[{"oa":1,"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1906.06347"}],"publication_status":"published","volume":880,"issue":"1","article_processing_charge":"No","arxiv":1,"abstract":[{"lang":"eng","text":"The well-known quasar SDSS J095253.83+011421.9 (J0952+0114) at z = 3.02 has one of the most peculiar spectra discovered so far, showing the presence of narrow Lyα and broad metal emission lines. Although recent studies have suggested that a proximate damped Lyα absorption (PDLA) system causes this peculiar spectrum, the origin of the gas associated with the PDLA is unknown. Here we report the results of observations with the Multi Unit Spectroscopic Explorer (MUSE) that reveal a new giant (≈100 physical kpc) Lyα nebula. The detailed analysis of the Lyα velocity, velocity dispersion, and surface brightness profiles suggests that the J0952+0114 Lyα nebula shares similar properties with other QSO nebulae previously detected with MUSE, implying that the PDLA in J0952+0144 is covering only a small fraction of the solid angle of the QSO emission. We also detected bright and spectrally narrow C iv λ1550 and He ii λ1640 extended emission around J0952+0114 with velocity centroids similar to the peak of the extended and central narrow Lyα emission. The presence of a peculiarly bright, unresolved, and relatively broad He ii λ1640 emission in the central region at exactly the same PDLA redshift hints at the possibility that the PDLA originates in a clumpy outflow with a bulk velocity of about 500 km s−1. The smaller velocity dispersion of the large-scale Lyα emission suggests that the high-speed outflow is confined to the central region. Lastly, the derived spatially resolved He ii/Lyα and C iv/Lyα maps show a positive gradient with the distance to the QSO, hinting at a non-homogeneous distribution of the ionization parameter."}],"_id":"11516","date_published":"2019-07-24T00:00:00Z","article_number":"47","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"date_updated":"2022-08-18T10:20:18Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","external_id":{"arxiv":["1906.06347"]},"scopus_import":"1","year":"2019","oa_version":"Preprint","article_type":"original","publisher":"IOP Publishing","intvolume":"       880","status":"public","quality_controlled":"1","publication":"The Astrophysical Journal","date_created":"2022-07-06T13:50:33Z","extern":"1","month":"07","acknowledgement":"We thank Lutz Wisotzki for stimulating discussions. This work is based on observations taken at ESO/VLT in Paranal and we would like to thank the ESO staff for their assistance and support during the MUSE GTO campaigns. This work was supported by the Swiss National Science Foundation. This research made use of Astropy, a community-developed core PYTHON package for astronomy (Astropy Collaboration et al. 2013), NumPy and SciPy (Oliphant 2007), Matplotlib (Hunter 2007), IPython (Perez & Granger 2007), and of the NASA Astrophysics Data System Bibliographic Services. S.C. and G.P. gratefully acknowledge support from Swiss National Science Foundation grant PP00P2−163824. A.F. acknowledges support from the ERC via Advanced Grant under grants agreement no. 339659-MUSICOS. J.B. acknowledges support by FCT/MCTES through national funds by grant UID/FIS/04434/2019 and through Investigador FCT Contract No. IF/01654/2014/CP1215/CT0003. S.D.J. is supported by a NASA Hubble Fellowship (HST-HF2-51375.001-A). T.N. acknowledges the Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO) top grant TOP1.16.057.","doi":"10.3847/1538-4357/ab2881","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"title":"A giant Lyα nebula and a small-scale clumpy outflow in the system of the exotic quasar J0952+0114 unveiled by MUSE","citation":{"short":"R.A. Marino, S. Cantalupo, G. Pezzulli, S.J. Lilly, S. Gallego, R. Mackenzie, J.J. Matthee, J. Brinchmann, N. Bouché, A. Feltre, S. Muzahid, I. Schroetter, S.D. Johnson, T. Nanayakkara, The Astrophysical Journal 880 (2019).","apa":"Marino, R. A., Cantalupo, S., Pezzulli, G., Lilly, S. J., Gallego, S., Mackenzie, R., … Nanayakkara, T. (2019). A giant Lyα nebula and a small-scale clumpy outflow in the system of the exotic quasar J0952+0114 unveiled by MUSE. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ab2881\">https://doi.org/10.3847/1538-4357/ab2881</a>","ama":"Marino RA, Cantalupo S, Pezzulli G, et al. A giant Lyα nebula and a small-scale clumpy outflow in the system of the exotic quasar J0952+0114 unveiled by MUSE. <i>The Astrophysical Journal</i>. 2019;880(1). doi:<a href=\"https://doi.org/10.3847/1538-4357/ab2881\">10.3847/1538-4357/ab2881</a>","ista":"Marino RA, Cantalupo S, Pezzulli G, Lilly SJ, Gallego S, Mackenzie R, Matthee JJ, Brinchmann J, Bouché N, Feltre A, Muzahid S, Schroetter I, Johnson SD, Nanayakkara T. 2019. A giant Lyα nebula and a small-scale clumpy outflow in the system of the exotic quasar J0952+0114 unveiled by MUSE. The Astrophysical Journal. 880(1), 47.","ieee":"R. A. Marino <i>et al.</i>, “A giant Lyα nebula and a small-scale clumpy outflow in the system of the exotic quasar J0952+0114 unveiled by MUSE,” <i>The Astrophysical Journal</i>, vol. 880, no. 1. IOP Publishing, 2019.","chicago":"Marino, Raffaella Anna, Sebastiano Cantalupo, Gabriele Pezzulli, Simon J. Lilly, Sofia Gallego, Ruari Mackenzie, Jorryt J Matthee, et al. “A Giant Lyα Nebula and a Small-Scale Clumpy Outflow in the System of the Exotic Quasar J0952+0114 Unveiled by MUSE.” <i>The Astrophysical Journal</i>. IOP Publishing, 2019. <a href=\"https://doi.org/10.3847/1538-4357/ab2881\">https://doi.org/10.3847/1538-4357/ab2881</a>.","mla":"Marino, Raffaella Anna, et al. “A Giant Lyα Nebula and a Small-Scale Clumpy Outflow in the System of the Exotic Quasar J0952+0114 Unveiled by MUSE.” <i>The Astrophysical Journal</i>, vol. 880, no. 1, 47, IOP Publishing, 2019, doi:<a href=\"https://doi.org/10.3847/1538-4357/ab2881\">10.3847/1538-4357/ab2881</a>."},"author":[{"first_name":"Raffaella Anna","full_name":"Marino, Raffaella Anna","last_name":"Marino"},{"last_name":"Cantalupo","first_name":"Sebastiano","full_name":"Cantalupo, Sebastiano"},{"last_name":"Pezzulli","full_name":"Pezzulli, Gabriele","first_name":"Gabriele"},{"last_name":"Lilly","full_name":"Lilly, Simon J.","first_name":"Simon J."},{"last_name":"Gallego","full_name":"Gallego, Sofia","first_name":"Sofia"},{"last_name":"Mackenzie","first_name":"Ruari","full_name":"Mackenzie, Ruari"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","last_name":"Matthee"},{"last_name":"Brinchmann","first_name":"Jarle","full_name":"Brinchmann, Jarle"},{"last_name":"Bouché","full_name":"Bouché, Nicolas","first_name":"Nicolas"},{"first_name":"Anna","full_name":"Feltre, Anna","last_name":"Feltre"},{"first_name":"Sowgat","full_name":"Muzahid, Sowgat","last_name":"Muzahid"},{"full_name":"Schroetter, Ilane","first_name":"Ilane","last_name":"Schroetter"},{"first_name":"Sean D.","full_name":"Johnson, Sean D.","last_name":"Johnson"},{"first_name":"Themiya","full_name":"Nanayakkara, Themiya","last_name":"Nanayakkara"}],"type":"journal_article","day":"24"},{"date_created":"2022-07-07T08:38:24Z","extern":"1","month":"06","intvolume":"       877","status":"public","quality_controlled":"1","publication":"The Astrophysical Journal","publisher":"IOP Publishing","author":[{"first_name":"Enci","full_name":"Wang, Enci","last_name":"Wang"},{"full_name":"Lilly, Simon J.","first_name":"Simon J.","last_name":"Lilly"},{"first_name":"Gabriele","full_name":"Pezzulli, Gabriele","last_name":"Pezzulli"},{"last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X"}],"type":"journal_article","day":"04","title":"On the elevation and suppression of star formation within galaxies","citation":{"short":"E. Wang, S.J. Lilly, G. Pezzulli, J.J. Matthee, The Astrophysical Journal 877 (2019).","apa":"Wang, E., Lilly, S. J., Pezzulli, G., &#38; Matthee, J. J. (2019). On the elevation and suppression of star formation within galaxies. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ab1c5b\">https://doi.org/10.3847/1538-4357/ab1c5b</a>","ama":"Wang E, Lilly SJ, Pezzulli G, Matthee JJ. On the elevation and suppression of star formation within galaxies. <i>The Astrophysical Journal</i>. 2019;877(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/ab1c5b\">10.3847/1538-4357/ab1c5b</a>","ieee":"E. Wang, S. J. Lilly, G. Pezzulli, and J. J. Matthee, “On the elevation and suppression of star formation within galaxies,” <i>The Astrophysical Journal</i>, vol. 877, no. 2. IOP Publishing, 2019.","ista":"Wang E, Lilly SJ, Pezzulli G, Matthee JJ. 2019. On the elevation and suppression of star formation within galaxies. The Astrophysical Journal. 877(2), 132.","chicago":"Wang, Enci, Simon J. Lilly, Gabriele Pezzulli, and Jorryt J Matthee. “On the Elevation and Suppression of Star Formation within Galaxies.” <i>The Astrophysical Journal</i>. IOP Publishing, 2019. <a href=\"https://doi.org/10.3847/1538-4357/ab1c5b\">https://doi.org/10.3847/1538-4357/ab1c5b</a>.","mla":"Wang, Enci, et al. “On the Elevation and Suppression of Star Formation within Galaxies.” <i>The Astrophysical Journal</i>, vol. 877, no. 2, 132, IOP Publishing, 2019, doi:<a href=\"https://doi.org/10.3847/1538-4357/ab1c5b\">10.3847/1538-4357/ab1c5b</a>."},"doi":"10.3847/1538-4357/ab1c5b","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"acknowledgement":"We are grateful to the anonymous referee for their thoughtful and constructive review of the paper and their several suggestions (including the analysis of Section 3.4), which have improved the paper. This research has been supported by the Swiss National Science Foundation.\r\n\r\nFunding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS website is www.sdss.org.\r\n\r\nSDSS-IV is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration, including the Brazilian Participation Group, the Carnegie Institution for Science, Carnegie Mellon University, the Chilean Participation Group, the French Participation Group, Harvard-Smithsonian Center for Astrophysics, Instituto de Astrofísica de Canarias, the Johns Hopkins University, Kavli Institute for the Physics and Mathematics of the Universe (IPMU)/University of Tokyo, Lawrence Berkeley National Laboratory, Leibniz Institut für Astrophysik Potsdam (AIP), Max-Planck-Institut für Astronomie (MPIA Heidelberg), Max-Planck-Institut für Astrophysik (MPA Garching), Max-Planck-Institut für Extraterrestrische Physik (MPE), National Astronomical Observatory of China, New Mexico State University, New York University, University of Notre Dame, Observatário Nacional/MCTI, the Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, Universidad Nacional Autónoma de México, University of Arizona, University of Colorado Boulder, University of Oxford, University of Portsmouth, University of Utah, University of Virginia, University of Washington, University of Wisconsin, Vanderbilt University, and Yale University","date_published":"2019-06-04T00:00:00Z","_id":"11517","abstract":[{"lang":"eng","text":"To understand star formation in galaxies, we investigate the star formation rate (SFR) surface density (ΣSFR) profiles for galaxies, based on a well-defined sample of 976 star-forming MaNGA galaxies. We find that the typical ΣSFR profiles within 1.5Re of normal SF galaxies can be well described by an exponential function for different stellar mass intervals, while the sSFR profile shows positive gradients, especially for more massive SF galaxies. This is due to the more pronounced central cores or bulges rather than the onset of a `quenching' process. While galaxies that lie significantly above (or below) the star formation main sequence (SFMS) show overall an elevation (or suppression) of ΣSFR at all radii, this central elevation (or suppression) is more pronounced in more massive galaxies. The degree of central enhancement and suppression is quite symmetric, suggesting that both the elevation and suppression of star formation are following the same physical processes. Furthermore, we find that the dispersion in ΣSFR within and across the population is found to be tightly correlated with the inferred gas depletion time, whether based on the stellar surface mass density or the orbital dynamical time. This suggests that we are seeing the response of a simple gas-regulator system to variations in the accretion rate. This is explored using a heuristic model that can quantitatively explain the dependence of σ(ΣSFR) on gas depletion timescale. Variations in accretion rate are progressively more damped out in regions of low star-formation efficiency leading to a reduced amplitude of variations in star-formation."}],"article_number":"132","issue":"2","article_processing_charge":"No","arxiv":1,"volume":877,"oa":1,"main_file_link":[{"url":"https://arxiv.org/abs/1901.10276","open_access":"1"}],"publication_status":"published","year":"2019","oa_version":"Preprint","article_type":"original","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"date_updated":"2022-08-18T10:19:08Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","external_id":{"arxiv":["1901.10276"]},"scopus_import":"1"},{"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"scopus_import":"1","external_id":{"arxiv":["1811.00556"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2022-08-19T06:38:42Z","oa_version":"Preprint","year":"2019","article_type":"original","main_file_link":[{"url":"https://arxiv.org/abs/1811.00556","open_access":"1"}],"oa":1,"publication_status":"published","volume":489,"article_processing_charge":"No","issue":"1","arxiv":1,"_id":"11535","date_published":"2019-10-01T00:00:00Z","abstract":[{"lang":"eng","text":"We investigate the clustering and halo properties of ∼5000 Ly α-selected emission-line galaxies (LAEs) from the Slicing COSMOS 4K (SC4K) and from archival NB497 imaging of SA22 split in 15 discrete redshift slices between z ∼ 2.5 and 6. We measure clustering lengths of r0 ∼ 3–6 h−1 Mpc and typical halo masses of ∼1011 M⊙ for our narrowband-selected LAEs with typical LLy α ∼ 1042–43 erg s−1. The intermediate-band-selected LAEs are observed to have r0 ∼ 3.5–15 h−1 Mpc with typical halo masses of ∼1011–12 M⊙ and typical LLy α ∼ 1043–43.6 erg s−1. We find a strong, redshift-independent correlation between halo mass and Ly α luminosity normalized by the characteristic Ly α luminosity, L⋆(z). The faintest LAEs (L ∼ 0.1 L⋆(z)) typically identified by deep narrowband surveys are found in 1010 M⊙ haloes and the brightest LAEs (L ∼ 7 L⋆(z)) are found in ∼5 × 1012 M⊙ haloes. A dependency on the rest-frame 1500 Å UV luminosity, MUV, is also observed where the halo masses increase from 1011 to 1013 M⊙ for MUV ∼ −19 to −23.5 mag. Halo mass is also observed to increase from 109.8 to 1012 M⊙ for dust-corrected UV star formation rates from ∼0.6 to 10 M⊙ yr−1 and continues to increase up to 1013 M⊙ in halo mass, where the majority of those sources are active galactic nuclei. All the trends we observe are found to be redshift independent. Our results reveal that LAEs are the likely progenitors of a wide range of galaxies depending on their luminosity, from dwarf-like, to Milky Way-type, to bright cluster galaxies. LAEs therefore provide unique insight into the early formation and evolution of the galaxies we observe in the local Universe."