[{"has_accepted_license":"1","month":"06","oa_version":"Published Version","ec_funded":1,"external_id":{"arxiv":["2405.04420"]},"day":"17","file_date_updated":"2024-07-29T07:18:12Z","abstract":[{"text":"We study selfish mining attacks in longest-chain blockchains like Bitcoin, but where the proof of work is replaced with efficient proof systems - like proofs of stake or proofs of space - and consider the problem of computing an optimal selfish mining attack which maximizes expected relative revenue of the adversary, thus minimizing the chain quality. To this end, we propose a novel selfish mining attack that aims to maximize this objective and formally model the attack as a Markov decision process (MDP). We then present a formal analysis procedure which computes an ϵ-tight lower bound on the optimal expected relative revenue in the MDP and a strategy that achieves this ϵ-tight lower bound, where ϵ > 0 may be any specified precision. Our analysis is fully automated and provides formal guarantees on the correctness. We evaluate our selfish mining attack and observe that it achieves superior expected relative revenue compared to two considered baselines.\r\nIn concurrent work [Sarenche FC'24] does an automated analysis on selfish mining in predictable longest-chain blockchains based on efficient proof systems. Predictable means the randomness for the challenges is fixed for many blocks (as used e.g., in Ouroboros), while we consider unpredictable (Bitcoin-like) chains where the challenge is derived from the previous block.","lang":"eng"}],"publication_status":"published","arxiv":1,"date_published":"2024-06-17T00:00:00Z","oa":1,"year":"2024","_id":"17328","publisher":"Association for Computing Machinery","file":[{"content_type":"application/pdf","file_size":832034,"access_level":"open_access","success":1,"relation":"main_file","checksum":"6122bd97b42751ff81c452a19970f67d","file_id":"17334","date_updated":"2024-07-29T07:18:12Z","file_name":"2024_ACM_Chatterjee.pdf","date_created":"2024-07-29T07:18:12Z","creator":"dernst"}],"type":"conference","author":[{"id":"2E5DCA20-F248-11E8-B48F-1D18A9856A87","full_name":"Chatterjee, Krishnendu","orcid":"0000-0002-4561-241X","first_name":"Krishnendu","last_name":"Chatterjee"},{"first_name":"Amirali","last_name":"Ebrahimzadeh","full_name":"Ebrahimzadeh, Amirali"},{"last_name":"Karrabi","first_name":"Mehrdad","orcid":"0009-0007-5253-9170","full_name":"Karrabi, Mehrdad","id":"67638922-f394-11eb-9cf6-f20423e08757"},{"full_name":"Pietrzak, Krzysztof Z","id":"3E04A7AA-F248-11E8-B48F-1D18A9856A87","orcid":"0000-0002-9139-1654","first_name":"Krzysztof Z","last_name":"Pietrzak"},{"id":"2D82B818-F248-11E8-B48F-1D18A9856A87","full_name":"Yeo, Michelle X","orcid":"0009-0001-3676-4809","first_name":"Michelle X","last_name":"Yeo"},{"first_name":"Dorde","last_name":"Zikelic","id":"294AA7A6-F248-11E8-B48F-1D18A9856A87","full_name":"Zikelic, Dorde","orcid":"0000-0002-4681-1699"}],"date_created":"2024-07-28T22:01:10Z","doi":"10.1145/3662158.3662769","project":[{"_id":"0599E47C-7A3F-11EA-A408-12923DDC885E","name":"Formal Methods for Stochastic Models: Algorithms and Applications","call_identifier":"H2020","grant_number":"863818"}],"department":[{"_id":"KrCh"},{"_id":"KrPi"}],"ddc":["000"],"corr_author":"1","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"citation":{"ama":"Chatterjee K, Ebrahimzadeh A, Karrabi M, Pietrzak KZ, Yeo MX, Zikelic D. Fully automated selfish mining analysis in efficient proof systems blockchains. In: <i>Proceedings of the 43rd Annual ACM Symposium on Principles of Distributed Computing</i>. Association for Computing Machinery; 2024:268-278. doi:<a href=\"https://doi.org/10.1145/3662158.3662769\">10.1145/3662158.3662769</a>","apa":"Chatterjee, K., Ebrahimzadeh, A., Karrabi, M., Pietrzak, K. Z., Yeo, M. X., &#38; Zikelic, D. (2024). Fully automated selfish mining analysis in efficient proof systems blockchains. In <i>Proceedings of the 43rd Annual ACM Symposium on Principles of Distributed Computing</i> (pp. 268–278). Nantes, France: Association for Computing Machinery. <a href=\"https://doi.org/10.1145/3662158.3662769\">https://doi.org/10.1145/3662158.3662769</a>","ieee":"K. Chatterjee, A. Ebrahimzadeh, M. Karrabi, K. Z. Pietrzak, M. X. Yeo, and D. Zikelic, “Fully automated selfish mining analysis in efficient proof systems blockchains,” in <i>Proceedings of the 43rd Annual ACM Symposium on Principles of Distributed Computing</i>, Nantes, France, 2024, pp. 268–278.","chicago":"Chatterjee, Krishnendu, Amirali Ebrahimzadeh, Mehrdad Karrabi, Krzysztof Z Pietrzak, Michelle X Yeo, and Dorde Zikelic. “Fully Automated Selfish Mining Analysis in Efficient Proof Systems Blockchains.” In <i>Proceedings of the 43rd Annual ACM Symposium on Principles of Distributed Computing</i>, 268–78. Association for Computing Machinery, 2024. <a href=\"https://doi.org/10.1145/3662158.3662769\">https://doi.org/10.1145/3662158.3662769</a>.","ista":"Chatterjee K, Ebrahimzadeh A, Karrabi M, Pietrzak KZ, Yeo MX, Zikelic D. 2024. Fully automated selfish mining analysis in efficient proof systems blockchains. Proceedings of the 43rd Annual ACM Symposium on Principles of Distributed Computing. PODC: Symposium on Principles of Distributed Computing, 268–278.","mla":"Chatterjee, Krishnendu, et al. “Fully Automated Selfish Mining Analysis in Efficient Proof Systems Blockchains.” <i>Proceedings of the 43rd Annual ACM Symposium on Principles of Distributed Computing</i>, Association for Computing Machinery, 2024, pp. 268–78, doi:<a href=\"https://doi.org/10.1145/3662158.3662769\">10.1145/3662158.3662769</a>.","short":"K. Chatterjee, A. Ebrahimzadeh, M. Karrabi, K.Z. Pietrzak, M.X. Yeo, D. Zikelic, in:, Proceedings of the 43rd Annual ACM Symposium on Principles of Distributed Computing, Association for Computing Machinery, 2024, pp. 268–278."},"page":"268-278","publication":"Proceedings of the 43rd Annual ACM Symposium on Principles of Distributed Computing","scopus_import":"1","das_tickbox":"1","status":"public","conference":{"name":"PODC: Symposium on Principles of Distributed Computing","location":"Nantes, France","end_date":"2024-06-21","start_date":"2024-06-17"},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"quality_controlled":"1","article_processing_charge":"Yes (via OA deal)","title":"Fully automated selfish mining analysis in efficient proof systems blockchains","acknowledgement":"This work was supported in part by the ERC-2020-CoG 863818 (FoRM-SMArt) grant and the MOE-T2EP20122-0014 (Data-Driven Distributed Algorithms) grant.\r\n","date_updated":"2026-07-07T13:30:07Z","publication_identifier":{"isbn":["9798400706684"]}},{"status":"public","isi":1,"scopus_import":"1","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"citation":{"ama":"Bose S, Henzinger TA, Lehtinen K, Schewe S, Totzke P. History-deterministic timed automata. <i>Logical Methods in Computer Science</i>. 2024;20(4):1-28. doi:<a href=\"https://doi.org/10.46298/lmcs-20(4:1)2024\">10.46298/lmcs-20(4:1)2024</a>","apa":"Bose, S., Henzinger, T. A., Lehtinen, K., Schewe, S., &#38; Totzke, P. (2024). History-deterministic timed automata. <i>Logical Methods in Computer Science</i>. EPI Sciences. <a href=\"https://doi.org/10.46298/lmcs-20(4:1)2024\">https://doi.org/10.46298/lmcs-20(4:1)2024</a>","ieee":"S. Bose, T. A. Henzinger, K. Lehtinen, S. Schewe, and P. Totzke, “History-deterministic timed automata,” <i>Logical Methods in Computer Science</i>, vol. 20, no. 4. EPI Sciences, pp. 1–28, 2024.","short":"S. Bose, T.A. Henzinger, K. Lehtinen, S. Schewe, P. Totzke, Logical Methods in Computer Science 20 (2024) 1–28.","chicago":"Bose, Sougata, Thomas A Henzinger, Karoliina Lehtinen, Sven Schewe, and Patrick Totzke. “History-Deterministic Timed Automata.” <i>Logical Methods in Computer Science</i>. EPI Sciences, 2024. <a href=\"https://doi.org/10.46298/lmcs-20(4:1)2024\">https://doi.org/10.46298/lmcs-20(4:1)2024</a>.","mla":"Bose, Sougata, et al. “History-Deterministic Timed Automata.” <i>Logical Methods in Computer Science</i>, vol. 20, no. 4, EPI Sciences, 2024, pp. 1–28, doi:<a href=\"https://doi.org/10.46298/lmcs-20(4:1)2024\">10.46298/lmcs-20(4:1)2024</a>.","ista":"Bose S, Henzinger TA, Lehtinen K, Schewe S, Totzke P. 2024. History-deterministic timed automata. Logical Methods in Computer Science. 20(4), 1–28."},"page":"1-28","publication":"Logical Methods in Computer Science","corr_author":"1","ddc":["000"],"issue":"4","department":[{"_id":"ToHe"}],"date_updated":"2026-07-07T13:37:45Z","acknowledgement":"This work has in parts been presented at the 33rd International Conference on Concurrency Theory (CONCUR’22) [HLT22] and at the 16th International Workshop on Reachability Problems (RP’22) [BHL+22]. This work was supported by the EU (ERC-2020-AdG 101020093); the EPSRC (EP/V025848/1, EP/X042596/1, EP/X017796/1 and EP/X03688X/1); and the ANR (QUASY 23-CE48-0008-01).","publication_identifier":{"eissn":["1860-5974"]},"title":"History-deterministic timed automata","article_processing_charge":"No","quality_controlled":"1","language":[{"iso":"eng"}],"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","OA_type":"gold","date_published":"2024-10-02T00:00:00Z","volume":20,"oa":1,"year":"2024","DOAJ_listed":"1","arxiv":1,"abstract":[{"text":"We explore the notion of history-determinism in the context of timed automata (TA) over infinite timed words. History-deterministic (HD) automata are those in which nondeterminism can be resolved on the fly, based on the run constructed thus far. History-determinism is a robust property that admits different game-based characterisations, and HD specifications allow for game-based verification without an expensive determinization step. We show that the class of timed ω\r\n-languages recognized by HD timed automata strictly extends that of deterministic ones, and is strictly included in those recognised by fully non-deterministic TA. For non-deterministic timed automata it is known that universality is already undecidable for safety/reachability TA. For history-deterministic TA with arbitrary parity acceptance, we show that timed universality, inclusion, and synthesis all remain decidable and are EXPTIME-complete. For the subclass of TA with safety or reachability acceptance, one can decide (in EXPTIME) whether such an automaton is history-deterministic. If so, it can effectively determinized without introducing new automaton states.","lang":"eng"}],"publication_status":"published","article_type":"original","related_material":{"record":[{"relation":"earlier_version","id":"12508","status":"public"}]},"file_date_updated":"2024-11-11T08:32:02Z","day":"02","OA_place":"publisher","oa_version":"Published Version","external_id":{"isi":["001332466900002"],"arxiv":["2304.03183"]},"ec_funded":1,"has_accepted_license":"1","month":"10","project":[{"_id":"62781420-2b32-11ec-9570-8d9b63373d4d","call_identifier":"H2020","name":"Vigilant Algorithmic Monitoring of Software","grant_number":"101020093"}],"doi":"10.46298/lmcs-20(4:1)2024","author":[{"last_name":"Bose","first_name":"Sougata","full_name":"Bose, Sougata"},{"first_name":"Thomas A","last_name":"Henzinger","id":"40876CD8-F248-11E8-B48F-1D18A9856A87","full_name":"Henzinger, Thomas A","orcid":"0000-0002-2985-7724"},{"full_name":"Lehtinen, Karoliina","last_name":"Lehtinen","first_name":"Karoliina"},{"last_name":"Schewe","first_name":"Sven","full_name":"Schewe, Sven"},{"full_name":"Totzke, Patrick","first_name":"Patrick","last_name":"Totzke"}],"date_created":"2024-11-10T23:02:01Z","intvolume":"        20","type":"journal_article","file":[{"date_updated":"2024-11-11T08:32:02Z","file_name":"2024_LMCS_Bose.pdf","date_created":"2024-11-11T08:32:02Z","creator":"dernst","relation":"main_file","success":1,"checksum":"26826786a960039b9501cfc5cb4f3fe6","file_id":"18532","content_type":"application/pdf","access_level":"open_access","file_size":563394}],"publisher":"EPI Sciences","_id":"18530"},{"file":[{"relation":"main_file","success":1,"checksum":"247bb057aed2fba1cd4711917aaa2d77","file_id":"18686","content_type":"application/pdf","file_size":7752253,"access_level":"open_access","date_updated":"2024-12-19T10:24:46Z","creator":"theiss","file_name":"Teresa_Heiss_PhD_Thesis_final.pdf","date_created":"2024-12-19T10:24:46Z"},{"creator":"theiss","date_created":"2024-12-19T10:24:50Z","file_name":"PhD_Thesis.zip","date_updated":"2024-12-19T10:24:50Z","access_level":"closed","file_size":17197731,"content_type":"application/zip","file_id":"18687","relation":"source_file","checksum":"9648b45c07a008ee11a07f99856a139d"}],"supervisor":[{"id":"3FB178DA-F248-11E8-B48F-1D18A9856A87","full_name":"Edelsbrunner, Herbert","orcid":"0000-0002-9823-6833","first_name":"Herbert","last_name":"Edelsbrunner"}],"_id":"18667","publisher":"Institute of Science and Technology Austria","author":[{"last_name":"Heiss","first_name":"Teresa","orcid":"0000-0002-1780-2689","id":"4879BB4E-F248-11E8-B48F-1D18A9856A87","full_name":"Heiss, Teresa"}],"date_created":"2024-12-17T16:17:55Z","project":[{"grant_number":"788183","_id":"266A2E9E-B435-11E9-9278-68D0E5697425","name":"Alpha Shape Theory Extended","call_identifier":"H2020"}],"doi":"10.15479/at:ista:18667","type":"dissertation","ec_funded":1,"oa_version":"Published Version","OA_place":"publisher","day":"17","month":"12","has_accepted_license":"1","alternative_title":["ISTA Thesis"],"year":"2024","oa":1,"date_published":"2024-12-17T00:00:00Z","file_date_updated":"2024-12-19T10:24:50Z","related_material":{"record":[{"status":"public","id":"10828","relation":"part_of_dissertation"},{"id":"11440","status":"public","relation":"part_of_dissertation"},{"relation":"part_of_dissertation","id":"18673","status":"public"},{"status":"public","id":"9345","relation":"part_of_dissertation"}]},"publication_status":"published","abstract":[{"lang":"eng","text":"Many chemical and physical properties of materials are determined by the material’s shape,\r\nfor example the size of its pores and the width of its tunnels. This makes materials science\r\na prime application area for geometrical and topological methods. Nevertheless many\r\nmethods in topological data analysis have not been satisfyingly extended to the needs of\r\nmaterials science. This thesis provides new methods and new mathematical theorems\r\ntargeted at those specific needs by answering four different research questions. While the\r\nmotivation for each of the research questions arises from materials science, the methods\r\nare versatile and can be applied in different areas as well. \r\n\r\nThe first research question is concerned with image data, for example a three-dimensional\r\ncomputed tomography (CT) scan of a material, like sand or stone. There are two commonly\r\nused topologies for digital images and depending on the application either of them might be\r\nrequired. However, software for computing the topological data analysis method persistence\r\nhomology, usually supports only one of the two topologies. We answer the question how to\r\ncompute persistent homology of an image with respect to one of the two topologies using\r\nsoftware that is intended for the other topology. \r\n\r\nThe second research question is concerned with image data as well, and asks how much\r\nof the topological information of an image is lost when the resolution is coarsened. As\r\ncomputer tomography scanners are more expensive the higher the resolution, it is an\r\nimportant question in materials science to know which resolution is enough to get satisfying\r\npersistent homology. We give theoretical bounds on the information loss based on different\r\ngeometrical properties of the object to be scanned. In addition, we conduct experiments on\r\nsand and stone CT image data. \r\n\r\nThe third research question is motivated by comparing crystalline materials efficiently. As\r\nthe atoms within a crystal repeat periodically, crystalline materials are either modeled by\r\nunmanageable infinite periodic point sets, or by one of their fundamental domains, which is\r\nunstable under perturbation. Therefore a fingerprint of crystalline materials is needed, with\r\nappropriate properties such that comparing the crystals can be eased by comparing the\r\nfingerprints instead. We define the density fingerprint and prove the necessary properties. \r\n\r\nThe fourth research question is motivated by studying the hole-structure or connectedness,\r\ni.e. persistent homology or merge trees, of crystalline materials. A common way to deal\r\nwith periodicity is to take a fundamental domain and identify opposite boundaries to form a\r\ntorus. However, computing persistent homology or merge trees on that torus loses some\r\nof the information materials scientists are interested in and is additionally not stable under\r\ncertain noise. We therefore decorate the merge tree stemming from the torus with additional\r\ninformation describing the density and growth rate of the periodic copies of a component\r\nwithin a growing spherical window. We prove all desired properties, like stability and efficient\r\ncomputability."