrating that it is possible to consistently recover accurate models that either show good agreement with, or improve on, prior work. We conclude that citizen science is a promising technique for modelling images of complex galaxies, and release our catalogue of models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.10450v2-abstract-full').style.display = 'none'; document.getElementById('2006.10450v2-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 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages, 16 figures, 2 tables. 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/1909.07461">arXiv:1909.07461</a> <span> [<a href="https://arxiv.org/pdf/1909.07461">pdf</a>, <a href="https://arxiv.org/format/1909.07461">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/ab2886">10.3847/1538-3881/ab2886 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The frequency of dust lanes in edge-on spiral galaxies identified by Galaxy Zoo in KiDS imaging of GAMA targets </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B+W">B. W. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Kelvin%2C+L">L. Kelvin</a>, <a href="/search/astro-ph?searchtype=author&query=Baldry%2C+I">I. Baldry</a>, <a href="/search/astro-ph?searchtype=author&query=Lintott%2C+C">C. Lintott</a>, <a href="/search/astro-ph?searchtype=author&query=Alpaslan%2C+M">M. Alpaslan</a>, <a href="/search/astro-ph?searchtype=author&query=Pimbblet%2C+K+A">K. A. Pimbblet</a>, <a href="/search/astro-ph?searchtype=author&query=Liske%2C+J">J. Liske</a>, <a href="/search/astro-ph?searchtype=author&query=Kitching%2C+T">T. Kitching</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S">S. Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=de+Jong%2C+J">J. de Jong</a>, <a href="/search/astro-ph?searchtype=author&query=Bilicki%2C+M">M. Bilicki</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A">A. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Bridge%2C+J">J. Bridge</a>, <a href="/search/astro-ph?searchtype=author&query=Steele%2C+R">R. Steele</a>, <a href="/search/astro-ph?searchtype=author&query=Jacques%2C+A">A. Jacques</a>, <a href="/search/astro-ph?searchtype=author&query=Goswami%2C+S">S. Goswami</a>, <a href="/search/astro-ph?searchtype=author&query=Kusmic%2C+S">S. Kusmic</a>, <a href="/search/astro-ph?searchtype=author&query=Roemer%2C+W">W. Roemer</a>, <a href="/search/astro-ph?searchtype=author&query=Kruk%2C+S">S. Kruk</a>, <a href="/search/astro-ph?searchtype=author&query=Popescu%2C+C+C">C. C. Popescu</a>, <a href="/search/astro-ph?searchtype=author&query=Kuijken%2C+K">K. Kuijken</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+L">L. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Wright%2C+A">A. Wright</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1909.07461v1-abstract-short" style="display: inline;"> Dust lanes bisect the plane of a typical edge-on spiral galaxy as a dark optical absorption feature. Their appearance is linked to the gravitational stability of spiral disks; the fraction of edge-on galaxies that displays a dust lane is a direct indicator of the typical vertical balance between gravity and turbulence; a balance struck between the energy input from star-formation and the gravitati… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.07461v1-abstract-full').style.display = 'inline'; document.getElementById('1909.07461v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1909.07461v1-abstract-full" style="display: none;"> Dust lanes bisect the plane of a typical edge-on spiral galaxy as a dark optical absorption feature. Their appearance is linked to the gravitational stability of spiral disks; the fraction of edge-on galaxies that displays a dust lane is a direct indicator of the typical vertical balance between gravity and turbulence; a balance struck between the energy input from star-formation and the gravitational pull into the plane of the disk. Based on morphological classifications by the Galaxy~Zoo project on the Kilo-Degree Survey (KiDS) imaging data in the Galaxy and Mass Assembly (GAMA) fields, we explore the relation of dust lanes to the galaxy characteristics, most of which were determined using the {\sc magphys} spectral energy distribution fitting tool: stellar mass, total and specific star-formation rates, and several parameters describing the cold dust component. We find that the fraction of dust lanes does depend on the stellar mass of the galaxy; they start to appear at $M^* \sim 10^9 M_\odot$. A dust lane also implies strongly a dust mass of at least $10^5 M_\odot$, but otherwise does not correlate with cold dust mass parameters of the {\sc magphys} spectral energy distribution analysis, nor is there a link with star-formation rate, specific or total. Dust lane identification does not depend on disk ellipticity (disk thickness) or Sersic profile but correlates with bulge morphology; a round bulge favors dust lane votes. The central component along the line of sight that produces the dust lane is not associated with either one of the components fit by {\sc magphys}, the cold diffuse component or the localized, heated component in HII regions, but a mix of these two. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.07461v1-abstract-full').style.display = 'none'; document.getElementById('1909.07461v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in the Astronomical 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/1909.03256">arXiv:1909.03256</a> <span> [<a href="https://arxiv.org/pdf/1909.03256">pdf</a>, <a href="https://arxiv.org/format/1909.03256">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/10.1051/0004-6361/201833522">10.1051/0004-6361/201833522 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multi-wavelength structure analysis of local cluster galaxies. The WINGS project </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Psychogyios%2C+A">A. Psychogyios</a>, <a href="/search/astro-ph?searchtype=author&query=Vika%2C+M">M. Vika</a>, <a href="/search/astro-ph?searchtype=author&query=Charmandaris%2C+V">V. Charmandaris</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S">S. Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Fasano%2C+G">G. Fasano</a>, <a href="/search/astro-ph?searchtype=author&query=H%C3%A4u%C3%9Fler%2C+B">B. H盲u脽ler</a>, <a href="/search/astro-ph?searchtype=author&query=Moretti%2C+A">A. Moretti</a>, <a href="/search/astro-ph?searchtype=author&query=Poggianti%2C+B">B. Poggianti</a>, <a href="/search/astro-ph?searchtype=author&query=Vulcani%2C+B">B. Vulcani</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1909.03256v1-abstract-short" style="display: inline;"> We present a multi-wavelength analysis of the galaxies in nine clusters selected from the WINGS dataset, examining how galaxy structure varies as a function of wavelength and environment using the state of the art software GALAPAGOSII. We simultaneously fit single S茅rsic functions on three optical (u, B and V) and two near-infrared (J and K) bands thus creating a wavelength-dependent model of each… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.03256v1-abstract-full').style.display = 'inline'; document.getElementById('1909.03256v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1909.03256v1-abstract-full" style="display: none;"> We present a multi-wavelength analysis of the galaxies in nine clusters selected from the WINGS dataset, examining how galaxy structure varies as a function of wavelength and environment using the state of the art software GALAPAGOSII. We simultaneously fit single S茅rsic functions on three optical (u, B and V) and two near-infrared (J and K) bands thus creating a wavelength-dependent model of each galaxy. We measure the magnitudes, effective radius ($R_{e}$) the S茅rsic index ($n$), axis ratio and position angle in each band. The sample contains 790 cluster members (located close to the cluster center < 0.64 R$_{200}$ and 254 non-member galaxies that we further separate based on their morphology into ellipticals, lenticulars and spirals. We find that the S茅rsic index of all galaxies inside clusters remains nearly constant with wavelength while $R_{e}$ decreases as wavelength increases for all morphological types. We do not observe a significant variation on n and $R_{e}$ as a function of projected local density and distance from the clusters center. Comparing the n and $R_{e}$ of bright cluster galaxies with a subsample of non-member galaxies we find that bright cluster galaxies are more concentrated (display high $n$ values) and are more compact (low $R_{e}$). Moreover, the light profile ($\mathcal{N}$) and size ($\mathcal{R}$) of bright cluster galaxies does not change as a function of wavelength in the same manner as non-member galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.03256v1-abstract-full').style.display = 'none'; document.getElementById('1909.03256v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 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">16 pages, 17 figures and 5 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1905.07424">arXiv:1905.07424</a> <span> [<a href="https://arxiv.org/pdf/1905.07424">pdf</a>, <a href="https://arxiv.org/format/1905.07424">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="Computer Vision and Pattern Recognition">cs.CV</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/stz2816">10.1093/mnras/stz2816 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galaxy Zoo: Probabilistic Morphology through Bayesian CNNs and Active Learning </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Walmsley%2C+M">Mike Walmsley</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+L">Lewis Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Lintott%2C+C">Chris Lintott</a>, <a href="/search/astro-ph?searchtype=author&query=Gal%2C+Y">Yarin Gal</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S">Steven Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+H">Hugh Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Fortson%2C+L">Lucy Fortson</a>, <a href="/search/astro-ph?searchtype=author&query=Kruk%2C+S">Sandor Kruk</a>, <a href="/search/astro-ph?searchtype=author&query=Masters%2C+K">Karen Masters</a>, <a href="/search/astro-ph?searchtype=author&query=Scarlata%2C+C">Claudia Scarlata</a>, <a href="/search/astro-ph?searchtype=author&query=Simmons%2C+B">Brooke Simmons</a>, <a href="/search/astro-ph?searchtype=author&query=Smethurst%2C+R">Rebecca Smethurst</a>, <a href="/search/astro-ph?searchtype=author&query=Wright%2C+D">Darryl Wright</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="1905.07424v2-abstract-short" style="display: inline;"> We use Bayesian convolutional neural networks and a novel generative model of Galaxy Zoo volunteer responses to infer posteriors for the visual morphology of galaxies. Bayesian CNN can learn from galaxy images with uncertain labels and then, for previously unlabelled galaxies, predict the probability of each possible label. Our posteriors are well-calibrated (e.g. for predicting bars, we achieve c… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.07424v2-abstract-full').style.display = 'inline'; document.getElementById('1905.07424v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1905.07424v2-abstract-full" style="display: none;"> We use Bayesian convolutional neural networks and a novel generative model of Galaxy Zoo volunteer responses to infer posteriors for the visual morphology of galaxies. Bayesian CNN can learn from galaxy images with uncertain labels and then, for previously unlabelled galaxies, predict the probability of each possible label. Our posteriors are well-calibrated (e.g. for predicting bars, we achieve coverage errors of 11.8% within a vote fraction deviation of 0.2) and hence are reliable for practical use. Further, using our posteriors, we apply the active learning strategy BALD to request volunteer responses for the subset of galaxies which, if labelled, would be most informative for training our network. We show that training our Bayesian CNNs using active learning requires up to 35-60% fewer labelled galaxies, depending on the morphological feature being classified. By combining human and machine intelligence, Galaxy Zoo will be able to classify surveys of any conceivable scale on a timescale of weeks, providing massive and detailed morphology catalogues to support research into galaxy evolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.07424v2-abstract-full').style.display = 'none'; document.getElementById('1905.07424v2-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 October, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 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">Accepted by MNRAS. 21 pages, including appendices</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1812.05629">arXiv:1812.05629</a> <span> [<a href="https://arxiv.org/pdf/1812.05629">pdf</a>, <a href="https://arxiv.org/ps/1812.05629">ps</a>, <a href="https://arxiv.org/format/1812.05629">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/stz007">10.1093/mnras/stz007 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> OMEGA -- OSIRIS Mapping of Emission-line Galaxies in A901/2 -- V. The rich population of jellyfish galaxies in the multi-cluster system Abell 901/2 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Roman-Oliveira%2C+F+V">Fernanda V. Roman-Oliveira</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=del+Pino%2C+B+R">Bruno Rodr铆guez del Pino</a>, <a href="/search/astro-ph?searchtype=author&query=Arag%C3%B3n-Salamanca%2C+A">A. Arag贸n-Salamanca</a>, <a href="/search/astro-ph?searchtype=author&query=Gray%2C+M+E">Meghan E. Gray</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S+P">Steven P. Bamford</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1812.05629v2-abstract-short" style="display: inline;"> We present the results of a systematic search and characterisation of jellyfish galaxy candidates in the multi-cluster system A901/2, at z ~ 0.165, as part of the OMEGA survey. By visual inspecting ACS/HST F606W images looking for morphological signatures of ram-pressure stripping events in Halpha-emitting galaxies, we identify a total of 70 candidates. Out of these, 53 are clearly star-forming ga… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.05629v2-abstract-full').style.display = 'inline'; document.getElementById('1812.05629v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1812.05629v2-abstract-full" style="display: none;"> We present the results of a systematic search and characterisation of jellyfish galaxy candidates in the multi-cluster system A901/2, at z ~ 0.165, as part of the OMEGA survey. By visual inspecting ACS/HST F606W images looking for morphological signatures of ram-pressure stripping events in Halpha-emitting galaxies, we identify a total of 70 candidates. Out of these, 53 are clearly star-forming galaxies and 5 are highly probable AGN hosts, the classification of the remaining galaxies is more uncertain. They have late-type and irregular morphologies and most of them are part of the blue cloud with only 4 being previously classified as dusty reds. The AGN activity is not prominent in the sample and, of the few cases of galaxies hosting AGN, such activity does not seem to be correlated to the gas stripping phenomenon. Our jellyfish galaxy candidates do not have a preferential pattern of motion within the multi-cluster system, although the most compelling cases appear to inhabit the inner regions of the most massive sub-cluster centres. The sSFR of these galaxies indicates that their star formation activity is enhanced, in contrast with what is observed for the rest of the star-forming galaxy population in the system. Half of the sample is forming stars at a higher rate than the main-sequence for field galaxies and this behaviour is more evident for the most compelling candidates. For some galaxies, the spatially resolved Halpha emission appears to be as disturbed and extended as their continuum counterparts. Our findings point towards a scenario where the ram pressure stripping is triggering a period of intense and extended star formation throughout the galaxy while it is also disturbing the morphology. This is the largest sample of jellyfish galaxy candidates found in a single system suggesting that cluster mergers might be the ideal environment for studying ram pressure stripping effects. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.05629v2-abstract-full').style.display = 'none'; document.getElementById('1812.05629v2-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 February, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 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">15 pages, 9 figures, MNRAS accepted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1808.00530">arXiv:1808.00530</a> <span> [<a href="https://arxiv.org/pdf/1808.00530">pdf</a>, <a href="https://arxiv.org/ps/1808.00530">ps</a>, <a href="https://arxiv.org/format/1808.00530">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/sty2112">10.1093/mnras/sty2112 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> OMEGA - OSIRIS Mapping of Emission-line Galaxies in A901/2: IV. - Extinction of Star-Formation Estimators with Inclination </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wolf%2C+C">Christian Wolf</a>, <a href="/search/astro-ph?searchtype=author&query=Weinzirl%2C+T">Tim Weinzirl</a>, <a href="/search/astro-ph?searchtype=author&query=Arag%C3%B3n-Salamanca%2C+A">Alfonso Arag贸n-Salamanca</a>, <a href="/search/astro-ph?searchtype=author&query=Gray%2C+M+E">Meghan E. Gray</a>, <a href="/search/astro-ph?searchtype=author&query=del+Pino%2C+B+R">Bruno Rodr铆guez del Pino</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=Bamford%2C+S+P">Steven P. Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6hm%2C+A">Asmus B枚hm</a>, <a href="/search/astro-ph?searchtype=author&query=Harborne%2C+K">Katherine Harborne</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="1808.00530v1-abstract-short" style="display: inline;"> We study the effect of inclination on the apparent brightness of star-forming galaxies in spectral passbands that are commonly used as star-formation indicators. As diagnostics we use mass-to-light ratios in three passbands: the UV continuum at 280 nm, the H$伪$ emission line, and the FIR 24$渭$-band. We include a study of inclination trends in the IR/UV ratio ("IRX") and the IR/H$伪$ ratio. Our samp… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.00530v1-abstract-full').style.display = 'inline'; document.getElementById('1808.00530v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1808.00530v1-abstract-full" style="display: none;"> We study the effect of inclination on the apparent brightness of star-forming galaxies in spectral passbands that are commonly used as star-formation indicators. As diagnostics we use mass-to-light ratios in three passbands: the UV continuum at 280 nm, the H$伪$ emission line, and the FIR 24$渭$-band. We include a study of inclination trends in the IR/UV ratio ("IRX") and the IR/H$伪$ ratio. Our sample comprises a few hundred galaxies from the region around the clusters Abell 901/902 with deep data and inclinations measured from outer disks in Hubble Space Telescope images. As a novelty, the H$伪$- and separately the NII-emission are measured by tunable-filter imaging and encompass galaxies in their entirety. At galaxy stellar masses above log $M_*/M_\odot > 10$ we find trends in the UV and H$伪$ mass-to-light ratio that suggest an inclination-induced attenuation from face-on to edge-on of $\sim 1$ mag and $\sim 0.7$ mag in UV and H$伪$, respectively, implying that star-formation rates of edge-on galaxies would be underestimated by $\sim 2.5\times$ in UV and $\sim 2\times$ in H$伪$. We find the luminosities in UV and H$伪$ to be well correlated, but the optical depth of diffuse dust that causes inclination dependence appears to be lower for stars emitting at 280 nm than for gas clouds emitting Balmer lines. For galaxies with log $M_*/M_\odot < 9.7$, we find no measurable effect at $>0.1$ mag. The absence of an inclination dependence at 24$渭$ confirms that the average galaxy is optically thin in the FIR. