$. We have found that in the innermost gas there is a high velocity structure, most likely indicating the presence of an outflow from the AGN while our analysis of the cluster cool core using RGS data indicates that the velocity of the gas agrees with the M87 optical redshift. An overall gradient in the velocity is seen, with larger values as we move away from the cluster core. The hot gas located within the western radio flow is redshifted, moving with a velocity $\\sim 331$ km\u002Fs while the hot gas located within the eastern radio flow is blueshifted, with a velocity $\\sim 258$ km\u002Fs, suggesting the presence of backflows. Our results reveal the effects of both AGN outflows and gas sloshing, in the complex velocity field of the Virgo cluster. ","authors":[{"name":"Efrain Gatuzz"},{"id":"53f433a2dabfaeecd6943a88","name":"J. S. Sanders"},{"name":"K. Dennerl"},{"id":"53f9c6efdabfae7f97afb7a3","name":"C. Pinto"},{"id":"54068c09dabfae92b421034c","name":"A. C. Fabian"},{"id":"53f4745adabfaee43ed2d4c5","name":"T. Tamura"},{"id":"53f3a8f8dabfae4b34aeb000","name":"S. A. Walker"},{"name":"J. ZuHone"}],"id":"614164545244ab9dcb9dd803","lang":"en","num_citation":0,"order":1,"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F\u002F21\u002F2109\u002F2109.06213.pdf","title":"Measuring sloshing, merging and feedback velocities in the Virgo cluster","urls":["https:\u002F\u002Farxiv.org\u002Fabs\u002F2109.06213"],"versions":[{"id":"614164545244ab9dcb9dd803","sid":"2109.06213","src":"arxiv","year":2021}],"year":2021},{"abstract":"We demonstrate a novel technique for calibrating the energy scale of the EPIC-pn detector on XMM-Newton, which allows us to measure bulk flows in the intracluster medium (ICM) of the Perseus and Coma galaxy clusters. The procedure uses the fluorescent instrumental background lines present in all observations, in particular, Cu-K alpha. By studying their spatial and temporal variations, in addition to incorporating calibration observations, we refined the absolute energy scale of the detector to better than 150 km s(-1) at the Fe-K line, a large improvement over the nominal calibration accuracy of 550 km s(-1). With our calibration, we mapped the bulk motions over much of the central 1200 and 800 kpc of Perseus and Coma, respectively, in spatial regions down to 65 and 140 kpc size. We cross-checked our procedure by comparing our measurements with those found in Perseus by Hitomi for an overlapping 65 kpc square region, finding consistent results. For Perseus, there is a relative line-of-sight velocity increase of 480 +\u002F- 210 km s(-1) (1 sigma) at a radius of 250 kpc east of the nucleus. This region is associated with a cold front, providing direct evidence of the ICM sloshing in the cluster potential well. Assuming the intrinsic distribution of bulk motions is Gaussian, its width is 214 +\u002F- 85 km s(-1), excluding systematic uncertainties. Removing the sloshing region, this is reduced to 20-150 km s(-1), which is similar in magnitude to the Hitomi line width measurements in undisturbed regions. In Coma, the line-of-sight velocity of the ICM varies between the velocities of the two central galaxies. Maps of the gas velocity and metallicity provide clues about the merger history of the Coma, with material to the north and east of the cluster core having a velocity similar to NGC 4874, while that to the south and west has velocities close to NGC 4889. Our results highlight the difference between a merging system, such as Coma, where we observe a similar to 1000 km s(-1) range in velocity, and a relatively relaxed system, such as Perseus, with much weaker bulk motions.","authors":[{"id":"53f433a2dabfaeecd6943a88","name":"J. S. Sanders"},{"name":"K. Dennerl"},{"id":"53f4352cdabfaedce552496a","name":"H. R. Russell"},{"id":"54054854dabfae91d3fcf9a6","name":"D. Eckert"},{"id":"53f9c6efdabfae7f97afb7a3","name":"C. Pinto"},{"id":"5434d30edabfaebba586c99b","name":"A. C. Fabian"},{"id":"53f3a8f8dabfae4b34aeb000","name":"S. A. Walker"},{"id":"53f4745adabfaee43ed2d4c5","name":"T. Tamura"},{"name":"J. ZuHone"},{"name":"F. Hofmann"}],"doi":"10.1051\u002F0004-6361\u002F201936468","id":"5e5e185293d709897cdf50cc","num_citation":0,"order":0,"pages":{"end":"","start":""},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F19\u002F1911\u002F1911.13108.pdf","title":"Measuring bulk flows of the intracluster medium in the Perseus and Coma galaxy clusters using XMM-Newton","urls":["https:\u002F\u002Fwww.aanda.org\u002F10.1051\u002F0004-6361\u002F201936468\u002Fpdf","https:\u002F\u002Farxiv.org\u002Fabs\u002F1911.13108","http:\u002F\u002Fwww.webofknowledge.com\u002F"],"venue":{"info":{"name":"ASTRONOMY & ASTROPHYSICS"},"issue":"","volume":"633"},"versions":[{"id":"5e5e185293d709897cdf50cc","sid":"2993135736","src":"mag","vsid":"205231332","year":2020},{"id":"5de4e0bf3a55ac2224ba55db","sid":"1911.13108","src":"arxiv","year":2019},{"id":"5fc6f65cd75e2ac63d577715","sid":"WOS:000506608400001","src":"wos","vsid":"ASTRONOMY & ASTROPHYSICS","year":2020}],"year":2020},{"abstract":" The pre-merging system of galaxy clusters Abell 3391-Abell 3395 located at a mean redshift of 0.053 has been observed at 1 GHz in an ASKAP\u002FEMU Early Science observation as well as in X-rays with eROSITA. The projected separation of the X-ray peaks of the two clusters is $\\sim$50 $ or $\\sim$ 3.1 Mpc. Here we present an inventory of interesting radio sources in this field around this cluster merger. While the eROSITA observations provide clear indications of a bridge of thermal gas between the clusters, neither ASKAP nor MWA observations show any diffuse radio emission coinciding with the X-ray bridge. We derive an upper limit on the radio emissivity in the bridge region of $\\langle J \\rangle_{1\\,{\\rm GHz}}\u003C 1.2 \\times 10^{-44} {\\rm W}\\, {\\rm Hz}^{-1} {\\rm m}^{-3}$. A non-detection of diffuse radio emission in the X-ray bridge between these two clusters has implications for particle-acceleration mechanisms in cosmological large-scale structure. We also report extended