}],"user_id":"ba8df636-2132-11f1-aed0-ed93e2281fdd","language":[{"iso":"eng"}],"title":"New methods for applying topological data analysis to materials science","publication_identifier":{"isbn":["978-3-99078-052-7"],"issn":["2663-337X"]},"date_updated":"2026-07-07T13:43:27Z","acknowledgement":"I was supported by the European Research Council (ERC) Horizon 2020 project\r\n“Alpha Shape Theory Extended” No. 788183 and by the Pöttinger Scholarship. In addition,\r\nI am very thankful for having been able to attend the second Workshop for Women in\r\nComputational Topology in July 2019, funded by the Mathematical Sciences Institute at\r\nANU, the US National Science Foundation through the award CCF-1841455, the Australian\r\nMathematical Sciences Institute and the Association for Women in Mathematics. Two of the\r\nprojects presented in this thesis started there. One of them reached completion thanks to\r\nfunding from the MSRI Summer Research in Mathematics program awarded to me and my\r\ncollaborators in 2020.","article_processing_charge":"No","ddc":["514","516","004"],"corr_author":"1","department":[{"_id":"GradSch"},{"_id":"HeEd"}],"keyword":["persistent homology","topological data analysis","periodic","crystalline materials","images","fingerprint"],"status":"public","page":"111","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"citation":{"short":"T. Heiss, New Methods for Applying Topological Data Analysis to Materials Science, Institute of Science and Technology Austria, 2024.","ista":"Heiss T. 2024. New methods for applying topological data analysis to materials science. Institute of Science and Technology Austria.","mla":"Heiss, Teresa. <i>New Methods for Applying Topological Data Analysis to Materials Science</i>. Institute of Science and Technology Austria, 2024, doi:<a href=\"https://doi.org/10.15479/at:ista:18667\">10.15479/at:ista:18667</a>.","chicago":"Heiss, Teresa. “New Methods for Applying Topological Data Analysis to Materials Science.” Institute of Science and Technology Austria, 2024. <a href=\"https://doi.org/10.15479/at:ista:18667\">https://doi.org/10.15479/at:ista:18667</a>.","ieee":"T. Heiss, “New methods for applying topological data analysis to materials science,” Institute of Science and Technology Austria, 2024.","ama":"Heiss T. New methods for applying topological data analysis to materials science. 2024. doi:<a href=\"https://doi.org/10.15479/at:ista:18667\">10.15479/at:ista:18667</a>","apa":"Heiss, T. (2024). <i>New methods for applying topological data analysis to materials science</i>. Institute of Science and Technology Austria. <a href=\"https://doi.org/10.15479/at:ista:18667\">https://doi.org/10.15479/at:ista:18667</a>"},"degree_awarded":"PhD"},{"external_id":{"arxiv":["2106.01274"]},"oa_version":"Preprint","day":"01","month":"02","arxiv":1,"oa":1,"year":"2024","volume":60,"date_published":"2024-02-01T00:00:00Z","publication_status":"published","article_type":"original","abstract":[{"text":"In this paper we consider an SPDE where the leading term is a second order operator with periodic boundary conditions, coefficients which are measurable in  (t,ω) , and Hölder continuous in space. Assuming stochastic parabolicity conditions, we prove Lp((0,T)×Ω,tκdt;Hσ,q(Td)) -estimates. The main novelty is that we do not require  p=q . Moreover, we allow arbitrary  σ∈R  and weights in time. Such mixed regularity estimates play a crucial role in applications to nonlinear SPDEs which is clear from our previous work. To prove our main results we develop a general perturbation theory for SPDEs. Moreover, we prove a new result on pointwise multiplication in spaces with fractional smoothness.","lang":"eng"}],"_id":"15119","publisher":"Institute of Mathematical Statistics","main_file_link":[{"open_access":"1","url":"https://doi.org/10.48550/arXiv.2106.01274"}],"author":[{"last_name":"Agresti","first_name":"Antonio","orcid":"0000-0002-9573-2962","id":"673cd0cc-9b9a-11eb-b144-88f30e1fbb72","full_name":"Agresti, Antonio"},{"full_name":"Veraar, Mark","first_name":"Mark","last_name":"Veraar"}],"date_created":"2024-03-17T23:00:58Z","doi":"10.1214/22-AIHP1333","intvolume":"        60","type":"journal_article","issue":"1","corr_author":"1","department":[{"_id":"JuFi"}],"das_tickbox":"1","status":"public","publication":"Annales de l'Institut Henri Poincaré, Probabilités et Statistiques","page":"413-430","citation":{"apa":"Agresti, A., &#38; Veraar, M. (2024). Stochastic maximal Lp(Lq)-regularity for second order systems with periodic boundary conditions. <i>Annales de l’Institut Henri Poincaré, Probabilités et Statistiques</i>. Institute of Mathematical Statistics. <a href=\"https://doi.org/10.1214/22-AIHP1333\">https://doi.org/10.1214/22-AIHP1333</a>","ama":"Agresti A, Veraar M. Stochastic maximal Lp(Lq)-regularity for second order systems with periodic boundary conditions. <i>Annales de l’Institut Henri Poincaré, Probabilités et Statistiques</i>. 2024;60(1):413-430. doi:<a href=\"https://doi.org/10.1214/22-AIHP1333\">10.1214/22-AIHP1333</a>","ieee":"A. Agresti and M. Veraar, “Stochastic maximal Lp(Lq)-regularity for second order systems with periodic boundary conditions,” <i>Annales de l’Institut Henri Poincaré, Probabilités et Statistiques</i>, vol. 60, no. 1. Institute of Mathematical Statistics, pp. 413–430, 2024.","short":"A. Agresti, M. Veraar, Annales de l’Institut Henri Poincaré, Probabilités et Statistiques 60 (2024) 413–430.","chicago":"Agresti, Antonio, and Mark Veraar. “Stochastic Maximal Lp(Lq)-Regularity for Second Order Systems with Periodic Boundary Conditions.” <i>Annales de l’Institut Henri Poincaré, Probabilités et Statistiques</i>. Institute of Mathematical Statistics, 2024. <a href=\"https://doi.org/10.1214/22-AIHP1333\">https://doi.org/10.1214/22-AIHP1333</a>.","mla":"Agresti, Antonio, and Mark Veraar. “Stochastic Maximal Lp(Lq)-Regularity for Second Order Systems with Periodic Boundary Conditions.” <i>Annales de l’Institut Henri Poincaré, Probabilités et Statistiques</i>, vol. 60, no. 1, Institute of Mathematical Statistics, 2024, pp. 413–30, doi:<a href=\"https://doi.org/10.1214/22-AIHP1333\">10.1214/22-AIHP1333</a>.","ista":"Agresti A, Veraar M. 2024. Stochastic maximal Lp(Lq)-regularity for second order systems with periodic boundary conditions. Annales de l’Institut Henri Poincaré, Probabilités et Statistiques. 60(1), 413–430."},"scopus_import":"1","language":[{"iso":"eng"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","quality_controlled":"1","title":"Stochastic maximal Lp(Lq)-regularity for second order systems with periodic boundary conditions","publication_identifier":{"issn":["0246-0203"]},"date_updated":"2026-07-08T06:16:26Z","acknowledgement":"The first author has been partially supported by the Nachwuchsring – Network for the promotion of young scientists – at TU Kaiserslautern. The second author is supported by the VIDI subsidy 639.032.427 of the Netherlands Organisation for Scientific Research (NWO). The authors thank the anonymous referees and Max Sauerbrey for careful reading and helpful suggestions.","article_processing_charge":"No"},{"isi":1,"scopus_import":"1","citation":{"chicago":"Shenar, T., J. Bodensteiner, H. Sana, P. A. Crowther, D. J. Lennon, M. Abdul-Masih, L. A. Almeida, et al. “Binarity at LOw Metallicity (BLOeM): A Spectroscopic VLT Monitoring Survey of Massive Stars in the SMC.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2024. <a href=\"https://doi.org/10.1051/0004-6361/202451586\">https://doi.org/10.1051/0004-6361/202451586</a>.","ista":"Shenar T, Bodensteiner J, Sana H, Crowther PA, Lennon DJ, Abdul-Masih M, Almeida LA, Backs F, Berlanas SR, Bernini-Peron M, Bestenlehner JM, Bowman DM, Bronner VA, Britavskiy N, De Koter A, De Mink SE, Deshmukh K, Evans CJ, Fabry M, Gieles M, Gilkis A, González-Torà G, Gräfener G, Götberg YLL, Hawcroft C, Hénault-Brunet V, Herrero A, Holgado G, Janssens S, Johnston C, Josiek J, Justham S, Kalari VM, Katabi ZZ, Keszthelyi Z, Klencki J, Kubát J, Kubátová B, Langer N, Lefever RR, Ludwig B, Mackey J, Mahy L, Maíz Apellániz J, Mandel I, Maravelias G, Marchant P, Menon A, Najarro F, Oskinova LM, O’Grady AJG, Ovadia R, Patrick LR, Pauli D, Pawlak M, Ramachandran V, Renzo M, Rocha DF, Sander AAC, Sayada T, Schneider FRN, Schootemeijer A, Schösser EC, Schürmann C, Sen K, Shahaf S, Simón-Díaz S, Stoop M, Toonen S, Tramper F, Van Loon JT, Valli R, Van Son LAC, Vigna-Gómez A, Villaseñor JI, Vink JS, Wang C, Willcox R. 2024. Binarity at LOw Metallicity (BLOeM): A spectroscopic VLT monitoring survey of massive stars in the SMC. Astronomy &#38; Astrophysics. 690, A289.","mla":"Shenar, T., et al. “Binarity at LOw Metallicity (BLOeM): A Spectroscopic VLT Monitoring Survey of Massive Stars in the SMC.” <i>Astronomy &#38; Astrophysics</i>, vol. 690, A289, EDP Sciences, 2024, doi:<a href=\"https://doi.org/10.1051/0004-6361/202451586\">10.1051/0004-6361/202451586</a>.","short":"T. Shenar, J. Bodensteiner, H. Sana, P.A. Crowther, D.J. Lennon, M. Abdul-Masih, L.A. Almeida, F. Backs, S.R. Berlanas, M. Bernini-Peron, J.M. Bestenlehner, D.M. Bowman, V.A. Bronner, N. Britavskiy, A. De Koter, S.E. De Mink, K. Deshmukh, C.J. Evans, M. Fabry, M. Gieles, A. Gilkis, G. González-Torà, G. Gräfener, Y.L.L. Götberg, C. Hawcroft, V. Hénault-Brunet, A. Herrero, G. Holgado, S. Janssens, C. Johnston, J. Josiek, S. Justham, V.M. Kalari, Z.Z. Katabi, Z. Keszthelyi, J. Klencki, J. Kubát, B. Kubátová, N. Langer, R.R. Lefever, B. Ludwig, J. Mackey, L. Mahy, J. Maíz Apellániz, I. Mandel, G. Maravelias, P. Marchant, A. Menon, F. Najarro, L.M. Oskinova, A.J.G. O’Grady, R. Ovadia, L.R. Patrick, D. Pauli, M. Pawlak, V. Ramachandran, M. Renzo, D.F. Rocha, A.A.C. Sander, T. Sayada, F.R.N. Schneider, A. Schootemeijer, E.C. Schösser, C. Schürmann, K. Sen, S. Shahaf, S. Simón-Díaz, M. Stoop, S. Toonen, F. Tramper, J.T. Van Loon, R. Valli, L.A.C. Van Son, A. Vigna-Gómez, J.I. Villaseñor, J.S. Vink, C. Wang, R. Willcox, Astronomy &#38; Astrophysics 690 (2024).","ama":"Shenar T, Bodensteiner J, Sana H, et al. Binarity at LOw Metallicity (BLOeM): A spectroscopic VLT monitoring survey of massive stars in the SMC. <i>Astronomy &#38; Astrophysics</i>. 2024;690. doi:<a href=\"https://doi.org/10.1051/0004-6361/202451586\">10.1051/0004-6361/202451586</a>","apa":"Shenar, T., Bodensteiner, J., Sana, H., Crowther, P. A., Lennon, D. J., Abdul-Masih, M., … Willcox, R. (2024). Binarity at LOw Metallicity (BLOeM): A spectroscopic VLT monitoring survey of massive stars in the SMC. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202451586\">https://doi.org/10.1051/0004-6361/202451586</a>","ieee":"T. Shenar <i>et al.</i>, “Binarity at LOw Metallicity (BLOeM): A spectroscopic VLT monitoring survey of massive stars in the SMC,” <i>Astronomy &#38; Astrophysics</i>, vol. 690. EDP Sciences, 2024."},"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"publication":"Astronomy & Astrophysics","status":"public","das_tickbox":"1","department":[{"_id":"YlGo"}],"ddc":["520"],"article_number":"A289","article_processing_charge":"Yes (in subscription journal)","date_updated":"2026-07-08T06:44:06Z","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 programme (grant agreement numbers 772225: MULTIPLES). PAC and JMB are supported by the Science and Technology Facilities Council research grant ST/V000853/1 (PI. V. Dhillon). DMB gratefully acknowledges support from UK Research and Innovation (UKRI) in the form of a Frontier Research grant under the UK government’s ERC Horizon Europe funding guarantee (SYMPHONY; PI Bowman; grant number: EP/Y031059/1), and a Royal Society University Research Fellowship (PI Bowman; grant number: URF\\R1\\231631). ZK acknowledges support from JSPS Kakenhi Grant-in-Aid for Scientific Research (23K19071). IM acknowledges support from the Australian Research Council (ARC) Centre of Excellence for Gravitational Wave Discovery (OzGrav), through project number CE230100016. AACS, VR, RRL, and MBP are funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) in the form of an Emmy Noether Research Group – Project-ID 445674056 (SA4064/1-1, PI Sander). GGT and JJ are supported by the German Deutsche Forschungsgemeinschaft (DFG) under Project-ID 496854903 (SA4064/2-1, PI Sander) VR, GGT, and AACS further acknowledge support from the Federal Ministry of Education and Research (BMBF) and the Baden-Württemberg Ministry of Science as part of the Excellence Strategy of the German Federal and State Governments. ECS acknowledges financial support by the Federal Ministry for Economic Affairs and Climate Action (BMWK) via the German Aerospace Center (Deutsches Zentrum für Luft- und Raumfahrt, DLR) grant 50 OR 2306 (PI: Ramachandran/Sander). This work has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (Grant agreement No. 945806) and is supported by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany’s Excellence Strategy EXC 2181/1-390900948 (the Heidelberg STRUCTURES Excellence Cluster). LMO is thankful for the funding provided by the DFG grant 443790621. This paper benefited from discussions at the International Space Science Institute (ISSI) in Bern through ISSI International Team project 512 (Multiwavelength View on Massive Stars in the Era of Multimessenger Astronomy). DP acknowledges financial support by the Deutsches Zentrum für Luft und Raumfahrt (DLR) grant FKZ 50OR2005. JIV acknowledges the European Research Council for support from the ERC Advanced grant ERC-2021-ADG101054731. JSV is supported by STFC (Science and Technology Facilities Council) funding under grant number ST/V000233/1. GH, SS-D, SRB and AH acknowledge support from the State Research Agency (AEI) of the Spanish Ministry of Science and Innovation (MICIN) and the European Regional Development Fund, FEDER under grants PID2021-122397NB-C21 and CEX2019-000920-S. SRB also acknowledges financial support by NextGeneration EU/PRTR and MIU (UNI/551/2021) through grant Margarita Salas-ULL. DFR is thankful for the support of the CAPES-Br and FAPERJ/DSC-10 (SEI-260003/001630/2023). F.N., and L.R.P. acknowledge support by grants PID2019-105552RB-C41 and PID2022-137779OB-C41 funded by MCIN/AEI/10.13039/501100011033 by “ERDF A way of making Europe”. MG acknowledges financial support from the grants PID2021-125485NB-C22, CEX2019-000918-M funded by MCIN/AEI/10.13039/501100011033 (State Agency for Research of the Spanish Ministry of Science and Innovation) and SGR-2021-01069 (AGAUR). GM acknowledges funding support from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (Grant agreement No. 772086). JMA acknowledges support from the Spanish Government Ministerio de Ciencia e Innovación and Agencia Estatal de Investigación (10.13 039/501 100 011 033) through grant PID2022-136640 NB-C22 and from the Consejo Superior de Investigaciones Científicas (CSIC) through grant 2022-AEP 005. MP is supported by the BEKKER fellowship BPN/BEK/2022/1/00106 from the Polish National Agency for Academic Exchange. KS is funded by the National Science Center (NCN), Poland, under grant number OPUS 2021/41/B/ST9/00757. JM acknowledges support from a Royal Society-Science Foundation Ireland University Research Fellowship. SJ acknowledges support from the FWO PhD fellowship under project 11E1721N. FB acknowledges the support of the European Research Council (ERC) Horizon Europe under grant agreement number 101044048.","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"title":"Binarity at LOw Metallicity (BLOeM): A spectroscopic VLT monitoring survey of massive stars in the SMC","OA_type":"hybrid","quality_controlled":"1","language":[{"iso":"eng"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","abstract":[{"text":"Surveys in the Milky Way and Large Magellanic Cloud have revealed that the majority of massive stars will interact with companions during their lives. However, knowledge of the binary properties of massive stars at low metallicity, and therefore in conditions approaching those of the Early Universe, remain sparse. We present the Binarity at LOw Metallicity (BLOeM) campaign, an ESO large programme designed to obtain 25 epochs of spectroscopy for 929 massive stars in the Small Magellanic Cloud, allowing us to probe multiplicity in the lowest-metallicity conditions to date (Z = 0.2 Z⊙). BLOeM will provide (i) the binary fraction, (ii) the orbital configurations of systems with periods of P ≲ 3 yr, (iii) dormant black-hole binary candidates (OB+BH), and (iv) a legacy database of physical parameters of massive stars at low metallicity. Main sequence (OB-type) and evolved (OBAF-type) massive stars are observed with the LR02 setup of the GIRAFFE instrument of the Very Large Telescope (3960–4570 Å resolving power R = 6200; typical signal-to-noise ratio(S/N) ≈70–100). This paper utilises the first nine epochs obtained over a three-month time period. We describe the survey and data reduction, perform a spectral classification of the stacked spectra, and construct a Hertzsprung-Russell diagram of the sample via spectral-type and photometric calibrations. Our detailed classification reveals that the sample covers spectral types from O4 to F5, spanning the effective temperature and luminosity ranges 6.5 ≲ Teff/kK ≲ 45 and 3.7 < log L/L⊙ < 6.1 and initial masses of 8 ≲ Mini ≲ 80 M⊙. The sample comprises 159 O-type stars, 331 early B-type (B0–3) dwarfs and giants (luminosity classes V–III), 303 early B-type supergiants (II–I), and 136 late-type BAF supergiants. At least 82 stars are OBe stars: 20 O-type and 62 B-type (13% and 11% of the respective samples). In addition, the sample includes 4 high-mass X-ray binaries, 3 stars resembling luminous blue variables, 2 bloated stripped-star candidates, 2 candidate magnetic stars, and 74 eclipsing binaries.","lang":"eng"}],"publication_status":"published","article_type":"original","file_date_updated":"2024-11-04T09:52:26Z","date_published":"2024-10-01T00:00:00Z","volume":690,"oa":1,"year":"2024","arxiv":1,"has_accepted_license":"1","month":"10","day":"01","OA_place":"publisher","oa_version":"Published Version","external_id":{"arxiv":["2407.14593"],"isi":["001336770600014"]},"intvolume":"       690","type":"journal_article","doi":"10.1051/0004-6361/202451586","author":[{"first_name":"T.","last_name":"Shenar","full_name":"Shenar, T."},{"full_name":"Bodensteiner, J.","last_name":"Bodensteiner","first_name":"J."},{"first_name":"H.","last_name":"Sana","full_name":"Sana, H."},{"full_name":"Crowther, P. A.","last_name":"Crowther","first_name":"P. A."},{"full_name":"Lennon, D. J.","first_name":"D. J.","last_name":"Lennon"},{"first_name":"M.","last_name":"Abdul-Masih","full_name":"Abdul-Masih, M."},{"full_name":"Almeida, L. A.","last_name":"Almeida","first_name":"L. A."