}],"acknowledgement":"We thank the anonymous referee for their useful comments and suggestions that helped improve this study. AAK acknowledges that this work was supported by NASA Headquarters under the NASA Earth and Space Science Fellowship Program – Grant NNX16AO92H. JM acknowledges support from the ETH Zwicky fellowship. RKC acknowledges funding from STFC via a studentship. APA acknowledges support from the Fundac¸ao para a Ci ˜ encia e a Tecnologia FCT through the fellowship PD/BD/52706/2014 and the research grant UID/FIS/04434/2013. JC and SS both acknowledge their support from the Lancaster University PhD Fellowship. We have benefited greatly from the publicly available programming language PYTHON, including the NUMPY, SCIPY, MATPLOTLIB, SCIKIT-LEARN, and ASTROPY packages, as well as the TOPCAT analysis program. The SC4K samples used in this paper are all publicly available for use by the community (Sobral et al. 2018a). The catalogue is also available on the COSMOS IPAC website (https://irsa.ipac.caltech.edu/data/COSMOS/overview.html).","doi":"10.1093/mnras/stz2149","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: haloes","galaxies: high-redshift","galaxies: star formation","cosmology: observations","large-scale structure of Universe"],"language":[{"iso":"eng"}],"title":"The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities","citation":{"ista":"Khostovan AA, Sobral D, Mobasher B, Matthee JJ, Cochrane RK, Chartab N, Jafariyazani M, Paulino-Afonso A, Santos S, Calhau J. 2019. The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities. Monthly Notices of the Royal Astronomical Society. 489(1), 555–573.","ieee":"A. A. Khostovan <i>et al.</i>, “The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 489, no. 1. Oxford University Press, pp. 555–573, 2019.","chicago":"Khostovan, A A, D Sobral, B Mobasher, Jorryt J Matthee, R K Cochrane, N Chartab, M Jafariyazani, A Paulino-Afonso, S Santos, and J Calhau. “The Clustering of Typical Ly α Emitters from z ∼ 2.5–6: Host Halo Masses Depend on Ly α and UV Luminosities.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2019. <a href=\"https://doi.org/10.1093/mnras/stz2149\">https://doi.org/10.1093/mnras/stz2149</a>.","mla":"Khostovan, A. A., et al. “The Clustering of Typical Ly α Emitters from z ∼ 2.5–6: Host Halo Masses Depend on Ly α and UV Luminosities.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 489, no. 1, Oxford University Press, 2019, pp. 555–73, doi:<a href=\"https://doi.org/10.1093/mnras/stz2149\">10.1093/mnras/stz2149</a>.","short":"A.A. Khostovan, D. Sobral, B. Mobasher, J.J. Matthee, R.K. Cochrane, N. Chartab, M. Jafariyazani, A. Paulino-Afonso, S. Santos, J. Calhau, Monthly Notices of the Royal Astronomical Society 489 (2019) 555–573.","apa":"Khostovan, A. A., Sobral, D., Mobasher, B., Matthee, J. J., Cochrane, R. K., Chartab, N., … Calhau, J. (2019). The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stz2149\">https://doi.org/10.1093/mnras/stz2149</a>","ama":"Khostovan AA, Sobral D, Mobasher B, et al. The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities. <i>Monthly Notices of the Royal Astronomical Society</i>. 2019;489(1):555-573. doi:<a href=\"https://doi.org/10.1093/mnras/stz2149\">10.1093/mnras/stz2149</a>"},"type":"journal_article","author":[{"last_name":"Khostovan","first_name":"A A","full_name":"Khostovan, A A"},{"first_name":"D","full_name":"Sobral, D","last_name":"Sobral"},{"last_name":"Mobasher","full_name":"Mobasher, B","first_name":"B"},{"orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","full_name":"Matthee, Jorryt J","first_name":"Jorryt J"},{"full_name":"Cochrane, R K","first_name":"R K","last_name":"Cochrane"},{"last_name":"Chartab","first_name":"N","full_name":"Chartab, N"},{"last_name":"Jafariyazani","full_name":"Jafariyazani, M","first_name":"M"},{"last_name":"Paulino-Afonso","full_name":"Paulino-Afonso, A","first_name":"A"},{"full_name":"Santos, S","first_name":"S","last_name":"Santos"},{"first_name":"J","full_name":"Calhau, J","last_name":"Calhau"}],"day":"01","publisher":"Oxford University Press","intvolume":"       489","status":"public","publication":"Monthly Notices of the Royal Astronomical Society","quality_controlled":"1","page":"555-573","date_created":"2022-07-07T13:01:03Z","month":"10","extern":"1"},{"publisher":"Oxford University Press","quality_controlled":"1","publication":"Monthly Notices of the Royal Astronomical Society","intvolume":"       484","status":"public","page":"915-932","extern":"1","month":"03","date_created":"2022-07-08T07:48:31Z","acknowledgement":"JM acknowledges the support of a Huygens PhD fellowship from Leiden University. We thank Camila Correa for help analysing snipshot merger trees. We thank the anonymous referee for constructive comments. We also thank Jarle Brinchmann, Rob Crain, Antonios Katsianis, Paola Popesso, and David Sobral for discussions and suggestions. We also thank the participants of the Lorentz Center workshop ‘A Decade of the Star-Forming Main Sequence’ held on 2017 September 4–8, for discussions and ideas. We have benefited from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, and SCIPY (Hunter 2007) packages and the TOPCAT analysis tool (Taylor 2013).","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics : galaxies: evolution","galaxies: formation","galaxies: star formation","cosmology: theory"],"doi":"10.1093/mnras/stz030","citation":{"apa":"Matthee, J. J., &#38; Schaye, J. (2019). The origin of scatter in the star formation rate–stellar mass relation. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stz030\">https://doi.org/10.1093/mnras/stz030</a>","ama":"Matthee JJ, Schaye J. The origin of scatter in the star formation rate–stellar mass relation. <i>Monthly Notices of the Royal Astronomical Society</i>. 2019;484(1):915-932. doi:<a href=\"https://doi.org/10.1093/mnras/stz030\">10.1093/mnras/stz030</a>","short":"J.J. Matthee, J. Schaye, Monthly Notices of the Royal Astronomical Society 484 (2019) 915–932.","mla":"Matthee, Jorryt J., and Joop Schaye. “The Origin of Scatter in the Star Formation Rate–Stellar Mass Relation.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 484, no. 1, Oxford University Press, 2019, pp. 915–32, doi:<a href=\"https://doi.org/10.1093/mnras/stz030\">10.1093/mnras/stz030</a>.","ista":"Matthee JJ, Schaye J. 2019. The origin of scatter in the star formation rate–stellar mass relation. Monthly Notices of the Royal Astronomical Society. 484(1), 915–932.","ieee":"J. J. Matthee and J. Schaye, “The origin of scatter in the star formation rate–stellar mass relation,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 484, no. 1. Oxford University Press, pp. 915–932, 2019.","chicago":"Matthee, Jorryt J, and Joop Schaye. “The Origin of Scatter in the Star Formation Rate–Stellar Mass Relation.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2019. <a href=\"https://doi.org/10.1093/mnras/stz030\">https://doi.org/10.1093/mnras/stz030</a>."},"title":"The origin of scatter in the star formation rate–stellar mass relation","day":"01","type":"journal_article","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J","first_name":"Jorryt J"},{"last_name":"Schaye","full_name":"Schaye, Joop","first_name":"Joop"}],"publication_status":"published","oa":1,"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1805.05956"}],"volume":484,"arxiv":1,"issue":"1","article_processing_charge":"No","_id":"11540","date_published":"2019-03-01T00:00:00Z","abstract":[{"text":"Observations have revealed that the star formation rate (SFR) and stellar mass (Mstar) of star-forming galaxies follow a tight relation known as the galaxy main sequence. However, what physical information is encoded in this relation is under debate. Here, we use the EAGLE cosmological hydrodynamical simulation to study the mass dependence, evolution, and origin of scatter in the SFR–Mstar relation. At z = 0, we find that the scatter decreases slightly with stellar mass from 0.35 dex at Mstar ≈ 109 M⊙ to 0.30 dex at Mstar ≳ 1010.5 M⊙. The scatter decreases from z = 0 to z = 5 by 0.05 dex at Mstar ≳ 1010 M⊙ and by 0.15 dex for lower masses. We show that the scatter at z = 0.1 originates from a combination of fluctuations on short time-scales (ranging from 0.2–2 Gyr) that are presumably associated with self-regulation from cooling, star formation, and outflows, but is dominated by long time-scale (∼10 Gyr) variations related to differences in halo formation times. Shorter time-scale fluctuations are relatively more important for lower mass galaxies. At high masses, differences in black hole formation efficiency cause additional scatter, but also diminish the scatter caused by different halo formation times. While individual galaxies cross the main sequence multiple times during their evolution, they fluctuate around tracks associated with their halo properties, i.e. galaxies above/below the main sequence at z = 0.1 tend to have been above/below the main sequence for ≫1 Gyr.","lang":"eng"}],"date_updated":"2022-08-19T06:42:43Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","scopus_import":"1","external_id":{"arxiv":["1805.05956"]},"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"article_type":"original","year":"2019","oa_version":"Preprint"},{"citation":{"short":"D. Sobral, J.J. Matthee, G. Brammer, A. Ferrara, L. Alegre, H. Röttgering, D. Schaerer, B. Mobasher, B. Darvish, Monthly Notices of the Royal Astronomical Society 482 (2019) 2422–2441.","apa":"Sobral, D., Matthee, J. J., Brammer, G., Ferrara, A., Alegre, L., Röttgering, H., … Darvish, B. (2019). On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/sty2779\">https://doi.org/10.1093/mnras/sty2779</a>","ama":"Sobral D, Matthee JJ, Brammer G, et al. On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components. <i>Monthly Notices of the Royal Astronomical Society</i>. 2019;482(2):2422-2441. doi:<a href=\"https://doi.org/10.1093/mnras/sty2779\">10.1093/mnras/sty2779</a>","ista":"Sobral D, Matthee JJ, Brammer G, Ferrara A, Alegre L, Röttgering H, Schaerer D, Mobasher B, Darvish B. 2019. On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components. Monthly Notices of the Royal Astronomical Society. 482(2), 2422–2441.","ieee":"D. Sobral <i>et al.</i>, “On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 482, no. 2. Oxford University Press, pp. 2422–2441, 2019.","chicago":"Sobral, David, Jorryt J Matthee, Gabriel Brammer, Andrea Ferrara, Lara Alegre, Huub Röttgering, Daniel Schaerer, Bahram Mobasher, and Behnam Darvish. “On the Nature and Physical Conditions of the Luminous Ly α Emitter CR7 and Its Rest-Frame UV Components.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2019. <a href=\"https://doi.org/10.1093/mnras/sty2779\">https://doi.org/10.1093/mnras/sty2779</a>.","mla":"Sobral, David, et al. “On the Nature and Physical Conditions of the Luminous Ly α Emitter CR7 and Its Rest-Frame UV Components.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 482, no. 2, Oxford University Press, 2019, pp. 2422–41, doi:<a href=\"https://doi.org/10.1093/mnras/sty2779\">10.1093/mnras/sty2779</a>."},"title":"On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components","day":"01","type":"journal_article","author":[{"first_name":"David","full_name":"Sobral, David","last_name":"Sobral"},{"last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X"},{"first_name":"Gabriel","full_name":"Brammer, Gabriel","last_name":"Brammer"},{"full_name":"Ferrara, Andrea","first_name":"Andrea","last_name":"Ferrara"},{"last_name":"Alegre","first_name":"Lara","full_name":"Alegre, Lara"},{"full_name":"Röttgering, Huub","first_name":"Huub","last_name":"Röttgering"},{"first_name":"Daniel","full_name":"Schaerer, Daniel","last_name":"Schaerer"},{"first_name":"Bahram","full_name":"Mobasher, Bahram","last_name":"Mobasher"},{"last_name":"Darvish","first_name":"Behnam","full_name":"Darvish, Behnam"}],"acknowledgement":"We thank the anonymous reviewer for the numerous detailed comments that led us to greatly improve the quality, extent, and statistical robustness of this work. DS acknowledges financial support from the Netherlands Organisation for Scientific research through a Veni fellowship. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. AF acknowledges support from the ERC Advanced Grant INTERSTELLAR H2020/740120. BD acknowledges financial support from NASA through the Astrophysics Data Analysis Program, grant number NNX12AE20G and the National Science Foundation, grant number 1716907. We are thankful for several discussions and constructive comments from Johannes Zabl, Eros Vanzella, Bo Milvang-Jensen, Henry McCracken, Max Gronke, Mark Dijkstra, Richard Ellis, and Nicolas Laporte. We also thank Umar Burhanudin and Izzy Garland for taking part in the XGAL internship in Lancaster and for exploring the HST grism data independently. Based on observations obtained with HST/WFC3 programs 12578, 14495, and 14596. Based on observations of the National Japanese Observatory with the Suprime-Cam on the Subaru telescope (S14A-086) on the big island of Hawaii. This work is based in part on data products produced at TERAPIX available at the Canadian Astronomy Data Centre as part of the Canada–France–Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme IDs 294.A-5018, 294.A-5039, 092.A 0786, 093.A-0561, 097.A0043, 097.A-0943, 098.A-0819, 298.A-5012, and 179.A-2005, and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. The authors acknowledge the award of service time (SW2014b20) on the William Herschel Telescope (WHT). WHT and its service programme are operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. This research was supported by the Munich Institute for Astro- and Particle Physics of the DFG cluster of excellence ‘Origin and Structure of the Universe’. We have benefitted immensely from the public available programming language PYTHON, including NUMPY and SCIPY (Jones et al. 2001; Van Der Walt, Colbert & Varoquaux 2011), MATPLOTLIB (Hunter 2007), ASTROPY (Astropy Collaboration et al. 2013), and the TOPCAT analysis program (Taylor 2013). This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France. All data used for this paper are publicly available, and we make all reduced data available with the refereed paper.","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","galaxies: ISM","cosmology: observations","dark ages","reionization","first stars","early Universe"],"doi":"10.1093/mnras/sty2779","page":"2422-2441","extern":"1","month":"01","date_created":"2022-07-08T10:40:05Z","publisher":"Oxford University Press","quality_controlled":"1","publication":"Monthly Notices of the Royal Astronomical Society","intvolume":"       482","status":"public","article_type":"original","oa_version":"Preprint","year":"2019","date_updated":"2022-08-19T06:49:36Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","scopus_import":"1","external_id":{"arxiv":["1710.08422"]},"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"arxiv":1,"issue":"2","article_processing_charge":"No","date_published":"2019-01-01T00:00:00Z","_id":"11541","abstract":[{"text":"We present new Hubble Space Telescope (HST)/WFC3 observations and re-analyse VLT data to unveil the continuum, variability, and rest-frame ultraviolet (UV) lines of the multiple UV clumps of the most luminous Lyα emitter at z = 6.6, CR7 (COSMOS Redshift 7). Our re-reduced, flux-calibrated X-SHOOTER spectra of CR7 reveal an He II emission line in observations obtained along the major axis of Lyα emission with the best seeing conditions. He II is spatially offset by ≈+0.8 arcsec from the peak of Lyα emission, and it is found towards clump B. Our WFC3 grism spectra detects the UV continuum of CR7’s clump A, yielding a power law with β=−2.5+0.6−0.7 and MUV=−21.87+0.25−0.20⁠. No significant variability is found for any of the UV clumps on their own, but there is tentative (≈2.2 σ) brightening of CR7 in F110W as a whole from 2012 to 2017. HST grism data fail to robustly detect rest-frame UV lines in any of the clumps, implying fluxes ≲2×10−17 erg s−1 cm−2 (3σ). We perform CLOUDY modelling to constrain the metallicity and the ionizing nature of CR7. CR7 seems to be actively forming stars without any clear active galactic nucleus activity in clump A, consistent with a metallicity of ∼0.05–0.2 Z⊙. Component C or an interclump component between B and C may host a high ionization source. Our results highlight the need for spatially resolved information to study the formation and assembly of early galaxies.","lang":"eng"}],"publication_status":"published","oa":1,"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1710.08422"}],"volume":482},{"type":"journal_article","author":[{"last_name":"Mathur","first_name":"Savita","full_name":"Mathur, Savita"},{"first_name":"Rafael A.","full_name":"García, Rafael A.","last_name":"García"},{"orcid":"0000-0003-0142-4000","id":"d9edb345-f866-11ec-9b37-d119b5234501","last_name":"Bugnet","first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle"},{"last_name":"Santos","first_name":"Ângela R.G.","full_name":"Santos, Ângela R.G."