or otherwise noteworthy radio sources in the 30 deg$^2$ field around Abell 3391-Abell 3395. We identified 20 Giant Radio Galaxies, plus 7 candidates, with linear projected sizes greater than 1 Mpc. The sky density of field radio galaxies with largest linear sizes of $\u003E0.7$ Mpc is $\\approx 1.7$ deg$^{-2}$, three times higher than previously reported. We find no evidence for a cosmological evolution of the population of Giant Radio Galaxies. Moreover, we find seven candidates for cluster radio relics and radio halos. ","authors":[{"id":"53f45788dabfaedd74e3276e","name":"M. Brüggen"},{"id":"53f4330adabfaeb22f44f0e1","name":"T. H. Reiprich"},{"id":"53f42e5ddabfaec09f121565","name":"E. Bulbul"},{"name":"B. S. Koribalski"},{"id":"548a26c9dabfae9b40134efc","name":"H. Andernach"},{"id":"560c020f45cedb339745a178","name":"L. Rudnick"},{"name":"D. N. Hoang"},{"name":"A. G. Wilber"},{"name":"S. W. Duchesne"},{"name":"A. Veronica"},{"id":"53f4476cdabfaee43ec81ce2","name":"F. Pacaud"},{"id":"53f433fedabfaeb1a7bdcd39","name":"A. M. Hopkins"},{"id":"560c249045cedb33974a906d","name":"R. P. Norris"},{"id":"53f453c1dabfaee02ad4ec57","name":"M. Johnston-Hollitt"},{"id":"53f38771dabfae4b34a1b76a","name":"M. J. I. Brown"},{"id":"53f43910dabfaee4dc79c82f","name":"A. Bonafede"},{"id":"53f438c7dabfaeecd697542b","name":"G. Brunetti"},{"name":"J. D. Collier"},{"id":"53f433a2dabfaeecd6943a88","name":"J. S. Sanders"},{"name":"E. Vardoulaki"}],"doi":"10.1051\u002F0004-6361\u002F202039533","id":"5fdb2d0591e0118a02c4f557","num_citation":0,"order":18,"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F20\u002F2012\u002F2012.08775.pdf","title":"Radio observations of the merging galaxy cluster system Abell 3391-Abell 3395","urls":["https:\u002F\u002Farxiv.org\u002Fabs\u002F2012.08775","https:\u002F\u002Fwww.aanda.org\u002F10.1051\u002F0004-6361\u002F202039533\u002Fpdf"],"venue":{"info":{"name":"Astronomy and Astrophysics"}},"versions":[{"id":"5fdb2d0591e0118a02c4f557","sid":"2012.08775","src":"arxiv","year":2020},{"id":"5ff68dffd4150a363cd6da4a","sid":"3107257134","src":"mag","vsid":"205231332","year":2020}],"year":2020},{"abstract":"We used dedicated SRG\u002FeROSITA X-ray, ASKAP\u002FEMU radio, and DECam optical observations of a 15 sq.deg region around the interacting galaxy cluster system A3391\u002F95 to study the warm-hot gas in cluster outskirts and filaments, the surrounding large-scale structure and its formation process. We relate the observations to expectations from cosmological hydrodynamic simulations from the Magneticum suite. We trace the irregular morphology of warm-hot gas of the main clusters from their centers out to well beyond their characteristic radii, $r_{200}$. Between the two main cluster systems, we observe an emission bridge; thanks to eROSITA\\u0027s unique soft response and large field of view, we discover tantalizing hints for warm gas. Several matter clumps physically surrounding the system are detected. For the \\\"Northern Clump,\\\" we provide evidence that it is falling towards A3391 from the hot gas morphology and radio lobe structure of its central AGN. Many of the extended sources in the field detected by eROSITA are known clusters or new clusters in the background, including a known SZ cluster at redshift z=1. We discover an emission filament north of the virial radius, $r_{100}$, of A3391 connecting to the Northern Clump and extending south of A3395 towards another galaxy cluster. The total projected length of this continuous warm-hot emission filament is 15 Mpc, running almost 4 degrees across the entire eROSITA observation. The DECam galaxy density map shows galaxy overdensities in the same regions. The new datasets provide impressive confirmation of the theoretically expected structure formation processes on the individual system level, including the surrounding warm-hot intergalactic medium distribution compared to the Magneticum simulation. Our spatially resolved findings show that baryons indeed reside in large-scale warm-hot gas filaments with a clumpy structure.","authors":[{"id":"53f4330adabfaeb22f44f0e1","name":"T. H. Reiprich"},{"name":"A. Veronica"},{"id":"53f4476cdabfaee43ec81ce2","name":"F. Pacaud"},{"name":"M. E. Ramos-Ceja"},{"name":"N. Ota"},{"id":"53f433a2dabfaeecd6943a88","name":"J. Sanders"},{"name":"M. Kara"},{"id":"53f45d72dabfaee43ecd5922","name":"T. Erben"},{"name":"M. Klein"},{"name":"J. Erler"},{"name":"J. Kerp"},{"name":"D. N. Hoang"},{"id":"53f45788dabfaedd74e3276e","name":"M. Brüggen"},{"name":"J. Marvil"},{"id":"560c020f45cedb339745a178","name":"L. Rudnick"},{"name":"V. Biffi"},{"id":"544821eedabfae87b7ddde10","name":"K. Dolag"},{"name":"J. Aschersleben"},{"id":"53f42e1edabfaee4dc7231f5","name":"K. Basu"},{"name":"H. Brunner"}],"doi":"10.1051\u002F0004-6361\u002F202039590","id":"5fd9f8c491e0111ad2b25664","num_citation":0,"order":5,"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F20\u002F2012\u002F2012.08491.pdf","title":"The Abell 3391\u002F95 galaxy cluster system: A 15 Mpc intergalactic medium emission filament, a warm gas bridge, infalling matter clumps, and (re-) accelerated plasma discovered by combining SRG\u002FeROSITA data with ASKAP\u002FEMU and DECam data","urls":["https:\u002F\u002Farxiv.org\u002Fabs\u002F2012.08491","https:\u002F\u002Finspirehep.net\u002Fliterature\u002F1836726"],"venue":{"info":{"name":"Astronomy and Astrophysics"}},"versions":[{"id":"5fd9f8c491e0111ad2b25664","sid":"2012.08491","src":"arxiv","year":2020},{"id":"600fe48bd4150a363c1e99f2","sid":"3110797196","src":"mag","vsid":"205231332","year":2020}],"year":2020},{"abstract":" We present new XMM-Newton observations extending the mosaic of the Perseus cluster out to the virial radius to the west. Previous studies with ROSAT have reported a large excess in surface brightness to the west, possibly the result of large scale gas sloshing, but lacked the spatial resolution and depth to determine if this excess lay behind a cold front. In our new XMM observations we have found that there is a sharp edge in X-ray surface brightness