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.00530v1-abstract-full').style.display = 'none'; document.getElementById('1808.00530v1-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, 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">12 pages, 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/1806.03199">arXiv:1806.03199</a> <span> [<a href="https://arxiv.org/pdf/1806.03199">pdf</a>, <a href="https://arxiv.org/ps/1806.03199">ps</a>, <a href="https://arxiv.org/format/1806.03199">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/sty2257">10.1093/mnras/sty2257 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galaxy Cluster Mass Reconstruction Project - IV. Understanding the effects of imperfect membership on cluster mass estimation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wojtak%2C+R">R. Wojtak</a>, <a href="/search/astro-ph?searchtype=author&query=Old%2C+L">L. Old</a>, <a href="/search/astro-ph?searchtype=author&query=Mamon%2C+G+A">G. A. Mamon</a>, <a href="/search/astro-ph?searchtype=author&query=Pearce%2C+F+R">F. R. Pearce</a>, <a href="/search/astro-ph?searchtype=author&query=de+Carvalho%2C+R">R. de Carvalho</a>, <a href="/search/astro-ph?searchtype=author&query=Sif%C3%B3n%2C+C">C. Sif贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Gray%2C+M+E">M. E. Gray</a>, <a href="/search/astro-ph?searchtype=author&query=Skibba%2C+R+A">R. A. Skibba</a>, <a href="/search/astro-ph?searchtype=author&query=Croton%2C+D">D. Croton</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S">S. Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Gifford%2C+D">D. Gifford</a>, <a href="/search/astro-ph?searchtype=author&query=von+der+Linden%2C+A">A. von der Linden</a>, <a href="/search/astro-ph?searchtype=author&query=Mu%C3%B1oz-Cuartas%2C+J+C">J. C. Mu帽oz-Cuartas</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%BCller%2C+V">V. M眉ller</a>, <a href="/search/astro-ph?searchtype=author&query=Pearson%2C+R+J">R. J. Pearson</a>, <a href="/search/astro-ph?searchtype=author&query=Rozo%2C+E">E. Rozo</a>, <a href="/search/astro-ph?searchtype=author&query=Rykoff%2C+E">E. Rykoff</a>, <a href="/search/astro-ph?searchtype=author&query=Saro%2C+A">A. Saro</a>, <a href="/search/astro-ph?searchtype=author&query=Sepp%2C+T">T. Sepp</a>, <a href="/search/astro-ph?searchtype=author&query=Tempel%2C+E">E. Tempel</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="1806.03199v2-abstract-short" style="display: inline;"> The primary difficulty in measuring dynamical masses of galaxy clusters from galaxy data lies in the separation between true cluster members from interloping galaxies along the line of sight. We study the impact of membership contamination and incompleteness on cluster mass estimates obtained with 25 commonly used techniques applied to nearly 1000 mock clusters. We show that all methods overestima… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.03199v2-abstract-full').style.display = 'inline'; document.getElementById('1806.03199v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1806.03199v2-abstract-full" style="display: none;"> The primary difficulty in measuring dynamical masses of galaxy clusters from galaxy data lies in the separation between true cluster members from interloping galaxies along the line of sight. We study the impact of membership contamination and incompleteness on cluster mass estimates obtained with 25 commonly used techniques applied to nearly 1000 mock clusters. We show that all methods overestimate or underestimate cluster masses when applied to contaminated or incomplete galaxy samples respectively. This appears to be the main source of the intrinsic scatter in the mass scaling relation. Applying corrections based on a prior knowledge of contamination and incompleteness can reduce the scatter to the level of shot noise expected for poorly sampled clusters. We establish an empirical model quantifying the effect of imperfect membership on cluster mass estimation and discuss its universal and method-dependent features. We find that both imperfect membership and the response of the mass estimators depend on cluster mass, effectively causing a flattening of the estimated - true mass relation. Imperfect membership thus alters cluster counts determined from spectroscopic surveys, hence the cosmological parameters that depend on such counts. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.03199v2-abstract-full').style.display = 'none'; document.getElementById('1806.03199v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 August, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 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">18 pages, 11 figures, 3tables; accepted for publication in MNRAS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> MNRAS, 481, 324 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1805.01782">arXiv:1805.01782</a> <span> [<a href="https://arxiv.org/pdf/1805.01782">pdf</a>, <a href="https://arxiv.org/format/1805.01782">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/sty1201">10.1093/mnras/sty1201 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galaxy Zoo: constraining the origin of spiral arms </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hart%2C+R+E">Ross E. Hart</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S+P">Steven P. Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Keel%2C+W+C">William C. Keel</a>, <a href="/search/astro-ph?searchtype=author&query=Kruk%2C+S+J">Sandor J. Kruk</a>, <a href="/search/astro-ph?searchtype=author&query=Masters%2C+K+L">Karen L. Masters</a>, <a href="/search/astro-ph?searchtype=author&query=Simmons%2C+B+D">Brooke D. Simmons</a>, <a href="/search/astro-ph?searchtype=author&query=Smethurst%2C+R+J">Rebecca J. Smethurst</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="1805.01782v1-abstract-short" style="display: inline;"> Since the discovery that the majority of low-redshift galaxies exhibit some level of spiral structure, a number of theories have been proposed as to why these patterns exist. A popular explanation is a process known as swing amplification, yet there is no observational evidence to prove that such a mechanism is at play. By using a number of measured properties of galaxies, and scaling relations wh… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.01782v1-abstract-full').style.display = 'inline'; document.getElementById('1805.01782v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1805.01782v1-abstract-full" style="display: none;"> Since the discovery that the majority of low-redshift galaxies exhibit some level of spiral structure, a number of theories have been proposed as to why these patterns exist. A popular explanation is a process known as swing amplification, yet there is no observational evidence to prove that such a mechanism is at play. By using a number of measured properties of galaxies, and scaling relations where there are no direct measurements, we model samples of SDSS and S$^4$G spiral galaxies in terms of their relative halo, bulge and disc mass and size. Using these models, we test predictions of swing amplification theory with respect to directly measured spiral arm numbers from Galaxy Zoo 2. We find that neither a universal cored or cuspy inner dark matter profile can correctly predict observed numbers of arms in galaxies. However, by invoking a halo contraction/expansion model, a clear bimodality in the spiral galaxy population emerges. Approximately 40 per cent of unbarred spiral galaxies at $z \lesssim 0.1$ and $\mathrm{M_*} \gtrsim 10^{10} \mathrm{M_\odot}$ have spiral arms that can be modelled by swing amplification. This population display a significant correlation between predicted and observed spiral arm numbers, evidence that they are swing amplified modes. The remainder are dominated by two-arm systems for which the model predicts significantly higher arm numbers. These are likely driven by tidal interactions or other mechanisms. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.01782v1-abstract-full').style.display = 'none'; document.getElementById('1805.01782v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 May, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">19 pages, 13 figures, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1801.08541">arXiv:1801.08541</a> <span> [<a href="https://arxiv.org/pdf/1801.08541">pdf</a>, <a href="https://arxiv.org/format/1801.08541">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> <span class="tag is-small is-grey 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/10.3847/1538-4357/aaa250">10.3847/1538-4357/aaa250 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galaxy Zoo: Morphological classification of galaxy images from the Illustris simulation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+H">Hugh Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Fortson%2C+L">Lucy Fortson</a>, <a href="/search/astro-ph?searchtype=author&query=Lintott%2C+C">Chris Lintott</a>, <a href="/search/astro-ph?searchtype=author&query=Scarlata%2C+C">Claudia Scarlata</a>, <a href="/search/astro-ph?searchtype=author&query=Willett%2C+K">Kyle Willett</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S">Steven Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Beck%2C+M">Melanie Beck</a>, <a href="/search/astro-ph?searchtype=author&query=Cardamone%2C+C">Carolin Cardamone</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+M">Melanie Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Simmons%2C+B">Brooke Simmons</a>, <a href="/search/astro-ph?searchtype=author&query=Keel%2C+W">William Keel</a>, <a href="/search/astro-ph?searchtype=author&query=Kruk%2C+S">Sandor Kruk</a>, <a href="/search/astro-ph?searchtype=author&query=Masters%2C+K">Karen Masters</a>, <a href="/search/astro-ph?searchtype=author&query=Vogelsberger%2C+M">Mark Vogelsberger</a>, <a href="/search/astro-ph?searchtype=author&query=Torrey%2C+P">Paul Torrey</a>, <a href="/search/astro-ph?searchtype=author&query=Snyder%2C+G+F">Gregory F. Snyder</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="1801.08541v1-abstract-short" style="display: inline;"> Modern cosmological simulations model the universe with increasing sophistication and at higher spatial and temporal resolutions. These enhancements permit detailed comparisons between the simulation outputs and real observational data. Recent projects such as Illustris are capable of producing simulated images that are comparable to those obtained from local surveys. This paper tests how well Ill… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.08541v1-abstract-full').style.display = 'inline'; document.getElementById('1801.08541v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1801.08541v1-abstract-full" style="display: none;"> Modern cosmological simulations model the universe with increasing sophistication and at higher spatial and temporal resolutions. These enhancements permit detailed comparisons between the simulation outputs and real observational data. Recent projects such as Illustris are capable of producing simulated images that are comparable to those obtained from local surveys. This paper tests how well Illustris achieves this goal across a diverse population of galaxies using visual morphologies derived from Galaxy Zoo citizen scientists. Morphological classifications provided by volunteers for simulated galaxies are compared with similar data for a compatible sample of images drawn from the SDSS Legacy Survey. This paper investigates how simple morphological characterization by human volunteers asked to distinguish smooth from featured systems differs between simulated and real galaxy images. Differences are identified, which are likely due to the limited resolution of the simulation, but which could be revealing real differences in the dynamical evolution of populations of galaxies in the real and model universes. Specifically, for stellar masses $M_{\star}\lesssim10^{11}M_{\odot}$, a larger proportion of Illustris galaxies that exhibit disk-like morphology or visible substructure, relative to their SDSS counterparts. Toward higher masses, simulated and observed galaxies converge and exhibit similar morphology distributions. The stellar mass threshold indicated by this divergent behavior confirms recent works using parametric measures of morphology from Illustris simulated images. When $M_{\star}\gtrsim10^{11}M_{\odot}$, the Illustris dataset contains fewer galaxies that classifiers regard as unambiguously featured. These results suggest that comparison between the detailed properties of observed and simulated galaxies, even when limited to reasonably massive systems, may be misleading. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.08541v1-abstract-full').style.display = 'none'; document.getElementById('1801.08541v1-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 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">12 pages, 7 figures, to be published 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/1801.04277">arXiv:1801.04277</a> <span> [<a href="https://arxiv.org/pdf/1801.04277">pdf</a>, <a href="https://arxiv.org/format/1801.04277">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/sty124">10.1093/mnras/sty124 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galaxy and Mass Assembly (GAMA): Morphological transformation of galaxies across the green valley </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bremer%2C+M+N">M. N. Bremer</a>, <a href="/search/astro-ph?searchtype=author&query=Phillipps%2C+S">S. Phillipps</a>, <a href="/search/astro-ph?searchtype=author&query=Kelvin%2C+L+S">L. S. Kelvin</a>, <a href="/search/astro-ph?searchtype=author&query=De+Propris%2C+R">R. De Propris</a>, <a href="/search/astro-ph?searchtype=author&query=Kennedy%2C+R">Rebecca Kennedy</a>, <a href="/search/astro-ph?searchtype=author&query=Moffett%2C+A+J">Amanda J. Moffett</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S">S. Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Davies%2C+L+J+M">L. J. M. Davies</a>, <a href="/search/astro-ph?searchtype=author&query=Driver%2C+S+P">S. P. Driver</a>, <a href="/search/astro-ph?searchtype=author&query=H%C3%A4u%C3%9Fler%2C+B">B. H盲u脽ler</a>, <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B">B. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A">A. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=James%2C+P+A">P. A. James</a>, <a href="/search/astro-ph?searchtype=author&query=Liske%2C+J">J. Liske</a>, <a href="/search/astro-ph?searchtype=author&query=Percival%2C+S">S. Percival</a>, <a href="/search/astro-ph?searchtype=author&query=Taylor%2C+E+N">E. N. Taylor</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="1801.04277v1-abstract-short" style="display: inline;"> We explore constraints on the joint photometric and morphological evolution of typical low redshift galaxies as they move from the blue cloud through the green valley and onto the red sequence. We select GAMA survey galaxies with $10.25<{\rm log}(M_*/M_\odot)<10.75$ and $z<0.2$ classified according to their intrinsic $u^*-r^*$ colour. From single component S茅rsic fits, we find that the stellar mas… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.04277v1-abstract-full').style.display = 'inline'; document.getElementById('1801.04277v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1801.04277v1-abstract-full" style="display: none;"> We explore constraints on the joint photometric and morphological evolution of typical low redshift galaxies as they move from the blue cloud through the green valley and onto the red sequence. We select GAMA survey galaxies with $10.25<{\rm log}(M_*/M_\odot)<10.75$ and $z<0.2$ classified according to their intrinsic $u^*-r^*$ colour. From single component S茅rsic fits, we find that the stellar mass-sensitive $K-$band profiles of red and green galaxy populations are very similar, while $g-$band profiles indicate more disk-like morphologies for the green galaxies: apparent (optical) morphological differences arise primarily from radial mass-to-light ratio variations. Two-component fits show that most green galaxies have significant bulge and disk components and that the blue to red evolution is driven by colour change in the disk. Together, these strongly suggest that galaxies evolve from blue to red through secular disk fading and that a strong bulge is present prior to any decline in star formation. The relative abundance of the green population implies a typical timescale for traversing the green valley $\sim 1-2$~Gyr and is independent of environment, unlike that of the red and blue populations. While environment likely plays a r么le in triggering the passage across the green valley, it appears to have little effect on time taken. These results are consistent with a green valley population dominated by (early type) disk galaxies that are insufficiently supplied with gas to maintain previous levels of disk star formation, eventually attaining passive colours. No single event is needed quench their star formation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.04277v1-abstract-full').style.display = 'none'; document.getElementById('1801.04277v1-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 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">MNRAS, 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/1801.02634">arXiv:1801.02634</a> <span> [<a href="https://arxiv.org/pdf/1801.02634">pdf</a>, <a href="https://arxiv.org/format/1801.02634">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/10.3847/1538-3881/aabc4f">10.3847/1538-3881/aabc4f <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Astropy Project: Building an inclusive, open-science project and status of the v2.0 core package </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Astropy+Collaboration"> The Astropy Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Price-Whelan%2C+A+M">A. M. Price-Whelan</a>, <a href="/search/astro-ph?searchtype=author&query=Sip%C5%91cz%2C+B+M">B. M. Sip艖cz</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%BCnther%2C+H+M">H. M. G眉nther</a>, <a href="/search/astro-ph?searchtype=author&query=Lim%2C+P+L">P. L. Lim</a>, <a href="/search/astro-ph?searchtype=author&query=Crawford%2C+S+M">S. M. Crawford</a>, <a href="/search/astro-ph?searchtype=author&query=Conseil%2C+S">S. Conseil</a>, <a href="/search/astro-ph?searchtype=author&query=Shupe%2C+D+L">D. L. Shupe</a>, <a href="/search/astro-ph?searchtype=author&query=Craig%2C+M+W">M. W. Craig</a>, <a href="/search/astro-ph?searchtype=author&query=Dencheva%2C+N">N. Dencheva</a>, <a href="/search/astro-ph?searchtype=author&query=Ginsburg%2C+A">A. Ginsburg</a>, <a href="/search/astro-ph?searchtype=author&query=VanderPlas%2C+J+T">J. T. VanderPlas</a>, <a href="/search/astro-ph?searchtype=author&query=Bradley%2C+L+D">L. D. Bradley</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A9rez-Su%C3%A1rez%2C+D">D. P茅rez-Su谩rez</a>, <a href="/search/astro-ph?searchtype=author&query=de+Val-Borro%2C+M">M. de Val-Borro</a>, <a href="/search/astro-ph?searchtype=author&query=Aldcroft%2C+T+L">T. L. Aldcroft</a>, <a href="/search/astro-ph?searchtype=author&query=Cruz%2C+K+L">K. L. Cruz</a>, <a href="/search/astro-ph?searchtype=author&query=Robitaille%2C+T+P">T. P. Robitaille</a>, <a href="/search/astro-ph?searchtype=author&query=Tollerud%2C+E+J">E. J. Tollerud</a>, <a href="/search/astro-ph?searchtype=author&query=Ardelean%2C+C">C. Ardelean</a>, <a href="/search/astro-ph?searchtype=author&query=Babej%2C+T">T. Babej</a>, <a href="/search/astro-ph?searchtype=author&query=Bachetti%2C+M">M. Bachetti</a>, <a href="/search/astro-ph?searchtype=author&query=Bakanov%2C+A+V">A. V. Bakanov</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S+P">S. P. Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Barentsen%2C+G">G. Barentsen</a> , et al. (112 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="1801.02634v2-abstract-short" style="display: inline;"> The Astropy project supports and fosters the development of open-source and openly-developed Python packages that provide commonly-needed functionality to the astronomical community. A key element of the Astropy project is the core package Astropy, which serves as the foundation for more specialized projects and packages. In this article, we provide an overview of the organization of the Astropy p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.02634v2-abstract-full').style.display = 'inline'; document.getElementById('1801.02634v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1801.02634v2-abstract-full" style="display: none;"> The Astropy project supports and fosters the development of open-source and openly-developed Python packages that provide commonly-needed functionality to the astronomical community. A key element of the Astropy project is the core package Astropy, which serves as the foundation for more specialized projects and packages. In this article, we provide an overview of the organization of the Astropy project and summarize key features in the core package as of the recent major release, version 2.0. We then describe the project infrastructure designed to facilitate and support development for a broader ecosystem of inter-operable packages. We conclude with a future outlook of planned new features and directions for the broader Astropy project. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.02634v2-abstract-full').style.display = 'none'; document.getElementById('1801.02634v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 January, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 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">Minor changes to author list and title. Comments and feedback welcome through the paper source repository: https://github.com/astropy/astropy-v2.0-paper For more information about Astropy, see http://www.astropy.org/</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1711.09139">arXiv:1711.09139</a> <span> [<a href="https://arxiv.org/pdf/1711.09139">pdf</a>, <a href="https://arxiv.org/ps/1711.09139">ps</a>, <a href="https://arxiv.org/format/1711.09139">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/stx3042">10.1093/mnras/stx3042 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galaxy And Mass Assembly (GAMA): the G02 field, Herschel-ATLAS target selection and Data Release 3 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Baldry%2C+I+K">I. K. Baldry</a>, <a href="/search/astro-ph?searchtype=author&query=Liske%2C+J">J. Liske</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+M+J+I">M. J. I. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Robotham%2C+A+S+G">A. S. G. Robotham</a>, <a href="/search/astro-ph?searchtype=author&query=Driver%2C+S+P">S. P. Driver</a>, <a href="/search/astro-ph?searchtype=author&query=Dunne%2C+L">L. Dunne</a>, <a href="/search/astro-ph?searchtype=author&query=Alpaslan%2C+M">M. Alpaslan</a>, <a href="/search/astro-ph?searchtype=author&query=Brough%2C+S">S. Brough</a>, <a href="/search/astro-ph?searchtype=author&query=Cluver%2C+M+E">M. E. Cluver</a>, <a href="/search/astro-ph?searchtype=author&query=Eardley%2C+E">E. Eardley</a>, <a href="/search/astro-ph?searchtype=author&query=Farrow%2C+D+J">D. J. Farrow</a>, <a href="/search/astro-ph?searchtype=author&query=Heymans%2C+C">C. Heymans</a>, <a href="/search/astro-ph?searchtype=author&query=Hildebrandt%2C+H">H. Hildebrandt</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A+M">A. M. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Kelvin%2C+L+S">L. S. Kelvin</a>, <a href="/search/astro-ph?searchtype=author&query=Loveday%2C+J">J. Loveday</a>, <a href="/search/astro-ph?searchtype=author&query=Moffett%2C+A+J">A. J. Moffett</a>, <a href="/search/astro-ph?searchtype=author&query=Norberg%2C+P">P. Norberg</a>, <a href="/search/astro-ph?searchtype=author&query=Owers%2C+M+S">M. S. Owers</a>, <a href="/search/astro-ph?searchtype=author&query=Taylor%2C+E+N">E. N. Taylor</a>, <a href="/search/astro-ph?searchtype=author&query=Wright%2C+A+H">A. H. Wright</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S+P">S. P. Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Bland-Hawthorn%2C+J">J. Bland-Hawthorn</a>, <a href="/search/astro-ph?searchtype=author&query=Bourne%2C+N">N. Bourne</a>, <a href="/search/astro-ph?searchtype=author&query=Bremer%2C+M+N">M. N. Bremer</a> , et al. (17 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="1711.09139v1-abstract-short" style="display: inline;"> We describe data release 3 (DR3) of the Galaxy And Mass Assembly (GAMA) survey. The GAMA survey is a spectroscopic redshift and multi-wavelength photometric survey in three equatorial regions each of 60.0 deg^2 (G09, G12, G15), and two southern regions of 55.7 deg^2 (G02) and 50.6 deg^2 (G23). DR3 consists of: the first release of data covering the G02 region and of data on H-ATLAS sources in the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1711.09139v1-abstract-full').style.display = 'inline'; document.getElementById('1711.09139v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1711.09139v1-abstract-full" style="display: none;"> We describe data release 3 (DR3) of the Galaxy And Mass Assembly (GAMA) survey. The GAMA survey is a spectroscopic redshift and multi-wavelength photometric survey in three equatorial regions each of 60.0 deg^2 (G09, G12, G15), and two southern regions of 55.7 deg^2 (G02) and 50.6 deg^2 (G23). DR3 consists of: the first release of data covering the G02 region and of data on H-ATLAS sources in the equatorial regions; and updates to data on sources released in DR2. DR3 includes 154809 sources with secure redshifts across four regions. A subset of the G02 region is 95.5% redshift complete to r<19.8 over an area of 19.5 deg^2, with 20086 galaxy redshifts, that overlaps substantially with the XXL survey (X-ray) and VIPERS (redshift survey). In the equatorial regions, the main survey has even higher completeness (98.5%), and spectra for about 75% of H-ATLAS filler targets were also obtained. This filler sample extends spectroscopic redshifts, for probable optical counterparts to H-ATLAS sub-mm sources, to 0.8 mag deeper (r<20.6) than the GAMA main survey. There are 25814 galaxy redshifts for H-ATLAS sources from the GAMA main or filler surveys. GAMA DR3 is available at the survey website (www.gama-survey.org/dr3/). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1711.09139v1-abstract-full').style.display = 'none'; document.getElementById('1711.09139v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 November, 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">14 pages, 15 figures, accepted by MNRAS. GAMA DR3 is available at http://www.gama-survey.org/dr3/</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Mon.Not.Roy.Astron.Soc. 474 (2018) 3875-3888 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1710.00093">arXiv:1710.00093</a> <span> [<a href="https://arxiv.org/pdf/1710.00093">pdf</a>, <a href="https://arxiv.org/format/1710.00093">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/stx2605">10.1093/mnras/stx2605 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galaxy Zoo: Secular evolution of barred galaxies from structural decomposition of multi-band images </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kruk%2C+S+J">Sandor J. Kruk</a>, <a href="/search/astro-ph?searchtype=author&query=Lintott%2C+C+J">Chris J. Lintott</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S+P">Steven P. Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Masters%2C+K+L">Karen L. Masters</a>, <a href="/search/astro-ph?searchtype=author&query=Simmons%2C+B+D">Brooke D. Simmons</a>, <a href="/search/astro-ph?searchtype=author&query=H%C3%A4u%C3%9Fler%2C+B">Boris H盲u脽ler</a>, <a href="/search/astro-ph?searchtype=author&query=Cardamone%2C+C+N">Carolin N. Cardamone</a>, <a href="/search/astro-ph?searchtype=author&query=Hart%2C+R+E">Ross E. Hart</a>, <a href="/search/astro-ph?searchtype=author&query=Kelvin%2C+L">Lee Kelvin</a>, <a href="/search/astro-ph?searchtype=author&query=Schawinski%2C+K">Kevin Schawinski</a>, <a href="/search/astro-ph?searchtype=author&query=Smethurst%2C+R+J">Rebecca J. Smethurst</a>, <a href="/search/astro-ph?searchtype=author&query=Vika%2C+M">Marina Vika</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="1710.00093v2-abstract-short" style="display: inline;"> We present the results of two-component (disc+bar) and three-component (disc+bar+bulge) multiwavelength 2D photometric decompositions of barred galaxies in five SDSS bands ($ugriz$). This sample of $\sim$3,500 nearby ($z<0.06$) galaxies with strong bars selected from the Galaxy Zoo citizen science project is the largest sample of barred galaxies to be studied using photometric decompositions which… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1710.00093v2-abstract-full').style.display = 'inline'; document.getElementById('1710.00093v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1710.00093v2-abstract-full" style="display: none;"> We present the results of two-component (disc+bar) and three-component (disc+bar+bulge) multiwavelength 2D photometric decompositions of barred galaxies in five SDSS bands ($ugriz$). This sample of $\sim$3,500 nearby ($z<0.06$) galaxies with strong bars selected from the Galaxy Zoo citizen science project is the largest sample of barred galaxies to be studied using photometric decompositions which include a bar component. With detailed structural analysis we obtain physical quantities such as the bar- and bulge-to-total luminosity ratios, effective radii, S茅rsic indices and colours of the individual components. We observe a clear difference in the colours of the components, the discs being bluer than the bars and bulges. An overwhelming fraction of bulge components have S茅rsic indices consistent with being pseudobulges. By comparing the barred galaxies with a mass-matched and volume-limited sample of unbarred galaxies, we examine the connection between the presence of a large-scale galactic bar and the properties of discs and bulges. We find that the discs of unbarred galaxies are significantly bluer compared to the discs of barred galaxies, while there is no significant difference in the colours of the bulges. We find possible evidence of secular evolution via bars that leads to the build-up of pseudobulges and to the quenching of star formation in the discs. We identify a subsample of unbarred galaxies with an inner lens/oval and find that their properties are similar to barred galaxies, consistent with an evolutionary scenario in which bars dissolve into lenses. This scenario deserves further investigation through both theoretical and observational work. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1710.00093v2-abstract-full').style.display = 'none'; document.getElementById('1710.00093v2-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 October, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 September, 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">26 pages, 21 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/1708.04628">arXiv:1708.04628</a> <span> [<a href="https://arxiv.org/pdf/1708.04628">pdf</a>, <a href="https://arxiv.org/format/1708.04628">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/stx2137">10.1093/mnras/stx2137 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galaxy Zoo and SpArcFiRe: Constraints on spiral arm formation mechanisms from spiral arm number and pitch angles </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hart%2C+R+E">Ross E. Hart</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S+P">Steven P. Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Hayes%2C+W+B">Wayne B. Hayes</a>, <a href="/search/astro-ph?searchtype=author&query=Cardamone%2C+C+N">Carolin N. Cardamone</a>, <a href="/search/astro-ph?searchtype=author&query=Keel%2C+W+C">William C. Keel</a>, <a href="/search/astro-ph?searchtype=author&query=Kruk%2C+S+J">Sandor J. Kruk</a>, <a href="/search/astro-ph?searchtype=author&query=Lintott%2C+C+J">Chris J. Lintott</a>, <a href="/search/astro-ph?searchtype=author&query=Masters%2C+K+L">Karen L. Masters</a>, <a href="/search/astro-ph?searchtype=author&query=Simmons%2C+B+D">Brooke D. Simmons</a>, <a href="/search/astro-ph?searchtype=author&query=Smethurst%2C+R+J">Rebecca J. Smethurst</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="1708.04628v1-abstract-short" style="display: inline;"> In this paper we study the morphological properties of spiral galaxies, including measurements of spiral arm number and pitch angle. Using Galaxy Zoo 2, a stellar mass-complete sample of 6,222 SDSS spiral galaxies is selected. We use the machine vision algorithm SpArcFiRe to identify spiral arm features and measure their associated geometries. A support vector machine classifier is employed to ide… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1708.04628v1-abstract-full').style.display = 'inline'; document.getElementById('1708.04628v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1708.04628v1-abstract-full" style="display: none;"> In this paper we study the morphological properties of spiral galaxies, including measurements of spiral arm number and pitch angle. Using Galaxy Zoo 2, a stellar mass-complete sample of 6,222 SDSS spiral galaxies is selected. We use the machine vision algorithm SpArcFiRe to identify spiral arm features and measure their associated geometries. A support vector machine classifier is employed to identify reliable spiral features, with which we are able to estimate pitch angles for half of our sample. We use these machine measurements to calibrate visual estimates of arm tightness, and hence estimate pitch angles for our entire sample. The properties of spiral arms are compared with respect to various galaxy properties. The star formation properties of galaxies vary significantly with arm number, but not pitch angle. We find that galaxies hosting strong bars have spiral arms substantially ($4-6^\mathrm{o}$) looser than unbarred galaxies. Accounting for this, spiral arms associated with many-arm structures are looser (by 2$^\mathrm{o}$) than those in two-arm galaxies. In contrast to this average trend, galaxies with greater bulge-to-total stellar mass ratios display both fewer and looser spiral arms. This effect is primarily driven by the galaxy disc, such that galaxies with more massive discs contain more spiral arms with tighter pitch angles. This implies that galaxy central mass concentration is not the dominant cause of pitch angle and arm number variations between galaxies, which in turn suggests that not all spiral arms are governed by classical density waves or modal theories. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1708.04628v1-abstract-full').style.display = 'none'; document.getElementById('1708.04628v1-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 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">18 pages, 13 figures, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1706.05199">arXiv:1706.05199</a> <span> [<a href="https://arxiv.org/pdf/1706.05199">pdf</a>, <a href="https://arxiv.org/format/1706.05199">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/stx1525">10.1093/mnras/stx1525 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> OMEGA - OSIRIS Mapping of Emission-line Galaxies in A901/2: III. - Galaxy Properties Across Projected Phase Space in A901/2 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Weinzirl%2C+T">Tim Weinzirl</a>, <a href="/search/astro-ph?searchtype=author&query=Aragon-Salamanca%2C+A">Alfonso Aragon-Salamanca</a>, <a href="/search/astro-ph?searchtype=author&query=Gray%2C+M+E">Meghan E. Gray</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S+P">Steven P. Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=del+Pino%2C+B+R">Bruno Rodriguez del Pino</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=Boehm%2C+A">Asmus Boehm</a>, <a href="/search/astro-ph?searchtype=author&query=Wolf%2C+C">Christian Wolf</a>, <a href="/search/astro-ph?searchtype=author&query=Cool%2C+R+J">Richard J. Cool</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="1706.05199v1-abstract-short" style="display: inline;"> We conduct a comprehensive projected phase-space analysis of the A901/2 multi-cluster system at $z\sim0.165$. Aggregating redshifts from spectroscopy, tunable-filter imaging, and prism techniques, we assemble a sample of 856 cluster galaxies reaching $10^{8.5}M_\odot$ in stellar mass. We look for variations in cluster galaxy properties between virialised and non-virialised regions of projected pha… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1706.05199v1-abstract-full').style.display = 'inline'; document.getElementById('1706.05199v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1706.05199v1-abstract-full" style="display: none;"> We conduct a comprehensive projected phase-space analysis of the A901/2 multi-cluster system at $z\sim0.165$. Aggregating redshifts from spectroscopy, tunable-filter imaging, and prism techniques, we assemble a sample of 856 cluster galaxies reaching $10^{8.5}M_\odot$ in stellar mass. We look for variations in cluster galaxy properties between virialised and non-virialised regions of projected phase-space (PPS). Our main conclusions point to relatively gentle environmental effects, expressed mainly on galaxy gas reservoirs. (1) Stacking the four subclusters in A901/2, we find galaxies in the virialised region are more massive, redder, and have marginally higher S猫rsic indices, but their half-light radii and Hubble types are not significantly different. (2) After accounting for trends in stellar mass, there is a remaining change in rest-frame colour across PPS. Primarily, the colour difference is due to an absence in the virialised region of galaxies with rest-frame $B-V<0.7$ and moderate-to-high ($M_\star>10^{9.85}M_\odot$) stellar mass. (3) There is an infalling population of lower-mass ($M_\star\leq10^{9.85}M_\odot$), relatively blue ($B-V<0.7$) elliptical or spheroidal galaxies that is strikingly absent in the virialised region. (4) The number of bona-fide star-forming and AGN galaxies in the PPS regions is strongly dictated by stellar mass. However, there remains a reduced fraction of star-forming galaxies in the centres of the clusters at fixed stellar mass, consistent with the star-formation-density relation in galaxy clusters. (5) There is no change in specific H$伪$-derived star-formation rates of star-forming galaxies at fixed mass across the cluster environment. This suggests that preprocessing of galaxies during infall plays a prominent role in quenching star formation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1706.05199v1-abstract-full').style.display = 'none'; document.getElementById('1706.05199v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 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">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/1705.03839">arXiv:1705.03839</a> <span> [<a href="https://arxiv.org/pdf/1705.03839">pdf</a>, <a href="https://arxiv.org/format/1705.03839">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/10.1051/0004-6361/201630252">10.1051/0004-6361/201630252 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The effects of the cluster environment on the galaxy mass-size relation in MACSJ J1206.2-0847 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kuchner%2C+U">U. Kuchner</a>, <a href="/search/astro-ph?searchtype=author&query=Ziegler%2C+B">B. Ziegler</a>, <a href="/search/astro-ph?searchtype=author&query=Verdugo%2C+M">M. Verdugo</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S">S. Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=H%C3%A4u%C3%9Fler%2C+B">B. H盲u脽ler</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="1705.03839v1-abstract-short" style="display: inline;"> The dense environment of galaxy clusters strongly influences the nature of galaxies. Here, we study the cause of the size distribution of a sample of 560 spectroscopic members spanning a wide dynamical range down to 10^8.5 M_sol (log(M)-2) in the massive CLASH cluster MACSJ 1206.2-0847 at z~0.44. We use Subaru SuprimeCam imaging covering the highest-density core out to the infall regions (3 virial… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1705.03839v1-abstract-full').style.display = 'inline'; document.getElementById('1705.03839v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1705.03839v1-abstract-full" style="display: none;"> The dense environment of galaxy clusters strongly influences the nature of galaxies. Here, we study the cause of the size distribution of a sample of 560 spectroscopic members spanning a wide dynamical range down to 10^8.5 M_sol (log(M)-2) in the massive CLASH cluster MACSJ 1206.2-0847 at z~0.44. We use Subaru SuprimeCam imaging covering the highest-density core out to the infall regions (3 virial radii) to look for cluster-specific effects. We also compare our measurements to a compatible large field study in order to span extreme environmental densities. This paper presents the trends we identified for cluster galaxies divided by their colors into star-forming and quiescent galaxies and into distinct morphological types (using S茅rsic index and bulge/disk decompositions). We observed larger sizes for early type and smaller sizes for massive late type galaxies in clusters in comparison to the field. We attribute this to longer quenching timescales of more massive galaxies in the cluster. Our analysis further revealed an increasing importance of recently quenched transition objects ("red disks"). This is a virialized population found at higher cluster-centric radii with sizes similar to the quiescent, spheroid-dominated population of the cluster center, but with disks still in-tact. The mass-size relation of cluster galaxies may therefore be understood as the consequence of a mix of progenitors formed at different quenching epochs. We also find that galaxy sizes smoothly decreasing as a function of bulge fraction. At same bulge-to-total ratio and same stellar mass, quiescent galaxies are smaller than star-forming galaxies. This is likely because of a fading of the outskirts of the disk, which we saw in comparing sizes of their disk-components. Ram-pressure stripping of the cold gas and other forms of more gradual gas starvation are likely responsible for this observation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1705.03839v1-abstract-full').style.display = 'none'; document.getElementById('1705.03839v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 May, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">20 Pages, 16 Figures; ; Accepted for publication in A&A on 2017 May 11</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 604, A54 (2017) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1705.00007">arXiv:1705.00007</a> <span> [<a href="https://arxiv.org/pdf/1705.00007">pdf</a>, <a href="https://arxiv.org/format/1705.00007">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/stx1026">10.1093/mnras/stx1026 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galaxy Zoo: Finding offset discs and bars in SDSS galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kruk%2C+S+J">Sandor J. Kruk</a>, <a href="/search/astro-ph?searchtype=author&query=Lintott%2C+C+J">Chris J. Lintott</a>, <a href="/search/astro-ph?searchtype=author&query=Simmons%2C+B+D">Brooke D. Simmons</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S+P">Steven P. Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Cardamone%2C+C+N">Carolin N. Cardamone</a>, <a href="/search/astro-ph?searchtype=author&query=Fortson%2C+L">Lucy Fortson</a>, <a href="/search/astro-ph?searchtype=author&query=Hart%2C+R+E">Ross E. Hart</a>, <a href="/search/astro-ph?searchtype=author&query=H%C3%A4u%C3%9Fler%2C+B">Boris H盲u脽ler</a>, <a href="/search/astro-ph?searchtype=author&query=Masters%2C+K+L">Karen L. Masters</a>, <a href="/search/astro-ph?searchtype=author&query=Nichol%2C+R+C">Robert C. Nichol</a>, <a href="/search/astro-ph?searchtype=author&query=Schawinski%2C+K">Kevin Schawinski</a>, <a href="/search/astro-ph?searchtype=author&query=Smethurst%2C+R+J">Rebecca J. Smethurst</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="1705.00007v1-abstract-short" style="display: inline;"> We use multi-wavelength SDSS images and Galaxy Zoo morphologies to identify a sample of $\sim$$270$ late-type galaxies with an off-centre bar. We measure offsets in the range 0.2-2.5 kpc between the photometric centres of the stellar disc and stellar bar. The measured offsets correlate with global asymmetries of the galaxies, with those with largest offsets showing higher lopsidedness. These findi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1705.00007v1-abstract-full').style.display = 'inline'; document.getElementById('1705.00007v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1705.00007v1-abstract-full" style="display: none;"> We use multi-wavelength SDSS images and Galaxy Zoo morphologies to identify a sample of $\sim$$270$ late-type galaxies with an off-centre bar. We measure offsets in the range 0.2-2.5 kpc between the photometric centres of the stellar disc and stellar bar. The measured offsets correlate with global asymmetries of the galaxies, with those with largest offsets showing higher lopsidedness. These findings are in good agreement with predictions from simulations of dwarf-dwarf tidal interactions producing off-centre bars. We find that the majority of galaxies with off-centre bars are of Magellanic type, with a median mass of $10^{9.6} M_{\odot}$, and 91% of them having $M_{\star}<3\times10^{10} M_{\odot}$, the characteristic mass at which galaxies start having higher central concentrations attributed to the presence of bulges. We conduct a search for companions to test the hypothesis of tidal interactions, but find that a similar fraction of galaxies with offset bars have companions within 100 kpc as galaxies with centred bars. Although this may be due to the incompleteness of the SDSS spectroscopic survey at the faint end, alternative scenarios that give rise to offset bars such as interactions with dark companions or the effect of lopsided halo potentials should be considered. Future observations are needed to confirm possible low mass companion candidates and to determine the shape of the dark matter halo, in order to find the explanation for the off-centre bars in these galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1705.00007v1-abstract-full').style.display = 'none'; document.getElementById('1705.00007v1-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 April, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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, 9 figures, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1704.06269">arXiv:1704.06269</a> <span> [<a href="https://arxiv.org/pdf/1704.06269">pdf</a>, <a href="https://arxiv.org/format/1704.06269">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/stx973">10.1093/mnras/stx973 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galaxy Zoo: The interplay of quenching mechanisms in the group environment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Smethurst%2C+R+J">R. J. Smethurst</a>, <a href="/search/astro-ph?searchtype=author&query=Lintott%2C+C+J">C. J. Lintott</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S+P">S. P. Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Hart%2C+R+E">R. E. Hart</a>, <a href="/search/astro-ph?searchtype=author&query=Kruk%2C+S+J">S. J. Kruk</a>, <a href="/search/astro-ph?searchtype=author&query=Masters%2C+K+L">K. L. Masters</a>, <a href="/search/astro-ph?searchtype=author&query=Nichol%2C+R+C">R. C. Nichol</a>, <a href="/search/astro-ph?searchtype=author&query=Simmons%2C+B+D">B. D. Simmons</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="1704.06269v1-abstract-short" style="display: inline;"> Does the environment of a galaxy directly influence the quenching history of a galaxy? Here we investigate the detailed morphological structures and star formation histories of a sample of SDSS group galaxies with both classifications from Galaxy Zoo 2 and NUV detections in GALEX. We use the optical and NUV colours to infer the quenching time and rate describing a simple exponentially declining SF… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1704.06269v1-abstract-full').style.display = 'inline'; document.getElementById('1704.06269v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1704.06269v1-abstract-full" style="display: none;"> Does the environment of a galaxy directly influence the quenching history of a galaxy? Here we investigate the detailed morphological structures and star formation histories of a sample of SDSS group galaxies with both classifications from Galaxy Zoo 2 and NUV detections in GALEX. We use the optical and NUV colours to infer the quenching time and rate describing a simple exponentially declining SFH for each galaxy, along with a control sample of field galaxies. We find that the time since quenching and the rate of quenching do not correlate with the relative velocity of a satellite but are correlated with the group potential. This quenching occurs within an average quenching timescale of $\sim2.5~\rm{Gyr}$ from star forming to complete quiescence, during an average infall time (from $\sim 10R_{200}$ to $0.01R_{200}$) of $\sim 2.6~\rm{Gyr}$. Our results suggest that the environment does play a direct role in galaxy quenching through quenching mechanisms which are correlated with the group potential, such as harassment, interactions or starvation. Environmental quenching mechanisms which are correlated with satellite velocity, such as ram pressure stripping, are not the main cause of quenching in the group environment. We find that no single mechanism dominates over another, except in the most extreme environments or masses. Instead an interplay of mergers, mass & morphological quenching and environment driven quenching mechanisms dependent on the group potential drive galaxy evolution in groups. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1704.06269v1-abstract-full').style.display = 'none'; document.getElementById('1704.06269v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 April, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">20 pages, 11 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1703.02053">arXiv:1703.02053</a> <span> [<a href="https://arxiv.org/pdf/1703.02053">pdf</a>, <a href="https://arxiv.org/format/1703.02053">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/stx581">10.1093/mnras/stx581 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galaxy Zoo: star-formation versus spiral arm number </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hart%2C+R+E">Ross E. Hart</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S+P">Steven P. Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Casteels%2C+K+R+V">Kevin R. V Casteels</a>, <a href="/search/astro-ph?searchtype=author&query=Kruk%2C+S+J">Sandor J. Kruk</a>, <a href="/search/astro-ph?searchtype=author&query=Lintott%2C+C+J">Chris J. Lintott</a>, <a href="/search/astro-ph?searchtype=author&query=Masters%2C+K+L">Karen L. Masters</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="1703.02053v1-abstract-short" style="display: inline;"> Spiral arms are common features in low-redshift disc galaxies, and are prominent sites of star-formation and dust obscuration. However, spiral structure can take many forms: from galaxies displaying two strong `grand design' arms, to those with many `flocculent' arms. We investigate how these different arm types are related to a galaxy's star-formation and gas properties by making use of visual sp… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.02053v1-abstract-full').style.display = 'inline'; document.getElementById('1703.02053v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1703.02053v1-abstract-full" style="display: none;"> Spiral arms are common features in low-redshift disc galaxies, and are prominent sites of star-formation and dust obscuration. However, spiral structure can take many forms: from galaxies displaying two strong `grand design' arms, to those with many `flocculent' arms. We investigate how these different arm types are related to a galaxy's star-formation and gas properties by making use of visual spiral arm number measurements from Galaxy Zoo 2. We combine UV and mid-IR photometry from GALEX and WISE to measure the rates and relative fractions of obscured and unobscured star formation in a sample of low-redshift SDSS spirals. Total star formation rate has little dependence on spiral arm multiplicity, but two-armed spirals convert their gas to stars more efficiently. We find significant differences in the fraction of obscured star-formation: an additional $\sim 10$ per cent of star-formation in two-armed galaxies is identified via mid-IR dust emission, compared to that in many-armed galaxies. The latter are also significantly offset below the IRX-$尾$ relation for low-redshift star-forming galaxies. We present several explanations for these differences versus arm number: variations in the spatial distribution, sizes or clearing timescales of star-forming regions (i.e., molecular clouds), or contrasting recent star-formation histories. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.02053v1-abstract-full').style.display = 'none'; document.getElementById('1703.02053v1-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 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">15 pages, 13 figures, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1701.06483">arXiv:1701.06483</a> <span> [<a href="https://arxiv.org/pdf/1701.06483">pdf</a>, <a href="https://arxiv.org/format/1701.06483">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/stx228">10.1093/mnras/stx228 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> OMEGA -- OSIRIS Mapping of Emission-line Galaxies in A901/2: II. -- Environmental influence on integrated star formation properties and AGN activity </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Del+Pino%2C+B+R">Bruno Rodr铆guez Del Pino</a>, <a href="/search/astro-ph?searchtype=author&query=Arag%C3%B3n-Salamanca%2C+A">Alfonso Arag贸n-Salamanca</a>, <a href="/search/astro-ph?searchtype=author&query=Chies-Santos%2C+A+L">Ana L. Chies-Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Weinzirl%2C+T">Tim Weinzirl</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S+P">Steven P. Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Gray%2C+M+E">Meghan E. Gray</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6hm%2C+A">Asmus B枚hm</a>, <a href="/search/astro-ph?searchtype=author&query=Wolf%2C+C">Christian Wolf</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="1701.06483v1-abstract-short" style="display: inline;"> We present a study of the star formation and AGN activity for galaxies in the Abell 901/2 multi-cluster system at z~0.167 as part of the OMEGA survey. Using Tuneable Filter data obtained with the OSIRIS instrument at the GTC we produce spectra covering the Halpha and [N II] spectral lines for more than 400 galaxies. Using optical emission-line diagnostics, we identify a significant number of galax… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1701.06483v1-abstract-full').style.display = 'inline'; document.getElementById('1701.06483v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1701.06483v1-abstract-full" style="display: none;"> We present a study of the star formation and AGN activity for galaxies in the Abell 901/2 multi-cluster system at z~0.167 as part of the OMEGA survey. Using Tuneable Filter data obtained with the OSIRIS instrument at the GTC we produce spectra covering the Halpha and [N II] spectral lines for more than 400 galaxies. Using optical emission-line diagnostics, we identify a significant number of galaxies hosting AGN, which tend to have high masses and a broad range of morphologies. Moreover, within the environmental densities probed by our study, we find no environmental dependence on the fraction of galaxies hosting AGN. The analysis of the integrated Halpha emission shows that the specific star formation rates (SSFRs) of a majority of the cluster galaxies are below the field values for a given stellar mass. We interpret this result as evidence for a slow decrease in the star formation activity of star-forming galaxies as they fall into higher-density regions, contrary to some previous studies which suggested a rapid truncation of star formation. We find that most of the intermediate- and high-mass spiral galaxies go through a phase in which their star formation is suppressed but still retain significant star-formation activity. During this phase, these galaxies tend to retain their spiral morphology while their colours become redder. The presence of this type of galaxies in high density regions indicates that the physical mechanism responsible for suppressing star-formation affects mainly the gas component of the galaxies, suggesting that ram-pressure stripping or starvation are potentially responsible. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1701.06483v1-abstract-full').style.display = 'none'; document.getElementById('1701.06483v1-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 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">20 pages, 16 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/1612.01957">arXiv:1612.01957</a> <span> [<a href="https://arxiv.org/pdf/1612.01957">pdf</a>, <a href="https://arxiv.org/format/1612.01957">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/stw3183">10.1093/mnras/stw3183 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Untangling galaxy components: full spectral bulge-disc decomposition </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Tabor%2C+M">Martha Tabor</a>, <a href="/search/astro-ph?searchtype=author&query=Merrifield%2C+M">Michael Merrifield</a>, <a href="/search/astro-ph?searchtype=author&query=Arag%C3%B3n-Salamanca%2C+A">Alfonso Arag贸n-Salamanca</a>, <a href="/search/astro-ph?searchtype=author&query=Cappellari%2C+M">Michele Cappellari</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S+P">Steven P. Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Johnston%2C+E">Evelyn Johnston</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="1612.01957v1-abstract-short" style="display: inline;"> To ascertain whether photometric decompositions of galaxies into bulges and disks are astrophysically meaningful, we have developed a new technique to decompose spectral data cubes into separate bulge and disk components, subject only to the constraint that they reproduce the conventional photometric decomposition. These decompositions allow us to study the kinematic and stellar population propert… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1612.01957v1-abstract-full').style.display = 'inline'; document.getElementById('1612.01957v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1612.01957v1-abstract-full" style="display: none;"> To ascertain whether photometric decompositions of galaxies into bulges and disks are astrophysically meaningful, we have developed a new technique to decompose spectral data cubes into separate bulge and disk components, subject only to the constraint that they reproduce the conventional photometric decomposition. These decompositions allow us to study the kinematic and stellar population properties of the individual components and how they vary with position, in order to assess their plausibility as discrete elements, and to start to reconstruct their distinct formation histories. An initial application of this method to CALIFA integral field unit observations of three isolated S0 galaxies confirms that in regions where both bulge and disc contribute significantly to the flux they can be physically and robustly decomposed into a rotating dispersion-dominated bulge component, and a rotating low-dispersion disc component. Analysis of the resulting stellar populations shows that the bulges of these galaxies have a range of ages relative to their discs, indicating that a variety of processes are necessary to describe their evolution. This simple test case indicates the broad potential for extracting from spectral data cubes the full spectral data of a wide variety of individual galaxy components, and for using such decompositions to understand the interplay between these various structures, and hence how such systems formed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1612.01957v1-abstract-full').style.display = 'none'; document.getElementById('1612.01957v1-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 December, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">11 pages, 10 figures, to be published in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1611.00609">arXiv:1611.00609</a> <span> [<a href="https://arxiv.org/pdf/1611.00609">pdf</a>, <a href="https://arxiv.org/ps/1611.00609">ps</a>, <a href="https://arxiv.org/format/1611.00609">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/stw2823">10.1093/mnras/stw2823 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> SDSS-IV MaNGA: Bulge-Disc Decomposition of IFU Datacubes (BUDDI) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Johnston%2C+E+J">Evelyn J. Johnston</a>, <a href="/search/astro-ph?searchtype=author&query=Haeussler%2C+B">Boris Haeussler</a>, <a href="/search/astro-ph?searchtype=author&query=Aragon-Salamanca%2C+A">Alfonso Aragon-Salamanca</a>, <a href="/search/astro-ph?searchtype=author&query=Merrifield%2C+M+R">Michael R. Merrifield</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S">Steven Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Bershady%2C+M+A">Matthew A. Bershady</a>, <a href="/search/astro-ph?searchtype=author&query=Bundy%2C+K">Kevin Bundy</a>, <a href="/search/astro-ph?searchtype=author&query=Drory%2C+N">Niv Drory</a>, <a href="/search/astro-ph?searchtype=author&query=Fu%2C+H">Hai Fu</a>, <a href="/search/astro-ph?searchtype=author&query=Law%2C+D">David Law</a>, <a href="/search/astro-ph?searchtype=author&query=Nitschelm%2C+C">Christian Nitschelm</a>, <a href="/search/astro-ph?searchtype=author&query=Thomas%2C+D">Daniel Thomas</a>, <a href="/search/astro-ph?searchtype=author&query=Lopes%2C+A+R">Alexandre Roman Lopes</a>, <a href="/search/astro-ph?searchtype=author&query=Wake%2C+D">David Wake</a>, <a href="/search/astro-ph?searchtype=author&query=Yan%2C+R">Renbin Yan</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="1611.00609v1-abstract-short" style="display: inline;"> With the availability of large integral-field unit (IFU) spectral surveys of nearby galaxies, there is now the potential to extract spectral information from across the bulges and discs of galaxies in a systematic way. This information can address questions such as how these components built up with time, how galaxies evolve and whether their evolution depends on other properties of the galaxy suc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.00609v1-abstract-full').style.display = 'inline'; document.getElementById('1611.00609v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1611.00609v1-abstract-full" style="display: none;"> With the availability of large integral-field unit (IFU) spectral surveys of nearby galaxies, there is now the potential to extract spectral information from across the bulges and discs of galaxies in a systematic way. This information can address questions such as how these components built up with time, how galaxies evolve and whether their evolution depends on other properties of the galaxy such as its mass or environment. We present BUDDI, a new approach to fit the two-dimensional light profiles of galaxies as a function of wavelength to extract the spectral properties of these galaxies' discs and bulges. The fitting is carried out using GalfitM, a modified form of Galfit which can fit multi-waveband images simultaneously. The benefit of this technique over traditional multi-waveband fits is that the stellar populations of each component can be constrained using knowledge over the whole image and spectrum available. The decomposition has been developed using commissioning data from the SDSS-IV Mapping Nearby Galaxies at APO (MaNGA) survey with redshifts z<0.14 and coverage of at least 1.5 effective radii for a spatial resolution of 2.5 arcsec FWHM and field of view of >22 arcsec, but can be applied to any IFU data of a nearby galaxy with similar or better spatial resolution and coverage. We present an overview of the fitting process, the results from our tests, and we finish with example stellar population analyses of early-type galaxies from the MaNGA survey to give an indication of the scientific potential of applying bulge-disc decomposition to IFU data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.00609v1-abstract-full').style.display = 'none'; document.getElementById('1611.00609v1-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, 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">Accepted for publication in MNRAS. BUDDI will be publicly available soon, please contact Evelyn Johnston (evelyn.johnston@eso.org) to be added to the mailing list</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1610.03070">arXiv:1610.03070</a> <span> [<a href="https://arxiv.org/pdf/1610.03070">pdf</a>, <a href="https://arxiv.org/format/1610.03070">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/stw2587">10.1093/mnras/stw2587 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galaxy Zoo: Quantitative Visual Morphological Classifications for 48,000 galaxies from CANDELS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Simmons%2C+B+D">B. D. Simmons</a>, <a href="/search/astro-ph?searchtype=author&query=Lintott%2C+C">Chris Lintott</a>, <a href="/search/astro-ph?searchtype=author&query=Willett%2C+K+W">Kyle W. Willett</a>, <a href="/search/astro-ph?searchtype=author&query=Masters%2C+K+L">Karen L. Masters</a>, <a href="/search/astro-ph?searchtype=author&query=Kartaltepe%2C+J+S">Jeyhan S. Kartaltepe</a>, <a href="/search/astro-ph?searchtype=author&query=H%C3%A4u%C3%9Fler%2C+B">Boris H盲u脽ler</a>, <a href="/search/astro-ph?searchtype=author&query=Kaviraj%2C+S">Sugata Kaviraj</a>, <a href="/search/astro-ph?searchtype=author&query=Krawczyk%2C+C">Coleman Krawczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Kruk%2C+S+J">S. J. Kruk</a>, <a href="/search/astro-ph?searchtype=author&query=McIntosh%2C+D+H">Daniel H. McIntosh</a>, <a href="/search/astro-ph?searchtype=author&query=Smethurst%2C+R+J">R. J. Smethurst</a>, <a href="/search/astro-ph?searchtype=author&query=Nichol%2C+R+C">Robert C. Nichol</a>, <a href="/search/astro-ph?searchtype=author&query=Scarlata%2C+C">Claudia Scarlata</a>, <a href="/search/astro-ph?searchtype=author&query=Schawinski%2C+K">Kevin Schawinski</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C+J">Christopher J. Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=Almaini%2C+O">Omar Almaini</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+H+C">Henry C. Ferguson</a>, <a href="/search/astro-ph?searchtype=author&query=Fortson%2C+L">Lucy Fortson</a>, <a href="/search/astro-ph?searchtype=author&query=Hartley%2C+W">William Hartley</a>, <a href="/search/astro-ph?searchtype=author&query=Kocevski%2C+D">Dale Kocevski</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Mortlock%2C+A">Alice Mortlock</a>, <a href="/search/astro-ph?searchtype=author&query=Newman%2C+J+A">Jeffrey A. Newman</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S+P">Steven P. Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Grogin%2C+N+A">N. A. Grogin</a> , et al. (23 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="1610.03070v1-abstract-short" style="display: inline;"> We present quantified visual morphologies of approximately 48,000 galaxies observed in three Hubble Space Telescope legacy fields by the Cosmic And Near-infrared Deep Extragalactic Legacy Survey (CANDELS) and classified by participants in the Galaxy Zoo project. 90% of galaxies have z < 3 and are observed in rest-frame optical wavelengths by CANDELS. Each galaxy received an average of 40 independe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1610.03070v1-abstract-full').style.display = 'inline'; document.getElementById('1610.03070v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1610.03070v1-abstract-full" style="display: none;"> We present quantified visual morphologies of approximately 48,000 galaxies observed in three Hubble Space Telescope legacy fields by the Cosmic And Near-infrared Deep Extragalactic Legacy Survey (CANDELS) and classified by participants in the Galaxy Zoo project. 90% of galaxies have z < 3 and are observed in rest-frame optical wavelengths by CANDELS. Each galaxy received an average of 40 independent classifications, which we combine into detailed morphological information on galaxy features such as clumpiness, bar instabilities, spiral structure, and merger and tidal signatures. We apply a consensus-based classifier weighting method that preserves classifier independence while effectively down-weighting significantly outlying classifications. After analysing the effect of varying image depth on reported classifications, we also provide depth-corrected classifications which both preserve the information in the deepest observations and also enable the use of classifications at comparable depths across the full survey. Comparing the Galaxy Zoo classifications to previous classifications of the same galaxies shows very good agreement; for some applications the high number of independent classifications provided by Galaxy Zoo provides an advantage in selecting galaxies with a particular morphological profile, while in others the combination of Galaxy Zoo with other classifications is a more promising approach than using any one method alone. We combine the Galaxy Zoo classifications of "smooth" galaxies with parametric morphologies to select a sample of featureless disks at 1 < z < 3, which may represent a dynamically warmer progenitor population to the settled disk galaxies seen at later epochs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1610.03070v1-abstract-full').style.display = 'none'; document.getElementById('1610.03070v1-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 October, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">30 pages, 14 figures, MNRAS accepted. Galaxy classifications available at data.galaxyzoo.org</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1610.03068">arXiv:1610.03068</a> <span> [<a href="https://arxiv.org/pdf/1610.03068">pdf</a>, <a href="https://arxiv.org/format/1610.03068">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/stw2568">10.1093/mnras/stw2568 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galaxy Zoo: Morphological Classifications for 120,000 Galaxies in HST Legacy Imaging </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Willett%2C+K+W">Kyle W. Willett</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+M+A">Melanie A. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S+P">Steven P. Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Lintott%2C+C+J">Chris J. Lintott</a>, <a href="/search/astro-ph?searchtype=author&query=Masters%2C+K+L">Karen L. Masters</a>, <a href="/search/astro-ph?searchtype=author&query=Scarlata%2C+C">Claudia Scarlata</a>, <a href="/search/astro-ph?searchtype=author&query=Simmons%2C+B+D">B. D. Simmons</a>, <a href="/search/astro-ph?searchtype=author&query=Beck%2C+M">Melanie Beck</a>, <a href="/search/astro-ph?searchtype=author&query=Cardamone%2C+C+N">Carolin N. Cardamone</a>, <a href="/search/astro-ph?searchtype=author&query=Cheung%2C+E">Edmond Cheung</a>, <a href="/search/astro-ph?searchtype=author&query=Edmondson%2C+E+M">Edward M. Edmondson</a>, <a href="/search/astro-ph?searchtype=author&query=Fortson%2C+L+F">Lucy F. Fortson</a>, <a href="/search/astro-ph?searchtype=author&query=Griffith%2C+R+L">Roger L. Griffith</a>, <a href="/search/astro-ph?searchtype=author&query=Haeussler%2C+B">Boris Haeussler</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+A">Anna Han</a>, <a href="/search/astro-ph?searchtype=author&query=Hart%2C+R">Ross Hart</a>, <a href="/search/astro-ph?searchtype=author&query=Melvin%2C+T">Thomas Melvin</a>, <a href="/search/astro-ph?searchtype=author&query=Parrish%2C+M">Michael Parrish</a>, <a href="/search/astro-ph?searchtype=author&query=Schawinski%2C+K">Kevin Schawinski</a>, <a href="/search/astro-ph?searchtype=author&query=Smethurst%2C+R+J">R. J. Smethurst</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+A+M">Arfon M. Smith</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="1610.03068v2-abstract-short" style="display: inline;"> We present the data release paper for the Galaxy Zoo: Hubble (GZH) project. This is the third phase in a large effort to measure reliable, detailed morphologies of galaxies by using crowdsourced visual classifications of colour composite images. Images in GZH were selected from various publicly-released Hubble Space Telescope Legacy programs conducted with the Advanced Camera for Surveys, with fil… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1610.03068v2-abstract-full').style.display = 'inline'; document.getElementById('1610.03068v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1610.03068v2-abstract-full" style="display: none;"> We present the data release paper for the Galaxy Zoo: Hubble (GZH) project. This is the third phase in a large effort to measure reliable, detailed morphologies of galaxies by using crowdsourced visual classifications of colour composite images. Images in GZH were selected from various publicly-released Hubble Space Telescope Legacy programs conducted with the Advanced Camera for Surveys, with filters that probe the rest-frame optical emission from galaxies out to $z \sim 1$. The bulk of the sample is selected to have $m_{I814W} < 23.5$,but goes as faint as $m_{I814W} < 26.8$ for deep images combined over 5 epochs. The median redshift of the combined samples is $z = 0.9 \pm 0.6$, with a tail extending out to $z \sim 4$. The GZH morphological data include measurements of both bulge- and disk-dominated galaxies, details on spiral disk structure that relate to the Hubble type, bar identification, and numerous measurements of clump identification and geometry. This paper also describes a new method for calibrating morphologies for galaxies of different luminosities and at different redshifts by using artificially-redshifted galaxy images as a baseline. The GZH catalogue contains both raw and calibrated morphological vote fractions for 119,849 galaxies, providing the largest dataset to date suitable for large-scale studies of galaxy evolution out to $z \sim 1$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1610.03068v2-abstract-full').style.display = 'none'; document.getElementById('1610.03068v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 October, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 October, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">32 pages, 14 figures. Accepted to MNRAS. Full data tables are available electronically from journal or https://data.galaxyzoo.org</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1609.00023">arXiv:1609.00023</a> <span> [<a href="https://arxiv.org/pdf/1609.00023">pdf</a>, <a href="https://arxiv.org/format/1609.00023">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/stw2204">10.1093/mnras/stw2204 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galaxy Zoo: Evidence for rapid, recent quenching within a population of AGN host galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Smethurst%2C+R+J">R. J. Smethurst</a>, <a href="/search/astro-ph?searchtype=author&query=Lintott%2C+C+J">C. J. Lintott</a>, <a href="/search/astro-ph?searchtype=author&query=Simmons%2C+B+D">B. D. Simmons</a>, <a href="/search/astro-ph?searchtype=author&query=Schawinski%2C+K">K. Schawinski</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S+P">S. P. Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Cardamone%2C+C+N">C. N. Cardamone</a>, <a href="/search/astro-ph?searchtype=author&query=Kruk%2C+S+J">S. J. Kruk</a>, <a href="/search/astro-ph?searchtype=author&query=Masters%2C+K+L">K. L. Masters</a>, <a href="/search/astro-ph?searchtype=author&query=Urry%2C+C+M">C. M. Urry</a>, <a href="/search/astro-ph?searchtype=author&query=Willett%2C+K+W">K. W. Willett</a>, <a href="/search/astro-ph?searchtype=author&query=Wong%2C+O+I">O. I. Wong</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="1609.00023v1-abstract-short" style="display: inline;"> We present a population study of the star formation history of 1244 Type 2 AGN host galaxies, compared to 6107 inactive galaxies. A Bayesian method is used to determine individual galaxy star formation histories, which are then collated to visualise the distribution for quenching and quenched galaxies within each population. We find evidence for some of the Type 2 AGN host galaxies having undergon… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.00023v1-abstract-full').style.display = 'inline'; document.getElementById('1609.00023v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1609.00023v1-abstract-full" style="display: none;"> We present a population study of the star formation history of 1244 Type 2 AGN host galaxies, compared to 6107 inactive galaxies. A Bayesian method is used to determine individual galaxy star formation histories, which are then collated to visualise the distribution for quenching and quenched galaxies within each population. We find evidence for some of the Type 2 AGN host galaxies having undergone a rapid drop in their star formation rate within the last 2 Gyr. AGN feedback is therefore important at least for this population of galaxies. This result is not seen for the quenching and quenched inactive galaxies whose star formation histories are dominated by the effects of downsizing at earlier epochs, a secondary effect for the AGN host galaxies. We show that histories of rapid quenching cannot account fully for the quenching of all the star formation in a galaxy's lifetime across the population of quenched AGN host galaxies, and that histories of slower quenching, attributed to secular (non-violent) evolution, are also key in their evolution. This is in agreement with recent results showing both merger-driven and non-merger processes are contributing to the co-evolution of galaxies and supermassive black holes. The availability of gas in the reservoirs of a galaxy, and its ability to be replenished, appear to be the key drivers behind this co-evolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.00023v1-abstract-full').style.display = 'none'; document.getElementById('1609.00023v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 August, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">12 pages, 11 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1608.03495">arXiv:1608.03495</a> <span> [<a href="https://arxiv.org/pdf/1608.03495">pdf</a>, <a href="https://arxiv.org/format/1608.03495">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/10.1051/0004-6361/201628715">10.1051/0004-6361/201628715 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galaxy And Mass Assembly (GAMA): Galaxy colour gradients versus colour, structure and luminosity </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kennedy%2C+R">Rebecca Kennedy</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S+P">Steven P. Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=H%C3%A4u%C3%9Fler%2C+B">Boris H盲u脽ler</a>, <a href="/search/astro-ph?searchtype=author&query=Brough%2C+S">Sarah Brough</a>, <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B">Benne Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A+M">Andrew M. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Vika%2C+M">Marina Vika</a>, <a href="/search/astro-ph?searchtype=author&query=Vulcani%2C+B">Benedetta Vulcani</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="1608.03495v1-abstract-short" style="display: inline;"> Using single-component fits to SDSS/UKIDSS images of galaxies in the G09 region of the GAMA survey we study radial colour gradients across the galaxy population. We use the multiwavelength information provided by MegaMorph analysis of galaxy light profiles to calculate intrinsic colour gradients, and divide into six subsamples split by overall S茅rsic index ($n$) and galaxy colour. We find a bimoda… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1608.03495v1-abstract-full').style.display = 'inline'; document.getElementById('1608.03495v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1608.03495v1-abstract-full" style="display: none;"> Using single-component fits to SDSS/UKIDSS images of galaxies in the G09 region of the GAMA survey we study radial colour gradients across the galaxy population. We use the multiwavelength information provided by MegaMorph analysis of galaxy light profiles to calculate intrinsic colour gradients, and divide into six subsamples split by overall S茅rsic index ($n$) and galaxy colour. We find a bimodality in the colour gradients of high- and low-$n$ galaxies in all wavebands, which varies with overall galaxy luminosity. Global trends in colour gradients therefore result from combining the contrasting behaviour of a number of different galaxy populations. The ubiquity of strong negative colour gradients supports the picture of inside-out growth through gas accretion for blue, low-$n$ galaxies, and through dry minor mergers for red, high-$n$ galaxies. An exception is the blue high-n population, with properties indicative of dissipative major mergers. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1608.03495v1-abstract-full').style.display = 'none'; document.getElementById('1608.03495v1-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, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">4 pages, 2 figures, accepted by 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 593, A84 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1607.01019">arXiv:1607.01019</a> <span> [<a href="https://arxiv.org/pdf/1607.01019">pdf</a>, <a href="https://arxiv.org/format/1607.01019">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/10.1093/mnras/stw1588">10.1093/mnras/stw1588 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galaxy Zoo: comparing the demographics of spiral arm number and a new method for correcting redshift bias </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hart%2C+R+E">Ross E. Hart</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S+P">Steven P. Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Willett%2C+K+W">Kyle W. Willett</a>, <a href="/search/astro-ph?searchtype=author&query=Masters%2C+K+L">Karen L. Masters</a>, <a href="/search/astro-ph?searchtype=author&query=Cardamone%2C+C">Carolin Cardamone</a>, <a href="/search/astro-ph?searchtype=author&query=Lintott%2C+C+J">Chris J. Lintott</a>, <a href="/search/astro-ph?searchtype=author&query=Mackay%2C+R+J">Robert J. Mackay</a>, <a href="/search/astro-ph?searchtype=author&query=Nichol%2C+R+C">Robert C. Nichol</a>, <a href="/search/astro-ph?searchtype=author&query=Rosslowe%2C+C+K">Christopher K. Rosslowe</a>, <a href="/search/astro-ph?searchtype=author&query=Simmons%2C+B+D">Brooke D. Simmons</a>, <a href="/search/astro-ph?searchtype=author&query=Smethurst%2C+R+J">Rebecca J Smethurst</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="1607.01019v1-abstract-short" style="display: inline;"> The majority of galaxies in the local Universe exhibit spiral structure with a variety of forms. Many galaxies possess two prominent spiral arms, some have more, while others display a many-armed flocculent appearance. Spiral arms are associated with enhanced gas content and star-formation in the disks of low-redshift galaxies, so are important in the understanding of star-formation in the local u… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1607.01019v1-abstract-full').style.display = 'inline'; document.getElementById('1607.01019v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1607.01019v1-abstract-full" style="display: none;"> The majority of galaxies in the local Universe exhibit spiral structure with a variety of forms. Many galaxies possess two prominent spiral arms, some have more, while others display a many-armed flocculent appearance. Spiral arms are associated with enhanced gas content and star-formation in the disks of low-redshift galaxies, so are important in the understanding of star-formation in the local universe. As both the visual appearance of spiral structure, and the mechanisms responsible for it vary from galaxy to galaxy, a reliable method for defining spiral samples with different visual morphologies is required. In this paper, we develop a new debiasing method to reliably correct for redshift-dependent bias in Galaxy Zoo 2, and release the new set of debiased classifications. Using these, a luminosity-limited sample of ~18,000 Sloan Digital Sky Survey spiral galaxies is defined, which are then further sub-categorised by spiral arm number. In order to explore how different spiral galaxies form, the demographics of spiral galaxies with different spiral arm numbers are compared. It is found that whilst all spiral galaxies occupy similar ranges of stellar mass and environment, many-armed galaxies display much bluer colours than their two-armed counterparts. We conclude that two-armed structure is ubiquitous in star-forming disks, whereas many-armed spiral structure appears to be a short-lived phase, associated with more recent, stochastic star-formation activity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1607.01019v1-abstract-full').style.display = 'none'; document.getElementById('1607.01019v1-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> 4 July, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">Accepted to MNRAS, 22 pages, 19 figures, 2 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1605.04720">arXiv:1605.04720</a> <span> [<a href="https://arxiv.org/pdf/1605.04720">pdf</a>, <a href="https://arxiv.org/format/1605.04720">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/stw1176">10.1093/mnras/stw1176 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galaxy And Mass Assembly (GAMA): Understanding the wavelength dependence of galaxy structure with bulge-disc decompositions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kennedy%2C+R">Rebecca Kennedy</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S+P">Steven P. Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=H%C3%A4u%C3%9Fler%2C+B">Boris H盲u脽ler</a>, <a href="/search/astro-ph?searchtype=author&query=Baldry%2C+I">Ivan Baldry</a>, <a href="/search/astro-ph?searchtype=author&query=Bremer%2C+M">Malcolm Bremer</a>, <a href="/search/astro-ph?searchtype=author&query=Brough%2C+S">Sarah Brough</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+M+J+I">Michael J. I. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Driver%2C+S">Simon Driver</a>, <a href="/search/astro-ph?searchtype=author&query=Duncan%2C+K">Kenneth Duncan</a>, <a href="/search/astro-ph?searchtype=author&query=Graham%2C+A+W">Alister W. Graham</a>, <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B+W">Benne W. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A+M">Andrew M. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Kelvin%2C+L+S">Lee S. Kelvin</a>, <a href="/search/astro-ph?searchtype=author&query=Lange%2C+R">Rebecca Lange</a>, <a href="/search/astro-ph?searchtype=author&query=Phillipps%2C+S">Steven Phillipps</a>, <a href="/search/astro-ph?searchtype=author&query=Vika%2C+M">Marina Vika</a>, <a href="/search/astro-ph?searchtype=author&query=Vulcani%2C+B">Benedetta Vulcani</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="1605.04720v1-abstract-short" style="display: inline;"> With a large sample of bright, low-redshift galaxies with optical$-$near-IR imaging from the GAMA survey we use bulge-disc decompositions to understand the wavelength-dependent behavior of single-S茅rsic structural measurements. We denote the variation in single-S茅rsic index with wavelength as $\mathcal{N}$, likewise for effective radius we use $\mathcal{R}$. We find that most galaxies with a sub… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.04720v1-abstract-full').style.display = 'inline'; document.getElementById('1605.04720v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1605.04720v1-abstract-full" style="display: none;"> With a large sample of bright, low-redshift galaxies with optical$-$near-IR imaging from the GAMA survey we use bulge-disc decompositions to understand the wavelength-dependent behavior of single-S茅rsic structural measurements. We denote the variation in single-S茅rsic index with wavelength as $\mathcal{N}$, likewise for effective radius we use $\mathcal{R}$. We find that most galaxies with a substantial disc, even those with no discernable bulge, display a high value of $\mathcal{N}$. The increase in S茅rsic index to longer wavelengths is therefore intrinsic to discs, apparently resulting from radial variations in stellar population and/or dust reddening. Similarly, low values of $\mathcal{R}$ ($<$ 1) are found to be ubiquitous, implying an element of universality in galaxy colour gradients. We also study how bulge and disc colour distributions vary with galaxy type. We find that, rather than all bulges being red and all discs being blue in absolute terms, both components become redder for galaxies with redder total colours. We even observe that bulges in bluer galaxies are typically bluer than discs in red galaxies, and that bulges and discs are closer in colour for fainter galaxies. Trends in total colour are therefore not solely due to the colour or flux dominance of the bulge or disc. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.04720v1-abstract-full').style.display = 'none'; document.getElementById('1605.04720v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 May, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">16 pages, 13 figures, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1604.00435">arXiv:1604.00435</a> <span> [<a href="https://arxiv.org/pdf/1604.00435">pdf</a>, <a href="https://arxiv.org/format/1604.00435">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/stw649">10.1093/mnras/stw649 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galaxy Zoo: Mergers - Dynamical Models of Interacting Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Holincheck%2C+A+J">Anthony J. Holincheck</a>, <a href="/search/astro-ph?searchtype=author&query=Wallin%2C+J+F">John F. Wallin</a>, <a href="/search/astro-ph?searchtype=author&query=Borne%2C+K">Kirk Borne</a>, <a href="/search/astro-ph?searchtype=author&query=Fortson%2C+L">Lucy Fortson</a>, <a href="/search/astro-ph?searchtype=author&query=Lintott%2C+C">Chris Lintott</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+A+M">Arfon M. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S">Steven Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Keel%2C+W+C">William C. Keel</a>, <a href="/search/astro-ph?searchtype=author&query=Parrish%2C+M">Michael Parrish</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="1604.00435v1-abstract-short" style="display: inline;"> The dynamical history of most merging galaxies is not well understood. Correlations between galaxy interaction and star formation have been found in previous studies, but require the context of the physical history of merging systems for full insight into the processes that lead to enhanced star formation. We present the results of simulations that reconstruct the orbit trajectories and disturbed… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.00435v1-abstract-full').style.display = 'inline'; document.getElementById('1604.00435v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1604.00435v1-abstract-full" style="display: none;"> The dynamical history of most merging galaxies is not well understood. Correlations between galaxy interaction and star formation have been found in previous studies, but require the context of the physical history of merging systems for full insight into the processes that lead to enhanced star formation. We present the results of simulations that reconstruct the orbit trajectories and disturbed morphologies of pairs of interacting galaxies. With the use of a restricted three-body simulation code and the help of Citizen Scientists, we sample 10^5 points in parameter space for each system. We demonstrate a successful recreation of the morphologies of 62 pairs of interacting galaxies through the review of more than 3 million simulations. We examine the level of convergence and uniqueness of the dynamical properties of each system. These simulations represent the largest collection of models of interacting galaxies to date, providing a valuable resource for the investigation of mergers. This paper presents the simulation parameters generated by the project. They are now publicly available in electronic format at http://data.galaxyzoo.org/mergers.html. Though our best-fit model parameters are not an exact match to previously published models, our method for determining uncertainty measurements will aid future comparisons between models. The dynamical clocks from our models agree with previous results of the time since the onset of star formation from star burst models in interacting systems and suggests that tidally induced star formation is triggered very soon after closest approach. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.00435v1-abstract-full').style.display = 'none'; document.getElementById('1604.00435v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 April, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">29 pages, 17 figures, 7 tables, Accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1602.01664">arXiv:1602.01664</a> <span> [<a href="https://arxiv.org/pdf/1602.01664">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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/10.1016/j.icarus.2016.01.021">10.1016/j.icarus.2016.01.021 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Moon Zoo citizen science project: Preliminary results for the Apollo 17 landing site </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bugiolacchi%2C+R">Roberto Bugiolacchi</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S">Steven Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Tar%2C+P">Paul Tar</a>, <a href="/search/astro-ph?searchtype=author&query=Thacker%2C+N">Neil Thacker</a>, <a href="/search/astro-ph?searchtype=author&query=Crawford%2C+I+A">Ian A. Crawford</a>, <a href="/search/astro-ph?searchtype=author&query=Joy%2C+K+H">Katherine H. Joy</a>, <a href="/search/astro-ph?searchtype=author&query=Grindrod%2C+P+M">Peter M. Grindrod</a>, <a href="/search/astro-ph?searchtype=author&query=Lintott%2C+C">Chris Lintott</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="1602.01664v1-abstract-short" style="display: inline;"> Moon Zoo is a citizen science project that utilises internet crowd-sourcing techniques. Moon Zoo users are asked to review high spatial resolution images from the Lunar Reconnaissance Orbiter Camera (LROC), onboard NASAs LRO spacecraft, and perform characterisation such as measuring impact crater sizes and identify morphological features of interest. The tasks are designed to address issues in lun… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1602.01664v1-abstract-full').style.display = 'inline'; document.getElementById('1602.01664v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1602.01664v1-abstract-full" style="display: none;"> Moon Zoo is a citizen science project that utilises internet crowd-sourcing techniques. Moon Zoo users are asked to review high spatial resolution images from the Lunar Reconnaissance Orbiter Camera (LROC), onboard NASAs LRO spacecraft, and perform characterisation such as measuring impact crater sizes and identify morphological features of interest. The tasks are designed to address issues in lunar science and to aid future exploration of the Moon. We have tested various methodologies and parameters therein to interrogate and reduce the Moon Zoo crater location and size dataset against a validated expert survey. We chose the Apollo 17 region as a test area since it offers a broad range of cratered terrains, including secondary-rich areas, older maria, and uplands. The assessment involved parallel testing in three key areas: (1) filtering of data to remove problematic mark-ups; (2) clustering methods of multiple notations per crater; and (3) derivation of alternative crater degradation indices, based on the statistical variability of multiple notations and the smoothness of local image structures. We compared different combinations of methods and parameters and assessed correlations between resulting crater summaries and the expert census. We derived the optimal data reduction steps and settings of the existing Moon Zoo crater data to agree with the expert census. Further, the regolith depth and crater degradation states derived from the data are also found to be in broad agreement with other estimates for the Apollo 17 region. Our study supports the validity of this citizen science project but also recommends improvements in key elements of the data acquisition planning and production. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1602.01664v1-abstract-full').style.display = 'none'; document.getElementById('1602.01664v1-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 February, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">Accepted for publication in Icarus</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1512.01185">arXiv:1512.01185</a> <span> [<a href="https://arxiv.org/pdf/1512.01185">pdf</a>, <a href="https://arxiv.org/format/1512.01185">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/stv2753">10.1093/mnras/stv2753 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The SLUGGS survey: chromo-dynamical modelling of the lenticular galaxy NGC 1023 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cortesi%2C+A">Arianna Cortesi</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=Pota%2C+V">Vincenzo Pota</a>, <a href="/search/astro-ph?searchtype=author&query=Foster%2C+C">Caroline Foster</a>, <a href="/search/astro-ph?searchtype=author&query=Coccato%2C+L">Lodovico Coccato</a>, <a href="/search/astro-ph?searchtype=author&query=de+Oliveira%2C+C+M">Claudia Mendes de Oliveira</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=Merrifield%2C+M+M">Michael M. Merrifield</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S+P">Steven P. Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Romanowsky%2C+A+J">Aaron J. Romanowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Brodie%2C+J+P">Jean P. Brodie</a>, <a href="/search/astro-ph?searchtype=author&query=Kartha%2C+S+S">Sreeja S. Kartha</a>, <a href="/search/astro-ph?searchtype=author&query=Alabi%2C+A+B">Adebusola B. Alabi</a>, <a href="/search/astro-ph?searchtype=author&query=Proctor%2C+R+N">Robert N. Proctor</a>, <a href="/search/astro-ph?searchtype=author&query=Almeida%2C+A">Andres Almeida</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="1512.01185v1-abstract-short" style="display: inline;"> Globular clusters (GCs) can be considered discrete, long-lived, dynamical tracers that retain crucial information about the assembly history of their parent galaxy. In this paper, we present a new catalogue of GC velocities and colours for the lenticular galaxy NGC 1023, we study their kinematics and spatial distribution, in comparison with the underlying stellar kinematics and surface brightness… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1512.01185v1-abstract-full').style.display = 'inline'; document.getElementById('1512.01185v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1512.01185v1-abstract-full" style="display: none;"> Globular clusters (GCs) can be considered discrete, long-lived, dynamical tracers that retain crucial information about the assembly history of their parent galaxy. In this paper, we present a new catalogue of GC velocities and colours for the lenticular galaxy NGC 1023, we study their kinematics and spatial distribution, in comparison with the underlying stellar kinematics and surface brightness profile, and we test a new method for studying GC properties. Specifically, we decompose the galaxy light into its spheroid (assumed to represent the bulge + halo components) and disk components and use it to assign to each GC a probability of belonging to one of the two components. Then we model the galaxy kinematics, assuming a disk and spheroidal component, using planetary nebulae (PNe) and integrated stellar light. We use this kinematic model and the probability previously obtained from the photometry to recalculate for each GC its likelihood of being associated with the disk, the spheroid, or neither. We find that the reddest GCs are likely to be associated with the disk, as found for faint fuzzies in this same galaxy, suggesting that the disk of this S0 galaxy originated at z ~ 2. The majority of blue GCs are found likely to be associated with the spheroidal (hot) component. The method also allows us to identify objects that are unlikely to be in equilibrium with the system. In NGC1023 some of the rejected GCs form a substructure in phase space that is connected with NGC 1023 companion galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1512.01185v1-abstract-full').style.display = 'none'; document.getElementById('1512.01185v1-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, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 10 figures, accepted 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/1509.06756">arXiv:1509.06756</a> <span> [<a href="https://arxiv.org/pdf/1509.06756">pdf</a>, <a href="https://arxiv.org/format/1509.06756">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/stv2032">10.1093/mnras/stv2032 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galaxy And Mass Assembly (GAMA): the wavelength dependence of galaxy structure versus redshift and luminosity </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kennedy%2C+R">Rebecca Kennedy</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S+P">Steven P. Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Baldry%2C+I">Ivan Baldry</a>, <a href="/search/astro-ph?searchtype=author&query=H%C3%A4u%C3%9Fler%2C+B">Boris H盲u脽ler</a>, <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B+W">Benne W. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A+M">Andrew M. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Kelvin%2C+L+S">Lee S. Kelvin</a>, <a href="/search/astro-ph?searchtype=author&query=Lange%2C+R">Rebecca Lange</a>, <a href="/search/astro-ph?searchtype=author&query=Moffett%2C+A+J">Amanda J. Moffett</a>, <a href="/search/astro-ph?searchtype=author&query=Popescu%2C+C+C">Cristina C. Popescu</a>, <a href="/search/astro-ph?searchtype=author&query=Taylor%2C+E+N">Edward N. Taylor</a>, <a href="/search/astro-ph?searchtype=author&query=Tuffs%2C+R+J">Richard J. Tuffs</a>, <a href="/search/astro-ph?searchtype=author&query=Vika%2C+M">Marina Vika</a>, <a href="/search/astro-ph?searchtype=author&query=Vulcani%2C+B">Benedetta Vulcani</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="1509.06756v3-abstract-short" style="display: inline;"> We study how the sizes and radial profiles of galaxies vary with wavelength, by fitting Sersic functions simultaneously to imaging in nine optical and near-infrared bands. To quantify the wavelength dependence of effective radius we use the ratio, $\mathcal{R}$, of measurements in two restframe bands. The dependence of Sersic index on wavelength, $\mathcal{N}$, is computed correspondingly. Vulcani… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.06756v3-abstract-full').style.display = 'inline'; document.getElementById('1509.06756v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1509.06756v3-abstract-full" style="display: none;"> We study how the sizes and radial profiles of galaxies vary with wavelength, by fitting Sersic functions simultaneously to imaging in nine optical and near-infrared bands. To quantify the wavelength dependence of effective radius we use the ratio, $\mathcal{R}$, of measurements in two restframe bands. The dependence of Sersic index on wavelength, $\mathcal{N}$, is computed correspondingly. Vulcani et al. (2014) have demonstrated that different galaxy populations present sharply contrasting behaviour in terms of $\mathcal{R}$ and $\mathcal{N}$. Here we study the luminosity dependence of this result. We find that at higher luminosities, early-type galaxies display a more substantial decrease in effective radius with wavelength, whereas late-types present a more pronounced increase in Sersic index. The structural contrast between types thus increases with luminosity. By considering samples at different redshifts, we demonstrate that lower data quality reduces the apparent difference between the main galaxy populations. However, our conclusions remain robust to this effect. We show that accounting for different redshift and luminosity selections partly reconciles the size variation measured by Vulcani et al. with the weaker trends found by other recent studies. Dividing galaxies by visual morphology confirms the behaviour inferred using morphological proxies, although the sample size is greatly reduced. Finally, we demonstrate that varying dust opacity and disc inclination can account for features of the joint distribution of $\mathcal{R}$ and $\mathcal{N}$ for late-type galaxies. However, dust does not appear to explain the highest values of $\mathcal{R}$ and $\mathcal{N}$. The bulge-disc nature of galaxies must also contribute to the wavelength-dependence of their structure. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.06756v3-abstract-full').style.display = 'none'; document.getElementById('1509.06756v3-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 September, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 September, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2015. </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, 11 figures, accepted by MNRAS; v2 corrected to match journal version</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1508.06831">arXiv:1508.06831</a> <span> [<a href="https://arxiv.org/pdf/1508.06831">pdf</a>, <a href="https://arxiv.org/format/1508.06831">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/10.1093/mnras/stv2230">10.1093/mnras/stv2230 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Wavelength Self-Calibration and Sky Subtraction for Fabry-Perot Interferometers: Applications to OSIRIS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Weinzirl%2C+T">Tim Weinzirl</a>, <a href="/search/astro-ph?searchtype=author&query=Aragon-Salamanca%2C+A">Alfonso Aragon-Salamanca</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S+P">Steven P. Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=del+Pino%2C+B+R">Bruno Rodriguez del Pino</a>, <a href="/search/astro-ph?searchtype=author&query=Gray%2C+M+E">Meghan E. Gray</a>, <a href="/search/astro-ph?searchtype=author&query=Chies-Santos%2C+A+L">Ana L. Chies-Santos</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="1508.06831v1-abstract-short" style="display: inline;"> We describe techniques concerning wavelength calibration and sky subtraction to maximise the scientific utility of data from tunable filter instruments. While we specifically address data from the Optical System for Imaging and low Resolution Integrated Spectroscopy instrument (OSIRIS) on the 10.4~m Gran Telescopio Canarias telescope, our discussion is generalisable to data from other tunable filt… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1508.06831v1-abstract-full').style.display = 'inline'; document.getElementById('1508.06831v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1508.06831v1-abstract-full" style="display: none;"> We describe techniques concerning wavelength calibration and sky subtraction to maximise the scientific utility of data from tunable filter instruments. While we specifically address data from the Optical System for Imaging and low Resolution Integrated Spectroscopy instrument (OSIRIS) on the 10.4~m Gran Telescopio Canarias telescope, our discussion is generalisable to data from other tunable filter instruments. A key aspect of our methodology is a coordinate transformation to polar coordinates, which simplifies matters when the tunable filter data is circularly symmetric around the optical centre. First, we present a method for rectifying inaccuracies in the wavelength calibration using OH sky emission rings. Using this technique, we improve the absolute wavelength calibration from an accuracy of 5 Angstroms to 1 Angstrom, equivalent to ~7% of our instrumental resolution, for 95% of our data. Then, we discuss a new way to estimate the background sky emission by median filtering in polar coordinates. This method suppresses contributions to the sky background from the outer envelopes of distant galaxies, maximising the fluxes of sources measured in the corresponding sky-subtracted images. We demonstrate for data tuned to a central wavelength of 7615~$\rm脜$ that galaxy fluxes in the new sky-subtracted image are ~37% higher, versus a sky-subtracted image from existing methods for OSIRIS tunable filter data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1508.06831v1-abstract-full').style.display = 'none'; document.getElementById('1508.06831v1-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 August, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2015. </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 accepted; 7 pages, 6 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1508.02076">arXiv:1508.02076</a> <span> [<a href="https://arxiv.org/pdf/1508.02076">pdf</a>, <a href="https://arxiv.org/format/1508.02076">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/stv2505">10.1093/mnras/stv2505 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galaxy And Mass Assembly (GAMA): Panchromatic Data Release (far-UV --- far-IR) and the low-z energy budget </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Driver%2C+S+P">Simon P. Driver</a>, <a href="/search/astro-ph?searchtype=author&query=Wright%2C+A+H">Angus H. Wright</a>, <a href="/search/astro-ph?searchtype=author&query=Andrews%2C+S+K">Stephen K. Andrews</a>, <a href="/search/astro-ph?searchtype=author&query=Davies%2C+L+J">Luke J. Davies</a>, <a href="/search/astro-ph?searchtype=author&query=Kafle%2C+P+R">Prajwal R. Kafle</a>, <a href="/search/astro-ph?searchtype=author&query=Lange%2C+R">Rebecca Lange</a>, <a href="/search/astro-ph?searchtype=author&query=Moffett%2C+A+J">Amanda J. Moffett</a>, <a href="/search/astro-ph?searchtype=author&query=Mannering%2C+E">Elizabeth Mannering</a>, <a href="/search/astro-ph?searchtype=author&query=Robotham%2C+A+S+G">Aaron S. G. Robotham</a>, <a href="/search/astro-ph?searchtype=author&query=Vinsen%2C+K">Kevin Vinsen</a>, <a href="/search/astro-ph?searchtype=author&query=Alpaslan%2C+M">Mehmet Alpaslan</a>, <a href="/search/astro-ph?searchtype=author&query=Andrae%2C+E">Ellen Andrae</a>, <a href="/search/astro-ph?searchtype=author&query=Baldry%2C+I+K">Ivan K. Baldry</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+A+E">Amanda E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S+P">Steven P. Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Bland-Hawthorn%2C+J">Joss Bland-Hawthorn</a>, <a href="/search/astro-ph?searchtype=author&query=Bourne%2C+N">Nathan Bourne</a>, <a href="/search/astro-ph?searchtype=author&query=Brough%2C+S">Sarah Brough</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+M+J+I">Michael J. I. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Cluver%2C+M+E">Michelle E. Cluver</a>, <a href="/search/astro-ph?searchtype=author&query=Croom%2C+S">Scott Croom</a>, <a href="/search/astro-ph?searchtype=author&query=Colless%2C+M">Matthew Colless</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C+J">Christopher J. Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=da+Cunha%2C+E">Elisabete da Cunha</a>, <a href="/search/astro-ph?searchtype=author&query=De+Propris%2C+R">Roberto De Propris</a> , et al. (38 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="1508.02076v2-abstract-short" style="display: inline;"> We present the GAMA Panchromatic Data Release (PDR) constituting over 230deg$^2$ of imaging with photometry in 21 bands extending from the far-UV to the far-IR. These data complement our spectroscopic campaign of over 300k galaxies, and are compiled from observations with a variety of facilities including: GALEX, SDSS, VISTA, WISE, and Herschel, with the GAMA regions currently being surveyed by VS… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1508.02076v2-abstract-full').style.display = 'inline'; document.getElementById('1508.02076v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1508.02076v2-abstract-full" style="display: none;"> We present the GAMA Panchromatic Data Release (PDR) constituting over 230deg$^2$ of imaging with photometry in 21 bands extending from the far-UV to the far-IR. These data complement our spectroscopic campaign of over 300k galaxies, and are compiled from observations with a variety of facilities including: GALEX, SDSS, VISTA, WISE, and Herschel, with the GAMA regions currently being surveyed by VST and scheduled for observations by ASKAP. These data are processed to a common astrometric solution, from which photometry is derived for 221,373 galaxies with r<19.8 mag. Online tools are provided to access and download data cutouts, or the full mosaics of the GAMA regions in each band. We focus, in particular, on the reduction and analysis of the VISTA VIKING data, and compare to earlier datasets (i.e., 2MASS and UKIDSS) before combining the data and examining its integrity. Having derived the 21-band photometric catalogue we proceed to fit the data using the energy balance code MAGPHYS. These measurements are then used to obtain the first fully empirical measurement of the 0.1-500$渭$m energy output of the Universe. Exploring the Cosmic Spectral Energy Distribution (CSED) across three time-intervals (0.3-1.1Gyr, 1.1-1.8~Gyr and 1.8---2.4~Gyr), we find that the Universe is currently generating $(1.5 \pm 0.3) \times 10^{35}$ h$_{70}$ W Mpc$^{-3}$, down from $(2.5 \pm 0.2) \times 10^{35}$ h$_{70}$ W Mpc$^{-3}$ 2.3~Gyr ago. More importantly, we identify significant and smooth evolution in the integrated photon escape fraction at all wavelengths, with the UV escape fraction increasing from 27(18)% at z=0.18 in NUV(FUV) to 34(23)% at z=0.06. The GAMA PDR will allow for detailed studies of the energy production and outputs of individual systems, sub-populations, and representative galaxy samples at $z<0.5$. The GAMA PDR can be found at: http://gama-psi.icrar.org/ <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1508.02076v2-abstract-full').style.display = 'none'; document.getElementById('1508.02076v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 November, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 August, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2015. </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 and 30 figures. Accepted in MNRAS. High-resolution copy available from our release site: http://gama-psi.icrar.org/ or directly via http://www.simondriver.org/mwavev05.pdf</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1507.07272">arXiv:1507.07272</a> <span> [<a href="https://arxiv.org/pdf/1507.07272">pdf</a>, <a href="https://arxiv.org/format/1507.07272">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/stv1688">10.1093/mnras/stv1688 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Radio Galaxy Zoo: host galaxies and radio morphologies derived from visual inspection </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Banfield%2C+J+K">J. K. Banfield</a>, <a href="/search/astro-ph?searchtype=author&query=Wong%2C+O+I">O. I. Wong</a>, <a href="/search/astro-ph?searchtype=author&query=Willett%2C+K+W">K. W. Willett</a>, <a href="/search/astro-ph?searchtype=author&query=Norris%2C+R+P">R. P. Norris</a>, <a href="/search/astro-ph?searchtype=author&query=Rudnick%2C+L">L. Rudnick</a>, <a href="/search/astro-ph?searchtype=author&query=Shabala%2C+S+S">S. S. Shabala</a>, <a href="/search/astro-ph?searchtype=author&query=Simmons%2C+B+D">B. D. Simmons</a>, <a href="/search/astro-ph?searchtype=author&query=Snyder%2C+C">C. Snyder</a>, <a href="/search/astro-ph?searchtype=author&query=Garon%2C+A">A. Garon</a>, <a href="/search/astro-ph?searchtype=author&query=Seymour%2C+N">N. Seymour</a>, <a href="/search/astro-ph?searchtype=author&query=Middelberg%2C+E">E. Middelberg</a>, <a href="/search/astro-ph?searchtype=author&query=Andernach%2C+H">H. Andernach</a>, <a href="/search/astro-ph?searchtype=author&query=Lintott%2C+C+J">C. J. Lintott</a>, <a href="/search/astro-ph?searchtype=author&query=Jacob%2C+K">K. Jacob</a>, <a href="/search/astro-ph?searchtype=author&query=Kapinska%2C+A+D">A. D. Kapinska</a>, <a href="/search/astro-ph?searchtype=author&query=Mao%2C+M+Y">M. Y. Mao</a>, <a href="/search/astro-ph?searchtype=author&query=Masters%2C+K+L">K. L. Masters</a>, <a href="/search/astro-ph?searchtype=author&query=Jarvis%2C+M+J">M. J. Jarvis</a>, <a href="/search/astro-ph?searchtype=author&query=Schawinski%2C+K">K. Schawinski</a>, <a href="/search/astro-ph?searchtype=author&query=Paget%2C+E">E. Paget</a>, <a href="/search/astro-ph?searchtype=author&query=Simpson%2C+R">R. Simpson</a>, <a href="/search/astro-ph?searchtype=author&query=Klockner%2C+H+R">H. R. Klockner</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S">S. Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Burchell%2C+T">T. Burchell</a>, <a href="/search/astro-ph?searchtype=author&query=Chow%2C+K+E">K. E. Chow</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="1507.07272v1-abstract-short" style="display: inline;"> We present results from the first twelve months of operation of Radio Galaxy Zoo, which upon completion will enable visual inspection of over 170,000 radio sources to determine the host galaxy of the radio emission and the radio morphology. Radio Galaxy Zoo uses $1.4\,$GHz radio images from both the Faint Images of the Radio Sky at Twenty Centimeters (FIRST) and the Australia Telescope Large Area… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1507.07272v1-abstract-full').style.display = 'inline'; document.getElementById('1507.07272v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1507.07272v1-abstract-full" style="display: none;"> We present results from the first twelve months of operation of Radio Galaxy Zoo, which upon completion will enable visual inspection of over 170,000 radio sources to determine the host galaxy of the radio emission and the radio morphology. Radio Galaxy Zoo uses $1.4\,$GHz radio images from both the Faint Images of the Radio Sky at Twenty Centimeters (FIRST) and the Australia Telescope Large Area Survey (ATLAS) in combination with mid-infrared images at $3.4\,渭$m from the {\it Wide-field Infrared Survey Explorer} (WISE) and at $3.6\,渭$m from the {\it Spitzer Space Telescope}. We present the early analysis of the WISE mid-infrared colours of the host galaxies. For images in which there is $>\,75\%$ consensus among the Radio Galaxy Zoo cross-identifications, the project participants are as effective as the science experts at identifying the host galaxies. The majority of the identified host galaxies reside in the mid-infrared colour space dominated by elliptical galaxies, quasi-stellar objects (QSOs), and luminous infrared radio galaxies (LIRGs). We also find a distinct population of Radio Galaxy Zoo host galaxies residing in a redder mid-infrared colour space consisting of star-forming galaxies and/or dust-enhanced non star-forming galaxies consistent with a scenario of merger-driven active galactic nuclei (AGN) formation. The completion of the full Radio Galaxy Zoo project will measure the relative populations of these hosts as a function of radio morphology and power while providing an avenue for the identification of rare and extreme radio structures. Currently, we are investigating candidates for radio galaxies with extreme morphologies, such as giant radio galaxies, late-type host galaxies with extended radio emission, and hybrid morphology radio sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1507.07272v1-abstract-full').style.display = 'none'; document.getElementById('1507.07272v1-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 July, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2015. </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, 17 pages, 13 figures, 1 table. Higher resolution figures available with MNRAS publication or contact author</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1506.08222">arXiv:1506.08222</a> <span> [<a href="https://arxiv.org/pdf/1506.08222">pdf</a>, <a href="https://arxiv.org/format/1506.08222">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/stv1436">10.1093/mnras/stv1436 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galaxy And Mass Assembly (GAMA): end of survey report and data release 2 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Liske%2C+J">J. Liske</a>, <a href="/search/astro-ph?searchtype=author&query=Baldry%2C+I+K">I. K. Baldry</a>, <a href="/search/astro-ph?searchtype=author&query=Driver%2C+S+P">S. P. Driver</a>, <a href="/search/astro-ph?searchtype=author&query=Tuffs%2C+R+J">R. J. Tuffs</a>, <a href="/search/astro-ph?searchtype=author&query=Alpaslan%2C+M">M. Alpaslan</a>, <a href="/search/astro-ph?searchtype=author&query=Andrae%2C+E">E. Andrae</a>, <a href="/search/astro-ph?searchtype=author&query=Brough%2C+S">S. Brough</a>, <a href="/search/astro-ph?searchtype=author&query=Cluver%2C+M+E">M. E. Cluver</a>, <a href="/search/astro-ph?searchtype=author&query=Grootes%2C+M+W">M. W. Grootes</a>, <a href="/search/astro-ph?searchtype=author&query=Gunawardhana%2C+M+L+P">M. L. P. Gunawardhana</a>, <a href="/search/astro-ph?searchtype=author&query=Kelvin%2C+L+S">L. S. Kelvin</a>, <a href="/search/astro-ph?searchtype=author&query=Loveday%2C+J">J. Loveday</a>, <a href="/search/astro-ph?searchtype=author&query=Robotham%2C+A+S+G">A. S. G. Robotham</a>, <a href="/search/astro-ph?searchtype=author&query=Taylor%2C+E+N">E. N. Taylor</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S+P">S. P. Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Bland-Hawthorn%2C+J">J. Bland-Hawthorn</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+M+J+I">M. J. I. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Drinkwater%2C+M+J">M. J. Drinkwater</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A+M">A. M. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Meyer%2C+M+J">M. J. Meyer</a>, <a href="/search/astro-ph?searchtype=author&query=Norberg%2C+P">P. Norberg</a>, <a href="/search/astro-ph?searchtype=author&query=Peacock%2C+J+A">J. A. Peacock</a>, <a href="/search/astro-ph?searchtype=author&query=Agius%2C+N+K">N. K. Agius</a>, <a href="/search/astro-ph?searchtype=author&query=Andrews%2C+S+K">S. K. Andrews</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+A+E">A. E. Bauer</a> , et al. (45 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="1506.08222v1-abstract-short" style="display: inline;"> The Galaxy And Mass Assembly (GAMA) survey is one of the largest contemporary spectroscopic surveys of low-redshift galaxies. Covering an area of ~286 deg^2 (split among five survey regions) down to a limiting magnitude of r < 19.8 mag, we have collected spectra and reliable redshifts for 238,000 objects using the AAOmega spectrograph on the Anglo-Australian Telescope. In addition, we have assembl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1506.08222v1-abstract-full').style.display = 'inline'; document.getElementById('1506.08222v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1506.08222v1-abstract-full" style="display: none;"> The Galaxy And Mass Assembly (GAMA) survey is one of the largest contemporary spectroscopic surveys of low-redshift galaxies. Covering an area of ~286 deg^2 (split among five survey regions) down to a limiting magnitude of r < 19.8 mag, we have collected spectra and reliable redshifts for 238,000 objects using the AAOmega spectrograph on the Anglo-Australian Telescope. In addition, we have assembled imaging data from a number of independent surveys in order to generate photometry spanning the wavelength range 1 nm - 1 m. Here we report on the recently completed spectroscopic survey and present a series of diagnostics to assess its final state and the quality of the redshift data. We also describe a number of survey aspects and procedures, or updates thereof, including changes to the input catalogue, redshifting and re-redshifting, and the derivation of ultraviolet, optical and near-infrared photometry. Finally, we present the second public release of GAMA data. In this release we provide input catalogue and targeting information, spectra, redshifts, ultraviolet, optical and near-infrared photometry, single-component S茅rsic fits, stellar masses, H$伪$-derived star formation rates, environment information, and group properties for all galaxies with r < 19.0 mag in two of our survey regions, and for all galaxies with r < 19.4 mag in a third region (72,225 objects in total). The database serving these data is available at http://www.gama-survey.org/. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1506.08222v1-abstract-full').style.display = 'none'; document.getElementById('1506.08222v1-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 June, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2015. </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 MMRAS, 40 pages, 33 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/1505.05518">arXiv:1505.05518</a> <span> [<a href="https://arxiv.org/pdf/1505.05518">pdf</a>, <a href="https://arxiv.org/format/1505.05518">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"> Galaxy And Mass Assembly (GAMA): Trends in galaxy colours, morphology, and stellar populations with large scale structure, group, and pair environments </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Alpaslan%2C+M">Mehmet Alpaslan</a>, <a href="/search/astro-ph?searchtype=author&query=Driver%2C+S">Simon Driver</a>, <a href="/search/astro-ph?searchtype=author&query=Robotham%2C+A+S+G">Aaron S. G. Robotham</a>, <a href="/search/astro-ph?searchtype=author&query=Obreschkow%2C+D">Danail Obreschkow</a>, <a href="/search/astro-ph?searchtype=author&query=Andrae%2C+E">Ellen Andrae</a>, <a href="/search/astro-ph?searchtype=author&query=Cluver%2C+M">Michelle Cluver</a>, <a href="/search/astro-ph?searchtype=author&query=Kelvin%2C+L+S">Lee S. Kelvin</a>, <a href="/search/astro-ph?searchtype=author&query=Lange%2C+R">Rebecca Lange</a>, <a href="/search/astro-ph?searchtype=author&query=Owers%2C+M">Matt Owers</a>, <a href="/search/astro-ph?searchtype=author&query=Taylor%2C+E+N">Edward N. Taylor</a>, <a href="/search/astro-ph?searchtype=author&query=Andrews%2C+S+K">Stephen K. Andrews</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S">Steven Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Bland-Hawthorn%2C+J">Joss Bland-Hawthorn</a>, <a href="/search/astro-ph?searchtype=author&query=Brough%2C+S">Sarah Brough</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+M+J+I">Michael J. I. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Colless%2C+M">Matthew Colless</a>, <a href="/search/astro-ph?searchtype=author&query=Davies%2C+L+J+M">Luke J. M. Davies</a>, <a href="/search/astro-ph?searchtype=author&query=Eardley%2C+E">Elizabeth Eardley</a>, <a href="/search/astro-ph?searchtype=author&query=Grootes%2C+M+W">Meiert W. Grootes</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A+M">Andrew M. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Kennedy%2C+R">Rebecca Kennedy</a>, <a href="/search/astro-ph?searchtype=author&query=Liske%2C+J">Jochen Liske</a>, <a href="/search/astro-ph?searchtype=author&query=Lara-Lopez%2C+M+A">Maritza A. Lara-Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez-Sanchez%2C+A+R">Angel R. Lopez-Sanchez</a>, <a href="/search/astro-ph?searchtype=author&query=Loveday%2C+J">Jon Loveday</a> , et al. (10 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1505.05518v1-abstract-short" style="display: inline;"> We explore trends in galaxy properties with Mpc-scale structures using catalogues of environment and large scale structure from the Galaxy And Mass Assembly (GAMA) survey. Existing GAMA catalogues of large scale structure, group and pair membership allow us to construct galaxy stellar mass functions for different environmental types. To avoid simply extracting the known underlying correlations bet… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1505.05518v1-abstract-full').style.display = 'inline'; document.getElementById('1505.05518v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1505.05518v1-abstract-full" style="display: none;"> We explore trends in galaxy properties with Mpc-scale structures using catalogues of environment and large scale structure from the Galaxy And Mass Assembly (GAMA) survey. Existing GAMA catalogues of large scale structure, group and pair membership allow us to construct galaxy stellar mass functions for different environmental types. To avoid simply extracting the known underlying correlations between galaxy properties and stellar mass, we create a mass matched sample of galaxies with stellar masses between $9.5 \leq \log{M_*/h^{-2} M_{\odot}} \leq 11$ for each environmental population. Using these samples, we show that mass normalised galaxies in different large scale environments have similar energy outputs, $u-r$ colours, luminosities, and morphologies. Extending our analysis to group and pair environments, we show galaxies that are not in groups or pairs exhibit similar characteristics to each other regardless of broader environment. For our mass controlled sample, we fail to see a strong dependence of S茅rsic index or galaxy luminosity on halo mass, but do find that it correlates very strongly with colour. Repeating our analysis for galaxies that have not been mass controlled introduces and amplifies trends in the properties of galaxies in pairs, groups, and large scale structure, indicating that stellar mass is the most important predictor of the galaxy properties we examine, as opposed to environmental classifications. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1505.05518v1-abstract-full').style.display = 'none'; document.getElementById('1505.05518v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 May, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2015. </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, 18 figures, accepted for publication in MNRAS on May 20, 2015</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1504.02053">arXiv:1504.02053</a> <span> [<a href="https://arxiv.org/pdf/1504.02053">pdf</a>, <a href="https://arxiv.org/format/1504.02053">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/stv779">10.1093/mnras/stv779 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> OMEGA -- OSIRIS Mapping of Emission-line Galaxies in A901/2: I.-- Survey description, data analysis, and star formation and AGN activity in the highest density regions </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=del+Pino%2C+B+R">Bruno Rodr铆guez del Pino</a>, <a href="/search/astro-ph?searchtype=author&query=Arag%C3%B3n-Salamanca%2C+A">Alfonso Arag贸n-Salamanca</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S+P">Steven P. Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Gray%2C+M+E">Meghan E. Gray</a>, <a href="/search/astro-ph?searchtype=author&query=Wolf%2C+C">Christian Wolf</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6hm%2C+A">Asmus B枚hm</a>, <a href="/search/astro-ph?searchtype=author&query=Maltby%2C+D+T">David T. Maltby</a>, <a href="/search/astro-ph?searchtype=author&query=Pintos-Castro%2C+I">Irene Pintos-Castro</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Portal%2C+M">Miguel S谩nchez-Portal</a>, <a href="/search/astro-ph?searchtype=author&query=Weinzirl%2C+T">Tim Weinzirl</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="1504.02053v1-abstract-short" style="display: inline;"> We present an overview of and first results from the OMEGA survey: the OSIRIS Mapping of Emission-line Galaxies in the multi-cluster system A901/2. The ultimate goal of this project is to study star formation and AGN activity across a broad range of environments at a single redshift. Using the tuneable-filter mode of the OSIRIS instrument on GTC, we target Halpha and [NII] emission lines over a ~0… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1504.02053v1-abstract-full').style.display = 'inline'; document.getElementById('1504.02053v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1504.02053v1-abstract-full" style="display: none;"> We present an overview of and first results from the OMEGA survey: the OSIRIS Mapping of Emission-line Galaxies in the multi-cluster system A901/2. The ultimate goal of this project is to study star formation and AGN activity across a broad range of environments at a single redshift. Using the tuneable-filter mode of the OSIRIS instrument on GTC, we target Halpha and [NII] emission lines over a ~0.5 X 0.5 deg2 region containing the z~0.167 multi-cluster system A901/2. In this paper we describe the design of the survey, the observations and the data analysis techniques developed. We then present early results from two OSIRIS pointings centred on the cores of the A901a and A902 clusters. AGN and star-forming (SF) objects are identified using the [NII]/Halpha vs. W_Halpha (WHAN) diagnostic diagram. The AGN hosts are brighter, more massive, and possess earlier-type morphologies than SF galaxies. Both populations tend to be located towards the outskirts of the high density regions we study. The typical Halpha luminosity of these sources is significantly lower than that of field galaxies at similar redshifts, but greater than that found for A1689, a rich cluster at z~0.2. The Halpha luminosities of our objects translate into star-formation rates (SFRs) between ~0.02 and 6 Msun/yr. Comparing the relationship between stellar mass and Halpha-derived SFR with that found in the field indicates a suppression of star formation in the cores of the clusters. These findings agree with previous investigations of this multi-cluster structure, based on other star formation indicators, and demonstrate the power of tuneable filters for this kind of study. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1504.02053v1-abstract-full').style.display = 'none'; document.getElementById('1504.02053v1-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 April, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2015. </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 accepted, 19 pages, 20 figures,1 table</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1502.07347">arXiv:1502.07347</a> <span> [<a href="https://arxiv.org/pdf/1502.07347">pdf</a>, <a href="https://arxiv.org/format/1502.07347">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/stv421">10.1093/mnras/stv421 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Galaxy Cluster Mass Reconstruction Project: II. Quantifying scatter and bias using contrasting mock catalogues </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Old%2C+L">L. Old</a>, <a href="/search/astro-ph?searchtype=author&query=Wojtak%2C+R">R. Wojtak</a>, <a href="/search/astro-ph?searchtype=author&query=Mamon%2C+G+A">G. A. Mamon</a>, <a href="/search/astro-ph?searchtype=author&query=Skibba%2C+R+A">R. A. Skibba</a>, <a href="/search/astro-ph?searchtype=author&query=Pearce%2C+F+R">F. R. Pearce</a>, <a href="/search/astro-ph?searchtype=author&query=Croton%2C+D">D. Croton</a>, <a href="/search/astro-ph?searchtype=author&query=Bamford%2C+S">S. Bamford</a>, <a href="/search/astro-ph?searchtype=author&query=Behroozi%2C+P">P. Behroozi</a>, <a href="/search/astro-ph?searchtype=author&query=de+Carvalho%2C+R">R. de Carvalho</a>, <a href="/search/astro-ph?searchtype=author&query=Mu%C3%B1oz-Cuartas%2C+J+C">J. C. Mu帽oz-Cuartas</a>, <a href="/search/astro-ph?searchtype=author&query=Gifford%2C+D">D. Gifford</a>, <a href="/search/astro-ph?searchtype=author&query=Gray%2C+M+E">M. E. Gray</a>, <a href="/search/astro-ph?searchtype=author&query=von+der+Linden%2C+A">A. von der Linden</a>, <a href="/search/astro-ph?searchtype=author&query=Merrifield%2C+M+R">M. R. Merrifield</a>, <a href="/search/astro-ph?searchtype=author&query=Muldrew%2C+S+I">S. I. Muldrew</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%BCller%2C+V">V. M眉ller</a>, <a href="/search/astro-ph?searchtype=author&query=Pearson%2C+R+J">R. J. Pearson</a>, <a href="/search/astro-ph?searchtype=author&query=Ponman%2C+T+J">T. J. Ponman</a>, <a href="/search/astro-ph?searchtype=author&query=Rozo%2C+E">E. Rozo</a>, <a href="/search/astro-ph?searchtype=author&query=Rykoff%2C+E">E. Rykoff</a>, <a href="/search/astro-ph?searchtype=author&query=Saro%2C+A">A. Saro</a>, <a href="/search/astro-ph?searchtype=author&query=Sepp%2C+T">T. Sepp</a>, <a href="/search/astro-ph?searchtype=author&query=Sif%C3%B3n%2C+C">C. Sif贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Tempel%2C+E">E. Tempel</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="1502.07347v1-abstract-short" style="display: inline;"> This article is the second in a series in which we perform an extensive comparison of various galaxy-based cluster mass estimation techniques that utilise the positions, velocities and colours of galaxies. Our aim is to quantify the scatter, systematic bias and completeness of cluster masses derived from a diverse set of 25 galaxy-based methods using two contrasting mock galaxy catalogues based on… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1502.07347v1-abstract-full').style.display = 'inline'; document.getElementById('1502.07347v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1502.07347v1-abstract-full" style="display: none;"> This article is the second in a series in which we perform an extensive comparison of various galaxy-based cluster mass estimation techniques that utilise the positions, velocities and colours of galaxies. Our aim is to quantify the scatter, systematic bias and completeness of cluster masses derived from a diverse set of 25 galaxy-based methods using two contrasting mock galaxy catalogues based on a sophisticated halo occupation model and a semi-analytic model. Analysing 968 clusters, we find a wide range in the RMS errors in log M200c delivered by the different methods (0.18 to 1.08 dex, i.e., a factor of ~1.5 to 12), with abundance matching and richness methods providing the best results, irrespective of the input model assumptions. In addition, certain methods produce a significant number of catastrophic cases where the mass is under- or over-estimated by a factor greater than 10. Given the steeply falling high-mass end of the cluster mass function, we recommend that richness or abundance matching-based methods are used in conjunction with these methods as a sanity check for studies selecting high mass clusters. We see a stronger correlation of the recovered to input number of galaxies for both catalogues in comparison with the group/cluster mass, however, this does not guarantee that the correct member galaxies are being selected. We do not observe significantly higher scatter for either mock galaxy catalogues. Our results have implications for cosmological analyses that utilise the masses, richnesses, or abundances of clusters, which have different uncertainties when different methods are used. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1502.07347v1-abstract-full').style.display = 'none'; document.getElementById('1502.07347v1-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 February, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2015. </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, 19 figures, 7 tables. Accepted for publication in MNRAS</span> </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Bamford%2C+S&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Bamford%2C+S&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Bamford%2C+S&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Bamford%2C+S&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=Bamford%2C+S&start=150" class="pagination-link " aria-label="Page 4" aria-current="page">4 </a> </li> </ul> </nav> <div class="is-hidden-tablet">  <span 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