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breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Lamer%2C+G&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Lamer%2C+G&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Lamer%2C+G&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> </ul> </nav> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.17238">arXiv:2501.17238</a> <span> [<a href="https://arxiv.org/pdf/2501.17238">pdf</a>, <a href="https://arxiv.org/format/2501.17238">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 First SRG/eROSITA All-Sky Survey. Characterization of clusters of galaxies misclassified in the eRASS1 point source catalog </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Balzer%2C+F">F. Balzer</a>, <a href="/search/?searchtype=author&query=Bulbul%2C+E">E. Bulbul</a>, <a href="/search/?searchtype=author&query=Kluge%2C+M">M. Kluge</a>, <a href="/search/?searchtype=author&query=Liu%2C+A">A. Liu</a>, <a href="/search/?searchtype=author&query=Salvato%2C+M">M. Salvato</a>, <a href="/search/?searchtype=author&query=Fabricius%2C+M">M. Fabricius</a>, <a href="/search/?searchtype=author&query=Seppi%2C+R">R. Seppi</a>, <a href="/search/?searchtype=author&query=Artis%2C+E">E. Artis</a>, <a href="/search/?searchtype=author&query=Bahar%2C+Y+E">Y. E. Bahar</a>, <a href="/search/?searchtype=author&query=Bender%2C+R">R. Bender</a>, <a href="/search/?searchtype=author&query=Clerc%2C+N">N. Clerc</a>, <a href="/search/?searchtype=author&query=Comparat%2C+J">J. Comparat</a>, <a href="/search/?searchtype=author&query=Ghirardini%2C+V">V. Ghirardini</a>, <a href="/search/?searchtype=author&query=Grandis%2C+S">S. Grandis</a>, <a href="/search/?searchtype=author&query=Krippendorf%2C+S">S. Krippendorf</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">G. Lamer</a>, <a href="/search/?searchtype=author&query=Malavasi%2C+N">N. Malavasi</a>, <a href="/search/?searchtype=author&query=Merloni%2C+A">A. Merloni</a>, <a href="/search/?searchtype=author&query=Nandra%2C+K">K. Nandra</a>, <a href="/search/?searchtype=author&query=Ramos-Ceja%2C+M+E">M. E. Ramos-Ceja</a>, <a href="/search/?searchtype=author&query=Sanders%2C+J+S">J. S. Sanders</a>, <a href="/search/?searchtype=author&query=Zhang%2C+X">X. Zhang</a>, <a href="/search/?searchtype=author&query=Zelmer%2C+S">S. Zelmer</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="2501.17238v1-abstract-short" style="display: inline;"> The detection of the extended X-ray-emission of the intracluster medium by the first SRG/eROSITA All-Sky Survey (eRASS1), combined with optical and near-infrared follow-up, resulted in the identification of more than 12000 galaxy clusters, yielding precise constraints on cosmological parameters. However, some clusters of galaxies can be misclassified as point sources by eROSITA's source detection… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.17238v1-abstract-full').style.display = 'inline'; document.getElementById('2501.17238v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.17238v1-abstract-full" style="display: none;"> The detection of the extended X-ray-emission of the intracluster medium by the first SRG/eROSITA All-Sky Survey (eRASS1), combined with optical and near-infrared follow-up, resulted in the identification of more than 12000 galaxy clusters, yielding precise constraints on cosmological parameters. However, some clusters of galaxies can be misclassified as point sources by eROSITA's source detection algorithm due to the interplay between the point-spread function, the shallow depth of the survey, compact (cool core) X-ray emission, and bright active galactic nuclei hosted in their centers or their vicinity. To identify such misclassified galaxy clusters and groups, we apply optical follow-up to the eRASS1 X-ray point sources analogously to the treatment of the extent-selected catalog. After rigorous filtering to ensure purity, we find a total of 8347 clusters of galaxies, of which 5819 are novel detections, in a redshift range $0.05 < z \lesssim 1.1$. This corresponds to a 70 % discovery rate, a fraction similar to that of the extent-selected sample. To facilitate finding new exceptional clusters such as the Phoenix cluster (which is recovered in our sample), we divide the clusters into five classes based on the optical properties of likely single-source counterparts to the X-ray emission. We further investigate potential biases in our selection process by analyzing the optical and X-ray data. With this work, we provide a catalog of galaxy clusters and groups in the eRASS1 point source catalog, including their optical and X-ray properties along with a meaningful classification. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.17238v1-abstract-full').style.display = 'none'; document.getElementById('2501.17238v1-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 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 pages, 16 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.17120">arXiv:2411.17120</a> <span> [<a href="https://arxiv.org/pdf/2411.17120">pdf</a>, <a href="https://arxiv.org/format/2411.17120">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="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Average X-ray properties of galaxy groups. From Milky Way-like halos to massive clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Popesso%2C+P">P. Popesso</a>, <a href="/search/?searchtype=author&query=Marini%2C+I">I. Marini</a>, <a href="/search/?searchtype=author&query=Dolag%2C+K">K. Dolag</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">G. Lamer</a>, <a href="/search/?searchtype=author&query=Csizi%2C+B">B. Csizi</a>, <a href="/search/?searchtype=author&query=Biffi%2C+V">V. Biffi</a>, <a href="/search/?searchtype=author&query=Robothan%2C+A">A. Robothan</a>, <a href="/search/?searchtype=author&query=Bravo%2C+M">M. Bravo</a>, <a href="/search/?searchtype=author&query=Biviano%2C+A">A. Biviano</a>, <a href="/search/?searchtype=author&query=Vladutesku-Zopp%2C+S">S. Vladutesku-Zopp</a>, <a href="/search/?searchtype=author&query=Lovisari%2C+L">L. Lovisari</a>, <a href="/search/?searchtype=author&query=Ettori%2C+S">S. Ettori</a>, <a href="/search/?searchtype=author&query=Angelinelli%2C+M">M. Angelinelli</a>, <a href="/search/?searchtype=author&query=Driver%2C+S">S. Driver</a>, <a href="/search/?searchtype=author&query=Toptun%2C+V">V. Toptun</a>, <a href="/search/?searchtype=author&query=Dev%2C+A">A. Dev</a>, <a href="/search/?searchtype=author&query=Mazengo%2C+D">D. Mazengo</a>, <a href="/search/?searchtype=author&query=Merloni%2C+A">A. Merloni</a>, <a href="/search/?searchtype=author&query=Zhang%2C+Y">Y. Zhang</a>, <a href="/search/?searchtype=author&query=Comparat%2C+J">J. Comparat</a>, <a href="/search/?searchtype=author&query=Ponti%2C+G">G. Ponti</a>, <a href="/search/?searchtype=author&query=Mroczkowski%2C+T">T. Mroczkowski</a>, <a href="/search/?searchtype=author&query=Bulbul%2C+E">E. Bulbul</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.17120v2-abstract-short" style="display: inline;"> This study examines the average X-ray properties of massive halos at z< 0.2, covering the largest halo mass range to date, from Milky Way-like halos to massive clusters. The analysis is based on stacking in the eFEDS area of the GAMA galaxy group sample, validated with synthetic data that mimic observed eROSITA X-ray and GAMA optical data using Magneticum lightcones. Stacking was conducted in halo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.17120v2-abstract-full').style.display = 'inline'; document.getElementById('2411.17120v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.17120v2-abstract-full" style="display: none;"> This study examines the average X-ray properties of massive halos at z< 0.2, covering the largest halo mass range to date, from Milky Way-like halos to massive clusters. The analysis is based on stacking in the eFEDS area of the GAMA galaxy group sample, validated with synthetic data that mimic observed eROSITA X-ray and GAMA optical data using Magneticum lightcones. Stacking was conducted in halo mass bins and tested for AGN and X-ray binary contamination, systematics in the halo mass proxy, and uncertainties in optical group centers. The study provides average X-ray surface brightness profiles in six mass bins, spanning Milky Way-like systems to poor clusters. The scatter in the X-ray luminosity-mass (LX-M) relation is attributed to gas concentration: low X-ray luminosity systems at fixed halo mass exhibit lower central gas concentrations than high-luminosity systems, consistent with Magneticum predictions. However, discrepancies in dark matter concentration arise, with Magneticum predicting undetected groups as older and more relaxed, while observations suggest the opposite. New LX-M relations are presented covering three decades of halo mass. These relations fit a single power law, aligning with previous studies. Magneticum matches observed gas distributions across all masses, whereas IllustrisTNG, EAGLE, Simba, and FLAMINGO exhibit significant discrepancies at various mass scales. Simulations calibrated on local galaxy properties accurately reproduce central galaxies but fail to capture gas properties. Conversely, simulations like Magneticum excel in gas predictions but produce overly massive central galaxies. Further exploration of gas and dark matter distributions and their effects on galaxy properties is critical to comprehending the role of gravitational forces and feedback in shaping large-scale structure and galaxy evolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.17120v2-abstract-full').style.display = 'none'; document.getElementById('2411.17120v2-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 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to A&A, 15 pages, 9 figures. Abstract adapted to arxiv submission. arXiv admin note: text overlap with arXiv:2411.16546</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.16555">arXiv:2411.16555</a> <span> [<a href="https://arxiv.org/pdf/2411.16555">pdf</a>, <a href="https://arxiv.org/format/2411.16555">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="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> The hot gas mass fraction in halos. From Milky Way-like groups to massive clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Popesso%2C+P">P. Popesso</a>, <a href="/search/?searchtype=author&query=Biviano%2C+A">A. Biviano</a>, <a href="/search/?searchtype=author&query=Marini%2C+I">I. Marini</a>, <a href="/search/?searchtype=author&query=Dolag%2C+K">K. Dolag</a>, <a href="/search/?searchtype=author&query=Vladutescu-Zopp%2C+S">S. Vladutescu-Zopp</a>, <a href="/search/?searchtype=author&query=Csizi%2C+B">B. Csizi</a>, <a href="/search/?searchtype=author&query=Biffi%2C+V">V. Biffi</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">G. Lamer</a>, <a href="/search/?searchtype=author&query=Robothan%2C+A">A. Robothan</a>, <a href="/search/?searchtype=author&query=Bravo%2C+M">M. Bravo</a>, <a href="/search/?searchtype=author&query=Lovisari%2C+L">L. Lovisari</a>, <a href="/search/?searchtype=author&query=Ettori%2C+S">S. Ettori</a>, <a href="/search/?searchtype=author&query=Angelinelli%2C+M">M. Angelinelli</a>, <a href="/search/?searchtype=author&query=Driver%2C+S">S. Driver</a>, <a href="/search/?searchtype=author&query=Toptun%2C+V">V. Toptun</a>, <a href="/search/?searchtype=author&query=Dev%2C+A">A. Dev</a>, <a href="/search/?searchtype=author&query=Mazengo%2C+D">D. Mazengo</a>, <a href="/search/?searchtype=author&query=Merloni%2C+A">A. Merloni</a>, <a href="/search/?searchtype=author&query=Comparat%2C+J">J. Comparat</a>, <a href="/search/?searchtype=author&query=Ponti%2C+G">G. Ponti</a>, <a href="/search/?searchtype=author&query=Mroczkowski%2C+T">T. Mroczkowski</a>, <a href="/search/?searchtype=author&query=Bulbul%2C+E">E. Bulbul</a>, <a href="/search/?searchtype=author&query=Grandis%2C+S">S. Grandis</a>, <a href="/search/?searchtype=author&query=Bahar%2C+E">E. Bahar</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.16555v2-abstract-short" style="display: inline;"> By using eROSITA data in the eFEDS area, we provide a measure of the hot gas fraction vs. halo mass relation over the largest halo mass range, from Milky Way-sized halos to massive clusters, and to the largest radii ever probed so far in local systems. To cope with the incompleteness and selection biases of the X-ray selection, we apply the stacking technique in eROSITA data of a highly complete a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.16555v2-abstract-full').style.display = 'inline'; document.getElementById('2411.16555v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.16555v2-abstract-full" style="display: none;"> By using eROSITA data in the eFEDS area, we provide a measure of the hot gas fraction vs. halo mass relation over the largest halo mass range, from Milky Way-sized halos to massive clusters, and to the largest radii ever probed so far in local systems. To cope with the incompleteness and selection biases of the X-ray selection, we apply the stacking technique in eROSITA data of a highly complete and tested sample of optically selected groups. The method has been extensively tested on mock observations. In massive clusters, the hot gas alone provides a baryon budget within $R_{200}$ consistent with the cosmic value. At the same time, at the group mass scale, it accounts only for 20-40% of it. The hot gas fraction vs. halo mass relation is well-fitted by a power law, with a consistent shape and a normalization varying at maximum by a factor of 2 from $r_{500}$ to $r_{200}$. Such a relation is consistent with other works in the literature that consider X-ray survey data at the same depth as eFEDS. However, it provides a lower average gas fraction in the group regime than works based on X-ray bright group samples. The comparison of the observed relation with the predictions of several hydrodynamical simulations (BAHAMAS, FLAMINGO, SIMBA, Illustris, IllustrisTNG, MillenniumTNG, and Magneticum) shows that all simulations but Magneticum and SIMBA overpredict the gas fraction, with the largest discrepancy (up to a factor of 3) in the massive group-poor cluster halo mass range. We emphasize the need for mechanisms that can effectively expel gas to larger radii in galaxy groups without excessively quenching star formation in their member galaxies. Current hydrodynamical simulations face a significant challenge in balancing their subgrid physics: none can sufficiently evacuate gas from the halo virial region without negatively impacting the properties of the resident galaxy population. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.16555v2-abstract-full').style.display = 'none'; document.getElementById('2411.16555v2-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 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">submitted to A&A, 11 pages, 8 figures. Abstract reduced for ArXiv submission</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.16546">arXiv:2411.16546</a> <span> [<a href="https://arxiv.org/pdf/2411.16546">pdf</a>, <a href="https://arxiv.org/format/2411.16546">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="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> The perils of stacking optically selected groups in eROSITA data. The Magneticum perspective </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Popesso%2C+P">P. Popesso</a>, <a href="/search/?searchtype=author&query=Marini%2C+I">I. Marini</a>, <a href="/search/?searchtype=author&query=Dolag%2C+K">K. Dolag</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">G. Lamer</a>, <a href="/search/?searchtype=author&query=Csizi%2C+B">B. Csizi</a>, <a href="/search/?searchtype=author&query=Vladutescu-Zopp%2C+S">S. Vladutescu-Zopp</a>, <a href="/search/?searchtype=author&query=Biffi%2C+V">V. Biffi</a>, <a href="/search/?searchtype=author&query=Robothan%2C+A">A. Robothan</a>, <a href="/search/?searchtype=author&query=Bravo%2C+M">M. Bravo</a>, <a href="/search/?searchtype=author&query=Tempel%2C+E">E. Tempel</a>, <a href="/search/?searchtype=author&query=Yang%2C+X">X. Yang</a>, <a href="/search/?searchtype=author&query=Li%2C+Q">Q. Li</a>, <a href="/search/?searchtype=author&query=Biviano%2C+A">A. Biviano</a>, <a href="/search/?searchtype=author&query=Lovisari%2C+L">L. Lovisari</a>, <a href="/search/?searchtype=author&query=Ettori%2C+S">S. Ettori</a>, <a href="/search/?searchtype=author&query=Angelinelli%2C+M">M. Angelinelli</a>, <a href="/search/?searchtype=author&query=Driver%2C+S">S. Driver</a>, <a href="/search/?searchtype=author&query=Toptun%2C+V">V. Toptun</a>, <a href="/search/?searchtype=author&query=Dev%2C+A">A. Dev</a>, <a href="/search/?searchtype=author&query=Mazengo%2C+D">D. Mazengo</a>, <a href="/search/?searchtype=author&query=Merloni%2C+A">A. Merloni</a>, <a href="/search/?searchtype=author&query=Mroczkowski%2C+T">T. Mroczkowski</a>, <a href="/search/?searchtype=author&query=Comparat%2C+J">J. Comparat</a>, <a href="/search/?searchtype=author&query=Zhang%2C+Y">Y. Zhang</a>, <a href="/search/?searchtype=author&query=Ponti%2C+G">G. Ponti</a> , et al. (1 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="2411.16546v2-abstract-short" style="display: inline;"> Hydrodynamical simulation predictions are often compared with observational data without fully accounting for systematics and biases specific to observational techniques. Using the magnetohydrodynamical simulation Magneticum, we generate mock eROSITA eRASS:4 data, combined with GAMA-like spectroscopic surveys and optically selected galaxy catalogs from the same light-cone, to analyze hot gas prope… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.16546v2-abstract-full').style.display = 'inline'; document.getElementById('2411.16546v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.16546v2-abstract-full" style="display: none;"> Hydrodynamical simulation predictions are often compared with observational data without fully accounting for systematics and biases specific to observational techniques. Using the magnetohydrodynamical simulation Magneticum, we generate mock eROSITA eRASS:4 data, combined with GAMA-like spectroscopic surveys and optically selected galaxy catalogs from the same light-cone, to analyze hot gas properties in galaxy groups via a stacking technique. This study aims to (i) incorporate observational systematics into predictions and (ii) evaluate the reliability of stacking techniques for determining average X-ray properties of galaxy groups. Our analysis provides X-ray emission predictions from Magneticum, including contributions from AGN, X-ray binaries (XRBs), and the Intra-Group Medium (IGM) as a function of halo mass, covering Milky Way (MW)-like groups to poor clusters. We find that AGN and XRBs dominate the X-ray surface brightness profiles of low-mass halos. The reliability of stacking techniques is tested by reproducing input X-ray surface brightness and electron density profiles, accounting for completeness and contamination of prior samples, miscentering of optical group centers, uncertainties in X-ray emissivity due to gas temperature and metallicity assumption, and systematics in halo mass proxies. The halo mass proxy emerges as the primary source of systematics, affecting X-ray surface brightness and scaling relations. We show that stacked X-ray luminosity-mass relations are flatter than input relations but consistent with observations. Additionally, the retrieved hot gas fraction-mass relation aligns well with observational data. These results highlight the need to account for systematic errors when comparing stacking techniques to other methods using different prior catalogs or predictions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.16546v2-abstract-full').style.display = 'none'; document.getElementById('2411.16546v2-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 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to A&A. 18 pages and 19 figures, Abstract reduced for ArXiv submission</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.16455">arXiv:2411.16455</a> <span> [<a href="https://arxiv.org/pdf/2411.16455">pdf</a>, <a href="https://arxiv.org/format/2411.16455">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="High Energy Astrophysical Phenomena">astro-ph.HE</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/10.1051/0004-6361/202452028">10.1051/0004-6361/202452028 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Detecting clusters and groups of galaxies populating the local Universe in large optical spectroscopic surveys </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Marini%2C+I">I. Marini</a>, <a href="/search/?searchtype=author&query=Popesso%2C+P">P. Popesso</a>, <a href="/search/?searchtype=author&query=Dolag%2C+K">K. Dolag</a>, <a href="/search/?searchtype=author&query=Bravo%2C+M">M. Bravo</a>, <a href="/search/?searchtype=author&query=Robotham%2C+A">A. Robotham</a>, <a href="/search/?searchtype=author&query=Tempel%2C+E">E. Tempel</a>, <a href="/search/?searchtype=author&query=Li%2C+Q">Q. Li</a>, <a href="/search/?searchtype=author&query=Yang%2C+X">X. Yang</a>, <a href="/search/?searchtype=author&query=Csizi%2C+B">B. Csizi</a>, <a href="/search/?searchtype=author&query=Behroozi%2C+P">P. Behroozi</a>, <a href="/search/?searchtype=author&query=Biffi%2C+V">V. Biffi</a>, <a href="/search/?searchtype=author&query=Biviano%2C+A">A. Biviano</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">G. Lamer</a>, <a href="/search/?searchtype=author&query=Malavasi%2C+N">N. Malavasi</a>, <a href="/search/?searchtype=author&query=Mazengo%2C+D">D. Mazengo</a>, <a href="/search/?searchtype=author&query=Toptun%2C+V">V. Toptun</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.16455v1-abstract-short" style="display: inline;"> Wide-field cosmological surveys provide hundreds of thousands of spectroscopically confirmed galaxy groups and clusters, valuable for tracing baryonic matter distribution. However, controlling systematics in identifying host dark matter halos and estimating their properties is crucial. We evaluate three group detection methods on a simulated dataset replicating the GAMA selection to understand sys… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.16455v1-abstract-full').style.display = 'inline'; document.getElementById('2411.16455v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.16455v1-abstract-full" style="display: none;"> Wide-field cosmological surveys provide hundreds of thousands of spectroscopically confirmed galaxy groups and clusters, valuable for tracing baryonic matter distribution. However, controlling systematics in identifying host dark matter halos and estimating their properties is crucial. We evaluate three group detection methods on a simulated dataset replicating the GAMA selection to understand systematics and selection effects. This is key for interpreting data from SDSS, GAMA, DESI, WAVES, and leveraging optical catalogues in the (X-ray) eROSITA era to quantify baryonic mass in galaxy groups. Using a lightcone from the Magneticum hydrodynamical simulation, we simulate a spectroscopic galaxy survey in the local Universe (down to $z<0.2$ and stellar mass completeness $M_{\star}\geq10^{9.8} M_{\odot}$). We assess completeness and contamination of reconstructed halo catalogues, evaluate membership accuracy, and analyse the halo mass recovery rate of group finders. All three group finders achieve high completeness ($>80\%$) at group and cluster scales, confirming optical selection's suitability for dense regions. Contamination at low masses ($M_{200}<10^{13} M_{\odot}$) arises from interlopers and fragmentation. Membership is at least 70\% accurate above the group mass scale, but inaccuracies bias halo mass estimates using galaxy velocity dispersion. Alternative proxies, like total stellar luminosity or mass, yield more accurate halo masses. The cumulative luminosity function of galaxy members matches predictions, showing the group finders' accuracy in identifying galaxy populations. These results confirm the reliability and completeness of spectroscopic catalogues produced by state-of-the-art group finders. This supports studies requiring large spectroscopic samples of galaxy groups and clusters, as well as investigations into galaxy evolution across diverse environments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.16455v1-abstract-full').style.display = 'none'; document.getElementById('2411.16455v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">submitted to A&A, 17 pages, 9 figures. Abstract reduced for ArXiv submission</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 694, A207 (2025) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.12719">arXiv:2404.12719</a> <span> [<a href="https://arxiv.org/pdf/2404.12719">pdf</a>, <a href="https://arxiv.org/format/2404.12719">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/10.1051/0004-6361/202450442">10.1051/0004-6361/202450442 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Detecting Galaxy Groups and AGNs populating the local Universe in the eROSITA era </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Marini%2C+I">I. Marini</a>, <a href="/search/?searchtype=author&query=Popesso%2C+P">P. Popesso</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">G. Lamer</a>, <a href="/search/?searchtype=author&query=Dolag%2C+K">K. Dolag</a>, <a href="/search/?searchtype=author&query=Biffi%2C+V">V. Biffi</a>, <a href="/search/?searchtype=author&query=Vladutescu-Zopp%2C+S">S. Vladutescu-Zopp</a>, <a href="/search/?searchtype=author&query=Dev%2C+A">A. Dev</a>, <a href="/search/?searchtype=author&query=Toptun%2C+V">V. Toptun</a>, <a href="/search/?searchtype=author&query=Bulbul%2C+E">E. Bulbul</a>, <a href="/search/?searchtype=author&query=Comparat%2C+J">J. Comparat</a>, <a href="/search/?searchtype=author&query=Malavasi%2C+N">N. Malavasi</a>, <a href="/search/?searchtype=author&query=Merloni%2C+A">A. Merloni</a>, <a href="/search/?searchtype=author&query=Mroczkowski%2C+T">T. Mroczkowski</a>, <a href="/search/?searchtype=author&query=Ponti%2C+G">G. Ponti</a>, <a href="/search/?searchtype=author&query=Seppi%2C+R">R. Seppi</a>, <a href="/search/?searchtype=author&query=Shreeram%2C+S">S. Shreeram</a>, <a href="/search/?searchtype=author&query=Zhang%2C+Y">Y. Zhang</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.12719v1-abstract-short" style="display: inline;"> The eROSITA will deliver an unprecedented volume of X-ray survey observations, 20-30 times more sensitive than ROSAT in the soft band (0.5-2 keV) and for the first time imaging in the hard band (2-10 keV) including galaxy clusters and groups along with obscured and unobscured AGNs. This calls for a powerful theoretical effort to control the systematics and biases that may affect the data analysis.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.12719v1-abstract-full').style.display = 'inline'; document.getElementById('2404.12719v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.12719v1-abstract-full" style="display: none;"> The eROSITA will deliver an unprecedented volume of X-ray survey observations, 20-30 times more sensitive than ROSAT in the soft band (0.5-2 keV) and for the first time imaging in the hard band (2-10 keV) including galaxy clusters and groups along with obscured and unobscured AGNs. This calls for a powerful theoretical effort to control the systematics and biases that may affect the data analysis. We investigate the detection technique and selection effects in the galaxy group and AGN populations of a mock eROSITA survey at the depth of eRASS:4. We create a $30\times 30$ deg$^{2}$ mock observation based on the cosmological hydrodynamical simulation Magneticum Pathfinder within z=0-0.2. We combine a physical background extracted from the real eFEDS background analysis with realistic simulations of X-ray emission for the hot gas, AGNs and X-ray binaries. We apply a detection procedure equivalent to the reduction done on eRASS data and evaluate the completeness and contamination to reconstruct the luminosity functions of the extended and point sources in the catalogue. We assess the completeness of extended detections as a function of the input X-ray flux and halo. We achieve full recovery of the brightest (most massive) clusters and AGNs. However, a significant fraction of galaxy groups remains undetected. Examining the gas properties between the detected and undetected galaxy groups at fixed halo mass, we observe that the detected population exhibits, on average, higher X-ray brightness compared to the undetected ones. Moreover, we find that X-ray luminosity primarily correlates with the hot gas fraction, rather than temperature or metallicity. Our simulation suggests the presence of a systematic selection effect in current surveys, resulting in X-ray survey catalogues predominantly composed of the lowest-entropy, gas-richest, and highest surface brightness halos on galaxy group scales. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.12719v1-abstract-full').style.display = 'none'; document.getElementById('2404.12719v1-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 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">18 pages, 14 figures, submitted to 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 689, A7 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.08458">arXiv:2402.08458</a> <span> [<a href="https://arxiv.org/pdf/2402.08458">pdf</a>, <a href="https://arxiv.org/format/2402.08458">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202348852">10.1051/0004-6361/202348852 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The SRG/eROSITA all-sky survey: Cosmology constraints from cluster abundances in the western Galactic hemisphere </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Ghirardini%2C+V">V. Ghirardini</a>, <a href="/search/?searchtype=author&query=Bulbul%2C+E">E. Bulbul</a>, <a href="/search/?searchtype=author&query=Artis%2C+E">E. Artis</a>, <a href="/search/?searchtype=author&query=Clerc%2C+N">N. Clerc</a>, <a href="/search/?searchtype=author&query=Garrel%2C+C">C. Garrel</a>, <a href="/search/?searchtype=author&query=Grandis%2C+S">S. Grandis</a>, <a href="/search/?searchtype=author&query=Kluge%2C+M">M. Kluge</a>, <a href="/search/?searchtype=author&query=Liu%2C+A">A. Liu</a>, <a href="/search/?searchtype=author&query=Bahar%2C+Y+E">Y. E. Bahar</a>, <a href="/search/?searchtype=author&query=Balzer%2C+F">F. Balzer</a>, <a href="/search/?searchtype=author&query=Chiu%2C+I">I. Chiu</a>, <a href="/search/?searchtype=author&query=Comparat%2C+J">J. Comparat</a>, <a href="/search/?searchtype=author&query=Gruen%2C+D">D. Gruen</a>, <a href="/search/?searchtype=author&query=Kleinebreil%2C+F">F. Kleinebreil</a>, <a href="/search/?searchtype=author&query=Krippendorf%2C+S">S. Krippendorf</a>, <a href="/search/?searchtype=author&query=Merloni%2C+A">A. Merloni</a>, <a href="/search/?searchtype=author&query=Nandra%2C+K">K. Nandra</a>, <a href="/search/?searchtype=author&query=Okabe%2C+N">N. Okabe</a>, <a href="/search/?searchtype=author&query=Pacaud%2C+F">F. Pacaud</a>, <a href="/search/?searchtype=author&query=Predehl%2C+P">P. Predehl</a>, <a href="/search/?searchtype=author&query=Ramos-Ceja%2C+M+E">M. E. Ramos-Ceja</a>, <a href="/search/?searchtype=author&query=Reiprich%2C+T+H">T. H. Reiprich</a>, <a href="/search/?searchtype=author&query=Sanders%2C+J+S">J. S. Sanders</a>, <a href="/search/?searchtype=author&query=Schrabback%2C+T">T. Schrabback</a>, <a href="/search/?searchtype=author&query=Seppi%2C+R">R. Seppi</a> , et al. (24 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="2402.08458v2-abstract-short" style="display: inline;"> The cluster mass function traces the growth of linear density perturbations and provides valuable insights into the growth of structures, the nature of dark matter, and the cosmological parameters governing the Universe. The primary science goal of eROSITA, on board the {\it Spectrum Roentgen Gamma (SRG)} mission, launched in 2019, is to constrain cosmology through the evolution of cluster mass fu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.08458v2-abstract-full').style.display = 'inline'; document.getElementById('2402.08458v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.08458v2-abstract-full" style="display: none;"> The cluster mass function traces the growth of linear density perturbations and provides valuable insights into the growth of structures, the nature of dark matter, and the cosmological parameters governing the Universe. The primary science goal of eROSITA, on board the {\it Spectrum Roentgen Gamma (SRG)} mission, launched in 2019, is to constrain cosmology through the evolution of cluster mass function. In this paper, we present the cosmological constraints obtained from 5259 clusters of galaxies detected over an area of 12791~deg$^2$ in the Western Galactic Hemisphere of the eROSITA's first All-Sky Survey (eRASS1). The common footprint region between the eROSITA Survey and DES, KiDS, and HSC surveys is used for calibration of the scaling between X-ray count rate and their total mass through measurements of their weak gravitational lensing signal. eRASS1 cluster abundances constrain the $螞$CDM parameters, which are the energy density of the total matter to $惟_{\mathrm{m}}=0.29^{+0.01}_{-0.02}$, and the normalization of the density fluctuations to $蟽_8=0.88\pm0.02$ and their combination yields $S_8=蟽_8 (惟_\mathrm{m} / 0.3)^{0.5}=0.86\pm0.01$, consistent and at a similar precision with the state-of-the-art CMB measurements. eRASS1 cosmological experiment places a most stringent upper limit on the summed masses of left-handed light neutrinos to $\sum m_谓< 0.22\mathrm{~eV}$ (95\% confidence interval). Combining eRASS1 cluster abundance measurements with CMB and ground-based neutrino oscillation experiments, we measure the summed neutrino masses to be $\sum m_谓=0.08_{-0.02}^{+0.03}\mathrm{~eV}$ or $\sum m_谓=0.12_{-0.01}^{+0.03}\mathrm{~eV}$ depending on the mass hierarchy scenario for neutrino eigenstates. eRASS1 cluster abundances significantly improve the constraints on the dark energy equation of state parameter to $w=-1.12\pm0.12$. (ABRIDGED) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.08458v2-abstract-full').style.display = 'none'; document.getElementById('2402.08458v2-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 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">41 pages, 22 figures, Accepted for publication 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 689, A298 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.08454">arXiv:2402.08454</a> <span> [<a href="https://arxiv.org/pdf/2402.08454">pdf</a>, <a href="https://arxiv.org/format/2402.08454">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The SRG/eROSITA All-Sky Survey: First catalog of superclusters in the western Galactic hemisphere </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Liu%2C+A">A. Liu</a>, <a href="/search/?searchtype=author&query=Bulbul%2C+E">E. Bulbul</a>, <a href="/search/?searchtype=author&query=Kluge%2C+M">M. Kluge</a>, <a href="/search/?searchtype=author&query=Ghirardini%2C+V">V. Ghirardini</a>, <a href="/search/?searchtype=author&query=Zhang%2C+X">X. Zhang</a>, <a href="/search/?searchtype=author&query=Sanders%2C+J+S">J. S. Sanders</a>, <a href="/search/?searchtype=author&query=Artis%2C+E">E. Artis</a>, <a href="/search/?searchtype=author&query=Bahar%2C+Y+E">Y. E. Bahar</a>, <a href="/search/?searchtype=author&query=Balzer%2C+F">F. Balzer</a>, <a href="/search/?searchtype=author&query=Brueggen%2C+M">M. Brueggen</a>, <a href="/search/?searchtype=author&query=Clerc%2C+N">N. Clerc</a>, <a href="/search/?searchtype=author&query=Comparat%2C+J">J. Comparat</a>, <a href="/search/?searchtype=author&query=Garrel%2C+C">C. Garrel</a>, <a href="/search/?searchtype=author&query=Gatuzz%2C+E">E. Gatuzz</a>, <a href="/search/?searchtype=author&query=Grandis%2C+S">S. Grandis</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">G. Lamer</a>, <a href="/search/?searchtype=author&query=Merloni%2C+A">A. Merloni</a>, <a href="/search/?searchtype=author&query=Migkas%2C+K">K. Migkas</a>, <a href="/search/?searchtype=author&query=Nandra%2C+K">K. Nandra</a>, <a href="/search/?searchtype=author&query=Predehl%2C+P">P. Predehl</a>, <a href="/search/?searchtype=author&query=Ramos-Ceja%2C+M+E">M. E. Ramos-Ceja</a>, <a href="/search/?searchtype=author&query=Reiprich%2C+T+H">T. H. Reiprich</a>, <a href="/search/?searchtype=author&query=Seppi%2C+R">R. Seppi</a>, <a href="/search/?searchtype=author&query=Zelmer%2C+S">S. Zelmer</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="2402.08454v1-abstract-short" style="display: inline;"> Superclusters of galaxies mark the large-scale overdense regions in the Universe. Superclusters provide an ideal environment to study structure formation and to search for the emission of the intergalactic medium such as cosmic filaments and WHIM. In this work, we present the largest-to-date catalog of X-ray-selected superclusters identified in the first SRG/eROSITA All-Sky Survey (eRASS1). By app… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.08454v1-abstract-full').style.display = 'inline'; document.getElementById('2402.08454v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.08454v1-abstract-full" style="display: none;"> Superclusters of galaxies mark the large-scale overdense regions in the Universe. Superclusters provide an ideal environment to study structure formation and to search for the emission of the intergalactic medium such as cosmic filaments and WHIM. In this work, we present the largest-to-date catalog of X-ray-selected superclusters identified in the first SRG/eROSITA All-Sky Survey (eRASS1). By applying the Friends-of-Friends method on the galaxy clusters detected in eRASS1, we identified 1338 supercluster systems in the western Galactic hemisphere up to redshift 0.8, including 818 cluster pairs and 520 rich superclusters with $\ge 3$ members. The most massive and richest supercluster system is the Shapley supercluster at redshift 0.05 with 45 members and a total mass of $2.58\pm0.51 \times10^{16} M_{\odot}$. The most extensive system has a projected length of 127~Mpc. The sizes of the superclusters we identified in this work are comparable to the structures found with galaxy survey data. We also found a good association between the eRASS1 superclusters and the large-scale structures formed by optical galaxies. 3948 clusters, corresponding to $45\%$ of the cluster sample, were identified as supercluster members. The reliability of each supercluster was estimated by considering the uncertainties in cluster redshifts and peculiar velocities. 63\% of the systems have a reliability larger than 0.7. The eRASS1 supercluster catalog provided in this work represents the most extensive sample of superclusters selected in the X-ray band in terms of the unprecedented sample volume, sky coverage, redshift range, the availability of X-ray properties, and the well-understood selection function of the parent cluster sample, which enables direct comparisons with numerical simulations. This legacy catalog will greatly advance our understanding of superclusters and the cosmic large-scale structure. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.08454v1-abstract-full').style.display = 'none'; document.getElementById('2402.08454v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">A&A 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/2402.08453">arXiv:2402.08453</a> <span> [<a href="https://arxiv.org/pdf/2402.08453">pdf</a>, <a href="https://arxiv.org/format/2402.08453">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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</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/10.1051/0004-6361/202349031">10.1051/0004-6361/202349031 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The SRG/eROSITA All-Sky Survey. Optical identification and properties of galaxy clusters and groups in the western galactic hemisphere </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Kluge%2C+M">M. Kluge</a>, <a href="/search/?searchtype=author&query=Comparat%2C+J">J. Comparat</a>, <a href="/search/?searchtype=author&query=Liu%2C+A">A. Liu</a>, <a href="/search/?searchtype=author&query=Balzer%2C+F">F. Balzer</a>, <a href="/search/?searchtype=author&query=Bulbul%2C+E">E. Bulbul</a>, <a href="/search/?searchtype=author&query=Chitham%2C+J+I">J. Ider Chitham</a>, <a href="/search/?searchtype=author&query=Ghirardini%2C+V">V. Ghirardini</a>, <a href="/search/?searchtype=author&query=Garrel%2C+C">C. Garrel</a>, <a href="/search/?searchtype=author&query=Bahar%2C+Y+E">Y. E. Bahar</a>, <a href="/search/?searchtype=author&query=Artis%2C+E">E. Artis</a>, <a href="/search/?searchtype=author&query=Bender%2C+R">R. Bender</a>, <a href="/search/?searchtype=author&query=Clerc%2C+N">N. Clerc</a>, <a href="/search/?searchtype=author&query=Dwelly%2C+T">T. Dwelly</a>, <a href="/search/?searchtype=author&query=Fabricius%2C+M+H">M. H. Fabricius</a>, <a href="/search/?searchtype=author&query=Grandis%2C+S">S. Grandis</a>, <a href="/search/?searchtype=author&query=Hern%C3%A1ndez-Lang%2C+D">D. Hern谩ndez-Lang</a>, <a href="/search/?searchtype=author&query=Hill%2C+G+J">G. J. Hill</a>, <a href="/search/?searchtype=author&query=Joshi%2C+J">J. Joshi</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">G. Lamer</a>, <a href="/search/?searchtype=author&query=Merloni%2C+A">A. Merloni</a>, <a href="/search/?searchtype=author&query=Nandra%2C+K">K. Nandra</a>, <a href="/search/?searchtype=author&query=Pacaud%2C+F">F. Pacaud</a>, <a href="/search/?searchtype=author&query=Predehl%2C+P">P. Predehl</a>, <a href="/search/?searchtype=author&query=Ramos-Ceja%2C+M+E">M. E. Ramos-Ceja</a>, <a href="/search/?searchtype=author&query=Reiprich%2C+T+H">T. H. Reiprich</a> , et al. (7 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="2402.08453v2-abstract-short" style="display: inline;"> The first SRG/eROSITA All-Sky Survey (eRASS1) provides the largest intracluster medium-selected galaxy cluster and group catalog covering the western galactic hemisphere. Compared to samples selected purely on X-ray extent, the sample purity can be enhanced by identifying cluster candidates using optical and near-infrared data from the DESI Legacy Imaging Surveys. Using the red-sequence-based clus… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.08453v2-abstract-full').style.display = 'inline'; document.getElementById('2402.08453v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.08453v2-abstract-full" style="display: none;"> The first SRG/eROSITA All-Sky Survey (eRASS1) provides the largest intracluster medium-selected galaxy cluster and group catalog covering the western galactic hemisphere. Compared to samples selected purely on X-ray extent, the sample purity can be enhanced by identifying cluster candidates using optical and near-infrared data from the DESI Legacy Imaging Surveys. Using the red-sequence-based cluster finder eROMaPPer, we measured individual photometric properties (redshift $z_位$, richness $位$, optical center, and BCG position) for 12,000 eRASS1 clusters over a sky area of 13,116 deg$^2$, augmented by 247 cases identified by matching the candidates with known clusters from the literature. The median redshift of the identified eRASS1 sample is $z=0.31$, with 10% of the clusters at $z>0.72$. The photometric redshifts have an accuracy of $未z/(1+z)<0.005$ for $0.05<z<0.9$. Spectroscopic cluster properties (redshift $z_{\rm spec}$ and velocity dispersion $蟽$) are measured a posteriori for a subsample of 3,210 and 1,499 eRASS1 clusters, respectively, using an extensive compilation of spectroscopic redshifts of galaxies from the literature. We infer that the primary eRASS1 sample has a purity of 86% and optical completeness >95% for $z>0.05$. For these and further quality assessments of the eRASS1 identified catalog, we applied our identification method to a collection of galaxy cluster catalogs in the literature, as well as blindly on the full Legacy Surveys covering 24,069 deg$^2$. Using a combination of these cluster samples, we investigated the velocity dispersion-richness relation, finding $\log(位)=2.401\times\log(蟽)-5.074$ with an intrinsic scatter of $0.10\pm0.01$ dex. Our main result is the identified eRASS1 cluster catalog with a high purity and a well-defined X-ray selection process, enabling precise cosmological analyses presented in companion papers. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.08453v2-abstract-full').style.display = 'none'; document.getElementById('2402.08453v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">36 pages, 23 figures, 6 tables. Accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 688, A210 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.08452">arXiv:2402.08452</a> <span> [<a href="https://arxiv.org/pdf/2402.08452">pdf</a>, <a href="https://arxiv.org/format/2402.08452">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> The SRG/eROSITA All-Sky Survey: The first catalog of galaxy clusters and groups in the Western Galactic Hemisphere </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Bulbul%2C+E">E. Bulbul</a>, <a href="/search/?searchtype=author&query=Liu%2C+A">A. Liu</a>, <a href="/search/?searchtype=author&query=Kluge%2C+M">M. Kluge</a>, <a href="/search/?searchtype=author&query=Zhang%2C+X">X. Zhang</a>, <a href="/search/?searchtype=author&query=Sanders%2C+J+S">J. S. Sanders</a>, <a href="/search/?searchtype=author&query=Bahar%2C+Y+E">Y. E. Bahar</a>, <a href="/search/?searchtype=author&query=Ghirardini%2C+V">V. Ghirardini</a>, <a href="/search/?searchtype=author&query=Artis%2C+E">E. Artis</a>, <a href="/search/?searchtype=author&query=Seppi%2C+R">R. Seppi</a>, <a href="/search/?searchtype=author&query=Garrel%2C+C">C. Garrel</a>, <a href="/search/?searchtype=author&query=Ramos-Ceja%2C+M+E">M. E. Ramos-Ceja</a>, <a href="/search/?searchtype=author&query=Comparat%2C+J">J. Comparat</a>, <a href="/search/?searchtype=author&query=Balzer%2C+F">F. Balzer</a>, <a href="/search/?searchtype=author&query=B%C3%B6ckmann%2C+K">K. B枚ckmann</a>, <a href="/search/?searchtype=author&query=Br%C3%BCggen%2C+M">M. Br眉ggen</a>, <a href="/search/?searchtype=author&query=Clerc%2C+N">N. Clerc</a>, <a href="/search/?searchtype=author&query=Dennerl%2C+K">K. Dennerl</a>, <a href="/search/?searchtype=author&query=Dolag%2C+K">K. Dolag</a>, <a href="/search/?searchtype=author&query=Freyberg%2C+M">M. Freyberg</a>, <a href="/search/?searchtype=author&query=Grandis%2C+S">S. Grandis</a>, <a href="/search/?searchtype=author&query=Gruen%2C+D">D. Gruen</a>, <a href="/search/?searchtype=author&query=Kleinebreil%2C+F">F. Kleinebreil</a>, <a href="/search/?searchtype=author&query=Krippendorf%2C+S">S. Krippendorf</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">G. Lamer</a>, <a href="/search/?searchtype=author&query=Merloni%2C+A">A. Merloni</a> , et al. (9 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="2402.08452v1-abstract-short" style="display: inline;"> Clusters of galaxies can be used as powerful probes to study astrophysical processes on large scales, test theories of the growth of structure, and constrain cosmological models. The driving science goal of the SRG/eROSITA All-Sky Survey (eRASS) is to assemble a large sample of X-ray-selected clusters with a well-defined selection function to determine the evolution of the mass function and, hence… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.08452v1-abstract-full').style.display = 'inline'; document.getElementById('2402.08452v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.08452v1-abstract-full" style="display: none;"> Clusters of galaxies can be used as powerful probes to study astrophysical processes on large scales, test theories of the growth of structure, and constrain cosmological models. The driving science goal of the SRG/eROSITA All-Sky Survey (eRASS) is to assemble a large sample of X-ray-selected clusters with a well-defined selection function to determine the evolution of the mass function and, hence, the cosmological parameters. We present here a catalog of 12247 optically confirmed galaxy groups and clusters detected in the 0.2-2.3 keV as extended X-ray sources in a 13,116deg$^2$ region in the western Galactic hemisphere of the sky, which eROSITA surveyed in its first six months of operation. The clusters in the sample span the redshift range $0.003<z<1.32$. The majority (68%) of these clusters, 8361 sources, represent new discoveries without known counterparts in the literature. The mass range of the sample covers three orders of magnitude from $5\times10^{12}M_{\rm sun}$ to $2\times10^{15}M_{\rm sun}$. We construct a sample for cosmology with a higher purity level (~95%) than the primary sample, comprising 5259 securely detected and confirmed clusters in the 12791deg$^{2}$ common footprint with the DESI Legacy Survey DR10. We characterize the X-ray properties of each cluster, including their flux, luminosity and temperature, the total mass, gas mass, gas mass fraction, and mass proxy $Y_{X}$. These are determined within two apertures, 300 kpc, and the overdensity radius $R_{500}$, and are calculated by applying a forward modeling approach with a rigorous X-ray background treatment, K-factor, and the Galactic absorption corrections. Population studies utilizing LogN-LogS, the number of clusters detected above a given flux limit, and the luminosity function show overall agreement with the previous X-ray surveys after accounting for the survey completeness and purity (ABRIDGED) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.08452v1-abstract-full').style.display = 'none'; document.getElementById('2402.08452v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">in press in A&A. 27 pages, 21 figures, 3 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/2401.17305">arXiv:2401.17305</a> <span> [<a href="https://arxiv.org/pdf/2401.17305">pdf</a>, <a href="https://arxiv.org/format/2401.17305">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> The eROSITA Upper Limits: Description and access to the data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Tub%C3%ADn-Arenas%2C+D">D. Tub铆n-Arenas</a>, <a href="/search/?searchtype=author&query=Krumpe%2C+M">M. Krumpe</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">G. Lamer</a>, <a href="/search/?searchtype=author&query=Haase%2C+J">J. Haase</a>, <a href="/search/?searchtype=author&query=Sanders%2C+J">J. Sanders</a>, <a href="/search/?searchtype=author&query=Brunner%2C+H">H. Brunner</a>, <a href="/search/?searchtype=author&query=Homan%2C+D">D. Homan</a>, <a href="/search/?searchtype=author&query=Schwope%2C+A">A. Schwope</a>, <a href="/search/?searchtype=author&query=Georgakakis%2C+A">A. Georgakakis</a>, <a href="/search/?searchtype=author&query=Poppenhaeger%2C+K">K. Poppenhaeger</a>, <a href="/search/?searchtype=author&query=Traulsen%2C+I">I. Traulsen</a>, <a href="/search/?searchtype=author&query=K%C3%B6nig%2C+O">O. K枚nig</a>, <a href="/search/?searchtype=author&query=Merloni%2C+A">A. Merloni</a>, <a href="/search/?searchtype=author&query=Gueguen%2C+A">A. Gueguen</a>, <a href="/search/?searchtype=author&query=Strong%2C+A">A. Strong</a>, <a href="/search/?searchtype=author&query=Liu%2C+Z">Z. Liu</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="2401.17305v1-abstract-short" style="display: inline;"> The soft X-ray instrument eROSITA on board the Spectrum-Roentgen-Gamma (SRG) observatory has successfully completed four of the eight planned all-sky surveys, detecting almost one million X-ray sources during the first survey (eRASS1). The catalog of this survey will be released as part of the first eROSITA data release (DR1). Based on X-ray aperture photometry, we provide flux upper limits for eR… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.17305v1-abstract-full').style.display = 'inline'; document.getElementById('2401.17305v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.17305v1-abstract-full" style="display: none;"> The soft X-ray instrument eROSITA on board the Spectrum-Roentgen-Gamma (SRG) observatory has successfully completed four of the eight planned all-sky surveys, detecting almost one million X-ray sources during the first survey (eRASS1). The catalog of this survey will be released as part of the first eROSITA data release (DR1). Based on X-ray aperture photometry, we provide flux upper limits for eRASS1 in several energy bands. We cover galactic longitudes between $180^{\circ}\lesssim l \lesssim 360^{\circ}$ (eROSITA-DE). These data are crucial for studying the X-ray properties of variable and transient objects, as well as non-detected sources in the eROSITA all-sky survey data. We performed aperture photometry on every pixel of the SRG/eROSITA standard pipeline data products for all available sky tiles in the single detection band ($0.2 - 2.3$ keV). Simultaneously, we performed the same analysis in the three-band detection at soft ($0.2-0.6$ keV), medium ($0.6-2.3$ keV), and hard ($2.3-5.0$ keV) energy bands. Based on the combination of products for the individual bands, we are also able to provide aperture photometry products and flux upper limits for the $0.2 - 5.0$ keV energy band. The upper limits were calculated based on a Bayesian approach that utilizes detected counts and background within the circular aperture. The final data products consist of tables with the aperture photometry products (detected counts, background counts, and exposure time), a close-neighbor flag, and the upper flux limit based on an absorbed power-law spectral model ($螕=2.0, \; N_{\rm H}=3\times10^{20}$ cm$^{-2}$). The upper limits are calculated using the one-sided $3蟽$ confidence interval (CL) of a normal distribution, representing CL = 99.87\%. The aperture photometry products allow for an easy computation of upper limits at any other confidence interval and spectral model. ... <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.17305v1-abstract-full').style.display = 'none'; document.getElementById('2401.17305v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">13 pages, 7 figures, accepted in A&A. Due to the limitation "The abstract field cannot be longer than 1,920 characters", the abstract appearing here has been truncated. See the PDF for the full abstract</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.17300">arXiv:2401.17300</a> <span> [<a href="https://arxiv.org/pdf/2401.17300">pdf</a>, <a href="https://arxiv.org/format/2401.17300">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1051/0004-6361/202449416">10.1051/0004-6361/202449416 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The eROSITA Final Equatorial Depth Survey (eFEDS): the hard X-ray selected sample </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Nandra%2C+K">K. Nandra</a>, <a href="/search/?searchtype=author&query=Waddell%2C+S+G+H">S. G. H. Waddell</a>, <a href="/search/?searchtype=author&query=Liu%2C+T">T. Liu</a>, <a href="/search/?searchtype=author&query=Buchner%2C+J">J. Buchner</a>, <a href="/search/?searchtype=author&query=Dwelly%2C+T">T. Dwelly</a>, <a href="/search/?searchtype=author&query=Salvato%2C+M">M. Salvato</a>, <a href="/search/?searchtype=author&query=Shen%2C+Y">Y. Shen</a>, <a href="/search/?searchtype=author&query=Wu%2C+Q">Q. Wu</a>, <a href="/search/?searchtype=author&query=Arcodia%2C+R">R. Arcodia</a>, <a href="/search/?searchtype=author&query=Boller%2C+T">Th. Boller</a>, <a href="/search/?searchtype=author&query=Brunner%2C+H">H. Brunner</a>, <a href="/search/?