near the cluster virial radius (1.7Mpc) to the west, with a width comparable to the mean free path. The temperature measurements obtained with Suzaku data across this edge show that the temperature increases sharply outside this edge. All of these properties are consistent with this edge being the largest cold front ever observed in a galaxy cluster. We also find a second edge to the west, 1.2Mpc from the core, which also appears to be a cold front. Our results indicate that magnetic fields are able to stabilize the cold fronts against turbulence all the way out to the cluster virial radius. By comparing with numerical simulations, we find that these large cold fronts require large impact parameter, low mass ratio mergers which can produce fast gas motions without destroying the cluster core. ","authors":[{"id":"53f3a8f8dabfae4b34aeb000","name":"S. A. Walker"},{"name":"M. S. Mirakhor"},{"name":"J. ZuHone"},{"id":"53f433a2dabfaeecd6943a88","name":"J. S. Sanders"},{"id":"5434d30edabfaebba586c99b","name":"A. C. Fabian"},{"name":"P. Diwanji"}],"id":"5ef5c78b91e011b29a69838b","num_citation":0,"order":3,"title":"Is there an enormous cold front at the virial radius of the Perseus cluster?","urls":["https:\u002F\u002Farxiv.org\u002Fabs\u002F2006.14043"],"versions":[{"id":"5ef5c78b91e011b29a69838b","sid":"2006.14043","src":"arxiv","year":2020}],"year":2020},{"abstract":"Clusters of galaxies are outstanding laboratories for understanding the physics of supermassive black hole (SMBH) feedback. Here we present the first Chandra, Karl G. Jansky Very Large Array, and Hubble Space Telescope analysis of MACS J1447.4+0827 (z = 0.3755), one of the strongest cool core clusters known, in which extreme feedback from its central SMBH is needed to prevent the hot intracluster gas from cooling. Using this multiwavelength approach, including 70 ks of Chandra X-ray observations, we detect the presence of collimated jetted outflows that coincide with a southern and a northern X-ray cavity. The total mechanical power associated with these outflows (P-cav 6 x 10(44)erg s(-1)) is roughly consistent with the energy required to prevent catastrophic cooling of the hot intracluster gas (L-cool = 1.71 0.01 x 10(45)erg s(-1)fort(cool) = 7.7 Gyr), implying that powerful SMBH feedback was in place several Gyr ago in MACS J1447.7+0827. In addition, we detect the presence of a radio minihalo that extends over 300 kpc in diameter (P-1.4GHz = 3.0 0.3 x 10(24)W Hz(-1)). The X-ray observations also reveal an similar to 20 kpc plumelike structure that coincides with optical dusty filaments that surround the central galaxy. Overall, this study demonstrates that the various physical phenomena occurring in the most nearby clusters of galaxies are also occurring in their more distant analogs.","authors":[{"name":"M. Prasow-Émond"},{"id":"53f47460dabfaeee22a87ad3","name":"J. Hlavacek-Larrondo"},{"name":"C. L. Rhea"},{"name":"M. Latulippe"},{"name":"M. L. Gendron-Marsolais"},{"name":"A. Richard-Laferrière"},{"id":"53f433a2dabfaeecd6943a88","name":"J. S. Sanders"},{"id":"53f4347ddabfaedce551ce3a","name":"A. C. Edge"},{"id":"53f7ed54dabfae938c6ecaa8","name":"S. W. Allen"},{"id":"53f43cafdabfaeecd6994100","name":"A. Mantz"},{"id":"53f38853dabfae4b34a20c13","name":"A. von der Linden"}],"doi":"10.3847\u002F1538-3881\u002Fab9ff3","id":"5ff68c43d4150a363cd1e240","num_citation":0,"order":6,"pages":{"start":"103"},"title":"A Multiwavelength Study of the Cool Core Cluster MACS J1447.4+0827","urls":["http:\u002F\u002Fui.adsabs.harvard.edu\u002Fabs\u002F2020AJ....160..103P\u002Fabstract","http:\u002F\u002Fwww.webofknowledge.com\u002F"],"venue":{"info":{"name":"ASTRONOMICAL JOURNAL"},"issue":"3","volume":"160"},"versions":[{"id":"5ff68c43d4150a363cd1e240","sid":"3101917720","src":"mag","vsid":"100695177","year":2020},{"id":"5fd560f3a4e4c3c83186c933","sid":"WOS:000560678300001","src":"wos","vsid":"ASTRONOMICAL JOURNAL","year":2020}],"year":2020},{"abstract":"We place constraints on the propagation velocity of bulk turbulence within the intracluster medium of three clusters and an elliptical galaxy. Using Reflection Grating Spectrometer measurements of turbulent line broadening, we show that for these clusters, the 90 per cent upper limit on turbulent velocities when accounting for instrumental broadening is too low to propagate energy radially to the cooling radius of the clusters within the required cooling time. In this way, we extend previous Hitomi-based analysis on the Perseus cluster to more clusters, with the intention of applying these results to a future, more extensive catalogue. These results constrain models of turbulent heating in active galactic nucleus feedback by requiring a mechanism which can not only provide sufficient energy to offset radiative cooling but also resupply that energy rapidly enough to balance cooling at each cluster radius.","authors":[{"name":"Christopher J. Bambic"},{"name":"Andrew C. Fabian"},{"name":"Ciro Pinto"},{"id":"53f433a2dabfaeecd6943a88","name":"J. S. Sanders"},{"id":"54853b27dabfaed7b5fa1fad","name":"Christopher S. Reynolds"}],"doi":"10.1093\u002Fmnrasl\u002Fsly060","id":"5c7573c6f56def97988d40c4","lang":"en","num_citation":4,"order":3,"pages":{"end":"L48","start":"L44"},"title":"Limits on turbulent propagation of energy in cool-core clusters of galaxies","venue":{"info":{"name":"MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY"},"issue":"1","volume":"478"},"versions":[{"id":"5c7573c6f56def97988d40c4","sid":"2790917152","src":"mag","vsid":"195663288","year":2018},{"id":"5efe1351dfae548d33e5a7e1","sid":"1803.08175","src":"arxiv","year":2018},{"id":"5fc9afcad83c7e914aa14d8c","sid":"WOS:000450777200009","src":"wos","vsid":"MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY","year":2018}],"year":2018},{"abstract":"Deep Chandra observations of the core of the Perseus cluster show a plethora of complex structures. It has been found that when the observed density fluctuations in the intracluster medium are converted into constraints on AGN-induced turbulence, the