[{"citation":{"short":"G. Ivanov, Canadian Mathematical Bulletin 64 (2021) 942–963.","ama":"Ivanov G. Tight frames and related geometric problems. <i>Canadian Mathematical Bulletin</i>. 2021;64(4):942-963. doi:<a href=\"https://doi.org/10.4153/s000843952000096x\">10.4153/s000843952000096x</a>","ieee":"G. Ivanov, “Tight frames and related geometric problems,” <i>Canadian Mathematical Bulletin</i>, vol. 64, no. 4. Canadian Mathematical Society, pp. 942–963, 2021.","chicago":"Ivanov, Grigory. “Tight Frames and Related Geometric Problems.” <i>Canadian Mathematical Bulletin</i>. Canadian Mathematical Society, 2021. <a href=\"https://doi.org/10.4153/s000843952000096x\">https://doi.org/10.4153/s000843952000096x</a>.","mla":"Ivanov, Grigory. “Tight Frames and Related Geometric Problems.” <i>Canadian Mathematical Bulletin</i>, vol. 64, no. 4, Canadian Mathematical Society, 2021, pp. 942–63, doi:<a href=\"https://doi.org/10.4153/s000843952000096x\">10.4153/s000843952000096x</a>.","ista":"Ivanov G. 2021. Tight frames and related geometric problems. Canadian Mathematical Bulletin. 64(4), 942–963.","apa":"Ivanov, G. (2021). Tight frames and related geometric problems. <i>Canadian Mathematical Bulletin</i>. Canadian Mathematical Society. <a href=\"https://doi.org/10.4153/s000843952000096x\">https://doi.org/10.4153/s000843952000096x</a>"},"intvolume":"        64","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1804.10055"}],"scopus_import":"1","oa_version":"Preprint","date_published":"2021-12-18T00:00:00Z","publication_status":"published","doi":"10.4153/s000843952000096x","month":"12","status":"public","oa":1,"publication_identifier":{"issn":["0008-4395"],"eissn":["1496-4287"]},"_id":"10860","date_updated":"2023-09-05T12:43:09Z","arxiv":1,"abstract":[{"text":"A tight frame is the orthogonal projection of some orthonormal basis of Rn onto Rk. We show that a set of vectors is a tight frame if and only if the set of all cross products of these vectors is a tight frame. We reformulate a range of problems on the volume of projections (or sections) of regular polytopes in terms of tight frames and write a first-order necessary condition for local extrema of these problems. As applications, we prove new results for the problem of maximization of the volume of zonotopes.","lang":"eng"}],"issue":"4","year":"2021","external_id":{"arxiv":["1804.10055"],"isi":["000730165300021"]},"keyword":["General Mathematics","Tight frame","Grassmannian","zonotope"],"quality_controlled":"1","volume":64,"article_processing_charge":"No","article_type":"original","type":"journal_article","language":[{"iso":"eng"}],"department":[{"_id":"UlWa"}],"page":"942-963","date_created":"2022-03-18T09:55:59Z","publication":"Canadian Mathematical Bulletin","publisher":"Canadian Mathematical Society","user_id":"c635000d-4b10-11ee-a964-aac5a93f6ac1","title":"Tight frames and related geometric problems","author":[{"full_name":"Ivanov, Grigory","first_name":"Grigory","id":"87744F66-5C6F-11EA-AFE0-D16B3DDC885E","last_name":"Ivanov"}],"isi":1,"acknowledgement":"The author was supported by the Swiss National Science Foundation grant 200021_179133. The author acknowledges the financial support from the Ministry of Education and Science of the Russian Federation in the framework of MegaGrant no. 075-15-2019-1926.","day":"18"},{"language":[{"iso":"eng"}],"department":[{"_id":"GaTk"}],"date_published":"2021-08-17T00:00:00Z","type":"preprint","oa_version":"Preprint","date_created":"2022-03-21T11:41:28Z","page":"37","publication_status":"submitted","doi":"10.48550/ARXIV.2108.06686","external_id":{"arxiv":["2108.06686"]},"citation":{"chicago":"Lombardi, Fabrizio, Selver Pepic, Oren Shriki, Gašper Tkačik, and Daniele De Martino. “Quantifying the Coexistence of Neuronal Oscillations and Avalanches.” arXiv, n.d. <a href=\"https://doi.org/10.48550/ARXIV.2108.06686\">https://doi.org/10.48550/ARXIV.2108.06686</a>.","apa":"Lombardi, F., Pepic, S., Shriki, O., Tkačik, G., &#38; De Martino, D. (n.d.). Quantifying the coexistence of neuronal oscillations and avalanches. arXiv. <a href=\"https://doi.org/10.48550/ARXIV.2108.06686\">https://doi.org/10.48550/ARXIV.2108.06686</a>","mla":"Lombardi, Fabrizio, et al. <i>Quantifying the Coexistence of Neuronal Oscillations and Avalanches</i>. arXiv, doi:<a href=\"https://doi.org/10.48550/ARXIV.2108.06686\">10.48550/ARXIV.2108.06686</a>.","ista":"Lombardi F, Pepic S, Shriki O, Tkačik G, De Martino D. Quantifying the coexistence of neuronal oscillations and avalanches. <a href=\"https://doi.org/10.48550/ARXIV.2108.06686\">10.48550/ARXIV.2108.06686</a>.","short":"F. Lombardi, S. Pepic, O. Shriki, G. Tkačik, D. De Martino, (n.d.).","ama":"Lombardi F, Pepic S, Shriki O, Tkačik G, De Martino D. Quantifying the coexistence of neuronal oscillations and avalanches. doi:<a href=\"https://doi.org/10.48550/ARXIV.2108.06686\">10.48550/ARXIV.2108.06686</a>","ieee":"F. Lombardi, S. Pepic, O. Shriki, G. Tkačik, and D. De Martino, “Quantifying the coexistence of neuronal oscillations and avalanches.” arXiv."},"ddc":["570"],"main_file_link":[{"url":"https://arxiv.org/abs/2108.06686","open_access":"1"}],"article_processing_charge":"No","_id":"10912","project":[{"name":"ISTplus - Postdoctoral Fellowships","call_identifier":"H2020","grant_number":"754411","_id":"260C2330-B435-11E9-9278-68D0E5697425"},{"name":"Efficient coding with biophysical realism","_id":"626c45b5-2b32-11ec-9570-e509828c1ba6","grant_number":"P34015"}],"author":[{"full_name":"Lombardi, Fabrizio","orcid":"0000-0003-2623-5249","first_name":"Fabrizio","last_name":"Lombardi","id":"A057D288-3E88-11E9-986D-0CF4E5697425"},{"full_name":"Pepic, Selver","first_name":"Selver","id":"F93245C4-C3CA-11E9-B4F0-C6F4E5697425","last_name":"Pepic"},{"first_name":"Oren","last_name":"Shriki","full_name":"Shriki, Oren"},{"id":"3D494DCA-F248-11E8-B48F-1D18A9856A87","last_name":"Tkačik","first_name":"Gašper","orcid":"0000-0002-6699-1455","full_name":"Tkačik, Gašper"},{"last_name":"De Martino","first_name":"Daniele","full_name":"De Martino, Daniele"}],"day":"17","year":"2021","date_updated":"2022-03-22T07:53:18Z","abstract":[{"text":"Brain dynamics display collective phenomena as diverse as neuronal oscillations and avalanches. Oscillations are rhythmic, with fluctuations occurring at a characteristic scale, whereas avalanches are scale-free cascades of neural activity. Here we show that such antithetic features can coexist in a very generic class of adaptive neural networks. In the most simple yet fully microscopic model from this class we make direct contact with human brain resting-state activity recordings via tractable inference of the model's two essential parameters. The inferred model quantitatively captures the dynamics over a broad range of scales, from single sensor fluctuations, collective behaviors of nearly-synchronous extreme events on multiple sensors, to neuronal avalanches unfolding over multiple sensors across multiple time-bins. Importantly, the inferred parameters correlate with model-independent signatures of \"closeness to criticality\", suggesting that the coexistence of scale-specific (neural oscillations) and scale-free (neuronal avalanches) dynamics in brain activity occurs close to a non-equilibrium critical point at the onset of self-sustained oscillations.","lang":"eng"}],"acknowledgement":"FL acknowledges support from the European Union’s Horizon 2020 research and innovation program under the Marie Sklodowska-Curie Grant Agreement No. 754411. GT\r\nacknowledges the support of the Austrian Science Fund (FWF) under Stand-Alone Grant\r\nNo. P34015.","arxiv":1,"ec_funded":1,"month":"08","title":"Quantifying the coexistence of neuronal oscillations and avalanches","oa":1,"publisher":"arXiv","status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87"},{"_id":"11053","date_updated":"2022-07-18T08:27:24Z","issue":"5","abstract":[{"lang":"eng","text":"Understanding basic mechanisms of aging holds great promise for developing interventions that prevent or delay many age-related declines and diseases simultaneously to increase human healthspan. However, a major confounding factor in aging research is the heterogeneity of the aging process itself. At the organismal level, it is clear that chronological age does not always predict biological age or susceptibility to frailty or pathology. While genetics and environment are major factors driving variable rates of aging, additional complexity arises because different organs, tissues, and cell types are intrinsically heterogeneous and exhibit different aging trajectories normally or in response to the stresses of the aging process (e.g., damage accumulation). Tackling the heterogeneity of aging requires new and specialized tools (e.g., single-cell analyses, mass spectrometry-based approaches, and advanced imaging) to identify novel signatures of aging across scales. Cutting-edge computational approaches are then needed to integrate these disparate datasets and elucidate network interactions between known aging hallmarks. There is also a need for improved, human cell-based models of aging to ensure that basic research findings are relevant to human aging and healthspan interventions. The San Diego Nathan Shock Center (SD-NSC) provides access to cutting-edge scientific resources to facilitate the study of the heterogeneity of aging in general and to promote the use of novel human cell models of aging. The center also has a robust Research Development Core that funds pilot projects on the heterogeneity of aging and organizes innovative training activities, including workshops and a personalized mentoring program, to help investigators new to the aging field succeed. Finally, the SD-NSC participates in outreach activities to educate the general community about the importance of aging research and promote the need for basic biology of aging research in particular."}],"year":"2021","month":"10","status":"public","publication_identifier":{"issn":["2509-2715","2509-2723"]},"oa":1,"oa_version":"Published Version","date_published":"2021-10-01T00:00:00Z","publication_status":"published","doi":"10.1007/s11357-021-00426-x","intvolume":"        43","citation":{"short":"G.S. Shadel, P.D. Adams, W.T. Berggren, J.K. Diedrich, K.E. Diffenderfer, F.H. Gage, N. Hah, M. Hansen, M. Hetzer, A.J.A. Molina, U. Manor, K. Marek, D.D. O’Keefe, A.F.M. Pinto, A. Sacco, T.O. Sharpee, M.N. Shokriev, S. Zambetti, GeroScience 43 (2021) 2139–2148.","ieee":"G. S. Shadel <i>et al.</i>, “The San Diego Nathan Shock Center: Tackling the heterogeneity of aging,” <i>GeroScience</i>, vol. 43, no. 5. Springer Nature, pp. 2139–2148, 2021.","ama":"Shadel GS, Adams PD, Berggren WT, et al. The San Diego Nathan Shock Center: Tackling the heterogeneity of aging. <i>GeroScience</i>. 2021;43(5):2139-2148. doi:<a href=\"https://doi.org/10.1007/s11357-021-00426-x\">10.1007/s11357-021-00426-x</a>","chicago":"Shadel, Gerald S., Peter D. Adams, W. Travis Berggren, Jolene K. Diedrich, Kenneth E. Diffenderfer, Fred H. Gage, Nasun Hah, et al. “The San Diego Nathan Shock Center: Tackling the Heterogeneity of Aging.” <i>GeroScience</i>. Springer Nature, 2021. <a href=\"https://doi.org/10.1007/s11357-021-00426-x\">https://doi.org/10.1007/s11357-021-00426-x</a>.","apa":"Shadel, G. S., Adams, P. D., Berggren, W. T., Diedrich, J. K., Diffenderfer, K. E., Gage, F. H., … Zambetti, S. (2021). The San Diego Nathan Shock Center: Tackling the heterogeneity of aging. <i>GeroScience</i>. Springer Nature. <a href=\"https://doi.org/10.1007/s11357-021-00426-x\">https://doi.org/10.1007/s11357-021-00426-x</a>","ista":"Shadel GS, Adams PD, Berggren WT, Diedrich JK, Diffenderfer KE, Gage FH, Hah N, Hansen M, Hetzer M, Molina AJA, Manor U, Marek K, O’Keefe DD, Pinto AFM, Sacco A, Sharpee TO, Shokriev MN, Zambetti S. 2021. The San Diego Nathan Shock Center: Tackling the heterogeneity of aging. GeroScience. 43(5), 2139–2148.","mla":"Shadel, Gerald S., et al. “The San Diego Nathan Shock Center: Tackling the Heterogeneity of Aging.” <i>GeroScience</i>, vol. 43, no. 5, Springer Nature, 2021, pp. 2139–48, doi:<a href=\"https://doi.org/10.1007/s11357-021-00426-x\">10.1007/s11357-021-00426-x</a>."},"scopus_import":"1","main_file_link":[{"open_access":"1","url":"https://www.ncbi.nlm.nih.gov/pmc/articles/PMC8599742/"}],"author":[{"last_name":"Shadel","first_name":"Gerald S.","full_name":"Shadel, Gerald S."},{"first_name":"Peter D.","last_name":"Adams","full_name":"Adams, Peter D."},{"full_name":"Berggren, W. Travis","last_name":"Berggren","first_name":"W. Travis"},{"last_name":"Diedrich","first_name":"Jolene K.","full_name":"Diedrich, Jolene K."},{"first_name":"Kenneth E.","last_name":"Diffenderfer","full_name":"Diffenderfer, Kenneth E."},{"first_name":"Fred H.","last_name":"Gage","full_name":"Gage, Fred H."},{"last_name":"Hah","first_name":"Nasun","full_name":"Hah, Nasun"},{"last_name":"Hansen","first_name":"Malene","full_name":"Hansen, Malene"},{"full_name":"HETZER, Martin W","first_name":"Martin W","orcid":"0000-0002-2111-992X","id":"86c0d31b-b4eb-11ec-ac5a-eae7b2e135ed","last_name":"HETZER"},{"first_name":"Anthony J. A.","last_name":"Molina","full_name":"Molina, Anthony J. A."},{"full_name":"Manor, Uri","first_name":"Uri","last_name":"Manor"},{"first_name":"Kurt","last_name":"Marek","full_name":"Marek, Kurt"},{"last_name":"O’Keefe","first_name":"David D.","full_name":"O’Keefe, David D."},{"last_name":"Pinto","first_name":"Antonio F. M.","full_name":"Pinto, Antonio F. M."},{"first_name":"Alessandra","last_name":"Sacco","full_name":"Sacco, Alessandra"},{"full_name":"Sharpee, Tatyana O.","last_name":"Sharpee","first_name":"Tatyana O."},{"last_name":"Shokriev","first_name":"Maxim N.","full_name":"Shokriev, Maxim N."},{"full_name":"Zambetti, Stefania","first_name":"Stefania","last_name":"Zambetti"}],"pmid":1,"day":"01","extern":"1","publisher":"Springer Nature","user_id":"72615eeb-f1f3-11ec-aa25-d4573ddc34fd","title":"The San Diego Nathan Shock Center: Tackling the heterogeneity of aging","type":"journal_article","language":[{"iso":"eng"}],"date_created":"2022-04-07T07:43:25Z","page":"2139-2148","publication":"GeroScience","external_id":{"pmid":["34370163"]},"quality_controlled":"1","volume":43,"keyword":["Geriatrics and Gerontology","Aging"],"article_processing_charge":"No","article_type":"original"},{"date_updated":"2022-06-07T06:53:36Z","issue":"9B","abstract":[{"text":"Asynchronous distributed algorithms are a popular way to reduce synchronization costs in large-scale optimization, and in particular for neural network training. However, for nonsmooth and nonconvex objectives, few convergence guarantees exist beyond cases where closed-form proximal operator solutions are available. As training most popular deep neural networks corresponds to optimizing nonsmooth and nonconvex objectives, there is a pressing need for such convergence guarantees. In this paper, we analyze for the first time the convergence of stochastic asynchronous optimization for this general class of objectives. In particular, we focus on stochastic subgradient methods allowing for block variable partitioning, where the shared model is asynchronously updated by concurrent processes. To this end, we use a probabilistic model which captures key features of real asynchronous scheduling between concurrent processes. Under this model, we establish convergence with probability one to an invariant set for stochastic subgradient methods with momentum. From a practical perspective, one issue with the family of algorithms that we consider is that they are not efficiently supported by machine learning frameworks, which mostly focus on distributed data-parallel strategies. To address this, we propose a new implementation strategy for shared-memory based training of deep neural networks for a partitioned but shared model in single- and multi-GPU settings. Based on this implementation, we achieve on average1.2x speed-up in comparison to state-of-the-art training methods for popular image classification tasks, without compromising accuracy.","lang":"eng"}],"arxiv":1,"year":"2021","_id":"11436","status":"public","publication_identifier":{"isbn":["9781713835974"],"eissn":["2374-3468"],"issn":["2159-5399"]},"oa":1,"month":"05","ec_funded":1,"publication_status":"published","conference":{"location":"Virtual, Online","end_date":"2021-02-09","name":"AAAI: Conference on Artificial Intelligence","start_date":"2021-02-02"},"oa_version":"Preprint","date_published":"2021-05-18T00:00:00Z","main_file_link":[{"url":" https://doi.org/10.48550/arXiv.1905.11845","open_access":"1"}],"scopus_import":"1","citation":{"chicago":"Kungurtsev, Vyacheslav, Malcolm Egan, Bapi Chatterjee, and Dan-Adrian Alistarh. “Asynchronous Optimization Methods for Efficient Training of Deep Neural Networks with Guarantees.” In <i>35th AAAI Conference on Artificial Intelligence, AAAI 2021</i>, 35:8209–16. AAAI Press, 2021.","ista":"Kungurtsev V, Egan M, Chatterjee B, Alistarh D-A. 2021. Asynchronous optimization methods for efficient training of deep neural networks with guarantees. 