},{"last_name":"Backs","first_name":"F.","full_name":"Backs, F."},{"full_name":"Berlanas, S. R.","last_name":"Berlanas","first_name":"S. R."},{"full_name":"Bernini-Peron, M.","first_name":"M.","last_name":"Bernini-Peron"},{"first_name":"J. M.","last_name":"Bestenlehner","full_name":"Bestenlehner, J. M."},{"last_name":"Bowman","first_name":"D. M.","full_name":"Bowman, D. M."},{"full_name":"Bronner, V. A.","last_name":"Bronner","first_name":"V. A."},{"last_name":"Britavskiy","first_name":"N.","full_name":"Britavskiy, N."},{"last_name":"De Koter","first_name":"A.","full_name":"De Koter, A."},{"full_name":"De Mink, S. E.","first_name":"S. E.","last_name":"De Mink"},{"full_name":"Deshmukh, K.","first_name":"K.","last_name":"Deshmukh"},{"last_name":"Evans","first_name":"C. J.","full_name":"Evans, C. J."},{"full_name":"Fabry, M.","first_name":"M.","last_name":"Fabry"},{"first_name":"M.","last_name":"Gieles","full_name":"Gieles, M."},{"first_name":"A.","last_name":"Gilkis","full_name":"Gilkis, A."},{"first_name":"G.","last_name":"González-Torà","full_name":"González-Torà, G."},{"first_name":"G.","last_name":"Gräfener","full_name":"Gräfener, G."},{"orcid":"0000-0002-6960-6911","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","full_name":"Götberg, Ylva Louise Linsdotter","last_name":"Götberg","first_name":"Ylva Louise Linsdotter"},{"full_name":"Hawcroft, C.","last_name":"Hawcroft","first_name":"C."},{"last_name":"Hénault-Brunet","first_name":"V.","full_name":"Hénault-Brunet, V."},{"last_name":"Herrero","first_name":"A.","full_name":"Herrero, A."},{"full_name":"Holgado, G.","first_name":"G.","last_name":"Holgado"},{"full_name":"Janssens, S.","first_name":"S.","last_name":"Janssens"},{"last_name":"Johnston","first_name":"C.","full_name":"Johnston, C."},{"first_name":"J.","last_name":"Josiek","full_name":"Josiek, J."},{"full_name":"Justham, S.","first_name":"S.","last_name":"Justham"},{"first_name":"V. M.","last_name":"Kalari","full_name":"Kalari, V. M."},{"last_name":"Katabi","first_name":"Z. Z.","full_name":"Katabi, Z. Z."},{"full_name":"Keszthelyi, Z.","first_name":"Z.","last_name":"Keszthelyi"},{"last_name":"Klencki","first_name":"J.","full_name":"Klencki, J."},{"full_name":"Kubát, J.","first_name":"J.","last_name":"Kubát"},{"full_name":"Kubátová, B.","first_name":"B.","last_name":"Kubátová"},{"full_name":"Langer, N.","first_name":"N.","last_name":"Langer"},{"full_name":"Lefever, R. R.","last_name":"Lefever","first_name":"R. R."},{"full_name":"Ludwig, B.","last_name":"Ludwig","first_name":"B."},{"full_name":"Mackey, J.","last_name":"Mackey","first_name":"J."},{"first_name":"L.","last_name":"Mahy","full_name":"Mahy, L."},{"full_name":"Maíz Apellániz, J.","last_name":"Maíz Apellániz","first_name":"J."},{"full_name":"Mandel, I.","first_name":"I.","last_name":"Mandel"},{"first_name":"G.","last_name":"Maravelias","full_name":"Maravelias, G."},{"full_name":"Marchant, P.","last_name":"Marchant","first_name":"P."},{"last_name":"Menon","first_name":"A.","full_name":"Menon, A."},{"full_name":"Najarro, F.","last_name":"Najarro","first_name":"F."},{"first_name":"L. M.","last_name":"Oskinova","full_name":"Oskinova, L. M."},{"first_name":"A. J.G.","last_name":"O'Grady","full_name":"O'Grady, A. J.G."},{"full_name":"Ovadia, R.","first_name":"R.","last_name":"Ovadia"},{"last_name":"Patrick","first_name":"L. R.","full_name":"Patrick, L. R."},{"first_name":"D.","last_name":"Pauli","full_name":"Pauli, D."},{"last_name":"Pawlak","first_name":"M.","full_name":"Pawlak, M."},{"full_name":"Ramachandran, V.","first_name":"V.","last_name":"Ramachandran"},{"full_name":"Renzo, M.","first_name":"M.","last_name":"Renzo"},{"last_name":"Rocha","first_name":"D. F.","full_name":"Rocha, D. F."},{"full_name":"Sander, A. A.C.","first_name":"A. A.C.","last_name":"Sander"},{"full_name":"Sayada, T.","last_name":"Sayada","first_name":"T."},{"last_name":"Schneider","first_name":"F. R.N.","full_name":"Schneider, F. R.N."},{"first_name":"A.","last_name":"Schootemeijer","full_name":"Schootemeijer, A."},{"last_name":"Schösser","first_name":"E. C.","full_name":"Schösser, E. C."},{"last_name":"Schürmann","first_name":"C.","full_name":"Schürmann, C."},{"first_name":"K.","last_name":"Sen","full_name":"Sen, K."},{"last_name":"Shahaf","first_name":"S.","full_name":"Shahaf, S."},{"full_name":"Simón-Díaz, S.","first_name":"S.","last_name":"Simón-Díaz"},{"full_name":"Stoop, M.","last_name":"Stoop","first_name":"M."},{"full_name":"Toonen, S.","first_name":"S.","last_name":"Toonen"},{"last_name":"Tramper","first_name":"F.","full_name":"Tramper, F."},{"full_name":"Van Loon, J. Th","last_name":"Van Loon","first_name":"J. Th"},{"last_name":"Valli","first_name":"R.","full_name":"Valli, R."},{"first_name":"L. A.C.","last_name":"Van Son","full_name":"Van Son, L. A.C."},{"full_name":"Vigna-Gómez, A.","last_name":"Vigna-Gómez","first_name":"A."},{"last_name":"Villaseñor","first_name":"J. I.","full_name":"Villaseñor, J. I."},{"first_name":"J. S.","last_name":"Vink","full_name":"Vink, J. S."},{"full_name":"Wang, C.","last_name":"Wang","first_name":"C."},{"full_name":"Willcox, R.","last_name":"Willcox","first_name":"R."}],"date_created":"2024-11-03T23:01:44Z","publisher":"EDP Sciences","_id":"18492","file":[{"access_level":"open_access","file_size":4267349,"content_type":"application/pdf","file_id":"18500","success":1,"checksum":"b378b36726591f3479a927d924ab8e77","relation":"main_file","creator":"dernst","date_created":"2024-11-04T09:52:26Z","file_name":"2024_AstronomyAstrophysics_Shenar.pdf","date_updated":"2024-11-04T09:52:26Z"}]},{"abstract":[{"text":"Aims. This paper utilises the James Webb Space Telescope (JWST) Mid-Infrared Instrument (MIRI) to extend the observational studies of dust and polycyclic aromatic hydrocarbon (PAH) emission to a new mass and star formation rate (SFR) parameter space beyond our local Universe. The combination of fully sampled spectral energy distributions (SEDs) with multiple mid-infrared (mid-IR) bands and the unprecedented sensitivity of MIRI allows us to investigate dust obscuration and PAH behaviour from z = 0.7 up to z = 2 in typical main-sequence galaxies. Our focus is on constraining the evolution of PAH strength and the dust-obscured luminosity fraction before and during cosmic noon, the epoch of peak star formation activity in the Universe.\r\n\r\nMethods. In this study, we utilise MIRI multi-band imaging data from the SMILES survey (5 to 25 μm), complemented with NIRCam photometry from the JADES survey (1 to 5 μm), available HST photometry (0.4 to 0.9 μm), and spectroscopic redshifts from the FRESCO and JADES surveys in GOODS-S for 443 star-forming (without dominant active galactic nucleus (AGN)) galaxies at z = 0.7 − 2.0. This redshift range was chosen to ensure that the MIRI data cover mid-IR dust emission. Our methodology involved employing ultraviolet (UV) to IR energy balance SED fitting to robustly constrain the fraction of dust mass in PAHs and dust-obscured luminosity. Additionally, we inferred dust sizes from MIRI 15 μm imaging data, enhancing our understanding of the physical characteristics of dust within these galaxies.\r\n\r\nResults. We find a strong correlation between the fraction of dust in PAHs (PAH fraction, qPAH) with stellar mass. Moreover, the sub-sample with robust qPAH measurements (N = 216) shows a similar behaviour between qPAH and gas-phase metallicity to that at z ∼ 0, suggesting a universal relation: qPAH is constant (∼3.4%) above a metallicity of Z ∼ 0.5 Z⊙ and decreases to < 1% at metallicities ≲0.3 Z⊙. This indicates that metallicity is a good indicator of the interstellar medium properties that affect the balance between the formation and destruction of PAHs. The lack of a redshift evolution from z ∼ 0 − 2 also implies that above Z ∼ 0.5 Z⊙ the PAH emission effectively traces obscured luminosity and the previous locally calibrated PAH-SFR calibrations remain applicable in this metallicity regime. We observe a strong correlation between the obscured UV luminosity fraction (ratio of obscured to total luminosity) and stellar mass. Above the stellar mass of M* > 5 × 109 M⊙, on average, more than half of the emitted luminosity is obscured, while there exists a non-negligible population of lower-mass galaxies with > 50% obscured fractions. At a fixed mass, the obscured fraction correlates with SFR surface density. This is a result of higher dust covering fractions in galaxies with more compact star-forming regions. Similarly, galaxies with high IRX (IR to UV luminosity) at a given mass or UV continuum slope (β) tend to have higher ΣSFR and shallower attenuation curves, owing to their higher effective dust optical depths and more compact star-forming regions.","lang":"eng"}],"publication_status":"published","article_type":"original","file_date_updated":"2024-10-21T11:52:29Z","date_published":"2024-10-01T00:00:00Z","volume":690,"oa":1,"year":"2024","arxiv":1,"has_accepted_license":"1","month":"10","day":"01","OA_place":"publisher","oa_version":"Published Version","external_id":{"isi":["001381135700006"],"arxiv":["2402.07989"]},"intvolume":"       690","type":"journal_article","doi":"10.1051/0004-6361/202449579","author":[{"last_name":"Shivaei","first_name":"Irene","full_name":"Shivaei, Irene"},{"last_name":"Alberts","first_name":"Stacey","full_name":"Alberts, Stacey"},{"last_name":"Florian","first_name":"Michael","full_name":"Florian, Michael"},{"last_name":"Rieke","first_name":"George","full_name":"Rieke, George"},{"last_name":"Wuyts","first_name":"Stijn","full_name":"Wuyts, Stijn"},{"full_name":"Bodansky, Sarah","first_name":"Sarah","last_name":"Bodansky"},{"full_name":"Bunker, Andrew J.","last_name":"Bunker","first_name":"Andrew J."},{"last_name":"Cameron","first_name":"Alex J.","full_name":"Cameron, Alex J."},{"last_name":"Curti","first_name":"Mirko","full_name":"Curti, Mirko"},{"first_name":"Francesco","last_name":"Da'Eugenio","full_name":"Da'Eugenio, Francesco"},{"full_name":"Dudzevičiūte, Ugne","first_name":"Ugne","last_name":"Dudzevičiūte"},{"full_name":"Ji, Zhiyuan","last_name":"Ji","first_name":"Zhiyuan"},{"first_name":"Benjamin D.","last_name":"Johnson","full_name":"Johnson, Benjamin D."},{"orcid":"0000-0001-5346-6048","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","full_name":"Kramarenko, Ivan","last_name":"Kramarenko","first_name":"Ivan"},{"full_name":"Lyu, Jianwei","last_name":"Lyu","first_name":"Jianwei"},{"first_name":"Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X"},{"first_name":"Jane","last_name":"Morrison","full_name":"Morrison, Jane"},{"full_name":"Naidu, Rohan","last_name":"Naidu","first_name":"Rohan"},{"first_name":"Pablo G.","last_name":"Pérez-González","full_name":"Pérez-González, Pablo G."},{"first_name":"Naveen","last_name":"Reddy","full_name":"Reddy, Naveen"},{"full_name":"Robertson, Brant","first_name":"Brant","last_name":"Robertson"},{"last_name":"Sun","first_name":"Yang","full_name":"Sun, Yang"},{"full_name":"Tacchella, Sandro","first_name":"Sandro","last_name":"Tacchella"},{"last_name":"Whitaker","first_name":"Katherine","full_name":"Whitaker, Katherine"},{"full_name":"Williams, Christina C.","first_name":"Christina C.","last_name":"Williams"},{"first_name":"Christopher N.A.","last_name":"Willmer","full_name":"Willmer, Christopher N.A."},{"last_name":"Witstok","first_name":"Joris","full_name":"Witstok, Joris"},{"first_name":"Mengyuan","last_name":"Xiao","full_name":"Xiao, Mengyuan"},{"full_name":"Zhu, Yongda","first_name":"Yongda","last_name":"Zhu"}],"date_created":"2024-10-20T22:02:06Z","publisher":"EDP Sciences","_id":"18448","file":[{"checksum":"f399be98968b9ca5611c832a9b1eee2b","relation":"main_file","success":1,"file_id":"18458","content_type":"application/pdf","access_level":"open_access","file_size":10777358,"date_updated":"2024-10-21T11:52:29Z","creator":"dernst","file_name":"2024_AstronomyAstrophysics_Shivaei.pdf","date_created":"2024-10-21T11:52:29Z"}],"isi":1,"scopus_import":"1","citation":{"ama":"Shivaei I, Alberts S, Florian M, et al. A new census of dust and polycyclic aromatic hydrocarbons at z = 0.7-2 with JWST MIRI. <i>Astronomy &#38; Astrophysics</i>. 2024;690. doi:<a href=\"https://doi.org/10.1051/0004-6361/202449579\">10.1051/0004-6361/202449579</a>","apa":"Shivaei, I., Alberts, S., Florian, M., Rieke, G., Wuyts, S., Bodansky, S., … Zhu, Y. (2024). A new census of dust and polycyclic aromatic hydrocarbons at z = 0.7-2 with JWST MIRI. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202449579\">https://doi.org/10.1051/0004-6361/202449579</a>","ieee":"I. Shivaei <i>et al.</i>, “A new census of dust and polycyclic aromatic hydrocarbons at z = 0.7-2 with JWST MIRI,” <i>Astronomy &#38; Astrophysics</i>, vol. 690. EDP Sciences, 2024.","chicago":"Shivaei, Irene, Stacey Alberts, Michael Florian, George Rieke, Stijn Wuyts, Sarah Bodansky, Andrew J. Bunker, et al. “A New Census of Dust and Polycyclic Aromatic Hydrocarbons at z = 0.7-2 with JWST MIRI.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2024. <a href=\"https://doi.org/10.1051/0004-6361/202449579\">https://doi.org/10.1051/0004-6361/202449579</a>.","mla":"Shivaei, Irene, et al. “A New Census of Dust and Polycyclic Aromatic Hydrocarbons at z = 0.7-2 with JWST MIRI.” <i>Astronomy &#38; Astrophysics</i>, vol. 690, A89, EDP Sciences, 2024, doi:<a href=\"https://doi.org/10.1051/0004-6361/202449579\">10.1051/0004-6361/202449579</a>.","ista":"Shivaei I, Alberts S, Florian M, Rieke G, Wuyts S, Bodansky S, Bunker AJ, Cameron AJ, Curti M, Da’Eugenio F, Dudzevičiūte U, Ji Z, Johnson BD, Kramarenko I, Lyu J, Matthee JJ, Morrison J, Naidu R, Pérez-González PG, Reddy N, Robertson B, Sun Y, Tacchella S, Whitaker K, Williams CC, Willmer CNA, Witstok J, Xiao M, Zhu Y. 2024. A new census of dust and polycyclic aromatic hydrocarbons at z = 0.7-2 with JWST MIRI. Astronomy &#38; Astrophysics. 690, A89.","short":"I. Shivaei, S. Alberts, M. Florian, G. Rieke, S. Wuyts, S. Bodansky, A.J. Bunker, A.J. Cameron, M. Curti, F. Da’Eugenio, U. Dudzevičiūte, Z. Ji, B.D. Johnson, I. Kramarenko, J. Lyu, J.J. Matthee, J. Morrison, R. Naidu, P.G. Pérez-González, N. Reddy, B. Robertson, Y. Sun, S. Tacchella, K. Whitaker, C.C. Williams, C.N.A. Willmer, J. Witstok, M. Xiao, Y. Zhu, Astronomy &#38; Astrophysics 690 (2024)."},"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"publication":"Astronomy & Astrophysics","status":"public","das_tickbox":"1","department":[{"_id":"JoMa"}],"ddc":["520"],"article_number":"A89","article_processing_charge":"Yes (in subscription journal)","acknowledgement":"IS thanks the members of the JWST/MIRI instrument team for their exceptional efforts and for providing an outstanding experience during the commissioning period of JWST, which fostered numerous fruitful discussions and significantly enhanced the quality of data reduction in this study. IS also thanks Karin Sandstrom and Joel Leja for their insightful discussions during the scientific development of this work. Additionally, IS acknowledges the contribution of Andras Gáspar to the construction of the F560W PSF utilised in this research. This work was supported in part by NASA grant NNX13AD82G. Part of this research has been funded by Atraccíon de Talento Grant No. 2022-T1/TIC-20472 of the Comunidad de Madrid, Spain. AJB and AC acknowledges funding from the ‘FirstGalaxies’ Advanced Grant from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (Grant agreement No. 789056). The work of CCW is supported by NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. PGP-G acknowledges support from grant PID2022-139567NB-I00 funded by Spanish Ministerio de Ciencia e Innovación CIN/AEI/10.13039/501100011033, FEDER Una manera de hacer Europa. SA acknowledges support from the JWST Mid-Infrared Instrument (MIRI) Science Team Lead, grant 80NSSC18K0555, from NASA Goddard Space Flight Center to the University of Arizona. This work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with program PID 1207, 1080, 1081, 1895, 1220, 1286, 1287, 1963. Based on observations made with the NASA/ESA Hubble Space Telescope, 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/ESAC/ESA) and the Canadian Astronomy Data Centre (CADC/NRC/CSA).","date_updated":"2026-07-08T06:43:45Z","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"title":"A new census of dust and polycyclic aromatic hydrocarbons at z = 0.7-2 with JWST MIRI","OA_type":"hybrid","quality_controlled":"1","language":[{"iso":"eng"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87"},{"doi":"10.1051/0004-6361/202450318","author":[{"full_name":"Torralba-Torregrosa, Alberto","first_name":"Alberto","last_name":"Torralba-Torregrosa"},{"first_name":"Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X"},{"full_name":"Naidu, Rohan P.","last_name":"Naidu","first_name":"Rohan P."