resulting turbulent heating rates are sufficient to balance cooling locally throughout the central 220 kpc. However, while the signatures of AGN feedback (inflated bubbles) dominate the central 60 kpc in X-ray images, beyond this radius the intracluster medium is increasingly shaped by the effects of gas sloshing, which can also produce subtle variations in X-ray surface brightness. We use mock Chandra observations of gas sloshing simulations to investigate what fraction of the observed density fluctuations in the core of the Perseus galaxy cluster may originate from sloshing rather than AGN-induced feedback. Outside 60 kpc, we find that the observed level of the density fluctuations is broadly consistent with being produced by sloshing alone. If this is the case, AGN-generated turbulence is likely to be insufficient in combating cooling outside 60 kpc.","authors":[{"name":"S. A. Walker"},{"id":"53f433a2dabfaeecd6943a88","name":"J. S. Sanders"},{"name":"A. C. Fabian"}],"doi":"10.1093\u002Fmnras\u002Fsty2390","id":"5c757d66f56def9798ad9833","lang":"en","num_citation":2,"order":1,"pages":{"end":"1725","start":"1718"},"title":"What fraction of the density fluctuations in the Perseus cluster core is due to gas sloshing rather than AGN feedback","venue":{"info":{"name":"MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY"},"issue":"2","volume":"481"},"versions":[{"id":"5c757d66f56def9798ad9833","sid":"2889406707","src":"mag","vsid":"195663288","year":2018},{"id":"5f049e47dfae54570ec4f259","sid":"1808.10460","src":"arxiv","year":2018},{"id":"5fc9afbfd83c7e914aa147f3","sid":"WOS:000449764000022","src":"wos","vsid":"MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY","year":2018}],"year":2018},{"abstract":"We analyse Chandra X-ray Observatory observations of a set of galaxy clusters selected by the South Pole Telescope using a new publicly available forward-modelling projection code, MBPROJ2, assuming hydrostatic equilibrium. By fitting a power law plus constant entropy model we find no evidence for a central entropy floor in the lowest entropy systems. A model of the underlying central entropy distribution shows a narrow peak close to zero entropy which accounts for 60 per cent of the systems, and a second broader peak around 130 keV cm(2). We look for evolution over the 0.28-1.2 redshift range of the sample in density, pressure, entropy and cooling time at 0.015R(500) and at 10 kpc radius. By modelling the evolution of the central quantities with a simple model, we find no evidence for a non-zero slope with redshift. In addition, a non-parametric sliding median shows no significant change. The fraction of cool-core clusters with central cooling times below 2 Gyr is consistent above and below z = 0.6 (similar to 30-40 per cent). Both by comparing the median thermodynamic profiles, centrally biased towards cool cores, in two redshift bins, and by modelling the evolution of the unbiased average profile as a function of redshift, we find no significant evolution beyond self-similar scaling in any of our examined quantities. Our average modelled radial density, entropy and cooling-time profiles appear as power laws with breaks around 0.2R(500). The dispersion in these quantities rises inwards of this radius to around 0.4 dex, although some of this scatter can be fitted by a bimodal model.","authors":[{"id":"53f433a2dabfaeecd6943a88","name":"J. S. Sanders"},{"id":"54068c09dabfae92b421034c","name":"A. C. Fabian"},{"id":"53f4352cdabfaedce552496a","name":"H. R. Russell"},{"name":"S. A. Walker"}],"doi":"10.1093\u002Fmnras\u002Fstx2796","id":"5ce2c824ced107d4c622387d","lang":"en","num_citation":4,"order":0,"pages":{"end":"1098","start":"1065"},"title":"Hydrostatic Chandra X-ray analysis of SPT-selected galaxy clusters – I. Evolution of profiles and core properties","venue":{"info":{"name":"MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY"},"issue":"1","volume":"474"},"versions":[{"id":"5ce2c824ced107d4c622387d","sid":"2618457823","src":"mag","vsid":"195663288","year":2018},{"id":"5f05396fdfae54570ec54cdd","sid":"1705.09299","src":"arxiv","year":2017},{"id":"5fc9afd5d83c7e914aa1561e","sid":"WOS:000424339500076","src":"wos","vsid":"MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY","year":2018}],"year":2018},{"abstract":"We present a low-frequency view of the Perseus cluster with new observations from the Karl G. Jansky Very Large Array (JVLA) at 230–470 MHz. The data reveal a multitude of new structures associated with the mini-halo. The mini-halo seems to be influenced both by the AGN activity and the sloshing motion of the cool core cluster's gas. In addition, it has a filamentary structure similar to that seen...","authors":[{"name":"M. Gendron-Marsolais"},{"id":"53f47460dabfaeee22a87ad3","name":"J. Hlavacek-Larrondo"},{"id":"53f461f0dabfaeee22a432a3","name":"R. J. van Weeren"},{"id":"53f42b94dabfaedf434fa519","name":"T. Clarke"},{"id":"54068c09dabfae92b421034c","name":"A. C. Fabian"},{"id":"53f47b30dabfaec09f28e16c","name":"H. T. Intema"},{"name":"G. B. Taylor"},{"id":"5405816fdabfae8faa5da2b4","name":"K. M. Blundell"},{"id":"53f433a2dabfaeecd6943a88","name":"J. S. Sanders"}],"doi":"10.1093\u002Fmnras\u002Fstx1042","id":"5ce2c566ced107d4c61bcafb","lang":"en","num_citation":6,"order":8,"pages":{"end":"3880","start":"3872"},"title":"Deep 230–470 MHz VLA observations of the mini-halo in the Perseus cluster","venue":{"info":{"name":"Monthly Notices of the Royal Astronomical Society"},"issue":"4","volume":"469"},"versions":[{"id":"5ce2c566ced107d4c61bcafb","sid":"2576875328","src":"mag","vsid":"195663288","year":2017},{"id":"5f01bba3dfae54360a4572f7","sid":"1701.03791","src":"arxiv","year":2017},{"id":"5f2df3a79fced0a24b454a85","sid":"8201275","src":"ieee","vsid":"8016813","year":2017},{"id":"5fc9afded83c7e914aa15c84","sid":"WOS:000406837900008","src":"wos","vsid":"MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY","year":2017}],"year":2017},{"authors":[{"name":"F. Hofmann"},{"id":"53f433a2dabfaeecd6943a88","name":"J. S. Sanders"},{"id":"53f4b9e6dabfaedce56503d9","name":"Kirpal