},{"last_name":"Santiago","first_name":"Netsha","full_name":"Santiago, Netsha"},{"full_name":"Beck, Paul G.","first_name":"Paul G.","last_name":"Beck"}],"day":"10","title":"Revisiting the impact of stellar magnetic activity on the detectability of solar-like oscillations by Kepler","citation":{"ieee":"S. Mathur, R. A. García, L. A. Bugnet, Â. R. G. Santos, N. Santiago, and P. G. Beck, “Revisiting the impact of stellar magnetic activity on the detectability of solar-like oscillations by Kepler,” <i>Frontiers in Astronomy and Space Sciences</i>, vol. 6. Frontiers Media, 2019.","ista":"Mathur S, García RA, Bugnet LA, Santos ÂRG, Santiago N, Beck PG. 2019. Revisiting the impact of stellar magnetic activity on the detectability of solar-like oscillations by Kepler. Frontiers in Astronomy and Space Sciences. 6, 46.","chicago":"Mathur, Savita, Rafael A. García, Lisa Annabelle Bugnet, Ângela R.G. Santos, Netsha Santiago, and Paul G. Beck. “Revisiting the Impact of Stellar Magnetic Activity on the Detectability of Solar-like Oscillations by Kepler.” <i>Frontiers in Astronomy and Space Sciences</i>. Frontiers Media, 2019. <a href=\"https://doi.org/10.3389/fspas.2019.00046\">https://doi.org/10.3389/fspas.2019.00046</a>.","mla":"Mathur, Savita, et al. “Revisiting the Impact of Stellar Magnetic Activity on the Detectability of Solar-like Oscillations by Kepler.” <i>Frontiers in Astronomy and Space Sciences</i>, vol. 6, 46, Frontiers Media, 2019, doi:<a href=\"https://doi.org/10.3389/fspas.2019.00046\">10.3389/fspas.2019.00046</a>.","short":"S. Mathur, R.A. García, L.A. Bugnet, Â.R.G. Santos, N. Santiago, P.G. Beck, Frontiers in Astronomy and Space Sciences 6 (2019).","apa":"Mathur, S., García, R. A., Bugnet, L. A., Santos, Â. R. G., Santiago, N., &#38; Beck, P. G. (2019). Revisiting the impact of stellar magnetic activity on the detectability of solar-like oscillations by Kepler. <i>Frontiers in Astronomy and Space Sciences</i>. Frontiers Media. <a href=\"https://doi.org/10.3389/fspas.2019.00046\">https://doi.org/10.3389/fspas.2019.00046</a>","ama":"Mathur S, García RA, Bugnet LA, Santos ÂRG, Santiago N, Beck PG. Revisiting the impact of stellar magnetic activity on the detectability of solar-like oscillations by Kepler. <i>Frontiers in Astronomy and Space Sciences</i>. 2019;6. doi:<a href=\"https://doi.org/10.3389/fspas.2019.00046\">10.3389/fspas.2019.00046</a>"},"doi":"10.3389/fspas.2019.00046","language":[{"iso":"eng"}],"keyword":["Astronomy and Astrophysics"],"acknowledgement":"This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Partly Based on observations obtained with the HERMES spectrograph on the Mercator Telescope, which was supported by the Research Foundation—Flanders (FWO), Belgium, the Research Council of KU Leuven, Belgium, the Fonds National de la Recherche Scientifique (F.R.S.-FNRS), Belgium, the Royal Observatory of Belgium, the Observatoire de Genève, Switzerland, and the Thüringer Landessternwarte Tautenburg, Germany. SM acknowledges support by the National Aeronautics and Space Administration under Grant NNX15AF13G, by the National Science Foundation grant AST-1411685, and the Ramon y Cajal fellowship number RYC-2015-17697. RG acknowledges the support from PLATO and GOLF CNES grants. ÂS acknowledges the support from National Aeronautics and Space Administration under Grant NNX17AF27G. PB acknowledges the support of the MINECO under the fellowship program Juan de la Cierva Incorporacion (IJCI-2015-26034).","date_created":"2022-07-18T14:00:36Z","extern":"1","month":"07","intvolume":"         6","status":"public","quality_controlled":"1","publication":"Frontiers in Astronomy and Space Sciences","publisher":"Frontiers Media","year":"2019","oa_version":"Preprint","article_type":"original","publication_identifier":{"eissn":["2296-987X"]},"date_updated":"2022-08-22T07:29:55Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","external_id":{"arxiv":["1907.01415"]},"scopus_import":"1","_id":"11613","abstract":[{"lang":"eng","text":"Over 2,000 stars were observed for 1 month with a high enough cadence in order to look for acoustic modes during the survey phase of the Kepler mission. Solar-like oscillations have been detected in about 540 stars. The question of why no oscillations were detected in the remaining stars is still open. Previous works explained the non-detection of modes with the high level of magnetic activity of the stars. However, the sample of stars studied contained some classical pulsators and red giants that could have biased the results. In this work, we revisit this analysis on a cleaner sample of main-sequence solar-like stars that consists of 1,014 stars. First we compute the predicted amplitude of the modes of that sample and for the stars with detected oscillation and compare it to the noise at high frequency in the power spectrum. We find that the stars with detected modes have an amplitude to noise ratio larger than 0.94. We measure reliable rotation periods and the associated photometric magnetic index for 684 stars out of the full sample and in particular for 323 stars where the amplitude of the modes is predicted to be high enough to be detected. We find that among these 323 stars 32% of them have a level of magnetic activity larger than the Sun during its maximum activity, explaining the non-detection of acoustic modes. Interestingly, magnetic activity cannot be the primary reason responsible for the absence of detectable modes in the remaining 68% of the stars without acoustic modes detected and with reliable rotation periods. Thus, we investigate metallicity, inclination angle of the rotation axis, and binarity as possible causes of low mode amplitudes. Using spectroscopic observations for a subsample, we find that a low metallicity could be the reason for suppressed modes. No clear correlation with binarity nor inclination is found. We also derive the lower limit for our photometric activity index (of 20–30 ppm) below which rotation and magnetic activity are not detected. Finally, with our analysis we conclude that stars with a photometric activity index larger than 2,000 ppm have 98.3% probability of not having oscillations detected."}],"date_published":"2019-07-10T00:00:00Z","article_number":"46","article_processing_charge":"No","arxiv":1,"volume":6,"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1907.01415"}],"oa":1,"publication_status":"published"},{"publication":"Astronomy & Astrophysics","quality_controlled":"1","intvolume":"       624","status":"public","publisher":"EDP Science","month":"04","extern":"1","date_created":"2022-07-18T14:13:34Z","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"language":[{"iso":"eng"}],"doi":"10.1051/0004-6361/201834780","acknowledgement":"We thank the enitre T’DA team for useful comments and discussions, in particular Andrew Tkachenko. We also acknowledge Marc Hon, Keaton Bell, and James Kuszlewicz for useful comments on the manuscript. L.B. and R.A.G. acknowledge the support from PLATO and GOLF CNES grants. S.M. acknowledges support by the Ramon y Cajal fellowship number RYC-2015-17697. O.J.H. and B.M.R. acknowledge the support of the UK Science and Technology Facilities Council (STFC). M.N.L. acknowledges the support of the ESA PRODEX programme (PEA 4000119301). Funding for the Stellar Astrophysics Centre is provided by the Danish National Research Foundation (Grant DNRF106).","day":"19","author":[{"last_name":"Bugnet","first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle","orcid":"0000-0003-0142-4000","id":"d9edb345-f866-11ec-9b37-d119b5234501"},{"last_name":"García","first_name":"R. A.","full_name":"García, R. A."},{"last_name":"Mathur","first_name":"S.","full_name":"Mathur, S."},{"last_name":"Davies","full_name":"Davies, G. R.","first_name":"G. R."},{"last_name":"Hall","first_name":"O. J.","full_name":"Hall, O. J."},{"last_name":"Lund","first_name":"M. N.","full_name":"Lund, M. N."},{"first_name":"B. M.","full_name":"Rendle, B. M.","last_name":"Rendle"}],"type":"journal_article","citation":{"mla":"Bugnet, Lisa Annabelle, et al. “FliPerClass: In Search of Solar-like Pulsators among TESS Targets.” <i>Astronomy &#38; Astrophysics</i>, vol. 624, A79, EDP Science, 2019, doi:<a href=\"https://doi.org/10.1051/0004-6361/201834780\">10.1051/0004-6361/201834780</a>.","chicago":"Bugnet, Lisa Annabelle, R. A. García, S. Mathur, G. R. Davies, O. J. Hall, M. N. Lund, and B. M. Rendle. “FliPerClass: In Search of Solar-like Pulsators among TESS Targets.” <i>Astronomy &#38; Astrophysics</i>. EDP Science, 2019. <a href=\"https://doi.org/10.1051/0004-6361/201834780\">https://doi.org/10.1051/0004-6361/201834780</a>.","ista":"Bugnet LA, García RA, Mathur S, Davies GR, Hall OJ, Lund MN, Rendle BM. 2019. FliPerClass: In search of solar-like pulsators among TESS targets. Astronomy &#38; Astrophysics. 624, A79.","ieee":"L. A. Bugnet <i>et al.</i>, “FliPerClass: In search of solar-like pulsators among TESS targets,” <i>Astronomy &#38; Astrophysics</i>, vol. 624. EDP Science, 2019.","ama":"Bugnet LA, García RA, Mathur S, et al. FliPerClass: In search of solar-like pulsators among TESS targets. <i>Astronomy &#38; Astrophysics</i>. 2019;624. doi:<a href=\"https://doi.org/10.1051/0004-6361/201834780\">10.1051/0004-6361/201834780</a>","apa":"Bugnet, L. A., García, R. A., Mathur, S., Davies, G. R., Hall, O. J., Lund, M. N., &#38; Rendle, B. M. (2019). FliPerClass: In search of solar-like pulsators among TESS targets. <i>Astronomy &#38; Astrophysics</i>. EDP Science. <a href=\"https://doi.org/10.1051/0004-6361/201834780\">https://doi.org/10.1051/0004-6361/201834780</a>","short":"L.A. Bugnet, R.A. García, S. Mathur, G.R. Davies, O.J. Hall, M.N. Lund, B.M. Rendle, Astronomy &#38; Astrophysics 624 (2019)."},"title":"FliPerClass: In search of solar-like pulsators among TESS targets","volume":624,"publication_status":"published","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1902.09854"}],"oa":1,"article_number":"A79","abstract":[{"text":"The NASA Transiting Exoplanet Survey Satellite (TESS) is about to provide full-frame images of almost the entire sky. The amount of stellar data to be analysed represents hundreds of millions stars, which is several orders of magnitude more than the number of stars observed by the Convection, Rotation and planetary Transits satellite (CoRoT), and NASA Kepler and K2 missions. We aim at automatically classifying the newly observed stars with near real-time algorithms to better guide the subsequent detailed studies. In this paper, we present a classification algorithm built to recognise solar-like pulsators among classical pulsators. This algorithm relies on the global amount of power contained in the power spectral density (PSD), also known as the flicker in spectral power density (FliPer). Because each type of pulsating star has a characteristic background or pulsation pattern, the shape of the PSD at different frequencies can be used to characterise the type of pulsating star. The FliPer classifier (FliPerClass) uses different FliPer parameters along with the effective temperature as input parameters to feed a ML algorithm in order to automatically classify the pulsating stars observed by TESS. Using noisy TESS-simulated data from the TESS Asteroseismic Science Consortium (TASC), we classify pulsators with a 98% accuracy. Among them, solar-like pulsating stars are recognised with a 99% accuracy, which is of great interest for a further seismic analysis of these stars, which are like our Sun. Similar results are obtained when we trained our classifier and applied it to 27-day subsets of real Kepler data. FliPerClass is part of the large TASC classification pipeline developed by the TESS Data for Asteroseismology (T’DA) classification working group.","lang":"eng"}],"_id":"11614","date_published":"2019-04-19T00:00:00Z","arxiv":1,"article_processing_charge":"No","external_id":{"arxiv":["1902.09854"]},"scopus_import":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2022-08-22T07:32:51Z","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"article_type":"original","oa_version":"Preprint","year":"2019"},{"month":"06","extern":"1","date_created":"2022-07-18T14:26:03Z","page":"5616-5630","publication":"Monthly Notices of the Royal Astronomical Society","quality_controlled":"1","status":"public","intvolume":"       485","publisher":"Oxford University Press","day":"01","author":[{"last_name":"Hon","first_name":"Marc","full_name":"Hon, Marc"},{"first_name":"Dennis","full_name":"Stello, Dennis","last_name":"Stello"},{"last_name":"García","full_name":"García, Rafael A","first_name":"Rafael A"},{"last_name":"Mathur","full_name":"Mathur, Savita","first_name":"Savita"},{"full_name":"Sharma, Sanjib","first_name":"Sanjib","last_name":"Sharma"},{"last_name":"Colman","first_name":"Isabel L","full_name":"Colman, Isabel L"},{"id":"d9edb345-f866-11ec-9b37-d119b5234501","orcid":"0000-0003-0142-4000","first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle","last_name":"Bugnet"}],"type":"journal_article","citation":{"chicago":"Hon, Marc, Dennis Stello, Rafael A García, Savita Mathur, Sanjib Sharma, Isabel L Colman, and Lisa Annabelle Bugnet. “A Search for Red Giant Solar-like Oscillations in All Kepler Data.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2019. <a href=\"https://doi.org/10.1093/mnras/stz622\">https://doi.org/10.1093/mnras/stz622</a>.","ieee":"M. Hon <i>et al.</i>, “A search for red giant solar-like oscillations in all Kepler data,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 485, no. 4. Oxford University Press, pp. 5616–5630, 2019.","ista":"Hon M, Stello D, García RA, Mathur S, Sharma S, Colman IL, Bugnet LA. 2019. A search for red giant solar-like oscillations in all Kepler data. Monthly Notices of the Royal Astronomical Society. 485(4), 5616–5630.","mla":"Hon, Marc, et al. “A Search for Red Giant Solar-like Oscillations in All Kepler Data.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 485, no. 4, Oxford University Press, 2019, pp. 5616–30, doi:<a href=\"https://doi.org/10.1093/mnras/stz622\">10.1093/mnras/stz622</a>.","short":"M. Hon, D. Stello, R.A. García, S. Mathur, S. Sharma, I.L. Colman, L.A. Bugnet, Monthly Notices of the Royal Astronomical Society 485 (2019) 5616–5630.","ama":"Hon M, Stello D, García RA, et al. A search for red giant solar-like oscillations in all Kepler data. <i>Monthly Notices of the Royal Astronomical Society</i>. 2019;485(4):5616-5630. doi:<a href=\"https://doi.org/10.1093/mnras/stz622\">10.1093/mnras/stz622</a>","apa":"Hon, M., Stello, D., García, R. A., Mathur, S., Sharma, S., Colman, I. L., &#38; Bugnet, L. A. (2019). A search for red giant solar-like oscillations in all Kepler data. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stz622\">https://doi.org/10.1093/mnras/stz622</a>"},"title":"A search for red giant solar-like oscillations in all Kepler data","keyword":["Space and Planetary Science","Astronomy and Astrophysics","asteroseismology","methods: data analysis","techniques: image processing","stars: oscillations","stars: statistics"],"language":[{"iso":"eng"}],"doi":"10.1093/mnras/stz622","acknowledgement":"Funding for this Discovery mission is provided by NASA’s Science mission Directorate. We thank the entire Kepler team without whom this investigation would not be possible. DS is the recipient of an Australian Research Council Future Fellowship (project number FT1400147). RAG acknowledges the support from CNES. SM acknowledges support from NASA grant NNX15AF13G, NSF grant AST-1411685, and the Ramon y Cajal fellowship number RYC-2015-17697. ILC acknowledges scholarship support from the University of Sydney. We would like to thank Nicholas Barbara and Timothy Bedding for providing us with a list of variable stars that helped to validate a number of detections in this study. We also thank the group at the University of Sydney for fruitful discussions. Finally, we gratefully acknowledge the support of NVIDIA Corporation with the donation of the Titan Xp GPU used for this research.","_id":"11615","date_published":"2019-06-01T00:00:00Z","abstract":[{"lang":"eng","text":"The recently published Kepler mission Data Release 25 (DR25) reported on ∼197 000 targets observed during the mission. Despite this, no wide search for red giants showing solar-like oscillations have been made across all stars observed in Kepler’s long-cadence mode. In this work, we perform this task using custom apertures on the Kepler pixel files and detect oscillations in 21 914 stars, representing the largest sample of solar-like oscillating stars to date. We measure their frequency at maximum power, νmax, down to νmax≃4μHz and obtain log (g) estimates with a typical uncertainty below 0.05 dex, which is superior to typical measurements from spectroscopy. Additionally, the νmax distribution of our detections show good agreement with results from a simulated model of the Milky Way, with a ratio of observed to predicted stars of 0.992 for stars with 10<νmax<270μHz. Among our red giant detections, we find 909 to be dwarf/subgiant stars whose flux signal is polluted by a neighbouring giant as a result of using larger photometric apertures than those used by the NASA Kepler science processing pipeline. We further find that only 293 of the polluting giants are known Kepler targets. The remainder comprises over 600 newly identified oscillating red giants, with many expected to belong to the Galactic halo, serendipitously falling within the Kepler pixel files of targeted stars."}],"arxiv":1,"article_processing_charge":"No","issue":"4","volume":485,"publication_status":"published","oa":1,"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1903.00115"}],"article_type":"original","oa_version":"Preprint","year":"2019","external_id":{"arxiv":["1903.00115"]},"scopus_import":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2022-08-22T07:35:19Z","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]}},{"article_number":"245","_id":"11616","date_published":"2019-05-30T00:00:00Z","abstract":[{"lang":"eng","text":"We present the discovery of HD 221416 b, the first transiting planet identified by the Transiting Exoplanet Survey Satellite (TESS) for which asteroseismology of the host star is possible. HD 221416 b (HIP 116158, TOI-197) is a bright (V = 8.2 mag), spectroscopically classified subgiant that oscillates with an average frequency of about 430 μHz and displays a clear signature of mixed modes. The oscillation amplitude confirms that the redder TESS bandpass compared to Kepler has a small effect on the oscillations, supporting the expected yield of thousands of solar-like oscillators with TESS 2 minute cadence observations. Asteroseismic modeling yields a robust determination of the host star radius (R⋆ = 2.943 ± 0.064 R⊙), mass (M⋆ = 1.212 ± 0.074 M⊙), and age (4.9 ± 1.1 Gyr), and demonstrates that it has just started ascending the red-giant branch. Combining asteroseismology with transit modeling and radial-velocity observations, we show that the planet is a \"hot Saturn\" (Rp = 9.17 ± 0.33 R⊕) with an orbital period of ∼14.3 days, irradiance of F = 343 ± 24 F⊕, and moderate mass (Mp = 60.5 ± 5.7 M⊕) and density (ρp = 0.431 ± 0.062 g cm−3). The properties of HD 221416 b show that the host-star metallicity–planet mass correlation found in sub-Saturns (4–8 R⊕) does not extend to larger radii, indicating that planets in the transition between sub-Saturns and Jupiters follow a relatively narrow range of densities. With a density measured to ∼15%, HD 221416 b is one of the best characterized Saturn-size planets to date, augmenting the small number of known transiting planets around evolved stars and demonstrating the power of TESS to characterize exoplanets and their host stars using asteroseismology."}],"arxiv":1,"article_processing_charge":"No","issue":"6","volume":157,"publication_status":"published","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1901.01643"}],"oa":1,"article_type":"original","oa_version":"Preprint","year":"2019","scopus_import":"1","external_id":{"arxiv":["1901.01643"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2022-08-22T07:38:34Z","publication_identifier":{"issn":["0004-6256"]},"month":"05","extern":"1","date_created":"2022-07-18T14:29:07Z","publication":"The Astronomical Journal","quality_controlled":"1","status":"public","intvolume":"       157","publisher":"IOP Publishing","day":"30","type":"journal_article","author":[{"last_name":"Huber","full_name":"Huber, Daniel","first_name":"Daniel"},{"first_name":"William J.","full_name":"Chaplin, William J.","last_name":"Chaplin"},{"full_name":"Chontos, Ashley","first_name":"Ashley","last_name":"Chontos"},{"full_name":"Kjeldsen, Hans","first_name":"Hans","last_name":"Kjeldsen"},{"full_name":"Christensen-Dalsgaard, Jørgen","first_name":"Jørgen","last_name":"Christensen-Dalsgaard"},{"full_name":"Bedding, Timothy R.","first_name":"Timothy R.","last_name":"Bedding"},{"last_name":"Ball","first_name":"Warrick","full_name":"Ball, Warrick"},{"full_name":"Brahm, Rafael","first_name":"Rafael","last_name":"Brahm"},{"last_name":"Espinoza","full_name":"Espinoza, Nestor","first_name":"Nestor"},{"first_name":"Thomas","full_name":"Henning, Thomas","last_name":"Henning"},{"full_name":"Jordán, Andrés","first_name":"Andrés","last_name":"Jordán"},{"first_name":"Paula","full_name":"Sarkis, Paula","last_name":"Sarkis"},{"first_name":"Emil","full_name":"Knudstrup, Emil","last_name":"Knudstrup"},{"last_name":"Albrecht","full_name":"Albrecht, Simon","first_name":"Simon"},{"full_name":"Grundahl, Frank","first_name":"Frank","last_name":"Grundahl"},{"last_name":"Andersen","first_name":"Mads Fredslund","full_name":"Andersen, Mads Fredslund"},{"last_name":"Pallé","full_name":"Pallé, Pere L.","first_name":"Pere L."},{"full_name":"Crossfield, Ian","first_name":"Ian","last_name":"Crossfield"},{"full_name":"Fulton, Benjamin","first_name":"Benjamin","last_name":"Fulton"},{"last_name":"Howard","full_name":"Howard, Andrew W.","first_name":"Andrew W."},{"last_name":"Isaacson","first_name":"Howard T.","full_name":"Isaacson, Howard T."},{"full_name":"Weiss, Lauren M.","first_name":"Lauren M.","last_name":"Weiss"},{"first_name":"Rasmus","full_name":"Handberg, Rasmus","last_name":"Handberg"},{"last_name":"Lund","full_name":"Lund, Mikkel N.","first_name":"Mikkel N."},{"last_name":"Serenelli","full_name":"Serenelli, Aldo M.","first_name":"Aldo M."},{"first_name":"Jakob","full_name":"Rørsted Mosumgaard, Jakob","last_name":"Rørsted Mosumgaard"},{"full_name":"Stokholm, Amalie","first_name":"Amalie","last_name":"Stokholm"},{"first_name":"Allyson","full_name":"Bieryla, Allyson","last_name":"Bieryla"},{"full_name":"Buchhave, Lars A.","first_name":"Lars A.","last_name":"Buchhave"},{"last_name":"Latham","first_name":"David W.","full_name":"Latham, David W."},{"first_name":"Samuel N.","full_name":"Quinn, Samuel N.","last_name":"Quinn"},{"last_name":"Gaidos","full_name":"Gaidos, Eric","first_name":"Eric"},{"full_name":"Hirano, Teruyuki","first_name":"Teruyuki","last_name":"Hirano"},{"full_name":"Ricker, George R.","first_name":"George R.","last_name":"Ricker"},{"last_name":"Vanderspek","first_name":"Roland K.","full_name":"Vanderspek, Roland K."},{"last_name":"Seager","first_name":"Sara","full_name":"Seager, Sara"},{"first_name":"Jon M.","full_name":"Jenkins, Jon M.","last_name":"Jenkins"},{"last_name":"Winn","full_name":"Winn, Joshua N.","first_name":"Joshua N."},{"full_name":"Antia, H. M.","first_name":"H. M.","last_name":"Antia"},{"full_name":"Appourchaux, Thierry","first_name":"Thierry","last_name":"Appourchaux"},{"first_name":"Sarbani","full_name":"Basu, Sarbani","last_name":"Basu"},{"full_name":"Bell, Keaton J.","first_name":"Keaton J.","last_name":"Bell"},{"last_name":"Benomar","full_name":"Benomar, Othman","first_name":"Othman"},{"last_name":"Bonanno","full_name":"Bonanno, Alfio","first_name":"Alfio"},{"last_name":"Buzasi","first_name":"Derek L.","full_name":"Buzasi, Derek L."},{"last_name":"Campante","full_name":"Campante, Tiago L.","first_name":"Tiago L."},{"last_name":"Çelik Orhan","full_name":"Çelik Orhan, Z.","first_name":"Z."},{"full_name":"Corsaro, Enrico","first_name":"Enrico","last_name":"Corsaro"},{"first_name":"Margarida S.","full_name":"Cunha, Margarida S.","last_name":"Cunha"},{"last_name":"Davies","full_name":"Davies, Guy R.","first_name":"Guy R."},{"last_name":"Deheuvels","first_name":"Sebastien","full_name":"Deheuvels, Sebastien"},{"first_name":"Samuel K.","full_name":"Grunblatt, Samuel K.","last_name":"Grunblatt"},{"full_name":"Hasanzadeh, Amir","first_name":"Amir","last_name":"Hasanzadeh"},{"full_name":"Di Mauro, Maria Pia","first_name":"Maria Pia","last_name":"Di Mauro"},{"full_name":"A. 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G. Monteiro, Mário J. P.","first_name":"Mário J. P.","last_name":"F. G. 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G.","full_name":"Tinney, C. G.","last_name":"Tinney"},{"first_name":"Johanna","full_name":"Teske, Johanna","last_name":"Teske"},{"first_name":"Alexandra","full_name":"Thomas, Alexandra","last_name":"Thomas"},{"last_name":"Trampedach","first_name":"Regner","full_name":"Trampedach, Regner"},{"last_name":"Wright","first_name":"Duncan","full_name":"Wright, Duncan"},{"first_name":"Thomas T.","full_name":"Yuan, Thomas T.","last_name":"Yuan"},{"first_name":"Farzaneh","full_name":"Zohrabi, Farzaneh","last_name":"Zohrabi"}],"citation":{"short":"D. Huber, W.J. Chaplin, A. Chontos, H. Kjeldsen, J. Christensen-Dalsgaard, T.R. Bedding, W. Ball, R. Brahm, N. Espinoza, T. Henning, A. Jordán, P. Sarkis, E. Knudstrup, S. Albrecht, F. Grundahl, M.F. Andersen, P.L. Pallé, I. Crossfield, B. Fulton, A.W. Howard, H.T. Isaacson, L.M. Weiss, R. Handberg, M.N. Lund, A.M. Serenelli, J. Rørsted Mosumgaard, A. Stokholm, A. Bieryla, L.A. Buchhave, D.W. Latham, S.N. Quinn, E. Gaidos, T. Hirano, G.R. Ricker, R.K. Vanderspek, S. Seager, J.M. Jenkins, J.N. Winn, H.M. Antia, T. Appourchaux, S. Basu, K.J. Bell, O. Benomar, A. Bonanno, D.L. Buzasi, T.L. Campante, Z. Çelik Orhan, E. Corsaro, M.S. Cunha, G.R. Davies, S. Deheuvels, S.K. Grunblatt, A. Hasanzadeh, M.P. Di Mauro, R. A. García, P. Gaulme, L. Girardi, J.A. Guzik, M. Hon, C. Jiang, T. Kallinger, S.D. Kawaler, J.S. Kuszlewicz, Y. Lebreton, T. Li, M. Lucas, M.S. Lundkvist, A.W. Mann, S. Mathis, S. Mathur, A. Mazumdar, T.S. Metcalfe, A. Miglio, M.J.P. F. G. Monteiro, B. Mosser, A. Noll, B. Nsamba, J.M. Joel Ong, S. Örtel, F. Pereira, P. Ranadive, C. Régulo, T.S. Rodrigues, I.W. Roxburgh, V.S. Aguirre, B. Smalley, M. Schofield, S.G. Sousa, K.G. Stassun, D. Stello, J. Tayar, T.R. White, K. Verma, M. Vrard, M. Yıldız, D. Baker, M. Bazot, C. Beichmann, C. Bergmann, L.A. Bugnet, B. Cale, R. Carlino, S.M. Cartwright, J.L. Christiansen, D.R. Ciardi, O. Creevey, J.A. Dittmann, J.-D.D. Nascimento, V.V. Eylen, G. Fürész, J. Gagné, P. Gao, K. Gazeas, F. Giddens, O.J. Hall, S. Hekker, M.J. Ireland, N. Latouf, D. LeBrun, A.M. Levine, W. Matzko, E. Natinsky, E. Page, P. Plavchan, M. Mansouri-Samani, S. McCauliff, S.E. Mullally, B. Orenstein, A.G. Soto, M. Paegert, J.L. van Saders, C. Schnaible, D.R. Soderblom, R. Szabó, A. Tanner, C.G. Tinney, J. Teske, A. Thomas, R. Trampedach, D. Wright, T.T. Yuan, F. Zohrabi, The Astronomical Journal 157 (2019).","apa":"Huber, D., Chaplin, W. J., Chontos, A., Kjeldsen, H., Christensen-Dalsgaard, J., Bedding, T. R., … Zohrabi, F. (2019). A hot Saturn orbiting an oscillating late subgiant discovered by TESS. <i>The Astronomical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-3881/ab1488\">https://doi.org/10.3847/1538-3881/ab1488</a>","ama":"Huber D, Chaplin WJ, Chontos A, et al. A hot Saturn orbiting an oscillating late subgiant discovered by TESS. <i>The Astronomical Journal</i>. 2019;157(6). doi:<a href=\"https://doi.org/10.3847/1538-3881/ab1488\">10.3847/1538-3881/ab1488</a>","ieee":"D. Huber <i>et al.</i>, “A hot Saturn orbiting an oscillating late subgiant discovered by TESS,” <i>The Astronomical Journal</i>, vol. 157, no. 6. IOP Publishing, 2019.","ista":"Huber D et al. 2019. A hot Saturn orbiting an oscillating late subgiant discovered by TESS. The Astronomical Journal. 157(6), 245.","chicago":"Huber, Daniel, William J. Chaplin, Ashley Chontos, Hans Kjeldsen, Jørgen Christensen-Dalsgaard, Timothy R. Bedding, Warrick Ball, et al. “A Hot Saturn Orbiting an Oscillating Late Subgiant Discovered by TESS.” <i>The Astronomical Journal</i>. IOP Publishing, 2019. <a href=\"https://doi.org/10.3847/1538-3881/ab1488\">https://doi.org/10.3847/1538-3881/ab1488</a>.","mla":"Huber, Daniel, et al. “A Hot Saturn Orbiting an Oscillating Late Subgiant Discovered by TESS.” <i>The Astronomical Journal</i>, vol. 157, no. 6, 245, IOP Publishing, 2019, doi:<a href=\"https://doi.org/10.3847/1538-3881/ab1488\">10.3847/1538-3881/ab1488</a>."},"title":"A hot Saturn orbiting an oscillating late subgiant discovered by TESS","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"language":[{"iso":"eng"}],"doi":"10.3847/1538-3881/ab1488","acknowledgement":"The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawai'ian community. We are most fortunate to have the opportunity to conduct observations from this mountain. We thank Andrei Tokovinin for helpful information on the Speckle observations obtained with SOAR. D.H. acknowledges support by the National Aeronautics and Space Administration through the TESS Guest Investigator Program (80NSSC18K1585) and by the National Science Foundation (AST-1717000). A.C. acknowledges support by the National Science Foundation under the Graduate Research Fellowship Program. W.J.C., W.H.B., A.M., O.J.H., and G.R.D. acknowledge support from the Science and Technology Facilities Council and UK Space Agency. H.K. and F.G. acknowledge support from the European Social Fund via the Lithuanian Science Council grant No. 09.3.3-LMT-K-712-01-0103. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (grant DNRF106). A.J. acknowledges support from FONDECYT project 1171208, CONICYT project BASAL AFB-170002, and by the Ministry for the Economy, Development, and Tourism's Programa Iniciativa Científica Milenio through grant IC 120009, awarded to the Millennium Institute of Astrophysics (MAS). R.B. acknowledges support from FONDECYT Post-doctoral Fellowship Project 3180246, and from the Millennium Institute of Astrophysics (MAS). A.M.S. is supported by grants ESP2017-82674-R (MINECO) and SGR2017-1131 (AGAUR). R.A.G. and L.B. acknowledge the support of the PLATO grant from the CNES. The research leading to the presented results has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP72007-2013)ERC grant agreement No. 338251 (StellarAges). S.M. acknowledges support from the European Research Council through the SPIRE grant 647383. This work was also supported by FCT (Portugal) through national funds and by FEDER through COMPETE2020 by these grants: UID/FIS/04434/2013 and POCI-01-0145-FEDER-007672, PTDC/FIS-AST/30389/2017, and POCI-01-0145-FEDER-030389. T.L.C. acknowledges support from the European Union's Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement No. 792848 (PULSATION). E.C. is funded by the European Union's Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement No. 664931. V.S.A. acknowledges support from the Independent Research Fund Denmark (Research grant 7027-00096B). D.S. acknowledges support from the Australian Research Council. S.B. acknowledges NASA grant NNX16AI09G and NSF grant AST-1514676. T.R.W. acknowledges support from the Australian Research Council through grant DP150100250. A.M. acknowledges support from the ERC Consolidator Grant funding scheme (project ASTEROCHRONOMETRY, G.A. n. 772293). S.M. acknowledges support from the Ramon y Cajal fellowship number RYC-2015-17697. M.S.L. is supported by the Carlsberg Foundation (grant agreement No. CF17-0760). A.M. and P.R. acknowledge support from the HBCSE-NIUS programme. J.K.T. and J.T. acknowledge that support for this work was provided by NASA through Hubble Fellowship grants HST-HF2-51399.001 and HST-HF2-51424.