},{"first_name":"Ruari","last_name":"Mackenzie","full_name":"Mackenzie, Ruari"},{"full_name":"Pezzulli, Gabriele","last_name":"Pezzulli","first_name":"Gabriele"},{"last_name":"Hutter","first_name":"Anne","full_name":"Hutter, Anne"},{"last_name":"Arnalte-Mur","first_name":"Pablo","full_name":"Arnalte-Mur, Pablo"},{"full_name":"Gurung-López, Siddhartha","first_name":"Siddhartha","last_name":"Gurung-López"},{"full_name":"Tacchella, Sandro","first_name":"Sandro","last_name":"Tacchella"},{"first_name":"Pascal","last_name":"Oesch","full_name":"Oesch, Pascal"},{"full_name":"Kashino, Daichi","last_name":"Kashino","first_name":"Daichi"},{"full_name":"Conroy, Charlie","first_name":"Charlie","last_name":"Conroy"},{"first_name":"David","last_name":"Sobral","full_name":"Sobral, David"}],"date_created":"2024-09-08T22:01:11Z","type":"journal_article","intvolume":"       689","file":[{"content_type":"application/pdf","file_size":6225413,"access_level":"open_access","relation":"main_file","success":1,"checksum":"a6c0df287c75e8929db9f42badeac859","file_id":"18055","date_updated":"2024-09-11T07:35:00Z","creator":"dernst","date_created":"2024-09-11T07:35:00Z","file_name":"2024_AstronomyAstrophysics_TorralbaTorregrosa.pdf"}],"publisher":"EDP Sciences","_id":"17889","date_published":"2024-09-01T00:00:00Z","volume":689,"year":"2024","oa":1,"arxiv":1,"abstract":[{"text":"The increasingly neutral intergalactic gas at z > 6 impacts the Lyman-α (Lyα) flux observed from galaxies. One luminous galaxy, COLA1, stands out because of its unique double-peaked Lyα line at z = 6.6, unseen in any simulation of reionization. Here, we present JWST/NIRCam wide-field slitless spectroscopy in a 21 arcmin2 field centered on COLA1. We find 141 galaxies spectroscopically selected through the [O III] doublet at 5.35 < z < 6.95, with 40 of these sources showing Hβ. For COLA1, we additionally detect [O III]4363 as well as Hγ. We measure a systemic redshift of z = 6.5917 for COLA1, confirming the classical double-peak nature of the Lyα profile. This implies that it resides in a highly ionized bubble and that it is leaking ionizing photons with a high escape fraction of fesc(LyC) = 20–50%, making it a prime laboratory to study Lyman continuum escape in the Epoch of Reionization. COLA1 shows all the signs of a prolific ionizer with a Lyα escape fraction of 81 ± 5%, Balmer decrement indicating no dust, a steep UV slope (βUV = −3.2 ± 0.4), and a star-formation surface density ≳10× that of typical galaxies at similar redshift. We detect five galaxies in COLA1’s close environment (Δz < 0.02). Exploiting the high spectroscopic completeness inherent to grism surveys, and using mock simulations that fully mimic the selection function, we show that the number of detected companions is very typical for a normal similarly UV-bright (MUV ∼ −21.3) galaxy – that is, the ionized bubble around COLA1 is unlikely to be due to an excessively large over-density. Instead, the measured ionizing properties suggest that COLA1 by itself might be powering the bubble required to explain its double-peaked Lyα profile (Rion ≈ 0.7 pMpc), with only minor contributions from detected neighbors (−19.5 ≲ MUV ≲ −17.5).","lang":"eng"}],"article_type":"original","publication_status":"published","file_date_updated":"2024-09-11T07:35:00Z","day":"01","oa_version":"Published Version","external_id":{"isi":["001303205700016"],"arxiv":["2404.10040"]},"has_accepted_license":"1","month":"09","acknowledgement":"The authors acknowledge the financial support from the MICIU with funding from the European Union NextGenerationEU and Generalitat Valenciana in the call Programa de Planes Complementarios de I+D+i (PRTR 2022) Project (VAL-JPAS), reference ASFAE/2022/025. This work has been funded by project PID2019-109592GBI00/AEI/10.13039/501100011033 from the Spanish Ministerio de Ciencia e Innovación (MCIN)-Agencia Estatal de Investigación, by the Project of Excellence Prometeo/2020/085 from the Conselleria d’Innovació Universitats, Ciència i Societat Digital de la Generalitat Valenciana. It has also be funded by the Project of Excellence Prometeo/2020/085 from the Conselleria d’Educació, Universitats, i Ocupació de la Generalitat Valenciana. Funded by the European Union (ERC, AGENTS, 101076224). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. ST acknowledges support by the Royal Society Research Grant G125142. AH acknowledges support by the VILLUM FONDEN under grant 37459. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant DNRF140. We acknowledge funding from JWST program GO-1933. Support for this work was provided by NASA through the NASA Hubble Fellowship grant HST-HF2-51515.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. This work has received funding from the Swiss State Secretariat for Education, Research and Innovation (SERI) under contract number MB22.00072, as well as from the Swiss National Science Foundation (SNSF) through project grant 200020_207349. This work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with program # 1933. The specific observations analyzed can be accessed via https://doi.org/10.17909/s9ht-7n34.","date_updated":"2026-07-08T06:45:34Z","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"title":"Anatomy of an ionized bubble: NIRCam grism spectroscopy of the z = 6.6 double-peaked Lyman- α emitter COLA1 and its environment","article_number":"A44","article_processing_charge":"Yes (in subscription journal)","quality_controlled":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"status":"public","das_tickbox":"1","isi":1,"scopus_import":"1","citation":{"short":"A. Torralba-Torregrosa, J.J. Matthee, R.P. Naidu, R. Mackenzie, G. Pezzulli, A. Hutter, P. Arnalte-Mur, S. Gurung-López, S. Tacchella, P. Oesch, D. Kashino, C. Conroy, D. Sobral, Astronomy &#38; Astrophysics 689 (2024).","ista":"Torralba-Torregrosa A, Matthee JJ, Naidu RP, Mackenzie R, Pezzulli G, Hutter A, Arnalte-Mur P, Gurung-López S, Tacchella S, Oesch P, Kashino D, Conroy C, Sobral D. 2024. Anatomy of an ionized bubble: NIRCam grism spectroscopy of the z = 6.6 double-peaked Lyman- α emitter COLA1 and its environment. Astronomy &#38; Astrophysics. 689, A44.","mla":"Torralba-Torregrosa, Alberto, et al. “Anatomy of an Ionized Bubble: NIRCam Grism Spectroscopy of the z = 6.6 Double-Peaked Lyman- α Emitter COLA1 and Its Environment.” <i>Astronomy &#38; Astrophysics</i>, vol. 689, A44, EDP Sciences, 2024, doi:<a href=\"https://doi.org/10.1051/0004-6361/202450318\">10.1051/0004-6361/202450318</a>.","chicago":"Torralba-Torregrosa, Alberto, Jorryt J Matthee, Rohan P. Naidu, Ruari Mackenzie, Gabriele Pezzulli, Anne Hutter, Pablo Arnalte-Mur, et al. “Anatomy of an Ionized Bubble: NIRCam Grism Spectroscopy of the z = 6.6 Double-Peaked Lyman- α Emitter COLA1 and Its Environment.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2024. <a href=\"https://doi.org/10.1051/0004-6361/202450318\">https://doi.org/10.1051/0004-6361/202450318</a>.","ieee":"A. Torralba-Torregrosa <i>et al.</i>, “Anatomy of an ionized bubble: NIRCam grism spectroscopy of the z = 6.6 double-peaked Lyman- α emitter COLA1 and its environment,” <i>Astronomy &#38; Astrophysics</i>, vol. 689. EDP Sciences, 2024.","apa":"Torralba-Torregrosa, A., Matthee, J. J., Naidu, R. P., Mackenzie, R., Pezzulli, G., Hutter, A., … Sobral, D. (2024). Anatomy of an ionized bubble: NIRCam grism spectroscopy of the z = 6.6 double-peaked Lyman- α emitter COLA1 and its environment. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202450318\">https://doi.org/10.1051/0004-6361/202450318</a>","ama":"Torralba-Torregrosa A, Matthee JJ, Naidu RP, et al. Anatomy of an ionized bubble: NIRCam grism spectroscopy of the z = 6.6 double-peaked Lyman- α emitter COLA1 and its environment. <i>Astronomy &#38; Astrophysics</i>. 2024;689. doi:<a href=\"https://doi.org/10.1051/0004-6361/202450318\">10.1051/0004-6361/202450318</a>"},"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"publication":"Astronomy & Astrophysics","ddc":["520"],"department":[{"_id":"JoMa"}]},{"author":[{"full_name":"Breton, S. N.","first_name":"S. N.","last_name":"Breton"},{"first_name":"A. F.","last_name":"Lanza","full_name":"Lanza, A. F."},{"full_name":"Messina, S.","last_name":"Messina","first_name":"S."},{"full_name":"Pagano, I.","first_name":"I.","last_name":"Pagano"},{"orcid":"0000-0003-0142-4000","full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","last_name":"Bugnet","first_name":"Lisa Annabelle"},{"first_name":"E.","last_name":"Corsaro","full_name":"Corsaro, E."},{"full_name":"García, R. A.","last_name":"García","first_name":"R. A."},{"last_name":"Mathur","first_name":"S.","full_name":"Mathur, S."},{"last_name":"Santos","first_name":"A. R. G.","full_name":"Santos, A. R. G."},{"full_name":"Aigrain, S.","first_name":"S.","last_name":"Aigrain"},{"first_name":"L.","last_name":"Amard","full_name":"Amard, L."},{"full_name":"Brun, A. S.","last_name":"Brun","first_name":"A. S."},{"last_name":"Degott","first_name":"L.","full_name":"Degott, L."},{"last_name":"Noraz","first_name":"Q.","full_name":"Noraz, Q."},{"full_name":"Palakkatharappil, D. B.","first_name":"D. B.","last_name":"Palakkatharappil"},{"full_name":"Panetier, E.","last_name":"Panetier","first_name":"E."},{"first_name":"A.","last_name":"Strugarek","full_name":"Strugarek, A."},{"first_name":"K.","last_name":"Belkacem","full_name":"Belkacem, K."},{"last_name":"Goupil","first_name":"M.-J","full_name":"Goupil, M.-J"},{"last_name":"Ouazzani","first_name":"R. M.","full_name":"Ouazzani, R. M."},{"full_name":"Philidet, J.","last_name":"Philidet","first_name":"J."},{"first_name":"C.","last_name":"Renié","full_name":"Renié, C."},{"full_name":"Roth, O.","last_name":"Roth","first_name":"O."}],"date_created":"2025-01-27T13:12:44Z","doi":"10.1051/0004-6361/202449893","intvolume":"       689","type":"journal_article","file":[{"date_updated":"2025-01-27T13:18:41Z","file_name":"2024_AstronomyAstrophysics_Breton.pdf","date_created":"2025-01-27T13:18:41Z","creator":"dernst","content_type":"application/pdf","file_size":6212007,"access_level":"open_access","success":1,"relation":"main_file","checksum":"5c871ba7370a507ed6ea9fb2304d8263","file_id":"18905"}],"_id":"18904","publisher":"EDP Sciences","arxiv":1,"date_published":"2024-09-01T00:00:00Z","volume":689,"oa":1,"year":"2024","file_date_updated":"2025-01-27T13:18:41Z","abstract":[{"lang":"eng","text":"The Planetary Transits and Oscillations of stars mission (PLATO) will allow us to measure surface rotation and monitor photometric activity of tens of thousands of main sequence solar-type and subgiant stars. This paper is the first of a series dedicated to the preparation of the analysis of stellar surface rotation and photospheric activity with the near-future PLATO data. We describe in this work the strategy that will be implemented in the PLATO pipeline to measure stellar surface rotation, photometric activity, and long-term modulations. The algorithms are applied on both noise-free and noisy simulations of solar-type stars, which include activity cycles, latitudinal differential rotation, and spot evolution. PLATO simulated systematics are included in the noisy light curves. We show that surface rotation periods can be recovered with confidence for most of the stars with only six months of observations and that the recovery rate of the analysis significantly improves as additional observations are collected. This means that the first PLATO data release will already provide a substantial set of measurements for this quantity, with a significant refinement on their quality as the instrument obtains longer light curves. Measuring the Schwabe-like magnetic activity cycle during the mission will require that the same field be observed over a significant timescale (more than four years). Nevertheless, PLATO will provide a vast and robust sample of solar-type stars with constraints on the activity-cycle length. Such a sample is lacking from previous missions dedicated to space photometry."}],"publication_status":"published","article_type":"original","oa_version":"Published Version","external_id":{"arxiv":["2407.03709"],"isi":["001366206400007"]},"day":"01","OA_place":"publisher","has_accepted_license":"1","month":"09","title":"Measuring stellar surface rotation and activity with the PLATO mission. I. Strategy and application to simulated light curves","date_updated":"2026-07-08T06:45:15Z","acknowledgement":"This work presents results from the European Space Agency (ESA) space mission PLATO. The PLATO payload, the PLATO Ground Segment and PLATO data processing are joint developments of ESA and the PLATO Mission Consortium (PMC). Funding for the PMC is provided at national levels, in particular by countries participating in the PLATO Multilateral Agreement (Austria, Belgium, Czech Republic, Denmark, France, Germany, Italy, Netherlands, Portugal, Spain, Sweden, Switzerland, Norway, and United Kingdom) and institutions from Brazil. Members of the PLATO Consortium can be found at https://platomission.com. The ESA PLATO mission website is https://www.cosmos.esa.int/plato. The authors thank the teams working for PLATO for all their work. They acknowledge the critical reading and the constructive comments from the anonymous referee that significantly allowed improving the original version of this paper. They finally thank R. Samadi for helpful advice and suggestions concerning the PSLS abilities. S.N.B, A.F.L, S.Me, I.P and E.C acknowledge support from PLATO ASI-INAF agreement no. 2022-28-HH.0 “PLATO Fase D”. S.N.B, L.A, A.S.B, Q.N, and A.S acknowledge financial support by ERC Whole Sun Synergy grant #810218. S.N.B, R.A.G, L.A, A.S.B, Q.N., D.B.P, E.P, and A.S acknowledge the support from PLATO CNES grant. R.A.G, D.B.P, and E.P acknowledge the support from SoHO/GOLF CNES grant. A.S.B, Q.N, and A.S acknowledge the support from INSU/PNST grant and Solar Orbiter CNES grant. A.S acknowledges funding from from the European Union’s Horizon-2020 research and innovation program (grant agreement no. 776403 ExoplANETS-A) and the Programme National de Planétologie (PNP). A.R.G.S acknowledges the support from the FCT through national funds and FEDER through COMPETE2020 (UIDB/04434/2020, UIDP/04434/2020, 2022.03993.PTDC) and the support from the FCT through the work contract No. 2020.02480.CEECIND/CP1631/CT0001. S.Ma acknowledges support from the Spanish Ministry of Science and Innovation (MICINN) with the Ramón y Cajal fellowship no. RYC-2015-17697 and through AEI under the Severo Ochoa Centres of Excellence Programme 2020–2023 (CEX2019-000920-S). S.Ma acknowledges support from the Spanish Ministry of Science and Innovation (MICINN) with the grant no. PID2019-107187GB-I00. M.J.G., K.B., R.M.O, J.P, O.R., C.R. acknowledge support from CNES. The computations were performed with the IRFU/CEA Saclay server facilities, funded by ERC Synergy grant WholeSun No.810218, the P2IO Labex emergence project FlarePredict, and CNES PLATO funds. Software:star-privateer (this work), pyspot (Aigrain et al. 2015), PSLS (Samadi et al. 2019), numpy (Harris et al. 2020), matplotlib (Hunter 2007), scipy (Virtanen et al. 2020), astropy (Astropy Collaboration 2022), pandas (Wes McKinney 2010; The pandas development team 2020), scikit-learn (Pedregosa et al. 2011).","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"article_processing_charge":"No","article_number":"A229","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"quality_controlled":"1","OA_type":"hybrid","das_tickbox":"1","status":"public","citation":{"ama":"Breton SN, Lanza AF, Messina S, et al. Measuring stellar surface rotation and activity with the PLATO mission. I. Strategy and application to simulated light curves. <i>Astronomy &#38; Astrophysics</i>. 2024;689. doi:<a href=\"https://doi.org/10.1051/0004-6361/202449893\">10.1051/0004-6361/202449893</a>","apa":"Breton, S. N., Lanza, A. F., Messina, S., Pagano, I., Bugnet, L. A., Corsaro, E., … Roth, O. (2024). Measuring stellar surface rotation and activity with the PLATO mission. I. Strategy and application to simulated light curves. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202449893\">https://doi.org/10.1051/0004-6361/202449893</a>","ieee":"S. N. Breton <i>et al.</i>, “Measuring stellar surface rotation and activity with the PLATO mission. I. Strategy and application to simulated light curves,” <i>Astronomy &#38; Astrophysics</i>, vol. 689. EDP Sciences, 2024.","chicago":"Breton, S. N., A. F. Lanza, S. Messina, I. Pagano, Lisa Annabelle Bugnet, E. Corsaro, R. A. García, et al. “Measuring Stellar Surface Rotation and Activity with the PLATO Mission. I. Strategy and Application to Simulated Light Curves.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2024. <a href=\"https://doi.org/10.1051/0004-6361/202449893\">https://doi.org/10.1051/0004-6361/202449893</a>.","mla":"Breton, S. N., et al. “Measuring Stellar Surface Rotation and Activity with the PLATO Mission. I. Strategy and Application to Simulated Light Curves.” <i>Astronomy &#38; Astrophysics</i>, vol. 689, A229, EDP Sciences, 2024, doi:<a href=\"https://doi.org/10.1051/0004-6361/202449893\">10.1051/0004-6361/202449893</a>.","ista":"Breton SN, Lanza AF, Messina S, Pagano I, Bugnet LA, Corsaro E, García RA, Mathur S, Santos ARG, Aigrain S, Amard L, Brun AS, Degott L, Noraz Q, Palakkatharappil DB, Panetier E, Strugarek A, Belkacem K, Goupil M-J, Ouazzani RM, Philidet J, Renié C, Roth O. 2024. Measuring stellar surface rotation and activity with the PLATO mission. I. Strategy and application to simulated light curves. Astronomy &#38; Astrophysics. 689, A229.","short":"S.N. Breton, A.F. Lanza, S. Messina, I. Pagano, L.A. Bugnet, E. Corsaro, R.A. García, S. Mathur, A.R.G. Santos, S. Aigrain, L. Amard, A.S. Brun, L. Degott, Q. Noraz, D.B. Palakkatharappil, E. Panetier, A. Strugarek, K. Belkacem, M.-J. Goupil, R.M. Ouazzani, J. Philidet, C. Renié, O. Roth, Astronomy &#38; Astrophysics 689 (2024)."