35th AAAI Conference on Artificial Intelligence, AAAI 2021. AAAI: Conference on Artificial Intelligence vol. 35, 8209–8216.","apa":"Kungurtsev, V., Egan, M., Chatterjee, B., &#38; Alistarh, D.-A. (2021). Asynchronous optimization methods for efficient training of deep neural networks with guarantees. In <i>35th AAAI Conference on Artificial Intelligence, AAAI 2021</i> (Vol. 35, pp. 8209–8216). Virtual, Online: AAAI Press.","mla":"Kungurtsev, Vyacheslav, et al. “Asynchronous Optimization Methods for Efficient Training of Deep Neural Networks with Guarantees.” <i>35th AAAI Conference on Artificial Intelligence, AAAI 2021</i>, vol. 35, no. 9B, AAAI Press, 2021, pp. 8209–16.","ieee":"V. Kungurtsev, M. Egan, B. Chatterjee, and D.-A. Alistarh, “Asynchronous optimization methods for efficient training of deep neural networks with guarantees,” in <i>35th AAAI Conference on Artificial Intelligence, AAAI 2021</i>, Virtual, Online, 2021, vol. 35, no. 9B, pp. 8209–8216.","ama":"Kungurtsev V, Egan M, Chatterjee B, Alistarh D-A. Asynchronous optimization methods for efficient training of deep neural networks with guarantees. In: <i>35th AAAI Conference on Artificial Intelligence, AAAI 2021</i>. Vol 35. AAAI Press; 2021:8209-8216.","short":"V. Kungurtsev, M. Egan, B. Chatterjee, D.-A. Alistarh, in:, 35th AAAI Conference on Artificial Intelligence, AAAI 2021, AAAI Press, 2021, pp. 8209–8216."},"intvolume":"        35","acknowledgement":"Vyacheslav Kungurtsev was supported by the OP VVV project CZ.02.1.01/0.0/0.0/16 019/0000765 “Research Center for Informatics. Bapi Chatterjee was supported by the European Union’s Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant agreement No. 754411 (ISTPlus). Dan Alistarh has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No 805223 ScaleML).","day":"18","project":[{"call_identifier":"H2020","name":"ISTplus - Postdoctoral Fellowships","_id":"260C2330-B435-11E9-9278-68D0E5697425","grant_number":"754411"},{"grant_number":"805223","_id":"268A44D6-B435-11E9-9278-68D0E5697425","name":"Elastic Coordination for Scalable Machine Learning","call_identifier":"H2020"}],"author":[{"last_name":"Kungurtsev","first_name":"Vyacheslav","full_name":"Kungurtsev, Vyacheslav"},{"last_name":"Egan","first_name":"Malcolm","full_name":"Egan, Malcolm"},{"full_name":"Chatterjee, Bapi","id":"3C41A08A-F248-11E8-B48F-1D18A9856A87","last_name":"Chatterjee","first_name":"Bapi"},{"full_name":"Alistarh, Dan-Adrian","id":"4A899BFC-F248-11E8-B48F-1D18A9856A87","last_name":"Alistarh","first_name":"Dan-Adrian","orcid":"0000-0003-3650-940X"}],"publisher":"AAAI Press","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","title":"Asynchronous optimization methods for efficient training of deep neural networks with guarantees","page":"8209-8216","date_created":"2022-06-05T22:01:52Z","publication":"35th AAAI Conference on Artificial Intelligence, AAAI 2021","type":"conference","language":[{"iso":"eng"}],"department":[{"_id":"DaAl"}],"article_processing_charge":"No","external_id":{"arxiv":["1905.11845"]},"volume":35,"quality_controlled":"1"},{"arxiv":1,"abstract":[{"lang":"eng","text":"We study efficient distributed algorithms for the fundamental problem of principal component analysis and leading eigenvector computation on the sphere, when the data are randomly distributed among a set of computational nodes. We propose a new quantized variant of Riemannian gradient descent to solve this problem, and prove that the algorithm converges with high probability under a set of necessary spherical-convexity properties. We give bounds on the number of bits transmitted by the algorithm under common initialization schemes, and investigate the dependency on the problem dimension in each case."}],"date_updated":"2022-06-20T08:31:52Z","year":"2021","_id":"11452","status":"public","oa":1,"publication_identifier":{"isbn":["9781713845393"],"issn":["1049-5258"]},"month":"12","ec_funded":1,"publication_status":"published","conference":{"name":"NeurIPS: Neural Information Processing Systems","start_date":"2021-12-06","location":"Virtual, Online","end_date":"2021-12-14"},"oa_version":"Published Version","date_published":"2021-12-01T00:00:00Z","main_file_link":[{"url":"https://proceedings.neurips.cc/paper/2021/file/1680e9fa7b4dd5d62ece800239bb53bd-Paper.pdf","open_access":"1"}],"scopus_import":"1","intvolume":"         4","citation":{"short":"F. Alimisis, P. Davies, B. Vandereycken, D.-A. Alistarh, in:, Advances in Neural Information Processing Systems - 35th Conference on Neural Information Processing Systems, Neural Information Processing Systems Foundation, 2021, pp. 2823–2834.","ieee":"F. Alimisis, P. Davies, B. Vandereycken, and D.-A. Alistarh, “Distributed principal component analysis with limited communication,” in <i>Advances in Neural Information Processing Systems - 35th Conference on Neural Information Processing Systems</i>, Virtual, Online, 2021, vol. 4, pp. 2823–2834.","ama":"Alimisis F, Davies P, Vandereycken B, Alistarh D-A. Distributed principal component analysis with limited communication. In: <i>Advances in Neural Information Processing Systems - 35th Conference on Neural Information Processing Systems</i>. Vol 4. Neural Information Processing Systems Foundation; 2021:2823-2834.","apa":"Alimisis, F., Davies, P., Vandereycken, B., &#38; Alistarh, D.-A. (2021). Distributed principal component analysis with limited communication. In <i>Advances in Neural Information Processing Systems - 35th Conference on Neural Information Processing Systems</i> (Vol. 4, pp. 2823–2834). Virtual, Online: Neural Information Processing Systems Foundation.","mla":"Alimisis, Foivos, et al. “Distributed Principal Component Analysis with Limited Communication.” <i>Advances in Neural Information Processing Systems - 35th Conference on Neural Information Processing Systems</i>, vol. 4, Neural Information Processing Systems Foundation, 2021, pp. 2823–34.","ista":"Alimisis F, Davies P, Vandereycken B, Alistarh D-A. 2021. Distributed principal component analysis with limited communication. Advances in Neural Information Processing Systems - 35th Conference on Neural Information Processing Systems. NeurIPS: Neural Information Processing Systems vol. 4, 2823–2834.","chicago":"Alimisis, Foivos, Peter Davies, Bart Vandereycken, and Dan-Adrian Alistarh. “Distributed Principal Component Analysis with Limited Communication.” In <i>Advances in Neural Information Processing Systems - 35th Conference on Neural Information Processing Systems</i>, 4:2823–34. Neural Information Processing Systems Foundation, 2021."},"acknowledgement":"We would like to thank the anonymous reviewers for helpful comments and suggestions. We also thank Aurelien Lucchi and Antonio Orvieto for fruitful discussions at an early stage of this work. FA is partially supported by the SNSF under research project No. 192363 and conducted part of this work while at IST Austria under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 805223 ScaleML). PD partly conducted this work while at IST Austria and was supported by the European Union’s Horizon 2020 programme under the Marie Skłodowska-Curie grant agreement No. 754411.","day":"01","author":[{"full_name":"Alimisis, Foivos","last_name":"Alimisis","first_name":"Foivos"},{"full_name":"Davies, Peter","first_name":"Peter","orcid":"0000-0002-5646-9524","last_name":"Davies","id":"11396234-BB50-11E9-B24C-90FCE5697425"},{"full_name":"Vandereycken, Bart","first_name":"Bart","last_name":"Vandereycken"},{"full_name":"Alistarh, Dan-Adrian","id":"4A899BFC-F248-11E8-B48F-1D18A9856A87","last_name":"Alistarh","orcid":"0000-0003-3650-940X","first_name":"Dan-Adrian"}],"project":[{"_id":"268A44D6-B435-11E9-9278-68D0E5697425","grant_number":"805223","name":"Elastic Coordination for Scalable Machine Learning","call_identifier":"H2020"},{"name":"ISTplus - Postdoctoral Fellowships","call_identifier":"H2020","_id":"260C2330-B435-11E9-9278-68D0E5697425","grant_number":"754411"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publisher":"Neural Information Processing Systems Foundation","title":"Distributed principal component analysis with limited communication","publication":"Advances in Neural Information Processing Systems - 35th Conference on Neural Information Processing Systems","page":"2823-2834","date_created":"2022-06-19T22:01:58Z","type":"conference","department":[{"_id":"DaAl"}],"language":[{"iso":"eng"}],"article_processing_charge":"No","quality_controlled":"1","volume":4,"external_id":{"arxiv":["2110.14391"]}},{"quality_controlled":"1","volume":20,"article_processing_charge":"No","language":[{"iso":"eng"}],"department":[{"_id":"TiVo"}],"type":"conference","date_created":"2022-06-19T22:01:59Z","page":"16437-16450","publication":"Advances in Neural Information Processing Systems - 35th Conference on Neural Information Processing Systems","title":"Online learning of neural computations from sparse temporal feedback","publisher":"Neural Information Processing Systems Foundation","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","project":[{"grant_number":"214316/Z/18/Z","_id":"c084a126-5a5b-11eb-8a69-d75314a70a87","name":"What’s in a memory? Spatiotemporal dynamics in strongly coupled recurrent neuronal networks."}],"author":[{"full_name":"Braun, Lukas","first_name":"Lukas","last_name":"Braun"},{"full_name":"Vogels, Tim P","last_name":"Vogels","id":"CB6FF8D2-008F-11EA-8E08-2637E6697425","orcid":"0000-0003-3295-6181","first_name":"Tim P"}],"day":"01","acknowledgement":"We would like to thank Professor Dr. Henning Sprekeler for his valuable suggestions and Dr. Andrew Saxe, Milan Klöwer and Anna Wallis for their constructive feedback on the manuscript. Lukas Braun was supported by the Network of European Neuroscience Schools through their NENS Exchange Grant program, by the European Union through their European Community Action Scheme for the Mobility of University Students, the Woodward Scholarship awarded by Wadham College, Oxford and the Medical Research Council [MR/N013468/1]. Tim P. Vogels was supported by a Wellcome Trust Senior Research Fellowship [214316/Z/18/Z].","intvolume":"        20","citation":{"short":"L. Braun, T.P. Vogels, in:, Advances in Neural Information Processing Systems - 35th Conference on Neural Information Processing Systems, Neural Information Processing Systems Foundation, 2021, pp. 16437–16450.","ieee":"L. Braun and T. P. Vogels, “Online learning of neural computations from sparse temporal feedback,” in <i>Advances in Neural Information Processing Systems - 35th Conference on Neural Information Processing Systems</i>, Virtual, Online, 2021, vol. 20, pp. 16437–16450.","ama":"Braun L, Vogels TP. Online learning of neural computations from sparse temporal feedback. In: <i>Advances in Neural Information Processing Systems - 35th Conference on Neural Information Processing Systems</i>. Vol 20. Neural Information Processing Systems Foundation; 2021:16437-16450.","chicago":"Braun, Lukas, and Tim P Vogels. “Online Learning of Neural Computations from Sparse Temporal Feedback.” In <i>Advances in Neural Information Processing Systems - 35th Conference on Neural Information Processing Systems</i>, 20:16437–50. Neural Information Processing Systems Foundation, 2021.","apa":"Braun, L., &#38; Vogels, T. P. (2021). Online learning of neural computations from sparse temporal feedback. In <i>Advances in Neural Information Processing Systems - 35th Conference on Neural Information Processing Systems</i> (Vol. 20, pp. 16437–16450). Virtual, Online: Neural Information Processing Systems Foundation.","ista":"Braun L, Vogels TP. 2021. Online learning of neural computations from sparse temporal feedback. Advances in Neural Information Processing Systems - 35th Conference on Neural Information Processing Systems. NeurIPS: Neural Information Processing Systems vol. 20, 16437–16450.","mla":"Braun, Lukas, and Tim P. Vogels. “Online Learning of Neural Computations from Sparse Temporal Feedback.” <i>Advances in Neural Information Processing Systems - 35th Conference on Neural Information Processing Systems</i>, vol. 20, Neural Information Processing Systems Foundation, 2021, pp. 16437–50."},"main_file_link":[{"url":"https://proceedings.neurips.cc/paper/2021/file/88e1ce84f9feef5a08d0df0334c53468-Paper.pdf","open_access":"1"}],"scopus_import":"1","date_published":"2021-12-01T00:00:00Z","oa_version":"Published Version","publication_status":"published","conference":{"name":"NeurIPS: Neural Information Processing Systems","start_date":"2021-12-06","location":"Virtual, Online","end_date":"2021-12-14"},"month":"12","publication_identifier":{"issn":["1049-5258"],"isbn":["9781713845393"]},"oa":1,"status":"public","_id":"11453","year":"2021","date_updated":"2022-06-20T07:12:58Z","abstract":[{"text":"Neuronal computations depend on synaptic connectivity and intrinsic electrophysiological properties. Synaptic connectivity determines which inputs from presynaptic neurons are integrated, while cellular properties determine how inputs are filtered over time. Unlike their biological counterparts, most computational approaches to learning in simulated neural networks are limited to changes in synaptic connectivity. However, if intrinsic parameters change, neural computations are altered drastically. Here, we include the parameters that determine the intrinsic properties,\r\ne.g., time constants and reset potential, into the learning paradigm. Using sparse feedback signals that indicate target spike times, and gradient-based parameter updates, we show that the intrinsic parameters can be learned along with the synaptic weights to produce specific input-output functions. Specifically, we use a teacher-student paradigm in which a randomly initialised leaky integrate-and-fire or resonate-and-fire neuron must recover the parameters of a teacher neuron. We show that complex temporal functions can be learned online and without backpropagation through time, relying on event-based updates only. Our results are a step towards online learning of neural computations from ungraded and unsigned sparse feedback signals with a biologically inspired learning mechanism.","lang":"eng"}]},{"language":[{"iso":"eng"}],"department":[{"_id":"GradSch"},{"_id":"DaAl"}],"type":"conference","page":"8557-8570","date_created":"2022-06-20T12:11:53Z","publication":"35th Conference on Neural Information Processing Systems","related_material":{"record":[{"relation":"dissertation_contains","status":"public","id":"13074"}]},"external_id":{"arxiv":["2106.12379"]},"volume":34,"quality_controlled":"1","article_processing_charge":"No","project":[{"_id":"268A44D6-B435-11E9-9278-68D0E5697425","grant_number":"805223","name":"Elastic Coordination for Scalable Machine Learning","call_identifier":"H2020"}],"author":[{"last_name":"Peste","id":"32D78294-F248-11E8-B48F-1D18A9856A87","first_name":"Elena-Alexandra","full_name":"Peste, Elena-Alexandra"},{"last_name":"Iofinova","id":"f9a17499-f6e0-11ea-865d-fdf9a3f77117","first_name":"Eugenia B","orcid":"0000-0002-7778-3221","full_name":"Iofinova, Eugenia B"},{"first_name":"Adrian","last_name":"Vladu","full_name":"Vladu, Adrian"},{"first_name":"Dan-Adrian","orcid":"0000-0003-3650-940X","id":"4A899BFC-F248-11E8-B48F-1D18A9856A87","last_name":"Alistarh","full_name":"Alistarh, Dan-Adrian"}],"day":"6","acknowledgement":"This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No 805223 ScaleML), and a CNRS PEPS grant. This research was supported by the Scientific Service Units (SSU) of IST Austria through resources provided by Scientific Computing (SciComp). We would also like to thank Christoph Lampert for his feedback on an earlier version of this work, as well as for providing hardware for the Transformer-XL experiments.","title":"AC/DC: Alternating Compressed/DeCompressed training of deep neural networks","publisher":"Curran Associates","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_published":"2021-12-06T00:00:00Z","oa_version":"Published Version","publication_status":"published","conference":{"location":"Virtual, Online","end_date":"2021-12-14","name":"NeurIPS: Neural Information Processing Systems","start_date":"2021-12-06"},"intvolume":"        34","citation":{"chicago":"Peste, Elena-Alexandra, Eugenia B Iofinova, Adrian Vladu, and Dan-Adrian Alistarh. “AC/DC: Alternating Compressed/DeCompressed Training of Deep Neural Networks.” In <i>35th Conference on Neural Information Processing Systems</i>, 34:8557–70. Curran Associates, 2021.","apa":"Peste, E.