[{"date_updated":"2026-05-17T22:31:16Z","intvolume":" 3","pubrep_id":"1056","has_accepted_license":"1","abstract":[{"lang":"eng","text":"There is a huge gap between the speeds of modern caches and main memories, and therefore cache misses account for a considerable loss of efficiency in programs. The predominant technique to address this issue has been Data Packing: data elements that are frequently accessed within time proximity are packed into the same cache block, thereby minimizing accesses to the main memory. We consider the algorithmic problem of Data Packing on a two-level memory system. Given a reference sequence R of accesses to data elements, the task is to partition the elements into cache blocks such that the number of cache misses on R is minimized. The problem is notoriously difficult: it is NP-hard even when the cache has size 1, and is hard to approximate for any cache size larger than 4. Therefore, all existing techniques for Data Packing are based on heuristics and lack theoretical guarantees. In this work, we present the first positive theoretical results for Data Packing, along with new and stronger negative results. We consider the problem under the lens of the underlying access hypergraphs, which are hypergraphs of affinities between the data elements, where the order of an access hypergraph corresponds to the size of the affinity group. We study the problem parameterized by the treewidth of access hypergraphs, which is a standard notion in graph theory to measure the closeness of a graph to a tree. Our main results are as follows: We show there is a number q* depending on the cache parameters such that (a) if the access hypergraph of order q* has constant treewidth, then there is a linear-time algorithm for Data Packing; (b)the Data Packing problem remains NP-hard even if the access hypergraph of order q*-1 has constant treewidth. Thus, we establish a fine-grained dichotomy depending on a single parameter, namely, the highest order among access hypegraphs that have constant treewidth; and establish the optimal value q* of this parameter. Finally, we present an experimental evaluation of a prototype implementation of our algorithm. Our results demonstrate that, in practice, access hypergraphs of many commonly-used algorithms have small treewidth. We compare our approach with several state-of-the-art heuristic-based algorithms and show that our algorithm leads to significantly fewer cache-misses. "}],"citation":{"ieee":"K. Chatterjee, A. K. Goharshady, N. Okati, and A. Pavlogiannis, “Efficient parameterized algorithms for data packing,” Proceedings of the ACM on Programming Languages, vol. 3, no. POPL. ACM, 2019.","mla":"Chatterjee, Krishnendu, et al. “Efficient Parameterized Algorithms for Data Packing.” Proceedings of the ACM on Programming Languages, vol. 3, no. POPL, 53, ACM, 2019, doi:10.1145/3290366.","short":"K. Chatterjee, A.K. Goharshady, N. Okati, A. Pavlogiannis, Proceedings of the ACM on Programming Languages 3 (2019).","apa":"Chatterjee, K., Goharshady, A. K., Okati, N., & Pavlogiannis, A. (2019). Efficient parameterized algorithms for data packing. Proceedings of the ACM on Programming Languages. ACM. https://doi.org/10.1145/3290366","ama":"Chatterjee K, Goharshady AK, Okati N, Pavlogiannis A. Efficient parameterized algorithms for data packing. Proceedings of the ACM on Programming Languages. 2019;3(POPL). doi:10.1145/3290366","chicago":"Chatterjee, Krishnendu, Amir Kafshdar Goharshady, Nastaran Okati, and Andreas Pavlogiannis. “Efficient Parameterized Algorithms for Data Packing.” Proceedings of the ACM on Programming Languages. ACM, 2019. https://doi.org/10.1145/3290366.","ista":"Chatterjee K, Goharshady AK, Okati N, Pavlogiannis A. 2019. Efficient parameterized algorithms for data packing. Proceedings of the ACM on Programming Languages. 3(POPL), 53."},"tmp":{"short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"related_material":{"record":[{"relation":"dissertation_contains","status":"public","id":"8934"}]},"date_published":"2019-01-01T00:00:00Z","file":[{"date_updated":"2020-07-14T12:47:29Z","creator":"dernst","access_level":"open_access","date_created":"2019-05-06T12:23:11Z","relation":"main_file","checksum":"c157752f96877b36685ad7063ada4524","file_name":"2019_ACM_POPL_Chatterjee.pdf","file_id":"6381","file_size":1294962,"content_type":"application/pdf"}],"acknowledgement":"The research was partially supported by Vienna Science and Technology Fund (WWTF) Project ICT15-003, Austrian Science Fund (FWF) NFN Grant No S11407-N23 (RiSE/SHiNE), ERC\r\nStarting Grant (279307: Graph Games), and