},"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"publication":"Astronomy & Astrophysics","isi":1,"scopus_import":"1","ddc":["520"],"department":[{"_id":"LiBu"}]},{"OA_place":"publisher","day":"01","external_id":{"arxiv":["2404.17629"],"isi":["001322237700004"]},"oa_version":"Published Version","month":"10","has_accepted_license":"1","year":"2024","oa":1,"volume":690,"date_published":"2024-10-01T00:00:00Z","arxiv":1,"article_type":"original","publication_status":"published","abstract":[{"text":"We present the first results on the spatial distribution of star formation in 454 star-forming galaxies just after the epoch of reionisation (4.8 < z < 6.5) using Hα emission-line maps and F444W imaging that traces the stellar continuum from the JWST FRESCO NIRCam Slitless Spectroscopy Survey. The Hα equivalent width profiles of star-forming galaxies across the main sequence at z ∼ 5.3 with stellar masses 6.8≤ log(M*/M⊙) < 11.1 increase with radius, which provides direct evidence for the inside-out growth of star-forming galaxies just after the epoch of reionisation. GALFIT was used to calculate half-light radii, Reff, and central surface densities within 1 kiloparsec, Σ1kpc of Hα and the continuum. At a fixed stellar mass of Log(M*/M⊙) = 9.5, Σ1kpc, Hα is 1.04 ± 0.05 times higher than Σ1kpc, C, Reff, Hα is 1.18 ± 0.03 times larger than Reff, C and both Reff measurements are smaller than 1 kiloparsec. These measurements suggest the rapid build-up of compact bulges via star formation just after the epoch of reionisation. By comparison to analogous work done at lower redshifts with Hubble Space Telescope WFC3 slitless spectroscopy as part of the 3D-HST (z ∼ 1) and CLEAR (z ∼ 0.5) surveys, we find that Reff(z) evolves at the same pace for Hα and the continuum, but Σ1kpc(z) evolves faster for Hα than the stellar continuum. As a function of the Hubble parameter, Reff, Hα/Reff,C = 1.1h(z) and Σ1 kpc, Hα/Σ1 kpc,C = h(z)1.3. These parametrisations suggest that the inside-out growth of the disk starts to dominate the inside-out growth of the bulge towards lower redshifts. This is supported by the redshift evolution in the EW(Hα) profiles from FRESCO, 3D-HST, and CLEAR at fixed stellar mass and when star-forming progenitors are traced, in which in EW(Hα) rapidly increases with radius within the half-light radius at z ∼ 5.3, but EW(Hα) increases only significantly with radius in the outer disk at z ∼ 0.5.","lang":"eng"}],"file_date_updated":"2024-10-21T11:45:35Z","file":[{"date_updated":"2024-10-21T11:45:35Z","file_name":"2024_AstronomyAstrophysics_Matharu.pdf","date_created":"2024-10-21T11:45:35Z","creator":"dernst","checksum":"10ae78291aa9fa9a9e64724c42d91588","relation":"main_file","success":1,"file_id":"18457","content_type":"application/pdf","file_size":825494,"access_level":"open_access"}],"publisher":"EDP Sciences","_id":"18447","doi":"10.1051/0004-6361/202450522","author":[{"full_name":"Matharu, Jasleen","first_name":"Jasleen","last_name":"Matharu"},{"first_name":"Erica J.","last_name":"Nelson","full_name":"Nelson, Erica J."},{"last_name":"Brammer","first_name":"Gabriel","full_name":"Brammer, Gabriel"},{"full_name":"Oesch, Pascal A.","last_name":"Oesch","first_name":"Pascal A."},{"first_name":"Natalie","last_name":"Allen","full_name":"Allen, Natalie"},{"full_name":"Shivaei, Irene","first_name":"Irene","last_name":"Shivaei"},{"full_name":"Naidu, Rohan P.","last_name":"Naidu","first_name":"Rohan P."},{"first_name":"John","last_name":"Chisholm","full_name":"Chisholm, John"},{"first_name":"Alba","last_name":"Covelo-Paz","full_name":"Covelo-Paz, Alba"},{"last_name":"Fudamoto","first_name":"Yoshinobu","full_name":"Fudamoto, Yoshinobu"},{"last_name":"Giovinazzo","first_name":"Emma","full_name":"Giovinazzo, Emma"},{"full_name":"Herard-Demanche, Thomas","last_name":"Herard-Demanche","first_name":"Thomas"},{"full_name":"Kerutt, Josephine","last_name":"Kerutt","first_name":"Josephine"},{"last_name":"Kramarenko","first_name":"Ivan","orcid":"0000-0001-5346-6048","full_name":"Kramarenko, Ivan","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4"},{"first_name":"Danilo","last_name":"Marchesini","full_name":"Marchesini, Danilo"},{"last_name":"Meyer","first_name":"Romain A.","full_name":"Meyer, Romain A."},{"full_name":"Prieto-Lyon, Gonzalo","first_name":"Gonzalo","last_name":"Prieto-Lyon"},{"full_name":"Reddy, Naveen","first_name":"Naveen","last_name":"Reddy"},{"full_name":"Shuntov, Marko","first_name":"Marko","last_name":"Shuntov"},{"full_name":"Weibel, Andrea","first_name":"Andrea","last_name":"Weibel"},{"last_name":"Wuyts","first_name":"Stijn","full_name":"Wuyts, Stijn"},{"last_name":"Xiao","first_name":"Mengyuan","full_name":"Xiao, Mengyuan"}],"date_created":"2024-10-20T22:02:06Z","intvolume":"       690","type":"journal_article","ddc":["520"],"department":[{"_id":"JoMa"}],"status":"public","das_tickbox":"1","scopus_import":"1","isi":1,"publication":"Astronomy & Astrophysics","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"citation":{"mla":"Matharu, Jasleen, et al. “A First Look at Spatially Resolved Star Formation at 4.8 &#60; z &#60; 6.5 with JWST FRESCO NIRCam Slitless Spectroscopy.” <i>Astronomy &#38; Astrophysics</i>, vol. 690, A64, EDP Sciences, 2024, doi:<a href=\"https://doi.org/10.1051/0004-6361/202450522\">10.1051/0004-6361/202450522</a>.","ista":"Matharu J, Nelson EJ, Brammer G, Oesch PA, Allen N, Shivaei I, Naidu RP, Chisholm J, Covelo-Paz A, Fudamoto Y, Giovinazzo E, Herard-Demanche T, Kerutt J, Kramarenko I, Marchesini D, Meyer RA, Prieto-Lyon G, Reddy N, Shuntov M, Weibel A, Wuyts S, Xiao M. 2024. A first look at spatially resolved star formation at 4.8 &#60; z &#60; 6.5 with JWST FRESCO NIRCam slitless spectroscopy. Astronomy &#38; Astrophysics. 690, A64.","chicago":"Matharu, Jasleen, Erica J. Nelson, Gabriel Brammer, Pascal A. Oesch, Natalie Allen, Irene Shivaei, Rohan P. Naidu, et al. “A First Look at Spatially Resolved Star Formation at 4.8 &#60; z &#60; 6.5 with JWST FRESCO NIRCam Slitless Spectroscopy.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2024. <a href=\"https://doi.org/10.1051/0004-6361/202450522\">https://doi.org/10.1051/0004-6361/202450522</a>.","short":"J. Matharu, E.J. Nelson, G. Brammer, P.A. Oesch, N. Allen, I. Shivaei, R.P. Naidu, J. Chisholm, A. Covelo-Paz, Y. Fudamoto, E. Giovinazzo, T. Herard-Demanche, J. Kerutt, I. Kramarenko, D. Marchesini, R.A. Meyer, G. Prieto-Lyon, N. Reddy, M. Shuntov, A. Weibel, S. Wuyts, M. Xiao, Astronomy &#38; Astrophysics 690 (2024).","ieee":"J. Matharu <i>et al.</i>, “A first look at spatially resolved star formation at 4.8 &#60; z &#60; 6.5 with JWST FRESCO NIRCam slitless spectroscopy,” <i>Astronomy &#38; Astrophysics</i>, vol. 690. EDP Sciences, 2024.","ama":"Matharu J, Nelson EJ, Brammer G, et al. A first look at spatially resolved star formation at 4.8 &#60; z &#60; 6.5 with JWST FRESCO NIRCam slitless spectroscopy. <i>Astronomy &#38; Astrophysics</i>. 2024;690. doi:<a href=\"https://doi.org/10.1051/0004-6361/202450522\">10.1051/0004-6361/202450522</a>","apa":"Matharu, J., Nelson, E. J., Brammer, G., Oesch, P. A., Allen, N., Shivaei, I., … Xiao, M. (2024). A first look at spatially resolved star formation at 4.8 &#60; z &#60; 6.5 with JWST FRESCO NIRCam slitless spectroscopy. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202450522\">https://doi.org/10.1051/0004-6361/202450522</a>"},"quality_controlled":"1","language":[{"iso":"eng"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","OA_type":"hybrid","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"acknowledgement":"JM is grateful to the Cosmic Dawn Center for the DAWN Fellowship. JM thanks Adam Muzzin, Viola Gelli and Anne Hutter for useful discussions that led to improvements in the analysis presented in this paper. This work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The raw data were obtained from the Mikulski Archive for\r\nSpace Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with JWST Cycle 1 GO program #1895. Support for program JWST-GO-1895 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Associations of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. The Cosmic Dawn Center  DAWN) is funded by the Danish National Research Foundation under grant DNRF140.\r\nThis work has received funding from the Swiss State Secretariat for Education, Research and Innovation (SERI) under contract number MB22.00072, as well as from the Swiss National Science Foundation (SNSF) through project grant 200020_207349. RPN thanks the NASA Hubble Fellowshp Program for the Hubble Fellowship. DM acknowledges funding from JWST-GO-01895.013, provided through a grant from the STScI under NASA contract NAS5-03127.","date_updated":"2026-07-08T06:43:28Z","title":"A first look at spatially resolved star formation at 4.8 < z < 6.5 with JWST FRESCO NIRCam slitless spectroscopy","article_number":"A64","article_processing_charge":"Yes (in subscription journal)"},{"month":"10","has_accepted_license":"1","OA_place":"publisher","day":"01","external_id":{"arxiv":["2408.00517"],"isi":["001339205700015"]},"oa_version":"Published Version","article_type":"original","publication_status":"published","abstract":[{"text":"Context. The escape of Lyman-α photons at redshifts greater than two is an ongoing subject of study and an important quantity to further understanding of Lyman-α emitters (LAEs), the transmission of Lyman-α photons through the interstellar medium and intergalactic medium, and the impact these LAEs have on cosmic reionisation.\r\n\r\nAims. This study aims to assess the Lyman-α escape fraction, fesc, Lyα, over the redshift range 2.9 < z < 6.7, focusing on Very Large Telescope/Multi Unit Spectroscopic Explorer (VLT/MUSE) selected, gravitationally lensed, intrinsically faint LAEs. These galaxies are of particular interest as the potential drivers of cosmic reionisation.\r\n\r\nMethods. We assessed fesc, Lyα in two ways: through an individual study of 96 LAEs behind the A2744 lensing cluster, with James Webb Space Telescope/Near-Infrared Camera (JWST/NIRCam) and HST data, and through a study of the global evolution of fesc, Lyα using the state-of-the-art luminosity functions for LAEs and the UV-selected ‘parent’ population (dust-corrected). We compared these studies to those in the literature based on brighter samples.\r\n\r\nResults. We find a negligible redshift evolution of fesc, Lyα for our individual galaxies; it is likely that it was washed out by significant intrinsic scatter. We observed a more significant evolution towards higher escape fractions with decreasing UV magnitude and fit this relation. When comparing the two luminosity functions to derive fesc, Lyα in a global sense, we saw agreement with previous literature when integrating the luminosity functions to a bright limit. However, when integrating using a faint limit equivalent to the observational limits of our samples, we observed enhanced values of fesc, Lyα, particularly around z ∼ 6, where fesc, Lyα becomes consistent with 100% escape. This indicates for the faint regimes we sampled that galaxies towards reionisation tend to allow very large fractions of Lyman-α photons to escape. We interpret this as evidence of a lack of any significant dust in these populations; our sample is likely dominated by young, highly star-forming chemically unevolved galaxies. Finally, we assessed the contribution of the LAE population to reionisation using our latest values for fesc, Lyα and the LAE luminosity density. The dependence on the escape fraction of Lyman continuum photons is strong, but for values similar to those observed recently in z ∼ 3 LAEs and high-redshift analogues, LAEs could provide all the ionising emissivity necessary for reionisation.","lang":"eng"}],"file_date_updated":"2024-11-04T08:04:44Z","year":"2024","oa":1,"volume":690,"date_published":"2024-10-01T00:00:00Z","arxiv":1,"publisher":"EDP Sciences","_id":"18493","file":[{"content_type":"application/pdf","file_size":2008461,"access_level":"open_access","success":1,"relation":"main_file","checksum":"4007e2b0fadf93bea61c5bec3fc97e87","file_id":"18495","date_updated":"2024-11-04T08:04:44Z","creator":"dernst","file_name":"2024_AstronomyAstrophysics_Goovaerts.pdf","date_created":"2024-11-04T08:04:44Z"}],"intvolume":"       690","type":"journal_article","doi":"10.1051/0004-6361/202451432","date_created":"2024-11-03T23:01:45Z","author":[{"full_name":"Goovaerts, I.","last_name":"Goovaerts","first_name":"I."},{"full_name":"Thai, T. T.","first_name":"T. T.","last_name":"Thai"},{"last_name":"Pello","first_name":"R.","full_name":"Pello, R."},{"full_name":"Tuan-Anh, P.","first_name":"P.","last_name":"Tuan-Anh"},{"first_name":"N.","last_name":"Laporte","full_name":"Laporte, N."},{"orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee","first_name":"Jorryt J"},{"full_name":"Nanayakkara, T.","last_name":"Nanayakkara","first_name":"T."},{"full_name":"Pharo, J.","last_name":"Pharo","first_name":"J."}],"department":[{"_id":"JoMa"}],"ddc":["520"],"scopus_import":"1","isi":1,"publication":"Astronomy & Astrophysics","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"citation":{"mla":"Goovaerts, I., et al. “Charting the Lyman-α Escape Fraction in the Range 2.9 &#60; z &#60; 6.7 and Consequences for the LAE Reionisation Contribution.” <i>Astronomy &#38; Astrophysics</i>, vol. 690, A302, EDP Sciences, 2024, doi:<a href=\"https://doi.org/10.1051/0004-6361/202451432\">10.1051/0004-6361/202451432</a>.","ista":"Goovaerts I, Thai TT, Pello R, Tuan-Anh P, Laporte N, Matthee JJ, Nanayakkara T, Pharo J. 2024. Charting the Lyman-α escape fraction in the range 2.9 &#60; z &#60; 6.7 and consequences for the LAE reionisation contribution. Astronomy &#38; Astrophysics. 690, A302.","chicago":"Goovaerts, I., T. T. Thai, R. Pello, P. Tuan-Anh, N. Laporte, Jorryt J Matthee, T. Nanayakkara, and J. Pharo. “Charting the Lyman-α Escape Fraction in the Range 2.9 &#60; z &#60; 6.7 and Consequences for the LAE Reionisation Contribution.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2024. <a href=\"https://doi.org/10.1051/0004-6361/202451432\">https://doi.org/10.1051/0004-6361/202451432</a>.","short":"I. Goovaerts, T.T. Thai, R. Pello, P. Tuan-Anh, N. Laporte, J.J. Matthee, T. Nanayakkara, J. Pharo, Astronomy &#38; Astrophysics 690 (2024).","ieee":"I. Goovaerts <i>et al.</i>, “Charting the Lyman-α escape fraction in the range 2.9 &#60; z &#60; 6.7 and consequences for the LAE reionisation contribution,” <i>Astronomy &#38; Astrophysics</i>, vol. 690. EDP Sciences, 2024.","ama":"Goovaerts I, Thai TT, Pello R, et al. Charting the Lyman-α escape fraction in the range 2.9 &#60; z &#60; 6.7 and consequences for the LAE reionisation contribution. <i>Astronomy &#38; Astrophysics</i>. 2024;690. doi:<a href=\"https://doi.org/10.1051/0004-6361/202451432\">10.1051/0004-6361/202451432</a>","apa":"Goovaerts, I., Thai, T. T., Pello, R., Tuan-Anh, P., Laporte, N., Matthee, J. J., … Pharo, J. (2024). Charting the Lyman-α escape fraction in the range 2.9 &#60; z &#60; 6.7 and consequences for the LAE reionisation contribution. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202451432\">https://doi.org/10.1051/0004-6361/202451432</a>"},"status":"public","das_tickbox":"1","OA_type":"diamond","quality_controlled":"1","language":[{"iso":"eng"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","article_number":"A302","article_processing_charge":"No","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"date_updated":"2026-07-08T06:44:21Z","acknowledgement":"This work is done based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 060.A-9345, 092.A-0472, 094.A-0115, 095.A-0181, 096.A-0710, 097.A0269, 100.A-0249, and 294.A-5032. Also based on observations obtained with the\r\nNASA/ESA Hubble Space Telescope, retrieved from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute (STScI). STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. All plots in this paper were created using Matplotlib (Hunter 2007). Part of this work was supported by the French CNRS, the Aix-Marseille University, the French Programme National de Cosmologie et Galaxies (PNCG) of CNRS/INSU with INP and IN2P3, co-funded by CEA and CNES. This work also received support from the French government under the France 2030 investment plan, as part of the Excellence Initiative of Aix-Marseille University - A*MIDEX (AMX-19-IET-008 - IPhU).\r\nFinancial support from the World Laboratory, the Odon Vallet Foundation and VNSC is gratefully acknowledged. Tran Thi Thai was funded by Vingroup JSC and supported by the Master, PhD Scholarship Programme of Vingroup Innovation Foundation (VINIF), Institute of Big Data, code VINIF.2023.TS.108. This research was funded by Vingroup Innovation Foundation under project code VINIF.2023.DA.057.","title":"Charting the Lyman-α escape fraction in the range 2.9 < z < 6.7 and consequences for the LAE reionisation contribution"},{"department":[{"_id":"LiBu"}],"corr_author":"1","ddc":["520"],"isi":1,"scopus_import":"1","citation":{"chicago":"Das, Srijan B, Lukas Einramhof, and Lisa Annabelle Bugnet. “Unveiling Complex Magnetic Field Configurations in Red Giant Stars.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2024. <a href=\"https://doi.org/10.1051/0004-6361/202450918\">https://doi.org/10.1051/0004-6361/202450918</a>.","mla":"Das, Srijan B., et al. “Unveiling Complex Magnetic Field Configurations in Red Giant Stars.” <i>Astronomy &#38; Astrophysics</i>, vol. 690, A217, EDP Sciences, 2024, doi:<a href=\"https://doi.org/10.1051/0004-6361/202450918\">10.1051/0004-6361/202450918</a>.","ista":"Das SB, Einramhof L, Bugnet LA. 2024. Unveiling complex magnetic field configurations in red giant stars. Astronomy &#38; Astrophysics. 690, A217.","short":"S.B. Das, L. Einramhof, L.A. Bugnet, Astronomy &#38; Astrophysics 690 (2024).","apa":"Das, S. B., Einramhof, L., &#38; Bugnet, L. A. (2024). Unveiling complex magnetic field configurations in red giant stars. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202450918\">https://doi.org/10.1051/0004-6361/202450918</a>","ama":"Das SB, Einramhof L, Bugnet LA. Unveiling complex magnetic field configurations in red giant stars. <i>Astronomy &#38; Astrophysics</i>. 2024;690. doi:<a href=\"https://doi.org/10.1051/0004-6361/202450918\">10.1051/0004-6361/202450918</a>","ieee":"S. B. Das, L. Einramhof, and L. A. Bugnet, “Unveiling complex magnetic field configurations in red giant stars,” <i>Astronomy &#38; Astrophysics</i>, vol. 690. EDP Sciences, 2024."