-A., Iofinova, E. B., Vladu, A., &#38; Alistarh, D.-A. (2021). AC/DC: Alternating Compressed/DeCompressed training of deep neural networks. In <i>35th Conference on Neural Information Processing Systems</i> (Vol. 34, pp. 8557–8570). Virtual, Online: Curran Associates.","mla":"Peste, Elena-Alexandra, et al. “AC/DC: Alternating Compressed/DeCompressed Training of Deep Neural Networks.” <i>35th Conference on Neural Information Processing Systems</i>, vol. 34, Curran Associates, 2021, pp. 8557–70.","ista":"Peste E-A, Iofinova EB, Vladu A, Alistarh D-A. 2021. AC/DC: Alternating Compressed/DeCompressed training of deep neural networks. 35th Conference on Neural Information Processing Systems. NeurIPS: Neural Information Processing Systems vol. 34, 8557–8570.","short":"E.-A. Peste, E.B. Iofinova, A. Vladu, D.-A. Alistarh, in:, 35th Conference on Neural Information Processing Systems, Curran Associates, 2021, pp. 8557–8570.","ieee":"E.-A. Peste, E. B. Iofinova, A. Vladu, and D.-A. Alistarh, “AC/DC: Alternating Compressed/DeCompressed training of deep neural networks,” in <i>35th Conference on Neural Information Processing Systems</i>, Virtual, Online, 2021, vol. 34, pp. 8557–8570.","ama":"Peste E-A, Iofinova EB, Vladu A, Alistarh D-A. AC/DC: Alternating Compressed/DeCompressed training of deep neural networks. In: <i>35th Conference on Neural Information Processing Systems</i>. Vol 34. Curran Associates; 2021:8557-8570."},"scopus_import":"1","main_file_link":[{"open_access":"1","url":"https://proceedings.neurips.cc/paper/2021/file/48000647b315f6f00f913caa757a70b3-Paper.pdf"}],"_id":"11458","acknowledged_ssus":[{"_id":"ScienComp"}],"year":"2021","date_updated":"2023-06-01T12:54:45Z","arxiv":1,"abstract":[{"text":"The increasing computational requirements of deep neural networks (DNNs) have led to significant interest in obtaining DNN models that are sparse, yet accurate. Recent work has investigated the even harder case of sparse training, where the DNN weights are, for as much as possible, already sparse to reduce computational costs during training. Existing sparse training methods are often empirical and can have lower accuracy relative to the dense baseline. In this paper, we present a general approach called Alternating Compressed/DeCompressed (AC/DC) training of DNNs, demonstrate convergence for a variant of the algorithm, and show that AC/DC outperforms existing sparse training methods in accuracy at similar computational budgets; at high sparsity levels, AC/DC even outperforms existing methods that rely on accurate pre-trained dense models. An important property of AC/DC is that it allows co-training of dense and sparse models, yielding accurate sparse–dense model pairs at the end of the training process. This is useful in practice, where compressed variants may be desirable for deployment in resource-constrained settings without re-doing the entire training flow, and also provides us with insights into the accuracy gap between dense and compressed models. The code is available at: https://github.com/IST-DASLab/ACDC.","lang":"eng"}],"ec_funded":1,"month":"12","publication_identifier":{"issn":["1049-5258"],"isbn":["9781713845393"]},"oa":1,"status":"public"},{"date_updated":"2022-06-27T07:05:12Z","abstract":[{"lang":"eng","text":"Efficiently approximating local curvature information of the loss function is a key tool for optimization and compression of deep neural networks. Yet, most existing methods to approximate second-order information have high computational\r\nor storage costs, which limits their practicality. In this work, we investigate matrix-free, linear-time approaches for estimating Inverse-Hessian Vector Products (IHVPs) for the case when the Hessian can be approximated as a sum of rank-one matrices, as in the classic approximation of the Hessian by the empirical Fisher matrix. We propose two new algorithms: the first is tailored towards network compression and can compute the IHVP for dimension d, if the Hessian is given as a sum of m rank-one matrices, using O(dm2) precomputation, O(dm) cost for computing the IHVP, and query cost O(m) for any single element of the inverse Hessian. The second algorithm targets an optimization setting, where we wish to compute the product between the inverse Hessian, estimated over a sliding window of optimization steps, and a given gradient direction, as required for preconditioned SGD. We give an algorithm with cost O(dm + m2) for computing the IHVP and O(dm + m3) for adding or removing any gradient from the sliding window. These\r\ntwo algorithms yield state-of-the-art results for network pruning and optimization with lower computational overhead relative to existing second-order methods. Implementations are available at [9] and [17]."}],"arxiv":1,"year":"2021","_id":"11463","status":"public","publication_identifier":{"issn":["1049-5258"],"isbn":["9781713845393"]},"oa":1,"month":"12","ec_funded":1,"publication_status":"published","conference":{"end_date":"2021-12-14","location":"Virtual, Online","start_date":"2021-12-06","name":"NeurIPS: Neural Information Processing Systems"},"oa_version":"Published Version","date_published":"2021-12-06T00:00:00Z","scopus_import":"1","main_file_link":[{"open_access":"1","url":"https://proceedings.neurips.cc/paper/2021/file/7cfd5df443b4eb0d69886a583b33de4c-Paper.pdf"}],"citation":{"ieee":"E. Frantar, E. Kurtic, and D.-A. Alistarh, “M-FAC: Efficient matrix-free approximations of second-order information,” in <i>35th Conference on Neural Information Processing Systems</i>, Virtual, Online, 2021, vol. 34, pp. 14873–14886.","ama":"Frantar E, Kurtic E, Alistarh D-A. M-FAC: Efficient matrix-free approximations of second-order information. In: <i>35th Conference on Neural Information Processing Systems</i>. Vol 34. Curran Associates; 2021:14873-14886.","short":"E. Frantar, E. Kurtic, D.-A. Alistarh, in:, 35th Conference on Neural Information Processing Systems, Curran Associates, 2021, pp. 14873–14886.","mla":"Frantar, Elias, et al. “M-FAC: Efficient Matrix-Free Approximations of Second-Order Information.” <i>35th Conference on Neural Information Processing Systems</i>, vol. 34, Curran Associates, 2021, pp. 14873–86.","apa":"Frantar, E., Kurtic, E., &#38; Alistarh, D.-A. (2021). M-FAC: Efficient matrix-free approximations of second-order information. In <i>35th Conference on Neural Information Processing Systems</i> (Vol. 34, pp. 14873–14886). Virtual, Online: Curran Associates.","ista":"Frantar E, Kurtic E, Alistarh D-A. 2021. M-FAC: Efficient matrix-free approximations of second-order information. 35th Conference on Neural Information Processing Systems. NeurIPS: Neural Information Processing Systems vol. 34, 14873–14886.","chicago":"Frantar, Elias, Eldar Kurtic, and Dan-Adrian Alistarh. “M-FAC: Efficient Matrix-Free Approximations of Second-Order Information.” In <i>35th Conference on Neural Information Processing Systems</i>, 34:14873–86. Curran Associates, 2021."},"intvolume":"        34","acknowledgement":"We gratefully acknowledge funding the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No 805223 ScaleML), as well as computational support from Amazon Web Services (AWS) EC2.","day":"06","project":[{"_id":"268A44D6-B435-11E9-9278-68D0E5697425","grant_number":"805223","name":"Elastic Coordination for Scalable Machine Learning","call_identifier":"H2020"}],"author":[{"first_name":"Elias","id":"09a8f98d-ec99-11ea-ae11-c063a7b7fe5f","last_name":"Frantar","full_name":"Frantar, Elias"},{"last_name":"Kurtic","id":"47beb3a5-07b5-11eb-9b87-b108ec578218","first_name":"Eldar","full_name":"Kurtic, Eldar"},{"last_name":"Alistarh","id":"4A899BFC-F248-11E8-B48F-1D18A9856A87","orcid":"0000-0003-3650-940X","first_name":"Dan-Adrian","full_name":"Alistarh, Dan-Adrian"}],"publisher":"Curran Associates","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","title":"M-FAC: Efficient matrix-free approximations of second-order information","date_created":"2022-06-26T22:01:35Z","page":"14873-14886","publication":"35th Conference on Neural Information Processing Systems","type":"conference","language":[{"iso":"eng"}],"department":[{"_id":"DaAl"}],"article_processing_charge":"No","external_id":{"arxiv":["2010.08222"]},"quality_controlled":"1","volume":34},{"_id":"11464","year":"2021","date_updated":"2022-06-27T06:54:31Z","abstract":[{"lang":"eng","text":"We consider a standard distributed optimisation setting where N machines, each holding a d-dimensional function\r\nfi, aim to jointly minimise the sum of the functions ∑Ni=1fi(x). This problem arises naturally in large-scale distributed optimisation, where a standard solution is to apply variants of (stochastic) gradient descent. We focus on the communication complexity of this problem: our main result provides the first fully unconditional bounds on total number of bits which need to be sent and received by the N machines to solve this problem under point-to-point communication, within a given error-tolerance. Specifically, we show that Ω(Ndlogd/Nε) total bits need to be communicated between the machines to find an additive ϵ-approximation to the minimum of ∑Ni=1fi(x). The result holds for both deterministic and randomised algorithms, and, importantly, requires no assumptions on the algorithm structure. The lower bound is tight under certain restrictions on parameter values, and is matched within constant factors for quadratic objectives by a new variant of quantised gradient descent, which we describe and analyse. Our results bring over tools from communication complexity to distributed optimisation, which has potential for further applications."}],"arxiv":1,"ec_funded":1,"month":"12","publication_identifier":{"isbn":["9781713845393"],"issn":["1049-5258"]},"oa":1,"status":"public","date_published":"2021-12-06T00:00:00Z","oa_version":"Published Version","publication_status":"published","conference":{"location":"Virtual, Online","end_date":"2021-12-14","name":"NeurIPS: Neural Information Processing Systems","start_date":"2021-12-06"},"citation":{"chicago":"Alistarh, Dan-Adrian, and Janne Korhonen. “Towards Tight Communication Lower Bounds for Distributed Optimisation.” In <i>35th Conference on Neural Information Processing Systems</i>, 34:7254–66. Curran Associates, 2021.","apa":"Alistarh, D.-A., &#38; Korhonen, J. (2021). Towards tight communication lower bounds for distributed optimisation. In <i>35th Conference on Neural Information Processing Systems</i> (Vol. 34, pp. 7254–7266). Virtual, Online: Curran Associates.","mla":"Alistarh, Dan-Adrian, and Janne Korhonen. “Towards Tight Communication Lower Bounds for Distributed Optimisation.” <i>35th Conference on Neural Information Processing Systems</i>, vol. 34, Curran Associates, 2021, pp. 7254–66.","ista":"Alistarh D-A, Korhonen J. 2021. Towards tight communication lower bounds for distributed optimisation. 35th Conference on Neural Information Processing Systems. NeurIPS: Neural Information Processing Systems vol. 34, 7254–7266.","ama":"Alistarh D-A, Korhonen J. Towards tight communication lower bounds for distributed optimisation. In: <i>35th Conference on Neural Information Processing Systems</i>. Vol 34. Curran Associates; 2021:7254-7266.","ieee":"D.-A. Alistarh and J. Korhonen, “Towards tight communication lower bounds for distributed optimisation,” in <i>35th Conference on Neural Information Processing Systems</i>, Virtual, Online, 2021, vol. 34, pp. 7254–7266.","short":"D.-A. Alistarh, J. Korhonen, in:, 35th Conference on Neural Information Processing Systems, Curran Associates, 2021, pp. 7254–7266."},"intvolume":"        34","scopus_import":"1","main_file_link":[{"open_access":"1","url":"https://proceedings.neurips.cc/paper/2021/file/3b92d18aa7a6176dd37d372bc2f1eb71-Paper.pdf"}],"project":[{"grant_number":"805223","_id":"268A44D6-B435-11E9-9278-68D0E5697425","name":"Elastic Coordination for Scalable Machine Learning","call_identifier":"H2020"}],"author":[{"full_name":"Alistarh, Dan-Adrian","last_name":"Alistarh","id":"4A899BFC-F248-11E8-B48F-1D18A9856A87","orcid":"0000-0003-3650-940X","first_name":"Dan-Adrian"},{"full_name":"Korhonen, Janne","id":"C5402D42-15BC-11E9-A202-CA2BE6697425","last_name":"Korhonen","first_name":"Janne"}],"day":"06","acknowledgement":"We thank the NeurIPS reviewers for insightful comments that helped us improve the positioning of our results, as well as for pointing out the subsampling approach for complementing the randomised lower bound. We also thank Foivos Alimisis and Peter Davies for useful discussions. This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No 805223 ScaleML).","title":"Towards tight communication lower bounds for distributed optimisation","publisher":"Curran Associates","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"department":[{"_id":"DaAl"}],"type":"conference","date_created":"2022-06-26T22:01:35Z","page":"7254-7266","publication":"35th Conference on Neural Information Processing Systems","external_id":{"arxiv":["2010.08222"]},"quality_controlled":"1","volume":34,"article_processing_charge":"No"},{"arxiv":1,"abstract":[{"text":"Rest-frame ultraviolet (UV) emission lines probe electron densities, gas-phase abundances, metallicities, and ionization parameters of the emitting star-forming galaxies and their environments. The strongest main UV emission line, Lyα, has been instrumental in advancing the general knowledge of galaxy formation in the early universe. However, observing Lyα emission becomes increasingly challenging at z ≳ 6 when the neutral hydrogen fraction of the circumgalactic and intergalactic media increases. Secondary weaker UV emission lines provide important alternative methods for studying galaxy properties at high redshift. We present a large sample of rest-frame UV emission line sources at intermediate redshift for calibrating and exploring the connection between secondary UV lines and the emitting galaxies’ physical properties and their Lyα emission. The sample of 2052 emission line sources with 1.5 < z < 6.4 was collected from integral field data from the MUSE-Wide and MUSE-Deep surveys taken as part of Guaranteed Time Observations. The