the IBM PhD Fellowship program.","volume":3,"ec_funded":1,"article_number":"53","ddc":["004"],"month":"01","issue":"POPL","publication":"Proceedings of the ACM on Programming Languages","status":"public","author":[{"orcid":"0000-0002-4561-241X","last_name":"Chatterjee","first_name":"Krishnendu","full_name":"Chatterjee, Krishnendu","id":"2E5DCA20-F248-11E8-B48F-1D18A9856A87"},{"full_name":"Goharshady, Amir Kafshdar","id":"391365CE-F248-11E8-B48F-1D18A9856A87","last_name":"Goharshady","orcid":"0000-0003-1702-6584","first_name":"Amir Kafshdar"},{"full_name":"Okati, Nastaran","first_name":"Nastaran","last_name":"Okati"},{"id":"49704004-F248-11E8-B48F-1D18A9856A87","full_name":"Pavlogiannis, Andreas","last_name":"Pavlogiannis","orcid":"0000-0002-8943-0722","first_name":"Andreas"}],"date_created":"2019-05-06T12:18:17Z","project":[{"name":"Efficient Algorithms for Computer Aided Verification","_id":"25892FC0-B435-11E9-9278-68D0E5697425","grant_number":"ICT15-003"},{"grant_number":"S 11407_N23","_id":"25832EC2-B435-11E9-9278-68D0E5697425","name":"Rigorous Systems Engineering","call_identifier":"FWF"},{"call_identifier":"FP7","name":"Quantitative Graph Games: Theory and Applications","_id":"2581B60A-B435-11E9-9278-68D0E5697425","grant_number":"279307"}],"quality_controlled":"1","doi":"10.1145/3290366","_id":"6380","oa_version":"Published Version","scopus_import":"1","article_type":"original","file_date_updated":"2020-07-14T12:47:29Z","language":[{"iso":"eng"}],"OA_place":"publisher","publication_identifier":{"issn":["2475-1421"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","article_processing_charge":"Yes (in subscription journal)","title":"Efficient parameterized algorithms for data packing","type":"journal_article","day":"01","oa":1,"OA_type":"hybrid","year":"2019","publication_status":"published","publisher":"ACM","department":[{"_id":"KrCh"}]},{"month":"05","ec_funded":1,"article_number":"8751326","status":"public","author":[{"id":"2E5DCA20-F248-11E8-B48F-1D18A9856A87","full_name":"Chatterjee, Krishnendu","first_name":"Krishnendu","last_name":"Chatterjee","orcid":"0000-0002-4561-241X"},{"full_name":"Goharshady, Amir Kafshdar","id":"391365CE-F248-11E8-B48F-1D18A9856A87","orcid":"0000-0003-1702-6584","last_name":"Goharshady","first_name":"Amir Kafshdar"},{"full_name":"Pourdamghani, Arash","first_name":"Arash","last_name":"Pourdamghani"}],"publication":"IEEE International Conference on Blockchain and Cryptocurrency","date_updated":"2026-05-17T22:31:16Z","date_published":"2019-05-01T00:00:00Z","related_material":{"record":[{"id":"8934","relation":"dissertation_contains","status":"public"}]},"citation":{"short":"K. Chatterjee, A.K. Goharshady, A. Pourdamghani, in:, IEEE International Conference on Blockchain and Cryptocurrency, IEEE, 2019.","mla":"Chatterjee, Krishnendu, et al. “Probabilistic Smart Contracts: Secure Randomness on the Blockchain.” IEEE International Conference on Blockchain and Cryptocurrency, 8751326, IEEE, 2019, doi:10.1109/BLOC.2019.8751326.","ieee":"K. Chatterjee, A. K. Goharshady, and A. Pourdamghani, “Probabilistic smart contracts: Secure randomness on the blockchain,” in IEEE International Conference on Blockchain and Cryptocurrency, Seoul, Korea, 2019.","apa":"Chatterjee, K., Goharshady, A. K., & Pourdamghani, A. (2019). Probabilistic smart contracts: Secure randomness on the blockchain. In IEEE International Conference on Blockchain and Cryptocurrency. Seoul, Korea: IEEE. https://doi.org/10.1109/BLOC.2019.8751326","ama":"Chatterjee K, Goharshady AK, Pourdamghani A. Probabilistic smart contracts: Secure randomness on the blockchain. In: IEEE International Conference on Blockchain and Cryptocurrency. IEEE; 2019. doi:10.1109/BLOC.2019.8751326","chicago":"Chatterjee, Krishnendu, Amir Kafshdar Goharshady, and Arash Pourdamghani. “Probabilistic Smart Contracts: Secure Randomness on the Blockchain.” In IEEE International Conference on Blockchain and Cryptocurrency. IEEE, 2019. https://doi.org/10.1109/BLOC.2019.8751326.","ista":"Chatterjee K, Goharshady AK, Pourdamghani A. 2019. Probabilistic smart contracts: Secure randomness on the blockchain. IEEE International Conference on Blockchain and Cryptocurrency. IEEE International Conference on Blockchain and Cryptocurrency, 8751326."