Nandra"},{"name":"N. Clerc"},{"id":"53f83ff8dabfae9060b1eaf6","name":"M. Gaspari"}],"doi":"10.1051\u002F0004-6361\u002F201526925e","id":"5c757293f56def97988250ba","lang":"en","num_citation":0,"order":1,"pages":{"end":"","start":""},"title":"Thermodynamic perturbations in the X-ray halo of 33 clusters of galaxies observed with Chandra ACIS (Corrigendum)","venue":{"info":{"name":"ASTRONOMY & ASTROPHYSICS"},"issue":"","volume":"608"},"versions":[{"id":"5c757293f56def97988250ba","sid":"2772806696","src":"mag","vsid":"205231332","year":2017},{"id":"5fc6f65fd75e2ac63d5778e6","sid":"WOS:000417619500001","src":"wos","vsid":"ASTRONOMY & ASTROPHYSICS","year":2017}],"year":2017},{"abstract":"The XMM Cluster Archive Super Survey (X-CLASS) is a serendipitously detected X-ray-selected sample of 845 galaxy clusters based on 2774 XMM archival observations and covering an approximately 90 deg2 spread across the high-Galactic latitude (|b| \u003E 20°) sky. The primary goal of this survey is to produce a well-selected sample of galaxy clusters on which cosmological analyses can be performed. This ...","authors":[{"name":"Jethro Ridl"},{"name":"N. Clerc"},{"name":"T. Sadibekova"},{"name":"L. Faccioli"},{"id":"53f4476cdabfaee43ec81ce2","name":"F. Pacaud"},{"id":"53f46bdddabfaee0d9c4440d","name":"J. Greiner"},{"id":"53f4758cdabfaefedbbaa775","name":"T. Krühler"},{"id":"5606866a45cedb33968b9958","name":"M. Salvato"},{"name":"Marie-Luise Menzel"},{"name":"H. Steinle"},{"name":"P. Wiseman"},{"id":"53f4b9e6dabfaedce56503d9","name":"Kirpal Nandra"},{"id":"53f433a2dabfaeecd6943a88","name":"J. S. Sanders"}],"doi":"10.1093\u002Fmnras\u002Fstx394","id":"5c756c8bf56def979849a605","lang":"en","num_citation":4,"order":12,"pages":{"end":"684","start":"662"},"title":"Cosmology with XMM galaxy clusters: the X-CLASS\u002FGROND catalogue and photometric redshifts","venue":{"info":{"name":"Monthly Notices of the Royal Astronomical Society"},"issue":"1","volume":"468"},"versions":[{"id":"5c756c8bf56def979849a605","sid":"2589910198","src":"mag","vsid":"195663288","year":2017},{"id":"5eff5503dfae5482196f8854","sid":"1702.04314","src":"arxiv","year":2017},{"id":"5f2e01d29fced0a24b493e5e","sid":"8213709","src":"ieee","vsid":"8016813","year":2017},{"id":"5fc9afe9d83c7e914aa1602f","sid":"WOS:000398419200049","src":"wos","vsid":"MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY","year":2017}],"year":2017},{"abstract":"The level of random motions in the intracluster gas lying between 20 and 60 kpc radius in the core of the Perseus cluster has been measured by the Hitomi Soft X-ray Spectrometer (SXS) at 164 +\u002F- 10 km s(-1). The maximum energy density in turbulent motions on that scale is therefore low. If dissipated as heat, the turbulent energy will be radiated away in less than 80 Myr and cannot spread across the core. Ahigher velocity is needed to prevent a cooling collapse. Gravity waves are shown to travel too slowly in a radial direction. Here we investigate propagation of energy by sound waves. The energy travels at similar to 1000 km s(-1) and can cross the core in a cooling time. We show that the displacement velocity amplitude of the gas required to carry the power is consistent with the Hitomi result and that the inferred density and temperature variations are consistent with Chandra observations.","authors":[{"id":"5434d30edabfaebba586c99b","name":"Andrew C. Fabian"},{"id":"53f3a8f8dabfae4b34aeb000","name":"S. A. Walker"},{"id":"53f4352cdabfaedce552496a","name":"H. R. Russell"},{"id":"53f9c6efdabfae7f97afb7a3","name":"Ciro Pinto"},{"id":"53f433a2dabfaeecd6943a88","name":"J. S. Sanders"},{"id":"54853b27dabfaed7b5fa1fad","name":"Christopher S. Reynolds"}],"doi":"10.1093\u002Fmnrasl\u002Fslw170","id":"5c7568cef56def979822bc91","lang":"en","num_citation":14,"order":4,"pages":{"end":"L5","start":"L1"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F16\u002F1608\u002F1608.07088.pdf","title":"Do sound waves transport the AGN energy in the Perseus cluster","venue":{"info":{"name":"MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY"},"issue":"1","volume":"464"},"versions":[{"id":"5c7568cef56def979822bc91","sid":"2510987906","src":"mag","vsid":"195663288","year":2017},{"id":"5c6109b0da56297340b890de","sid":"1608.07088","src":"arxiv","year":2016},{"id":"5fc9aff1d83c7e914aa16549","sid":"WOS:000403097500001","src":"wos","vsid":"MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY","year":2017}],"year":2017},{"abstract":"The hot intra-cluster medium (ICM) permeating galaxy clusters and groups is not pristine, as it has been continuously enriched by metals synthesised in Type Ia (SNIa) and core-collapse (SNcc) supernovae since the major epoch of star formation (z similar or equal to 2-3). The cluster\u002Fgroup enrichment history and mechanisms responsible for releasing and mixing the metals can be probed via the radial distribution of SNIa and SNcc products within the ICM. In this paper, we use deep XMM-Newton\u002FEPIC observations from a sample of 44 nearby cool-core galaxy clusters, groups, and ellipticals (CHEERS) to constrain the average radial O, Mg, Si, S, Ar, Ca, Fe, and Ni abundance profiles. The radial distributions of all these elements, averaged over a large sample for the first time, represent the best constrained profiles available currently. Specific attention is devoted to a proper modelling of the EPIC spectral components, and to other systematic uncertainties that may affect our results. We find an overall decrease of the Fe abundance with radius out to similar to 0.9 r(500) and similar to 0.6 r(500) for clusters and groups, respectively, in good agreement with predictions from the most recent hydrodynamical simulations. The average radial profiles of all the other elements (X) are also centrally peaked and, when rescaled to their average central X\u002FFe ratios, follow well the Fe profile out to at least similar to 0.5 r(500). As predicted by recent simulations, we find that the relative contribution of SNIa (SNcc) to the total