},"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"publication":"Astronomy & Astrophysics","status":"public","das_tickbox":"1","OA_type":"hybrid","quality_controlled":"1","language":[{"iso":"eng"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","article_number":"A217","article_processing_charge":"No","date_updated":"2026-07-08T06:44:58Z","acknowledgement":"The authors thank S. Mathis, L. Barrault, S. Torres, A. Cristea, and K. M. Smith for very useful discussions. This project has received funding from the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curíe grant agreement No 101034413. The authors thank the anonymous referee for valuable comments and suggestions to improve the manuscript.","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"title":"Unveiling complex magnetic field configurations in red giant stars","has_accepted_license":"1","month":"10","day":"01","OA_place":"publisher","oa_version":"Published Version","external_id":{"arxiv":["2405.20133"],"isi":["001336485200015"]},"ec_funded":1,"abstract":[{"text":"The recent measurement of magnetic field strength inside the radiative interior of red giant stars has opened the way toward full 3D characterization of the geometry of stable large-scale magnetic fields. However, current measurements, which are limited to dipolar (ℓ = 1) mixed modes, do not properly constrain the topology of magnetic fields due to degeneracies on the observed magnetic field signature on such ℓ = 1 mode frequencies. Efforts focused toward unambiguous detections of magnetic field configurations are now key to better understand angular momentum transport in stars. We investigated the detectability of complex magnetic field topologies (such as the ones observed at the surface of stars with a radiative envelope with spectropolarimetry) inside the radiative interior of red giants. We focused on a field composed of a combination of a dipole and a quadrupole (quadrudipole) and on an offset field. We explored the potential of probing such magnetic field topologies from a combined measurement of magnetic signatures on ℓ = 1 and quadrupolar (ℓ = 2) mixed mode oscillation frequencies. We first derived the asymptotic theoretical formalism for computing the asymmetric signature in the frequency pattern for ℓ = 2 modes due to a quadrudipole magnetic field. To access asymmetry parameters for more complex magnetic field topologies, we numerically performed a grid search over the parameter space to map the degeneracy of the signatures of given topologies. We demonstrate the crucial role played by ℓ = 2 mixed modes in accessing internal magnetic fields with a quadrupolar component. The degeneracy of the quadrudipole compared to pure dipolar fields is lifted when considering magnetic asymmetries in both ℓ = 1 and ℓ = 2 mode frequencies. In addition to the analytical derivation for the quadrudipole, we present the prospect for complex magnetic field inversions using magnetic sensitivity kernels from standard perturbation analysis for forward modeling. Using this method, we explored the detectability of offset magnetic fields from ℓ = 1 and ℓ = 2 frequencies and demonstrate that offset fields may be mistaken for weak and centered magnetic fields, resulting in underestimating the magnetic field strength in stellar cores. We emphasize the need to characterize ℓ = 2 mixed-mode frequencies, (along with the currently characterized ℓ = 1 mixed modes), to unveil the higher-order components of the geometry of buried magnetic fields and to better constrain angular momentum transport inside stars.","lang":"eng"}],"article_type":"original","publication_status":"published","file_date_updated":"2024-11-11T09:01:11Z","date_published":"2024-10-01T00:00:00Z","volume":690,"year":"2024","oa":1,"arxiv":1,"publisher":"EDP Sciences","_id":"18528","file":[{"file_id":"18534","relation":"main_file","success":1,"checksum":"d43bbe6ed8ce4512e65e2d0d87070cf6","file_size":5306256,"access_level":"open_access","content_type":"application/pdf","creator":"dernst","date_created":"2024-11-11T09:01:11Z","file_name":"2024_AstronomyAstrophysics_Das.pdf","date_updated":"2024-11-11T09:01:11Z"}],"type":"journal_article","intvolume":"       690","project":[{"name":"IST-BRIDGE: International postdoctoral program","call_identifier":"H2020","_id":"fc2ed2f7-9c52-11eb-aca3-c01059dda49c","grant_number":"101034413"}],"doi":"10.1051/0004-6361/202450918","author":[{"first_name":"Srijan B","last_name":"Das","id":"9ce7c423-dacf-11ed-8942-e09c6cb27149","full_name":"Das, Srijan B","orcid":"0000-0003-0896-7972"},{"first_name":"Lukas","last_name":"Einramhof","id":"f1497a1a-72ef-11ef-b75a-fd877bbf6e8c","full_name":"Einramhof, Lukas"},{"full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","orcid":"0000-0003-0142-4000","first_name":"Lisa Annabelle","last_name":"Bugnet"}],"date_created":"2024-11-10T23:02:00Z"},{"_id":"15336","publisher":"EDP Sciences","file":[{"date_updated":"2024-04-23T06:59:18Z","creator":"dernst","file_name":"2024_AstronomyAstrophysics_Pensabene.pdf","date_created":"2024-04-23T06:59:18Z","content_type":"application/pdf","file_size":4410627,"access_level":"open_access","relation":"main_file","success":1,"checksum":"ab48775b6946cebfa27ddded5a68fdd2","file_id":"15341"}],"type":"journal_article","intvolume":"       684","author":[{"last_name":"Pensabene","first_name":"A.","full_name":"Pensabene, A."},{"last_name":"Cantalupo","first_name":"S.","full_name":"Cantalupo, S."},{"full_name":"Cicone, C.","first_name":"C.","last_name":"Cicone"},{"first_name":"R.","last_name":"Decarli","full_name":"Decarli, R."},{"first_name":"M.","last_name":"Galbiati","full_name":"Galbiati, M."},{"last_name":"Ginolfi","first_name":"M.","full_name":"Ginolfi, M."},{"full_name":"De Beer, S.","first_name":"S.","last_name":"De Beer"},{"full_name":"Fossati, M.","last_name":"Fossati","first_name":"M."},{"full_name":"Fumagalli, M.","last_name":"Fumagalli","first_name":"M."},{"first_name":"T.","last_name":"Lazeyras","full_name":"Lazeyras, T."},{"last_name":"Pezzulli","first_name":"G.","full_name":"Pezzulli, G."},{"full_name":"Travascio, A.","first_name":"A.","last_name":"Travascio"},{"full_name":"Wang, W.","last_name":"Wang","first_name":"W."},{"first_name":"Jorryt J","last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X"},{"full_name":"Maseda, M. V.","last_name":"Maseda","first_name":"M. V."}],"date_created":"2024-04-21T22:00:53Z","doi":"10.1051/0004-6361/202348659","has_accepted_license":"1","month":"04","oa_version":"Published Version","external_id":{"isi":["001199982500009"],"arxiv":["2401.04765"]},"day":"01","file_date_updated":"2024-04-23T06:59:18Z","abstract":[{"lang":"eng","text":"Submillimeter surveys toward overdense regions in the early Universe are essential for uncovering the obscured star formation and the cold gas content of assembling galaxies within massive dark matter halos. In this work, we present deep ALMA mosaic observations covering an area of ∼2′×2′ around MUSE Quasar Nebula 01 (MQN01), one of the largest and brightest Ly-α emitting nebulae discovered thus far; it surrounds a radio-quiet quasar at z ≃ 3.25. Our observations target the 1.2 and the 3 mm dust continuum as well as the carbon monoxide CO(4–3) transition in galaxies in the vicinity of the quasar. We identify a robust sample of 11 CO-line-emitting galaxies (including a closely separated quasar companion) that lie within ±4000 km s−1 of the quasar systemic redshift. A fraction of these objects were missed in previous deep rest-frame optical/UV surveys, which highlights the critical role of (sub)millimeter imaging. We also detect a total of 11 sources revealed in the dust continuum at 1.2 mm; six of them have either high-fidelity spectroscopic redshift information from rest-frame UV metal absorptions or the CO(4–3) line that places them in the same narrow redshift range. A comparison of the CO luminosity function and 1.2 mm number count density with those of the general fields points to a galaxy overdensity of δ > 10. We find evidence of a systematic flattening at the bright end of the CO luminosity function with respect to the trend measured in blank fields. Our findings reveal that galaxies in dense regions at z ∼ 3 are more massive and significantly richer in molecular gas than galaxies in fields, which enables a faster and accelerated assembly. This is the first in a series of studies aimed at characterizing one of the densest regions of the Universe found so far at z > 3."}],"article_type":"original","publication_status":"published","arxiv":1,"date_published":"2024-04-01T00:00:00Z","volume":684,"year":"2024","oa":1,"language":[{"iso":"eng"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","quality_controlled":"1","article_processing_charge":"Yes (in subscription journal)","article_number":"A119","title":"ALMA survey of a massive node of the Cosmic Web at z ∼ 3: I. Discovery of a large overdensity of CO emitters","date_updated":"2026-07-08T06:39:24Z","acknowledgement":"We thank the anonymous referee for the careful reading of the paper and useful suggestions which improved the manuscript. We thank Dr. Leindert Boogaard for sharing data and providing support in the data analysis process. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2021.1.00793.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST 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. This project was supported by the European Research Council (ERC) Consolidator Grant 864361 (CosmicWeb) and by Fondazione Cariplo grant no. 2020-0902. M.M. was supported in part by grant HST-GO-17065. This research made use of Astropy (http://www.astropy.org), a community-developed core Python package for Astronomy (Astropy Collaboration 2013, 2018), NumPy (Harris et al. 2020), SciPy (Virtanen et al. 2020), Matplotlib (Hunter 2007), and Statsmodel (Seabold & Perktold 2010).","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"department":[{"_id":"JoMa"}],"ddc":["520"],"citation":{"short":"A. Pensabene, S. Cantalupo, C. Cicone, R. Decarli, M. Galbiati, M. Ginolfi, S. De Beer, M. Fossati, M. Fumagalli, T. Lazeyras, G. Pezzulli, A. Travascio, W. Wang, J.J. Matthee, M.V. Maseda, Astronomy &#38; Astrophysics 684 (2024).","mla":"Pensabene, A., et al. “ALMA Survey of a Massive Node of the Cosmic Web at z ∼ 3: I. Discovery of a Large Overdensity of CO Emitters.” <i>Astronomy &#38; Astrophysics</i>, vol. 684, A119, EDP Sciences, 2024, doi:<a href=\"https://doi.org/10.1051/0004-6361/202348659\">10.1051/0004-6361/202348659</a>.","ista":"Pensabene A, Cantalupo S, Cicone C, Decarli R, Galbiati M, Ginolfi M, De Beer S, Fossati M, Fumagalli M, Lazeyras T, Pezzulli G, Travascio A, Wang W, Matthee JJ, Maseda MV. 2024. ALMA survey of a massive node of the Cosmic Web at z ∼ 3: I. Discovery of a large overdensity of CO emitters. Astronomy &#38; Astrophysics. 684, A119.","chicago":"Pensabene, A., S. Cantalupo, C. Cicone, R. Decarli, M. Galbiati, M. Ginolfi, S. De Beer, et al. “ALMA Survey of a Massive Node of the Cosmic Web at z ∼ 3: I. Discovery of a Large Overdensity of CO Emitters.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2024. <a href=\"https://doi.org/10.1051/0004-6361/202348659\">https://doi.org/10.1051/0004-6361/202348659</a>.","ieee":"A. Pensabene <i>et al.</i>, “ALMA survey of a massive node of the Cosmic Web at z ∼ 3: I. Discovery of a large overdensity of CO emitters,” <i>Astronomy &#38; Astrophysics</i>, vol. 684. EDP Sciences, 2024.","apa":"Pensabene, A., Cantalupo, S., Cicone, C., Decarli, R., Galbiati, M., Ginolfi, M., … Maseda, M. V. (2024). ALMA survey of a massive node of the Cosmic Web at z ∼ 3: I. Discovery of a large overdensity of CO emitters. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202348659\">https://doi.org/10.1051/0004-6361/202348659</a>","ama":"Pensabene A, Cantalupo S, Cicone C, et al. ALMA survey of a massive node of the Cosmic Web at z ∼ 3: I. Discovery of a large overdensity of CO emitters. <i>Astronomy &#38; Astrophysics</i>. 2024;684. doi:<a href=\"https://doi.org/10.1051/0004-6361/202348659\">10.1051/0004-6361/202348659</a>"},"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"publication":"Astronomy & Astrophysics","isi":1,"scopus_import":"1","das_tickbox":"1","status":"public"},{"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"date_updated":"2026-07-08T06:44:39Z","acknowledgement":"The authors would like to thank the anonymous referee for the useful suggestions which improved this article. This paper is based on data obtained with the ALMA Observatory, under Large Program 2017.1.00428.L. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), MOST 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. CDC would like to thank the GESO group at the European Southern Observatory (ESO) for the useful discussions while preparing this manuscript. The simulated data underlying this article will be shared on reasonable request to the corresponding author. CDC acknowledged support from Sapienza University of Rome program “Bando per la mobilità individuale all’estero” (DR n.1607 del 14 June 2021) during the visiting period (June-November 2022) at ESO Garching, Germany. LG and RS acknowledge support from the PRIN 2022 MUR project 2022CB3PJ3 – First Light And Galaxy aSsembly (FLAGS) funded by the European Union – Next Generation EU, and from the Amaldi Research Center funded by the MIUR program “Dipartimento di Eccellenza” (CUP:B81I18001170001). MR acknowledges support from the Narodowe Centrum Nauki (UMO-2020/38/E/ST9/00077) and support from the Foundation for Polish Science (FNP) under the program START 063.2023. We have benefited from the publicly available software CASA and CARTA and programming language Python, including the numpy (https://numpy.org), matplotlib (https://matplotlib.org), scipy (https://scipy.org) and astropy (http://www.astropy.org) packages. ","title":"Carbon envelopes around merging galaxies at z ~ 4.5","article_number":"A255","article_processing_charge":"No","quality_controlled":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"OA_type":"hybrid","status":"public","das_tickbox":"1","scopus_import":"1","isi":1,"publication":"Astronomy & Astrophysics","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"citation":{"ista":"Di Cesare C, Ginolfi M, Graziani L, Schneider R, Romano M, Popping G. 2024. Carbon envelopes around merging galaxies at z ~ 4.5. Astronomy &#38; Astrophysics. 690, A255.","mla":"Di Cesare, Claudia, et al. “Carbon Envelopes around Merging Galaxies at z ~ 4.5.” <i>Astronomy &#38; Astrophysics</i>, vol. 690, A255, EDP Sciences, 2024, doi:<a href=\"https://doi.org/10.1051/0004-6361/202449164\">10.1051/0004-6361/202449164</a>.","chicago":"Di Cesare, Claudia, M. Ginolfi, L. Graziani, R. Schneider, M. Romano, and G. Popping. “Carbon Envelopes around Merging Galaxies at z ~ 4.5.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2024. <a href=\"https://doi.org/10.1051/0004-6361/202449164\">https://doi.org/10.1051/0004-6361/202449164</a>.","short":"C. Di Cesare, M. Ginolfi, L. Graziani, R. Schneider, M. Romano, G. Popping, Astronomy &#38; Astrophysics 690 (2024).","ieee":"C. Di Cesare, M. Ginolfi, L. Graziani, R. Schneider, M. Romano, and G. Popping, “Carbon envelopes around merging galaxies at z ~ 4.5,” <i>Astronomy &#38; Astrophysics</i>, vol. 690. EDP Sciences, 2024.","ama":"Di Cesare C, Ginolfi M, Graziani L, Schneider R, Romano M, Popping G. Carbon envelopes around merging galaxies at z ~ 4.5. <i>Astronomy &#38; Astrophysics</i>. 2024;690. doi:<a href=\"https://doi.org/10.1051/0004-6361/202449164\">10.1051/0004-6361/202449164</a>","apa":"Di Cesare, C., Ginolfi, M., Graziani, L., Schneider, R., Romano, M., &#38; Popping, G. (2024). Carbon envelopes around merging galaxies at z ~ 4.5. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202449164\">https://doi.org/10.1051/0004-6361/202449164</a>"},"ddc":["520"],"corr_author":"1","department":[{"_id":"JoMa"}],"doi":"10.1051/0004-6361/202449164","date_created":"2024-11-10T23:02:00Z","author":[{"first_name":"Claudia","last_name":"Di Cesare","full_name":"Di Cesare, Claudia","id":"2d002343-372f-11ef-98ec-a164d20427cb"},{"first_name":"M.","last_name":"Ginolfi","full_name":"Ginolfi, M."},{"last_name":"Graziani","first_name":"L.","full_name":"Graziani, L."},{"last_name":"Schneider","first_name":"R.","full_name":"Schneider, R."},{"full_name":"Romano, M.","first_name":"M.","last_name":"Romano"},{"full_name":"Popping, G.","last_name":"Popping","first_name":"G."}],"intvolume":"       690","type":"journal_article","file":[{"creator":"dernst","file_name":"2024_AstronomyAstrophysics_diCesare.pdf","date_created":"2024-11-11T08:54:11Z","date_updated":"2024-11-11T08:54:11Z","file_id":"18533","checksum":"24c65a64047aba156f39b01425269bdb","relation":"main_file","success":1,"file_size":8033864,"access_level":"open_access","content_type":"application/pdf"}],"publisher":"EDP Sciences","_id":"18527","oa":1,"year":"2024","date_published":"2024-10-01T00:00:00Z","volume":690,"arxiv":1,"publication_status":"published","article_type":"original","abstract":[{"lang":"eng","text":"Context. Galaxies evolve through a dynamic exchange of material with their immediate surrounding environment, the so-called circumgalactic medium (CGM). Understanding the physics of gas flows and the nature of the CGM is fundamental to studying galaxy evolution, especially at 4 ≤ z ≤ 6 (i.e., after the Epoch of Reionization) when galaxies rapidly assembled their masses and reached their chemical maturity. Galactic outflows are predicted to enrich the CGM with metals, although it has also been suggested that gas stripping in systems undergoing a major merger may play a role.\r\n\r\nAims. In this work, we explore the metal enrichment of the medium around merging galaxies at z ∼ 4.5, observed by the ALMA Large Program to INvestigate [CII] at Early times (ALPINE). To do so, we study the nature of the [CII] 158 μm emission in the CGM around these systems, using simulations to help disentangle the mechanisms contributing to the CGM metal pollution.\r\n\r\nMethods. By adopting an updated classification of major merger systems in the ALPINE survey, we selected and analyzed merging galaxies whose components can be spatially and/or spectrally resolved in a robust way. This makes it possible to distinguish between the [CII] emission coming from the single components of the system and that coming from the system as a whole. We also made use of the dustyGadget cosmological simulation to select synthetic analogs of observed galaxies and guide the interpretation of the observational results.