},"abstract":[{"lang":"eng","text":"In today's programmable blockchains, smart contracts are limited to being deterministic and non-probabilistic. This lack of randomness is a consequential limitation, given that a wide variety of real-world financial contracts, such as casino games and lotteries, depend entirely on randomness. As a result, several ad-hoc random number generation approaches have been developed to be used in smart contracts. These include ideas such as using an oracle or relying on the block hash. However, these approaches are manipulatable, i.e. their output can be tampered with by parties who might not be neutral, such as the owner of the oracle or the miners.We propose a novel game-theoretic approach for generating provably unmanipulatable pseudorandom numbers on the blockchain. Our approach allows smart contracts to access a trustworthy source of randomness that does not rely on potentially compromised miners or oracles, hence enabling the creation of a new generation of smart contracts that are not limited to being non-probabilistic and can be drawn from the much more general class of probabilistic programs."}],"conference":{"name":"IEEE International Conference on Blockchain and Cryptocurrency","location":"Seoul, Korea","start_date":"2019-05-14","end_date":"2019-05-17"},"article_processing_charge":"No","title":"Probabilistic smart contracts: Secure randomness on the blockchain","arxiv":1,"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","main_file_link":[{"url":"https://arxiv.org/abs/1902.07986","open_access":"1"}],"department":[{"_id":"KrCh"}],"publication_status":"published","year":"2019","publisher":"IEEE","day":"01","external_id":{"isi":["000491257000076"],"arxiv":["1902.07986"]},"oa":1,"type":"conference","quality_controlled":"1","project":[{"grant_number":"ICT15-003","_id":"25892FC0-B435-11E9-9278-68D0E5697425","name":"Efficient Algorithms for Computer Aided Verification"},{"name":"Rigorous Systems Engineering","_id":"25832EC2-B435-11E9-9278-68D0E5697425","call_identifier":"FWF","grant_number":"S 11407_N23"},{"_id":"2581B60A-B435-11E9-9278-68D0E5697425","name":"Quantitative Graph Games: Theory and Applications","call_identifier":"FP7","grant_number":"279307"},{"name":"Quantitative Game-theoretic Analysis of Blockchain Applications and Smart Contracts","_id":"266EEEC0-B435-11E9-9278-68D0E5697425"},{"name":"Quantitative Analysis of Probabilistic Systems with a focus on Crypto-Currencies","_id":"267066CE-B435-11E9-9278-68D0E5697425"}],"isi":1,"date_created":"2019-02-26T09:03:15Z","language":[{"iso":"eng"}],"_id":"6056","scopus_import":"1","oa_version":"Preprint","doi":"10.1109/BLOC.2019.8751326"},{"date_created":"2019-07-11T12:00:32Z","isi":1,"project":[{"grant_number":"282300","_id":"25716A02-B435-11E9-9278-68D0E5697425","name":"Polarity and subcellular dynamics in plants","call_identifier":"FP7"},{"grant_number":"665385","name":"International IST Doctoral Program","_id":"2564DBCA-B435-11E9-9278-68D0E5697425","call_identifier":"H2020"},{"_id":"B67AFEDC-15C9-11EA-A837-991A96BB2854","name":"IST Austria Open Access Fund"}],"quality_controlled":"1","doi":"10.3390/ijms20133337","_id":"6627","oa_version":"Published Version","scopus_import":"1","article_type":"original","file_date_updated":"2020-07-14T12:47:34Z","language":[{"iso":"eng"}],"publication_identifier":{"eissn":["1422-0067"]},"user_id":"4359f0d1-fa6c-11eb-b949-802e58b17ae8","article_processing_charge":"Yes","title":"Reorientation of cortical microtubule arrays in the hypocotyl of arabidopsis thaliana is induced by the cell growth process and independent of auxin signaling","type":"journal_article","pmid":1,"day":"07","external_id":{"isi":["000477041100221"],"pmid":["31284661"]},"oa":1,"year":"2019","publication_status":"published","publisher":"MDPI","department":[{"_id":"JiFr"}],"date_updated":"2026-05-17T22:31:18Z","intvolume":" 20","has_accepted_license":"1","corr_author":"1","abstract":[{"text":"Cortical microtubule arrays in elongating epidermal cells in both the root and stem of plants have the propensity of dynamic reorientations that are correlated with the activation or inhibition of growth. Factors regulating plant growth, among them the hormone auxin, have been recognized as regulators of microtubule array orientations. Some previous work in the field has aimed at elucidating the causal relationship between cell growth, the signaling of auxin or other growth-regulating factors, and microtubule array reorientations, with various conclusions. Here, we revisit this problem of causality with a comprehensive set of experiments in Arabidopsis thaliana, using the now available pharmacological and genetic tools. We use isolated, auxin-depleted hypocotyls, an experimental system allowing for full control of both growth and auxin signaling. We demonstrate that reorientation of microtubules is not directly triggered by an auxin signal during growth activation. Instead, reorientation is triggered by the activation of the growth process itself and is auxin-independent in its nature. We discuss these findings in the context of previous relevant work, including that on the mechanical regulation of microtubule array orientation.","lang":"eng"}],"citation":{"ista":"Adamowski M, Li L, Friml J. 2019. Reorientation of cortical microtubule arrays in the hypocotyl of arabidopsis thaliana is induced by the cell growth process and independent of auxin signaling. International Journal of Molecular Sciences. 