ICM enrichment is consistent with being uniform at all radii, both for clusters and groups using two sets of SNIa and SNcc yield models that reproduce the X\u002FFe abundance pattern in the core well. In addition to implying that the central metal peak is balanced between SNIa and SNcc, our results suggest that the enriching SNIa and SNcc products must share the same origin and that the delay between the bulk of the SNIa and SNcc explosions must be shorter than the timescale necessary to diffuse out the metals. Finally, we report an apparent abundance drop in the very core of 14 systems (similar to 32% of the sample). Possible origins of these drops are discussed.","authors":[{"name":"F. Mernier"},{"name":"F. Mernier"},{"id":"53f46b50dabfaedf43659114","name":"J. de Plaa"},{"id":"53f43949dabfaec09f198c2c","name":"Jelle S. Kaastra"},{"id":"53f43949dabfaec09f198c2c","name":"Jelle S. Kaastra"},{"id":"53f42f95dabfaeb2ac005b50","name":"Y. Zhang"},{"id":"56315e8845cedb3399db1bda","name":"Hiroki Akamatsu"},{"id":"53f31cc7dabfae9a8443e845","name":"Liyi Gu"},{"name":"P. Kosec"},{"id":"53f44991dabfaedd74dfb5c2","name":"J. Mao"},{"id":"53f44991dabfaedd74dfb5c2","name":"J. Mao"},{"id":"53f9c6efdabfae7f97afb7a3","name":"Ciro Pinto"},{"id":"53f4330adabfaeb22f44f0e1","name":"Thomas H. Reiprich"},{"id":"53f433a2dabfaeecd6943a88","name":"J. S. Sanders"},{"id":"53f465e0dabfaec09f23d928","name":"A. Simionescu"},{"id":"53f447b7dabfaee1c0af1d70","name":"N. Werner"},{"id":"53f447b7dabfaee1c0af1d70","name":"N. Werner"}],"doi":"10.1051\u002F0004-6361\u002F201630075","id":"5c88ff934895d9cbc6a75130","lang":"en","num_citation":18,"order":13,"pages":{"end":"27","start":"1"},"title":"Radial metal abundance profiles in the intra-cluster medium of cool-core galaxy clusters, groups, and ellipticals","venue":{"info":{"name":"ASTRONOMY & ASTROPHYSICS"},"issue":"","volume":"603"},"versions":[{"id":"5c756cacf56def97984b15b7","sid":"2592146358","src":"mag","vsid":"205231332","year":2017},{"id":"5f02559fdfae54360a45cee1","sid":"1703.01183","src":"arxiv","year":2017},{"id":"5ff68d91d4150a363cd5cdaf","sid":"3106051527","src":"mag","vsid":"205231332","year":2017},{"id":"5fc6f68fd75e2ac63d579341","sid":"WOS:000406619100055","src":"wos","vsid":"ASTRONOMY & ASTROPHYSICS","year":2017}],"year":2017},{"abstract":"Deep observations of nearby galaxy clusters with Chandra have revealed concave 'bay' structures in a number of systems (Perseus, Centaurus and Abell 1795), which have similar X-ray and radio properties. These bays have all the properties of cold fronts, where the temperature rises and density falls sharply, but are concave rather than convex. By comparing to simulations of gas sloshing, we find that the bay in the Perseus cluster bears a striking resemblance in its size, location and thermal structure, to a giant (approximate to 50 kpc) roll resulting from Kelvin-Helmholtz instabilities. If true, the morphology of this structure can be compared to simulations to put constraints on the initial average ratio of the thermal and magnetic pressure, beta = p(th)\u002Fp(B), throughout the overall cluster before the sloshing occurs, for which we find beta = 200 to best match the observations. Simulations with a stronger magnetic field (beta = 100) are disfavoured, as in these the large Kelvin-Helmholtz rolls do not form, while in simulations with a lower magnetic field (beta = 500), the level of instabilities is much larger than is observed. We find that the bay structures in Centaurus and Abell 1795 may also be explained by such features of gas sloshing.","authors":[{"name":"S. A. Walker"},{"id":"53f47460dabfaeee22a87ad3","name":"J. Hlavacek-Larrondo"},{"name":"M. Gendron-Marsolais"},{"id":"54068c09dabfae92b421034c","name":"A. C. Fabian"},{"name":"H. T. Intema"},{"id":"53f433a2dabfaeecd6943a88","name":"J. S. Sanders"},{"name":"J. T. Bamford"},{"id":"53f461f0dabfaeee22a432a3","name":"R. J. van Weeren"}],"doi":"10.1093\u002Fmnras\u002Fstx640","id":"5c756db9f56def9798559581","lang":"en","num_citation":14,"order":5,"pages":{"end":"2516","start":"2506"},"title":"Is there a giant Kelvin-Helmholtz instability in the sloshing cold front of the Perseus cluster?","venue":{"info":{"name":"MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY"},"issue":"2.0","volume":"468"},"versions":[{"id":"5c756db9f56def9798559581","sid":"2606196770","src":"mag","vsid":"195663288","year":2017},{"id":"5f029a38dfae54360a45f2f0","sid":"1705.00011","src":"arxiv","year":2017},{"id":"5fc9afe8d83c7e914aa16005","sid":"WOS:000399429600095","src":"wos","vsid":"MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY","year":2017}],"year":2017},{"abstract":"Context. The eROSITA mission will provide the largest sample of galaxy clusters detected in X-ray to date (one hundred thousand expected). This sample will be used to constrain cosmological models by measuring cluster masses. An important mass proxy is the electron temperature of the hot plasma detected in X-rays. Aims. We want to understand the detection properties and possible bias in temperatures due to unresolved substructures in the cluster halos. Methods. We simulated a large number of galaxy cluster spectra with known temperature substructures and compared the results from analysing eROSITA simulated observations to earlier results from Chandra. Results. We were able to constrain a bias in cluster temperatures and its impact on cluster masses, as well as cosmological parameters derived from the survey. We found temperatures in the eROSITA survey to be biased low by about five per cent due to unresolved temperature substructures (compared to emission-weighted average temperatures from the Chandra maps). This bias would have a significant impact on the eROSITA cosmology constraints if not accounted for in the calibration. Conclusions. We isolated the bias effect that substructures in galaxy clusters have on temperature measurements and their impact on derived cosmological parameters in the eROSITA cluster