\r\n\r\nResults. We find a large diffuse [CII] envelope (≳20 kpc) embedding all the merging systems, with at least 25% of the total [CII] emission coming from the medium between the galaxies. Using predictions from dustyGadget, we suggest that this emission has a multi-fold nature, with dynamical interactions between galaxies playing a major role in stripping the gas and enriching the medium with heavy elements."}],"file_date_updated":"2024-11-11T08:54:11Z","OA_place":"publisher","day":"01","external_id":{"arxiv":["2401.03020"],"isi":["001332213700013"]},"oa_version":"Published Version","month":"10","has_accepted_license":"1"},{"ddc":["500"],"issue":"10","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"page":"3196-3208","citation":{"short":"M. Kwan, Y. Wigderson, Bulletin of the London Mathematical Society 56 (2024) 3196–3208.","ista":"Kwan M, Wigderson Y. 2024. The inertia bound is far from tight. Bulletin of the London Mathematical Society. 56(10), 3196–3208.","mla":"Kwan, Matthew, and Yuval Wigderson. “The Inertia Bound Is Far from Tight.” <i>Bulletin of the London Mathematical Society</i>, vol. 56, no. 10, Wiley, 2024, pp. 3196–208, doi:<a href=\"https://doi.org/10.1112/blms.13127\">10.1112/blms.13127</a>.","chicago":"Kwan, Matthew, and Yuval Wigderson. “The Inertia Bound Is Far from Tight.” <i>Bulletin of the London Mathematical Society</i>. Wiley, 2024. <a href=\"https://doi.org/10.1112/blms.13127\">https://doi.org/10.1112/blms.13127</a>.","ieee":"M. Kwan and Y. Wigderson, “The inertia bound is far from tight,” <i>Bulletin of the London Mathematical Society</i>, vol. 56, no. 10. Wiley, pp. 3196–3208, 2024.","apa":"Kwan, M., &#38; Wigderson, Y. (2024). The inertia bound is far from tight. <i>Bulletin of the London Mathematical Society</i>. Wiley. <a href=\"https://doi.org/10.1112/blms.13127\">https://doi.org/10.1112/blms.13127</a>","ama":"Kwan M, Wigderson Y. The inertia bound is far from tight. <i>Bulletin of the London Mathematical Society</i>. 2024;56(10):3196-3208. doi:<a href=\"https://doi.org/10.1112/blms.13127\">10.1112/blms.13127</a>"},"publication":"Bulletin of the London Mathematical Society","scopus_import":"1","status":"public","OA_type":"hybrid","language":[{"iso":"eng"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","quality_controlled":"1","article_processing_charge":"Yes (via OA deal)","title":"The inertia bound is far from tight","acknowledgement":"Open access funding provided by Eidgenossische Technische Hochschule Zurich.","date_updated":"2026-07-08T07:34:36Z","publication_identifier":{"issn":["0024-6093"],"eissn":["1469-2120"]},"extern":"1","month":"10","oa_version":"Published Version","external_id":{"arxiv":["2312.04925"]},"day":"01","OA_place":"publisher","abstract":[{"lang":"eng","text":"The inertia bound and ratio bound (also known as the Cvetković bound and Hoffman bound) are two fundamental inequalities in spectral graph theory, giving upper bounds on the independence number a(G) of a graph G in terms of spectral information about a weighted adjacency matrix of G. For both inequalities, given a graph G, one needs to make a judicious choice of weighted adjacency matrix to obtain as strong a bound as possible. While there is a well‐established theory surrounding the ratio bound, the inertia bound is much more mysterious, and its limits are rather unclear. In fact, only recently did Sinkovic find the first example of a graph for which the inertia bound is not tight (for any weighted adjacency matrix), answering a longstanding question of Godsil. We show that the inertia bound can be extremely far from tight, and in fact can significantly underperform the ratio bound: for example, one of our results is that for infinitely many n, there is an n‐vertex graph for which even the unweighted ratio bound can prove a(G)<4n^3/4, but the inertia bound is always at least n/4. In particular, these results address questions of Rooney, Sinkovic, and Wocjan–Elphick–Abiad."}],"publication_status":"published","article_type":"original","arxiv":1,"volume":56,"date_published":"2024-10-01T00:00:00Z","oa":1,"year":"2024","_id":"22154","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1112/blms.13127"}],"publisher":"Wiley","intvolume":"        56","type":"journal_article","date_created":"2026-06-29T10:49:18Z","author":[{"last_name":"Kwan","first_name":"Matthew","full_name":"Kwan, Matthew"},{"last_name":"Wigderson","first_name":"Yuval","full_name":"Wigderson, Yuval","id":"2d0023a0-1567-11f0-833d-d5c1e476d4b5"}],"doi":"10.1112/blms.13127"},{"project":[{"_id":"bdb2a702-d553-11ed-ba76-f12e3e5a3bc6","name":"A quantum hybrid of atoms and milligram-scale pendulums: towards gravitational quantum mechanics","grant_number":"101087907"}],"doi":"10.1103/physrevresearch.6.013141","date_created":"2024-02-12T11:42:18Z","author":[{"orcid":"0000-0003-0582-2946","full_name":"Agafonova, Sofya","id":"09501ff6-dca7-11ea-a8ae-b3e0b9166e80","last_name":"Agafonova","first_name":"Sofya"},{"full_name":"Mishra, Umang","id":"4328fa4c-f128-11eb-9611-c107b0fe4d51","last_name":"Mishra","first_name":"Umang"},{"id":"2E054C4C-F248-11E8-B48F-1D18A9856A87","full_name":"Diorico, Fritz R","orcid":"0000-0002-4947-8924","first_name":"Fritz R","last_name":"Diorico"},{"first_name":"Onur","last_name":"Hosten","full_name":"Hosten, Onur","id":"4C02D85E-F248-11E8-B48F-1D18A9856A87","orcid":"0000-0002-2031-204X"}],"type":"journal_article","intvolume":"         6","file":[{"success":1,"checksum":"3a39ebffb24c1cc1dd0b547a726dc52d","relation":"main_file","file_id":"14981","content_type":"application/pdf","file_size":1437167,"access_level":"open_access","date_updated":"2024-02-12T11:46:50Z","date_created":"2024-02-12T11:46:50Z","file_name":"2024_PhysicalRevResearch_Agafonova.pdf","creator":"dernst"}],"publisher":"American Physical Society","_id":"14980","year":"2024","oa":1,"volume":6,"date_published":"2024-02-05T00:00:00Z","arxiv":1,"DOAJ_listed":"1","publication_status":"published","article_type":"original","abstract":[{"lang":"eng","text":"Precision sensing and manipulation of milligram-scale mechanical oscillators has attracted growing interest in the fields of table-top explorations of gravity and tests of quantum mechanics at macroscopic scales. Torsional oscillators present an opportunity in this regard due to their remarked isolation from environmental noise. For torsional motion, an effective employment of optical cavities to enhance optomechanical interactions—as already established for linear oscillators—so far faced certain challenges. Here, we propose a concept for sensing and manipulating torsional motion, where exclusively the torsional rotations of a pendulum are mapped onto the path length of a single two-mirror optical cavity. The concept inherently alleviates many limitations of previous approaches. A proof-of-principle experiment is conducted with a rigidly controlled pendulum to explore the sensing aspects of the concept and to identify practical limitations in a potential state-of-the art setup. Based on this study, we anticipate development of precision torque sensors utilizing torsional pendulums that can support sensitivities below 10−19Nm/√Hz, while the motion of the pendulums are dominated by quantum radiation pressure noise at sub-microwatts of incoming laser power. These developments will provide horizons for experiments at the interface of quantum mechanics and gravity."}],"file_date_updated":"2024-02-12T11:46:50Z","OA_place":"publisher","researchdata_availability":"no","day":"05","external_id":{"arxiv":["2306.12804"]},"APC_amount":"2933,65 EUR","oa_version":"Published Version","month":"02","has_accepted_license":"1","publication_identifier":{"eissn":["2643-1564"]},"acknowledgement":"We thank Pere Rosselló for his contributions to the initial modeling of the presented sensing technique. This work was supported by Institute of Science and Technology Austria, and\r\nthe European Research Council under Grant No. 101087907 (ERC CoG QuHAMP).","date_updated":"2026-07-08T07:52:51Z","title":"Zigzag optical cavity for sensing and controlling torsional motion","article_number":"013141","article_processing_charge":"Yes","quality_controlled":"1","supplementarymaterial":"no","language":[{"iso":"eng"}],"user_id":"68b8ca59-c5b3-11ee-8790-cd641c68093d","OA_type":"gold","status":"public","das_tickbox":"0","scopus_import":"1","publication":"Physical Review Research","citation":{"apa":"Agafonova, S., Mishra, U., Diorico, F. R., &#38; Hosten, O. (2024). Zigzag optical cavity for sensing and controlling torsional motion. <i>Physical Review Research</i>. American Physical Society. <a href=\"https://doi.org/10.1103/physrevresearch.6.013141\">https://doi.org/10.1103/physrevresearch.6.013141</a>","ama":"Agafonova S, Mishra U, Diorico FR, Hosten O. Zigzag optical cavity for sensing and controlling torsional motion. <i>Physical Review Research</i>. 2024;6(1). doi:<a href=\"https://doi.org/10.1103/physrevresearch.6.013141\">10.1103/physrevresearch.6.013141</a>","ieee":"S. Agafonova, U. Mishra, F. R. Diorico, and O. Hosten, “Zigzag optical cavity for sensing and controlling torsional motion,” <i>Physical Review Research</i>, vol. 6, no. 1. American Physical Society, 2024.","chicago":"Agafonova, Sofia, Umang Mishra, Fritz R Diorico, and Onur Hosten. “Zigzag Optical Cavity for Sensing and Controlling Torsional Motion.” <i>Physical Review Research</i>. American Physical Society, 2024. <a href=\"https://doi.org/10.1103/physrevresearch.6.013141\">https://doi.org/10.1103/physrevresearch.6.013141</a>.","ista":"Agafonova S, Mishra U, Diorico FR, Hosten O. 2024. Zigzag optical cavity for sensing and controlling torsional motion. Physical Review Research. 6(1), 013141.","mla":"Agafonova, Sofia, et al. “Zigzag Optical Cavity for Sensing and Controlling Torsional Motion.” <i>Physical Review Research</i>, vol. 6, no. 1, 013141, American Physical Society, 2024, doi:<a href=\"https://doi.org/10.1103/physrevresearch.6.013141\">10.1103/physrevresearch.6.013141</a>.","short":"S. Agafonova, U. Mishra, F.R. Diorico, O. Hosten, Physical Review Research 6 (2024)."},"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"issue":"1","corr_author":"1","ddc":["530"],"department":[{"_id":"OnHo"}]},{"acknowledgement":"We thank Rishabh Sahu and Sebastian Wald for technical contributions to the experiment. Funding by Institute of Science and Technology Austria.","date_updated":"2026-07-08T08:25:12Z","publication_identifier":{"issn":["2334-2536"]},"dataavailabilitystatement":"Data underlying the results presented in this paper are not publicly available at this time but may be obtained from the authors upon reasonable request.","title":"Laser-cavity locking utilizing beam ellipticity: accessing the 10<sup>−7</sup> instability scale relative to cavity linewidth","article_processing_charge":"Yes","supplementarymaterial":"no","quality_controlled":"1","user_id":"68b8ca59-c5b3-11ee-8790-cd641c68093d","language":[{"iso":"eng"}],"OA_type":"gold","status":"public","keyword":["Atomic and Molecular Physics","and Optics","Electronic","Optical and Magnetic Materials"],"das_tickbox":"1","isi":1,"scopus_import":"1","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"page":"26-31","citation":{"ama":"Diorico FR, Zhutov A, Hosten O. Laser-cavity locking utilizing beam ellipticity: accessing the 10<sup>−7</sup> instability scale relative to cavity linewidth. <i>Optica</i>. 2024;11(1):26-31. doi:<a href=\"https://doi.org/10.1364/optica.507451\">10.1364/optica.507451</a>","apa":"Diorico, F. R., Zhutov, A., &#38; Hosten, O. (2024). Laser-cavity locking utilizing beam ellipticity: accessing the 10<sup>−7</sup> instability scale relative to cavity linewidth. <i>Optica</i>. Optica Publishing Group. <a href=\"https://doi.org/10.1364/optica.507451\">https://doi.org/10.1364/optica.507451</a>","ieee":"F. R. Diorico, A. Zhutov, and O. Hosten, “Laser-cavity locking utilizing beam ellipticity: accessing the 10<sup>−7</sup> instability scale relative to cavity linewidth,” <i>Optica</i>, vol. 11, no. 1. Optica Publishing Group, pp. 26–31, 2024.","chicago":"Diorico, Fritz R, Artem Zhutov, and Onur Hosten. “Laser-Cavity Locking Utilizing Beam Ellipticity: Accessing the 10<sup>−7</sup> Instability Scale Relative to Cavity Linewidth.” <i>Optica</i>. Optica Publishing Group, 2024. <a href=\"https://doi.org/10.1364/optica.507451\">https://doi.org/10.1364/optica.507451</a>.","ista":"Diorico FR, Zhutov A, Hosten O. 2024. Laser-cavity locking utilizing beam ellipticity: accessing the 10<sup>−7</sup> instability scale relative to cavity linewidth. Optica. 11(1), 26–31.","mla":"Diorico, Fritz R., et al. “Laser-Cavity Locking Utilizing Beam Ellipticity: Accessing the 10<sup>−7</sup> Instability Scale Relative to Cavity Linewidth.” <i>Optica</i>, vol. 11, no. 1, Optica Publishing Group, 2024, pp. 26–31, doi:<a href=\"https://doi.org/10.1364/optica.507451\">10.1364/optica.507451</a>.","short":"F.R. Diorico, A. Zhutov, O. Hosten, Optica 11 (2024) 26–31."},"publication":"Optica","corr_author":"1","ddc":["530"],"issue":"1","department":[{"_id":"OnHo"}],"doi":"10.1364/optica.507451","author":[{"first_name":"Fritz R","last_name":"Diorico","id":"2E054C4C-F248-11E8-B48F-1D18A9856A87","full_name":"Diorico, Fritz R","orcid":"0000-0002-4947-8924"},{"first_name":"Artem","last_name":"Zhutov","full_name":"Zhutov, Artem","id":"0f02ed6a-b514-11ee-b891-8379c5f19cb7"},{"orcid":"0000-0002-2031-204X","full_name":"Hosten, Onur","id":"4C02D85E-F248-11E8-B48F-1D18A9856A87","last_name":"Hosten","first_name":"Onur"}],"date_created":"2024-01-15T10:25:38Z","intvolume":"        11","type":"journal_article","file":[{"date_updated":"2024-01-17T08:53:16Z","file_name":"2023_Optica_Diorico.pdf","date_created":"2024-01-17T08:53:16Z","creator":"dernst","success":1,"checksum":"eb99ca7d0fe73e22f121875175546ed7","relation":"main_file","file_id":"14824","content_type":"application/pdf","access_level":"open_access","file_size":4558986}],"publisher":"Optica Publishing Group","_id":"14802","volume":11,"date_published":"2024-01-20T00:00:00Z","year":"2024","oa":1,"DOAJ_listed":"1","abstract":[{"text":"Frequency-stable lasers form the back bone of precision measurements in science and technology. Such lasers typically attain their stability through frequency locking to reference cavities. State-of-the-art locking performances to date had been achieved using frequency modulation based methods, complemented with active drift cancellation systems. We demonstrate an all passive, modulation-free laser-cavity locking technique (squash locking) that utilizes changes in spatial beam ellipticity for error signal generation, and a coherent polarization post-selection for noise resilience. By comparing two identically built proof-of-principle systems, we show a frequency locking instability of 5×10<jats:sup>−7</jats:sup> relative to the cavity linewidth at 10 s averaging. The results surpass the demonstrated performances of methods engineered over the last five decades, potentially enabling an advancement in the precision control of lasers, while creating avenues for bridging the performance gaps between industrial grade lasers with scientific ones due to the afforded simplicity and scalability.","lang":"eng"}],"article_type":"original","publication_status":"published","file_date_updated":"2024-01-17T08:53:16Z","day":"20","researchdata_availability":"upon request","OA_place":"publisher","oa_version":"Published Version","APC_amount":"3393,38 EUR","external_id":{"isi":["001202817000004"]},"has_accepted_license":"1","month":"01"},{"user_id":"ba8df636-2132-11f1-aed0-ed93e2281fdd","language":[{"iso":"eng"}],"article_processing_charge":"No","date_updated":"2026-07-08T08:50:57Z","publication_identifier":{"issn":["2663-337X"]},"title":"Towards a quantum entanglement enhanced atom interferomter","license":"https://creativecommons.org/licenses/by-nc-sa/4.0/","department":[{"_id":"GradSch"},{"_id":"OnHo"}],"ddc":["530"],"corr_author":"1","degree_awarded":"PhD","page":"79","tmp":{"short":"CC BY-NC-SA (4.0)","image":"/images/cc_by_nc_sa.png","legal_code_url":"https://creativecommons.org/licenses/by-nc-sa/4.0/legalcode","name":"Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)"},"citation":{"short":"V. Li, Towards a Quantum Entanglement Enhanced Atom Interferomter, Institute of Science and Technology Austria, 2024.","chicago":"Li, Vyacheslav. “Towards a Quantum Entanglement Enhanced Atom Interferomter.” Institute of Science and Technology Austria, 2024. <a href=\"https://doi.org/10.15479/at:ista:17225\">https://doi.org/10.15479/at:ista:17225</a>.","ista":"Li V. 2024. Towards a quantum entanglement enhanced atom interferomter. Institute of Science and Technology Austria.","mla":"Li, Vyacheslav. <i>Towards a Quantum Entanglement Enhanced Atom Interferomter</i>. Institute of Science and Technology Austria, 2024, doi:<a href=\"https://doi.org/10.15479/at:ista:17225\">10.15479/at:ista:17225</a>.","apa":"Li, V. (2024). <i>Towards a quantum entanglement enhanced atom interferomter</i>. Institute of Science and Technology Austria. <a href=\"https://doi.org/10.15479/at:ista:17225\">https://doi.org/10.15479/at:ista:17225</a>","ama":"Li V. Towards a quantum entanglement enhanced atom interferomter. 2024. doi:<a href=\"https://doi.org/10.15479/at:ista:17225\">10.15479/at:ista:17225</a>","ieee":"V. Li, “Towards a quantum entanglement enhanced atom interferomter,” Institute of Science and Technology Austria, 2024."