20(13), 3337.","ama":"Adamowski M, Li L, Friml J. Reorientation of cortical microtubule arrays in the hypocotyl of arabidopsis thaliana is induced by the cell growth process and independent of auxin signaling. International Journal of Molecular Sciences. 2019;20(13). doi:10.3390/ijms20133337","chicago":"Adamowski, Maciek, Lanxin Li, and Jiří Friml. “Reorientation of Cortical Microtubule Arrays in the Hypocotyl of Arabidopsis Thaliana Is Induced by the Cell Growth Process and Independent of Auxin Signaling.” International Journal of Molecular Sciences. MDPI, 2019. https://doi.org/10.3390/ijms20133337.","ieee":"M. Adamowski, L. Li, and J. Friml, “Reorientation of cortical microtubule arrays in the hypocotyl of arabidopsis thaliana is induced by the cell growth process and independent of auxin signaling,” International Journal of Molecular Sciences, vol. 20, no. 13. MDPI, 2019.","short":"M. Adamowski, L. Li, J. Friml, International Journal of Molecular Sciences 20 (2019).","mla":"Adamowski, Maciek, et al. “Reorientation of Cortical Microtubule Arrays in the Hypocotyl of Arabidopsis Thaliana Is Induced by the Cell Growth Process and Independent of Auxin Signaling.” International Journal of Molecular Sciences, vol. 20, no. 13, 3337, MDPI, 2019, doi:10.3390/ijms20133337.","apa":"Adamowski, M., Li, L., & Friml, J. (2019). Reorientation of cortical microtubule arrays in the hypocotyl of arabidopsis thaliana is induced by the cell growth process and independent of auxin signaling. International Journal of Molecular Sciences. MDPI. https://doi.org/10.3390/ijms20133337"},"related_material":{"record":[{"status":"public","relation":"dissertation_contains","id":"10083"}]},"tmp":{"short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"date_published":"2019-07-07T00:00:00Z","file":[{"creator":"dernst","date_updated":"2020-07-14T12:47:34Z","access_level":"open_access","date_created":"2019-07-17T06:17:15Z","relation":"main_file","checksum":"dd9d1cbb933a72ceb666c9667890ac51","file_name":"2019_JournalMolecularScience_Adamowski.pdf","file_id":"6645","file_size":3330291,"content_type":"application/pdf"}],"ec_funded":1,"volume":20,"ddc":["580"],"article_number":"3337","month":"07","publication":"International Journal of Molecular Sciences","issue":"13","status":"public","author":[{"first_name":"Maciek","orcid":"0000-0001-6463-5257","last_name":"Adamowski","full_name":"Adamowski, Maciek","id":"45F536D2-F248-11E8-B48F-1D18A9856A87"},{"id":"367EF8FA-F248-11E8-B48F-1D18A9856A87","full_name":"Li, Lanxin","orcid":"0000-0002-5607-272X","last_name":"Li","first_name":"Lanxin"},{"first_name":"Jiří","last_name":"Friml","orcid":"0000-0002-8302-7596","id":"4159519E-F248-11E8-B48F-1D18A9856A87","full_name":"Friml, Jiří"}]},{"oa":1,"external_id":{"arxiv":["1809.05865"],"isi":["000472860000042"]},"day":"27","type":"journal_article","department":[{"_id":"JoFi"}],"main_file_link":[{"url":"https://arxiv.org/abs/1809.05865","open_access":"1"}],"publisher":"Nature Publishing Group","publication_status":"published","year":"2019","arxiv":1,"user_id":"4359f0d1-fa6c-11eb-b949-802e58b17ae8","title":"Stationary entangled radiation from micromechanical motion","article_processing_charge":"No","scopus_import":"1","oa_version":"Preprint","_id":"6609","doi":"10.1038/s41586-019-1320-2","acknowledged_ssus":[{"_id":"NanoFab"}],"language":[{"iso":"eng"}],"isi":1,"date_created":"2019-07-07T21:59:20Z","quality_controlled":"1","project":[{"grant_number":"732894","name":"Hybrid Optomechanical Technologies","_id":"257EB838-B435-11E9-9278-68D0E5697425","call_identifier":"H2020"},{"grant_number":"758053","call_identifier":"H2020","_id":"26336814-B435-11E9-9278-68D0E5697425","name":"A Fiber Optic Transceiver for Superconducting Qubits"},{"grant_number":"707438","call_identifier":"H2020","name":"Microwave-to-Optical Quantum Link: Quantum Teleportation and Quantum Illumination with cavity Optomechanics","_id":"258047B6-B435-11E9-9278-68D0E5697425"},{"_id":"2671EB66-B435-11E9-9278-68D0E5697425","name":"Coherent on-chip conversion of superconducting qubit signals from microwaves to optical