objects were selected through untargeted source detection (i.e., no preselection of sources as in dedicated spectroscopic campaigns) in the three-dimensional MUSE data cubes. We searched optimally extracted one-dimensional spectra of the full sample for UV emission features via emission line template matching, resulting in a sample of more than 100 rest-frame UV emission line detections. We show that the detection efficiency of (non-Lyα) UV emission lines increases with survey depth, and that the emission line strength of He IIλ1640 Å, [O III] λ1661 + O III] λ1666, and [Si III] λ1883 + Si III] λ1892 correlate with the strength of [C III] λ1907 + C III] λ1909. The rest-frame equivalent width (EW0) of [C III] λ1907 + C III] λ1909 is found to be roughly 0.22 ± 0.18 of EW0(Lyα). We measured the velocity offsets of resonant emission lines with respect to systemic tracers. For C IVλ1548 + C IVλ1551 we find that ΔvC IV ≲ 250 km s−1, whereas ΔvLyα falls in the range of 250−500 km s−1 which is in agreement with previous results from the literature. The electron density ne measured from [Si III] λ1883 + Si III] λ1892 and [C III] λ1907 + C III] λ1909 line flux ratios is generally < 105 cm−3 and the gas-phase abundance is below solar at 12 + log10(O/H)≈8. Lastly, we used “PhotoIonization Model Probability Density Functions” to infer physical parameters of the full sample and individual systems based on photoionization model parameter grids and observational constraints from our UV emission line searches. This reveals that the UV line emitters generally have ionization parameter log10(U) ≈ −2.5 and metal mass fractions that scatter around Z ≈ 10−2, that is Z ≈ 0.66 Z⊙. Value-added catalogs of the full sample of MUSE objects studied in this work and a collection of UV line emitters from the literature are provided with this paper.","lang":"eng"}],"date_updated":"2022-07-19T09:34:36Z","year":"2021","article_number":"A80","_id":"11498","status":"public","oa":1,"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"month":"10","doi":"10.1051/0004-6361/202140876","publication_status":"published","oa_version":"Published Version","date_published":"2021-10-15T00:00:00Z","scopus_import":"1","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2108.01713"}],"citation":{"ama":"Schmidt KB, Kerutt J, Wisotzki L, et al. Recovery and analysis of rest-frame UV emission lines in 2052 galaxies observed with MUSE at 1.5 &#60; z &#60; 6.4. <i>Astronomy &#38; Astrophysics</i>. 2021;654. doi:<a href=\"https://doi.org/10.1051/0004-6361/202140876\">10.1051/0004-6361/202140876</a>","ieee":"K. B. Schmidt <i>et al.</i>, “Recovery and analysis of rest-frame UV emission lines in 2052 galaxies observed with MUSE at 1.5 &#60; z &#60; 6.4,” <i>Astronomy &#38; Astrophysics</i>, vol. 654. EDP Sciences, 2021.","short":"K.B. Schmidt, J. Kerutt, L. Wisotzki, T. Urrutia, A. Feltre, M.V. Maseda, T. Nanayakkara, R. Bacon, L.A. Boogaard, S. Conseil, T. Contini, E.C. Herenz, W. Kollatschny, M. Krumpe, F. Leclercq, G. Mahler, J.J. Matthee, V. Mauerhofer, J. Richard, J. Schaye, Astronomy &#38; Astrophysics 654 (2021).","ista":"Schmidt KB, Kerutt J, Wisotzki L, Urrutia T, Feltre A, Maseda MV, Nanayakkara T, Bacon R, Boogaard LA, Conseil S, Contini T, Herenz EC, Kollatschny W, Krumpe M, Leclercq F, Mahler G, Matthee JJ, Mauerhofer V, Richard J, Schaye J. 2021. Recovery and analysis of rest-frame UV emission lines in 2052 galaxies observed with MUSE at 1.5 &#60; z &#60; 6.4. Astronomy &#38; Astrophysics. 654, A80.","mla":"Schmidt, K. B., et al. “Recovery and Analysis of Rest-Frame UV Emission Lines in 2052 Galaxies Observed with MUSE at 1.5 &#60; z &#60; 6.4.” <i>Astronomy &#38; Astrophysics</i>, vol. 654, A80, EDP Sciences, 2021, doi:<a href=\"https://doi.org/10.1051/0004-6361/202140876\">10.1051/0004-6361/202140876</a>.","apa":"Schmidt, K. B., Kerutt, J., Wisotzki, L., Urrutia, T., Feltre, A., Maseda, M. V., … Schaye, J. (2021). Recovery and analysis of rest-frame UV emission lines in 2052 galaxies observed with MUSE at 1.5 &#60; z &#60; 6.4. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202140876\">https://doi.org/10.1051/0004-6361/202140876</a>","chicago":"Schmidt, K. B., J. Kerutt, L. Wisotzki, T. Urrutia, A. Feltre, M. V. Maseda, T. Nanayakkara, et al. “Recovery and Analysis of Rest-Frame UV Emission Lines in 2052 Galaxies Observed with MUSE at 1.5 &#60; z &#60; 6.4.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2021. <a href=\"https://doi.org/10.1051/0004-6361/202140876\">https://doi.org/10.1051/0004-6361/202140876</a>."},"intvolume":"       654","acknowledgement":"We would like to thank Charlotte Mason for useful discussions and for providing the data for the curves shown in Fig. 13 and Dawn Erb for providing the observational data for the comparison sample studied by Steidel et al. (2014), also shown in Fig. 13. This work has been supported by the BMBF grant 05A14BAC and we acknowledge support by the Competitive Fund of the Leibniz Association through grant SAW-2015-AIP-2. AF acknowledges the support from grant PRIN MIUR2017-20173ML3WW_001. JS acknowledges the support from Vici grant 639.043.409 from the Dutch Research Council (NWO). GM received funding from the European Union’s Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant agreement No MARACAS – DLV-896778. This paper is based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programmes 094.A-0289(B), 095.A-0010(A), 096.A-0045(A), 096.A-0045(B), 094.A-0205, 095.A-0240, 096.A-0090, 097.A-0160, and 098.A-0017. This paper also makes use of observations made with the NASA/ESA Hubble Space Telescope obtained at STScI. This research made use of the following programs and open-source packages for Python and we are thankful to their developers: DS9 (Joye & Mandel 2003), Astropy (Astropy Collaboration 2013, 2018), APLpy (Robitaille & Bressert 2012), iPython (Pérez & Granger 2007), numpy (van der Walt et al. 2011), matplotlib (Hunter 2007), and SciPy (Jones et al. 2001).","extern":"1","day":"15","author":[{"first_name":"K. B.","last_name":"Schmidt","full_name":"Schmidt, K. B."},{"full_name":"Kerutt, J.","last_name":"Kerutt","first_name":"J."},{"full_name":"Wisotzki, L.","last_name":"Wisotzki","first_name":"L."},{"full_name":"Urrutia, T.","last_name":"Urrutia","first_name":"T."},{"full_name":"Feltre, A.","last_name":"Feltre","first_name":"A."},{"full_name":"Maseda, M. V.","first_name":"M. V.","last_name":"Maseda"},{"first_name":"T.","last_name":"Nanayakkara","full_name":"Nanayakkara, T."},{"first_name":"R.","last_name":"Bacon","full_name":"Bacon, R."},{"first_name":"L. A.","last_name":"Boogaard","full_name":"Boogaard, L. A."},{"full_name":"Conseil, S.","first_name":"S.","last_name":"Conseil"},{"full_name":"Contini, T.","first_name":"T.","last_name":"Contini"},{"full_name":"Herenz, E. C.","first_name":"E. C.","last_name":"Herenz"},{"full_name":"Kollatschny, W.","first_name":"W.","last_name":"Kollatschny"},{"last_name":"Krumpe","first_name":"M.","full_name":"Krumpe, M."},{"full_name":"Leclercq, F.","first_name":"F.","last_name":"Leclercq"},{"full_name":"Mahler, G.","last_name":"Mahler","first_name":"G."},{"full_name":"Matthee, Jorryt J","first_name":"Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee"},{"first_name":"V.","last_name":"Mauerhofer","full_name":"Mauerhofer, V."},{"first_name":"J.","last_name":"Richard","full_name":"Richard, J."},{"first_name":"J.","last_name":"Schaye","full_name":"Schaye, J."}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publisher":"EDP Sciences","title":"Recovery and analysis of rest-frame UV emission lines in 2052 galaxies observed with MUSE at 1.5 < z < 6.4","publication":"Astronomy & Astrophysics","date_created":"2022-07-06T08:49:03Z","type":"journal_article","language":[{"iso":"eng"}],"article_type":"original","article_processing_charge":"No","volume":654,"keyword":["Space and Planetary Science","Astronomy and Astrophysics","ultraviolet: galaxies / galaxies: high-redshift / galaxies: ISM / ISM: lines and bands / methods: observational / techniques: imaging spectroscopy"],"quality_controlled":"1","external_id":{"arxiv":["2108.01713"]}},{"type":"journal_article","language":[{"iso":"eng"}],"date_created":"2022-07-06T09:31:50Z","publication":"Astronomy & Astrophysics","external_id":{"arxiv":["2102.05516"]},"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift / galaxies: groups: general / cosmology: observations"],"volume":647,"quality_controlled":"1","article_type":"original","article_processing_charge":"No","author":[{"last_name":"Bacon","first_name":"R.","full_name":"Bacon, R."},{"last_name":"Mary","first_name":"D.","full_name":"Mary, D."},{"last_name":"Garel","first_name":"T.","full_name":"Garel, T."},{"last_name":"Blaizot","first_name":"J.","full_name":"Blaizot, J."},{"full_name":"Maseda, M.","last_name":"Maseda","first_name":"M."},{"first_name":"J.","last_name":"Schaye","full_name":"Schaye, J."},{"first_name":"L.","last_name":"Wisotzki","full_name":"Wisotzki, L."},{"last_name":"Conseil","first_name":"S.","full_name":"Conseil, S."},{"last_name":"Brinchmann","first_name":"J.","full_name":"Brinchmann, J."},{"full_name":"Leclercq, F.","first_name":"F.","last_name":"Leclercq"},{"last_name":"Abril-Melgarejo","first_name":"V.","full_name":"Abril-Melgarejo, V."},{"full_name":"Boogaard, L.","last_name":"Boogaard","first_name":"L."},{"full_name":"Bouché, N. F.","first_name":"N. F.","last_name":"Bouché"},{"full_name":"Contini, T.","last_name":"Contini","first_name":"T."},{"last_name":"Feltre","first_name":"A.","full_name":"Feltre, A."},{"last_name":"Guiderdoni","first_name":"B.","full_name":"Guiderdoni, B."},{"full_name":"Herenz, C.","first_name":"C.","last_name":"Herenz"},{"full_name":"Kollatschny, W.","last_name":"Kollatschny","first_name":"W."},{"full_name":"Kusakabe, H.","last_name":"Kusakabe","first_name":"H."},{"full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X","first_name":"Jorryt J"},{"last_name":"Michel-Dansac","first_name":"L.","full_name":"Michel-Dansac, L."},{"full_name":"Nanayakkara, T.","first_name":"T.","last_name":"Nanayakkara"},{"last_name":"Richard","first_name":"J.","full_name":"Richard, J."},{"full_name":"Roth, M.","last_name":"Roth","first_name":"M."},{"full_name":"Schmidt, K. B.","last_name":"Schmidt","first_name":"K. B."},{"first_name":"M.","last_name":"Steinmetz","full_name":"Steinmetz, M."},{"full_name":"Tresse, L.","last_name":"Tresse","first_name":"L."},{"last_name":"Urrutia","first_name":"T.","full_name":"Urrutia, T."},{"full_name":"Verhamme, A.","last_name":"Verhamme","first_name":"A."},{"first_name":"P. M.","last_name":"Weilbacher","full_name":"Weilbacher, P. M."},{"first_name":"J.","last_name":"Zabl","full_name":"Zabl, J."},{"full_name":"Zoutendijk, S. L.","first_name":"S. L.","last_name":"Zoutendijk"}],"acknowledgement":"We warmly thank ESO Paranal staff for their great professional support during all MXDF GTO observing runs. We thank the anonymous referee for a careful reading of the manuscript and helpful comments. We also thank Matthew Lehnert for fruitful discussions. RB, AF, SC acknowledge support from the ERC advanced grant 339659-MUSICOS. JB acknowledges support by Fundação para a Ciência e a Tecnologia (FCT) through the research grants UID/FIS/04434/2019, UIDB/04434/2020, UIDP/04434/2020 and through the Investigador FCT Contract No. IF/01654/2014/CP1215/CT0003. TG, AV acknowledges support from the European Research Council under grant agreement ERC-stg-757258 (TRIPLE). DM acknowledges A. Dabbech for useful interactions about IUWT and support from the GDR ISIS through the Projets exploratoires program (project TASTY). AF acknowledges the support from grant PRIN MIUR2017-20173ML3WW_001. SLZ acknowledges support by The Netherlands Organisation for Scientific Research (NWO) through a TOP Grant Module 1 under project number 614.001.652. This research made use of the following open-source software and we are thankful to the developers of these: GNU Octave (Eaton et al. 2018) and its statistics, signal and image packages, the Python packages Matplotlib (Hunter 2007), Numpy (van der Walt et al. 2010), MPDAF (Piqueras et al. 2017), Astropy (Astropy Collaboration 2018), PyWavelets (Lee et al. 2019).","day":"18","extern":"1","publisher":"EDP Sciences","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","title":"The MUSE Extremely Deep Field: The cosmic web in emission at high redshift","oa_version":"Published Version","date_published":"2021-03-18T00:00:00Z","publication_status":"published","doi":"10.1051/0004-6361/202039887","citation":{"ama":"Bacon R, Mary D, Garel T, et al. The MUSE Extremely Deep Field: The cosmic web in emission at high redshift. <i>Astronomy &#38; Astrophysics</i>. 2021;647. doi:<a href=\"https://doi.org/10.1051/0004-6361/202039887\">10.1051/0004-6361/202039887</a>","ieee":"R. Bacon <i>et al.</i>, “The MUSE Extremely Deep Field: The cosmic web in emission at high redshift,” <i>Astronomy &#38; Astrophysics</i>, vol. 647. EDP Sciences, 2021.","short":"R. Bacon, D. Mary, T. Garel, J. Blaizot, M. Maseda, J. Schaye, L. Wisotzki, S. Conseil, J. Brinchmann, F. Leclercq, V. Abril-Melgarejo, L. Boogaard, N.F. Bouché, T. Contini, A. Feltre, B. Guiderdoni, C. Herenz, W. Kollatschny, H. Kusakabe, J.J. Matthee, L. Michel-Dansac, T. Nanayakkara, J. Richard, M. Roth, K.B. Schmidt, M. Steinmetz, L. Tresse, T. Urrutia, A. Verhamme, P.M. Weilbacher, J. Zabl, S.L. Zoutendijk, Astronomy &#38; Astrophysics 647 (2021).","apa":"Bacon, R., Mary, D., Garel, T., Blaizot, J., Maseda, M., Schaye, J., … Zoutendijk, S. L. (2021). The MUSE Extremely Deep Field: The cosmic web in emission at high redshift. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202039887\">https://doi.org/10.1051/0004-6361/202039887</a>","mla":"Bacon, R., et al. “The MUSE Extremely Deep Field: The Cosmic Web in Emission at High Redshift.” <i>Astronomy &#38; Astrophysics</i>, vol. 647, A107, EDP Sciences, 2021, doi:<a href=\"https://doi.org/10.1051/0004-6361/202039887\">10.1051/0004-6361/202039887</a>.","ista":"Bacon R, Mary D, Garel T, Blaizot J, Maseda M, Schaye J, Wisotzki L, Conseil S, Brinchmann J, Leclercq F, Abril-Melgarejo V, Boogaard L, Bouché NF, Contini T, Feltre A, Guiderdoni B, Herenz C, Kollatschny W, Kusakabe H, Matthee JJ, Michel-Dansac L, Nanayakkara T, Richard J, Roth M, Schmidt KB, Steinmetz M, Tresse L, Urrutia T, Verhamme A, Weilbacher PM, Zabl J, Zoutendijk SL. 2021. The MUSE Extremely Deep Field: The cosmic web in emission at high redshift. Astronomy &#38; Astrophysics. 647, A107.","chicago":"Bacon, R., D. Mary, T. Garel, J. Blaizot, M. Maseda, J. Schaye, L. Wisotzki, et al. “The MUSE Extremely Deep Field: The Cosmic Web in Emission at High Redshift.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2021. <a href=\"https://doi.org/10.1051/0004-6361/202039887\">https://doi.org/10.1051/0004-6361/202039887</a>."