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/?searchtype=author&query=Collmar%2C+W">W. Collmar</a>, <a href="/search/?searchtype=author&query=Comparat%2C+J">J. Comparat</a>, <a href="/search/?searchtype=author&query=Georgakakis%2C+A">A. Georgakakis</a>, <a href="/search/?searchtype=author&query=Grau%2C+M">M. Grau</a>, <a href="/search/?searchtype=author&query=H%C3%A4mmerich%2C+S">S. H盲mmerich</a>, <a href="/search/?searchtype=author&query=Ibarra-Medel%2C+H">H. Ibarra-Medel</a>, <a href="/search/?searchtype=author&query=Igo%2C+Z">Z. Igo</a>, <a href="/search/?searchtype=author&query=Krumpe%2C+M">M. Krumpe</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">G. Lamer</a>, <a href="/search/?searchtype=author&query=Merloni%2C+A">A. Merloni</a>, <a href="/search/?searchtype=author&query=Musiimenta%2C+B">B. Musiimenta</a>, <a href="/search/?searchtype=author&query=Wolf%2C+J">J. Wolf</a>, <a href="/search/?searchtype=author&query=Assef%2C+R+J">R. J. Assef</a> , et al. (3 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.17300v1-abstract-short" style="display: inline;"> During its calibration and performance verification phase, the eROSITA instrument aboard the SRG satellite performed a uniform wide--area X-ray survey of approximately 140 deg$^{2}$ in a region of the sky known as the eROSITA Final Equatorial Depth Survey (eFEDS). The primary aim of eFEDS is to demonstrate the scientific performance to be expected at the end of the 8-pass eROSITA all sky survey. T… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.17300v1-abstract-full').style.display = 'inline'; document.getElementById('2401.17300v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.17300v1-abstract-full" style="display: none;"> During its calibration and performance verification phase, the eROSITA instrument aboard the SRG satellite performed a uniform wide--area X-ray survey of approximately 140 deg$^{2}$ in a region of the sky known as the eROSITA Final Equatorial Depth Survey (eFEDS). The primary aim of eFEDS is to demonstrate the scientific performance to be expected at the end of the 8-pass eROSITA all sky survey. This will provide the first focussed image of the whole sky in the hard X-ray ($>2$~keV) bandpass. The expected source population in this energy range is thus of great interest, particularly for AGN studies. We use the 2.3--5 keV selection presented by Brunner et al. (2022) to construct a sample of 246 point-like hard X-ray sources for further study and characterization. These are classified as either extragalactic ($\sim 90$~\%) or Galactic ($\sim 10$~\%), with the former consisting overwhelmingly of AGN and the latter active stars. We concentrate our further analysis on the extragalactic/AGN sample, describing their X-ray and multiwavelength properties and comparing them to the eFEDS main AGN sample selected in the softer 0.2-2.3 keV band. The eROSITA hard band selects a subsample of sources that is a factor $>10$ brighter than the eFEDS main sample. The AGN within the hard population reach up to $z=3.2$ but on the whole are relatively nearby, with median $z$=0.34 compared to $z$=0.94 for the main sample. The hard survey probes typical luminosities in the range $\log L_{\rm X} = 43-46$. X-ray spectral analysis shows significant intrinsic absorption (with $\log N_{\rm H}>21$) in $\sim 20$~\% of the sources, with a hard X-ray power law continuum with mean $<螕>=1.83\pm0.04$, typical of AGN, but slightly harder than the soft-selected eROSITA sample. (abridged) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.17300v1-abstract-full').style.display = 'none'; document.getElementById('2401.17300v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to A&A as part of eROSITA Data Release 1</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 693, A212 (2025) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.17274">arXiv:2401.17274</a> <span> [<a href="https://arxiv.org/pdf/2401.17274">pdf</a>, <a href="https://arxiv.org/format/2401.17274">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </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/10.1051/0004-6361/202347165">10.1051/0004-6361/202347165 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The SRG/eROSITA all-sky survey: First X-ray catalogues and data release of the western Galactic hemisphere </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Merloni%2C+A">A. Merloni</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">G. Lamer</a>, <a href="/search/?searchtype=author&query=Liu%2C+T">T. Liu</a>, <a href="/search/?searchtype=author&query=Ramos-Ceja%2C+M+E">M. E. Ramos-Ceja</a>, <a href="/search/?searchtype=author&query=Brunner%2C+H">H. Brunner</a>, <a href="/search/?searchtype=author&query=Bulbul%2C+E">E. Bulbul</a>, <a href="/search/?searchtype=author&query=Dennerl%2C+K">K. Dennerl</a>, <a href="/search/?searchtype=author&query=Doroshenko%2C+V">V. Doroshenko</a>, <a href="/search/?searchtype=author&query=Freyberg%2C+M+J">M. J. Freyberg</a>, <a href="/search/?searchtype=author&query=Friedrich%2C+S">S. Friedrich</a>, <a href="/search/?searchtype=author&query=Gatuzz%2C+E">E. Gatuzz</a>, <a href="/search/?searchtype=author&query=Georgakakis%2C+A">A. Georgakakis</a>, <a href="/search/?searchtype=author&query=Haberl%2C+F">F. Haberl</a>, <a href="/search/?searchtype=author&query=Igo%2C+Z">Z. Igo</a>, <a href="/search/?searchtype=author&query=Kreykenbohm%2C+I">I. Kreykenbohm</a>, <a href="/search/?searchtype=author&query=Liu%2C+A">A. Liu</a>, <a href="/search/?searchtype=author&query=Maitra%2C+C">C. Maitra</a>, <a href="/search/?searchtype=author&query=Malyali%2C+A">A. Malyali</a>, <a href="/search/?searchtype=author&query=Mayer%2C+M+G+F">M. G. F. Mayer</a>, <a href="/search/?searchtype=author&query=Nandra%2C+K">K. Nandra</a>, <a href="/search/?searchtype=author&query=Predehl%2C+P">P. Predehl</a>, <a href="/search/?searchtype=author&query=Robrade%2C+J">J. Robrade</a>, <a href="/search/?searchtype=author&query=Salvato%2C+M">M. Salvato</a>, <a href="/search/?searchtype=author&query=Sanders%2C+J+S">J. S. Sanders</a>, <a href="/search/?searchtype=author&query=Stewart%2C+I">I. Stewart</a> , et al. (120 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="2401.17274v1-abstract-short" style="display: inline;"> The eROSITA telescope array aboard the Spektrum Roentgen Gamma (SRG) satellite began surveying the sky in December 2019, with the aim of producing all-sky X-ray source lists and sky maps of an unprecedented depth. Here we present catalogues of both point-like and extended sources using the data acquired in the first six months of survey operations (eRASS1; completed June 2020) over the half sky wh… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.17274v1-abstract-full').style.display = 'inline'; document.getElementById('2401.17274v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.17274v1-abstract-full" style="display: none;"> The eROSITA telescope array aboard the Spektrum Roentgen Gamma (SRG) satellite began surveying the sky in December 2019, with the aim of producing all-sky X-ray source lists and sky maps of an unprecedented depth. Here we present catalogues of both point-like and extended sources using the data acquired in the first six months of survey operations (eRASS1; completed June 2020) over the half sky whose proprietary data rights lie with the German eROSITA Consortium. We describe the observation process, the data analysis pipelines, and the characteristics of the X-ray sources. With nearly 930000 entries detected in the most sensitive 0.2-2.3 keV energy range, the eRASS1 main catalogue presented here increases the number of known X-ray sources in the published literature by more than 60%, and provides a comprehensive inventory of all classes of X-ray celestial objects, covering a wide range of physical processes. A smaller catalogue of 5466 sources detected in the less sensitive but harder 2.3-5 keV band is the result of the first true imaging survey of the entire sky above 2 keV. We show that the number counts of X-ray sources in eRASS1 are consistent with those derived over narrower fields by past X-ray surveys of a similar depth, and we explore the number counts variation as a function of the location in the sky. Adopting a uniform all-sky flux limit (at 50% completeness) of F_{0.5-2 keV} > 5 \times 10^{-14}$ erg\,s$^{-1}$\,cm$^{-2}$, we estimate that the eROSITA all-sky survey resolves into individual sources about 20% of the cosmic X-ray background in the 1-2 keV range. The catalogues presented here form part of the first data release (DR1) of the SRG/eROSITA all-sky survey. Beyond the X-ray catalogues, DR1 contains all detected and calibrated event files, source products (light curves and spectra), and all-sky maps. Illustrative examples of these are provided. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.17274v1-abstract-full').style.display = 'none'; document.getElementById('2401.17274v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">39 pages, 23 figures. Accepted for publication in A&A. Accompanying eROSITA-DE Data Release 1</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A, vol. 682, A34 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.06745">arXiv:2312.06745</a> <span> [<a href="https://arxiv.org/pdf/2312.06745">pdf</a>, <a href="https://arxiv.org/format/2312.06745">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="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Broadband maps of eROSITA and their comparison with the ROSAT survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Zheng%2C+X">Xueying Zheng</a>, <a href="/search/?searchtype=author&query=Ponti%2C+G">Gabriele Ponti</a>, <a href="/search/?searchtype=author&query=Freyberg%2C+M">Michael Freyberg</a>, <a href="/search/?searchtype=author&query=Sanders%2C+J">Jeremy Sanders</a>, <a href="/search/?searchtype=author&query=Locatelli%2C+N">Nicola Locatelli</a>, <a href="/search/?searchtype=author&query=Merloni%2C+A">Andrea Merloni</a>, <a href="/search/?searchtype=author&query=Strong%2C+A">Andy Strong</a>, <a href="/search/?searchtype=author&query=Sasaki%2C+M">Manami Sasaki</a>, <a href="/search/?searchtype=author&query=Comparat%2C+J">Johan Comparat</a>, <a href="/search/?searchtype=author&query=Becker%2C+W">Werner Becker</a>, <a href="/search/?searchtype=author&query=Kerp%2C+J">Juergen Kerp</a>, <a href="/search/?searchtype=author&query=Maitra%2C+C">Chandreyee Maitra</a>, <a href="/search/?searchtype=author&query=Liu%2C+T">Teng Liu</a>, <a href="/search/?searchtype=author&query=Predehl%2C+P">Peter Predehl</a>, <a href="/search/?searchtype=author&query=Anastasopoulou%2C+K">Konstantina Anastasopoulou</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">Georg Lamer</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="2312.06745v1-abstract-short" style="display: inline;"> By June of 2020, the extended ROentgen Survey with an Imaging Telescope Array (eROSITA) on board the Spectrum Roentgen Gamma observatory had completed its first of the planned eight X-ray all-sky survey (eRASS1). The large effective area of the X-ray telescope makes it ideal for a survey of the faint X-ray diffuse emission over half of the sky with an unprecedented energy resolution and position a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.06745v1-abstract-full').style.display = 'inline'; document.getElementById('2312.06745v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.06745v1-abstract-full" style="display: none;"> By June of 2020, the extended ROentgen Survey with an Imaging Telescope Array (eROSITA) on board the Spectrum Roentgen Gamma observatory had completed its first of the planned eight X-ray all-sky survey (eRASS1). The large effective area of the X-ray telescope makes it ideal for a survey of the faint X-ray diffuse emission over half of the sky with an unprecedented energy resolution and position accuracy. In this work, we produce the X-ray diffuse emission maps of the eRASS1 data with a current calibration, covering the energy range from 0.2 to 8.0 keV. We validated these maps by comparison with X-ray background maps derived from the ROSAT All Sky Survey (RASS). We generated X-ray images with a pixel area of 9 arcmin$^2$ using the observations available to the German eROSITA consortium. The contribution of the particle background to the photons was subtracted from the final maps. We also subtracted all the point sources above a flux threshold dependent on the goal of the subtraction, exploiting the eRASS1 catalog that will soon be available. The accuracy of the eRASS1 maps is shown by a flux match to the RASS X-ray maps, obtained by converting the eROSITA rates into equivalent ROSAT count rates in the standard ROSAT energy bands R4, R5, R6, and R7, within 1.25$蟽$. We find small residual deviations in the R4, R5, and R6 bands, where eROSITA tends to observe lower flux than ROSAT (~11%), while a better agreement is achieved in the R7 band (~1%). The eRASS maps exhibit lower noise levels than RASS maps at the same resolution above 0.3 keV. We report the average surface brightness and total flux of different large sky regions as a reference. The detection of faint emission from diffuse hot gas in the Milky Way is corroborated by the consistency of the eRASS1 and RASS maps shown in this paper and by their comparable flux dynamic range. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.06745v1-abstract-full').style.display = 'none'; document.getElementById('2312.06745v1-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 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">A&A, in press. 27 pages; 26 figures; 3 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/2306.13808">arXiv:2306.13808</a> <span> [<a href="https://arxiv.org/pdf/2306.13808">pdf</a>, <a href="https://arxiv.org/format/2306.13808">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/stad1893">10.1093/mnras/stad1893 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Improving the selection of changing-look AGNs through multi-wavelength photometric variability </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=L%C3%B3pez-Navas%2C+E">E. L贸pez-Navas</a>, <a href="/search/?searchtype=author&query=S%C3%A1nchez-S%C3%A1ez%2C+P">P. S谩nchez-S谩ez</a>, <a href="/search/?searchtype=author&query=Ar%C3%A9valo%2C+P">P. Ar茅valo</a>, <a href="/search/?searchtype=author&query=Bernal%2C+S">S. Bernal</a>, <a href="/search/?searchtype=author&query=Graham%2C+M+J">M. J. Graham</a>, <a href="/search/?searchtype=author&query=Hern%C3%A1ndez-Garc%C3%ADa%2C+L">L. Hern谩ndez-Garc铆a</a>, <a href="/search/?searchtype=author&query=Homan%2C+D">D. Homan</a>, <a href="/search/?searchtype=author&query=Krumpe%2C+M">M. Krumpe</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">G. Lamer</a>, <a href="/search/?searchtype=author&query=Lira%2C+P">P. Lira</a>, <a href="/search/?searchtype=author&query=Mart%C3%ADnez-Aldama%2C+M+L">M. L. Mart铆nez-Aldama</a>, <a href="/search/?searchtype=author&query=Merloni%2C+A">A. Merloni</a>, <a href="/search/?searchtype=author&query=R%C3%ADos%2C+S">S. R铆os</a>, <a href="/search/?searchtype=author&query=Salvato%2C+M">M. Salvato</a>, <a href="/search/?searchtype=author&query=Stern%2C+D">D. Stern</a>, <a href="/search/?searchtype=author&query=Tub%C3%ADn-Arenas%2C+D">D. Tub铆n-Arenas</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="2306.13808v1-abstract-short" style="display: inline;"> We present second epoch optical spectra for 30 changing-look (CL) candidates found by searching for Type-1 optical variability in a sample of active galactic nuclei (AGNs) spectroscopically classified as Type 2. We use a random-forest-based light curve classifier and spectroscopic follow-up, confirming 50 per cent of candidates as turning-on CLs. In order to improve this selection method and to be… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.13808v1-abstract-full').style.display = 'inline'; document.getElementById('2306.13808v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.13808v1-abstract-full" style="display: none;"> We present second epoch optical spectra for 30 changing-look (CL) candidates found by searching for Type-1 optical variability in a sample of active galactic nuclei (AGNs) spectroscopically classified as Type 2. We use a random-forest-based light curve classifier and spectroscopic follow-up, confirming 50 per cent of candidates as turning-on CLs. In order to improve this selection method and to better understand the nature of the not-confirmed CL candidates, we perform a multi-wavelength variability analysis including optical, mid-infrared (MIR) and X-ray data, and compare the results from the confirmed and not-confirmed CLs identified in this work. We find that most of the not-confirmed CLs are consistent with weak Type 1s dominated by host-galaxy contributions, showing weaker optical and MIR variability. On the contrary, the confirmed CLs present stronger optical fluctuations and experience a long (from five to ten years) increase in their MIR fluxes and the colour W1-W2 over time. In the 0.2-2.3 keV band, at least four out of 11 CLs with available SRG/eROSITA detections have increased their flux in comparison with archival upper limits. These common features allow us to select the most promising CLs from our list of candidates, leading to nine sources with similar multi-wavelength photometric properties to our CL sample. The use of machine learning algorithms with optical and MIR light curves will be very useful to identify CLs in future large-scale surveys. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.13808v1-abstract-full').style.display = 'none'; document.getElementById('2306.13808v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 June, 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">Journal ref:</span> Monthly Notices of the Royal Astronomical Society, 2023; stad1893 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.02499">arXiv:2304.02499</a> <span> [<a href="https://arxiv.org/pdf/2304.02499">pdf</a>, <a href="https://arxiv.org/format/2304.02499">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="High Energy Astrophysical Phenomena">astro-ph.HE</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/10.1051/0004-6361/202346316">10.1051/0004-6361/202346316 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery of the lensed quasar eRASS1 J050129.5-073309 with $\textit{SRG}/$eROSITA and ${\it Gaia}$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Tub%C3%ADn-Arenas%2C+D">D. Tub铆n-Arenas</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">G. Lamer</a>, <a href="/search/?searchtype=author&query=Krumpe%2C+M">M. Krumpe</a>, <a href="/search/?searchtype=author&query=Urrutia%2C+T">T. Urrutia</a>, <a href="/search/?searchtype=author&query=Schwope%2C+A">A. Schwope</a>, <a href="/search/?searchtype=author&query=Brogan%2C+R">R. Brogan</a>, <a href="/search/?searchtype=author&query=Comparat%2C+J">J. Comparat</a>, <a href="/search/?searchtype=author&query=Salvato%2C+M">M. Salvato</a>, <a href="/search/?searchtype=author&query=Bulbul%2C+E">E. Bulbul</a>, <a href="/search/?searchtype=author&query=Garrel%2C+C">C. Garrel</a>, <a href="/search/?searchtype=author&query=Schramm%2C+M">M. Schramm</a>, <a href="/search/?searchtype=author&query=Liu%2C+T">T. Liu</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="2304.02499v2-abstract-short" style="display: inline;"> We report the discovery and spectroscopic identification of the bright doubly lensed quasar eRASS1 J050129.5-073309 at redshift $z=2.47$, selected from the first all-sky survey of the ${\it Spectrum\; Roentgen\; Gamma\; (SRG)}$ eROSITA telescope and the ${\it Gaia}$ EDR3 catalog. We systematically search for extragalactic sources with eROSITA X-ray positions having multiple ${\it Gaia}$ counterpar… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.02499v2-abstract-full').style.display = 'inline'; document.getElementById('2304.02499v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.02499v2-abstract-full" style="display: none;"> We report the discovery and spectroscopic identification of the bright doubly lensed quasar eRASS1 J050129.5-073309 at redshift $z=2.47$, selected from the first all-sky survey of the ${\it Spectrum\; Roentgen\; Gamma\; (SRG)}$ eROSITA telescope and the ${\it Gaia}$ EDR3 catalog. We systematically search for extragalactic sources with eROSITA X-ray positions having multiple ${\it Gaia}$ counterparts and have started spectroscopic follow-up of the most promising candidates using long-slit spectroscopy with NTT/EFOSC2 to confirm the lens nature. The two images are separated by $2.7''$ and their average ${\it Gaia}$ ${\it g}$-band magnitudes are 16.95 and 17.33. Legacy Survey DR10 imaging and image modeling reveal both the lensing galaxy and tentatively the lensed image of the quasar host galaxy. Archival optical light curves show evidence of a variability time delay with the fainter component lagging the brighter by about 100 days. The fainter image has also decreased its brightness by about 1 magnitude since 2019. This dimming was still obvious at the time of the spectroscopic observations and is probably caused by microlensing. The optical spectroscopic follow-up obtained from NTT/EFOSC2 and the evidence provided by the imaging and timing analysis allow us to confirm the lensed nature of eRASS1 J050129.5-073309. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.02499v2-abstract-full').style.display = 'none'; document.getElementById('2304.02499v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in 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 672, L9 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.13315">arXiv:2302.13315</a> <span> [<a href="https://arxiv.org/pdf/2302.13315">pdf</a>, <a href="https://arxiv.org/format/2302.13315">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</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/10.1051/0004-6361/202345966">10.1051/0004-6361/202345966 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Serendipitous discovery of the magnetic cataclysmic variable SRGE J075818-612027 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Ok%2C+S">Samet Ok</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">Georg Lamer</a>, <a href="/search/?searchtype=author&query=Schwope%2C+A">Axel Schwope</a>, <a href="/search/?searchtype=author&query=Buckley%2C+D+A+H">David A. H. Buckley</a>, <a href="/search/?searchtype=author&query=Brink%2C+J">Jaco Brink</a>, <a href="/search/?searchtype=author&query=Kurpas%2C+J">Jan Kurpas</a>, <a href="/search/?searchtype=author&query=Tub%C3%ADn%2C+D">Dus谩n Tub铆n</a>, <a href="/search/?searchtype=author&query=Traulsen%2C+I">Iris Traulsen</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="2302.13315v1-abstract-short" style="display: inline;"> We report the discovery of SRGE J075818-612027, a deep stream-eclipsing magnetic cataclysmic variable found serendipitously in SRG/eROSITA CalPV observations of the open cluster NGC~2516 as an unrelated X-ray source. An X-ray timing and spectral analysis of the eROSITA data is presented and supplemented by an analysis of TESS photometry and SALT spectroscopy. X-ray photometry reveals two pronounce… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.13315v1-abstract-full').style.display = 'inline'; document.getElementById('2302.13315v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.13315v1-abstract-full" style="display: none;"> We report the discovery of SRGE J075818-612027, a deep stream-eclipsing magnetic cataclysmic variable found serendipitously in SRG/eROSITA CalPV observations of the open cluster NGC~2516 as an unrelated X-ray source. An X-ray timing and spectral analysis of the eROSITA data is presented and supplemented by an analysis of TESS photometry and SALT spectroscopy. X-ray photometry reveals two pronounced dips repeating with a period of $106.144(1)$ min. The 14-month TESS data reveal the same unique period. A low-resolution identification spectrum obtained with SALT displays hydrogen Balmer emission lines on a fairly blue continuum. The spectrum and the stability of the photometric signal led to the classification of the new object as a polar-type cataclysmic variable. In this picture, the dips in the X-ray light curve are explained by absorption in the intervening accretion stream and by a self-eclipse of the main accretion region. The object displays large magnitude differences on long (months) timescales both at optical and X-ray wavelengths, being interpreted as high and low states and thus supporting the identification as a polar. The bright phase X-ray spectrum can be reflected with single temperature thermal emission with 9.7 keV and bolometric X-ray luminosity $L_{\rm X} \simeq 8\times 10^{32}$erg s$^{-1}$ at a distance of about 2.7 kpc. It lacks the pronounced soft X-ray emission component prominently found in ROSAT-discovered polars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.13315v1-abstract-full').style.display = 'none'; document.getElementById('2302.13315v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 February, 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">9 Pages, 10 figures, accepted to A&A, 24 Feb 2023</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 672, A188 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.06989">arXiv:2302.06989</a> <span> [<a href="https://arxiv.org/pdf/2302.06989">pdf</a>, <a href="https://arxiv.org/format/2302.06989">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </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/10.1051/0004-6361/202245078">10.1051/0004-6361/202245078 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery of the luminous X-ray ignition eRASSt J234402.9$-$352640; I. Tidal disruption event or a rapid increase in accretion in an active galactic nucleus? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Homan%2C+D">D. Homan</a>, <a href="/search/?searchtype=author&query=Krumpe%2C+M">M. Krumpe</a>, <a href="/search/?searchtype=author&query=Markowitz%2C+A">A. Markowitz</a>, <a href="/search/?searchtype=author&query=Saha%2C+T">T. Saha</a>, <a href="/search/?searchtype=author&query=Gokus%2C+A">A. Gokus</a>, <a href="/search/?searchtype=author&query=Partington%2C+E">E. Partington</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">G. Lamer</a>, <a href="/search/?searchtype=author&query=Malyali%2C+A">A. Malyali</a>, <a href="/search/?searchtype=author&query=Liu%2C+Z">Z. Liu</a>, <a href="/search/?searchtype=author&query=Rau%2C+A">A. Rau</a>, <a href="/search/?searchtype=author&query=Grotova%2C+I">I. Grotova</a>, <a href="/search/?searchtype=author&query=Cackett%2C+E+M">E. M. Cackett</a>, <a href="/search/?searchtype=author&query=Buckley%2C+D+A+H">D. A. H. Buckley</a>, <a href="/search/?searchtype=author&query=Ciroi%2C+S">S. Ciroi</a>, <a href="/search/?searchtype=author&query=Di+Mille%2C+F">F. Di Mille</a>, <a href="/search/?searchtype=author&query=Gendreau%2C+K">K. Gendreau</a>, <a href="/search/?searchtype=author&query=Gromadzki%2C+M">M. Gromadzki</a>, <a href="/search/?searchtype=author&query=Krishnan%2C+S">S. Krishnan</a>, <a href="/search/?searchtype=author&query=Schramm%2C+M">M. Schramm</a>, <a href="/search/?searchtype=author&query=Steiner%2C+J+F">J. F. Steiner</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2302.06989v1-abstract-short" style="display: inline;"> In November 2020, a new, bright object, eRASSt J234402.9$-$352640, was discovered in the second all-sky survey of SRG/eROSITA. The object brightened by a factor of at least 150 in 0.2--2.0 keV flux compared to an upper limit found six months previous, reaching an observed peak of $1.76_{-0.24}^{+0.03} \times 10^{-11}$ erg cm$^{-2}$ s$^{-1}$. The X-ray ignition is associated with a galaxy at… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.06989v1-abstract-full').style.display = 'inline'; document.getElementById('2302.06989v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.06989v1-abstract-full" style="display: none;"> In November 2020, a new, bright object, eRASSt J234402.9$-$352640, was discovered in the second all-sky survey of SRG/eROSITA. The object brightened by a factor of at least 150 in 0.2--2.0 keV flux compared to an upper limit found six months previous, reaching an observed peak of $1.76_{-0.24}^{+0.03} \times 10^{-11}$ erg cm$^{-2}$ s$^{-1}$. The X-ray ignition is associated with a galaxy at $z=0.10$, making the peak luminosity log$_{10}(L_{\rm 0.2-2keV}/[\textrm{erg s}^{-1}])$=$44.7\pm0.1$. Around the time of the rise in X-ray flux, the nucleus of the galaxy brightened by approximately 3 mag. in optical photometry, after correcting for the host. We present data from Swift, XMM-Newton, and NICER, which reveal a very soft spectrum as well as strong 0.2--2.0 keV flux variability on multiple timescales. Optical spectra taken in the weeks after the ignition event show a blue continuum with broad, asymmetric Balmer emission lines, and high-ionisation ([OIII]$位位$4959,5007) and low-ionisation ([NII]$位$6585, [SII]$位位$6716,6731) narrow emission lines. Following the peak in the optical light curve, the X-ray, UV, and optical photometry all show a rapid decline. The X-ray light curve shows a decrease in luminosity of $\sim$0.45 over 33 days and the UV shows a drop of $\sim$0.35. eRASSt J234402.9$-$352640 also shows a brightening in the mid-infrared, likely powered by a dust echo of the luminous ignition. We find no evidence in Fermi-LAT $纬$-ray data for jet-like emission. The event displays characteristics of a tidal disruption event (TDE) as well as of an active galactic nucleus (AGN), complicating its classification. Based on the softness of the X-ray spectrum, the presence of high-ionisation optical emission lines, and the likely infrared echo, we find that a TDE within a turned-off AGN best matches our observations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.06989v1-abstract-full').style.display = 'none'; document.getElementById('2302.06989v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 February, 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">25 pages, 17 figures, 9 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/2202.09430">arXiv:2202.09430</a> <span> [<a href="https://arxiv.org/pdf/2202.09430">pdf</a>, <a href="https://arxiv.org/format/2202.09430">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </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/10.1051/0004-6361/202243362">10.1051/0004-6361/202243362 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The eROSITA extragalactic CalPV serendipitous catalog </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Liu%2C+T">Teng Liu</a>, <a href="/search/?searchtype=author&query=Merloni%2C+A">Andrea Merloni</a>, <a href="/search/?searchtype=author&query=Wolf%2C+J">Julien Wolf</a>, <a href="/search/?searchtype=author&query=Salvato%2C+M">Mara Salvato</a>, <a href="/search/?searchtype=author&query=Reiprich%2C+T">Thomas Reiprich</a>, <a href="/search/?searchtype=author&query=Arcodia%2C+R">Riccardo Arcodia</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">Georg Lamer</a>, <a href="/search/?searchtype=author&query=Georgakakis%2C+A">Antonis Georgakakis</a>, <a href="/search/?searchtype=author&query=Dwelly%2C+T">Tom Dwelly</a>, <a href="/search/?searchtype=author&query=Sanders%2C+J">Jeremy Sanders</a>, <a href="/search/?searchtype=author&query=Buchner%2C+J">Johannes Buchner</a>, <a href="/search/?searchtype=author&query=Haberl%2C+F">Frank Haberl</a>, <a href="/search/?searchtype=author&query=Ramos-Ceja%2C+M">Miriam Ramos-Ceja</a>, <a href="/search/?searchtype=author&query=Wilms%2C+J">Joern Wilms</a>, <a href="/search/?searchtype=author&query=Nandra%2C+K">Kirpal Nandra</a>, <a href="/search/?searchtype=author&query=Brunner%2C+H">Hermann Brunner</a>, <a href="/search/?searchtype=author&query=Brusa%2C+M">Marcella Brusa</a>, <a href="/search/?searchtype=author&query=Schwope%2C+A">Axel Schwope</a>, <a href="/search/?searchtype=author&query=Robrade%2C+J">Jan Robrade</a>, <a href="/search/?searchtype=author&query=Freyberg%2C+M+J">Michael J. Freyberg</a>, <a href="/search/?searchtype=author&query=Boller%2C+T">Thomas Boller</a>, <a href="/search/?searchtype=author&query=Maitra%2C+C">Chandreyee Maitra</a>, <a href="/search/?searchtype=author&query=Veronica%2C+A">Angie Veronica</a>, <a href="/search/?searchtype=author&query=Malyali%2C+A">Adam Malyali</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="2202.09430v2-abstract-short" style="display: inline;"> The eROSITA X-ray telescope on board the Spectrum-Roentgen-Gamma (SRG) observatory performed calibration and performance verification (CalPV) observations between September 2019 and December 2019, ahead of the planned four-year all-sky surveys. Most of them were deep, pointing-mode observations. We present here the X-ray catalog detected from the set of extra-galactic CalPV observations released t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.09430v2-abstract-full').style.display = 'inline'; document.getElementById('2202.09430v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.09430v2-abstract-full" style="display: none;"> The