frequencies"}],"publication":"Nature","author":[{"full_name":"Barzanjeh, Shabir","id":"2D25E1F6-F248-11E8-B48F-1D18A9856A87","first_name":"Shabir","orcid":"0000-0003-0415-1423","last_name":"Barzanjeh"},{"id":"2C21D6E8-F248-11E8-B48F-1D18A9856A87","full_name":"Redchenko, Elena","last_name":"Redchenko","first_name":"Elena"},{"first_name":"Matilda","last_name":"Peruzzo","orcid":"0000-0002-3415-4628","full_name":"Peruzzo, Matilda","id":"3F920B30-F248-11E8-B48F-1D18A9856A87"},{"orcid":"0000-0001-6613-1378","last_name":"Wulf","first_name":"Matthias","id":"45598606-F248-11E8-B48F-1D18A9856A87","full_name":"Wulf, Matthias"},{"full_name":"Lewis, Dylan","first_name":"Dylan","last_name":"Lewis"},{"full_name":"Arnold, Georg M","id":"3770C838-F248-11E8-B48F-1D18A9856A87","first_name":"Georg M","last_name":"Arnold","orcid":"0000-0003-1397-7876"},{"full_name":"Fink, Johannes M","id":"4B591CBA-F248-11E8-B48F-1D18A9856A87","first_name":"Johannes M","orcid":"0000-0001-8112-028X","last_name":"Fink"}],"status":"public","page":"480-483","month":"06","ec_funded":1,"volume":570,"citation":{"ista":"Barzanjeh S, Redchenko E, Peruzzo M, Wulf M, Lewis D, Arnold GM, Fink JM. 2019. Stationary entangled radiation from micromechanical motion. Nature. 570, 480–483.","chicago":"Barzanjeh, Shabir, Elena Redchenko, Matilda Peruzzo, Matthias Wulf, Dylan Lewis, Georg M Arnold, and Johannes M Fink. “Stationary Entangled Radiation from Micromechanical Motion.” Nature. Nature Publishing Group, 2019. https://doi.org/10.1038/s41586-019-1320-2.","ama":"Barzanjeh S, Redchenko E, Peruzzo M, et al. Stationary entangled radiation from micromechanical motion. Nature. 2019;570:480-483. doi:10.1038/s41586-019-1320-2","apa":"Barzanjeh, S., Redchenko, E., Peruzzo, M., Wulf, M., Lewis, D., Arnold, G. M., & Fink, J. M. (2019). Stationary entangled radiation from micromechanical motion. Nature. Nature Publishing Group. https://doi.org/10.1038/s41586-019-1320-2","ieee":"S. Barzanjeh et al., “Stationary entangled radiation from micromechanical motion,” Nature, vol. 570. Nature Publishing Group, pp. 480–483, 2019.","short":"S. Barzanjeh, E. Redchenko, M. Peruzzo, M. Wulf, D. Lewis, G.M. Arnold, J.M. Fink, Nature 570 (2019) 480–483.","mla":"Barzanjeh, Shabir, et al. “Stationary Entangled Radiation from Micromechanical Motion.” Nature, vol. 570, Nature Publishing Group, 2019, pp. 480–83, doi:10.1038/s41586-019-1320-2."},"abstract":[{"lang":"eng","text":"Mechanical systems facilitate the development of a hybrid quantum technology comprising electrical, optical, atomic and acoustic degrees of freedom1, and entanglement is essential to realize quantum-enabled devices. Continuous-variable entangled fields—known as Einstein–Podolsky–Rosen (EPR) states—are spatially separated two-mode squeezed states that can be used for quantum teleportation and quantum communication2. In the optical domain, EPR states are typically generated using nondegenerate optical amplifiers3, and at microwave frequencies Josephson circuits can serve as a nonlinear medium4,5,6. An outstanding goal is to deterministically generate and distribute entangled states with a mechanical oscillator, which requires a carefully arranged balance between excitation, cooling and dissipation in an ultralow noise environment. Here we observe stationary emission of path-entangled microwave radiation from a parametrically driven 30-micrometre-long silicon nanostring oscillator, squeezing the joint field operators of two thermal modes by 3.40 decibels below the vacuum level. The motion of this micromechanical system correlates up to 50 photons per second per hertz, giving rise to a quantum discord that is robust with respect to microwave noise7. Such generalized quantum correlations of separable states are important for quantum-enhanced detection8 and provide direct evidence of the non-classical nature of the mechanical oscillator without directly measuring its state9. This noninvasive measurement scheme allows to infer information about otherwise inaccessible objects, with potential implications for sensing, open-system dynamics and fundamental tests of quantum gravity. In the future, similar on-chip devices could be used to entangle subsystems on very different energy scales, such as microwave and optical photons."}],"date_published":"2019-06-27T00:00:00Z","related_material":{"record":[{"id":"18871","status":"public","relation":"dissertation_contains"}]},"date_updated":"2026-05-17T22:31:20Z","intvolume":" 570"},{"article_number":"A136","acknowledgement":"JM acknowledges the award of a Huygens PhD fellowship from Leiden University. MG acknowledges support from NASA grant NNX17AK58G. APA, PhD::SPACE fellow, acknowledges support from the FCT through the fellowship PD/BD/52706/2014. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 294.A-5018, 098.A-0819, 099.A-0254 and 0100.A-0213. We are grateful for the excellent data-sets from the COSMOS and UltraVISTA survey teams. This research was supported by the Munich Institute for Astro- and Particle Physics (MIAPP) of the DFG cluster of excellence “Origin and Structure of the Universe”. We thank the referee for their comments that improved the paper. We also thank Christoph Behrens, Len Cowie, Koki Kakiichi, Peter Laursen, Charlotte Mason, Eros Vanzella, Lewis Weinberger and Johannes Zabl for discussions. We have benefited from the public available programming language Python, including the numpy, matplotlib, scipy and astropy packages (Hunter 2007; Astropy Collaboration 2013), the astronomical imaging tools Swarp (Bertin 2010) and ds9 and the Topcat analysis tool (Taylor 2013).","volume":619,"month":"11","publication":"Astronomy & Astrophysics","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","first_name":"Jorryt J"},{"full_name":"Sobral, David","first_name":"David","last_name":"Sobral"},{"last_name":"Gronke","first_name":"Max","full_name":"Gronke, Max"},{"last_name":"Paulino-Afonso","first_name":"Ana","full_name":"Paulino-Afonso, Ana"},{"last_name":"Stefanon","first_name":"Mauro","full_name":"Stefanon, Mauro"},{"full_name":"Röttgering, Huub","last_name":"Röttgering","first_name":"Huub"}],"status":"public","date_updated":"2024-10-14T11:31:36Z","extern":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift / galaxies: formation / dark ages / reionization / first stars / techniques: spectroscopic / intergalactic medium"],"intvolume":" 619","citation":{"ama":"Matthee JJ, Sobral D, Gronke M, Paulino-Afonso A, Stefanon M, Röttgering H. Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly contributing to the reionisation of the universe. Astronomy & Astrophysics. 2018;619. doi:10.1051/0004-6361/201833528","chicago":"Matthee, Jorryt J, David Sobral, Max Gronke, Ana Paulino-Afonso, Mauro Stefanon, and Huub Röttgering. “Confirmation of Double Peaked Lyα Emission at z = 6.593: Witnessing a Galaxy Directly Contributing to the Reionisation of the Universe.” Astronomy & Astrophysics. EDP Sciences, 2018. https://doi.org/10.1051/0004-6361/201833528.","short":"J.J. Matthee, D. Sobral, M. Gronke, A. Paulino-Afonso, M. Stefanon, H. Röttgering, Astronomy & Astrophysics 619 (2018).","ieee":"J. J. Matthee, D. Sobral, M. Gronke, A. Paulino-Afonso, M. Stefanon, and H. Röttgering, “Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly contributing to the reionisation of the universe,” Astronomy & Astrophysics, vol. 619. EDP Sciences, 2018.","mla":"Matthee, Jorryt J., et al. “Confirmation of Double Peaked Lyα Emission at z = 6.593: Witnessing a Galaxy Directly Contributing to the Reionisation of the Universe.” Astronomy & Astrophysics, vol. 619, A136, EDP Sciences, 2018, doi:10.1051/0004-6361/201833528.","apa":"Matthee, J. J., Sobral, D., Gronke, M., Paulino-Afonso, A., Stefanon, M., & Röttgering, H. (2018). Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly contributing to the reionisation of the universe. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201833528","ista":"Matthee JJ, Sobral D, Gronke M, Paulino-Afonso A, Stefanon M, Röttgering H. 2018. Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly contributing to the reionisation of the universe. Astronomy & Astrophysics. 619, A136."},"abstract":[{"text":"Distant luminous Lyman-α emitters (LAEs) are excellent targets for spectroscopic observations of galaxies in the epoch of reionisation (EoR). We present deep high-resolution (R = 5000) VLT/X-shooter observations, along with an extensive collection of photometric data of COLA1, a proposed double peaked LAE at z = 6.6. We rule out the possibility that COLA1’s emission line is an [OII] doublet at z = 1.475 on the basis of i) the asymmetric red line-profile and flux ratio of the peaks (blue/red=0.31 ± 0.03) and ii) an unphysical [OII]/Hα ratio ([OII]/Hα > 22). We show that COLA1’s observed B-band flux is explained by a faint extended foreground LAE, for which we detect Lyα and [OIII] at z = 2.142. We thus conclude that COLA1 is a real double-peaked LAE at z = 6.593, the first discovered at z > 6. COLA1 is UV luminous (M1500 = −21.6 ± 0.3), has a high equivalent width (EW0,Lyα = 120−40+50 Å) and very compact Lyα emission (r50,Lyα = 0.33−0.04+0.07 kpc). Relatively weak inferred Hβ+[OIII] line-emission from Spitzer/IRAC indicates