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. T.S.R. acknowledges financial support from Premiale 2015 MITiC (PI B. Garilli). This project has been supported by the NKFIH K-115709 grant and the Lendület Program of the Hungarian Academy of Sciences, project No. LP2018-7/2018.\r\n\r\nBased on observations made with the Hertzsprung SONG telescope operated on the Spanish Observatorio del Teide on the island of Tenerife by the Aarhus and Copenhagen Universities and by the Instituto de Astrofísica de Canarias. Funding for the TESS mission is provided by NASA's Science Mission directorate. We acknowledge the use of public TESS Alert data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. This research has made use of the Exoplanet Follow-up Observation Program website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST).\r\n\r\nSoftware: Astropy (Astropy Collaboration et al. 2018), Matplotlib (Hunter 2007), DIAMONDS (Corsaro & De Ridder 2014), isoclassify (Huber et al. 2017), EXOFASTv2 (Eastman 2017), ktransit (Barclay 2018)."},{"acknowledgement":"The authors thank Róbert Szabó Paul G. Beck, Katrien Kolenberg, and Isabel L. Colman for helping on the classification of stars. This paper includes data collected by the Kepler mission and obtained from the MAST data archive at the Space Telescope Science Institute (STScI). Funding for the Kepler mission is provided by the National Aeronautics and Space Administration (NASA) Science Mission Directorate. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–26555. A.R.G.S. acknowledges the support from NASA under grant NNX17AF27G. R.A.G. and L.B. acknowledge the support from PLATO and GOLF CNES grants. S.M. acknowledges the support from the Ramon y Cajal fellowship number RYC-2015-17697. T.S.M. acknowledges support from a Visiting Fellowship at the Max Planck Institute for Solar System Research. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program.\r\n\r\nSoftware: KADACS (García et al. 2011), NumPy (van der Walt et al. 2011), SciPy (Jones et al. 2001), Matplotlib (Hunter 2007).\r\n\r\nFacilities: MAST - , Kepler Eclipsing Binary Catalog - , Exoplanet Archive. -","keyword":["Space and Planetary Science","Astronomy and Astrophysics","methods: data analysis","stars: activity","stars: low-mass","stars: rotation","starspots","techniques: photometric"],"language":[{"iso":"eng"}],"doi":"10.3847/1538-4365/ab3b56","citation":{"apa":"Santos, A. R. G., García, R. A., Mathur, S., Bugnet, L. A., van Saders, J. L., Metcalfe, T. S., … Pinsonneault, M. H. (2019). Surface rotation and photometric activity for Kepler targets. I. M and K main-sequence stars. <i>The Astrophysical Journal Supplement Series</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4365/ab3b56\">https://doi.org/10.3847/1538-4365/ab3b56</a>","ama":"Santos ARG, García RA, Mathur S, et al. Surface rotation and photometric activity for Kepler targets. I. M and K main-sequence stars. <i>The Astrophysical Journal Supplement Series</i>. 2019;244(1). doi:<a href=\"https://doi.org/10.3847/1538-4365/ab3b56\">10.3847/1538-4365/ab3b56</a>","short":"A.R.G. Santos, R.A. García, S. Mathur, L.A. Bugnet, J.L. van Saders, T.S. Metcalfe, G.V.A. Simonian, M.H. Pinsonneault, The Astrophysical Journal Supplement Series 244 (2019).","mla":"Santos, A. R. G., et al. “Surface Rotation and Photometric Activity for Kepler Targets. I. M and K Main-Sequence Stars.” <i>The Astrophysical Journal Supplement Series</i>, vol. 244, no. 1, 21, IOP Publishing, 2019, doi:<a href=\"https://doi.org/10.3847/1538-4365/ab3b56\">10.3847/1538-4365/ab3b56</a>.","ista":"Santos ARG, García RA, Mathur S, Bugnet LA, van Saders JL, Metcalfe TS, Simonian GVA, Pinsonneault MH. 2019. Surface rotation and photometric activity for Kepler targets. I. M and K main-sequence stars. The Astrophysical Journal Supplement Series. 244(1), 21.","ieee":"A. R. G. Santos <i>et al.</i>, “Surface rotation and photometric activity for Kepler targets. I. M and K main-sequence stars,” <i>The Astrophysical Journal Supplement Series</i>, vol. 244, no. 1. IOP Publishing, 2019.","chicago":"Santos, A. R. G., R. A. García, S. Mathur, Lisa Annabelle Bugnet, J. L. van Saders, T. S. Metcalfe, G. V. A. Simonian, and M. H. Pinsonneault. “Surface Rotation and Photometric Activity for Kepler Targets. I. M and K Main-Sequence Stars.” <i>The Astrophysical Journal Supplement Series</i>. IOP Publishing, 2019. <a href=\"https://doi.org/10.3847/1538-4365/ab3b56\">https://doi.org/10.3847/1538-4365/ab3b56</a>."},"title":"Surface rotation and photometric activity for Kepler targets. I. M and K main-sequence stars","day":"19","author":[{"last_name":"Santos","full_name":"Santos, A. R. G.","first_name":"A. R. G."},{"last_name":"García","full_name":"García, R. A.","first_name":"R. A."},{"last_name":"Mathur","first_name":"S.","full_name":"Mathur, S."},{"last_name":"Bugnet","first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","orcid":"0000-0003-0142-4000"},{"first_name":"J. L.","full_name":"van Saders, J. L.","last_name":"van Saders"},{"full_name":"Metcalfe, T. S.","first_name":"T. S.","last_name":"Metcalfe"},{"full_name":"Simonian, G. V. A.","first_name":"G. V. A.","last_name":"Simonian"},{"last_name":"Pinsonneault","full_name":"Pinsonneault, M. H.","first_name":"M. H."}],"type":"journal_article","publisher":"IOP Publishing","publication":"The Astrophysical Journal Supplement Series","quality_controlled":"1","intvolume":"       244","status":"public","month":"09","extern":"1","date_created":"2022-07-19T09:21:58Z","scopus_import":"1","external_id":{"arxiv":["1908.05222"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2022-08-22T08:10:38Z","publication_identifier":{"issn":["0067-0049"]},"article_type":"original","year":"2019","oa_version":"Preprint","publication_status":"published","main_file_link":[{"url":"https://arxiv.org/abs/1908.05222","open_access":"1"}],"oa":1,"volume":244,"arxiv":1,"article_processing_charge":"No","issue":"1","article_number":"21","_id":"11623","date_published":"2019-09-19T00:00:00Z","abstract":[{"text":"Brightness variations due to dark spots on the stellar surface encode information about stellar surface rotation and magnetic activity. In this work, we analyze the Kepler long-cadence data of 26,521 main-sequence stars of spectral types M and K in order to measure their surface rotation and photometric activity level. Rotation-period estimates are obtained by the combination of a wavelet analysis and autocorrelation function of the light curves. Reliable rotation estimates are determined by comparing the results from the different rotation diagnostics and four data sets. We also measure the photometric activity proxy Sph using the amplitude of the flux variations on an appropriate timescale. We report rotation periods and photometric activity proxies for about 60% of the sample, including 4431 targets for which McQuillan et al. did not report a rotation period. For the common targets with rotation estimates in this study and in McQuillan et al., our rotation periods agree within 99%. In this work, we also identify potential polluters, such as misclassified red giants and classical pulsator candidates. Within the parameter range we study, there is a mild tendency for hotter stars to have shorter rotation periods. The photometric activity proxy spans a wider range of values with increasing effective temperature. The rotation period and photometric activity proxy are also related, with Sph being larger for fast rotators. Similar to McQuillan et al., we find a bimodal distribution of rotation periods.","lang":"eng"}]},{"language":[{"iso":"eng"}],"keyword":["General Biochemistry","Genetics and Molecular Biology","General Physics and Astronomy","General Chemistry"],"doi":"10.1038/s41467-019-10490-9","pmid":1,"day":"19","type":"journal_article","author":[{"last_name":"Gauto","first_name":"Diego F.","full_name":"Gauto, Diego F."},{"first_name":"Leandro F.","full_name":"Estrozi, Leandro F.","last_name":"Estrozi"},{"full_name":"Schwieters, Charles D.","first_name":"Charles D.","last_name":"Schwieters"},{"full_name":"Effantin, Gregory","first_name":"Gregory","last_name":"Effantin"},{"last_name":"Macek","full_name":"Macek, Pavel","first_name":"Pavel"},{"full_name":"Sounier, Remy","first_name":"Remy","last_name":"Sounier"},{"first_name":"Astrid C.","full_name":"Sivertsen, Astrid C.","last_name":"Sivertsen"},{"last_name":"Schmidt","first_name":"Elena","full_name":"Schmidt, Elena"},{"last_name":"Kerfah","full_name":"Kerfah, Rime","first_name":"Rime"},{"first_name":"Guillaume","full_name":"Mas, Guillaume","last_name":"Mas"},{"last_name":"Colletier","first_name":"Jacques-Philippe","full_name":"Colletier, Jacques-Philippe"},{"first_name":"Peter","full_name":"Güntert, Peter","last_name":"Güntert"},{"full_name":"Favier, Adrien","first_name":"Adrien","last_name":"Favier"},{"last_name":"Schoehn","first_name":"Guy","full_name":"Schoehn, Guy"},{"id":"7B541462-FAF6-11E9-A490-E8DFE5697425","orcid":"0000-0002-9350-7606","last_name":"Schanda","first_name":"Paul","full_name":"Schanda, Paul"},{"full_name":"Boisbouvier, Jerome","first_name":"Jerome","last_name":"Boisbouvier"}],"citation":{"chicago":"Gauto, Diego F., Leandro F. Estrozi, Charles D. Schwieters, Gregory Effantin, Pavel Macek, Remy Sounier, Astrid C. Sivertsen, et al. “Integrated NMR and Cryo-EM Atomic-Resolution Structure Determination of a Half-Megadalton Enzyme Complex.” <i>Nature Communications</i>. Springer Nature, 2019. <a href=\"https://doi.org/10.1038/s41467-019-10490-9\">https://doi.org/10.1038/s41467-019-10490-9</a>.","ieee":"D. F. Gauto <i>et al.</i>, “Integrated NMR and cryo-EM atomic-resolution structure determination of a half-megadalton enzyme complex,” <i>Nature Communications</i>, vol. 10. Springer Nature, 2019.","ista":"Gauto DF, Estrozi LF, Schwieters CD, Effantin G, Macek P, Sounier R, Sivertsen AC, Schmidt E, Kerfah R, Mas G, Colletier J-P, Güntert P, Favier A, Schoehn G, Schanda P, Boisbouvier J. 2019. Integrated NMR and cryo-EM atomic-resolution structure determination of a half-megadalton enzyme complex. Nature Communications. 10, 2697.","mla":"Gauto, Diego F., et al. “Integrated NMR and Cryo-EM Atomic-Resolution Structure Determination of a Half-Megadalton Enzyme Complex.” <i>Nature Communications</i>, vol. 10, 2697, Springer Nature, 2019, doi:<a href=\"https://doi.org/10.1038/s41467-019-10490-9\">10.1038/s41467-019-10490-9</a>.","short":"D.F. Gauto, L.F. Estrozi, C.D. Schwieters, G. Effantin, P. Macek, R. Sounier, A.C. Sivertsen, E. Schmidt, R. Kerfah, G. Mas, J.-P. Colletier, P. Güntert, A. Favier, G. Schoehn, P. Schanda, J. Boisbouvier, Nature Communications 10 (2019).","ama":"Gauto DF, Estrozi LF, Schwieters CD, et al. Integrated NMR and cryo-EM atomic-resolution structure determination of a half-megadalton enzyme complex. <i>Nature Communications</i>. 2019;10. doi:<a href=\"https://doi.org/10.1038/s41467-019-10490-9\">10.1038/s41467-019-10490-9</a>","apa":"Gauto, D. F., Estrozi, L. F., Schwieters, C. D., Effantin, G., Macek, P., Sounier, R., … Boisbouvier, J. (2019). Integrated NMR and cryo-EM atomic-resolution structure determination of a half-megadalton enzyme complex. <i>Nature Communications</i>. Springer Nature. <a href=\"https://doi.org/10.1038/s41467-019-10490-9\">https://doi.org/10.1038/s41467-019-10490-9</a>"},"title":"Integrated NMR and cryo-EM atomic-resolution structure determination of a half-megadalton enzyme complex","quality_controlled":"1","publication":"Nature Communications","intvolume":"        10","status":"public","publisher":"Springer Nature","extern":"1","month":"06","date_created":"2020-09-17T10:28:25Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2021-01-12T08:19:03Z","external_id":{"pmid":["31217444"]},"publication_identifier":{"issn":["2041-1723"]},"article_type":"original","year":"2019","oa_version":"Published Version","volume":10,"publication_status":"published","oa":1,"main_file_link":[{"open_access":"1","url":"https://doi.org/10.1038/s41467-019-10490-9"}],"article_number":"2697","abstract":[{"lang":"eng","text":"Atomic-resolution structure determination is crucial for understanding protein function. Cryo-EM and NMR spectroscopy both provide structural information, but currently cryo-EM does not routinely give access to atomic-level structural data, and, generally, NMR structure determination is restricted to small (<30 kDa) proteins. We introduce an integrated structure determination approach that simultaneously uses NMR and EM data to overcome the limits of each of these methods. The approach enables structure determination of the 468 kDa large dodecameric aminopeptidase TET2 to a precision and accuracy below 1 Å by combining secondary-structure information obtained from near-complete magic-angle-spinning NMR assignments of the 39 kDa-large subunits, distance restraints from backbone amides and ILV methyl groups, and a 4.1 Å resolution EM map. The resulting structure exceeds current standards of NMR and EM structure determination in terms of molecular weight and precision. Importantly, the approach is successful even in cases where only medium-resolution cryo-EM data are available."}],"_id":"8405","date_published":"2019-06-19T00:00:00Z","article_processing_charge":"No"},{"date_created":"2023-08-03T10:13:52Z","month":"11","extern":"1","publisher":"EDP Sciences","intvolume":"       631","status":"public","publication":"Astronomy & Astrophysics","quality_controlled":"1","title":"The diverse lives of progenitors of hydrogen-rich core-collapse supernovae: The role of binary interaction","citation":{"mla":"Zapartas, Emmanouil, et al. “The Diverse Lives of Progenitors of Hydrogen-Rich Core-Collapse Supernovae: The Role of Binary Interaction.” <i>Astronomy &#38; Astrophysics</i>, vol. 631, A5, EDP Sciences, 2019, doi:<a href=\"https://doi.org/10.1051/0004-6361/201935854\">10.1051/0004-6361/201935854</a>.","ieee":"E. Zapartas <i>et al.</i>, “The diverse lives of progenitors of hydrogen-rich core-collapse supernovae: The role of binary interaction,” <i>Astronomy &#38; Astrophysics</i>, vol. 631. EDP Sciences, 2019.","ista":"Zapartas E, de Mink SE, Justham S, Smith N, de Koter A, Renzo M, Arcavi I, Farmer R, Götberg YLL, Toonen S. 2019. The diverse lives of progenitors of hydrogen-rich core-collapse supernovae: The role of binary interaction. Astronomy &#38; Astrophysics. 631, A5.","chicago":"Zapartas, Emmanouil, Selma E. de Mink, Stephen Justham, Nathan Smith, Alex de Koter, Mathieu Renzo, Iair Arcavi, Rob Farmer, Ylva Louise Linsdotter Götberg, and Silvia Toonen. “The Diverse Lives of Progenitors of Hydrogen-Rich Core-Collapse Supernovae: The Role of Binary Interaction.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2019. <a href=\"https://doi.org/10.1051/0004-6361/201935854\">https://doi.org/10.1051/0004-6361/201935854</a>.","apa":"Zapartas, E., de Mink, S. E., Justham, S., Smith, N., de Koter, A., Renzo, M., … Toonen, S. (2019). The diverse lives of progenitors of hydrogen-rich core-collapse supernovae: The role of binary interaction. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201935854\">https://doi.org/10.1051/0004-6361/201935854</a>","ama":"Zapartas E, de Mink SE, Justham S, et al. The diverse lives of progenitors of hydrogen-rich core-collapse supernovae: The role of binary interaction. <i>Astronomy &#38; Astrophysics</i>. 2019;631. doi:<a href=\"https://doi.org/10.1051/0004-6361/201935854\">10.1051/0004-6361/201935854</a>","short":"E. Zapartas, S.E. de Mink, S. Justham, N. Smith, A. de Koter, M. Renzo, I. Arcavi, R. Farmer, Y.L.L. Götberg, S. Toonen, Astronomy &#38; Astrophysics 631 (2019)."