survey.","authors":[{"name":"F. Hofmann"},{"id":"53f433a2dabfaeecd6943a88","name":"J. S. Sanders"},{"name":"N. Clerc"},{"name":"N. Clerc"},{"name":"N. Clerc"},{"id":"53f4b9e6dabfaedce56503d9","name":"Kirpal Nandra"},{"name":"Jethro Ridl"},{"id":"53f4340fdabfaec22ba6aa57","name":"Konrad Dennerl"},{"name":"M. E. Ramos-Ceja"},{"id":"53f79514dabfae8faa49bad3","name":"A. Finoguenov"},{"id":"53f79514dabfae8faa49bad3","name":"A. Finoguenov"},{"id":"53f4330adabfaeb22f44f0e1","name":"Thomas H. Reiprich"}],"doi":"10.1051\u002F0004-6361\u002F201730742","id":"5c7570dff56def979873092e","lang":"en","num_citation":2,"order":1,"pages":{"end":"","start":"118"},"title":"eROSITA cluster cosmology forecasts: Cluster temperature substructure bias","venue":{"info":{"name":"ASTRONOMY & ASTROPHYSICS"},"issue":"","volume":"606"},"versions":[{"id":"5c7570dff56def979873092e","sid":"2750273462","src":"mag","vsid":"205231332","year":2017},{"id":"5f0340d8dfae54360a46530f","sid":"1708.05205","src":"arxiv","year":2017},{"id":"5ff68c60d4150a363cd23641","sid":"3102222322","src":"mag","vsid":"205231332","year":2017},{"id":"5fc6f686d75e2ac63d578d7c","sid":"WOS:000413564000007","src":"wos","vsid":"ASTRONOMY & ASTROPHYSICS","year":2017}],"year":2017},{"abstract":"The Wide Field Imager (WFI) is one of two instruments for the Advanced Telescope for High-ENergy Astrophysics (Athena). In this paper we summarise three of the many key science objectives for the WFI - the formation and growth of supermassive black holes, non-gravitational heating in clusters of galaxies, and spin measurements of stellar mass black holes - and describe their translation into the science requirements and ultimately instrument requirements. The WFI will be designed to provide excellent point source sensitivity and grasp for performing wide area surveys, surface brightness sensitivity, survey power, and absolute temperature and density calibration for in-depth studies of the outskirts of nearby clusters of galaxies and very good high-count rate capability, throughput, and low pile-up, paired with very good spectral resolution, for detailed explorations of bright Galactic compact objects.","authors":[{"id":"53f4b9e6dabfaedce56503d9","name":"Kirpal Nandra"},{"name":"James Aird"},{"id":"543352dbdabfaeb4c6ab63a7","name":"A. Comastri"},{"name":"T. Dauser"},{"id":"53f4505edabfaee4dc7f996e","name":"Andrea Merloni"},{"id":"53f48a2fdabfaea6fb77b41f","name":"G. W. Pratt"},{"id":"53f4330adabfaeb22f44f0e1","name":"Thomas H. Reiprich"},{"name":"Andrew C. Fabian"},{"id":"5447f813dabfae87b7db71b0","name":"A. Georgakakis"},{"id":"53f3a1badabfae4b34abe3b3","name":"M. Güdel"},{"id":"53f43094dabfaee0d9b2566d","name":"Agata Rozanska"},{"id":"53f433a2dabfaeecd6943a88","name":"J. S. Sanders"},{"id":"53f42e30dabfaec22ba22498","name":"Manami Sasaki"},{"id":"54353294dabfaebba58b071c","name":"S. Vaughan"},{"id":"53f45019dabfaeb22f4e7ced","name":"J. Wilms"},{"id":"53f4536cdabfaee2a1d687ea","name":"Norbert Meidinger"}],"doi":"10.1117\u002F12.2235268","id":"5c7566eaf56def97981208fa","lang":"en","num_citation":0,"order":11,"pages":{"end":"11","start":"1"},"title":"Athena Wide Field Imager Key Science Drivers","venue":{"info":{"name":"Proceedings of SPIE"},"issue":"","volume":"9905"},"versions":[{"id":"5c7566eaf56def97981208fa","sid":"2469338889","src":"mag","vsid":"183492911","year":2016},{"id":"5ff68b17d4150a363cce4dae","sid":"3098096787","src":"mag","vsid":"183492911","year":2016},{"id":"5ff5b046bf33bee3ba044421","sid":"WOS:000387731500064","src":"wos","vsid":"Proceedings of SPIE","year":2016}],"year":2016},{"abstract":"Aims. We aim to systematically investigate the cores of a sample of fossil galaxy groups and clusters (\"fossil systems\"), using Chandra data, to see what hints they can offer about the properties of the intracluster medium in these particular objects. Methods. We chose a sample of 17 fossil systems from literature with archival Chandra data and determined the cool-core fraction for fossils via three observable diagnostics, namely the central cooling time, cuspiness, and concentration parameter. We quantified the dynamical state of the fossils by the X-ray peak\u002Fbrightest cluster galaxy (BCG) separation, and the X-ray peak\u002Femission weighted centre separation. We also investigated the X-ray emission coincident with the brightest cluster galaxy (BCG) to detect the presence of potential thermal coronae. A deprojection analysis was performed for fossils with z \u003C 0.05 to resolve subtle temperature structures, and to obtain the cooling time and entropy profiles. We also investigated the L-X - T relation for fossils from the 400d catalogue to test whether the scaling relation deviates from what is typically observed for other groups. Results. Most fossils are identified as cool-core objects via at least two cool-core diagnostics with the population of weak cool-core fossils being the highest. All fossils have their dominant elliptical galaxy within 50 kpc of the X-ray peak, and most also have the emission weighted centre within that distance. We do not see clear indications of an X-ray corona associated with the BCG unlike coronae observed for some other clusters. Fossils lack universal temperature profiles, with some low-temperature objects generally not showing features that are expected for ostensibly relaxed objects with a cool-core. The entropy profiles of the z \u003C 0.05 fossil systems can be described well by a power law with shallower indices than what is expected for pure gravitational processes. Finally, the fossils L-X - T relation shows indications of an elevated normalisation with respect to other groups, which seems to persist even after factoring in selection effects. Conclusions. We interpret these results within the context of the formation and evolution of fossils, and speculate that nongravitational heating, and AGN feedback in particular, could have had an impact on the ICM properties of these systems.","abstract_zh":"","authors":[{"name":"v bharadwaj"},{"id":"53f4330adabfaeb22f44f0e1","name":"thomas h reiprich"},{"id":"53f433a2dabfaeecd6943a88","name":"j s sanders"},{"name":"g