eROSITA X-ray telescope on board the Spectrum-Roentgen-Gamma (SRG) observatory performed calibration and performance verification (CalPV) observations between September 2019 and December 2019, ahead of the planned four-year all-sky surveys. Most of them were deep, pointing-mode observations. We present here the X-ray catalog detected from the set of extra-galactic CalPV observations released to the public by the German eROSITA consortium, and the multiband counterparts of these X-ray sources. We developed a source detection method optimized for point-like X-ray sources by including extended X-ray emission in the background measurement. The multiband counterparts were identified using a Bayesian method from the CatWISE catalog. Combining 11 CalPV fields, we present a catalog containing 9515 X-ray sources, whose X-ray fluxes were measured through spectral fitting. CatWISE counterparts are presented for 77% of the sources. Significant variabilities are found in 99 of the sources, which are also presented with this paper. Most of these fields show similar number counts of point sources as typical extragalactic fields, and a few harbor particular stellar populations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.09430v2-abstract-full').style.display = 'none'; document.getElementById('2202.09430v2-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 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">to be published in A&A, 23 pages, 14 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 664, A126 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.14533">arXiv:2106.14533</a> <span> [<a href="https://arxiv.org/pdf/2106.14533">pdf</a>, <a href="https://arxiv.org/format/2106.14533">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202141105">10.1051/0004-6361/202141105 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Phase-resolved X-ray spectroscopy of PSR B0656+14 with SRG/eROSITA and XMM-Newton </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Schwope%2C+A">Axel Schwope</a>, <a href="/search/?searchtype=author&query=Pires%2C+A+M">Adriana M. Pires</a>, <a href="/search/?searchtype=author&query=Kurpas%2C+J">Jan Kurpas</a>, <a href="/search/?searchtype=author&query=Doroshenko%2C+V">Victor Doroshenko</a>, <a href="/search/?searchtype=author&query=Suleimanov%2C+V+F">Valery F. Suleimanov</a>, <a href="/search/?searchtype=author&query=Freyberg%2C+M">Michael Freyberg</a>, <a href="/search/?searchtype=author&query=Becker%2C+W">Werner Becker</a>, <a href="/search/?searchtype=author&query=Dennerl%2C+K">Konrad Dennerl</a>, <a href="/search/?searchtype=author&query=Haberl%2C+F">Frank Haberl</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">Georg Lamer</a>, <a href="/search/?searchtype=author&query=Maitra%2C+C">Chandreyee Maitra</a>, <a href="/search/?searchtype=author&query=Potekhin%2C+A+Y">Alexander Y. Potekhin</a>, <a href="/search/?searchtype=author&query=Ramos-Ceja%2C+M+E">Miriam E. Ramos-Ceja</a>, <a href="/search/?searchtype=author&query=Santangelo%2C+A">Andrea Santangelo</a>, <a href="/search/?searchtype=author&query=Traulsen%2C+I">Iris Traulsen</a>, <a href="/search/?searchtype=author&query=Werner%2C+K">Klaus Werner</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2106.14533v1-abstract-short" style="display: inline;"> (abridged version) We present a detailed spectroscopic and timing analysis of X-ray observations of the bright radio-to-gamma-ray emitting pulsar PSR B0656+14, which were obtained simultaneously with eROSITA and XMM-Newton during the Calibration and Performance Verification phase of the Spektrum-Roentgen-Gamma mission (SRG) for 100 ks. Using XMM-Newton and NICER we firstly established an X-ray eph… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.14533v1-abstract-full').style.display = 'inline'; document.getElementById('2106.14533v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.14533v1-abstract-full" style="display: none;"> (abridged version) We present a detailed spectroscopic and timing analysis of X-ray observations of the bright radio-to-gamma-ray emitting pulsar PSR B0656+14, which were obtained simultaneously with eROSITA and XMM-Newton during the Calibration and Performance Verification phase of the Spektrum-Roentgen-Gamma mission (SRG) for 100 ks. Using XMM-Newton and NICER we firstly established an X-ray ephemeris for the time interval 2015 to 2020, which connects all X-ray observations in this period without cycle count alias and phase shifts. The mean eROSITA spectrum clearly reveals an absorption feature originating from the star at 570 eV with a Gaussian sigma of about 70 eV, tentatively identified earlier in a long XMM-Newton observation (Arumugasamy et al. 2018). A second absorption feature, described here as an absorption edge, occurs at 260-265 eV. It could be of atmospheric or of instrumental origin. These absorption features are superposed on various emission components, phenomenologically described as the sum of hot (120 eV) and cold (65 eV) blackbody components, both of photospheric origin, and a power-law with photon index Gamma=2. The phase-resolved spectroscopy reveals that the Gaussian absorption line at 570 eV is clearly present throughout ~60% of the spin cycle. The visibility of the line strength coincides in phase with the maximum flux of the hot blackbody. We also present three families of model atmospheres: a magnetised atmosphere, a condensed surface, and a mixed model, which were applied to the mean observed spectrum and whose continuum fit the observed data well. The atmosphere model, however, predicts too short distances. For the mixed model, the Gaussian absorption may be interpreted as proton cyclotron absorption in a field as high as 10^14 G, which is significantly higher than that derived from the moderate observed spin-down. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.14533v1-abstract-full').style.display = 'none'; document.getElementById('2106.14533v1-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 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to A&A for the Special Issue: The Early Data Release of eROSITA and Mikhail Pavlinsky ART-XC on the SRG Mission. 21 pages, 13 figures, 13 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 661, A41 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.14528">arXiv:2106.14528</a> <span> [<a href="https://arxiv.org/pdf/2106.14528">pdf</a>, <a href="https://arxiv.org/format/2106.14528">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</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/10.1051/0004-6361/202141178">10.1051/0004-6361/202141178 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Establishing the X-ray Source Detection Strategy for eROSITA with Simulations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Liu%2C+T">Teng Liu</a>, <a href="/search/?searchtype=author&query=Merloni%2C+A">Andrea Merloni</a>, <a href="/search/?searchtype=author&query=Comparat%2C+J">Johan Comparat</a>, <a href="/search/?searchtype=author&query=Nandra%2C+K">Kirpal Nandra</a>, <a href="/search/?searchtype=author&query=Sanders%2C+J+S">Jeremy S. Sanders</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">Georg Lamer</a>, <a href="/search/?searchtype=author&query=Buchner%2C+J">Johannes Buchner</a>, <a href="/search/?searchtype=author&query=Dwelly%2C+T">Tom Dwelly</a>, <a href="/search/?searchtype=author&query=Freyberg%2C+M">Michael Freyberg</a>, <a href="/search/?searchtype=author&query=Malyali%2C+A">Adam Malyali</a>, <a href="/search/?searchtype=author&query=Georgakakis%2C+A">Antonis Georgakakis</a>, <a href="/search/?searchtype=author&query=Salvato%2C+M">Mara Salvato</a>, <a href="/search/?searchtype=author&query=Brunner%2C+H">Hermann Brunner</a>, <a href="/search/?searchtype=author&query=Brusa%2C+M">Marcella Brusa</a>, <a href="/search/?searchtype=author&query=Klein%2C+M">Matthias Klein</a>, <a href="/search/?searchtype=author&query=Ghirardini%2C+V">Vittorio Ghirardini</a>, <a href="/search/?searchtype=author&query=Clerc%2C+N">Nicolas Clerc</a>, <a href="/search/?searchtype=author&query=Pacaud%2C+F">Florian Pacaud</a>, <a href="/search/?searchtype=author&query=Bulbul%2C+E">Esra Bulbul</a>, <a href="/search/?searchtype=author&query=Liu%2C+A">Ang Liu</a>, <a href="/search/?searchtype=author&query=Schwope%2C+A">Axel Schwope</a>, <a href="/search/?searchtype=author&query=Robrade%2C+J">Jan Robrade</a>, <a href="/search/?searchtype=author&query=Wilms%2C+J">J枚rn Wilms</a>, <a href="/search/?searchtype=author&query=Dauser%2C+T">Thomas Dauser</a>, <a href="/search/?searchtype=author&query=Ramos-Ceja%2C+M+E">Miriam E. Ramos-Ceja</a> , et al. (3 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2106.14528v2-abstract-short" style="display: inline;"> The eROSITA X-ray telescope on board the Spectrum-Roentgen-Gamma (SRG) satellite has started to detect new X-ray sources over the full sky at an unprecedented rate. Understanding the performance and selection function of the source detection is important for the subsequent scientific analysis of the eROSITA catalogs. Through simulations, we test and optimize the eROSITA source detection procedures… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.14528v2-abstract-full').style.display = 'inline'; document.getElementById('2106.14528v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.14528v2-abstract-full" style="display: none;"> The eROSITA X-ray telescope on board the Spectrum-Roentgen-Gamma (SRG) satellite has started to detect new X-ray sources over the full sky at an unprecedented rate. Understanding the performance and selection function of the source detection is important for the subsequent scientific analysis of the eROSITA catalogs. Through simulations, we test and optimize the eROSITA source detection procedures, and we characterize the detected catalog quantitatively. Taking the eROSITA Final Equatorial-Depth Survey (eFEDS) as an example, we ran extensive photon-event simulations based on our best knowledge of the instrument characteristics, the background spectrum, and the population of astronomical X-ray sources. We introduce a method of analyzing source detection completeness, purity, and efficiency based on the origin of each photon. According to the source detection efficiency measured in the simulation, we chose a two-pronged strategy to build eROSITA X-ray catalogs, creating a main catalog using only the most sensitive band (0.2-2.3 keV) and an independent hard-band-selected catalog using multiband detection in a range up to 5 keV. Because our mock data are highly representative of the real eFEDS data, we used the mock catalogs to measure the completeness and purity of the eFEDS catalogs as a function of multiple parameters, such as detection likelihood, flux, and luminosity. These measurements provide a basis for choosing the eFEDS catalog selection thresholds. The mock catalogs (available with this paper) can be used to construct the selection function of active galactic nuclei and galaxy clusters. A direct comparison of the output and input mock catalogs also gives rise to a correction curve that converts the raw point-source flux distribution into the intrinsic number counts distribution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.14528v2-abstract-full').style.display = 'none'; document.getElementById('2106.14528v2-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted by A&A for the Special Issue: The Early Data Release of eROSITA and Mikhail Pavlinsky ART-XC on the SRG Mission</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 661, A27 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.14527">arXiv:2106.14527</a> <span> [<a href="https://arxiv.org/pdf/2106.14527">pdf</a>, <a href="https://arxiv.org/format/2106.14527">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="High Energy Astrophysical Phenomena">astro-ph.HE</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/10.1051/0004-6361/202141547">10.1051/0004-6361/202141547 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The eROSITA Final Equatorial-Depth Survey (eFEDS): A multiwavelength view of WISE mid-infrared galaxies/active galactic nuclei </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Toba%2C+Y">Yoshiki Toba</a>, <a href="/search/?searchtype=author&query=Liu%2C+T">Teng Liu</a>, <a href="/search/?searchtype=author&query=Urrutia%2C+T">Tanya Urrutia</a>, <a href="/search/?searchtype=author&query=Salvato%2C+M">Mara Salvato</a>, <a href="/search/?searchtype=author&query=Li%2C+J">Junyao Li</a>, <a href="/search/?searchtype=author&query=Ueda%2C+Y">Yoshihiro Ueda</a>, <a href="/search/?searchtype=author&query=Brusa%2C+M">Marcella Brusa</a>, <a href="/search/?searchtype=author&query=Yutani%2C+N">Naomichi Yutani</a>, <a href="/search/?searchtype=author&query=Wada%2C+K">Keiichi Wada</a>, <a href="/search/?searchtype=author&query=Nishizawa%2C+A+J">Atsushi J. Nishizawa</a>, <a href="/search/?searchtype=author&query=Buchner%2C+J">Johannes Buchner</a>, <a href="/search/?searchtype=author&query=Nagao%2C+T">Tohru Nagao</a>, <a href="/search/?searchtype=author&query=Merloni%2C+A">Andrea Merloni</a>, <a href="/search/?searchtype=author&query=Akiyama%2C+M">Masayuki Akiyama</a>, <a href="/search/?searchtype=author&query=Arcodia%2C+R">Riccardo Arcodia</a>, <a href="/search/?searchtype=author&query=Hsieh%2C+B">Bau-Ching Hsieh</a>, <a href="/search/?searchtype=author&query=Ichikawa%2C+K">Kohei Ichikawa</a>, <a href="/search/?searchtype=author&query=Imanishi%2C+M">Masatoshi Imanishi</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K+T">Kaiki T. Inoue</a>, <a href="/search/?searchtype=author&query=Kawaguchi%2C+T">Toshihiro Kawaguchi</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">Georg Lamer</a>, <a href="/search/?searchtype=author&query=Nandra%2C+K">Kirpal Nandra</a>, <a href="/search/?searchtype=author&query=Silverman%2C+J+D">John D. Silverman</a>, <a href="/search/?searchtype=author&query=Terashima%2C+Y">Yuichi Terashima</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2106.14527v2-abstract-short" style="display: inline;"> We investigate the physical properties--such as the stellar mass, SFR, IR luminosity, X-ray luminosity, and hydrogen column density--of MIR galaxies and AGN at $z < 4$ in the 140 deg$^2$ field observed by SRG/eROSITA through the eFEDS survey. By cross-matching the WISE 22 $渭$m (W4)-detected sample and the eFEDS X-ray point-source catalog, we find that 692 extragalactic objects are detected by eROS… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.14527v2-abstract-full').style.display = 'inline'; document.getElementById('2106.14527v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.14527v2-abstract-full" style="display: none;"> We investigate the physical properties--such as the stellar mass, SFR, IR luminosity, X-ray luminosity, and hydrogen column density--of MIR galaxies and AGN at $z < 4$ in the 140 deg$^2$ field observed by SRG/eROSITA through the eFEDS survey. By cross-matching the WISE 22 $渭$m (W4)-detected sample and the eFEDS X-ray point-source catalog, we find that 692 extragalactic objects are detected by eROSITA. We have compiled a multiwavelength dataset. We have also performed (i) an X-ray spectral analysis, (ii) SED fitting using X-CIGALE, (iii) 2D image-decomposition analysis using Subaru HSC images, and (iv) optical spectral fitting with QSFit to investigate the AGN and host-galaxy properties. For 7,088 WISE W4 objects that are undetected by eROSITA, we have performed an X-ray stacking analysis to examine the typical physical properties of these X-ray faint and/or probably obscured objects. We find that (i) 82% of the eFEDS-W4 sources are classified as X-ray AGN with $\log\,L_{\rm X} >$ 42 erg s$^{-1}$; (ii) 67% and 24% of the objects have $\log\,(L_{\rm IR}/L_{\odot}) > 12$ and 13, respectively; (iii) the relationship between $L_{\rm X}$ and the 6 $渭$m luminosity is consistent with that reported in previous works; and (iv) the relationship between the Eddington ratio and $N_{\rm H}$ for the eFEDS-W4 sample and a comparison with a model prediction from a galaxy-merger simulation indicates that approximately 5% of the eFEDS-W4 sources in our sample are likely to be in an AGN-feedback phase, in which strong radiation pressure from the AGN blows out the surrounding material from the nuclear region. Thanks to the wide area coverage of eFEDS, we have been able to constrain the ranges of the physical properties of the WISE W4 sample of AGNs at $z < 4$, providing a benchmark for forthcoming studies on a complete census of MIR galaxies selected from the full-depth eROSITA all-sky survey. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.14527v2-abstract-full').style.display = 'none'; document.getElementById('2106.14527v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 19 figures, and 3 tables, accepted to appear on A&A, Special Issue: The Early Data Release of eROSITA and Mikhail Pavlinsky ART-XC on the SRG Mission</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 661, A15 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.14526">arXiv:2106.14526</a> <span> [<a href="https://arxiv.org/pdf/2106.14526">pdf</a>, <a href="https://arxiv.org/format/2106.14526">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="High Energy Astrophysical Phenomena">astro-ph.HE</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/10.1051/0004-6361/202141641">10.1051/0004-6361/202141641 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The eROSITA Final Equatorial-Depth Survey (eFEDS): Presenting The Demographics of X-ray Emission From Normal Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Vulic%2C+N">N. Vulic</a>, <a href="/search/?searchtype=author&query=Hornschemeier%2C+A+E">A. E. Hornschemeier</a>, <a href="/search/?searchtype=author&query=Haberl%2C+F">F. Haberl</a>, <a href="/search/?searchtype=author&query=Basu-Zych%2C+A+R">A. R. Basu-Zych</a>, <a href="/search/?searchtype=author&query=Kyritsis%2C+E">E. Kyritsis</a>, <a href="/search/?searchtype=author&query=Zezas%2C+A">A. Zezas</a>, <a href="/search/?searchtype=author&query=Salvato%2C+M">M. Salvato</a>, <a href="/search/?searchtype=author&query=Ptak%2C+A">A. Ptak</a>, <a href="/search/?searchtype=author&query=Bogdan%2C+A">A. Bogdan</a>, <a href="/search/?searchtype=author&query=Kovlakas%2C+K">K. Kovlakas</a>, <a href="/search/?searchtype=author&query=Wilms%2C+J">J. Wilms</a>, <a href="/search/?searchtype=author&query=Sasaki%2C+M">M. Sasaki</a>, <a href="/search/?searchtype=author&query=Liu%2C+T">T. Liu</a>, <a href="/search/?searchtype=author&query=Merloni%2C+A">A. Merloni</a>, <a href="/search/?searchtype=author&query=Dwelly%2C+T">T. Dwelly</a>, <a href="/search/?searchtype=author&query=Brunner%2C+H">H. Brunner</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">G. Lamer</a>, <a href="/search/?searchtype=author&query=Maitra%2C+C">C. Maitra</a>, <a href="/search/?searchtype=author&query=Nandra%2C+K">K. Nandra</a>, <a href="/search/?searchtype=author&query=Santangelo%2C+A">A. Santangelo</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2106.14526v1-abstract-short" style="display: inline;"> The $\it{eROSITA}$ Final Equatorial Depth Survey (eFEDS), completed during the calibration and performance verification phase of the $\it{eROSITA}$ instrument on $\it{Spectrum\, Roentgen\, Gamma}$, delivers data at and beyond the final depth of the four-year $\it{eROSITA}$ all-sky survey (eRASS:8), $f_{0.5-2\,\text{ keV}}$ = $1.1\times10^{-14}$ erg s$^{-1}$ cm$^{2}$, over 140 deg$^{2}$. It provide… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.14526v1-abstract-full').style.display = 'inline'; document.getElementById('2106.14526v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.14526v1-abstract-full" style="display: none;"> The $\it{eROSITA}$ Final Equatorial Depth Survey (eFEDS), completed during the calibration and performance verification phase of the $\it{eROSITA}$ instrument on $\it{Spectrum\, Roentgen\, Gamma}$, delivers data at and beyond the final depth of the four-year $\it{eROSITA}$ all-sky survey (eRASS:8), $f_{0.5-2\,\text{ keV}}$ = $1.1\times10^{-14}$ erg s$^{-1}$ cm$^{2}$, over 140 deg$^{2}$. It provides the first view of normal galaxy X-ray emission from X-ray binaries (XRBs) and the hot interstellar medium at the full depth of eRASS:8. We use the Heraklion Extragalactic Catalogue (HECATE) of galaxies to correlate with eFEDS X-ray sources and identify 94 X-ray detected normal galaxies. We classify galaxies as star-forming, early-type, composite, and AGN using SDSS and 6dF optical spectroscopy. The eFEDS field harbours 37 normal galaxies: 36 late-type (star-forming) galaxies and 1 early-type galaxy. There are 1.9 times as many normal galaxies as predicted by scaling relations via SIXTE simulations, with an overabundance of late-type galaxies and a dearth of early-type galaxies. Dwarf galaxies with high specific star formation rate (SFR) have elevated L$_{\text{X}}$/SFR when compared with specific SFR and metallicity, indicating an increase in XRB emission due to low-metallicity. We expect that eRASS:8 will detect 12,500 normal galaxies, the majority of which will be star-forming, with the caveat that there are unclassified sources in eFEDS and galaxy catalogue incompleteness issues that could increase the actual number of detected galaxies over these current estimates. eFEDS observations detected a rare population of galaxies -- the metal-poor dwarf starbursts -- that do not follow known scaling relations. eRASS is expected to discover significant numbers of these high-redshift analogues, which are important for studying the heating of the intergalactic medium at high-redshift. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.14526v1-abstract-full').style.display = 'none'; document.getElementById('2106.14526v1-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 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 10 figures, 3 tables. Submitted to A&A for the Special Issue: The Early Data Release of eROSITA and Mikhail Pavlinsky ART-XC on the SRG Mission</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 661, A16 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.14522">arXiv:2106.14522</a> <span> [<a href="https://arxiv.org/pdf/2106.14522">pdf</a>, <a href="https://arxiv.org/format/2106.14522">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </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/10.1051/0004-6361/202141643">10.1051/0004-6361/202141643 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The eROSITA Final Equatorial-Depth Survey (eFEDS): The AGN Catalogue and its X-ray Spectral Properties </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Liu%2C+T">Teng Liu</a>, <a href="/search/?searchtype=author&query=Buchner%2C+J">Johannes Buchner</a>, <a href="/search/?searchtype=author&query=Nandra%2C+K">Kirpal Nandra</a>, <a href="/search/?searchtype=author&query=Merloni%2C+A">Andrea Merloni</a>, <a href="/search/?searchtype=author&query=Dwelly%2C+T">Tom Dwelly</a>, <a href="/search/?searchtype=author&query=Sanders%2C+J+S">Jeremy S. Sanders</a>, <a href="/search/?searchtype=author&query=Salvato%2C+M">Mara Salvato</a>, <a href="/search/?searchtype=author&query=Arcodia%2C+R">Riccardo Arcodia</a>, <a href="/search/?searchtype=author&query=Brusa%2C+M">Marcella Brusa</a>, <a href="/search/?searchtype=author&query=Wolf%2C+J">Julien Wolf</a>, <a href="/search/?searchtype=author&query=Georgakakis%2C+A">Antonis Georgakakis</a>, <a href="/search/?searchtype=author&query=Boller%2C+T">Thomas Boller</a>, <a href="/search/?searchtype=author&query=Krumpe%2C+M">Mirko Krumpe</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">Georg Lamer</a>, <a href="/search/?searchtype=author&query=Waddell%2C+S">Sophia Waddell</a>, <a href="/search/?searchtype=author&query=Urrutia%2C+T">Tanya Urrutia</a>, <a href="/search/?searchtype=author&query=Schwope%2C+A">Axel Schwope</a>, <a href="/search/?searchtype=author&query=Robrade%2C+J">Jan Robrade</a>, <a href="/search/?searchtype=author&query=Wilms%2C+J">J枚rn Wilms</a>, <a href="/search/?searchtype=author&query=Dauser%2C+T">Thomas Dauser</a>, <a href="/search/?searchtype=author&query=Comparat%2C+J">Johan Comparat</a>, <a href="/search/?searchtype=author&query=Toba%2C+Y">Yoshiki Toba</a>, <a href="/search/?searchtype=author&query=Ichikawa%2C+K">Kohei Ichikawa</a>, <a href="/search/?searchtype=author&query=Iwasawa%2C+K">Kazushi Iwasawa</a>, <a href="/search/?searchtype=author&query=Shen%2C+Y">Yue Shen</a> , et al. (1 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="2106.14522v1-abstract-short" style="display: inline;"> Context: After the successful launch of the Spectrum-Roentgen-Gamma (SRG) mission in July 2019, eROSITA, the soft X-ray instrument aboard SRG, performed scanning observations of a large contiguous field, namely the eROSITA Final Equatorial Depth Survey (eFEDS), ahead of the planned four-year all-sky survey. eFEDS yielded a large sample of X-ray sources with very rich multi-band photometric and spe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.14522v1-abstract-full').style.display = 'inline'; document.getElementById('2106.14522v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.14522v1-abstract-full" style="display: none;"> Context: After the successful launch of the Spectrum-Roentgen-Gamma (SRG) mission in July 2019, eROSITA, the soft X-ray instrument aboard SRG, performed scanning observations of a large contiguous field, namely the eROSITA Final Equatorial Depth Survey (eFEDS), ahead of the planned four-year all-sky survey. eFEDS yielded a large sample of X-ray sources with very rich multi-band photometric and spectroscopic coverage. Aims: We present here the eFEDS Active Galactic Nuclei (AGN) catalog and the eROSITA X-ray spectral properties of the eFEDS sources. Methods: Using a Bayesian method, we perform a systematic X-ray spectral analysis for all eFEDS sources. The appropriate model is chosen based on the source classification and the spectral quality, and, in the case of AGN, including the possibility of intrinsic (rest-frame) absorption and/or soft excess emission. Hierarchical Bayesian modeling (HBM) is used to estimate the spectral parameter distribution of the sample. Results: X-ray spectral properties are presented for all eFEDS X-ray sources. There are 21952 candidate AGN, which comprise 79% of the eFEDS sample. Despite a large number of faint sources with low photon counts, our spectral fitting provides meaningful measurements of fluxes, luminosities, and spectral shapes for a majority of the sources. This AGN catalog is dominated by X-ray unobscured sources, with an obscured (logNH>21.5) fraction of 10% derived by HBM. The power-law slope of the catalog can be described by a Gaussian distribution of 1.94+-0.22. Above a photon counts threshold of 500, nine out of 50 AGN have soft excess detected. For the sources with blue UV to optical color (type-I AGN), the X-ray emission is well correlated with the UV emission with the usual anti-correlation between the X-ray to UV spectral slope 伪_{OX} and the UV luminosity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.14522v1-abstract-full').style.display = 'none'; document.getElementById('2106.14522v1-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 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to A&A for the Special Issue: The Early Data Release of eROSITA and Mikhail Pavlinsky ART-XC on the SRG Mission 24 pages, 23 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 661, A5 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.14520">arXiv:2106.14520</a> <span> [<a href="https://arxiv.org/pdf/2106.14520">pdf</a>, <a href="https://arxiv.org/format/2106.14520">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </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/10.1051/0004-6361/202141631">10.1051/0004-6361/202141631 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The eROSITA Final Equatorial-Depth Survey (eFEDS): Identification and characterization of the counterparts to the point-like sources </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Salvato%2C+M">M. Salvato</a>, <a href="/search/?searchtype=author&query=Wolf%2C+J">J. Wolf</a>, <a href="/search/?searchtype=author&query=Dwelly%2C+T">T. Dwelly</a>, <a href="/search/?searchtype=author&query=Georgakakis%2C+A">A. Georgakakis</a>, <a href="/search/?