},"type":"journal_article","author":[{"first_name":"Emmanouil","full_name":"Zapartas, Emmanouil","last_name":"Zapartas"},{"first_name":"Selma E.","full_name":"de Mink, Selma E.","last_name":"de Mink"},{"last_name":"Justham","full_name":"Justham, Stephen","first_name":"Stephen"},{"last_name":"Smith","first_name":"Nathan","full_name":"Smith, Nathan"},{"first_name":"Alex","full_name":"de Koter, Alex","last_name":"de Koter"},{"full_name":"Renzo, Mathieu","first_name":"Mathieu","last_name":"Renzo"},{"last_name":"Arcavi","full_name":"Arcavi, Iair","first_name":"Iair"},{"last_name":"Farmer","first_name":"Rob","full_name":"Farmer, Rob"},{"last_name":"Götberg","full_name":"Götberg, Ylva Louise Linsdotter","first_name":"Ylva Louise Linsdotter","orcid":"0000-0002-6960-6911","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d"},{"first_name":"Silvia","full_name":"Toonen, Silvia","last_name":"Toonen"}],"day":"20","doi":"10.1051/0004-6361/201935854","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"language":[{"iso":"eng"}],"article_processing_charge":"No","arxiv":1,"abstract":[{"text":"Hydrogen-rich supernovae, known as Type II (SNe II), are the most common class of explosions observed following the collapse of the core of massive stars. We used analytical estimates and population synthesis simulations to assess the fraction of SNe II progenitors that are expected to have exchanged mass with a companion prior to explosion. We estimate that 1/3 to 1/2 of SN II progenitors have a history of mass exchange with a binary companion before exploding. The dominant binary channels leading to SN II progenitors involve the merger of binary stars. Mergers are expected to produce a diversity of SN II progenitor characteristics, depending on the evolutionary timing and properties of the merger. Alternatively, SN II progenitors from interacting binaries may have accreted mass from their companion, and subsequently been ejected from the binary system after their companion exploded. We show that the overall fraction of SN II progenitors that are predicted to have experienced binary interaction is robust against the main physical uncertainties in our models. However, the relative importance of different binary evolutionary channels is affected by changing physical assumptions. We further discuss ways in which binarity might contribute to the observed diversity of SNe II by considering potential observational signatures arising from each binary channel. For supernovae which have a substantial H-rich envelope at explosion (i.e., excluding Type IIb SNe), a surviving non-compact companion would typically indicate that the supernova progenitor star was in a wide, non-interacting binary. We argue that a significant fraction of even Type II-P SNe are expected to have gained mass from a companion prior to explosion.","lang":"eng"}],"_id":"13468","date_published":"2019-11-20T00:00:00Z","article_number":"A5","oa":1,"main_file_link":[{"url":"https://doi.org/10.1051/0004-6361/201935854","open_access":"1"}],"publication_status":"published","volume":631,"oa_version":"Published Version","year":"2019","article_type":"original","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"scopus_import":"1","external_id":{"arxiv":["1907.06687"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2023-08-09T12:36:09Z"},{"article_type":"original","year":"2019","oa_version":"Published Version","scopus_import":"1","external_id":{"arxiv":["1908.06102"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2023-08-09T12:34:11Z","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"arxiv":1,"article_processing_charge":"No","article_number":"A134","abstract":[{"text":"Stars stripped of their envelopes from interaction with a binary companion emit a significant fraction of their radiation as ionizing photons. They are potentially important stellar sources of ionizing radiation, however, they are still often neglected in spectral synthesis simulations or simulations of stellar feedback. In anticipating the large datasets of galaxy spectra from the upcoming James Webb Space Telescope, we modeled the radiative contribution from stripped stars by using detailed evolutionary and spectral models. We estimated their impact on the integrated spectra and specifically on the emission rates of H I-, He I-, and He II-ionizing photons from stellar populations. We find that stripped stars have the largest impact on the ionizing spectrum of a population in which star formation halted several Myr ago. In such stellar populations, stripped stars dominate the emission of ionizing photons, mimicking a younger stellar population in which massive stars are still present. Our models also suggest that stripped stars have harder ionizing spectra than massive stars. The additional ionizing radiation, with which stripped stars contribute affects observable properties that are related to the emission of ionizing photons from stellar populations. In co-eval stellar populations, the ionizing radiation from stripped stars increases the ionization parameter and the production efficiency of hydrogen ionizing photons. They also cause high values for these parameters for about ten times longer than what is predicted for massive stars. The effect on properties related to non-ionizing wavelengths is less pronounced, such as on the ultraviolet continuum slope or stellar contribution to emission lines. However, the hard ionizing radiation from stripped stars likely introduces a characteristic ionization structure of the nebula, which leads to the emission of highly ionized elements such as O2+ and C3+. We, therefore, expect that the presence of stripped stars affects the location in the BPT diagram and the diagnostic ratio of O III to O II nebular emission lines. Our models are publicly available through CDS database and on the STARBURST99 website.","lang":"eng"}],"_id":"13469","date_published":"2019-09-17T00:00:00Z","publication_status":"published","main_file_link":[{"url":"https://doi.org/10.1051/0004-6361/201834525","open_access":"1"}],"oa":1,"volume":629,"citation":{"short":"Y.L.L. Götberg, S.E. de Mink, J.H. Groh, C. Leitherer, C. Norman, Astronomy &#38; Astrophysics 629 (2019).","apa":"Götberg, Y. L. L., de Mink, S. E., Groh, J. H., Leitherer, C., &#38; Norman, C. (2019). The impact of stars stripped in binaries on the integrated spectra of stellar populations. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201834525\">https://doi.org/10.1051/0004-6361/201834525</a>","ama":"Götberg YLL, de Mink SE, Groh JH, Leitherer C, Norman C. The impact of stars stripped in binaries on the integrated spectra of stellar populations. <i>Astronomy &#38; Astrophysics</i>. 2019;629. doi:<a href=\"https://doi.org/10.1051/0004-6361/201834525\">10.1051/0004-6361/201834525</a>","ieee":"Y. L. L. Götberg, S. E. de Mink, J. H. Groh, C. Leitherer, and C. Norman, “The impact of stars stripped in binaries on the integrated spectra of stellar populations,” <i>Astronomy &#38; Astrophysics</i>, vol. 629. EDP Sciences, 2019.","ista":"Götberg YLL, de Mink SE, Groh JH, Leitherer C, Norman C. 2019. The impact of stars stripped in binaries on the integrated spectra of stellar populations. Astronomy &#38; Astrophysics. 629, A134.","chicago":"Götberg, Ylva Louise Linsdotter, S. E. de Mink, J. H. Groh, C. Leitherer, and C. Norman. “The Impact of Stars Stripped in Binaries on the Integrated Spectra of Stellar Populations.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2019. <a href=\"https://doi.org/10.1051/0004-6361/201834525\">https://doi.org/10.1051/0004-6361/201834525</a>.","mla":"Götberg, Ylva Louise Linsdotter, et al. “The Impact of Stars Stripped in Binaries on the Integrated Spectra of Stellar Populations.” <i>Astronomy &#38; Astrophysics</i>, vol. 629, A134, EDP Sciences, 2019, doi:<a href=\"https://doi.org/10.1051/0004-6361/201834525\">10.1051/0004-6361/201834525</a>."},"title":"The impact of stars stripped in binaries on the integrated spectra of stellar populations","day":"17","author":[{"id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","orcid":"0000-0002-6960-6911","last_name":"Götberg","full_name":"Götberg, Ylva Louise Linsdotter","first_name":"Ylva Louise Linsdotter"},{"last_name":"de Mink","full_name":"de Mink, S. E.","first_name":"S. E."},{"last_name":"Groh","first_name":"J. H.","full_name":"Groh, J. H."},{"first_name":"C.","full_name":"Leitherer, C.","last_name":"Leitherer"},{"last_name":"Norman","first_name":"C.","full_name":"Norman, C."}],"type":"journal_article","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"language":[{"iso":"eng"}],"doi":"10.1051/0004-6361/201834525","month":"09","extern":"1","date_created":"2023-08-03T10:14:00Z","publisher":"EDP Sciences","publication":"Astronomy & Astrophysics","quality_controlled":"1","status":"public","intvolume":"       629"},{"oa":1,"main_file_link":[{"url":"https://doi.org/10.1051/0004-6361/201935684","open_access":"1"}],"publication_status":"published","volume":627,"article_processing_charge":"No","date_published":"2019-07-16T00:00:00Z","_id":"13470","abstract":[{"text":"Context. Massive Wolf–Rayet (WR) stars dominate the radiative and mechanical energy budget of galaxies and probe a critical phase in the evolution of massive stars prior to core collapse. It is not known whether core He-burning WR stars (classical WR; cWR) form predominantly through wind stripping (w-WR) or binary stripping (b-WR). Whereas spectroscopy of WR binaries has so-far largely been avoided because of its complexity, our study focuses on the 44 WR binaries and binary candidates of the Large Magellanic Cloud (LMC; metallicity Z ≈ 0.5 Z⊙), which were identified on the basis of radial velocity variations, composite spectra, or high X-ray luminosities.\r\n\r\nAims. Relying on a diverse spectroscopic database, we aim to derive the physical and orbital parameters of our targets, confronting evolution models of evolved massive stars at subsolar metallicity and constraining the impact of binary interaction in forming these stars.\r\n\r\nMethods. Spectroscopy was performed using the Potsdam Wolf–Rayet (PoWR) code and cross-correlation techniques. Disentanglement was performed using the code Spectangular or the shift-and-add algorithm. Evolutionary status was interpreted using the Binary Population and Spectral Synthesis (BPASS) code, exploring binary interaction and chemically homogeneous evolution.\r\n\r\nResults. Among our sample, 28/44 objects show composite spectra and are analyzed as such. An additional five targets show periodically moving WR primaries but no detected companions (SB1); two (BAT99 99 and 112) are potential WR + compact-object candidates owing to their high X-ray luminosities. We cannot confirm the binary nature of the remaining 11 candidates. About two-thirds of the WN components in binaries are identified as cWR, and one-third as hydrogen-burning WR stars. We establish metallicity-dependent mass-loss recipes, which broadly agree with those recently derived for single WN stars, and in which so-called WN3/O3 stars are clear outliers. We estimate that 45  ±  30% of the cWR stars in our sample have interacted with a companion via mass transfer. However, only ≈12  ±  7% of the cWR stars in our sample naively appear to have formed purely owing to stripping via a companion (12% b-WR). Assuming that apparently single WR stars truly formed as single stars, this comprises ≈4% of the whole LMC WN population, which is about ten times less than expected. No obvious differences in the properties of single and binary WN stars, whose luminosities extend down to log L ≈ 5.2 [L⊙], are apparent. With the exception of a few systems (BAT99 19, 49, and 103), the equatorial rotational velocities of the OB-type companions are moderate (veq ≲ 250 km s−1) and challenge standard formalisms of angular-momentum accretion. For most objects, chemically homogeneous evolution can be rejected for the secondary, but not for the WR progenitor.\r\n\r\nConclusions. No obvious dichotomy in the locations of apparently single and binary WN stars on the Hertzsprung-Russell diagram is apparent. According to commonly used stellar evolution models (BPASS, Geneva), most apparently single WN stars could not have formed as single stars, implying that they were stripped by an undetected companion. Otherwise, it must follow that pre-WR mass-loss/mixing (e.g., during the red supergiant phase) are strongly underestimated in standard stellar evolution models.","lang":"eng"}],"article_number":"A151","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"date_updated":"2023-08-09T12:29:58Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","scopus_import":"1","year":"2019","oa_version":"Published Version","article_type":"original","publisher":"EDP Sciences","status":"public","intvolume":"       627","quality_controlled":"1","publication":"Astronomy & Astrophysics","date_created":"2023-08-03T10:14:09Z","extern":"1","month":"07","related_material":{"link":[{"url":"https://doi.org/10.1051/0004-6361/201935684e","relation":"erratum"}]},"doi":"10.1051/0004-6361/201935684","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"title":"The Wolf–Rayet binaries of the nitrogen sequence in the Large Magellanic Cloud","citation":{"ista":"Shenar T, Sablowski DP, Hainich R, Todt H, Moffat AFJ, Oskinova LM, Ramachandran V, Sana H, Sander AAC, Schnurr O, St-Louis N, Vanbeveren D, Götberg YLL, Hamann W-R. 2019. The Wolf–Rayet binaries of the nitrogen sequence in the Large Magellanic Cloud. Astronomy &#38; Astrophysics. 627, A151.","ieee":"T. Shenar <i>et al.</i>, “The Wolf–Rayet binaries of the nitrogen sequence in the Large Magellanic Cloud,” <i>Astronomy &#38; Astrophysics</i>, vol. 627. EDP Sciences, 2019.","chicago":"Shenar, T., D. P. Sablowski, R. Hainich, H. Todt, A. F. J. Moffat, L. M. Oskinova, V. Ramachandran, et al. “The Wolf–Rayet Binaries of the Nitrogen Sequence in the Large Magellanic Cloud.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2019. <a href=\"https://doi.org/10.1051/0004-6361/201935684\">https://doi.org/10.1051/0004-6361/201935684</a>.","mla":"Shenar, T., et al. “The Wolf–Rayet Binaries of the Nitrogen Sequence in the Large Magellanic Cloud.” <i>Astronomy &#38; Astrophysics</i>, vol. 627, A151, EDP Sciences, 2019, doi:<a href=\"https://doi.org/10.1051/0004-6361/201935684\">10.1051/0004-6361/201935684</a>.","short":"T. Shenar, D.P. Sablowski, R. Hainich, H. Todt, A.F.J. Moffat, L.M. Oskinova, V. Ramachandran, H. Sana, A.A.C. Sander, O. Schnurr, N. St-Louis, D. Vanbeveren, Y.L.L. Götberg, W.-R. Hamann, Astronomy &#38; Astrophysics 627 (2019).","apa":"Shenar, T., Sablowski, D. P., Hainich, R., Todt, H., Moffat, A. F. J., Oskinova, L. M., … Hamann, W.-R. (2019). The Wolf–Rayet binaries of the nitrogen sequence in the Large Magellanic Cloud. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201935684\">https://doi.org/10.1051/0004-6361/201935684</a>","ama":"Shenar T, Sablowski DP, Hainich R, et al. The Wolf–Rayet binaries of the nitrogen sequence in the Large Magellanic Cloud. <i>Astronomy &#38; Astrophysics</i>. 2019;627. doi:<a href=\"https://doi.org/10.1051/0004-6361/201935684\">10.1051/0004-6361/201935684</a>"},"author":[{"full_name":"Shenar, T.","first_name":"T.","last_name":"Shenar"},{"full_name":"Sablowski, D. P.","first_name":"D. P.","last_name":"Sablowski"},{"last_name":"Hainich","first_name":"R.","full_name":"Hainich, R."},{"last_name":"Todt","full_name":"Todt, H.","first_name":"H."},{"last_name":"Moffat","first_name":"A. F. J.","full_name":"Moffat, A. F. J."},{"last_name":"Oskinova","first_name":"L. M.","full_name":"Oskinova, L. M."},{"first_name":"V.","full_name":"Ramachandran, V.","last_name":"Ramachandran"},{"last_name":"Sana","first_name":"H.","full_name":"Sana, H."},{"last_name":"Sander","first_name":"A. A. C.","full_name":"Sander, A. A. C."},{"first_name":"O.","full_name":"Schnurr, O.","last_name":"Schnurr"},{"full_name":"St-Louis, N.","first_name":"N.","last_name":"St-Louis"},{"first_name":"D.","full_name":"Vanbeveren, D.","last_name":"Vanbeveren"},{"last_name":"Götberg","first_name":"Ylva Louise Linsdotter","full_name":"Götberg, Ylva Louise Linsdotter","orcid":"0000-0002-6960-6911","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d"},{"first_name":"W.