schellenberger"}],"doi":"10.1051\u002F0004-6361\u002F201525824","id":"56d91f4bdabfae2eee9399b7","lang":"en","num_citation":4,"order":2,"pages":{"end":"14","start":"1"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F15\u002F1509\u002F1509.04275.pdf","title":"Investigating the cores of fossil systems with Chandra","urls":["http:\u002F\u002Fdx.doi.org\u002F10.1051\u002F0004-6361\u002F201525824","https:\u002F\u002Farxiv.org\u002Fabs\u002F1509.04275","https:\u002F\u002Fui.adsabs.harvard.edu\u002Fabs\u002F2016A&A...585A.125B\u002Fabstract","https:\u002F\u002Fpure.mpg.de\u002Fpubman\u002Ffaces\u002FViewItemOverviewPage.jsp?itemId=item_2264246","http:\u002F\u002Fpubman.mpdl.mpg.de\u002Fpubman\u002Fitem\u002Fescidoc:2264246","http:\u002F\u002Fwww.webofknowledge.com\u002F"],"venue":{"info":{"name":"ASTRONOMY & ASTROPHYSICS"},"issue":"","volume":"585"},"versions":[{"id":"56d91f4bdabfae2eee9399b7","sid":"2200373900","src":"mag","year":2016},{"id":"5c610944da56297340b6ca6e","sid":"1509.04275","src":"arxiv","year":2015},{"id":"5ff68c2dd4150a363cd19e08","sid":"3101643798","src":"mag","vsid":"205231332","year":2016},{"id":"5fc6f6afd75e2ac63d579dd0","sid":"WOS:000369710300132","src":"wos","vsid":"ASTRONOMY & ASTROPHYSICS","year":2016}],"year":2016},{"abstract":"The effects of many physical processes in the intracluster medium of galaxy clusters imprint themselves in X-ray surface brightness images. It is therefore important to choose optimal methods for extracting information from and enhancing the interpretability of such images. We describe in detail a gradient filtering edge detection method that we previously applied to images of the Centaurus cluste...","authors":[{"id":"53f433a2dabfaeecd6943a88","name":"J. S. Sanders"},{"id":"5434d30edabfaebba586c99b","name":"Andrew C. Fabian"},{"id":"53f4352cdabfaedce552496a","name":"H. R. Russell"},{"id":"53f3a8f8dabfae4b34aeb000","name":"S. A. Walker"},{"id":"5405816fdabfae8faa5da2b4","name":"Katherine M. Blundell"}],"doi":"10.1093\u002Fmnras\u002Fstw1119","id":"5c755b55f56def979890ea29","lang":"en","num_citation":0,"order":0,"pages":{"end":"1911","start":"1898"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F16\u002F1605\u002F1605.02911.pdf","title":"Detecting edges in the X-ray surface brightness of galaxy clusters","venue":{"info":{"name":"Monthly Notices of the Royal Astronomical Society"},"issue":"2","volume":"460"},"versions":[{"id":"5c755b55f56def979890ea29","sid":"2356435318","src":"mag","vsid":"195663288","year":2016},{"id":"5c61098fda56297340b80426","sid":"1605.02911","src":"arxiv","year":2016},{"id":"5f2d9be79fced0a24b2a1e57","sid":"8166205","src":"ieee","vsid":"8016813","year":2016},{"id":"5fc9affcd83c7e914aa16d85","sid":"WOS:000379832800059","src":"wos","vsid":"MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY","year":2016}],"year":2016},{"abstract":"We present ALMA CO(1-0) and CO(3-2) observations of the brightest cluster galaxy (BCG) in the 2A 0335+096 galaxy cluster (z = 0.0346). The total molecular gas mass of 1.13 +\u002F- 0.15 x 10(9) M-circle dot is divided into two components: a nuclear region and a 7 kpc long dusty filament. The central molecular gas component accounts for 3.2 +\u002F- 0.4 x 10(8) M-circle dot of the total supply of cold gas. Instead of forming a rotationally supported ring or disk, it is composed of two distinct, blueshifted clumps south of the nucleus and a series of low-significance redshifted clumps extending toward a nearby companion galaxy. The velocity of the redshifted clouds increases with radius to a value consistent with the companion galaxy, suggesting that an interaction between these galaxies \u003C20 Myr ago disrupted a pre-existing molecular gas reservoir within the BCG. Most of the molecular gas, 7.8 +\u002F- 0.9 x 10(8) M-circle dot, is located in the filament. The CO emission is co-spatial with a 10(4) K emission-line nebula and soft X-rays from 0.5 keV gas, indicating that the molecular gas has cooled out of the intracluster medium over a period of 25-100 Myr. The filament trails an X-ray cavity, suggesting that the gas has cooled from low-entropy gas that has been lifted out of the cluster core and become thermally unstable. We are unable to distinguish between inflow and outflow along the filament with the present data. Cloud velocities along the filament are consistent with gravitational free-fall near the plane of the sky, although their increasing blueshifts with radius are consistent with outflow.","authors":[{"name":"An Vantyghem"},{"id":"53f4353bdabfaeb22f467922","name":"Br McNamara"},{"id":"53f4352cdabfaedce552496a","name":"Helen Rebecca Russell"},{"name":"Mt Hogan"},{"name":"Ac Edge"},{"name":"Pej Nulsen"},{"id":"5434d30edabfaebba586c99b","name":"Andrew Christopher Fabian"},{"id":"53f431d0dabfaec22ba50ab9","name":"F Combes"},{"id":"53f7bb04dabfae9060ae2114","name":"P Salome"},{"name":"Sa Baum"},{"id":"53f4be6cdabfaedce5656757","name":"M Donahue"},{"name":"Ra Main"},{"name":"Nw Murray"},{"name":"Rw O'Connell"},{"name":"Cp O'Dea"},{"name":"Jbr Oonk"},{"name":"Ij Parrish"},{"id":"53f433a2dabfaeecd6943a88","name":"Js Sanders"},{"id":"53f4423fdabfaee43ec70158","name":"G Tremblay"},{"name":"Gm Voit"}],"doi":"10.3847\u002F0004-637X\u002F832\u002F2\u002F148","id":"5ce2c382ced107d4c616a3e5","lang":"en","num_citation":0,"order":17,"pages":{"end":"","start":"148"},"title":"MOLECULAR GAS ALONG A BRIGHT Hα FILAMENT in 2A 0335+096 REVEALED by ALMA","venue":{"info":{"name":"ASTROPHYSICAL JOURNAL"},"issue":"2","volume":"832"},"versions":[{"id":"5ce2c382ced107d4c616a3e5","sid":"2528756926","src":"mag","vsid":"1980519","year":2016},{"id":"5efdec56dfae548d33e5907c","sid":"1610.00716","src":"arxiv","year":2016},{"id":"5fc6f8c0d75e2ac63d58f700","sid":"WOS:000390490100008","src":"wos","vsid":"ASTROPHYSICAL JOURNAL","year":2016}],"year":2016}],"profilePubsTotal":183,"profilePatentsPage":1,"profilePatents":[],"profilePatentsTotal":0,"profilePatentsEnd":true,"profileProjectsPage":0,"profileProjects":null,"profileProjectsTotal":null,"newInfo":null,"checkDelPubs":[]}};