},"intvolume":"       647","scopus_import":"1","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2102.05516"}],"article_number":"A107","_id":"11500","date_updated":"2022-07-19T09:34:57Z","abstract":[{"text":"We report the discovery of diffuse extended Lyα emission from redshift 3.1 to 4.5, tracing cosmic web filaments on scales of 2.5−4 cMpc. These structures have been observed in overdensities of Lyα emitters in the MUSE Extremely Deep Field, a 140 h deep MUSE observation located in the Hubble Ultra-Deep Field. Among the 22 overdense regions identified, five are likely to harbor very extended Lyα emission at high significance with an average surface brightness of 5 × 10−20 erg s−1 cm−2 arcsec−2. Remarkably, 70% of the total Lyα luminosity from these filaments comes from beyond the circumgalactic medium of any identified Lyα emitter. Fluorescent Lyα emission powered by the cosmic UV background can only account for less than 34% of this emission at z ≈ 3 and for not more than 10% at higher redshift. We find that the bulk of this diffuse emission can be reproduced by the unresolved Lyα emission of a large population of ultra low-luminosity Lyα emitters (< 1040 erg s−1), provided that the faint end of the Lyα luminosity function is steep (α ⪅ −1.8), it extends down to luminosities lower than 1038 − 1037 erg s−1, and the clustering of these Lyα emitters is significant (filling factor < 1/6). If these Lyα emitters are powered by star formation, then this implies their luminosity function needs to extend down to star formation rates < 10−4 M⊙ yr−1. These observations provide the first detection of the cosmic web in Lyα emission in typical filamentary environments and the first observational clue indicating the existence of a large population of ultra low-luminosity Lyα emitters at high redshift.","lang":"eng"}],"arxiv":1,"year":"2021","month":"03","status":"public","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"oa":1},{"publication_status":"published","doi":"10.3847/1538-4357/ac01d7","oa_version":"Preprint","date_published":"2021-07-20T00:00:00Z","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2105.12489"}],"scopus_import":"1","citation":{"chicago":"Boogaard, Leindert A., Rychard J. Bouwens, Dominik Riechers, Paul van der Werf, Roland Bacon, Jorryt J Matthee, Mauro Stefanon, et al. “Measuring the Average Molecular Gas Content of Star-Forming Galaxies at z = 3–4.” <i>The Astrophysical Journal</i>. IOP Publishing, 2021. <a href=\"https://doi.org/10.3847/1538-4357/ac01d7\">https://doi.org/10.3847/1538-4357/ac01d7</a>.","mla":"Boogaard, Leindert A., et al. “Measuring the Average Molecular Gas Content of Star-Forming Galaxies at z = 3–4.” <i>The Astrophysical Journal</i>, vol. 916, no. 1, 12, IOP Publishing, 2021, doi:<a href=\"https://doi.org/10.3847/1538-4357/ac01d7\">10.3847/1538-4357/ac01d7</a>.","ista":"Boogaard LA, Bouwens RJ, Riechers D, van der Werf P, Bacon R, Matthee JJ, Stefanon M, Feltre A, Maseda M, Inami H, Aravena M, Brinchmann J, Carilli C, Contini T, Decarli R, González-López J, Nanayakkara T, Walter F. 2021. Measuring the average molecular gas content of star-forming galaxies at z = 3–4. The Astrophysical Journal. 916(1), 12.","apa":"Boogaard, L. A., Bouwens, R. J., Riechers, D., van der Werf, P., Bacon, R., Matthee, J. J., … Walter, F. (2021). Measuring the average molecular gas content of star-forming galaxies at z = 3–4. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/ac01d7\">https://doi.org/10.3847/1538-4357/ac01d7</a>","short":"L.A. Boogaard, R.J. Bouwens, D. Riechers, P. van der Werf, R. Bacon, J.J. Matthee, M. Stefanon, A. Feltre, M. Maseda, H. Inami, M. Aravena, J. Brinchmann, C. Carilli, T. Contini, R. Decarli, J. González-López, T. Nanayakkara, F. Walter, The Astrophysical Journal 916 (2021).","ieee":"L. A. Boogaard <i>et al.</i>, “Measuring the average molecular gas content of star-forming galaxies at z = 3–4,” <i>The Astrophysical Journal</i>, vol. 916, no. 1. IOP Publishing, 2021.","ama":"Boogaard LA, Bouwens RJ, Riechers D, et al. Measuring the average molecular gas content of star-forming galaxies at z = 3–4. <i>The Astrophysical Journal</i>. 2021;916(1). doi:<a href=\"https://doi.org/10.3847/1538-4357/ac01d7\">10.3847/1538-4357/ac01d7</a>"},"intvolume":"       916","date_updated":"2022-07-19T09:32:48Z","abstract":[{"lang":"eng","text":"We study the molecular gas content of 24 star-forming galaxies at z = 3–4, with a median stellar mass of 109.1 M⊙, from the MUSE Hubble Ultra Deep Field (HUDF) Survey. Selected by their Lyα λ1216 emission and HF160W-band magnitude, the galaxies show an average $\\langle {\\mathrm{EW}}_{\\mathrm{Ly}\\alpha }^{0}\\rangle \\approx 20$ Å, below the typical selection threshold for Lyα emitters (${\\mathrm{EW}}_{\\mathrm{Ly}\\alpha }^{0}\\gt 25$ Å), and a rest-frame UV spectrum similar to Lyman-break galaxies. We use rest-frame optical spectroscopy from KMOS and MOSFIRE, and the UV features observed with MUSE, to determine the systemic redshifts, which are offset from Lyα by 〈Δv(Lyα)〉 = 346 km s−1, with a 100 to 600 km s−1 range. Stacking 12CO J = 4 → 3 and [C i]3P1 → 3P0 (and higher-J CO lines) from the ALMA Spectroscopic Survey of the HUDF, we determine 3σ upper limits on the line luminosities of 4.0 × 108 K km s−1pc2 and 5.6 × 108 K km s−1pc2, respectively (for a 300 km s−1 line width). Stacking the 1.2 mm and 3 mm dust-continuum flux densities, we find a 3σ upper limits of 9 μJy and 1.2 μJy, respectively. The inferred gas fractions, under the assumption of a \"Galactic\" CO-to-H2 conversion factor and gas-to-dust ratio, are in tension with previously determined scaling relations. This implies a substantially higher αCO ≥ 10 and δGDR ≥ 1200, consistent with the subsolar metallicity estimated for these galaxies ($12+\\mathrm{log}({\\rm{O}}/{\\rm{H}})\\approx 7.8\\pm 0.2$). The low metallicity of z ≥ 3 star-forming galaxies may thus make it very challenging to unveil their cold gas through CO or dust emission, warranting further exploration of alternative tracers, such as [C ii]."}],"issue":"1","arxiv":1,"year":"2021","article_number":"12","_id":"11512","status":"public","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"oa":1,"month":"07","date_created":"2022-07-06T13:05:50Z","publication":"The Astrophysical Journal","type":"journal_article","language":[{"iso":"eng"}],"article_type":"original","article_processing_charge":"No","external_id":{"arxiv":["2105.12489"]},"volume":916,"quality_controlled":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"acknowledgement":"We would like to thank the referee for a constructive and helpful report. L.A.B. is grateful to Corentin Schreiber for assisting with the near-infrared spectroscopy during the early stages of this work. L.A.B. acknowledges support from the Leids Kerkhoven-Bosscha Fonds under subsidy numbers 18.2.074 and 19.1.147. D.R. acknowledges support from the National Science Foundation under grant numbers AST-1614213 and AST-1910107. D.R. also acknowledges support from the Alexander von Humboldt Foundation through a Humboldt Research Fellowship for Experienced Researchers. A.F. acknowledges the support from grant PRIN MIUR 201720173ML3WW_001. J.B. acknowledges support by Fundação para a Ciência e a Tecnologia (FCT) through the research grants UID/FIS/04434/2019, UIDB/04434/2020, UIDP/04434/2020. H.I. acknowledges support from JSPS KAKENHI grant No. JP19K23462. This work is based on observations collected at the European Southern Observatory under ESO programs 094.A-2089(B), 095.A-0010(A), 096.A-0045(A), 096.A-0045(B), 099.A-0858(A), and 0101.A-0725(A). This paper makes use of the following ALMA data: ADS/JAO.ALMA#2016.1.00324.L. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This work was supported by a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. Data presented herein were obtained at the W. M. Keck Observatory from telescope time allocated to the National Aeronautics and Space Administration through the agency's scientific partnership with the California Institute of Technology and the University of California. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. 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 Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.","day":"20","extern":"1","author":[{"first_name":"Leindert A.","last_name":"Boogaard","full_name":"Boogaard, Leindert A."},{"last_name":"Bouwens","first_name":"Rychard J.","full_name":"Bouwens, Rychard J."},{"first_name":"Dominik","last_name":"Riechers","full_name":"Riechers, Dominik"},{"full_name":"van der Werf, Paul","last_name":"van der Werf","first_name":"Paul"},{"full_name":"Bacon, Roland","first_name":"Roland","last_name":"Bacon"},{"full_name":"Matthee, Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"},{"full_name":"Stefanon, Mauro","first_name":"Mauro","last_name":"Stefanon"},{"full_name":"Feltre, Anna","first_name":"Anna","last_name":"Feltre"},{"last_name":"Maseda","first_name":"Michael","full_name":"Maseda, Michael"},{"last_name":"Inami","first_name":"Hanae","full_name":"Inami, Hanae"},{"first_name":"Manuel","last_name":"Aravena","full_name":"Aravena, Manuel"},{"full_name":"Brinchmann, Jarle","first_name":"Jarle","last_name":"Brinchmann"},{"last_name":"Carilli","first_name":"Chris","full_name":"Carilli, Chris"},{"last_name":"Contini","first_name":"Thierry","full_name":"Contini, Thierry"},{"last_name":"Decarli","first_name":"Roberto","full_name":"Decarli, Roberto"},{"last_name":"González-López","first_name":"Jorge","full_name":"González-López, Jorge"},{"full_name":"Nanayakkara, Themiya","last_name":"Nanayakkara","first_name":"Themiya"},{"full_name":"Walter, Fabian","first_name":"Fabian","last_name":"Walter"}],"publisher":"IOP Publishing","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","title":"Measuring the average molecular gas content of star-forming galaxies at z = 3–4"},{"citation":{"short":"M. Gronke, P. Ocvirk, C. Mason, J.J. Matthee, S.E.I. Bosman, J.G. Sorce, J. Lewis, K. Ahn, D. Aubert, T. Dawoodbhoy, I.T. Iliev, P.R. Shapiro, G. Yepes, Monthly Notices of the Royal Astronomical Society 508 (2021) 3697–3709.","ieee":"M. Gronke <i>et al.</i>, “Lyman-α transmission properties of the intergalactic medium in the CoDaII simulation,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 508, no. 3. Oxford University Press, pp. 3697–3709, 2021.","ama":"Gronke M, Ocvirk P, Mason C, et al. Lyman-α transmission properties of the intergalactic medium in the CoDaII simulation. <i>Monthly Notices of the Royal Astronomical Society</i>. 2021;508(3):3697-3709. doi:<a href=\"https://doi.org/10.1093/mnras/stab2762\">10.1093/mnras/stab2762</a>","ista":"Gronke M, Ocvirk P, Mason C, Matthee JJ, Bosman SEI, Sorce JG, Lewis J, Ahn K, Aubert D, Dawoodbhoy T, Iliev IT, Shapiro PR, Yepes G. 2021. Lyman-α transmission properties of the intergalactic medium in the CoDaII simulation. Monthly Notices of the Royal Astronomical Society. 508(3), 3697–3709.","apa":"Gronke, M., Ocvirk, P., Mason, C., Matthee, J. J., Bosman, S. E. I., Sorce, J. G., … Yepes, G. (2021). Lyman-α transmission properties of the intergalactic medium in the CoDaII simulation. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stab2762\">https://doi.org/10.1093/mnras/stab2762</a>","mla":"Gronke, Max, et al. “Lyman-α Transmission Properties of the Intergalactic Medium in the CoDaII Simulation.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 508, no. 3, Oxford University Press, 2021, pp. 3697–709, doi:<a href=\"https://doi.org/10.1093/mnras/stab2762\">10.1093/mnras/stab2762</a>.","chicago":"Gronke, Max, Pierre Ocvirk, Charlotte Mason, Jorryt J Matthee, Sarah E I Bosman, Jenny G Sorce, Joseph Lewis, et al. “Lyman-α Transmission Properties of the Intergalactic Medium in the CoDaII Simulation.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2021. <a href=\"https://doi.org/10.1093/mnras/stab2762\">https://doi.org/10.1093/mnras/stab2762</a>."},"intvolume":"       508","scopus_import":"1","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2004.14496"}],"oa_version":"Preprint","date_published":"2021-12-01T00:00:00Z","publication_status":"published","doi":"10.1093/mnras/stab2762","month":"12","status":"public","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"oa":1,"_id":"11522","date_updated":"2022-08-18T10:45:56Z","abstract":[{"text":"The decline in abundance of Lyman-α (Lyα) emitting galaxies at z ≳ 6 is a powerful and commonly used probe to constrain the progress of cosmic reionization. We use the CODAII simulation, which is a radiation hydrodynamic simulation featuring a box of ∼94 comoving Mpc side length, to compute the Lyα transmission properties of the intergalactic medium (IGM) at z ∼ 5.8 to 7. Our results mainly confirm previous studies, i.e. we find a declining Lyα transmission with redshift and a large sightline-to-sightline variation. However, motivated by the recent discovery of blue Lyα peaks at high redshift, we also analyse the IGM transmission on the blue side, which shows a rapid decline at z ≳ 6 of the blue transmission. This low transmission can be attributed not only to the presence of neutral regions but also to the residual neutral hydrogen within ionized regions, for which a density even as low as nHI∼10−9cm−3 (sometimes combined with kinematic effects) leads to a significantly reduced visibility. Still, we find that ∼1 per cent of sightlines towards M1600AB ∼ −21 galaxies at z ∼ 7 are transparent enough to allow a transmission of a blue Lyα peak. We discuss our results in the context of the interpretation of observations.","lang":"eng"}],"issue":"3","arxiv":1,"year":"2021","external_id":{"arxiv":["2004.14496"]},"volume":508,"keyword":["dark ages","reionization","first stars","intergalactic medium","galaxies: formation"],"quality_controlled":"1","article_processing_charge":"No","article_type":"original","type":"journal_article","language":[{"iso":"eng"}],"page":"3697-3709","date_created":"2022-07-07T09:30:21Z","publication":"Monthly Notices of the Royal Astronomical Society","publisher":"Oxford University Press","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","title":"Lyman-α transmission properties of the intergalactic medium in the CoDaII simulation","author":[{"first_name":"Max","last_name":"Gronke","full_name":"Gronke, Max"},{"first_name":"Pierre","last_name":"Ocvirk","full_name":"Ocvirk, Pierre"},{"last_name":"Mason","first_name":"Charlotte","full_name":"Mason, Charlotte"},{"full_name":"Matthee, Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"},{"full_name":"Bosman, Sarah E I","first_name":"Sarah E I","last_name":"Bosman"},{"first_name":"Jenny G","last_name":"Sorce","full_name":"Sorce, Jenny G"},{"last_name":"Lewis","first_name":"Joseph","full_name":"Lewis, Joseph"},{"full_name":"Ahn, Kyungjin","first_name":"Kyungjin","last_name":"Ahn"},{"full_name":"Aubert, Dominique","last_name":"Aubert","first_name":"Dominique"},{"full_name":"Dawoodbhoy, Taha","last_name":"Dawoodbhoy","first_name":"Taha"},{"full_name":"Iliev, Ilian T","first_name":"Ilian T","last_name":"Iliev"},{"last_name":"Shapiro","first_name":"Paul R","full_name":"Shapiro, Paul R"},{"full_name":"Yepes, Gustavo","first_name":"Gustavo","last_name":"Yepes"}],"acknowledgement":"The authors thank the referee for constructive feedback that improved the outcome of this study. We are grateful to Antoinette Songaila Cowie for sharing the ‘NEPLA4’ spectrum with us. This research has made use of NASA’s Astrophysics Data System, and many open source projects such as trident (Hummels et al. 2017), IPython (Pérez & Granger 2007), SciPy (Virtanen et al. 2019), NumPy (Walt et al. 2011), matplotlib (Hunter 2007), pandas (McKinney 2010), and the yt-project (Turk et al. 2011). MG was supported by NASA through the NASA Hubble Fellowship grant HST-HF2-51409 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. MG acknowledges support from NASA grants HST-GO-15643.017, and HST-AR15797.001 as well as XSEDE grant TG-AST180036. CAM acknowledges support by NASA Headquarters through the NASA Hubble Fellowship grant HST-HF2-51413.001-A. PRS was supported in part by U.S. NSF grant AST-1009799, NASA grant NNX11AE09G, and supercomputer resources from NSF XSEDE grant TG AST090005 and the Texas Advanced Computing Center (TACC) at The University of Texas at Austin. JM acknowledges a Zwicky Prize Fellowship from ETH Zurich. GY acknowledges financial support by MICIU/FEDER under project grant PGC2018-094975-C21. SEIB acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 669253). ITI was supported by the Science and Technology Facilities Council [grants ST/I000976/1, ST/F002858/1, ST/P000525/1, and ST/T000473/1]; and The Southeast Physics Network (SEPNet). KA was supported by NRF2016R1D1A1B04935414 and NRF-2016R1A5A1013277. KA also appreciates APCTP for its hospitality during completion of this work. PO acknowledges support from the French ANR funded project ORAGE (ANR-14-CE33-0016). ND and DA acknowledge funding from the French ANR for project ANR-12-JS05- 0001 (EMMA). The CoDa II simulation was performed at Oak Ridge National Laboratory/Oak Ridge Leadership Computing Facility on the Titan supercomputer (INCITE 2016 award AST031). Processing was performed on the Eos and Rhea clusters. Resolution study simulations were performed on Piz Daint at the Swiss National Supercomputing Center (PRACE Tier 0 award, project id pr37). The authors would like to acknowledge the High Performance Computing center of the University of Strasbourg for supporting this work by providing scientific support and access to computing resources. Part of the computing resources were funded by the Equipex EquipMeso project (Programme Investissements d’Avenir) and the CPER Alsacalcul/Big Data.","day":"01","extern":"1"},{"article_processing_charge":"No","article_type":"original","external_id":{"arxiv":["2102.07779"]},"volume":505,"quality_controlled":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: formation","galaxies: ISM","galaxies: starburst","dark ages","reionization","first stars"],"page":"1382-1412","date_created":"2022-07-07T09:33:39Z","publication":"Monthly Notices of the Royal Astronomical Society","type":"journal_article","language":[{"iso":"eng"}],"publisher":"Oxford University Press","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","title":"The X-SHOOTER Lyman α survey at z = 2 (XLS-z2) I: What makes a galaxy a Lyman α emitter?","acknowledgement":"We thank the referee for constructive comments and suggestions. We thank Dawn Erb, Ruari Mackenzie, Ivan Oteo, Ryan Sanders, and Johannes Zabl for useful discussions and suggestions. It is a pleasure to thank the ESO User Support, in particular Giacomo Beccari, Carlo Manara, John Pritchard, Marina Rejkuba, and Lowell Tacconi-Garman for assistance in the preparation and execution of the observations. Based on observations obtained with the VLT, programs 084.A-0303, 088.A-0672, 091.A-0413, 091.A-0546, 092.A0774, 097.A-0153, 098.A-0819, 099.A-0758, 099.A-0254, 101.B0779, and 102.A-0652. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by CALET and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. Based on observations made with the NASA/ESA HST through programs 9133, 9367, 11694, and 12471, and obtained from the Hubble Legacy Archive, which is a collaboration between the Space Telescope Science Institute (STScI/NASA), the Space Telescope European Coordinating Facility (ST-ECF/ESA), and the Canadian Astronomy Data Centre (CADC/NRC/CSA). This work is based on observations taken by the CANDELS Multi-Cycle Treasury Program with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. MG was supported by NASA through the NASA Hubble Fellowship grant HST-HF2-51409 and acknowledges support from HST grants\r\nHST-GO-15643.017-A, HST-AR-15039.003-A, and XSEDE grant TG-AST180036. GP acknowledges support from the Netherlands Research School for Astronomy (NOVA). RA acknowledges the support of ANID FONDECYT Regular Grant 1202007. We gratefully acknowledge the PYTHON programming language, its NUMPY, MATPLOTLIB, SCIPY, LMFIT (Jones et al. 2001; Hunter 2007; van der Walt, Colbert & Varoquaux 2011), PANDAS (McKinney 2010), and ASTROPY (Astropy Collaboration 2013) packages, and the TOPCAT analysis tool (Taylor 2013). Dedicated to the memory of A. C. J.Matthee (1953–2020).","day":"01","extern":"1","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","first_name":"Jorryt J","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J"},{"full_name":"Sobral, David","first_name":"David","last_name":"Sobral"},{"last_name":"Hayes","first_name":"Matthew","full_name":"Hayes, Matthew"},{"first_name":"Gabriele","last_name":"Pezzulli","full_name":"Pezzulli, Gabriele"},{"full_name":"Gronke, Max","last_name":"Gronke","first_name":"Max"},{"last_name":"Schaerer","first_name":"Daniel","full_name":"Schaerer, Daniel"},{"full_name":"Naidu, Rohan P","first_name":"Rohan P","last_name":"Naidu"},{"first_name":"Huub","last_name":"Röttgering","full_name":"Röttgering, Huub"},{"full_name":"Calhau, João","first_name":"João","last_name":"Calhau"},{"first_name":"Ana","last_name":"Paulino-Afonso","full_name":"Paulino-Afonso, Ana"},{"last_name":"Santos","first_name":"Sérgio","full_name":"Santos, Sérgio"},{"first_name":"Ricardo","last_name":"Amorín","full_name":"Amorín, Ricardo"}],"main_file_link":[{"url":"https://arxiv.org/abs/2102.07779","open_access":"1"}],"scopus_import":"1","intvolume":"       505","citation":{"short":"J.J. Matthee, D. Sobral, M. Hayes, G. Pezzulli, M. Gronke, D. Schaerer, R.P. Naidu, H. Röttgering, J. Calhau, A. Paulino-Afonso, S. Santos, R. Amorín, Monthly Notices of the Royal Astronomical Society 505 (2021) 1382–1412.","ieee":"J. J. Matthee <i>et al.</i>, “The X-SHOOTER Lyman α survey at z = 2 (XLS-z2) I: What makes a galaxy a Lyman α emitter?,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 505, no. 1. Oxford University Press, pp. 1382–1412, 2021.","ama":"Matthee JJ, Sobral D, Hayes M, et al. The X-SHOOTER Lyman α survey at z = 2 (XLS-z2) I: What makes a galaxy a Lyman α emitter? <i>Monthly Notices of the Royal Astronomical Society</i>. 2021;505(1):1382-1412. doi:<a href=\"https://doi.org/10.1093/mnras/stab1304\">10.1093/mnras/stab1304</a>","chicago":"Matthee, Jorryt J, David Sobral, Matthew Hayes, Gabriele Pezzulli, Max Gronke, Daniel Schaerer, Rohan P Naidu, et al. “The X-SHOOTER Lyman α Survey at z = 2 (XLS-Z2) I: What Makes a Galaxy a Lyman α Emitter?” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2021. <a href=\"https://doi.org/10.1093/mnras/stab1304\">https://doi.org/10.1093/mnras/stab1304</a>.","apa":"Matthee, J. J., Sobral, D., Hayes, M., Pezzulli, G., Gronke, M., Schaerer, D., … Amorín, R. (2021). The X-SHOOTER Lyman α survey at z = 2 (XLS-z2) I: What makes a galaxy a Lyman α emitter? <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stab1304\">https://doi.org/10.1093/mnras/stab1304</a>","mla":"Matthee, Jorryt J., et al. “The X-SHOOTER Lyman α Survey at z = 2 (XLS-Z2) I: What Makes a Galaxy a Lyman α Emitter?” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 505, no. 1, Oxford University Press, 2021, pp. 1382–412, doi:<a href=\"https://doi.org/10.1093/mnras/stab1304\">10.1093/mnras/stab1304</a>.","ista":"Matthee JJ, Sobral D, Hayes M, Pezzulli G, Gronke M, Schaerer D, Naidu RP, Röttgering H, Calhau J, Paulino-Afonso A, Santos S, Amorín R. 2021. The X-SHOOTER Lyman α survey at z = 2 (XLS-z2) I: What makes a galaxy a Lyman α emitter? Monthly Notices of the Royal Astronomical Society. 505(1), 1382–1412."},"publication_status":"published","doi":"10.1093/mnras/stab1304","oa_version":"Preprint","date_published":"2021-07-01T00:00:00Z","status":"public","oa":1,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"month":"07","date_updated":"2022-08-18T10:49:00Z","abstract":[{"lang":"eng","text":"We present the first results from the X-SHOOTER Lyman α survey at z = 2 (XLS-z2). XLS-z2 is a deep spectroscopic survey of 35 Lyman α emitters (LAEs) utilizing ≈90 h of exposure time with Very Large Telescope/X-SHOOTER and covers rest-frame Ly α to H α emission with R ≈ 4000. We present the sample selection, the observations, and the data reduction. Systemic redshifts are measured from rest-frame optical lines for 33/35 sources. In the stacked spectrum, our LAEs are characterized by an interstellar medium with little dust, a low metallicity, and a high ionization state. The ionizing sources are young hot stars that power strong emission lines in the optical and high-ionization lines in the ultraviolet (UV). The LAEs exhibit clumpy UV morphologies and have outflowing kinematics with blueshifted Si II absorption, a broad [O III] component, and a red-skewed Ly α line. Typically, 30 per cent of the Ly α photons escape, of which one quarter on the blue side of the systemic velocity. A fraction of Ly α photons escape directly at the systemic suggesting clear channels enabling an ≈10 per cent escape of ionizing photons, consistent with an inference based on Mg II. A combination of a low effective H I column density, a low dust content, and young starburst determines whether a star-forming galaxy is observed as an LAE. The first is possibly related to outflows and/or a fortunate viewing angle, while we find that the latter two in LAEs are typical for their stellar mass of 109 M⊙."}],"arxiv":1,"issue":"1","year":"2021","_id":"11523"},{"intvolume":"       505","citation":{"ieee":"S. Santos <i>et al.</i>, “The evolution of the UV luminosity and stellar mass functions of Lyman-α emitters from z ∼ 2 to z ∼ 6,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 505, no. 1. Oxford University Press, pp. 1117–1134, 2021.","ama":"Santos S, Sobral D, Butterworth J, et al. The evolution of the UV luminosity and stellar mass functions of Lyman-α emitters from z ∼ 2 to z ∼ 6. <i>Monthly Notices of the Royal Astronomical Society</i>. 2021;505(1):1117-1134. doi:<a href=\"https://doi.org/10.1093/mnras/stab1218\">10.1093/mnras/stab1218</a>","short":"S. Santos, D. Sobral, J. Butterworth, A. Paulino-Afonso, B. Ribeiro, E. da Cunha, J. Calhau, A.A. Khostovan, J.J. Matthee, P. Arrabal Haro, Monthly Notices of the Royal Astronomical Society 505 (2021) 1117–1134.","ista":"Santos S, Sobral D, Butterworth J, Paulino-Afonso A, Ribeiro B, da Cunha E, Calhau J, Khostovan AA, Matthee JJ, Arrabal Haro P. 2021. The evolution of the UV luminosity and stellar mass functions of Lyman-α emitters from z ∼ 2 to z ∼ 6. Monthly Notices of the Royal Astronomical Society. 505(1), 1117–1134.","apa":"Santos, S., Sobral, D., Butterworth, J., Paulino-Afonso, A., Ribeiro, B., da Cunha, E., … Arrabal Haro, P. (2021). The evolution of the UV luminosity and stellar mass functions of Lyman-α emitters from z ∼ 2 to z ∼ 6. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stab1218\">https://doi.org/10.1093/mnras/stab1218</a>","mla":"Santos, S., et al. “The Evolution of the UV Luminosity and Stellar Mass Functions of Lyman-α Emitters from z ∼ 2 to z ∼ 6.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 505, no. 1, Oxford University Press, 2021, pp. 1117–34, doi:<a href=\"https://doi.org/10.1093/mnras/stab1218\">10.1093/mnras/stab1218</a>.","chicago":"Santos, S, D Sobral, J Butterworth, A Paulino-Afonso, B Ribeiro, E da Cunha, J Calhau, A A Khostovan, Jorryt J Matthee, and P Arrabal Haro. “The Evolution of the UV Luminosity and Stellar Mass Functions of Lyman-α Emitters from z ∼ 2 to z ∼ 6.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2021. <a href=\"https://doi.org/10.1093/mnras/stab1218\">https://doi.org/10.1093/mnras/stab1218</a>."},"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2105.00007"}],"scopus_import":"1","oa_version":"Preprint","date_published":"2021-07-01T00:00:00Z","doi":"10.1093/mnras/stab1218","publication_status":"published","month":"07","status":"public","oa":1,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"_id":"11524","issue":"1","arxiv":1,"abstract":[{"text":"We measure the evolution of the rest-frame UV luminosity function (LF) and the stellar mass function (SMF) of Lyman-α (Ly α) emitters (LAEs) from z ∼ 2 to z ∼ 6 by exploring ∼4000 LAEs from the SC4K sample. We find a correlation between Ly α luminosity (LLy α) and rest-frame UV (MUV), with best fit MUV=−1.6+0.2−0.3log10(LLyα/ergs−1)+47+12−11 and a shallower relation between LLy α and stellar mass (M⋆), with best fit log10(M⋆/M⊙)=0.9+0.1−0.1log10(LLyα/ergs−1)−28+4.0−3.8⁠. An increasing LLy α cut predominantly lowers the number density of faint MUV and low M⋆ LAEs. We estimate a proxy for the full UV LFs and SMFs of LAEs with simple assumptions of the faint end slope. For the UV LF, we find a brightening of the characteristic UV luminosity (M∗UV⁠) with increasing redshift and a decrease of the characteristic number density (Φ*). For the SMF, we measure a characteristic stellar mass (⁠M∗⋆/M⊙⁠) increase with increasing redshift, and a Φ* decline. However, if we apply a uniform luminosity cut of log10(LLyα/ergs−1)≥43.0⁠, we find much milder to no evolution in the UV and SMF of LAEs. The UV luminosity density (ρUV) of the full sample of LAEs shows moderate evolution and the stellar mass density (ρM) decreases, with both being always lower than the total ρUV and ρM of more typical galaxies but slowly approaching them with increasing redshift. Overall, our results indicate that both ρUV and ρM of LAEs slowly approach the measurements of continuum-selected galaxies at z > 6, which suggests a key role of LAEs in the epoch of reionization.","lang":"eng"}],"date_updated":"2022-08-18T10:51:47Z","year":"2021","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","galaxies: luminosity function","mass function"],"quality_controlled":"1","volume":505,"external_id":{"arxiv":["2105.00007"]},"article_type":"original","article_processing_charge":"No","type":"journal_article","language":[{"iso":"eng"}],"publication":"Monthly Notices of the Royal Astronomical Society","page":"1117-1134","date_created":"2022-07-07T10:02:59Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publisher":"Oxford University Press","title":"The evolution of the UV luminosity and stellar mass functions of Lyman-α emitters from z ∼ 2 to z ∼ 6","author":[{"first_name":"S","last_name":"Santos","full_name":"Santos, S"},{"first_name":"D","last_name":"Sobral","full_name":"Sobral, D"},{"last_name":"Butterworth","first_name":"J","full_name":"Butterworth, J"},{"last_name":"Paulino-Afonso","first_name":"A","full_name":"Paulino-Afonso, A"},{"last_name":"Ribeiro","first_name":"B","full_name":"Ribeiro, B"},{"first_name":"E","last_name":"da Cunha","full_name":"da Cunha, E"},{"first_name":"J","last_name":"Calhau","full_name":"Calhau, J"},{"last_name":"Khostovan","first_name":"A A","full_name":"Khostovan, A A"},{"first_name":"Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J"},{"last_name":"Arrabal Haro","first_name":"P","full_name":"Arrabal Haro, P"}],"acknowledgement":"This research made use of Astropy, a community developed core Python package for Astronomy (Astropy Collaboration et al. 2013). topcat, a graphical tool for manipulating tabular data, was also utilized in this analysis (Taylor 2005). SG would like to thank Nastasha Wijers for the discussion on the column density distribution in EAGLE. SC gratefully acknowledges support from Swiss National Science Foundation grants PP00P2 163824 and PP00P2 190092, and from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme grant agreement No 864361. GP acknowledges support from the Swiss National Science Foundation (SNF) and from the Netherlands Research School for Astronomy (NOVA).","extern":"1","day":"01"},{"_id":"11525","year":"2021","abstract":[{"text":"The intensity of the Cosmic UV background (UVB), coming from all sources of ionizing photons such as star-forming galaxies and quasars, determines the thermal evolution and ionization state of the intergalactic medium (IGM) and is, therefore, a critical ingredient for models of cosmic structure formation. Most of the previous estimates are based on the comparison between observed and simulated Lyman-α forest. We present the results of an independent method to constrain the product of the UVB photoionization rate and the covering fraction of Lyman limit systems (LLSs) by searching for the fluorescent Lyman-α emission produced by self-shielded clouds. Because the expected surface brightness is well below current sensitivity limits for direct imaging, we developed a new method based on 3D stacking of the IGM around Lyman-α emitting galaxies (LAEs) between 2.9 < z < 6.6 using deep MUSE observations. Combining our results with covering fractions of LLSs obtained from mock cubes extracted from the EAGLE simulation, we obtain new and independent constraints on the UVB at z > 3 that are consistent with previous measurements, with a preference for relatively low UVB intensities at z = 3, and which suggest a non-monotonic decrease of ΓH I with increasing redshift between 3 < z < 5. This could suggest a possible tension between some UVB models and current observations which however require deeper and wider observations in Lyman-α emission and absorption to be confirmed. Assuming instead a value of UVB from current models, our results constrain the covering fraction of LLSs at 3 < z < 4.5 to be less than 25 per cent within 150 kpc from LAEs.","lang":"eng"}],"arxiv":1,"issue":"1","date_updated":"2022-08-18T10:54:19Z","month":"06","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"oa":1,"status":"public","date_published":"2021-06-01T00:00:00Z","oa_version":"Preprint","doi":"10.1093/mnras/stab796","publication_status":"published","citation":{"ista":"Gallego SG, Cantalupo S, Sarpas S, Duboeuf B, Lilly S, Pezzulli G, Marino RA, Matthee JJ, Wisotzki L, Schaye J, Richard J, Kusakabe H, Mauerhofer V. 2021. Constraining the cosmic UV background at z &#62; 3 with MUSE Lyman-α emission observations. Monthly Notices of the Royal Astronomical Society. 