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/?searchtype=author&query=Merloni%2C+A">A. Merloni</a>, <a href="/search/?searchtype=author&query=Liu%2C+T">T. Liu</a>, <a href="/search/?searchtype=author&query=Toba%2C+Y">Y. Toba</a>, <a href="/search/?searchtype=author&query=Nandra%2C+K">K. Nandra</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">G. Lamer</a>, <a href="/search/?searchtype=author&query=Buchner%2C+J">J. Buchner</a>, <a href="/search/?searchtype=author&query=Schneider%2C+C">C. Schneider</a>, <a href="/search/?searchtype=author&query=Freund%2C+S">S. Freund</a>, <a href="/search/?searchtype=author&query=Rau%2C+A">A. Rau</a>, <a href="/search/?searchtype=author&query=Schwope%2C+A">A. Schwope</a>, <a href="/search/?searchtype=author&query=Nishizawa%2C+A">A. Nishizawa</a>, <a href="/search/?searchtype=author&query=Klein%2C+M">M. Klein</a>, <a href="/search/?searchtype=author&query=Arcodia%2C+R">R. Arcodia</a>, <a href="/search/?searchtype=author&query=Comparat%2C+J">J. Comparat</a>, <a href="/search/?searchtype=author&query=Musiimenta%2C+B">B. Musiimenta</a>, <a href="/search/?searchtype=author&query=Nagao%2C+T">T. Nagao</a>, <a href="/search/?searchtype=author&query=Brunner%2C+H">H. Brunner</a>, <a href="/search/?searchtype=author&query=Malyali%2C+A">A. Malyali</a>, <a href="/search/?searchtype=author&query=Finoguenov%2C+A">A. Finoguenov</a>, <a href="/search/?searchtype=author&query=Anderson%2C+S">S. Anderson</a> , et al. (19 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="2106.14520v2-abstract-short" style="display: inline;"> In November 2019, eROSITA on board of SRG observatory started to map the entire sky in X-rays. After the 4-year survey program, it will reach flux limits about 25 times deeper than ROSAT. During the SRG Performance Verification phase, eROSITA observed a contiguous 140 deg$^2$ area of the sky down to the final depth of the eROSITA all-sky survey ("eROSITA Final Equatorial-Depth Survey": eFEDS), wit… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.14520v2-abstract-full').style.display = 'inline'; document.getElementById('2106.14520v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.14520v2-abstract-full" style="display: none;"> In November 2019, eROSITA on board of SRG observatory started to map the entire sky in X-rays. After the 4-year survey program, it will reach flux limits about 25 times deeper than ROSAT. During the SRG Performance Verification phase, eROSITA observed a contiguous 140 deg$^2$ area of the sky down to the final depth of the eROSITA all-sky survey ("eROSITA Final Equatorial-Depth Survey": eFEDS), with the goal of obtaining a census of the X-ray emitting populations (stars, compact objects, galaxies, clusters of galaxies, AGN) that will be discovered over the entire sky. This paper presents the identification of the counterparts to the point-sources detected in eFEDS in the Main and Hard samples described in Brunner et al 2021, and their multi-wavelength properties, including redshift. For the identification of the counterparts we combined the results from two independent methods (NWAY and ASTROMATCH), trained on the multi-wavelength properties of a sample of 23k XMM-Newton sources detected in the DESI Legacy Imaging Survey DR8. Then spectroscopic redshifts and photometry from ancillary surveys are collated for the computation of photometric redshifts. The eFEDS sources with a reliable counterparts are 24774/27369 (90.5\%) in the Main sample and 231/246 (93.9\%) in the Hard sample, including 2514 (3) sources for which a second counterpart is equally likely. [abridged] This paper is accompanying the eROSITA early data release of all the observations performed during the performance and verification phase. Together with the catalogs of primary and secondary counterparts to the Main and Hard samples of the eFEDS survey this paper releases their multi-wavelength properties and redshifts. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.14520v2-abstract-full').style.display = 'none'; document.getElementById('2106.14520v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted by A&A for the Special Issue: The Early Data Release of eROSITA and Mikhail Pavlinsky ART-XC on the SRG Mission. NOTE: Paper completely revised wrt the first version submitted to arXiv. Revised catalogs available via https://erosita.mpe.mpg.de/edr/eROSITAObservations/Catalogues/</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 661, A3 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.14518">arXiv:2106.14518</a> <span> [<a href="https://arxiv.org/pdf/2106.14518">pdf</a>, <a href="https://arxiv.org/format/2106.14518">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/10.1051/0004-6361/202141120">10.1051/0004-6361/202141120 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The eROSITA Final Equatorial-Depth Survey (eFEDS): Catalog of galaxy clusters and groups </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Liu%2C+A">A. Liu</a>, <a href="/search/?searchtype=author&query=Bulbul%2C+E">E. Bulbul</a>, <a href="/search/?searchtype=author&query=Ghirardini%2C+V">V. Ghirardini</a>, <a href="/search/?searchtype=author&query=Liu%2C+T">T. Liu</a>, <a href="/search/?searchtype=author&query=Klein%2C+M">M. Klein</a>, <a href="/search/?searchtype=author&query=Clerc%2C+N">N. Clerc</a>, <a href="/search/?searchtype=author&query=Oezsoy%2C+Y">Y. Oezsoy</a>, <a href="/search/?searchtype=author&query=Ramos-Ceja%2C+M+E">M. E. Ramos-Ceja</a>, <a href="/search/?searchtype=author&query=Pacaud%2C+F">F. Pacaud</a>, <a href="/search/?searchtype=author&query=Comparat%2C+J">J. Comparat</a>, <a href="/search/?searchtype=author&query=Okabe%2C+N">N. Okabe</a>, <a href="/search/?searchtype=author&query=Bahar%2C+Y+E">Y. E. Bahar</a>, <a href="/search/?searchtype=author&query=Biffi%2C+V">V. Biffi</a>, <a href="/search/?searchtype=author&query=Brunner%2C+H">H. Brunner</a>, <a href="/search/?searchtype=author&query=Brueggen%2C+M">M. Brueggen</a>, <a href="/search/?searchtype=author&query=Buchner%2C+J">J. Buchner</a>, <a href="/search/?searchtype=author&query=Chitham%2C+J+I">J. Ider Chitham</a>, <a href="/search/?searchtype=author&query=Chiu%2C+I">I. Chiu</a>, <a href="/search/?searchtype=author&query=Dolag%2C+K">K. Dolag</a>, <a href="/search/?searchtype=author&query=Gatuzz%2C+E">E. Gatuzz</a>, <a href="/search/?searchtype=author&query=Gonzalez%2C+J">J. Gonzalez</a>, <a href="/search/?searchtype=author&query=Hoang%2C+D+N">D. N. Hoang</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">G. Lamer</a>, <a href="/search/?searchtype=author&query=Merloni%2C+A">A. Merloni</a>, <a href="/search/?searchtype=author&query=Nandra%2C+K">K. Nandra</a> , et al. (9 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="2106.14518v2-abstract-short" style="display: inline;"> The eROSITA Final Equatorial-Depth Survey has been carried out during the PV phase of the SRG/eROSITA telescope and completed in November 2019. This survey is designed to provide the first eROSITA-selected sample of galaxy clusters and groups and to test the predictions for the all-sky survey in the context of cosmological studies with clusters. In the 140 deg$^2$ area covered by eFEDS, 542 candid… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.14518v2-abstract-full').style.display = 'inline'; document.getElementById('2106.14518v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.14518v2-abstract-full" style="display: none;"> The eROSITA Final Equatorial-Depth Survey has been carried out during the PV phase of the SRG/eROSITA telescope and completed in November 2019. This survey is designed to provide the first eROSITA-selected sample of galaxy clusters and groups and to test the predictions for the all-sky survey in the context of cosmological studies with clusters. In the 140 deg$^2$ area covered by eFEDS, 542 candidate clusters and groups are detected as extended X-ray sources, down to a flux of $\sim10^{-14} $erg/s/cm$^2$ in the soft band (0.5-2 keV) within 1'. In this work, we provide the catalog of candidate galaxy clusters and groups in eFEDS. We perform imaging and spectral analysis on the eFEDS clusters with eROSITA X-ray data, and study the properties of the sample. The clusters are distributed in the redshift range [0.01, 1.3], with the median redshift at 0.35. We obtain the ICM temperature measurement with $>2蟽$ c.l. for $\sim$1/5 (102/542) of the sample. The average temperature of these clusters is $\sim$2 keV. Radial profiles of flux, luminosity, electron density, and gas mass are measured from the precise modeling of the imaging data. The selection function, the purity and completeness of the catalog are examined and discussed in detail. The contamination fraction is $\sim1/5$ in this sample, dominated by misidentified point sources. The X-ray Luminosity Function of the clusters agrees well with the results obtained from other recent X-ray surveys. We also find 19 supercluster candidates in eFEDS, most of which are located at redshifts between 0.1 and 0.5. The eFEDS cluster and group catalog provides a benchmark proof-of-concept for the eROSITA All-Sky Survey extended source detection and characterization. We confirm the excellent performance of eROSITA for cluster science and expect no significant deviations from our pre-launch expectations for the final All-Sky Survey. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.14518v2-abstract-full').style.display = 'none'; document.getElementById('2106.14518v2-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, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to A&A for the Special Issue: The Early Data Release of eROSITA and Mikhail Pavlinsky ART-XC on the SRG Mission. 25 pages, 13 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 661, A2 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.14517">arXiv:2106.14517</a> <span> [<a href="https://arxiv.org/pdf/2106.14517">pdf</a>, <a href="https://arxiv.org/format/2106.14517">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1051/0004-6361/202141266">10.1051/0004-6361/202141266 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The eROSITA Final Equatorial Depth Survey (eFEDS): The X-ray catalog </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Brunner%2C+H">H. Brunner</a>, <a href="/search/?searchtype=author&query=Liu%2C+T">T. Liu</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">G. Lamer</a>, <a href="/search/?searchtype=author&query=Georgakakis%2C+A">A. Georgakakis</a>, <a href="/search/?searchtype=author&query=Merloni%2C+A">A. Merloni</a>, <a href="/search/?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/?searchtype=author&query=Bulbul%2C+E">E. Bulbul</a>, <a href="/search/?searchtype=author&query=Dennerl%2C+K">K. Dennerl</a>, <a href="/search/?searchtype=author&query=Friedrich%2C+S">S. Friedrich</a>, <a href="/search/?searchtype=author&query=Liu%2C+A">A. Liu</a>, <a href="/search/?searchtype=author&query=Maitra%2C+C">C. Maitra</a>, <a href="/search/?searchtype=author&query=Nandra%2C+K">K. Nandra</a>, <a href="/search/?searchtype=author&query=Ramos-Ceja%2C+M+E">M. E. Ramos-Ceja</a>, <a href="/search/?searchtype=author&query=Sanders%2C+J+S">J. S. Sanders</a>, <a href="/search/?searchtype=author&query=Stewart%2C+I+M">I. M. Stewart</a>, <a href="/search/?searchtype=author&query=Boller%2C+T">T. Boller</a>, <a href="/search/?searchtype=author&query=Buchner%2C+J">J. Buchner</a>, <a href="/search/?searchtype=author&query=Clerc%2C+N">N. Clerc</a>, <a href="/search/?searchtype=author&query=Comparat%2C+J">J. Comparat</a>, <a href="/search/?searchtype=author&query=Dwelly%2C+T">T. Dwelly</a>, <a href="/search/?searchtype=author&query=Eckert%2C+D">D. Eckert</a>, <a href="/search/?searchtype=author&query=Finoguenov%2C+A">A. Finoguenov</a>, <a href="/search/?searchtype=author&query=Freyberg%2C+M">M. Freyberg</a>, <a href="/search/?searchtype=author&query=Ghirardini%2C+V">V. Ghirardini</a>, <a href="/search/?searchtype=author&query=Gueguen%2C+A">A. Gueguen</a> , et al. (13 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="2106.14517v2-abstract-short" style="display: inline;"> Context. The eROSITA X-ray telescope on board the Spectrum-Roentgen-Gamma (SRG) observatory combines a large field of view and collecting area in the energy range $\sim$0.2 to $\sim$8.0 keV with the capability to perform uniform scanning observations of large sky areas. Aims. SRG/eROSITA performed scanning observations of the $\sim$140 square degrees eROSITA Final Equatorial Depth Survey (eFEDS)… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.14517v2-abstract-full').style.display = 'inline'; document.getElementById('2106.14517v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.14517v2-abstract-full" style="display: none;"> Context. The eROSITA X-ray telescope on board the Spectrum-Roentgen-Gamma (SRG) observatory combines a large field of view and collecting area in the energy range $\sim$0.2 to $\sim$8.0 keV with the capability to perform uniform scanning observations of large sky areas. Aims. SRG/eROSITA performed scanning observations of the $\sim$140 square degrees eROSITA Final Equatorial Depth Survey (eFEDS) field as part of its performance verification phase. The observing time was chosen to slightly exceed the depth of equatorial fields after the completion of the eROSITA all-sky survey. We present a catalog of detected X-ray sources in the eFEDS field providing source positions and extent information, as well as fluxes in multiple energy bands and document a suite of tools and procedures developed for eROSITA data processing and analysis, validated and optimized by the eFEDS work. Methods. A multi-stage source detection procedure was optimized and calibrated by performing realistic simulations of the eROSITA eFEDS observations. We cross-matched the eROSITA eFEDS source catalog with previous XMM-ATLAS observations, confirming excellent agreement of the eROSITA and XMM-ATLAS source fluxes. Result. We present a primary catalog of 27910 X-ray sources, including 542 with significant spatial extent, detected in the 0.2-2.3 keV energy range with detection likelihoods $\ge 6$, corresponding to a (point source) flux limit of $\approx 6.5 \times 10^{-15}$ erg/cm$^2$/s in the 0.5-2.0 keV energy band (80% completeness). A supplementary catalog contains 4774 low-significance source candidates with detection likelihoods between 5 and 6. In addition, a hard band sample of 246 sources detected in the energy range 2.3-5.0 keV above a detection likelihood of 10 is provided. The dedicated data analysis software package, calibration database, and calibrated data products are described in an appendix. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.14517v2-abstract-full').style.display = 'none'; document.getElementById('2106.14517v2-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 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages, 15 figures, accepted, A&A Special Issue: The Early Data Release of eROSITA and Mikhail Pavlinsky ART-XC on the SRG Mission</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2104.13388">arXiv:2104.13388</a> <span> [<a href="https://arxiv.org/pdf/2104.13388">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1038/s41586-021-03394-6">10.1038/s41586-021-03394-6 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> X-ray Quasi-Periodic Eruptions from two previously quiescent galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Arcodia%2C+R">R. Arcodia</a>, <a href="/search/?searchtype=author&query=Merloni%2C+A">A. Merloni</a>, <a href="/search/?searchtype=author&query=Nandra%2C+K">K. Nandra</a>, <a href="/search/?searchtype=author&query=Buchner%2C+J">J. Buchner</a>, <a href="/search/?searchtype=author&query=Salvato%2C+M">M. Salvato</a>, <a href="/search/?searchtype=author&query=Pasham%2C+D">D. Pasham</a>, <a href="/search/?searchtype=author&query=Remillard%2C+R">R. Remillard</a>, <a href="/search/?searchtype=author&query=Comparat%2C+J">J. Comparat</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">G. Lamer</a>, <a href="/search/?searchtype=author&query=Ponti%2C+G">G. Ponti</a>, <a href="/search/?searchtype=author&query=Malyali%2C+A">A. Malyali</a>, <a href="/search/?searchtype=author&query=Wolf%2C+J">J. Wolf</a>, <a href="/search/?searchtype=author&query=Arzoumanian%2C+Z">Z. Arzoumanian</a>, <a href="/search/?searchtype=author&query=Bogensberger%2C+D">D. Bogensberger</a>, <a href="/search/?searchtype=author&query=Buckley%2C+D+A+H">D. A. H. Buckley</a>, <a href="/search/?searchtype=author&query=Gendreau%2C+K">K. Gendreau</a>, <a href="/search/?searchtype=author&query=Gromadzki%2C+M">M. Gromadzki</a>, <a href="/search/?searchtype=author&query=Kara%2C+E">E. Kara</a>, <a href="/search/?searchtype=author&query=Krumpe%2C+M">M. Krumpe</a>, <a href="/search/?searchtype=author&query=Markwardt%2C+C">C. Markwardt</a>, <a href="/search/?searchtype=author&query=Ramos-Ceja%2C+M+E">M. E. Ramos-Ceja</a>, <a href="/search/?searchtype=author&query=Rau%2C+A">A. Rau</a>, <a href="/search/?searchtype=author&query=Schramm%2C+M">M. Schramm</a>, <a href="/search/?searchtype=author&query=Schwope%2C+A">A. Schwope</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="2104.13388v1-abstract-short" style="display: inline;"> Quasi-Periodic Eruptions (QPEs) are extreme high-amplitude bursts of X-ray radiation recurring every few hours and originating near the central supermassive black holes in galactic nuclei. It is currently unknown what triggers these events, how long they last and how they are connected to the physical properties of the inner accretion flows. Previously, only two such sources were known, found eith… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.13388v1-abstract-full').style.display = 'inline'; document.getElementById('2104.13388v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2104.13388v1-abstract-full" style="display: none;"> Quasi-Periodic Eruptions (QPEs) are extreme high-amplitude bursts of X-ray radiation recurring every few hours and originating near the central supermassive black holes in galactic nuclei. It is currently unknown what triggers these events, how long they last and how they are connected to the physical properties of the inner accretion flows. Previously, only two such sources were known, found either serendipitously or in archival data, with emission lines in their optical spectra classifying their nuclei as hosting an actively accreting supermassive black hole. Here we present the detection of QPEs in two further galaxies, obtained with a blind and systematic search over half of the X-ray sky. The optical spectra of these galaxies show no signature of black hole activity, indicating that a pre-existing accretion flow typical of active nuclei is not required to trigger these events. Indeed, the periods, amplitudes and profiles of the newly discovered QPEs are inconsistent with current models that invoke radiation-pressure driven accretion disk instabilities. Instead, QPEs might be driven by an orbiting compact object. Furthermore, their observed properties require the mass of the secondary object to be much smaller than the main body and future X-ray observations may constrain possible changes in the period due to orbital evolution. This scenario could make QPEs a viable candidate for the electromagnetic counterparts of the so-called extreme mass ratio inspirals, with considerable implications for multi-messenger astrophysics and cosmology. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.13388v1-abstract-full').style.display = 'none'; document.getElementById('2104.13388v1-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 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">Published in Nature: https://dx.doi.org/10.1038/s41586-021-03394-6</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nature volume 592, pages 704-707 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2104.02462">arXiv:2104.02462</a> <span> [<a href="https://arxiv.org/pdf/2104.02462">pdf</a>, <a href="https://arxiv.org/format/2104.02462">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="High Energy Astrophysical Phenomena">astro-ph.HE</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/10.1051/0004-6361/202140317">10.1051/0004-6361/202140317 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The eROSITA Final Equatorial-Depth Survey (eFEDS): An X-ray bright, extremely luminous infrared galaxy at z = 1.87 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Toba%2C+Y">Yoshiki Toba</a>, <a href="/search/?searchtype=author&query=Brusa%2C+M">Marcella Brusa</a>, <a href="/search/?searchtype=author&query=Liu%2C+T">Teng Liu</a>, <a href="/search/?searchtype=author&query=Buchner%2C+J">Johannes Buchner</a>, <a href="/search/?searchtype=author&query=Terashima%2C+Y">Yuichi Terashima</a>, <a href="/search/?searchtype=author&query=Urrutia%2C+T">Tanya Urrutia</a>, <a href="/search/?searchtype=author&query=Salvato%2C+M">Mara Salvato</a>, <a href="/search/?searchtype=author&query=Akiyama%2C+M">Masayuki Akiyama</a>, <a href="/search/?searchtype=author&query=Arcodia%2C+R">Riccardo Arcodia</a>, <a href="/search/?searchtype=author&query=Goulding%2C+A+D">Andy D. Goulding</a>, <a href="/search/?searchtype=author&query=Higuchi%2C+Y">Yuichi Higuchi</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K+T">Kaiki T. Inoue</a>, <a href="/search/?searchtype=author&query=Kawaguchi%2C+T">Toshihiro Kawaguchi</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">Georg Lamer</a>, <a href="/search/?searchtype=author&query=Merloni%2C+A">Andrea Merloni</a>, <a href="/search/?searchtype=author&query=Nagao%2C+T">Tohru Nagao</a>, <a href="/search/?searchtype=author&query=Ueda%2C+Y">Yoshihiro Ueda</a>, <a href="/search/?searchtype=author&query=Nandra%2C+K">Kirpal Nandra</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="2104.02462v1-abstract-short" style="display: inline;"> In this study, we investigate the X-ray properties of WISE J090924.01+000211.1 (WISEJ0909+0002), an extremely luminous infrared (IR) galaxy (ELIRG) at $z_{\rm spec}$= 1.871 in the eROSITA final equatorial depth survey (eFEDS). WISEJ0909+0002 is a WISE 22 $渭$m source, located in the GAMA-09 field, detected by eROSITA during the performance and verification phase. The corresponding optical spectrum… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.02462v1-abstract-full').style.display = 'inline'; document.getElementById('2104.02462v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2104.02462v1-abstract-full" style="display: none;"> In this study, we investigate the X-ray properties of WISE J090924.01+000211.1 (WISEJ0909+0002), an extremely luminous infrared (IR) galaxy (ELIRG) at $z_{\rm spec}$= 1.871 in the eROSITA final equatorial depth survey (eFEDS). WISEJ0909+0002 is a WISE 22 $渭$m source, located in the GAMA-09 field, detected by eROSITA during the performance and verification phase. The corresponding optical spectrum indicates that this object is a type-1 active galactic nucleus (AGN). Observations from eROSITA combined with Chandra and XMM-Newton archival data indicate a very luminous ($L$ (2--10 keV) = ($2.1 \pm 0.2) \times 10^{45}$ erg s$^{-1}$) unobscured AGN with a power-law photon index of $螕$ = 1.73$_{-0.15}^{+0.16}$, and an absorption hydrogen column density of $\log\,(N_{\rm H}/{\rm cm}^{-2}) < 21.0$. The IR luminosity was estimated to be $L_{\rm IR}$ = (1.79 $\pm$ 0.09) $\times 10^{14}\, L_{\odot}$ from spectral energy distribution modeling based on 22 photometric data (X-ray to far-IR) with X-CIGALE, which confirmed that WISEJ0909+0002 is an ELIRG. A remarkably high $L_{\rm IR}$ despite very low $N_{\rm H}$ would indicate that we are witnessing a short-lived phase in which hydrogen gas along the line of sight is blown outwards, whereas warm and hot dust heated by AGNs still exist. As a consequence of eROSITA all-sky survey, $6.8_{-5.6}^{+16}\times 10^2$ such X-ray bright ELIRGs are expected to be discovered in the entire extragalactic sky ($|b| > 10^\circ$). This can potentially be the key population to constrain the bright-end of IR luminosity functions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.02462v1-abstract-full').style.display = 'none'; document.getElementById('2104.02462v1-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 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">10 pages, 5 figures, and 3 tables, accepted for publication in A&A Letters (special Issue: First science highlights from SRG/eROSITA)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 649, L11 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.05585">arXiv:2101.05585</a> <span> [<a href="https://arxiv.org/pdf/2101.05585">pdf</a>, <a href="https://arxiv.org/format/2101.05585">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="High Energy Astrophysical Phenomena">astro-ph.HE</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/10.1051/0004-6361/202039724">10.1051/0004-6361/202039724 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First constraints on the AGN X-ray luminosity function at $z \sim 6$ from an eROSITA-detected quasar </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Wolf%2C+J">Julien Wolf</a>, <a href="/search/?searchtype=author&query=Nandra%2C+K">Kirpal Nandra</a>, <a href="/search/?searchtype=author&query=Salvato%2C+M">Mara Salvato</a>, <a href="/search/?searchtype=author&query=Liu%2C+T">Teng Liu</a>, <a href="/search/?searchtype=author&query=Buchner%2C+J">Johannes Buchner</a>, <a href="/search/?searchtype=author&query=Brusa%2C+M">Marcella Brusa</a>, <a href="/search/?searchtype=author&query=Hoang%2C+D+N">Duy N. Hoang</a>, <a href="/search/?searchtype=author&query=Moss%2C+V">Vanessa Moss</a>, <a href="/search/?searchtype=author&query=Arcodia%2C+R">Riccardo Arcodia</a>, <a href="/search/?searchtype=author&query=Br%C3%BCggen%2C+M">Marcus Br眉ggen</a>, <a href="/search/?searchtype=author&query=Comparat%2C+J">Johan Comparat</a>, <a href="/search/?searchtype=author&query=de+Gasperin%2C+F">Francesco de Gasperin</a>, <a href="/search/?searchtype=author&query=Georgakakis%2C+A">Antonis Georgakakis</a>, <a href="/search/?searchtype=author&query=Hotan%2C+A">Aidan Hotan</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">Georg Lamer</a>, <a href="/search/?searchtype=author&query=Merloni%2C+A">Andrea Merloni</a>, <a href="/search/?searchtype=author&query=Rau%2C+A">Arne Rau</a>, <a href="/search/?searchtype=author&query=Rottgering%2C+H+J+A">Huub J. A. Rottgering</a>, <a href="/search/?searchtype=author&query=Shimwell%2C+T+W">Timothy W. Shimwell</a>, <a href="/search/?searchtype=author&query=Urrutia%2C+T">Tanya Urrutia</a>, <a href="/search/?searchtype=author&query=Whiting%2C+M">Matthew Whiting</a>, <a href="/search/?searchtype=author&query=Williams%2C+W+L">Wendy L. Williams</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2101.05585v1-abstract-short" style="display: inline;"> We searched for high-z quasars within the X-ray source population detected in the contiguous $\sim 140^2$ eFEDS field observed by eROSITA during the performance verification phase. We collected the available spectroscopic information in the field, including the sample of all currently known optically selected z>5.5 quasars and cross-matched secure Legacy DR8 counterparts of eROSITA-detected X-ray… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.05585v1-abstract-full').style.display = 'inline'; document.getElementById('2101.05585v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.05585v1-abstract-full" style="display: none;"> We searched for high-z quasars within the X-ray source population detected in the contiguous $\sim 140^2$ eFEDS field observed by eROSITA during the performance verification phase. We collected the available spectroscopic information in the field, including the sample of all currently known optically selected z>5.5 quasars and cross-matched secure Legacy DR8 counterparts of eROSITA-detected X-ray point-like sources with this spectroscopic sample. We report the X-ray detection of an eROSITA source securely matched to the well-known quasar SDSS J083643.85+005453.3 (z=5.81). The soft X-ray flux of the source derived from eROSITA is consistent with previous Chandra observations. In addition, we report the detection of the quasar with LOFAR at 145 MHz and ASKAP at 888 MHz. The reported flux densities confirm a spectral flattening at lower frequencies in the emission of the radio core, indicating that the quasar could be a (sub-) gigahertz peaked spectrum source. The inferred spectral shape and the parsec-scale radio morphology of SDSS J083643.85+005453.3 suggest that it is in an early stage of its evolution into a large-scale radio source or confined in a dense environment. We find no indications for a strong jet contribution to the X-ray emission of the quasar, which is therefore likely to be linked to accretion processes. The detection of this source allows us to place the first constraints on the XLF at z>5.5 based on a secure spectroscopic redshift. Compared to extrapolations from lower-redshift observations, this favours a relatively flat slope for the XLF at $z\sim 6$ beyond $L_*$. The population of X-ray luminous AGNs at high redshift may be larger than previously thought. From our XLF constraints, we make the conservative prediction that eROSITA will detect $\sim 90$ X-ray luminous AGNs at redshifts 5.7<z<6.4 in the full-sky survey (De+RU). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.05585v1-abstract-full').style.display = 'none'; document.getElementById('2101.05585v1-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 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 647, A5 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.11754">arXiv:2012.11754</a> <span> [<a href="https://arxiv.org/pdf/2012.11754">pdf</a>, <a href="https://arxiv.org/format/2012.11754">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </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/10.1051/0004-6361/202039757">10.1051/0004-6361/202039757 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A giant X-ray dust scattering ring around the black hole transient MAXI J1348-630 discovered with SRG/eROSITA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Lamer%2C+G">G. Lamer</a>, <a href="/search/?searchtype=author&query=Schwope%2C+A+D">A. D. Schwope</a>, <a href="/search/?searchtype=author&query=Predehl%2C+P">P. Predehl</a>, <a href="/search/?searchtype=author&query=Traulsen%2C+I">I. Traulsen</a>, <a href="/search/?searchtype=author&query=Wilms%2C+J">J. Wilms</a>, <a href="/search/?searchtype=author&query=Freyberg%2C+M">M. Freyberg</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="2012.11754v1-abstract-short" style="display: inline;"> We report the discovery of a giant dust scattering ring around the Black Hole transient MAXI J1348-630 with SRG/eROSITA during its first X-ray all-sky survey. During the discovery observation in February 2020 the ring had an outer diameter of 1.3 deg, growing to 1.6 deg by the time of the second all sky survey scan in August 2020. This makes the new dust ring the by far largest X-ray scattering ri… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.11754v1-abstract-full').style.display = 'inline'; document.getElementById('2012.11754v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.11754v1-abstract-full" style="display: none;"> We report the discovery of a giant dust scattering ring around the Black Hole transient MAXI J1348-630 with SRG/eROSITA during its first X-ray all-sky survey. During the discovery observation in February 2020 the ring had an outer diameter of 1.3 deg, growing to 1.6 deg by the time of the second all sky survey scan in August 2020. This makes the new dust ring the by far largest X-ray scattering ring observed so far. Dust scattering halos, in particular the rings found around transient sources, offer the possibility of precise distance measurements towards the original X-ray sources. We combine data from SRG/eROSITA, XMM-Newton, MAXI, and Gaia to measure the geometrical distance of MAXI J1348-630. The Gaia data place the scattering dust at a distance of 2050 pc, from the measured time lags and the geometry of the ring, we find MAXI J1348-630 at a distance of 3390 pc with a statistical uncertainty of only 1.1% and a systematic uncertainty of 10% caused mainly by the parallax offset of Gaia. This result makes MAXI J1348-630 one of the black hole transients with the best determined distances. The new distance leads to a revised mass estimate for the black hole of 11+-2 solar masses, the transition to the soft state during the outburst occurred when the bolometric luminosity of MAXI J1348-630 had reached 1.7% of its Eddington luminosity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.11754v1-abstract-full').style.display = 'none'; document.getElementById('2012.11754v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 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">10 pages, 10 figures, 3 tables, accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 647, A7 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2010.03477">arXiv:2010.03477</a> <span> [<a href="https://arxiv.org/pdf/2010.03477">pdf</a>, <a href="https://arxiv.org/format/2010.03477">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1051/0004-6361/202039313">10.1051/0004-6361/202039313 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The eROSITA X-ray telescope on SRG </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Predehl%2C+P">P. Predehl</a>, <a href="/search/?searchtype=author&query=Andritschke%2C+R">R. Andritschke</a>, <a href="/search/?searchtype=author&query=Arefiev%2C+V">V. Arefiev</a>, <a href="/search/?searchtype=author&query=Babyshkin%2C+V">V. Babyshkin</a>, <a href="/search/?searchtype=author&query=Batanov%2C+O">O. Batanov</a>, <a href="/search/?searchtype=author&query=Becker%2C+W">W. Becker</a>, <a href="/search/?searchtype=author&query=B%C3%B6hringer%2C+H">H. B枚hringer</a>, <a href="/search/?searchtype=author&query=Bogomolov%2C+A">A. Bogomolov</a>, <a href="/search/?searchtype=author&query=Boller%2C+T">T. Boller</a>, <a href="/search/?searchtype=author&query=Borm%2C+K">K. Borm</a>, <a href="/search/?searchtype=author&query=Bornemann%2C+W">W. Bornemann</a>, <a href="/search/?searchtype=author&query=Br%C3%A4uninger%2C+H">H. Br盲uninger</a>, <a href="/search/?searchtype=author&query=Br%C3%BCggen%2C+M">M. Br眉ggen</a>, <a href="/search/?searchtype=author&query=Brunner%2C+H">H. Brunner</a>, <a href="/search/?searchtype=author&query=Brusa%2C+M">M. Brusa</a>, <a href="/search/?searchtype=author&query=Bulbul%2C+E">E. Bulbul</a>, <a href="/search/?searchtype=author&query=Buntov%2C+M">M. Buntov</a>, <a href="/search/?searchtype=author&query=Burwitz%2C+V">V. Burwitz</a>, <a href="/search/?searchtype=author&query=Burkert%2C+W">W. Burkert</a>, <a href="/search/?searchtype=author&query=Clerc%2C+N">N. Clerc</a>, <a href="/search/?searchtype=author&query=Churazov%2C+E">E. Churazov</a>, <a href="/search/?searchtype=author&query=Coutinho%2C+D">D. Coutinho</a>, <a href="/search/?searchtype=author&query=Dauser%2C+T">T. Dauser</a>, <a href="/search/?searchtype=author&query=Dennerl%2C+K">K. Dennerl</a>, <a href="/search/?searchtype=author&query=Doroshenko%2C+V">V. Doroshenko</a> , et al. (68 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="2010.03477v1-abstract-short" style="display: inline;"> eROSITA (extended ROentgen Survey with an Imaging Telescope Array) is the primary instrument on the Spectrum-Roentgen-Gamma (SRG) mission, which was successfully launched on July 13, 2019, from the Baikonour cosmodrome. After the commissioning of the instrument and a subsequent calibration and performance verification phase, eROSITA started a survey of the entire sky on December 13, 2019. By the e… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.03477v1-abstract-full').style.display = 'inline'; document.getElementById('2010.03477v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.03477v1-abstract-full" style="display: none;"> eROSITA (extended ROentgen Survey with an Imaging Telescope Array) is the primary instrument on the Spectrum-Roentgen-Gamma (SRG) mission, which was successfully launched on July 13, 2019, from the Baikonour cosmodrome. After the commissioning of the instrument and a subsequent calibration and performance verification phase, eROSITA started a survey of the entire sky on December 13, 2019. By the end of 2023, eight complete scans of the celestial sphere will have been performed, each lasting six months. At the end of this program, the eROSITA all-sky survey in the soft X-ray band (0.2--2.3\,keV) will be about 25 times more sensitive than the ROSAT All-Sky Survey, while in the hard band (2.3--8\,keV) it will provide the first ever true imaging survey of the sky. The eROSITA design driving science is the detection of large samples of galaxy clusters up to redshifts $z>1$ in order to study the large-scale structure of the universe and test cosmological models including Dark Energy. In addition, eROSITA is expected to yield a sample of a few million AGNs, including obscured objects, revolutionizing our view of the evolution of supermassive black holes. The survey will also provide new insights into a wide range of astrophysical phenomena, including X-ray binaries, active stars, and diffuse emission within the Galaxy. Results from early observations, some of which are presented here, confirm that the performance of the instrument is able to fulfil its scientific promise. With this paper, we aim to give a concise description of the instrument, its performance as measured on ground, its operation in space, and also the first results from in-orbit measurements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.03477v1-abstract-full').style.display = 'none'; document.getElementById('2010.03477v1-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 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">16 pages, 19 figures, accepted by Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 647, A1 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.02932">arXiv:2007.02932</a> <span> [<a href="https://arxiv.org/pdf/2007.02932">pdf</a>, <a href="https://arxiv.org/format/2007.02932">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1051/0004-6361/202037706">10.1051/0004-6361/202037706 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The XMM-Newton serendipitous survey. X: The second source catalogue from overlapping XMM-Newton observations and its long-term variable content </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Traulsen%2C+I">I. Traulsen</a>, <a href="/search/?searchtype=author&query=Schwope%2C+A+D">A. D. Schwope</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">G. Lamer</a>, <a href="/search/?searchtype=author&query=Ballet%2C+J">J. Ballet</a>, <a href="/search/?searchtype=author&query=Carrera%2C+F+J">F. J. Carrera</a>, <a href="/search/?searchtype=author&query=Ceballos%2C+M+T">M. T. Ceballos</a>, <a href="/search/?searchtype=author&query=Coriat%2C+M">M. Coriat</a>, <a href="/search/?searchtype=author&query=Freyberg%2C+M+J">M. J. Freyberg</a>, <a href="/search/?searchtype=author&query=Koliopanos%2C+F">F. Koliopanos</a>, <a href="/search/?searchtype=author&query=Kurpas%2C+J">J. Kurpas</a>, <a href="/search/?searchtype=author&query=Michel%2C+L">L. Michel</a>, <a href="/search/?searchtype=author&query=Motch%2C+C">C. Motch</a>, <a href="/search/?searchtype=author&query=Page%2C+M+J">M. J. Page</a>, <a href="/search/?searchtype=author&query=Watson%2C+M+G">M. G. Watson</a>, <a href="/search/?searchtype=author&query=Webb%2C+N+A">N. A. Webb</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="2007.02932v1-abstract-short" style="display: inline;"> The XMM-Newton Survey Science Centre Consortium (SSC) develops software in close collaboration with the Science Operations Centre to perform a pipeline analysis of all XMM-Newton observations. In celebration of the 20th launch anniversary, the SSC has compiled the 4th generation of serendipitous source catalogues, 4XMM. The catalogue described here, 4XMM-DR9s, explores sky areas that were observed… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.02932v1-abstract-full').style.display = 'inline'; document.getElementById('2007.02932v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.02932v1-abstract-full" style="display: none;"> The XMM-Newton Survey Science Centre Consortium (SSC) develops software in close collaboration with the Science Operations Centre to perform a pipeline analysis of all XMM-Newton observations. In celebration of the 20th launch anniversary, the SSC has compiled the 4th generation of serendipitous source catalogues, 4XMM. The catalogue described here, 4XMM-DR9s, explores sky areas that were observed more than once by XMM-Newton. It was constructed from simultaneous source detection on the overlapping observations, which were bundled in groups ("stacks"). Stacking leads to a higher sensitivity, resulting in newly discovered sources and better constrained source parameters, and unveils long-term brightness variations. As a novel feature, positional rectification was applied beforehand. Observations with all filters and suitable camera settings were included. Exposures with a high background were discarded, which was determined through a statistical analysis of all exposures in each instrument configuration. The X-ray background maps used in source detection were modelled via adaptive smoothing with newly determined parameters. Source fluxes were derived for all contributing observations, irrespective of whether the source would be detectable in an individual observation. From 1,329 stacks with 6,604 contributing observations over repeatedly covered 300 square degrees in the sky, 4XMM-DR9s lists 288,191 sources. 218,283 of them were observed several times. Most stacks are composed of two observations, the largest one comprises 352. The number of observations of a source ranges from 1 to 40. Auxiliary products like X-ray images, long-term light curves, and optical finding charts are published as well. 4XMM-DR9s is considered a prime resource to explore long-term variability of X-ray sources discovered by XMM-Newton. Regular incremental releases including new public observations are planned. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.02932v1-abstract-full').style.display = 'none'; document.getElementById('2007.02932v1-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 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A. 20 pages</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 641, A137 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.02899">arXiv:2007.02899</a> <span> [<a href="https://arxiv.org/pdf/2007.02899">pdf</a>, <a href="https://arxiv.org/ps/2007.02899">ps</a>, <a href="https://arxiv.org/format/2007.02899">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </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/10.1051/0004-6361/201937353">10.1051/0004-6361/201937353 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The XMM-Newton serendipitous survey IX. The fourth XMM-Newton serendipitous source catalogue </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Webb%2C+N+A">N. A. Webb</a>, <a href="/search/?searchtype=author&query=Coriat%2C+M">M. Coriat</a>, <a href="/search/?searchtype=author&query=Traulsen%2C+I">I. Traulsen</a>, <a href="/search/?searchtype=author&query=Ballet%2C+J">J. Ballet</a>, <a href="/search/?searchtype=author&query=Motch%2C+C">C. Motch</a>, <a href="/search/?searchtype=author&query=Carrera%2C+F+J">F. J. Carrera</a>, <a href="/search/?searchtype=author&query=Koliopanos%2C+F">F. Koliopanos</a>, <a href="/search/?searchtype=author&query=Authier%2C+J">J. Authier</a>, <a href="/search/?searchtype=author&query=de+la+Calle%2C+I">I. de la Calle</a>, <a href="/search/?searchtype=author&query=Ceballos%2C+M+T">M. T. Ceballos</a>, <a href="/search/?searchtype=author&query=Colomo%2C+E">E. Colomo</a>, <a href="/search/?searchtype=author&query=Chuard%2C+D">D. Chuard</a>, <a href="/search/?searchtype=author&query=Freyberg%2C+M">M. Freyberg</a>, <a href="/search/?searchtype=author&query=Garcia%2C+T">T. Garcia</a>, <a href="/search/?searchtype=author&query=Kolehmainen%2C+M">M. Kolehmainen</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">G. Lamer</a>, <a href="/search/?searchtype=author&query=Lin%2C+D">D. Lin</a>, <a href="/search/?searchtype=author&query=Maggi%2C+P">P. Maggi</a>, <a href="/search/?searchtype=author&query=Michel%2C+L">L. Michel</a>, <a href="/search/?searchtype=author&query=Page%2C+C+G">C. G. Page</a>, <a href="/search/?searchtype=author&query=Page%2C+M+J">M. J. Page</a>, <a href="/search/?searchtype=author&query=Perea-Calderon%2C+J+V">J. V. Perea-Calderon</a>, <a href="/search/?searchtype=author&query=Pineau%2C+F+-">F. -X. Pineau</a>, <a href="/search/?searchtype=author&query=Rodriguez%2C+P">P. Rodriguez</a>, <a href="/search/?searchtype=author&query=Rosen%2C+S+R">S. R. Rosen</a> , et al. (6 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2007.02899v1-abstract-short" style="display: inline;"> Sky surveys produce enormous quantities of data on extensive regions of the sky. The easiest way to access this information is through catalogues of standardised data products. {\em XMM-Newton} has been surveying the sky in the X-ray, ultra-violet, and optical bands for 20 years. The {\em XMM-Newton} Survey Science Centre has been producing standardised data products and catalogues to facilitate a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.02899v1-abstract-full').style.display = 'inline'; document.getElementById('2007.02899v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.02899v1-abstract-full" style="display: none;"> Sky surveys produce enormous quantities of data on extensive regions of the sky. The easiest way to access this information is through catalogues of standardised data products. {\em XMM-Newton} has been surveying the sky in the X-ray, ultra-violet, and optical bands for 20 years. The {\em XMM-Newton} Survey Science Centre has been producing standardised data products and catalogues to facilitate access to the serendipitous X-ray sky. Using improved calibration and enhanced software, we re-reduced all of the 14041 {\em XMM-Newton} X-ray observations, of which 11204 observations contained data with at least one detection and with these we created a new, high quality version of the {\em XMM-Newton} serendipitous source catalogue, 4XMM-DR9. 4XMM-DR9 contains 810795 detections down to a detection significance of 3 $蟽$, of which 550124 are unique sources, which cover 1152 degrees$^{2}$ (2.85\%) of the sky. Filtering 4XMM-DR9 to retain only the cleanest sources with at least a 5 $蟽$ detection significance leaves 433612 detections. Of these detections, 99.6\% have no pileup. Furthermore, 336 columns of information on each detection are provided, along with images. The quality of the source detection is shown to have improved significantly with respect to previous versions of the catalogues. Spectra and lightcurves are also made available for more than 288000 of the brightest sources (36\% of all detections). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.02899v1-abstract-full').style.display = 'none'; document.getElementById('2007.02899v1-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 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 11 figures, accepted to be published Astronomy and Astrophysics (A&A)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 641, A136 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1903.02472">arXiv:1903.02472</a> <span> [<a href="https://arxiv.org/pdf/1903.02472">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.18727/0722-6691/5125">10.18727/0722-6691/5125 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> 4MOST Consortium Survey 6: Active Galactic Nuclei </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Merloni%2C+A">A. Merloni</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+A">D. A. Alexander</a>, <a href="/search/?searchtype=author&query=Banerji%2C+M">M. Banerji</a>, <a href="/search/?searchtype=author&query=Boller%2C+T">T. Boller</a>, <a href="/search/?searchtype=author&query=Comparat%2C+J">J. Comparat</a>, <a href="/search/?searchtype=author&query=Dwelly%2C+T">T. Dwelly</a>, <a href="/search/?searchtype=author&query=Fotopoulou%2C+S">S. Fotopoulou</a>, <a href="/search/?searchtype=author&query=McMahon%2C+R">R. McMahon</a>, <a href="/search/?searchtype=author&query=Nandra%2C+K">K. Nandra</a>, <a href="/search/?searchtype=author&query=Salvato%2C+M">M. Salvato</a>, <a href="/search/?searchtype=author&query=Croom%2C+S">S. Croom</a>, <a href="/search/?searchtype=author&query=Finoguenov%2C+A">A. Finoguenov</a>, <a href="/search/?searchtype=author&query=Krumpe%2C+M">M. Krumpe</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">G. Lamer</a>, <a href="/search/?searchtype=author&query=Rosario%2C+D">D. Rosario</a>, <a href="/search/?searchtype=author&query=Schwope%2C+A">A. Schwope</a>, <a href="/search/?searchtype=author&query=Shanks%2C+T">T. Shanks</a>, <a href="/search/?searchtype=author&query=Steinmetz%2C+M">M. Steinmetz</a>, <a href="/search/?searchtype=author&query=Wisotzki%2C+L">L. Wisotzki</a>, <a href="/search/?searchtype=author&query=Worseck%2C+G">G. Worseck</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1903.02472v2-abstract-short" style="display: inline;"> X-ray and mid-infrared emission are signposts of the accretion of matter onto the supermassive black holes that reside at the centres of most galaxies. As a major step towards understanding accreting supermassive black holes and their role in the evolution of galaxies, we will use the 4MOST multi-object spectrograph to provide a highly complete census of active galactic nuclei over a large fractio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.02472v2-abstract-full').style.display = 'inline'; document.getElementById('1903.02472v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1903.02472v2-abstract-full" style="display: none;"> X-ray and mid-infrared emission are signposts of the accretion of matter onto the supermassive black holes that reside at the centres of most galaxies. As a major step towards understanding accreting supermassive black holes and their role in the evolution of galaxies, we will use the 4MOST multi-object spectrograph to provide a highly complete census of active galactic nuclei over a large fraction of the extragalactic sky observed in X-rays by eROSITA that is visible to 4MOST. We will systematically follow up all eROSITA point-like extragalactic X-ray sources (mostly active galactic nuclei), and complement them with a heavily obscured active galactic nuclei selection approach using mid-infrared data from the Wide-field Infrared Survey Explorer (WISE). The X-ray and mid-infrared flux limits of eROSITA and WISE are well matched to the spectroscopic capabilities of a 4-metre-class telescope, allowing us to reach completeness levels of ~80-90% for all X-ray selected active galactic nuclei with fluxes $f_{0.5-2\ {\rm keV}} > 10^{-14}$ erg s$^{-1}$ cm$^{-2}$; this is about a factor of 30 deeper than the ROSAT all-sky survey. With these data we will determine the physical properties (redshift, luminosity, line emission strength, masses, etc.) of up to one million supermassive black holes, constrain their cosmic evolution and clustering properties, and explore the connection between active galactic nuclei and large-scale structure over redshifts $0 \le z \le 6$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.02472v2-abstract-full').style.display = 'none'; document.getElementById('1903.02472v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 March, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Part of the 4MOST issue of The Messenger, published in preparation of the 4MOST Community Workshop, see http://www.eso.org/sci/meetings/2019/4MOST.html</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Messenger, 2019, 175, 42 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1903.02464">arXiv:1903.02464</a> <span> [<a href="https://arxiv.org/pdf/1903.02464">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div 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/10.18727/0722-6691/5117">10.18727/0722-6691/5117 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> 4MOST: Project overview and information for the First Call for Proposals </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=de+Jong%2C+R+S">R. S. de Jong</a>, <a href="/search/?searchtype=author&query=Agertz%2C+O">O. Agertz</a>, <a href="/search/?searchtype=author&query=Berbel%2C+A+A">A. Agudo Berbel</a>, <a href="/search/?searchtype=author&query=Aird%2C+J">J. Aird</a>, <a href="/search/?searchtype=author&query=Alexander%2C+D+A">D. A. Alexander</a>, <a href="/search/?searchtype=author&query=Amarsi%2C+A">A. Amarsi</a>, <a href="/search/?searchtype=author&query=Anders%2C+F">F. Anders</a>, <a href="/search/?searchtype=author&query=Andrae%2C+R">R. Andrae</a>, <a href="/search/?searchtype=author&query=Ansarinejad%2C+B">B. Ansarinejad</a>, <a href="/search/?searchtype=author&query=Ansorge%2C+W">W. Ansorge</a>, <a href="/search/?searchtype=author&query=Antilogus%2C+P">P. Antilogus</a>, <a href="/search/?searchtype=author&query=Anwand-Heerwart%2C+H">H. Anwand-Heerwart</a>, <a href="/search/?searchtype=author&query=Arentsen%2C+A">A. Arentsen</a>, <a href="/search/?searchtype=author&query=Arnadottir%2C+A">A. Arnadottir</a>, <a href="/search/?searchtype=author&query=Asplund%2C+M">M. Asplund</a>, <a href="/search/?searchtype=author&query=Auger%2C+M">M. Auger</a>, <a href="/search/?searchtype=author&query=Azais%2C+N">N. Azais</a>, <a href="/search/?searchtype=author&query=Baade%2C+D">D. Baade</a>, <a href="/search/?searchtype=author&query=Baker%2C+G">G. Baker</a>, <a href="/search/?searchtype=author&query=Baker%2C+S">S. Baker</a>, <a href="/search/?searchtype=author&query=Balbinot%2C+E">E. Balbinot</a>, <a href="/search/?searchtype=author&query=Baldry%2C+I+K">I. K. Baldry</a>, <a href="/search/?searchtype=author&query=Banerji%2C+M">M. Banerji</a>, <a href="/search/?searchtype=author&query=Barden%2C+S">S. Barden</a>, <a href="/search/?searchtype=author&query=Barklem%2C+P">P. Barklem</a> , et al. (313 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1903.02464v2-abstract-short" style="display: inline;"> We introduce the 4-metre Multi-Object Spectroscopic Telescope (4MOST), a new high-multiplex, wide-field spectroscopic survey facility under development for the four-metre-class Visible and Infrared Survey Telescope for Astronomy (VISTA) at Paranal. Its key specifications are: a large field of view (FoV) of 4.2 square degrees and a high multiplex capability, with 1624 fibres feeding two low-resolut… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.02464v2-abstract-full').style.display = 'inline'; document.getElementById('1903.02464v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1903.02464v2-abstract-full" style="display: none;"> We introduce the 4-metre Multi-Object Spectroscopic Telescope (4MOST), a new high-multiplex, wide-field spectroscopic survey facility under development for the four-metre-class Visible and Infrared Survey Telescope for Astronomy (VISTA) at Paranal. Its key specifications are: a large field of view (FoV) of 4.2 square degrees and a high multiplex capability, with 1624 fibres feeding two low-resolution spectrographs ($R = 位/螖位\sim 6500$), and 812 fibres transferring light to the high-resolution spectrograph ($R \sim 20\,000$). After a description of the instrument and its expected performance, a short overview is given of its operational scheme and planned 4MOST Consortium science; these aspects are covered in more detail in other articles in this edition of The Messenger. Finally, the processes, schedules, and policies concerning the selection of ESO Community Surveys are presented, commencing with a singular opportunity to submit Letters of Intent for Public Surveys during the first five years of 4MOST operations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.02464v2-abstract-full').style.display = 'none'; document.getElementById('1903.02464v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 March, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Part of the 4MOST issue of The Messenger, published in preparation of 4MOST Community Workshop, see http://www.eso.org/sci/meetings/2019/4MOST.html</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Messenger, 2019, 175, 3 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1807.09178">arXiv:1807.09178</a> <span> [<a href="https://arxiv.org/pdf/1807.09178">pdf</a>, <a href="https://arxiv.org/format/1807.09178">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </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/10.1051/0004-6361/201833938">10.1051/0004-6361/201833938 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The XMM-Newton serendipitous survey. VIII: The first XMM-Newton serendipitous source catalogue from overlapping observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Traulsen%2C+I">I. Traulsen</a>, <a href="/search/?searchtype=author&query=Schwope%2C+A+D">A. D. Schwope</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">G. Lamer</a>, <a href="/search/?searchtype=author&query=Ballet%2C+J">J. Ballet</a>, <a href="/search/?searchtype=author&query=Carrera%2C+F">F. Carrera</a>, <a href="/search/?searchtype=author&query=Coriat%2C+M">M. Coriat</a>, <a href="/search/?searchtype=author&query=Freyberg%2C+M+J">M. J. Freyberg</a>, <a href="/search/?searchtype=author&query=Michel%2C+L">L. Michel</a>, <a href="/search/?searchtype=author&query=Motch%2C+C">C. Motch</a>, <a href="/search/?searchtype=author&query=Rosen%2C+S+R">S. R. Rosen</a>, <a href="/search/?searchtype=author&query=Webb%2C+N">N. Webb</a>, <a href="/search/?searchtype=author&query=Ceballos%2C+M+T">M. T. Ceballos</a>, <a href="/search/?searchtype=author&query=Koliopanos%2C+F">F. Koliopanos</a>, <a href="/search/?searchtype=author&query=Kurpas%2C+J">J. Kurpas</a>, <a href="/search/?searchtype=author&query=Page%2C+M">M. Page</a>, <a href="/search/?searchtype=author&query=Watson%2C+M+G">M. G. Watson</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1807.09178v2-abstract-short" style="display: inline;"> XMM-Newton has observed the X-ray sky since early 2000. The XMM-Newton Survey Science Centre Consortium has published catalogues of X-ray and ultraviolet sources found serendipitously in the individual observations. This series is now augmented by a catalogue dedicated to X-ray sources detected in spatially overlapping XMM-Newton observations. The aim of this catalogue is to explore repeatedly obs… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.09178v2-abstract-full').style.display = 'inline'; document.getElementById('1807.09178v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1807.09178v2-abstract-full" style="display: none;"> XMM-Newton has observed the X-ray sky since early 2000. The XMM-Newton Survey Science Centre Consortium has published catalogues of X-ray and ultraviolet sources found serendipitously in the individual observations. This series is now augmented by a catalogue dedicated to X-ray sources detected in spatially overlapping XMM-Newton observations. The aim of this catalogue is to explore repeatedly observed sky regions. It thus makes use of the long(er) effective exposure time per sky area and offers the opportunity to investigate long-term flux variability directly through the source detection process. A new standardised strategy for simultaneous source detection on multiple observations is introduced. It is coded as a new task within the XMM-Newton Science Analysis System and used to compile a catalogue of sources from 434 stacks comprising 1,789 overlapping XMM-Newton observations that entered the 3XMM-DR7 catalogue, have a low background and full-frame readout of all EPIC cameras. The first stacked catalogue is called 3XMM-DR7s. It contains 71,951 unique sources with positions and parameters such as fluxes, hardness ratios, quality estimates, and information on inter-observation variability. About 15% of the sources are new with respect to 3XMM-DR7. Through stacked source detection, the parameters of repeatedly observed sources can be determined with higher accuracy than in the individual observations. The method is more sensitive to faint sources and tends to produce fewer spurious detections. With this first stacked catalogue we demonstrate the feasibility and benefit of the approach. It supplements the large data base of XMM-Newton detections by additional, in particular faint, sources and adds variability information. In the future, the catalogue will be expanded to larger samples and continued within the series of serendipitous XMM-Newton source catalogues. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.09178v2-abstract-full').style.display = 'none'; document.getElementById('1807.09178v2-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 March, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 July, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A. 27 pages, ~4MB</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 624, A77 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1806.08652">arXiv:1806.08652</a> <span> [<a href="https://arxiv.org/pdf/1806.08652">pdf</a>, <a href="https://arxiv.org/format/1806.08652">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/10.1051/0004-6361/201732119">10.1051/0004-6361/201732119 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Synthetic simulations of the extragalactic sky seen by eROSITA. I. Pre-launch selection functions from Monte-Carlo simulations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Clerc%2C+N">N. Clerc</a>, <a href="/search/?searchtype=author&query=Ramos-Ceja%2C+M+E">M. E. Ramos-Ceja</a>, <a href="/search/?searchtype=author&query=Ridl%2C+J">J. Ridl</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">G. Lamer</a>, <a href="/search/?searchtype=author&query=Brunner%2C+H">H. Brunner</a>, <a href="/search/?searchtype=author&query=Hofmann%2C+F">F. Hofmann</a>, <a href="/search/?searchtype=author&query=Comparat%2C+J">J. Comparat</a>, <a href="/search/?searchtype=author&query=Pacaud%2C+F">F. Pacaud</a>, <a href="/search/?searchtype=author&query=K%C3%A4fer%2C+F">F. K盲fer</a>, <a href="/search/?searchtype=author&query=Reiprich%2C+T+H">T. H. Reiprich</a>, <a href="/search/?searchtype=author&query=Merloni%2C+A">A. Merloni</a>, <a href="/search/?searchtype=author&query=Schmid%2C+C">C. Schmid</a>, <a href="/search/?searchtype=author&query=Brand%2C+T">T. Brand</a>, <a href="/search/?searchtype=author&query=Wilms%2C+J">J. Wilms</a>, <a href="/search/?searchtype=author&query=Friedrich%2C+P">P. Friedrich</a>, <a href="/search/?searchtype=author&query=Finoguenov%2C+A">A. Finoguenov</a>, <a href="/search/?searchtype=author&query=Dauser%2C+T">T. Dauser</a>, <a href="/search/?searchtype=author&query=Kreykenbohm%2C+I">I. Kreykenbohm</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="1806.08652v1-abstract-short" style="display: inline;"> Studies of galaxy clusters provide stringent constraints on models of structure formation. Provided that selection effects are under control, large X-ray surveys are well suited to derive cosmological parameters, in particular those governing the dark energy equation of state. We forecast the capabilities of the all-sky eROSITA (the extended ROentgen Survey with an Imaging Telescope Array) survey… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.08652v1-abstract-full').style.display = 'inline'; document.getElementById('1806.08652v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1806.08652v1-abstract-full" style="display: none;"> Studies of galaxy clusters provide stringent constraints on models of structure formation. Provided that selection effects are under control, large X-ray surveys are well suited to derive cosmological parameters, in particular those governing the dark energy equation of state. We forecast the capabilities of the all-sky eROSITA (the extended ROentgen Survey with an Imaging Telescope Array) survey to be achieved by the early 2020s. We bring special attention to modeling the entire chain from photon emission to source detection and cataloguing. The selection function of galaxy clusters for the upcoming eROSITA mission is investigated by means of extensive and dedicated Monte-Carlo simulations. Employing a combination of accurate instrument characterization and of state-of-the-art source detection technique, we determine a cluster detection efficiency based on the cluster fluxes and sizes. Using this eROSITA cluster selection function, we find that eROSITA will detect a total of $\sim 10^5$ clusters in the extra-galactic sky. This number of clusters will allow eROSITA to put stringent constraints on cosmological models. We show that incomplete assumptions on selection effects, such as neglecting the distribution of cluster sizes, induce a bias in the derived value of cosmological parameters. Synthetic simulations of the eROSITA sky capture the essential characteristics impacting the next-generation galaxy cluster surveys and they highlight parameters requiring tight monitoring in order to avoid biases in cosmological analyses. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.08652v1-abstract-full').style.display = 'none'; document.getElementById('1806.08652v1-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 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">Accepted in A&A. Image quality degraded for arXiv submission</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 617, A92 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1709.02436">arXiv:1709.02436</a> <span> [<a href="https://arxiv.org/pdf/1709.02436">pdf</a>, <a href="https://arxiv.org/format/1709.02436">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/10.1051/0004-6361/201731128">10.1051/0004-6361/201731128 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Distant clusters of galaxies in the 2XMM/SDSS footprint: follow-up observations with the LBT </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Rabitz%2C+A">Andreas Rabitz</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">Georg Lamer</a>, <a href="/search/?searchtype=author&query=Schwope%2C+A">Axel Schwope</a>, <a href="/search/?searchtype=author&query=Takey%2C+A">Ali Takey</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1709.02436v1-abstract-short" style="display: inline;"> Context: Galaxy clusters at high redshift are important to test cosmological models and models for the growth of structure. They are difficult to find in wide-angle optical surveys, however, leaving dedicated follow-up of X-ray selected candidates as one promising identification route. Aims: We aim to increase the number of galaxy clusters beyond the SDSS-limit, z ~ 0.75. Methods: We compiled a li… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1709.02436v1-abstract-full').style.display = 'inline'; document.getElementById('1709.02436v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1709.02436v1-abstract-full" style="display: none;"> Context: Galaxy clusters at high redshift are important to test cosmological models and models for the growth of structure. They are difficult to find in wide-angle optical surveys, however, leaving dedicated follow-up of X-ray selected candidates as one promising identification route. Aims: We aim to increase the number of galaxy clusters beyond the SDSS-limit, z ~ 0.75. Methods: We compiled a list of extended X-ray sources from the 2XMMp catalogue within the footprint of the Sloan Digital Sky Survey. Fields without optical counterpart were selected for further investigation. Deep optical imaging and follow-up spectroscopy were obtained with the Large Binocular Telescope, Arizona (LBT), of those candidates not known to the literature. Results: From initially 19 candidates, selected by visually screening X-ray images of 478 XMM-Newton observations and the corresponding SDSS images, 6 clusters were found in the literature. Imaging data through r,z filters were obtained for the remaining candidates, and 7 were chosen for multi-object (MOS) spectroscopy. Spectroscopic redshifts, optical magnitudes, and X-ray parameters (flux, temperature, and luminosity) are presented for the clusters with spectroscopic redshifts. The distant clusters studied here constitute one additional redshift bin for studies of the L-T relation, which does not seem to evolve from high to low redshifts. ... <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1709.02436v1-abstract-full').style.display = 'none'; document.getElementById('1709.02436v1-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, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">This is a abridged version of the paper. The full version can be downloaded at the following URL: https://cloud.aip.de/index.php/s/2Btv7ST1KTLHfTG</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1504.07051">arXiv:1504.07051</a> <span> [<a href="https://arxiv.org/pdf/1504.07051">pdf</a>, <a href="https://arxiv.org/ps/1504.07051">ps</a>, <a href="https://arxiv.org/format/1504.07051">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </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/10.1051/0004-6361/201526416">10.1051/0004-6361/201526416 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The XMM-Newton serendipitous survey. VII. The third XMM-Newton serendipitous source catalogue </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Rosen%2C+S+R">S. R. Rosen</a>, <a href="/search/?searchtype=author&query=Webb%2C+N+A">N. A. Webb</a>, <a href="/search/?searchtype=author&query=Watson%2C+M+G">M. G. Watson</a>, <a href="/search/?searchtype=author&query=Ballet%2C+J">J. Ballet</a>, <a href="/search/?searchtype=author&query=Barret%2C+D">D. Barret</a>, <a href="/search/?searchtype=author&query=Braito%2C+V">V. Braito</a>, <a href="/search/?searchtype=author&query=Carrera%2C+F+J">F. J. Carrera</a>, <a href="/search/?searchtype=author&query=Ceballos%2C+M+T">M. T. Ceballos</a>, <a href="/search/?searchtype=author&query=Coriat%2C+M">M. Coriat</a>, <a href="/search/?searchtype=author&query=Della+Ceca%2C+R">R. Della Ceca</a>, <a href="/search/?searchtype=author&query=Denkinson%2C+G">G. Denkinson</a>, <a href="/search/?searchtype=author&query=Esquej%2C+P">P. Esquej</a>, <a href="/search/?searchtype=author&query=Farrell%2C+S+A">S. A. Farrell</a>, <a href="/search/?searchtype=author&query=Freyberg%2C+M">M. Freyberg</a>, <a href="/search/?searchtype=author&query=Gris%C3%A9%2C+F">F. Gris茅</a>, <a href="/search/?searchtype=author&query=Guillout%2C+P">P. Guillout</a>, <a href="/search/?searchtype=author&query=Heil%2C+L">L. Heil</a>, <a href="/search/?searchtype=author&query=Koliopanos%2C+F">F. Koliopanos</a>, <a href="/search/?searchtype=author&query=Law-Green%2C+D">D. Law-Green</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">G. Lamer</a>, <a href="/search/?searchtype=author&query=Lin%2C+D">D. Lin</a>, <a href="/search/?searchtype=author&query=Martino%2C+R">R. Martino</a>, <a href="/search/?searchtype=author&query=Michel%2C+L">L. Michel</a>, <a href="/search/?searchtype=author&query=Motch%2C+C">C. Motch</a>, <a href="/search/?searchtype=author&query=Gomez-Moran%2C+A+N">A. Nebot Gomez-Moran</a> , et al. (15 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="1504.07051v3-abstract-short" style="display: inline;"> Thanks to the large collecting area (3 x ~1500 cm$^2$ at 1.5 keV) and wide field of view (30' across in full field mode) of the X-ray cameras on board the European Space Agency X-ray observatory XMM-Newton, each individual pointing can result in the detection of hundreds of X-ray sources, most of which are newly discovered. Recently, many improvements in the XMM-Newton data reduction algorithms ha… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1504.07051v3-abstract-full').style.display = 'inline'; document.getElementById('1504.07051v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1504.07051v3-abstract-full" style="display: none;"> Thanks to the large collecting area (3 x ~1500 cm$^2$ at 1.5 keV) and wide field of view (30' across in full field mode) of the X-ray cameras on board the European Space Agency X-ray observatory XMM-Newton, each individual pointing can result in the detection of hundreds of X-ray sources, most of which are newly discovered. Recently, many improvements in the XMM-Newton data reduction algorithms have been made. These include enhanced source characterisation and reduced spurious source detections, refined astrometric precision, greater net sensitivity and the extraction of spectra and time series for fainter sources, with better signal-to-noise. Further, almost 50\% more observations are in the public domain compared to 2XMMi-DR3, allowing the XMM-Newton Survey Science Centre (XMM-SSC) to produce a much larger and better quality X-ray source catalogue. The XMM-SSC has developed a pipeline to reduce the XMM-Newton data automatically and using improved calibration a new catalogue version has been produced from XMM-Newton data made public by 2013 Dec. 31 (13 years of data). Manual screening ensures the highest data quality. This catalogue is known as 3XMM. In the latest release, 3XMM-DR5, there are 565962 X-ray detections comprising 396910 unique X-ray sources. For the 133000 brightest sources, spectra and lightcurves are provided. For all detections, the positions on the sky, a measure of the quality of the detection, and an evaluation of the X-ray variability is provided, along with the fluxes and count rates in 7 X-ray energy bands, the total 0.2-12 keV band counts, and four hardness ratios. To identify the detections, a cross correlation with 228 catalogues is also provided for each X-ray detection. 3XMM-DR5 is the largest X-ray source catalogue ever produced. Thanks to the large array of data products, it is an excellent resource in which to find new and extreme objects. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1504.07051v3-abstract-full').style.display = 'none'; document.getElementById('1504.07051v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 February, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 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">23 pages, version 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 590, A1 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1403.0758">arXiv:1403.0758</a> <span> [<a href="https://arxiv.org/pdf/1403.0758">pdf</a>, <a href="https://arxiv.org/ps/1403.0758">ps</a>, <a href="https://arxiv.org/format/1403.0758">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/10.1051/0004-6361/201322973">10.1051/0004-6361/201322973 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The 2XMMi/SDSS Galaxy Cluster Survey. III. Clusters associated with spectroscopically targeted luminous red galaxies in SDSS-DR10 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Takey%2C+A">A. Takey</a>, <a href="/search/?searchtype=author&query=Schwope%2C+A">A. Schwope</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">G. Lamer</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="1403.0758v1-abstract-short" style="display: inline;"> We present a sample of 383 X-ray selected galaxy groups and clusters with spectroscopic redshift measurements (up to z ~ 0.79) from the 2XMMi/SDSS Galaxy Cluster Survey. The X-ray cluster candidates were selected as serendipitously detected sources from the 2XMMi-DR3 catalogue that were located in the footprint of the Sloan Digital Sky Survey (SDSS-DR7). The cluster galaxies with available spectro… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1403.0758v1-abstract-full').style.display = 'inline'; document.getElementById('1403.0758v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1403.0758v1-abstract-full" style="display: none;"> We present a sample of 383 X-ray selected galaxy groups and clusters with spectroscopic redshift measurements (up to z ~ 0.79) from the 2XMMi/SDSS Galaxy Cluster Survey. The X-ray cluster candidates were selected as serendipitously detected sources from the 2XMMi-DR3 catalogue that were located in the footprint of the Sloan Digital Sky Survey (SDSS-DR7). The cluster galaxies with available spectroscopic redshifts were selected from the SDSS-DR10. We developed an algorithm for identifying the cluster candidates that are associated with spectroscopically targeted luminous red galaxies and for constraining the cluster spectroscopic redshift. A cross-correlation of the constructed cluster sample with published optically selected cluster catalogues yielded 264 systems with available redshifts. The present redshift measurements are consistent with the published values. The current cluster sample extends the optically confirmed cluster sample from our cluster survey by 67 objects. Moreover, it provides spectroscopic confirmation for 78 clusters among our published cluster sample, which previously had only photometric redshifts. Of the new cluster sample that comprises 67 systems, 55 objects are newly X-ray discovered clusters and 52 systems are sources newly discovered as galaxy clusters in optical and X-ray wavelengths. Based on the measured redshifts and the fluxes given in the 2XMMi-DR3 catalogue, we estimated the X-ray luminosities and masses of the cluster sample. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1403.0758v1-abstract-full').style.display = 'none'; document.getElementById('1403.0758v1-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 March, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">A&A in press, 12 pages, 15 figures, 1 table, http://www.aanda.org/index.php?option=com_article&access=doi&doi=10.1051/0004-6361/201322973</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1311.4879">arXiv:1311.4879</a> <span> [<a href="https://arxiv.org/pdf/1311.4879">pdf</a>, <a href="https://arxiv.org/ps/1311.4879">ps</a>, <a href="https://arxiv.org/format/1311.4879">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/10.1051/0004-6361/201322321">10.1051/0004-6361/201322321 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Kinematic analysis of a sample of X-ray luminous distant galaxy clusters. The $L_X$ - $蟽_v$ relation in the $z>0.6$ universe </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Nastasi%2C+A">Alessandro Nastasi</a>, <a href="/search/?searchtype=author&query=B%C3%B6hringer%2C+H">Hans B枚hringer</a>, <a href="/search/?searchtype=author&query=Fassbender%2C+R">Rene Fassbender</a>, <a href="/search/?searchtype=author&query=de+Hoon%2C+A">Arjen de Hoon</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">Georg Lamer</a>, <a href="/search/?searchtype=author&query=Mohr%2C+J+J">Joseph J. Mohr</a>, <a href="/search/?searchtype=author&query=Padilla%2C+N">Nelson Padilla</a>, <a href="/search/?searchtype=author&query=Pratt%2C+G+W">Gabriel W. Pratt</a>, <a href="/search/?searchtype=author&query=Quintana%2C+H">Hernan Quintana</a>, <a href="/search/?searchtype=author&query=Rosati%2C+P">Piero Rosati</a>, <a href="/search/?searchtype=author&query=Santos%2C+J+S">Joana S. Santos</a>, <a href="/search/?searchtype=author&query=Schwope%2C+A+D">Axel D. Schwope</a>, <a href="/search/?searchtype=author&query=%C5%A0uhada%2C+R">Robert 艩uhada</a>, <a href="/search/?searchtype=author&query=Verdugo%2C+M">Miguel Verdugo</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="1311.4879v2-abstract-short" style="display: inline;"> Observations and cosmological simulations show galaxy clusters as a family of nearly self-similar objects with properties that can be described by scaling relations as a function of e.g. mass and time. Here we study the scaling relations between the galaxy velocity dispersion and X-ray quantities like X-ray bolometric luminosity and temperature in galaxy clusters at high redshifts (0.64 $\leq$ z… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1311.4879v2-abstract-full').style.display = 'inline'; document.getElementById('1311.4879v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1311.4879v2-abstract-full" style="display: none;"> Observations and cosmological simulations show galaxy clusters as a family of nearly self-similar objects with properties that can be described by scaling relations as a function of e.g. mass and time. Here we study the scaling relations between the galaxy velocity dispersion and X-ray quantities like X-ray bolometric luminosity and temperature in galaxy clusters at high redshifts (0.64 $\leq$ z $\leq$ 1.46). We also compare our results with the similar study of the local HIFLUGCS sample. For the analysis, we use a set of 15 distant galaxy clusters extracted from the literature plus a sample of 10 newly discovered clusters selected in X-rays by the \XMM Distant Cluster Project (XDCP) with more than 10 confirmed spectroscopic members per cluster. We also study the evolution of this scaling relation by comparing the high redshift results with the data from the local HIFLUGCS sample. We also investigated the $L_X - T_X$ and the $蟽_v - T_X$ relations for the 15 clusters in the literature sample. We report the results of the X-ray and kinematic analysis of 10 newly detected high redshift clusters and provide their spectroscopic and kinematic details. For the entire, distant sample we find a slope fully consistent with the one typical of local clusters, albeit with a large associated uncertainty. The study on the evolution of the amplitude reveals a positive offset if the self-similar evolution is neglected, hence possibly indicating the need for including evolutionary effects. However, the $L_X - T_X$ relation is found to be in good agreement with the local relation without any significant redshift evolution. Finally, the $蟽_v - T_X$ relation appears to slightly deviate from the theoretical expectation that galaxies and gas particles have a similar specific kinetic energy. However, the associated uncertainty is currently too large for making any conclusive statement in this regard. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1311.4879v2-abstract-full').style.display = 'none'; document.getElementById('1311.4879v2-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, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 November, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, 20 figures, 11 tables, accepted for publication in A&A (v2: typos/language style corrections, updated references)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1308.6699">arXiv:1308.6699</a> <span> [<a href="https://arxiv.org/pdf/1308.6699">pdf</a>, <a href="https://arxiv.org/ps/1308.6699">ps</a>, <a href="https://arxiv.org/format/1308.6699">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/10.1051/0004-6361/201220213">10.1051/0004-6361/201220213 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The 2XMMi/SDSS Galaxy Cluster Survey. II. The optically confirmed cluster sample and the L_X-T relation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Takey%2C+A">A. Takey</a>, <a href="/search/?searchtype=author&query=Schwope%2C+A">A. Schwope</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">G Lamer</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="1308.6699v2-abstract-short" style="display: inline;"> We compile a sample of X-ray-selected galaxy groups and clusters from the XMM-Newton serendipitous source catalogue (2XMMi-DR3) with optical confirmation and redshift measurement from the Sloan Digital Sky Survey (SDSS). The X-ray cluster candidates were selected from the 2XMMi-DR3 catalogue in the footprint of the SDSS-DR7. We developed a finding algorithm to search for overdensities of galaxies… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1308.6699v2-abstract-full').style.display = 'inline'; document.getElementById('1308.6699v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1308.6699v2-abstract-full" style="display: none;"> We compile a sample of X-ray-selected galaxy groups and clusters from the XMM-Newton serendipitous source catalogue (2XMMi-DR3) with optical confirmation and redshift measurement from the Sloan Digital Sky Survey (SDSS). The X-ray cluster candidates were selected from the 2XMMi-DR3 catalogue in the footprint of the SDSS-DR7. We developed a finding algorithm to search for overdensities of galaxies at the positions of the X-ray cluster candidates in the photometric redshift space and to measure the redshifts of the clusters from the SDSS data. The detection algorithm provides the photometric redshift of 530 galaxy clusters. Of these, 310 clusters have a spectroscopic redshift for at least one member galaxy. About 75 percent of the optically confirmed cluster sample are newly discovered X-ray clusters. Moreover, 301 systems are known as optically selected clusters in the literature while the remainder are new discoveries in X-ray and optical bands. The optically confirmed cluster sample spans a wide redshift range 0.03-0.70 (median z=0.32). In this paper, we present the catalogue of X-ray-selected galaxy groups and clusters from the 2XMMi/SDSS galaxy cluster survey. The catalogue has two subsamples: (i) a cluster sample comprising 345 objects with their X-ray spectroscopic temperature and flux from the spectral fitting, and (ii) a cluster sample consisting of 185 systems with their X-ray flux from the 2XMMi-DR3 catalogue, because their X-ray data are insufficient for spectral fitting. The updated L_X-T relation of the current sample with X-ray spectroscopic parameters is presented. We see no evidence for evolution in the slope and intrinsic scatter of the L_X-T relation with redshift when excluding the low-luminosity groups. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1308.6699v2-abstract-full').style.display = 'none'; document.getElementById('1308.6699v2-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 October, 2013; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 August, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2013. </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">A&A in press, 18 pages, 25 figures, 3 tables (revised version after language editing)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1306.2319">arXiv:1306.2319</a> <span> [<a href="https://arxiv.org/pdf/1306.2319">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> The Hot and Energetic Universe: The evolution of galaxy groups and clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Pointecouteau%2C+E">E. Pointecouteau</a>, <a href="/search/?searchtype=author&query=Reiprich%2C+T+H">T. H. Reiprich</a>, <a href="/search/?searchtype=author&query=Adami%2C+C">C. Adami</a>, <a href="/search/?searchtype=author&query=Arnaud%2C+M">M. Arnaud</a>, <a href="/search/?searchtype=author&query=Biffi%2C+V">V. Biffi</a>, <a href="/search/?searchtype=author&query=Borgani%2C+S">S. Borgani</a>, <a href="/search/?searchtype=author&query=Borm%2C+K">K. Borm</a>, <a href="/search/?searchtype=author&query=Bourdin%2C+H">H. Bourdin</a>, <a href="/search/?searchtype=author&query=Brueggen%2C+M">M. Brueggen</a>, <a href="/search/?searchtype=author&query=Bulbul%2C+E">E. Bulbul</a>, <a href="/search/?searchtype=author&query=Clerc%2C+N">N. Clerc</a>, <a href="/search/?searchtype=author&query=Croston%2C+J+H">J. H. Croston</a>, <a href="/search/?searchtype=author&query=Dolag%2C+K">K. Dolag</a>, <a href="/search/?searchtype=author&query=Ettori%2C+S">S. Ettori</a>, <a href="/search/?searchtype=author&query=Finoguenov%2C+A">A. Finoguenov</a>, <a href="/search/?searchtype=author&query=Kaastra%2C+J">J. Kaastra</a>, <a href="/search/?searchtype=author&query=Lovisari%2C+L">L. Lovisari</a>, <a href="/search/?searchtype=author&query=Maughan%2C+B">B. Maughan</a>, <a href="/search/?searchtype=author&query=Mazzotta%2C+P">P. Mazzotta</a>, <a href="/search/?searchtype=author&query=Pacaud%2C+F">F. Pacaud</a>, <a href="/search/?searchtype=author&query=de+Plaa%2C+J">J. de Plaa</a>, <a href="/search/?searchtype=author&query=Pratt%2C+G+W">G. W. Pratt</a>, <a href="/search/?searchtype=author&query=Ramos-Ceja%2C+M">M. Ramos-Ceja</a>, <a href="/search/?searchtype=author&query=Rasia%2C+E">E. Rasia</a>, <a href="/search/?searchtype=author&query=Sanders%2C+J">J. Sanders</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="1306.2319v1-abstract-short" style="display: inline;"> Major astrophysical questions related to the formation and evolution of structures, and more specifically of galaxy groups and clusters, will still be open in the coming decade and beyond: what is the interplay of galaxy, supermassive black hole, and intergalactic gas evolution in the most massive objects in the Universe - galaxy groups and clusters? What are the processes driving the evolution of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1306.2319v1-abstract-full').style.display = 'inline'; document.getElementById('1306.2319v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1306.2319v1-abstract-full" style="display: none;"> Major astrophysical questions related to the formation and evolution of structures, and more specifically of galaxy groups and clusters, will still be open in the coming decade and beyond: what is the interplay of galaxy, supermassive black hole, and intergalactic gas evolution in the most massive objects in the Universe - galaxy groups and clusters? What are the processes driving the evolution of chemical enrichment of the hot diffuse gas in large-scale structures? How and when did the first galaxy groups in the Universe, massive enough to bind more than 10^7 K gas, form? Focussing on the period when groups and clusters assembled (0.5<z<2.5), we show that, due to the continuum and line emission of this hot intergalactic gas at X-ray wavelengths, Athena+, combining high sensitivity with excellent spectral and spatial resolution, will deliver breakthrough observations in view of the aforementioned issues. Indeed, the physical and chemical properties of the hot intra-cluster gas, and their evolution across time, are a key to understand the co-evolution of galaxy and supermassive black hole within their environments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1306.2319v1-abstract-full').style.display = 'none'; document.getElementById('1306.2319v1-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 June, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2013. </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">Supporting paper for the science theme The Hot and Energetic Universe to be implemented by the Athena+ X-ray observatory (http://www.the-athena-x-ray-observatory.eu). 