an extremely low metallicity of Z < 1/20 Z⊙ or reduced strength of nebular lines due to high escape of ionising photons. The small Lyα peak separation of 220 ± 20 km s−1 implies a low HI column density and an ionising photon escape fraction of ≈15 − 30%, providing the first direct evidence that such galaxies contribute actively to the reionisation of the Universe at z > 6. Based on simple estimates, we find that COLA1 could have provided just enough photons to reionise its own ≈0.3 pMpc (2.3 cMpc) bubble, allowing the blue Lyα line to be observed. However, we also discuss alternative scenarios explaining the detected double peaked nature of COLA1. Our results show that future high-resolution observations of statistical samples of double peaked LAEs at z > 5 are a promising probe of the occurrence of ionised regions around galaxies in the EoR.","lang":"eng"}],"date_published":"2018-11-19T00:00:00Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"arxiv":1,"title":"Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly contributing to the reionisation of the universe","article_processing_charge":"No","type":"journal_article","oa":1,"day":"19","external_id":{"arxiv":["1805.11621"]},"publisher":"EDP Sciences","year":"2018","publication_status":"published","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1805.11621"}],"date_created":"2022-07-06T11:14:23Z","quality_controlled":"1","doi":"10.1051/0004-6361/201833528","oa_version":"Published Version","scopus_import":"1","_id":"11508","article_type":"original","language":[{"iso":"eng"}]},{"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: haloes","galaxies: high-redshift","galaxies: star formation","cosmology: observations","large-scale structure of Universe"],"intvolume":" 478","date_updated":"2022-08-19T06:53:39Z","extern":"1","date_published":"2018-08-01T00:00:00Z","abstract":[{"text":"We investigate the clustering properties of ∼7000 H β + [O III] and [O II] narrowband-selected emitters at z ∼ 0.8–4.7 from the High-z Emission Line Survey. We find clustering lengths, r0, of 1.5–4.0 h−1 Mpc and minimum dark matter halo masses of 1010.7–12.1 M⊙ for our z = 0.8–3.2 H β + [O III] emitters and r0 ∼ 2.0–8.3 h−1 Mpc and halo masses of 1011.5–12.6 M⊙ for our z = 1.5–4.7 [O II] emitters. We find r0 to strongly increase both with increasing line luminosity and redshift. By taking into account the evolution of the characteristic line luminosity, L⋆(z), and using our model predictions of halo mass given r0, we find a strong, redshift-independent increasing trend between L/L⋆(z) and minimum halo mass. The faintest H β + [O III] emitters are found to reside in 109.5 M⊙ haloes and the brightest emitters in 1013.0 M⊙ haloes. For [O II] emitters, the faintest emitters are found in 1010.5 M⊙ haloes and the brightest emitters in 1012.6 M⊙ haloes. A redshift-independent stellar mass dependency is also observed where the halo mass increases from 1011 to 1012.5 M⊙ for stellar masses of 108.5 to 1011.5 M⊙, respectively. We investigate the interdependencies of these trends by repeating our analysis in a Lline−Mstar grid space for our most populated samples (H β + [O III] z = 0.84 and [O II] z = 1.47) and find that the line luminosity dependency is stronger than the stellar mass dependency on halo mass. For L > L⋆ emitters at all epochs, we find a relatively flat trend with halo masses of 1012.5–13 M⊙, which may be due to quenching mechanisms in massive haloes that is consistent with a transitional halo mass predicted by models.","lang":"eng"}],"citation":{"apa":"Khostovan, A. A., Sobral, D., Mobasher, B., Best, P. N., Smail, I., Matthee, J. J., … Stott, J. P. (2018). The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar mass. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/sty925","mla":"Khostovan, A. A., et al. “The Clustering of H β + [O III] and [O II] Emitters since z ∼ 5: Dependencies with Line Luminosity and Stellar Mass.” Monthly Notices of the Royal Astronomical Society, vol. 478, no. 3, Oxford University Press, 2018, pp. 2999–3015, doi:10.1093/mnras/sty925.","short":"A.A. Khostovan, D. Sobral, B. Mobasher, P.N. Best, I. Smail, J.J. Matthee, B. Darvish, H. Nayyeri, S. Hemmati, J.P. Stott, Monthly Notices of the Royal Astronomical Society 478 (2018) 2999–3015.","ieee":"A. A. Khostovan et al., “The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar mass,” Monthly Notices of the Royal Astronomical Society, vol. 478, no. 3. Oxford University Press, pp. 2999–3015, 2018.","chicago":"Khostovan, A A, D Sobral, B Mobasher, P N Best, I Smail, Jorryt J Matthee, B Darvish, H Nayyeri, S Hemmati, and J P Stott. “The Clustering of H β + [O III] and [O II] Emitters since z ∼ 5: Dependencies with Line Luminosity and Stellar Mass.