504(1), 16–32.","mla":"Gallego, Sofia G., et al. “Constraining the Cosmic UV Background at z &#62; 3 with MUSE Lyman-α Emission Observations.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 504, no. 1, Oxford University Press, 2021, pp. 16–32, doi:<a href=\"https://doi.org/10.1093/mnras/stab796\">10.1093/mnras/stab796</a>.","apa":"Gallego, S. G., Cantalupo, S., Sarpas, S., Duboeuf, B., Lilly, S., Pezzulli, G., … Mauerhofer, V. (2021). Constraining the cosmic UV background at z &#62; 3 with MUSE Lyman-α emission observations. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stab796\">https://doi.org/10.1093/mnras/stab796</a>","chicago":"Gallego, Sofia G, Sebastiano Cantalupo, Saeed Sarpas, Bastien Duboeuf, Simon Lilly, Gabriele Pezzulli, Raffaella Anna Marino, et al. “Constraining the Cosmic UV Background at z &#62; 3 with MUSE Lyman-α Emission Observations.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2021. <a href=\"https://doi.org/10.1093/mnras/stab796\">https://doi.org/10.1093/mnras/stab796</a>.","short":"S.G. Gallego, S. Cantalupo, S. Sarpas, B. Duboeuf, S. Lilly, G. Pezzulli, R.A. Marino, J.J. Matthee, L. Wisotzki, J. Schaye, J. Richard, H. Kusakabe, V. Mauerhofer, Monthly Notices of the Royal Astronomical Society 504 (2021) 16–32.","ama":"Gallego SG, Cantalupo S, Sarpas S, et al. Constraining the cosmic UV background at z &#62; 3 with MUSE Lyman-α emission observations. <i>Monthly Notices of the Royal Astronomical Society</i>. 2021;504(1):16-32. doi:<a href=\"https://doi.org/10.1093/mnras/stab796\">10.1093/mnras/stab796</a>","ieee":"S. G. Gallego <i>et al.</i>, “Constraining the cosmic UV background at z &#62; 3 with MUSE Lyman-α emission observations,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 504, no. 1. Oxford University Press, pp. 16–32, 2021."},"intvolume":"       504","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2103.09250"}],"scopus_import":"1","author":[{"full_name":"Gallego, Sofia G","first_name":"Sofia G","last_name":"Gallego"},{"last_name":"Cantalupo","first_name":"Sebastiano","full_name":"Cantalupo, Sebastiano"},{"full_name":"Sarpas, Saeed","first_name":"Saeed","last_name":"Sarpas"},{"full_name":"Duboeuf, Bastien","first_name":"Bastien","last_name":"Duboeuf"},{"full_name":"Lilly, Simon","last_name":"Lilly","first_name":"Simon"},{"full_name":"Pezzulli, Gabriele","last_name":"Pezzulli","first_name":"Gabriele"},{"last_name":"Marino","first_name":"Raffaella Anna","full_name":"Marino, Raffaella Anna"},{"orcid":"0000-0003-2871-127X","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","full_name":"Matthee, Jorryt J"},{"full_name":"Wisotzki, Lutz","first_name":"Lutz","last_name":"Wisotzki"},{"full_name":"Schaye, Joop","last_name":"Schaye","first_name":"Joop"},{"last_name":"Richard","first_name":"Johan","full_name":"Richard, Johan"},{"full_name":"Kusakabe, Haruka","first_name":"Haruka","last_name":"Kusakabe"},{"full_name":"Mauerhofer, Valentin","last_name":"Mauerhofer","first_name":"Valentin"}],"extern":"1","day":"01","acknowledgement":"This research made use of Astropy, a community developed core Python package for Astronomy (Astropy Collaboration et al. 2013). topcat, a graphical tool for manipulating tabular data, was also utilized in this analysis (Taylor 2005). SG would like to thank Nastasha Wijers for the discussion on the column density distribution in EAGLE. SC gratefully acknowledges support from Swiss National Science Foundation grants PP00P2 163824 and PP00P2 190092, and from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme grant agreement No 864361. GP acknowledges support from the Swiss National Science Foundation (SNF) and from the Netherlands Research School for Astronomy (NOVA).","title":"Constraining the cosmic UV background at z > 3 with MUSE Lyman-α emission observations","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publisher":"Oxford University Press","language":[{"iso":"eng"}],"type":"journal_article","publication":"Monthly Notices of the Royal Astronomical Society","date_created":"2022-07-07T10:07:11Z","page":"16-32","volume":504,"quality_controlled":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"external_id":{"arxiv":["2103.09250"]},"article_type":"original","article_processing_charge":"No"},{"month":"03","oa":1,"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"status":"public","_id":"11526","year":"2021","date_updated":"2022-08-18T10:56:28Z","abstract":[{"text":"We present the results from a MUSE survey of twelve z ≃ 3.15 quasars, which were selected to be much fainter (20 < iSDSS < 23) than in previous studies of giant Ly α nebulae around the brightest quasars (16.6 < iAB < 18.7). We detect H I Ly α nebulae around 100 per cent of our target quasars, with emission extending to scales of at least 60 physical kpc, and up to 190 pkpc. We explore correlations between properties of the nebulae and their host quasars, with the goal of connecting variations in the properties of the illuminating QSO to the response in nebular emission. We show that the surface brightness profiles of the nebulae are similar to those of nebulae around bright quasars, but with a lower normalization. Our targeted quasars are on average 3.7 mag (≃30 times) fainter in UV continuum than our bright reference sample, and yet the nebulae around them are only 4.3 times fainter in mean Ly α surface brightness, measured between 20 and 50 pkpc. We find significant correlations between the surface brightness of the nebula and the luminosity of the quasar in both UV continuum and Ly α. The latter can be interpreted as evidence for a substantial contribution from unresolved inner parts of the nebulae to the narrow components seen in the Ly α lines of some of our faint quasars, possibly from the inner circumgalactic medium or from the host galaxy’s interstellar medium.","lang":"eng"}],"arxiv":1,"issue":"1","citation":{"ama":"Mackenzie R, Pezzulli G, Cantalupo S, et al. Revealing the impact of quasar luminosity on giant Lyα nebulae. <i>Monthly Notices of the Royal Astronomical Society</i>. 2021;502(1):494-509. doi:<a href=\"https://doi.org/10.1093/mnras/staa3277\">10.1093/mnras/staa3277</a>","ieee":"R. Mackenzie <i>et al.</i>, “Revealing the impact of quasar luminosity on giant Lyα nebulae,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 502, no. 1. Oxford University Press, pp. 494–509, 2021.","short":"R. Mackenzie, G. Pezzulli, S. Cantalupo, R.A. Marino, S. Lilly, S. Muzahid, J.J. Matthee, J. Schaye, L. Wisotzki, Monthly Notices of the Royal Astronomical Society 502 (2021) 494–509.","chicago":"Mackenzie, Ruari, Gabriele Pezzulli, Sebastiano Cantalupo, Raffaella A Marino, Simon Lilly, Sowgat Muzahid, Jorryt J Matthee, Joop Schaye, and Lutz Wisotzki. “Revealing the Impact of Quasar Luminosity on Giant Lyα Nebulae.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2021. <a href=\"https://doi.org/10.1093/mnras/staa3277\">https://doi.org/10.1093/mnras/staa3277</a>.","mla":"Mackenzie, Ruari, et al. “Revealing the Impact of Quasar Luminosity on Giant Lyα Nebulae.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 502, no. 1, Oxford University Press, 2021, pp. 494–509, doi:<a href=\"https://doi.org/10.1093/mnras/staa3277\">10.1093/mnras/staa3277</a>.","ista":"Mackenzie R, Pezzulli G, Cantalupo S, Marino RA, Lilly S, Muzahid S, Matthee JJ, Schaye J, Wisotzki L. 2021. Revealing the impact of quasar luminosity on giant Lyα nebulae. Monthly Notices of the Royal Astronomical Society. 502(1), 494–509.","apa":"Mackenzie, R., Pezzulli, G., Cantalupo, S., Marino, R. A., Lilly, S., Muzahid, S., … Wisotzki, L. (2021). Revealing the impact of quasar luminosity on giant Lyα nebulae. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staa3277\">https://doi.org/10.1093/mnras/staa3277</a>"},"intvolume":"       502","main_file_link":[{"url":"https://arxiv.org/abs/2010.12589","open_access":"1"}],"scopus_import":"1","date_published":"2021-03-01T00:00:00Z","oa_version":"Preprint","publication_status":"published","doi":"10.1093/mnras/staa3277","title":"Revealing the impact of quasar luminosity on giant Lyα nebulae","publisher":"Oxford University Press","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","author":[{"full_name":"Mackenzie, Ruari","first_name":"Ruari","last_name":"Mackenzie"},{"last_name":"Pezzulli","first_name":"Gabriele","full_name":"Pezzulli, Gabriele"},{"last_name":"Cantalupo","first_name":"Sebastiano","full_name":"Cantalupo, Sebastiano"},{"first_name":"Raffaella A","last_name":"Marino","full_name":"Marino, Raffaella A"},{"full_name":"Lilly, Simon","first_name":"Simon","last_name":"Lilly"},{"last_name":"Muzahid","first_name":"Sowgat","full_name":"Muzahid, Sowgat"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X","first_name":"Jorryt J","full_name":"Matthee, Jorryt J"},{"full_name":"Schaye, Joop","first_name":"Joop","last_name":"Schaye"},{"full_name":"Wisotzki, Lutz","first_name":"Lutz","last_name":"Wisotzki"}],"day":"01","extern":"1","acknowledgement":"The authors thank Daichi Kashino, for providing access to unpublished zCOSMOS Deep data, and Jakob S. den Brok for sharing code used in den Brok et al. (2020). GP and SC acknowledge the support of the Swiss National Science Foundation [grant PP00P2163824]. SM is supported by the Experienced Researchers Fellowship, Alexander von Humboldt-Stiftung, Germany. This work is based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under the MUSE GTO programme. The major analysis and production of figures in this work was conducted in Python, using standard libraries which include NumPy (Harris et al. 2020), SciPy (Virtanen et al. 2020), Matplotlib (Hunter 2007) and the interactive command shell IPython (Pérez & Granger 2007). This research also made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013), and Photutils, an Astropy package for detection and photometry of astronomica sources (Bradley et al. 2019). The python interface dustmaps (Green 2018) was used to query galactic extinction maps. topcat, a graphical tool for manipulating tabular data, was also utilized in this analysis (Taylor 2005). This research has made use of the \"Aladin sky atlas\" developed at CDS, Strasbourg Observatory, France (Bonnarel et al. 2000).","external_id":{"arxiv":["2010.12589"]},"quality_controlled":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics","techniques: imaging spectroscopy","intergalactic medium","quasars: emission lines","quasars: general"],"volume":502,"article_type":"original","article_processing_charge":"No","language":[{"iso":"eng"}],"type":"journal_article","date_created":"2022-07-07T10:11:15Z","page":"494-509","publication":"Monthly Notices of the Royal Astronomical Society"},{"acknowledgement":"We thank the anonymous referee for their constructive comments. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. We thank Jarle Brinchmann, Rob Crain and David Sobral for discussions. We acknowledge the use of the Topcat software (Taylor 2013) for assisting in rapid exploration of multi-dimensional datasets and the use of Python and its numpy, matplotlib and pandas packages.","day":"05","extern":"1","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X","first_name":"Jorryt J","full_name":"Matthee, Jorryt J"}],"publisher":"Springer Nature","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","title":"Differences in galaxy colours are not just about the mass","date_created":"2022-07-14T13:13:39Z","page":"984-985","publication":"Nature Astronomy","type":"journal_article","language":[{"iso":"eng"}],"article_type":"original","article_processing_charge":"No","external_id":{"arxiv":["1802.06786"]},"quality_controlled":"1","keyword":["Astronomy and Astrophysics","galaxies","formation - galaxies","evolution - galaxies","star formation - galaxies","abundances"],"volume":5,"date_updated":"2022-08-19T08:37:58Z","arxiv":1,"abstract":[{"text":"Observations show that star-forming galaxies reside on a tight three-dimensional plane between mass, gas-phase metallicity and star formation rate (SFR), which can be explained by the interplay between metal-poor gas inflows, SFR and outflows. However, different metals are released on different time-scales, which may affect the slope of this relation. Here, we use central, star-forming galaxies with Mstar = 109.0−10.5 M\f from the EAGLE hydrodynamical simulation to examine three-dimensional relations between mass, SFR and chemical enrichment using absolute and relative C, N, O and Fe abundances. We show that the scatter is smaller when gas-phase α-enhancement is used rather than metallicity. A similar plane also exists for stellar α-enhancement, implying that present-day specific SFRs are correlated with long time-scale star formation histories. Between z = 0 and 1, the α-enhancement plane is even more insensitive to redshift than the plane using metallicity. However, it evolves at z > 1 due to lagging iron yields. At fixed mass, galaxies with higher SFRs have star formation histories shifted toward late times, are more α-enhanced and this α-enhancement increases with redshift as observed. These findings suggest that relations between physical properties inferred from observations may be affected by systematic variations in α-enhancements.","lang":"eng"}],"year":"2021","_id":"11585","status":"public","publication_identifier":{"eissn":["2397-3366"]},"oa":1,"month":"07","publication_status":"published","doi":"10.1038/s41550-021-01415-y","oa_version":"Preprint","date_published":"2021-07-05T00:00:00Z","scopus_import":"1","main_file_link":[{"url":"https://arxiv.org/abs/1802.06786","open_access":"1"}],"intvolume":"         5","citation":{"short":"J.J. Matthee, Nature Astronomy 5 (2021) 984–985.","ama":"Matthee JJ. Differences in galaxy colours are not just about the mass. <i>Nature Astronomy</i>. 2021;5:984-985. doi:<a href=\"https://doi.org/10.1038/s41550-021-01415-y\">10.1038/s41550-021-01415-y</a>","ieee":"J. J. Matthee, “Differences in galaxy colours are not just about the mass,” <i>Nature Astronomy</i>, vol. 5. Springer Nature, pp. 984–985, 2021.","chicago":"Matthee, Jorryt J. “Differences in Galaxy Colours Are Not Just about the Mass.” <i>Nature Astronomy</i>. Springer Nature, 2021. <a href=\"https://doi.org/10.1038/s41550-021-01415-y\">https://doi.org/10.1038/s41550-021-01415-y</a>.","apa":"Matthee, J. J. (2021). Differences in galaxy colours are not just about the mass. <i>Nature Astronomy</i>. Springer Nature. <a href=\"https://doi.org/10.1038/s41550-021-01415-y\">https://doi.org/10.1038/s41550-021-01415-y</a>","mla":"Matthee, Jorryt J. “Differences in Galaxy Colours Are Not Just about the Mass.” <i>Nature Astronomy</i>, vol. 5, Springer Nature, 2021, pp. 984–85, doi:<a href=\"https://doi.org/10.1038/s41550-021-01415-y\">10.1038/s41550-021-01415-y</a>.","ista":"Matthee JJ. 2021. Differences in galaxy colours are not just about the mass. Nature Astronomy. 