-R.","full_name":"Hamann, W.-R.","last_name":"Hamann"}],"type":"journal_article","day":"16"},{"doi":"10.1051/0004-6361/201833297","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"title":"Massive runaway and walkaway stars","citation":{"ieee":"M. Renzo <i>et al.</i>, “Massive runaway and walkaway stars,” <i>Astronomy &#38; Astrophysics</i>, vol. 624. EDP Sciences, 2019.","ista":"Renzo M, Zapartas E, de Mink SE, Götberg YLL, Justham S, Farmer RJ, Izzard RG, Toonen S, Sana H. 2019. Massive runaway and walkaway stars. Astronomy &#38; Astrophysics. 624, A66.","chicago":"Renzo, M., E. Zapartas, S. E. de Mink, Ylva Louise Linsdotter Götberg, S. Justham, R. J. Farmer, R. G. Izzard, S. Toonen, and H. Sana. “Massive Runaway and Walkaway Stars.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2019. <a href=\"https://doi.org/10.1051/0004-6361/201833297\">https://doi.org/10.1051/0004-6361/201833297</a>.","mla":"Renzo, M., et al. “Massive Runaway and Walkaway Stars.” <i>Astronomy &#38; Astrophysics</i>, vol. 624, A66, EDP Sciences, 2019, doi:<a href=\"https://doi.org/10.1051/0004-6361/201833297\">10.1051/0004-6361/201833297</a>.","short":"M. Renzo, E. Zapartas, S.E. de Mink, Y.L.L. Götberg, S. Justham, R.J. Farmer, R.G. Izzard, S. Toonen, H. Sana, Astronomy &#38; Astrophysics 624 (2019).","apa":"Renzo, M., Zapartas, E., de Mink, S. E., Götberg, Y. L. L., Justham, S., Farmer, R. J., … Sana, H. (2019). Massive runaway and walkaway stars. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201833297\">https://doi.org/10.1051/0004-6361/201833297</a>","ama":"Renzo M, Zapartas E, de Mink SE, et al. Massive runaway and walkaway stars. <i>Astronomy &#38; Astrophysics</i>. 2019;624. doi:<a href=\"https://doi.org/10.1051/0004-6361/201833297\">10.1051/0004-6361/201833297</a>"},"type":"journal_article","author":[{"full_name":"Renzo, M.","first_name":"M.","last_name":"Renzo"},{"full_name":"Zapartas, E.","first_name":"E.","last_name":"Zapartas"},{"full_name":"de Mink, S. E.","first_name":"S. E.","last_name":"de Mink"},{"first_name":"Ylva Louise Linsdotter","full_name":"Götberg, Ylva Louise Linsdotter","last_name":"Götberg","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","orcid":"0000-0002-6960-6911"},{"last_name":"Justham","first_name":"S.","full_name":"Justham, S."},{"last_name":"Farmer","full_name":"Farmer, R. J.","first_name":"R. J."},{"last_name":"Izzard","full_name":"Izzard, R. G.","first_name":"R. G."},{"last_name":"Toonen","full_name":"Toonen, S.","first_name":"S."},{"last_name":"Sana","first_name":"H.","full_name":"Sana, H."}],"day":"11","publisher":"EDP Sciences","status":"public","intvolume":"       624","quality_controlled":"1","publication":"Astronomy & Astrophysics","date_created":"2023-08-03T10:14:18Z","extern":"1","month":"04","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"date_updated":"2023-08-09T12:26:08Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","external_id":{"arxiv":["1804.09164"]},"scopus_import":"1","year":"2019","oa_version":"Published Version","article_type":"original","main_file_link":[{"url":"https://doi.org/10.1051/0004-6361/201833297","open_access":"1"}],"oa":1,"publication_status":"published","volume":624,"article_processing_charge":"No","arxiv":1,"abstract":[{"text":"We perform an extensive numerical study of the evolution of massive binary systems to predict the peculiar velocities that stars obtain when their companion collapses and disrupts the system. Our aim is to (i) identify which predictions are robust against model uncertainties and assess their implications, (ii) investigate which physical processes leave a clear imprint and may therefore be constrained observationally, and (iii) provide a suite of publicly available model predictions to allow for the use of kinematic constraints from the Gaia mission. We find that 22+26−8% of all massive binary systems merge prior to the first core-collapse in the system. Of the remainder, 86+11−9% become unbound because of the core-collapse. Remarkably, this rarely produces runaway stars (observationally defined as stars with velocities above 30 km s−1). These are outnumbered by more than an order of magnitude by slower unbound companions, or “walkaway stars”. This is a robust outcome of our simulations and is due to the reversal of the mass ratio prior to the explosion and widening of the orbit, as we show analytically and numerically. For stars more massive than 15 M⊙, we estimate that 10+5−8% are walkaways and only 0.5+1.0−0.4% are runaways, nearly all of which have accreted mass from their companion. Our findings are consistent with earlier studies; however, the low runaway fraction we find is in tension with observed fractions of about 10%. Thus, astrometric data on presently single massive stars can potentially constrain the physics of massive binary evolution. Finally, we show that the high end of the mass distributions of runaway stars is very sensitive to the assumed black hole natal kicks, and we propose this as a potentially stringent test for the explosion mechanism. We also discuss companions remaining bound that can evolve into X-ray and gravitational wave sources.","lang":"eng"}],"_id":"13471","date_published":"2019-04-11T00:00:00Z","article_number":"A66"},{"volume":623,"oa":1,"main_file_link":[{"url":"https://doi.org/10.1051/0004-6361/201732206","open_access":"1"}],"publication_status":"published","abstract":[{"text":"Massive stars in binaries can give rise to extreme phenomena such as X-ray binaries and gravitational wave sources after one or both stars end their lives as core-collapse supernovae. Stars in close orbit around a stellar or compact companion are expected to explode as “stripped-envelope supernovae”, showing no (Type Ib/c) or little (Type IIb) signs of hydrogen in the spectra, because hydrogen-rich progenitors are too large to fit. The physical processes responsible for the stripping process and the fate of the companion are still very poorly understood. Aiming to find new clues, we investigate Cas A, which is a very young (∼340 yr) and near (∼3.4 kpc) remnant of a core-collapse supernova. Cas A has been subject to several searches for possible companions, all unsuccessfully. We present new measurements of the proper motions and photometry of stars in the vicinity based on deep HST ACS/WFC and WFC3-IR data. We identify stellar sources that are close enough in projection but using their proper motions we show that none are compatible with being at the location of center at the time of explosion, in agreement with earlier findings. Our photometric measurements allow us to place much deeper (order-of-magnitude) upper limits on the brightness of possible undetected companions. We systematically compare them with model predictions for a wide variety of scenarios. We can confidently rule out the presence of any stellar companion of any reasonable mass and age (main sequence, pre main sequence or stripped) ruling out what many considered to be likely evolutionary scenarios for Type IIb supernova (SN IIb). More exotic scenarios that predict the presence of a compact companion (white dwarf, neutron star or black hole) are still possible as well as scenarios where the progenitor of Cas A was single at the moment of explosion (either because it was truly single, or resulted from a binary that was disrupted, or from a binary merger). The presence of a compact companion would imply that Cas A is of interest to study exotic outcomes of binary evolution. The single-at-death solution would still require fine-tuning of the process that removed most of the envelope through a mass-loss mechanism yet to be identified. We discuss how future constraints from Gaia and even deeper photometric studies may help to place further constraints.","lang":"eng"}],"_id":"13472","date_published":"2019-03-27T00:00:00Z","article_number":"A34","article_processing_charge":"No","arxiv":1,"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"date_updated":"2023-08-09T12:28:17Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","external_id":{"arxiv":["1711.00055"]},"scopus_import":"1","oa_version":"Published Version","year":"2019","article_type":"original","status":"public","intvolume":"       623","quality_controlled":"1","publication":"Astronomy & Astrophysics","publisher":"EDP Sciences","date_created":"2023-08-03T10:14:27Z","extern":"1","month":"03","doi":"10.1051/0004-6361/201732206","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"type":"journal_article","author":[{"last_name":"Kerzendorf","first_name":"Wolfgang E.","full_name":"Kerzendorf, Wolfgang E."},{"last_name":"Do","full_name":"Do, Tuan","first_name":"Tuan"},{"last_name":"de Mink","full_name":"de Mink, Selma E.","first_name":"Selma E."},{"orcid":"0000-0002-6960-6911","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","first_name":"Ylva Louise Linsdotter","full_name":"Götberg, Ylva Louise Linsdotter","last_name":"Götberg"},{"first_name":"Dan","full_name":"Milisavljevic, Dan","last_name":"Milisavljevic"},{"full_name":"Zapartas, Emmanouil","first_name":"Emmanouil","last_name":"Zapartas"},{"first_name":"Mathieu","full_name":"Renzo, Mathieu","last_name":"Renzo"},{"full_name":"Justham, Stephen","first_name":"Stephen","last_name":"Justham"},{"first_name":"Philipp","full_name":"Podsiadlowski, Philipp","last_name":"Podsiadlowski"},{"last_name":"Fesen","full_name":"Fesen, Robert A.","first_name":"Robert A."}],"day":"27","title":"No surviving non-compact stellar companion to Cassiopeia A","citation":{"ama":"Kerzendorf WE, Do T, de Mink SE, et al. No surviving non-compact stellar companion to Cassiopeia A. <i>Astronomy &#38; Astrophysics</i>. 2019;623. doi:<a href=\"https://doi.org/10.1051/0004-6361/201732206\">10.1051/0004-6361/201732206</a>","apa":"Kerzendorf, W. E., Do, T., de Mink, S. E., Götberg, Y. L. L., Milisavljevic, D., Zapartas, E., … Fesen, R. A. (2019). No surviving non-compact stellar companion to Cassiopeia A. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201732206\">https://doi.org/10.1051/0004-6361/201732206</a>","short":"W.E. Kerzendorf, T. Do, S.E. de Mink, Y.L.L. Götberg, D. Milisavljevic, E. Zapartas, M. Renzo, S. Justham, P. Podsiadlowski, R.A. Fesen, Astronomy &#38; Astrophysics 623 (2019).","mla":"Kerzendorf, Wolfgang E., et al. “No Surviving Non-Compact Stellar Companion to Cassiopeia A.” <i>Astronomy &#38; Astrophysics</i>, vol. 623, A34, EDP Sciences, 2019, doi:<a href=\"https://doi.org/10.1051/0004-6361/201732206\">10.1051/0004-6361/201732206</a>.","chicago":"Kerzendorf, Wolfgang E., Tuan Do, Selma E. de Mink, Ylva Louise Linsdotter Götberg, Dan Milisavljevic, Emmanouil Zapartas, Mathieu Renzo, Stephen Justham, Philipp Podsiadlowski, and Robert A. Fesen. “No Surviving Non-Compact Stellar Companion to Cassiopeia A.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2019. <a href=\"https://doi.org/10.1051/0004-6361/201732206\">https://doi.org/10.1051/0004-6361/201732206</a>.","ista":"Kerzendorf WE, Do T, de Mink SE, Götberg YLL, Milisavljevic D, Zapartas E, Renzo M, Justham S, Podsiadlowski P, Fesen RA. 2019. No surviving non-compact stellar companion to Cassiopeia A. Astronomy &#38; Astrophysics. 623, A34.","ieee":"W. E. Kerzendorf <i>et al.</i>, “No surviving non-compact stellar companion to Cassiopeia A,” <i>Astronomy &#38; Astrophysics</i>, vol. 623. EDP Sciences, 2019."}},{"license":"https://creativecommons.org/licenses/by/4.0/","publication_status":"published","oa":1,"file_date_updated":"2021-02-02T13:47:21Z","tmp":{"legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","short":"CC BY (4.0)"},"volume":10,"arxiv":1,"article_processing_charge":"No","issue":"1","file":[{"checksum":"70c6e5d6fbea0932b0669505ab6633ec","date_updated":"2021-02-02T13:47:21Z","access_level":"open_access","file_name":"2019_NatureComm_Ramananarivo.pdf","file_size":2820337,"creator":"cziletti","date_created":"2021-02-02T13:47:21Z","success":1,"content_type":"application/pdf","relation":"main_file","file_id":"9061"}],"article_number":"3380","_id":"9060","date_published":"2019-07-29T00:00:00Z","abstract":[{"lang":"eng","text":"Molecular motors are essential to the living, generating fluctuations that boost transport and assist assembly. Active colloids, that consume energy to move, hold similar potential for man-made materials controlled by forces generated from within. Yet, their use as a powerhouse in materials science lacks. Here we show a massive acceleration of the annealing of a monolayer of passive beads by moderate addition of self-propelled microparticles. We rationalize our observations with a model of collisions that drive active fluctuations and activate the annealing. The experiment is quantitatively compared with Brownian dynamic simulations that further unveil a dynamical transition in the mechanism of annealing. Active dopants travel uniformly in the system or co-localize at the grain boundaries as a result of the persistence of their motion. Our findings uncover the potential of internal activity to control materials and lay the groundwork for the rise of materials science beyond equilibrium."}],"external_id":{"arxiv":["1909.07382"],"pmid":["31358762"]},"scopus_import":"1","date_updated":"2023-02-23T13:47:59Z","user_id":"D865714E-FA4E-11E9-B85B-F5C5E5697425","publication_identifier":{"issn":["2041-1723"]},"article_type":"original","has_accepted_license":"1","year":"2019","oa_version":"Published Version","publisher":"Springer Nature","publication":"Nature Communications","quality_controlled":"1","status":"public","intvolume":"        10","month":"07","extern":"1","date_created":"2021-02-02T13:43:36Z","pmid":1,"keyword":["General Biochemistry","Genetics and Molecular Biology","General Physics and Astronomy","General Chemistry"],"language":[{"iso":"eng"}],"doi":"10.1038/s41467-019-11362-y","ddc":["530"],"citation":{"ieee":"S. Ramananarivo, E. Ducrot, and J. A. Palacci, “Activity-controlled annealing of colloidal monolayers,” <i>Nature Communications</i>, vol. 10, no. 1. Springer Nature, 2019.","ista":"Ramananarivo S, Ducrot E, Palacci JA. 2019. Activity-controlled annealing of colloidal monolayers. Nature Communications. 10(1), 3380.","chicago":"Ramananarivo, Sophie, Etienne Ducrot, and Jérémie A Palacci. “Activity-Controlled Annealing of Colloidal Monolayers.” <i>Nature Communications</i>. Springer Nature, 2019. <a href=\"https://doi.org/10.1038/s41467-019-11362-y\">https://doi.org/10.1038/s41467-019-11362-y</a>.","mla":"Ramananarivo, Sophie, et al. “Activity-Controlled Annealing of Colloidal Monolayers.” <i>Nature Communications</i>, vol. 10, no. 1, 3380, Springer Nature, 2019, doi:<a href=\"https://doi.org/10.1038/s41467-019-11362-y\">10.1038/s41467-019-11362-y</a>.","short":"S. Ramananarivo, E. Ducrot, J.A. Palacci, Nature Communications 10 (2019).","apa":"Ramananarivo, S., Ducrot, E., &#38; Palacci, J. A. (2019). Activity-controlled annealing of colloidal monolayers. <i>Nature Communications</i>. Springer Nature. <a href=\"https://doi.org/10.1038/s41467-019-11362-y\">https://doi.org/10.1038/s41467-019-11362-y</a>","ama":"Ramananarivo S, Ducrot E, Palacci JA. Activity-controlled annealing of colloidal monolayers. <i>Nature Communications</i>. 2019;10(1). doi:<a href=\"https://doi.org/10.1038/s41467-019-11362-y\">10.1038/s41467-019-11362-y</a>"},"title":"Activity-controlled annealing of colloidal monolayers","day":"29","author":[{"last_name":"Ramananarivo","first_name":"Sophie","full_name":"Ramananarivo, Sophie"},{"last_name":"Ducrot","full_name":"Ducrot, Etienne","first_name":"Etienne"},{"id":"8fb92548-2b22-11eb-b7c1-a3f0d08d7c7d","orcid":"0000-0002-7253-9465","last_name":"Palacci","first_name":"Jérémie A","full_name":"Palacci, Jérémie A"}],"type":"journal_article"},{"day":"16","type":"journal_article","author":[{"full_name":"Zhou, H.","first_name":"H.","last_name":"Zhou"},{"full_name":"Polshyn, Hryhoriy","first_name":"Hryhoriy","last_name":"Polshyn","id":"edfc7cb1-526e-11ec-b05a-e6ecc27e4e48","orcid":"0000-0001-8223-8896"},{"first_name":"T.","full_name":"Taniguchi, T.","last_name":"Taniguchi"},{"last_name":"Watanabe","first_name":"K.","full_name":"Watanabe, K."