10 pages, 4 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/1302.5329">arXiv:1302.5329</a> <span> [<a href="https://arxiv.org/pdf/1302.5329">pdf</a>, <a href="https://arxiv.org/ps/1302.5329">ps</a>, <a href="https://arxiv.org/format/1302.5329">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/10.1051/0004-6361/201218832">10.1051/0004-6361/201218832 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The XMM-Newton Wide Angle Survey (XWAS) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Esquej%2C+P">P. Esquej</a>, <a href="/search/?searchtype=author&query=Page%2C+M">M. Page</a>, <a href="/search/?searchtype=author&query=Carrera%2C+F+J">F. J. Carrera</a>, <a href="/search/?searchtype=author&query=Mateos%2C+S">S. Mateos</a>, <a href="/search/?searchtype=author&query=Tedds%2C+J">J. Tedds</a>, <a href="/search/?searchtype=author&query=Watson%2C+M+G">M. G. Watson</a>, <a href="/search/?searchtype=author&query=Corral%2C+A">A. Corral</a>, <a href="/search/?searchtype=author&query=Ebrero%2C+J">J. Ebrero</a>, <a href="/search/?searchtype=author&query=Krumpe%2C+M">M. Krumpe</a>, <a href="/search/?searchtype=author&query=Rosen%2C+S+R">S. R. Rosen</a>, <a href="/search/?searchtype=author&query=Ceballos%2C+M+T">M. T. Ceballos</a>, <a href="/search/?searchtype=author&query=Schwope%2C+A">A. Schwope</a>, <a href="/search/?searchtype=author&query=Page%2C+C">C. Page</a>, <a href="/search/?searchtype=author&query=Alonso-Herrero%2C+A">A. Alonso-Herrero</a>, <a href="/search/?searchtype=author&query=Caccianiga%2C+A">A. Caccianiga</a>, <a href="/search/?searchtype=author&query=Della+Ceca%2C+R">R. Della Ceca</a>, <a href="/search/?searchtype=author&query=Gonzalez-Mart%C3%ADn%2C+O">O. Gonzalez-Mart铆n</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">G. Lamer</a>, <a href="/search/?searchtype=author&query=Severgnini%2C+P">P. Severgnini</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="1302.5329v1-abstract-short" style="display: inline;"> This programme is aimed at obtaining one of the largest X-ray selected samples of identified active galactic nuclei to date in order to characterise such a population at intermediate fluxes, where most of the Universe's accretion power originates. We present the XMM-Newton Wide Angle Survey (XWAS), a new catalogue of almost a thousand X-ray sources spectroscopically identified through optical obse… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1302.5329v1-abstract-full').style.display = 'inline'; document.getElementById('1302.5329v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1302.5329v1-abstract-full" style="display: none;"> This programme is aimed at obtaining one of the largest X-ray selected samples of identified active galactic nuclei to date in order to characterise such a population at intermediate fluxes, where most of the Universe's accretion power originates. We present the XMM-Newton Wide Angle Survey (XWAS), a new catalogue of almost a thousand X-ray sources spectroscopically identified through optical observations. A sample of X-ray sources detected in 68 XMM-Newton pointed observations was selected for optical multi-fibre spectroscopy. Optical counterparts and corresponding photometry of the X-ray sources were obtained from the SuperCOSMOS Sky Survey. Candidates for spectroscopy were initially selected with magnitudes down to R~21, with preference for X-ray sources having a flux F(0.5-4.5 keV) >10^-14 erg s^-1 cm^-2. Optical spectroscopic observations performed at the Anglo Australian Telescope Two Degree Field were analysed, and the derived spectra were classified based on optical emission lines. We have identified through optical spectroscopy 940 X-ray sources over ~11.8 deg^2 of the sky. Source populations in our sample can be summarised as 65% broad line active galactic nuclei (BLAGN), 16% narrow emission line galaxies (NELGs), 6% absorption line galaxies (ALGs) and 13% stars. An active nucleus is likely to be present also in the large majority of the X-ray sources spectroscopically classified as NELGs or ALGs. Sources lie in high-galactic latitude (|b| > 20 deg) XMM-Newton fields mainly in the southern hemisphere. Due to the large parameter space in redshift (0 < z < 4.25) and flux (10^-15 < F(0.5-4.5 keV) < 10^-12 erg s^-1 cm^-2) covered by the XWAS this work provides an excellent resource to further study subsamples and particular cases. The overall properties of the extragalactic objects are presented in this paper. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1302.5329v1-abstract-full').style.display = 'none'; document.getElementById('1302.5329v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 February, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A, 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/1301.3506">arXiv:1301.3506</a> <span> [<a href="https://arxiv.org/pdf/1301.3506">pdf</a>, <a href="https://arxiv.org/ps/1301.3506">ps</a>, <a href="https://arxiv.org/format/1301.3506">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</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/10.1051/0004-6361/201220389">10.1051/0004-6361/201220389 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Distant galaxy clusters in a deep XMM-Newton field within the CFTHLS D4 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=de+Hoon%2C+A">Arjen de Hoon</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">Georg Lamer</a>, <a href="/search/?searchtype=author&query=Schwope%2C+A">Axel Schwope</a>, <a href="/search/?searchtype=author&query=Muehlegger%2C+M">Martin Muehlegger</a>, <a href="/search/?searchtype=author&query=Fassbender%2C+R">Rene Fassbender</a>, <a href="/search/?searchtype=author&query=Boeohringer%2C+H">Hans Boeohringer</a>, <a href="/search/?searchtype=author&query=Lerchster%2C+M">Mike Lerchster</a>, <a href="/search/?searchtype=author&query=Nastasi%2C+A">Alessandro Nastasi</a>, <a href="/search/?searchtype=author&query=Suhada%2C+R">Robert Suhada</a>, <a href="/search/?searchtype=author&query=Verdugo%2C+M">Miguel Verdugo</a>, <a href="/search/?searchtype=author&query=Dietrich%2C+J+P">Joerg P. Dietrich</a>, <a href="/search/?searchtype=author&query=Brimioulle%2C+F">Fabrice Brimioulle</a>, <a href="/search/?searchtype=author&query=Rosati%2C+P">Piero Rosati</a>, <a href="/search/?searchtype=author&query=Pierini%2C+D">Daniele Pierini</a>, <a href="/search/?searchtype=author&query=Santos%2C+J">Joana Santos</a>, <a href="/search/?searchtype=author&query=Quintana%2C+H">Hernan Quintana</a>, <a href="/search/?searchtype=author&query=Rabitz%2C+A">Andrea Rabitz</a>, <a href="/search/?searchtype=author&query=Takey%2C+A">Ali Takey</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="1301.3506v1-abstract-short" style="display: inline;"> The XMM-Newton Distant Cluster Project (XDCP) aims at the identification of a well defined sample of X-ray selected clusters of galaxies at redshifts z>0.8. We present a catalogue of the extended sources in one the deepest ~250 ksec XMM-Newton fields targeting LBQS 2215-175 covering the CFHTLS deep field four. The cluster identification is based, among others, on deep imaging with the ESO VLT and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1301.3506v1-abstract-full').style.display = 'inline'; document.getElementById('1301.3506v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1301.3506v1-abstract-full" style="display: none;"> The XMM-Newton Distant Cluster Project (XDCP) aims at the identification of a well defined sample of X-ray selected clusters of galaxies at redshifts z>0.8. We present a catalogue of the extended sources in one the deepest ~250 ksec XMM-Newton fields targeting LBQS 2215-175 covering the CFHTLS deep field four. The cluster identification is based, among others, on deep imaging with the ESO VLT and from the CFHT legacy survey. The confirmation of cluster candidates is done by VLT/FORS2 multi-object spectroscopy. Photometric redshifts from the CFHTLS D4 are utilized to confirm the effectiveness of the X-ray cluster selection method. The survey sensitivity is computed with extensive simulations. At a flux limit of S(0.5-2.0 keV) ~ 2.5e-15 erg/s we achieve a completeness level higher than 50% in an area of ~0.13 square degrees. We detect six galaxy clusters above this limit with optical counterparts, of which 5 are new spectroscopic discoveries. Two newly discovered X-ray luminous galaxy clusters are at z>1.0, another two at z=0.41 and one at z=0.34. For the most distant X-ray selected cluster in this field at z=1.45 we find additional (active) member galaxies from both X-ray and spectroscopic data. Additionally, we find evidence of large scale structures at moderate redshifts of z=0.41 and z=0.34. The quest for distant clusters in archival XMM-Newton data has led to the detection of six clusters in a single field, making XMM-Newton an outstanding tool for cluster surveys. Three of these clusters are at z>1, which emphasises the valuable contribution of small, yet deep surveys to cosmology. Beta-models are appropriate descriptions for the cluster surface brightness to perform cluster detection simulations in order to compute the X-ray selection function. The constructed logN-logS tends to favour a scenario where no evolution in the cluster X-ray luminosity function (XLF) takes place. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1301.3506v1-abstract-full').style.display = 'none'; document.getElementById('1301.3506v1-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 January, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2013. </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">Some figures are available in full resolution only in the printed A&A version of the document</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1206.6885">arXiv:1206.6885</a> <span> [<a href="https://arxiv.org/pdf/1206.6885">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <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="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1117/12.926239">10.1117/12.926239 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> 4MOST - 4-metre Multi-Object Spectroscopic Telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=de+Jong%2C+R+S">Roelof S. de Jong</a>, <a href="/search/?searchtype=author&query=Bellido-Tirado%2C+O">Olga Bellido-Tirado</a>, <a href="/search/?searchtype=author&query=Chiappini%2C+C">Cristina Chiappini</a>, <a href="/search/?searchtype=author&query=Depagne%2C+%C3%89">脡ric Depagne</a>, <a href="/search/?searchtype=author&query=Haynes%2C+R">Roger Haynes</a>, <a href="/search/?searchtype=author&query=Johl%2C+D">Diane Johl</a>, <a href="/search/?searchtype=author&query=Schnurr%2C+O">Olivier Schnurr</a>, <a href="/search/?searchtype=author&query=Schwope%2C+A">Axel Schwope</a>, <a href="/search/?searchtype=author&query=Walcher%2C+J">Jakob Walcher</a>, <a href="/search/?searchtype=author&query=Dionies%2C+F">Frank Dionies</a>, <a href="/search/?searchtype=author&query=Haynes%2C+D">Dionne Haynes</a>, <a href="/search/?searchtype=author&query=Kelz%2C+A">Andreas Kelz</a>, <a href="/search/?searchtype=author&query=Kitaura%2C+F+S">Francisco S. Kitaura</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">Georg Lamer</a>, <a href="/search/?searchtype=author&query=Minchev%2C+I">Ivan Minchev</a>, <a href="/search/?searchtype=author&query=M%C3%BCller%2C+V">Volker M眉ller</a>, <a href="/search/?searchtype=author&query=Nuza%2C+S+E">Sebasti谩n E. Nuza</a>, <a href="/search/?searchtype=author&query=Olaya%2C+J">Jean-Christophe Olaya</a>, <a href="/search/?searchtype=author&query=Piffl%2C+T">Tilmann Piffl</a>, <a href="/search/?searchtype=author&query=Popow%2C+E">Emil Popow</a>, <a href="/search/?searchtype=author&query=Steinmetz%2C+M">Matthias Steinmetz</a>, <a href="/search/?searchtype=author&query=Ural%2C+U">U臒ur Ural</a>, <a href="/search/?searchtype=author&query=Williams%2C+M">Mary Williams</a>, <a href="/search/?searchtype=author&query=Winkler%2C+R">Roland Winkler</a>, <a href="/search/?searchtype=author&query=Wisotzki%2C+L">Lutz Wisotzki</a> , et al. (60 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="1206.6885v1-abstract-short" style="display: inline;"> The 4MOST consortium is currently halfway through a Conceptual Design study for ESO with the aim to develop a wide-field (>3 square degree, goal >5 square degree), high-multiplex (>1500 fibres, goal 3000 fibres) spectroscopic survey facility for an ESO 4m-class telescope (VISTA). 4MOST will run permanently on the telescope to perform a 5 year public survey yielding more than 20 million spectra at… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1206.6885v1-abstract-full').style.display = 'inline'; document.getElementById('1206.6885v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1206.6885v1-abstract-full" style="display: none;"> The 4MOST consortium is currently halfway through a Conceptual Design study for ESO with the aim to develop a wide-field (>3 square degree, goal >5 square degree), high-multiplex (>1500 fibres, goal 3000 fibres) spectroscopic survey facility for an ESO 4m-class telescope (VISTA). 4MOST will run permanently on the telescope to perform a 5 year public survey yielding more than 20 million spectra at resolution R~5000 (位=390-1000 nm) and more than 2 million spectra at R~20,000 (395-456.5 nm & 587-673 nm). The 4MOST design is especially intended to complement three key all-sky, space-based observatories of prime European interest: Gaia, eROSITA and Euclid. Initial design and performance estimates for the wide-field corrector concepts are presented. We consider two fibre positioner concepts, a well-known Phi-Theta system and a new R-Theta concept with a large patrol area. The spectrographs are fixed configuration two-arm spectrographs, with dedicated spectrographs for the high- and low-resolution. A full facility simulator is being developed to guide trade-off decisions regarding the optimal field-of-view, number of fibres needed, and the relative fraction of high-to-low resolution fibres. Mock catalogues with template spectra from seven Design Reference Surveys are simulated to verify the science requirements of 4MOST. The 4MOST consortium aims to deliver the full 4MOST facility by the end of 2018 and start delivering high-level data products for both consortium and ESO community targets a year later with yearly increments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1206.6885v1-abstract-full').style.display = 'none'; document.getElementById('1206.6885v1-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 June, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2012. </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">To appear in the proceedings of the SPIE Astronomical Instrumentation + Telescopes conference, Amsterdam, 2012. 15 pages, 16 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/1201.1925">arXiv:1201.1925</a> <span> [<a href="https://arxiv.org/pdf/1201.1925">pdf</a>, <a href="https://arxiv.org/ps/1201.1925">ps</a>, <a href="https://arxiv.org/format/1201.1925">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/10.1051/0004-6361/201116674">10.1051/0004-6361/201116674 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First simultaneous optical/near-infrared imaging of an X-ray selected, high-redshift cluster of galaxies with GROND: the galaxy population of XMMU J0338.7+0030 at z=1.1 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Pierini%2C+D">D. Pierini</a>, <a href="/search/?searchtype=author&query=Suhada%2C+R">R. Suhada</a>, <a href="/search/?searchtype=author&query=Fassbender%2C+R">R. Fassbender</a>, <a href="/search/?searchtype=author&query=Nastasi%2C+A">A. Nastasi</a>, <a href="/search/?searchtype=author&query=Boehringer%2C+H">H. Boehringer</a>, <a href="/search/?searchtype=author&query=Salvato%2C+M">M. Salvato</a>, <a href="/search/?searchtype=author&query=Pratt%2C+G+W">G. W. Pratt</a>, <a href="/search/?searchtype=author&query=Lerchster%2C+M">M. Lerchster</a>, <a href="/search/?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/?searchtype=author&query=Santos%2C+J+S">J. S. Santos</a>, <a href="/search/?searchtype=author&query=de+Hoon%2C+A">A. de Hoon</a>, <a href="/search/?searchtype=author&query=Kohnert%2C+J">J. Kohnert</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">G. Lamer</a>, <a href="/search/?searchtype=author&query=Mohr%2C+J+J">J. J. Mohr</a>, <a href="/search/?searchtype=author&query=Muehlegger%2C+M">M. Muehlegger</a>, <a href="/search/?searchtype=author&query=Quintana%2C+H">H. Quintana</a>, <a href="/search/?searchtype=author&query=Schwope%2C+A">A. Schwope</a>, <a href="/search/?searchtype=author&query=Biffi%2C+V">V. Biffi</a>, <a href="/search/?searchtype=author&query=Chon%2C+G">G. Chon</a>, <a href="/search/?searchtype=author&query=Giodini%2C+S">S. Giodini</a>, <a href="/search/?searchtype=author&query=Koppenhoefer%2C+J">J. Koppenhoefer</a>, <a href="/search/?searchtype=author&query=Verdugo%2C+M">M. Verdugo</a>, <a href="/search/?searchtype=author&query=Ziparo%2C+F">F. Ziparo</a>, <a href="/search/?searchtype=author&query=Afonso%2C+P+M+J">P. M. J. Afonso</a>, <a href="/search/?searchtype=author&query=Clemens%2C+C">C. Clemens</a> , et al. (6 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="1201.1925v1-abstract-short" style="display: inline;"> The XMM-Newton Distant Cluster Project is a serendipitous survey for clusters of galaxies at redshifts z>=0.8 based on deep archival XMM-Newton observations. ... Low-significance candidate high-z clusters are followed up with the seven-channel imager GROND (Gamma-Ray Burst Optical and Near-Infrared Detector) that is mounted at a 2m-class telescope. ... The test case is XMMU J0338.7+0030, suggested… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1201.1925v1-abstract-full').style.display = 'inline'; document.getElementById('1201.1925v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1201.1925v1-abstract-full" style="display: none;"> The XMM-Newton Distant Cluster Project is a serendipitous survey for clusters of galaxies at redshifts z>=0.8 based on deep archival XMM-Newton observations. ... Low-significance candidate high-z clusters are followed up with the seven-channel imager GROND (Gamma-Ray Burst Optical and Near-Infrared Detector) that is mounted at a 2m-class telescope. ... The test case is XMMU J0338.7+0030, suggested to be at z~1.45+/-0.15 from the analysis of the z-H vs H colour-magnitude diagram obtained from the follow-up imaging. Later VLT-FORS2 spectroscopy enabled us to identify four members, which set this cluster at z=1.097+/-0.002. To reach a better knowledge of its galaxy population, we observed XMMU J0338.7+0030 with GROND for about 6 hr. The publicly available photo-z code le Phare was used. The Ks-band number counts of the non-stellar sources out of the 832 detected down to z'~26 AB-mag in the 3.9x4.3 square arcmin region of XMMU J0338.7+0030 imaged at all GROND bands clearly exceed those computed in deep fields/survey areas at ~20.5 - 22.5 AB-mag. The photo-z's of the three imaged spectroscopic members yield z=1.12+/-0.09. The spatial distribution and the properties of the GROND sources with a photo-z in the range 1.01 - 1.23 confirm the correspondence of the X-ray source with a galaxy over-density at a significance of at least 4.3 sigma. Candidate members that are spectro-photometrically classified as elliptical galaxies define a red locus in the i'-z' vs z' colour-magnitude diagram that is consistent with the red sequence of the cluster RDCS J0910+5422 at z=1.106. XMMU J0338.7+0030 hosts also a population of bluer late-type spirals and irregulars. The starbursts among the photometric members populate both loci, consistently with previous results. The analysis of the available data set indicates that XMMU J0338.7+0030 is a low-mass cluster (M_200 ~ 1E14 M_sun) at z=1.1. (Abridged) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1201.1925v1-abstract-full').style.display = 'none'; document.getElementById('1201.1925v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 January, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2012. </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 Astronomy & Astrophysics Main Journal, 27 pages, 24 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/1111.0009">arXiv:1111.0009</a> <span> [<a href="https://arxiv.org/pdf/1111.0009">pdf</a>, <a href="https://arxiv.org/ps/1111.0009">ps</a>, <a href="https://arxiv.org/format/1111.0009">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/10.1088/1367-2630/13/12/125014">10.1088/1367-2630/13/12/125014 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The X-ray luminous galaxy cluster population at 0.9<z<~1.6 as revealed by the XMM-Newton Distant Cluster Project </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Fassbender%2C+R">R. Fassbender</a>, <a href="/search/?searchtype=author&query=Boehringer%2C+H">H. Boehringer</a>, <a href="/search/?searchtype=author&query=Nastasi%2C+A">A. Nastasi</a>, <a href="/search/?searchtype=author&query=Suhada%2C+R">R. Suhada</a>, <a href="/search/?searchtype=author&query=Muehlegger%2C+M">M. Muehlegger</a>, <a href="/search/?searchtype=author&query=de+Hoon%2C+A">A. de Hoon</a>, <a href="/search/?searchtype=author&query=Kohnert%2C+J">J. Kohnert</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">G. Lamer</a>, <a href="/search/?searchtype=author&query=Mohr%2C+J+J">J. J. Mohr</a>, <a href="/search/?searchtype=author&query=Pierini%2C+D">D. Pierini</a>, <a href="/search/?searchtype=author&query=Pratt%2C+G+W">G. W. Pratt</a>, <a href="/search/?searchtype=author&query=Quintana%2C+H">H. Quintana</a>, <a href="/search/?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/?searchtype=author&query=Santos%2C+J+S">J. S. Santos</a>, <a href="/search/?searchtype=author&query=Schwope%2C+A+D">A. D. Schwope</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="1111.0009v1-abstract-short" style="display: inline;"> We present the largest sample of spectroscopically confirmed X-ray luminous high-redshift galaxy clusters to date comprising 22 systems in the range 0.9<z<\sim1.6 as part of the XMM-Newton Distant Cluster Project (XDCP). All systems were initially selected as extended X-ray sources over 76.1 deg^2 of non-contiguous deep archival XMM-Newton coverage. We test and calibrate the most promising two-ban… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1111.0009v1-abstract-full').style.display = 'inline'; document.getElementById('1111.0009v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1111.0009v1-abstract-full" style="display: none;"> We present the largest sample of spectroscopically confirmed X-ray luminous high-redshift galaxy clusters to date comprising 22 systems in the range 0.9<z<\sim1.6 as part of the XMM-Newton Distant Cluster Project (XDCP). All systems were initially selected as extended X-ray sources over 76.1 deg^2 of non-contiguous deep archival XMM-Newton coverage. We test and calibrate the most promising two-band redshift estimation techniques based on the R-z and z-H colors for efficient distant cluster identifications and find a good redshift accuracy performance of the z-H color out to at least z\sim1.5, while the redshift evolution of the R-z color leads to increasingly large uncertainties at z>\sim0.9. We present first details of two newly identified clusters, XDCP J0338.5+0029 at z=0.916 and XDCP J0027.2+1714 at z=0.959, and investigate the Xray properties of SpARCS J003550-431224 at z=1.335, which shows evidence for ongoing major merger activity along the line-of-sight. We provide X-ray properties and luminosity-based total mass estimates for the full sample, which has a median system mass of M200\simeq2\times10^14M\odot. In contrast to local clusters, the z>0.9 systems do mostly not harbor central dominant galaxies coincident with the X-ray centroid position, but rather exhibit significant BCG offsets from the X-ray center with a median value of about 50 kpc in projection and a smaller median luminosity gap to the second-ranked galaxy of \sim0.3mag. We estimate a fraction of cluster-associated NVSS 1.4GHz radio sources of about 30%, preferentially located within 1' from the X-ray center. The galaxy populations in z>\sim1.5 cluster environments show first evidence for drastic changes on the high-mass end of galaxies and signs for a gradual disappearance of a well-defined cluster red-sequence as strong star formation activity is observed in an increasing fraction of massive galaxies down to the densest core regions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1111.0009v1-abstract-full').style.display = 'none'; document.getElementById('1111.0009v1-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 October, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2011. </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">61 pages, 13 color figures, accepted for publication in New Journal of Physics for the focus issue on 'Galaxy Clusters'</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> New Journal of Physics, Volume 13, Issue 12, pp. 125014 (2011) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1109.1743">arXiv:1109.1743</a> <span> [<a href="https://arxiv.org/pdf/1109.1743">pdf</a>, <a href="https://arxiv.org/format/1109.1743">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/10.1051/0004-6361/201117498">10.1051/0004-6361/201117498 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The 2XMMi/SDSS Galaxy Cluster Survey I. The first cluster sample and X-ray luminosity-temperature relation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Takey%2C+A">A. Takey</a>, <a href="/search/?searchtype=author&query=Schwope%2C+A">A. Schwope</a>, <a href="/search/?searchtype=author&query=Lamer%2C+G">G. Lamer</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="1109.1743v1-abstract-short" style="display: inline;"> We present a catalogue of X-ray selected galaxy clusters and groups as a first release of the 2XMMi/SDSS Galaxy Cluster Survey. The survey is a search for galaxy clusters detected serendipitously in observations with XMM-Newton in the footprint of the Sloan Digital Sky Survey (SDSS). The main aims of the survey are to identify new X-ray galaxy clusters, investigate their X-ray scaling relations, i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1109.1743v1-abstract-full').style.display = 'inline'; document.getElementById('1109.1743v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1109.1743v1-abstract-full" style="display: none;"> We present a catalogue of X-ray selected galaxy clusters and groups as a first release of the 2XMMi/SDSS Galaxy Cluster Survey. The survey is a search for galaxy clusters detected serendipitously in observations with XMM-Newton in the footprint of the Sloan Digital Sky Survey (SDSS). The main aims of the survey are to identify new X-ray galaxy clusters, investigate their X-ray scaling relations, identify distant cluster candidates and study the correlation of the X-ray and optical properties. In this paper we describe the basic strategy to identify and characterize the X-ray cluster candidates that currently comprise 1180 objects selected from the second XMM-Newton serendipitous source catalogue (2XMMi-DR3). Cross-correlation of the initial catalogue with recently published optically selected SDSS galaxy cluster catalogues yields photometric redshifts for 275 objects. Of these, 182 clusters have at least one member with a spectroscopic redshift from existing public data (SDSS-DR8). Here we present the X-ray properties of the first cluster sample which comprises 175 clusters, among which 139 objects are new X-ray discoveries while the others were previously known as X-ray sources. The first cluster sample from the survey covers a wide range of redshifts from 0.09 to 0.61, bolometric luminosities L_500 = 1.9 x 10^42 - 1.2 x 10^45 erg/s, and masses M_500 = 2.3 x 10^13 - 4.9 x 10^14 Msun. We extend the relation between the X-ray bolometric luminosity L_500 and the X-ray temperature towards significantly lower T and L and still find that the slope of the linear L-T relation is consistent with values published for high luminosities. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1109.1743v1-abstract-full').style.display = 'none'; document.getElementById('1109.1743v1-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 September, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2011. </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">A&A accepted, 14 pages, 17 figures, 2 tables. The first cluster catalogue with the X-ray-optical overlay and fitted spectra for each cluster is publicly available from http://www.aip.de/groups/xray/XMM_SDSS_CLUSTERS</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=Lamer%2C+G&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Lamer%2C+G&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Lamer%2C+G&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> </ul> </nav> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> 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