},"status":"public","publisher":"Institute of Science and Technology Austria","_id":"17225","supervisor":[{"full_name":"Hosten, Onur","id":"4C02D85E-F248-11E8-B48F-1D18A9856A87","orcid":"0000-0002-2031-204X","first_name":"Onur","last_name":"Hosten"}],"file":[{"creator":"vli","date_created":"2024-07-11T10:26:22Z","file_name":"PhD_Thesis_Vyacheslav_Li_no_signatures_PDFA.pdf","date_updated":"2024-07-11T10:26:22Z","file_size":6729761,"access_level":"open_access","content_type":"application/pdf","file_id":"17228","checksum":"15b2dbe8d2c9ed7ca5dd413827928077","success":1,"relation":"main_file"},{"creator":"vli","file_name":"PhD Thesis Vyacheslav Li.zip","date_created":"2024-07-11T10:26:22Z","date_updated":"2024-07-11T10:26:22Z","file_id":"17229","relation":"source_file","checksum":"16e904a11d8d0ebb167cb654ddfc7fe5","access_level":"closed","file_size":9542859,"content_type":"application/x-zip-compressed"}],"type":"dissertation","doi":"10.15479/at:ista:17225","project":[{"grant_number":"101087907","name":"A quantum hybrid of atoms and milligram-scale pendulums: towards gravitational quantum mechanics","_id":"bdb2a702-d553-11ed-ba76-f12e3e5a3bc6"}],"date_created":"2024-07-11T09:46:48Z","author":[{"id":"3A4FAA92-F248-11E8-B48F-1D18A9856A87","full_name":"Li, Vyacheslav","first_name":"Vyacheslav","last_name":"Li"}],"has_accepted_license":"1","month":"07","day":"11","OA_place":"publisher","oa_version":"Published Version","abstract":[{"text":"This thesis describes the development of an atom interferometer designed to exploit the\r\nadvantages of utilizing quantum entanglement for enhanced precision measurements beyond\r\nthe standard quantum limit. While the project remains ongoing, significant progress has been\r\nmade.\r\nA key contribution of this work is the development of Quantrol, an experimental control\r\nsystem leveraging the ARTIQ framework. This software enables precise timing and control\r\nwithout requiring prior knowledge of ARTIQ’s implementation details or coding experience.\r\nThe interface offers user friendly visual comprehension of the experimental sequence and\r\nextended capabilities, allowing researchers to scan variables with a simple click of a mouse.\r\nThe main proposed project is to implement atom interferometric sequence with squeezed input\r\nstates inside of a dipole trap generated by a high finesse cavity. The presence of the dipole\r\ntrap allows one dimensional atomic cloud split while maintaining relatively strong confinement\r\nin other directions.\r\nWe are currently able to trap and cool 87Rb atoms to few micro kelvin temperatures, load\r\nthem into the dipole trap and state prepare them to be used for squeezing and interferometric\r\nsequence.","lang":"eng"}],"publication_status":"published","related_material":{"record":[{"status":"public","id":"11438","relation":"part_of_dissertation"}]},"file_date_updated":"2024-07-11T10:26:22Z","date_published":"2024-07-11T00:00:00Z","year":"2024","oa":1,"alternative_title":["ISTA Thesis"]},{"das_tickbox":"1","status":"public","citation":{"ieee":"C. Chintaluri <i>et al.</i>, “kCSD-python, reliable current source density estimation with quality control,” <i>PLoS Computational Biology</i>, vol. 20, no. 3. Public Library of Science, 2024.","apa":"Chintaluri, C., Bejtka, M., Sredniawa, W., Czerwinski, M., Dzik, J. M., Jedrzejewska-Szmek, J., &#38; Wojciki, D. K. (2024). kCSD-python, reliable current source density estimation with quality control. <i>PLoS Computational Biology</i>. Public Library of Science. <a href=\"https://doi.org/10.1371/journal.pcbi.1011941\">https://doi.org/10.1371/journal.pcbi.1011941</a>","ama":"Chintaluri C, Bejtka M, Sredniawa W, et al. kCSD-python, reliable current source density estimation with quality control. <i>PLoS Computational Biology</i>. 2024;20(3). doi:<a href=\"https://doi.org/10.1371/journal.pcbi.1011941\">10.1371/journal.pcbi.1011941</a>","mla":"Chintaluri, Chaitanya, et al. “KCSD-Python, Reliable Current Source Density Estimation with Quality Control.” <i>PLoS Computational Biology</i>, vol. 20, no. 3, e1011941, Public Library of Science, 2024, doi:<a href=\"https://doi.org/10.1371/journal.pcbi.1011941\">10.1371/journal.pcbi.1011941</a>.","ista":"Chintaluri C, Bejtka M, Sredniawa W, Czerwinski M, Dzik JM, Jedrzejewska-Szmek J, Wojciki DK. 2024. kCSD-python, reliable current source density estimation with quality control. PLoS Computational Biology. 20(3), e1011941.","chicago":"Chintaluri, Chaitanya, Marta Bejtka, Wladyslaw Sredniawa, Michal Czerwinski, Jakub M. Dzik, Joanna Jedrzejewska-Szmek, and Daniel K. Wojciki. “KCSD-Python, Reliable Current Source Density Estimation with Quality Control.” <i>PLoS Computational Biology</i>. Public Library of Science, 2024. <a href=\"https://doi.org/10.1371/journal.pcbi.1011941\">https://doi.org/10.1371/journal.pcbi.1011941</a>.","short":"C. Chintaluri, M. Bejtka, W. Sredniawa, M. Czerwinski, J.M. Dzik, J. Jedrzejewska-Szmek, D.K. Wojciki, PLoS Computational Biology 20 (2024)."},"tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png"},"publication":"PLoS Computational Biology","isi":1,"scopus_import":"1","corr_author":"1","ddc":["000","570"],"issue":"3","department":[{"_id":"TiVo"}],"pmid":1,"title":"kCSD-python, reliable current source density estimation with quality control","date_updated":"2026-07-13T12:30:33Z","acknowledgement":"The Python implementation of kCSD was started by Grzegorz Parka during Google Summer of Code project through the International Neuroinformatics Coordinating Facility. Jan Mąka implemented the first Python version of skCSD class. This work was supported by the Polish National Science Centre (2013/08/W/NZ4/00691 to DKW; 2015/17/B/ST7/04123 to DKW). ","publication_identifier":{"issn":["1553-734X"],"eissn":["1553-7358"]},"article_processing_charge":"Yes","article_number":"e1011941","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"quality_controlled":"1","OA_type":"gold","DOAJ_listed":"1","date_published":"2024-03-14T00:00:00Z","volume":20,"year":"2024","oa":1,"related_material":{"link":[{"relation":"software","url":"https://github.com/Neuroinflab/kCSD-python"}]},"file_date_updated":"2025-06-25T05:47:36Z","abstract":[{"text":"Interpretation of extracellular recordings can be challenging due to the long range of electric field. This challenge can be mitigated by estimating the current source density (CSD). Here we introduce kCSD-python, an open Python package implementing Kernel Current Source Density (kCSD) method and related tools to facilitate CSD analysis of experimental data and the interpretation of results. We show how to counter the limitations imposed by noise and assumptions in the method itself. kCSD-python allows CSD estimation for an arbitrary distribution of electrodes in 1D, 2D, and 3D, assuming distributions of sources in tissue, a slice, or in a single cell, and includes a range of diagnostic aids. We demonstrate its features in a Jupyter Notebook tutorial which illustrates a typical analytical workflow and main functionalities useful in validating analysis results.","lang":"eng"}],"article_type":"original","publication_status":"published","oa_version":"Published Version","external_id":{"isi":["001190689800001"],"pmid":["38484020"]},"day":"14","OA_place":"publisher","has_accepted_license":"1","month":"03","author":[{"first_name":"Chaitanya","last_name":"Chintaluri","id":"BA06AFEE-A4BA-11EA-AE5C-14673DDC885E","full_name":"Chintaluri, Chaitanya","orcid":"0000-0003-4252-1608"},{"first_name":"Marta","last_name":"Bejtka","full_name":"Bejtka, Marta"},{"last_name":"Sredniawa","first_name":"Wladyslaw","full_name":"Sredniawa, Wladyslaw"},{"first_name":"Michal","last_name":"Czerwinski","full_name":"Czerwinski, Michal"},{"full_name":"Dzik, Jakub M.","first_name":"Jakub M.","last_name":"Dzik"},{"full_name":"Jedrzejewska-Szmek, Joanna","first_name":"Joanna","last_name":"Jedrzejewska-Szmek"},{"last_name":"Wojciki","first_name":"Daniel K.","full_name":"Wojciki, Daniel K."}],"date_created":"2024-03-24T23:00:59Z","doi":"10.1371/journal.pcbi.1011941","intvolume":"        20","type":"journal_article","file":[{"file_size":2540277,"access_level":"open_access","content_type":"application/pdf","file_id":"19897","relation":"main_file","success":1,"checksum":"c09718d0d09614642d877d0716ce32e8","date_created":"2025-06-25T05:47:36Z","file_name":"2024_PLoSCompBio_Chintaluri.pdf","creator":"dernst","date_updated":"2025-06-25T05:47:36Z"}],"_id":"15169","publisher":"Public Library of Science"},{"date_published":"2024-04-19T00:00:00Z","year":"2024","oa":1,"abstract":[{"text":"Efficient utilization of large-scale biobank data is crucial for inferring the genetic basis of disease and predicting health outcomes from the DNA. Yet we lack efficient, accurate methods that scale to data where electronic health records are linked to whole genome sequence information. To address this issue, our paper develops a new algorithmic paradigm based on Approximate Message Passing (AMP), which is specifically tailored for genomic prediction and association testing. Our method yields comparable out-of-sample prediction accuracy to the state of the art on UK Biobank traits, whilst dramatically improving computational complexity, with a 8x-speed up in the run time. In addition, AMP theory provides a joint association testing framework, which outperforms the currently used REGENIE method, in roughly a third of the compute time. This first, truly large-scale application of the AMP framework lays the foundations for a far wider range of statistical analyses for hundreds of millions of variables measured on millions of people.","lang":"eng"}],"acknowledged_ssus":[{"_id":"ScienComp"}],"publication_status":"published","day":"19","OA_place":"repository","oa_version":"Submitted Version","external_id":{"isi":["001396233806078"]},"month":"04","project":[{"_id":"059876FA-7A3F-11EA-A408-12923DDC885E","name":"Prix Lopez-Loretta 2019 - Marco Mondelli"},{"name":"Improving estimation and prediction of common complex disease risk","_id":"9B8D11D6-BA93-11EA-9121-9846C619BF3A","grant_number":"PCEGP3_181181"}],"doi":"10.1109/ICASSP48485.2024.10447198","date_created":"2024-06-16T22:01:07Z","author":[{"first_name":"Al","last_name":"Depope","full_name":"Depope, Al","id":"0b77531d-dbcd-11ea-9d1d-a8eee0bf3830"},{"first_name":"Marco","last_name":"Mondelli","full_name":"Mondelli, Marco","id":"27EB676C-8706-11E9-9510-7717E6697425","orcid":"0000-0002-3242-7020"},{"full_name":"Robinson, Matthew Richard","id":"E5D42276-F5DA-11E9-8E24-6303E6697425","orcid":"0000-0001-8982-8813","first_name":"Matthew Richard","last_name":"Robinson"}],"type":"conference","publisher":"IEEE","main_file_link":[{"open_access":"1","url":"https://openreview.net/forum?id=aQYCDxfZV0"}],"_id":"17147","status":"public","isi":1,"scopus_import":"1","page":"13151-13155","citation":{"ama":"Depope A, Mondelli M, Robinson MR. Inference of genetic effects via approximate message passing. In: <i>2024 IEEE International Conference on Acoustics, Speech, and Signal Processing</i>. IEEE; 2024:13151-13155. doi:<a href=\"https://doi.org/10.1109/ICASSP48485.2024.10447198\">10.1109/ICASSP48485.2024.10447198</a>","apa":"Depope, A., Mondelli, M., &#38; Robinson, M. R. (2024). Inference of genetic effects via approximate message passing. In <i>2024 IEEE International Conference on Acoustics, Speech, and Signal Processing</i> (pp. 13151–13155). Seoul, Korea: IEEE. <a href=\"https://doi.org/10.1109/ICASSP48485.2024.10447198\">https://doi.org/10.1109/ICASSP48485.2024.10447198</a>","ieee":"A. Depope, M. Mondelli, and M. R. Robinson, “Inference of genetic effects via approximate message passing,” in <i>2024 IEEE International Conference on Acoustics, Speech, and Signal Processing</i>, Seoul, Korea, 2024, pp. 13151–13155.","chicago":"Depope, Al, Marco Mondelli, and Matthew Richard Robinson. “Inference of Genetic Effects via Approximate Message Passing.” In <i>2024 IEEE International Conference on Acoustics, Speech, and Signal Processing</i>, 13151–55. IEEE, 2024. <a href=\"https://doi.org/10.1109/ICASSP48485.2024.10447198\">https://doi.org/10.1109/ICASSP48485.2024.10447198</a>.","ista":"Depope A, Mondelli M, Robinson MR. 2024. Inference of genetic effects via approximate message passing. 2024 IEEE International Conference on Acoustics, Speech, and Signal Processing. ICASSP: International Conference on Acoustics, Speech and Signal Processing, 13151–13155.","mla":"Depope, Al, et al. “Inference of Genetic Effects via Approximate Message Passing.” <i>2024 IEEE International Conference on Acoustics, Speech, and Signal Processing</i>, IEEE, 2024, pp. 13151–55, doi:<a href=\"https://doi.org/10.1109/ICASSP48485.2024.10447198\">10.1109/ICASSP48485.2024.10447198</a>.","short":"A. Depope, M. Mondelli, M.R. Robinson, in:, 2024 IEEE International Conference on Acoustics, Speech, and Signal Processing, IEEE, 2024, pp. 13151–13155."},"publication":"2024 IEEE International Conference on Acoustics, Speech, and Signal Processing","corr_author":"1","department":[{"_id":"MaMo"},{"_id":"MaRo"}],"date_updated":"2026-07-13T14:57:55Z","acknowledgement":"This work was supported by a Lopez-Loreta Prize to MM, an SNSF Eccellenza Grant to MRR (PCEGP3-181181), and core funding from ISTA. The authors thank Philip Schniter, Matthew Stephens and Pragya Sur for valuable suggestions on an early version of the work. The authors acknowledge the participants and investigators of the UK Biobank study. High-performance\r\ncomputing was supported by the Scientific Service Units (SSU) of IST Austria through resources provided by Scientific Computing (SciComp).","publication_identifier":{"isbn":["9798350344851"],"issn":["1520-6149"]},"title":"Inference of genetic effects via approximate message passing","article_processing_charge":"No","quality_controlled":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"conference":{"name":"ICASSP: International Conference on Acoustics, Speech and Signal Processing","location":"Seoul, Korea","end_date":"2024-04-19","start_date":"2024-04-14"},"OA_type":"green"},{"main_file_link":[{"url":"https://doi.org/10.48550/arXiv.2105.02383","open_access":"1"}],"publisher":"Springer Nature","_id":"22179","intvolume":"       263","type":"journal_article","doi":"10.1007/s11856-024-2624-y","date_created":"2026-06-29T10:59:02Z","author":[{"full_name":"Fox, Jacob","last_name":"Fox","first_name":"Jacob"},{"last_name":"He","first_name":"Xiaoyu","full_name":"He, Xiaoyu"},{"first_name":"Yuval","last_name":"Wigderson","id":"2d0023a0-1567-11f0-833d-d5c1e476d4b5","full_name":"Wigderson, Yuval"}],"extern":"1","month":"10","day":"01","OA_place":"repository","oa_version":"Preprint","external_id":{"arxiv":["2105.02383"]},"abstract":[{"text":"Burr and Erd˝os in 1975 conjectured, and Chv´atal, R¨odl, Szemer´edi and\r\nTrotter later proved, that the Ramsey number of any bounded degree\r\ngraph is linear in the number of vertices. In this paper, we disprove\r\nthe natural directed analogue of the Burr–Erd˝os conjecture, answering a\r\nquestion of Buci´c, Letzter, and Sudakov. If H is an acyclic digraph, the\r\noriented Ramsey number of H, denoted −→r1(H), is the least N such that\r\nevery tournament on N vertices contains a copy of H. We show that for\r\nany Δ ≥ 2 and any sufficiently large n, there exists an acyclic digraph H\r\nwith n vertices and maximum degree Δ such that\r\n−→r1(H) ≥ nΩ(Δ2/3/ log5/3 Δ).\r\nThis proves that −→r1(H) is not always linear in the number of vertices for\r\nbounded-degree H. On the other hand, we show that −→r1(H) is nearly linear\r\nin the number of vertices for typical bounded-degree acyclic digraphs H,\r\nand obtain linear or nearly linear bounds for several natural families of\r\nbounded-degree acyclic digraphs.\r\nFor multiple colors, we prove a quasi-polynomial upper bound −→rk(H)=\r\n2(log n)Ok(1) for all bounded-degree acyclic digraphs H on n vertices, where −→rk(H) is the least N such that every k-edge-colored tournament on N\r\nvertices contains a monochromatic copy of H. For k ≥ 2 and n ≥ 4, we\r\nexhibit an acyclic digraph H with n vertices and maximum degree 3 such\r\nthat −→rk(H) ≥ nΩ(log n/ log log n), showing that these Ramsey numbers can\r\ngrow faster than any polynomial in the number of vertices.","lang":"eng"}],"article_type":"original","publication_status":"published","date_published":"2024-10-01T00:00:00Z","volume":263,"oa":1,"year":"2024","arxiv":1,"OA_type":"green","quality_controlled":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"article_processing_charge":"No","date_updated":"2026-07-14T09:08:32Z","publication_identifier":{"eissn":["1565-8511"],"issn":["0021-2172"]},"title":"Ramsey numbers of sparse digraphs","issue":"1","scopus_import":"1","citation":{"chicago":"Fox, Jacob, Xiaoyu He, and Yuval Wigderson. “Ramsey Numbers of Sparse Digraphs.” <i>Israel Journal of Mathematics</i>. Springer Nature, 2024. <a href=\"https://doi.org/10.1007/s11856-024-2624-y\">https://doi.org/10.1007/s11856-024-2624-y</a>.","mla":"Fox, Jacob, et al. “Ramsey Numbers of Sparse Digraphs.” <i>Israel Journal of Mathematics</i>, vol. 263, no. 1, Springer Nature, 2024, pp. 1–48, doi:<a href=\"https://doi.org/10.1007/s11856-024-2624-y\">10.1007/s11856-024-2624-y</a>.","ista":"Fox J, He X, Wigderson Y. 2024. Ramsey numbers of sparse digraphs. Israel Journal of Mathematics. 263(1), 1–48.","short":"J. Fox, X. He, Y. Wigderson, Israel Journal of Mathematics 263 (2024) 1–48.","ama":"Fox J, He X, Wigderson Y. Ramsey numbers of sparse digraphs. <i>Israel Journal of Mathematics</i>. 2024;263(1):1-48. doi:<a href=\"https://doi.org/10.1007/s11856-024-2624-y\">10.1007/s11856-024-2624-y</a>","apa":"Fox, J., He, X., &#38; Wigderson, Y. (2024). Ramsey numbers of sparse digraphs. <i>Israel Journal of Mathematics</i>. Springer Nature. <a href=\"https://doi.org/10.1007/s11856-024-2624-y\">https://doi.org/10.1007/s11856-024-2624-y</a>","ieee":"J. Fox, X. He, and Y. Wigderson, “Ramsey numbers of sparse digraphs,” <i>Israel Journal of Mathematics</i>, vol. 263, no. 1. Springer Nature, pp. 1–48, 2024."},"page":"1-48","publication":"Israel Journal of Mathematics","status":"public"}]