5, 984–985."}},{"doi":"10.3847/1538-3881/ac166a","publication_status":"published","oa_version":"Preprint","date_published":"2021-10-21T00:00:00Z","scopus_import":"1","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2107.06301"}],"citation":{"ama":"Audenaert J, Kuszlewicz JS, Handberg R, et al. TESS Data for Asteroseismology (T’DA) stellar variability classification pipeline: Setup and application to the Kepler Q9 data. <i>The Astronomical Journal</i>. 2021;162(5). doi:<a href=\"https://doi.org/10.3847/1538-3881/ac166a\">10.3847/1538-3881/ac166a</a>","ieee":"J. Audenaert <i>et al.</i>, “TESS Data for Asteroseismology (T’DA) stellar variability classification pipeline: Setup and application to the Kepler Q9 data,” <i>The Astronomical Journal</i>, vol. 162, no. 5. IOP Publishing, 2021.","short":"J. Audenaert, J.S. Kuszlewicz, R. Handberg, A. Tkachenko, D.J. Armstrong, M. Hon, R. Kgoadi, M.N. Lund, K.J. Bell, L.A. Bugnet, D.M. Bowman, C. Johnston, R.A. García, D. Stello, L. Molnár, E. Plachy, D. Buzasi, C. Aerts, The Astronomical Journal 162 (2021).","chicago":"Audenaert, J., J. S. Kuszlewicz, R. Handberg, A. Tkachenko, D. J. Armstrong, M. Hon, R. Kgoadi, et al. “TESS Data for Asteroseismology (T’DA) Stellar Variability Classification Pipeline: Setup and Application to the Kepler Q9 Data.” <i>The Astronomical Journal</i>. IOP Publishing, 2021. <a href=\"https://doi.org/10.3847/1538-3881/ac166a\">https://doi.org/10.3847/1538-3881/ac166a</a>.","mla":"Audenaert, J., et al. “TESS Data for Asteroseismology (T’DA) Stellar Variability Classification Pipeline: Setup and Application to the Kepler Q9 Data.” <i>The Astronomical Journal</i>, vol. 162, no. 5, 209, IOP Publishing, 2021, doi:<a href=\"https://doi.org/10.3847/1538-3881/ac166a\">10.3847/1538-3881/ac166a</a>.","ista":"Audenaert J, Kuszlewicz JS, Handberg R, Tkachenko A, Armstrong DJ, Hon M, Kgoadi R, Lund MN, Bell KJ, Bugnet LA, Bowman DM, Johnston C, García RA, Stello D, Molnár L, Plachy E, Buzasi D, Aerts C. 2021. TESS Data for Asteroseismology (T’DA) stellar variability classification pipeline: Setup and application to the Kepler Q9 data. The Astronomical Journal. 162(5), 209.","apa":"Audenaert, J., Kuszlewicz, J. S., Handberg, R., Tkachenko, A., Armstrong, D. J., Hon, M., … Aerts, C. (2021). TESS Data for Asteroseismology (T’DA) stellar variability classification pipeline: Setup and application to the Kepler Q9 data. <i>The Astronomical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-3881/ac166a\">https://doi.org/10.3847/1538-3881/ac166a</a>"},"intvolume":"       162","arxiv":1,"abstract":[{"lang":"eng","text":"The NASA Transiting Exoplanet Survey Satellite (TESS) is observing tens of millions of stars with time spans ranging from ∼27 days to about 1 yr of continuous observations. This vast amount of data contains a wealth of information for variability, exoplanet, and stellar astrophysics studies but requires a number of processing steps before it can be fully utilized. In order to efficiently process all the TESS data and make it available to the wider scientific community, the TESS Data for Asteroseismology working group, as part of the TESS Asteroseismic Science Consortium, has created an automated open-source processing pipeline to produce light curves corrected for systematics from the short- and long-cadence raw photometry data and to classify these according to stellar variability type. We will process all stars down to a TESS magnitude of 15. This paper is the next in a series detailing how the pipeline works. Here, we present our methodology for the automatic variability classification of TESS photometry using an ensemble of supervised learners that are combined into a metaclassifier. We successfully validate our method using a carefully constructed labeled sample of Kepler Q9 light curves with a 27.4 days time span mimicking single-sector TESS observations, on which we obtain an overall accuracy of 94.9%. We demonstrate that our methodology can successfully classify stars outside of our labeled sample by applying it to all ∼167,000 stars observed in Q9 of the Kepler space mission."}],"issue":"5","date_updated":"2022-08-19T10:01:56Z","year":"2021","article_number":"209","_id":"11604","status":"public","oa":1,"publication_identifier":{"eissn":["1538-3881"],"issn":["0004-6256"]},"month":"10","publication":"The Astronomical Journal","date_created":"2022-07-18T11:54:55Z","type":"journal_article","language":[{"iso":"eng"}],"article_type":"original","article_processing_charge":"No","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"volume":162,"quality_controlled":"1","external_id":{"arxiv":["2107.06301"]},"acknowledgement":"The research leading to these results has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement No. 670519: MAMSIE), from the KU Leuven Research Council (grant C16/18/005: PARADISE), from the Research Foundation Flanders (FWO) under grant agreement G0H5416N (ERC Runner Up Project), as well as from the BELgian federal Science Policy Office (BELSPO) through PRODEX grant PLATO. D.J.A acknowledges support from the STFC via an Ernest Rutherford Fellowship (ST/R00384X/1). Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (grant agreement No.: DNRF106). R.H. and M.N.L. acknowledge the ESA PRODEX program. This research was supported by the National Aeronautics and Space Administration (80NSSC18K1585 and 80NSSC19K0379) awarded through the TESS Guest Investigator Program. K.J.B. is supported by the National Science Foundation under Award AST-1903828. J.S.K and K.J.B. were supported by funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement no. 338251 (StellarAges). D.M.B. gratefully acknowledges funding from a senior postdoctoral fellowship from the Research Foundation Flanders (FWO) with grant agreement No. 1286521N. The research leading to these results has received funding from the Research Foundation Flanders (FWO) under grant agreement G0A2917N (BlackGEM). R.A.G. acknowledges support from the GOLF and PLATO CNES grants. L.M. was supported by the Premium Postdoctoral Research Program of the Hungarian Academy of Sciences. The research leading to these results has been supported by the Hungarian National Research, Development, and Innovation Office (NKFIH) grant KH_18 130405 and the Lendület LP2014-17 and LP2018-7/2020 grants of the Hungarian Academy of Sciences. D.B. acknowledges support from the NASA TESS Guest Investigator Program under award 80NSSC19K0385.\r\n\r\nThis paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). Funding for the TESS mission is provided by NASA's Science Mission directorate. This research has made use of NASA's Astrophysics Data System as well as the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Funding for the TESS Asteroseismic Science Operations Centre is provided by the Danish National Research Foundation (Grant agreement no.: DNRF106), ESA PRODEX (PEA 4000119301), and the Stellar Astrophysics Centre (SAC) at Aarhus University. We thank the TESS team and staff and TASC/TASOC for their support of the present work.\r\n\r\nThis paper includes data collected by the Kepler mission. Funding for the Kepler and K2 mission was provided by NASA's Science Mission Directorate. The authors acknowledge the efforts of the Kepler Mission team in obtaining the light-curve data and data validation products used in this publication. These data were generated by the Kepler Mission science pipeline through the efforts of the Kepler Science Operations Center and Science Office. The Kepler light curves are archived at the Mikulski Archive for Space Telescopes.\r\n\r\nThe numerical results presented in this work were obtained at the Centre for Scientific Computing, Aarhus. 37 This research made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013, 2018).\r\n\r\nSoftware: Scikit-learn (Pedregosa et al. 2011), Numpy (Harris et al. 2020), Astropy (Astropy Collaboration et al. 2013, 2018), Scipy (Virtanen et al. 2020), Pandas (McKinney 2010; Pandas Development Team 2020), Lightkurve (Lightkurve Collaboration et al. 2018), XGBoost (Chen & Guestrin 2016), Tensorflow (Abadi et al. 2015).","extern":"1","day":"21","author":[{"full_name":"Audenaert, J.","first_name":"J.","last_name":"Audenaert"},{"first_name":"J. S.","last_name":"Kuszlewicz","full_name":"Kuszlewicz, J. S."},{"first_name":"R.","last_name":"Handberg","full_name":"Handberg, R."},{"first_name":"A.","last_name":"Tkachenko","full_name":"Tkachenko, A."},{"full_name":"Armstrong, D. J.","first_name":"D. J.","last_name":"Armstrong"},{"last_name":"Hon","first_name":"M.","full_name":"Hon, M."},{"full_name":"Kgoadi, R.","last_name":"Kgoadi","first_name":"R."},{"last_name":"Lund","first_name":"M. N.","full_name":"Lund, M. N."},{"first_name":"K. J.","last_name":"Bell","full_name":"Bell, K. J."},{"id":"d9edb345-f866-11ec-9b37-d119b5234501","last_name":"Bugnet","orcid":"0000-0003-0142-4000","first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle"},{"full_name":"Bowman, D. M.","first_name":"D. M.","last_name":"Bowman"},{"first_name":"C.","last_name":"Johnston","full_name":"Johnston, C."},{"first_name":"R. A.","last_name":"García","full_name":"García, R. A."},{"last_name":"Stello","first_name":"D.","full_name":"Stello, D."},{"full_name":"Molnár, L.","last_name":"Molnár","first_name":"L."},{"full_name":"Plachy, E.","first_name":"E.","last_name":"Plachy"},{"first_name":"D.","last_name":"Buzasi","full_name":"Buzasi, D."},{"first_name":"C.","last_name":"Aerts","full_name":"Aerts, C."}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publisher":"IOP Publishing","title":"TESS Data for Asteroseismology (T’DA) stellar variability classification pipeline: Setup and application to the Kepler Q9 data"},{"author":[{"first_name":"Lisa Annabelle","orcid":"0000-0003-0142-4000","last_name":"Bugnet","id":"d9edb345-f866-11ec-9b37-d119b5234501","full_name":"Bugnet, Lisa Annabelle"},{"full_name":"Prat, V.","last_name":"Prat","first_name":"V."},{"full_name":"Mathis, S.","first_name":"S.","last_name":"Mathis"},{"first_name":"A.","last_name":"Astoul","full_name":"Astoul, A."},{"full_name":"Augustson, K.","last_name":"Augustson","first_name":"K."},{"full_name":"García, R. A.","last_name":"García","first_name":"R. A."},{"last_name":"Mathur","first_name":"S.","full_name":"Mathur, S."},{"first_name":"L.","last_name":"Amard","full_name":"Amard, L."},{"first_name":"C.","last_name":"Neiner","full_name":"Neiner, C."}],"extern":"1","day":"07","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publisher":"EDP Sciences","title":"Magnetic signatures on mixed-mode frequencies: I. An axisymmetric fossil field inside the core of red giants","type":"journal_article","language":[{"iso":"eng"}],"publication":"Astronomy & Astrophysics","date_created":"2022-07-18T12:10:59Z","quality_controlled":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics","stars","oscillations / stars","magnetic field / stars","interiors / stars","evolution / stars","rotation"],"volume":650,"external_id":{"arxiv":["2102.01216"]},"article_processing_charge":"No","article_type":"original","article_number":"A53","_id":"11605","arxiv":1,"abstract":[{"text":"Context. The discovery of moderate differential rotation between the core and the envelope of evolved solar-like stars could be the signature of a strong magnetic field trapped inside the radiative interior. The population of intermediate-mass red giants presenting surprisingly low-amplitude mixed modes (i.e. oscillation modes that behave as acoustic modes in their external envelope and as gravity modes in their core) could also arise from the effect of an internal magnetic field. Indeed, stars more massive than about 1.1 solar masses are known to develop a convective core during their main sequence. The field generated by the dynamo triggered by this convection could be the progenitor of a strong fossil magnetic field trapped inside the core of the star for the remainder of its evolution.\r\n\r\nAims. Observations of mixed modes can constitute an excellent probe of the deepest layers of evolved solar-like stars, and magnetic fields in those regions can impact their propagation. The magnetic perturbation on mixed modes may therefore be visible in asteroseismic data. To unravel which constraints can be obtained from observations, we theoretically investigate the effects of a plausible mixed axisymmetric magnetic field with various amplitudes on the mixed-mode frequencies of evolved solar-like stars.\r\n\r\nMethods. First-order frequency perturbations due to an axisymmetric magnetic field were computed for dipolar and quadrupolar mixed modes. These computations were carried out for a range of stellar ages, masses, and metallicities.\r\n\r\nConclusions. We show that typical fossil-field strengths of 0.1 − 1 MG, consistent with the presence of a dynamo in the convective core during the main sequence, provoke significant asymmetries on mixed-mode frequency multiplets during the red giant branch. We provide constraints and methods for the detectability of such magnetic signatures. We show that these signatures may be detectable in asteroseismic data for field amplitudes small enough for the amplitude of the modes not to be affected by the conversion of gravity into Alfvén waves inside the magnetised interior. Finally, we infer an upper limit for the strength of the field and the associated lower limit for the timescale of its action in order to redistribute angular momentum in stellar interiors.","lang":"eng"}],"date_updated":"2022-08-19T10:06:33Z","year":"2021","month":"06","status":"public","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"oa":1,"oa_version":"Preprint","date_published":"2021-06-07T00:00:00Z","doi":"10.1051/0004-6361/202039159","publication_status":"published","citation":{"chicago":"Bugnet, Lisa Annabelle, V. Prat, S. Mathis, A. Astoul, K. Augustson, R. A. García, S. Mathur, L. Amard, and C. Neiner. “Magnetic Signatures on Mixed-Mode Frequencies: I. An Axisymmetric Fossil Field inside the Core of Red Giants.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2021. <a href=\"https://doi.org/10.1051/0004-6361/202039159\">https://doi.org/10.1051/0004-6361/202039159</a>.","ista":"Bugnet LA, Prat V, Mathis S, Astoul A, Augustson K, García RA, Mathur S, Amard L, Neiner C. 2021. Magnetic signatures on mixed-mode frequencies: I. An axisymmetric fossil field inside the core of red giants. Astronomy &#38; Astrophysics. 650, A53.","apa":"Bugnet, L. A., Prat, V., Mathis, S., Astoul, A., Augustson, K., García, R. A., … Neiner, C. (2021). Magnetic signatures on mixed-mode frequencies: I. An axisymmetric fossil field inside the core of red giants. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202039159\">https://doi.org/10.1051/0004-6361/202039159</a>","mla":"Bugnet, Lisa Annabelle, et al. “Magnetic Signatures on Mixed-Mode Frequencies: I. An Axisymmetric Fossil Field inside the Core of Red Giants.” <i>Astronomy &#38; Astrophysics</i>, vol. 650, A53, EDP Sciences, 2021, doi:<a href=\"https://doi.org/10.1051/0004-6361/202039159\">10.1051/0004-6361/202039159</a>.","ama":"Bugnet LA, Prat V, Mathis S, et al. Magnetic signatures on mixed-mode frequencies: I. An axisymmetric fossil field inside the core of red giants. <i>Astronomy &#38; Astrophysics</i>. 2021;650. doi:<a href=\"https://doi.org/10.1051/0004-6361/202039159\">10.1051/0004-6361/202039159</a>","ieee":"L. A. Bugnet <i>et al.</i>, “Magnetic signatures on mixed-mode frequencies: I. An axisymmetric fossil field inside the core of red giants,” <i>Astronomy &#38; Astrophysics</i>, vol. 650. EDP Sciences, 2021.","short":"L.A. Bugnet, V. Prat, S. Mathis, A. Astoul, K. Augustson, R.A. García, S. Mathur, L. Amard, C. Neiner, Astronomy &#38; Astrophysics 650 (2021)."},"intvolume":"       650","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2102.01216"}],"scopus_import":"1"}]