},{"first_name":"A. F.","full_name":"Young, A. F.","last_name":"Young"}],"citation":{"mla":"Zhou, H., et al. “Solids of Quantum Hall Skyrmions in Graphene.” <i>Nature Physics</i>, vol. 16, no. 2, Springer Nature, 2019, pp. 154–58, doi:<a href=\"https://doi.org/10.1038/s41567-019-0729-8\">10.1038/s41567-019-0729-8</a>.","chicago":"Zhou, H., Hryhoriy Polshyn, T. Taniguchi, K. Watanabe, and A. F. Young. “Solids of Quantum Hall Skyrmions in Graphene.” <i>Nature Physics</i>. Springer Nature, 2019. <a href=\"https://doi.org/10.1038/s41567-019-0729-8\">https://doi.org/10.1038/s41567-019-0729-8</a>.","ista":"Zhou H, Polshyn H, Taniguchi T, Watanabe K, Young AF. 2019. Solids of quantum Hall skyrmions in graphene. Nature Physics. 16(2), 154–158.","ieee":"H. Zhou, H. Polshyn, T. Taniguchi, K. Watanabe, and A. F. Young, “Solids of quantum Hall skyrmions in graphene,” <i>Nature Physics</i>, vol. 16, no. 2. Springer Nature, pp. 154–158, 2019.","ama":"Zhou H, Polshyn H, Taniguchi T, Watanabe K, Young AF. Solids of quantum Hall skyrmions in graphene. <i>Nature Physics</i>. 2019;16(2):154-158. doi:<a href=\"https://doi.org/10.1038/s41567-019-0729-8\">10.1038/s41567-019-0729-8</a>","apa":"Zhou, H., Polshyn, H., Taniguchi, T., Watanabe, K., &#38; Young, A. F. (2019). Solids of quantum Hall skyrmions in graphene. <i>Nature Physics</i>. Springer Nature. <a href=\"https://doi.org/10.1038/s41567-019-0729-8\">https://doi.org/10.1038/s41567-019-0729-8</a>","short":"H. Zhou, H. Polshyn, T. Taniguchi, K. Watanabe, A.F. Young, Nature Physics 16 (2019) 154–158."},"title":"Solids of quantum Hall skyrmions in graphene","language":[{"iso":"eng"}],"keyword":["General Physics and Astronomy"],"doi":"10.1038/s41567-019-0729-8","acknowledgement":"We acknowledge discussions with B. Halperin, C. Huang, A. Macdonald and M. Zalatel. Experimental work at UCSB was supported by the Army Research Office under awards nos. MURI W911NF-16-1-0361 and W911NF-16-1-0482. K.W. and T.T. acknowledge support from the Elemental Strategy Initiative conducted by MEXT (Japan) and CREST (JPMJCR15F3), JST. A.F.Y. acknowledges the support of the David and Lucile Packard Foundation and and Alfred. P. Sloan Foundation.","extern":"1","month":"12","date_created":"2022-01-13T14:45:16Z","page":"154-158","quality_controlled":"1","publication":"Nature Physics","intvolume":"        16","status":"public","publisher":"Springer Nature","article_type":"original","year":"2019","oa_version":"None","user_id":"ea97e931-d5af-11eb-85d4-e6957dddbf17","date_updated":"2022-01-13T15:34:44Z","scopus_import":"1","publication_identifier":{"issn":["1745-2473"],"eissn":["1745-2481"]},"date_published":"2019-12-16T00:00:00Z","_id":"10620","abstract":[{"text":"Partially filled Landau levels host competing electronic orders. For example, electron solids may prevail close to integer filling of the Landau levels before giving way to fractional quantum Hall liquids at higher carrier density1,2. Here, we report the observation of an electron solid with non-collinear spin texture in monolayer graphene, consistent with solidification of skyrmions3—topological spin textures characterized by quantized electrical charge4,5. We probe the spin texture of the solids using a modified Corbino geometry that allows ferromagnetic magnons to be launched and detected6,7. We find that magnon transport is highly efficient when one Landau level is filled (ν=1), consistent with quantum Hall ferromagnetic spin polarization. However, even minimal doping immediately quenches the magnon signal while leaving the vanishing low-temperature charge conductivity unchanged. Our results can be understood by the formation of a solid of charged skyrmions near ν=1, whose non-collinear spin texture leads to rapid magnon decay. Data near fractional fillings show evidence of several fractional skyrmion solids, suggesting that graphene hosts a highly tunable landscape of coupled spin and charge orders.","lang":"eng"}],"issue":"2","article_processing_charge":"No","volume":16,"publication_status":"published"},{"status":"public","intvolume":"        15","publication":"Nature Physics","quality_controlled":"1","publisher":"Springer Nature","date_created":"2022-01-13T15:00:58Z","month":"08","extern":"1","page":"1011-1016","doi":"10.1038/s41567-019-0596-3","keyword":["general physics and astronomy"],"language":[{"iso":"eng"}],"acknowledgement":"The authors thank S. Das Sarma and F. Wu for sharing their unpublished theoretical results, and acknowledge further discussions with L. Balents and T. Senthil. Work at both Columbia and UCSB was funded by the Army Research Office under award W911NF-17-1-0323. Sample device design and fabrication was partially supported by DoE Pro-QM EFRC (DE-SC0019443). A.F.Y. and C.R.D. separately acknowledge the support of the David and Lucile Packard Foundation. K.W. and T.T. acknowledge support from the Elemental Strategy Initiative conducted by the MEXT, Japan and the CREST (JPMJCR15F3), JST. A portion of this work was carried out at the KITP, Santa Barbara, supported by the National Science Foundation under grant number NSF PHY-1748958.","author":[{"id":"edfc7cb1-526e-11ec-b05a-e6ecc27e4e48","orcid":"0000-0001-8223-8896","first_name":"Hryhoriy","full_name":"Polshyn, Hryhoriy","last_name":"Polshyn"},{"last_name":"Yankowitz","first_name":"Matthew","full_name":"Yankowitz, Matthew"},{"full_name":"Chen, Shaowen","first_name":"Shaowen","last_name":"Chen"},{"first_name":"Yuxuan","full_name":"Zhang, Yuxuan","last_name":"Zhang"},{"first_name":"K.","full_name":"Watanabe, K.","last_name":"Watanabe"},{"last_name":"Taniguchi","full_name":"Taniguchi, T.","first_name":"T."},{"last_name":"Dean","first_name":"Cory R.","full_name":"Dean, Cory R."},{"last_name":"Young","first_name":"Andrea F.","full_name":"Young, Andrea F."}],"type":"journal_article","day":"05","title":"Large linear-in-temperature resistivity in twisted bilayer graphene","citation":{"mla":"Polshyn, Hryhoriy, et al. “Large Linear-in-Temperature Resistivity in Twisted Bilayer Graphene.” <i>Nature Physics</i>, vol. 15, no. 10, Springer Nature, 2019, pp. 1011–16, doi:<a href=\"https://doi.org/10.1038/s41567-019-0596-3\">10.1038/s41567-019-0596-3</a>.","ieee":"H. Polshyn <i>et al.</i>, “Large linear-in-temperature resistivity in twisted bilayer graphene,” <i>Nature Physics</i>, vol. 15, no. 10. Springer Nature, pp. 1011–1016, 2019.","ista":"Polshyn H, Yankowitz M, Chen S, Zhang Y, Watanabe K, Taniguchi T, Dean CR, Young AF. 2019. Large linear-in-temperature resistivity in twisted bilayer graphene. Nature Physics. 15(10), 1011–1016.","chicago":"Polshyn, Hryhoriy, Matthew Yankowitz, Shaowen Chen, Yuxuan Zhang, K. Watanabe, T. Taniguchi, Cory R. Dean, and Andrea F. Young. “Large Linear-in-Temperature Resistivity in Twisted Bilayer Graphene.” <i>Nature Physics</i>. Springer Nature, 2019. <a href=\"https://doi.org/10.1038/s41567-019-0596-3\">https://doi.org/10.1038/s41567-019-0596-3</a>.","apa":"Polshyn, H., Yankowitz, M., Chen, S., Zhang, Y., Watanabe, K., Taniguchi, T., … Young, A. F. (2019). Large linear-in-temperature resistivity in twisted bilayer graphene. <i>Nature Physics</i>. Springer Nature. <a href=\"https://doi.org/10.1038/s41567-019-0596-3\">https://doi.org/10.1038/s41567-019-0596-3</a>","ama":"Polshyn H, Yankowitz M, Chen S, et al. Large linear-in-temperature resistivity in twisted bilayer graphene. <i>Nature Physics</i>. 2019;15(10):1011-1016. doi:<a href=\"https://doi.org/10.1038/s41567-019-0596-3\">10.1038/s41567-019-0596-3</a>","short":"H. Polshyn, M. Yankowitz, S. Chen, Y. Zhang, K. Watanabe, T. Taniguchi, C.R. Dean, A.F. Young, Nature Physics 15 (2019) 1011–1016."},"volume":15,"main_file_link":[{"url":"https://arxiv.org/abs/1902.00763","open_access":"1"}],"oa":1,"publication_status":"published","_id":"10621","abstract":[{"text":"Twisted bilayer graphene has recently emerged as a platform for hosting correlated phenomena. For twist angles near θ ≈ 1.1°, the low-energy electronic structure of twisted bilayer graphene features isolated bands with a flat dispersion1,2. Recent experiments have observed a variety of low-temperature phases that appear to be driven by electron interactions, including insulating states, superconductivity and magnetism3,4,5,6. Here we report electrical transport measurements up to room temperature for twist angles varying between 0.75° and 2°. We find that the resistivity, ρ, scales linearly with temperature, T, over a wide range of T before falling again owing to interband activation. The T-linear response is much larger than observed in monolayer graphene for all measured devices, and in particular increases by more than three orders of magnitude in the range where the flat band exists. Our results point to the dominant role of electron–phonon scattering in twisted bilayer graphene, with possible implications for the origin of the observed superconductivity.","lang":"eng"}],"date_published":"2019-08-05T00:00:00Z","article_processing_charge":"No","issue":"10","arxiv":1,"publication_identifier":{"eissn":["1745-2481"],"issn":["1745-2473"]},"scopus_import":"1","external_id":{"arxiv":["1902.00763"]},"user_id":"ea97e931-d5af-11eb-85d4-e6957dddbf17","date_updated":"2022-01-20T09:33:38Z","year":"2019","oa_version":"Preprint","article_type":"original"},{"doi":"10.1051/0004-6361/201833528","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift / galaxies: formation / dark ages / reionization / first stars / techniques: spectroscopic / intergalactic medium"],"language":[{"iso":"eng"}],"acknowledgement":"JM acknowledges the award of a Huygens PhD fellowship from Leiden University. MG acknowledges support from NASA grant NNX17AK58G. APA, PhD::SPACE fellow, acknowledges support from the FCT through the fellowship PD/BD/52706/2014. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 294.A-5018, 098.A-0819, 099.A-0254 and 0100.A-0213. We are grateful for the excellent data-sets from the COSMOS and UltraVISTA survey teams. This research was supported by the Munich Institute for Astro- and Particle Physics (MIAPP) of the DFG cluster of excellence “Origin and Structure of the Universe”. We thank the referee for their comments that improved the paper. We also thank Christoph Behrens, Len Cowie, Koki Kakiichi, Peter Laursen, Charlotte Mason, Eros Vanzella, Lewis Weinberger and Johannes Zabl for discussions. We have benefited from the public available programming language Python, including the numpy, matplotlib, scipy and astropy packages (Hunter 2007; Astropy Collaboration 2013), the astronomical imaging tools Swarp (Bertin 2010) and ds9 and the Topcat analysis tool (Taylor 2013).","type":"journal_article","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J"},{"first_name":"David","full_name":"Sobral, David","last_name":"Sobral"},{"last_name":"Gronke","full_name":"Gronke, Max","first_name":"Max"},{"first_name":"Ana","full_name":"Paulino-Afonso, Ana","last_name":"Paulino-Afonso"},{"last_name":"Stefanon","full_name":"Stefanon, Mauro","first_name":"Mauro"},{"full_name":"Röttgering, Huub","first_name":"Huub","last_name":"Röttgering"}],"day":"19","title":"Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly contributing to the reionisation of the universe","citation":{"ama":"Matthee JJ, Sobral D, Gronke M, Paulino-Afonso A, Stefanon M, Röttgering H. Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly contributing to the reionisation of the universe. <i>Astronomy &#38; Astrophysics</i>. 2018;619. doi:<a href=\"https://doi.org/10.1051/0004-6361/201833528\">10.1051/0004-6361/201833528</a>","apa":"Matthee, J. J., Sobral, D., Gronke, M., Paulino-Afonso, A., Stefanon, M., &#38; Röttgering, H. (2018). Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly contributing to the reionisation of the universe. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201833528\">https://doi.org/10.1051/0004-6361/201833528</a>","short":"J.J. Matthee, D. Sobral, M. Gronke, A. Paulino-Afonso, M. Stefanon, H. Röttgering, Astronomy &#38; Astrophysics 619 (2018).","mla":"Matthee, Jorryt J., et al. “Confirmation of Double Peaked Lyα Emission at z = 6.593: Witnessing a Galaxy Directly Contributing to the Reionisation of the Universe.” <i>Astronomy &#38; Astrophysics</i>, vol. 619, A136, EDP Sciences, 2018, doi:<a href=\"https://doi.org/10.1051/0004-6361/201833528\">10.1051/0004-6361/201833528</a>.","chicago":"Matthee, Jorryt J, David Sobral, Max Gronke, Ana Paulino-Afonso, Mauro Stefanon, and Huub Röttgering. “Confirmation of Double Peaked Lyα Emission at z = 6.593: Witnessing a Galaxy Directly Contributing to the Reionisation of the Universe.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2018. <a href=\"https://doi.org/10.1051/0004-6361/201833528\">https://doi.org/10.1051/0004-6361/201833528</a>.","ieee":"J. J. Matthee, D. Sobral, M. Gronke, A. Paulino-Afonso, M. Stefanon, and H. Röttgering, “Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly contributing to the reionisation of the universe,” <i>Astronomy &#38; Astrophysics</i>, vol. 619. EDP Sciences, 2018.","ista":"Matthee JJ, Sobral D, Gronke M, Paulino-Afonso A, Stefanon M, Röttgering H. 2018. Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly contributing to the reionisation of the universe. Astronomy &#38; Astrophysics. 619, A136."},"intvolume":"       619","status":"public","publication":"Astronomy & Astrophysics","quality_controlled":"1","publisher":"EDP Sciences","date_created":"2022-07-06T11:14:23Z","month":"11","extern":"1","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"scopus_import":"1","external_id":{"arxiv":["1805.11621"]},"date_updated":"2022-07-19T09:32:08Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","year":"2018","oa_version":"Published Version","article_type":"original","volume":619,"oa":1,"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1805.11621"}],"publication_status":"published","abstract":[{"text":"Distant luminous Lyman-α emitters (LAEs) are excellent targets for spectroscopic observations of galaxies in the epoch of reionisation (EoR). We present deep high-resolution (R = 5000) VLT/X-shooter observations, along with an extensive collection of photometric data of COLA1, a proposed double peaked LAE at z = 6.6. We rule out the possibility that COLA1’s emission line is an [OII] doublet at z = 1.475 on the basis of i) the asymmetric red line-profile and flux ratio of the peaks (blue/red=0.31 ± 0.03) and ii) an unphysical [OII]/Hα ratio ([OII]/Hα >  22). We show that COLA1’s observed B-band flux is explained by a faint extended foreground LAE, for which we detect Lyα and [OIII] at z = 2.142. We thus conclude that COLA1 is a real double-peaked LAE at z = 6.593, the first discovered at z >  6. COLA1 is UV luminous (M1500 = −21.6 ± 0.3), has a high equivalent width (EW0,Lyα = 120−40+50 Å) and very compact Lyα emission (r50,Lyα = 0.33−0.04+0.07 kpc). Relatively weak inferred Hβ+[OIII] line-emission from Spitzer/IRAC indicates an extremely low metallicity of Z <  1/20 Z⊙ or reduced strength of nebular lines due to high escape of ionising photons. The small Lyα peak separation of 220 ± 20 km s−1 implies a low HI column density and an ionising photon escape fraction of ≈15 − 30%, providing the first direct evidence that such galaxies contribute actively to the reionisation of the Universe at z >  6. Based on simple estimates, we find that COLA1 could have provided just enough photons to reionise its own ≈0.3 pMpc (2.3 cMpc) bubble, allowing the blue Lyα line to be observed. However, we also discuss alternative scenarios explaining the detected double peaked nature of COLA1. Our results show that future high-resolution observations of statistical samples of double peaked LAEs at z >  5 are a promising probe of the occurrence of ionised regions around galaxies in the EoR.","lang":"eng"}],"_id":"11508","date_published":"2018-11-19T00:00:00Z","article_number":"A136","article_processing_charge":"No","arxiv":1}]