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2018. https://doi.org/10.1093/mnras/sty925.","ama":"Khostovan AA, Sobral D, Mobasher B, et al. The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar mass. Monthly Notices of the Royal Astronomical Society. 2018;478(3):2999-3015. doi:10.1093/mnras/sty925","ista":"Khostovan AA, Sobral D, Mobasher B, Best PN, Smail I, Matthee JJ, Darvish B, Nayyeri H, Hemmati S, Stott JP. 2018. The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar mass. Monthly Notices of the Royal Astronomical Society. 478(3), 2999–3015."},"volume":478,"acknowledgement":"We thank the anonymous referee for their useful comments and suggestions that improved this study. AAK thanks Anahita Alavi and Irene Shivaei for useful discussion in the making of this paper. AAK acknowledges that this work was supported by NASA Headquarters under the NASA Earth and Space Science Fellowship Program – Grant NNX16AO92H. DS acknowledges financial support from the Netherlands Organization for Scientific Research (NWO) through a Veni fellowship and from Lancaster University through an Early Career Internal Grant A100679. PNB is grateful for support from STFC via grant STM001229/1. IRS acknowledges support from STFC (ST/L00075X/1), the ERC Advanced Grant DUSTYGAL (321334), and a Royal Society/Wolfson Merit award. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. BD acknowledges financial support from NASA through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G.","month":"08","page":"2999-3015","status":"public","author":[{"last_name":"Khostovan","first_name":"A A","full_name":"Khostovan, A A"},{"full_name":"Sobral, D","first_name":"D","last_name":"Sobral"},{"full_name":"Mobasher, B","first_name":"B","last_name":"Mobasher"},{"last_name":"Best","first_name":"P N","full_name":"Best, P N"},{"last_name":"Smail","first_name":"I","full_name":"Smail, I"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J"},{"full_name":"Darvish, B","last_name":"Darvish","first_name":"B"},{"full_name":"Nayyeri, H","last_name":"Nayyeri","first_name":"H"},{"full_name":"Hemmati, S","last_name":"Hemmati","first_name":"S"},{"full_name":"Stott, J P","first_name":"J P","last_name":"Stott"}],"issue":"3","publication":"Monthly Notices of the Royal Astronomical Society","quality_controlled":"1","date_created":"2022-07-08T11:48:48Z","article_type":"original","language":[{"iso":"eng"}],"doi":"10.1093/mnras/sty925","_id":"11549","scopus_import":"1","oa_version":"Published Version","article_processing_charge":"No","title":"The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar mass","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","arxiv":1,"year":"2018","publication_status":"published","publisher":"Oxford University Press","main_file_link":[{"url":"https://arxiv.org/abs/1705.01101"}],"type":"journal_article","external_id":{"arxiv":["1705.01101"]},"day":"01"},{"year":"2018","publication_status":"published","publisher":"Oxford University Press","main_file_link":[{"url":"https://arxiv.org/abs/1712.03985","open_access":"1"}],"type":"journal_article","external_id":{"arxiv":["1712.03985"]},"day":"01","oa":1,"article_processing_charge":"No","title":"Kiloparsec-scale gaseous clumps and star formation at z = 5–7","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","arxiv":1,"article_type":"original","language":[{"iso":"eng"}],"doi":"10.1093/mnras/sty1088","_id":"11555","oa_version":"Preprint","scopus_import":"1","quality_controlled":"1","date_created":"2022-07-11T08:05:42Z","status":"public","author":[{"last_name":"Carniani","first_name":"S","full_name":"Carniani, S"},{"full_name":"Maiolino, R","first_name":"R","last_name":"Maiolino"},{"full_name":"Amorin, R","first_name":"R","last_name":"Amorin"},{"first_name":"L","last_name":"Pentericci","full_name":"Pentericci, L"},{"full_name":"Pallottini, A","first_name":"A","last_name":"Pallottini"},{"full_name":"Ferrara, A","first_name":"A","last_name":"Ferrara"},{"last_name":"Willott","first_name":"C J","full_name":"Willott, C J"},{"first_name":"R","last_name":"Smit","full_name":"Smit, R"},{"first_name":"Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"full_name":"Sobral, D","last_name":"Sobral","first_name":"D"},{"full_name":"Santini, P","first_name":"P","last_name":"Santini"},{"full_name":"Castellano, M","first_name":"M","last_name":"Castellano"},{"full_name":"De Barros, S","first_name":"S","last_name":"De Barros"},{"full_name":"Fontana, A","last_name":"Fontana","first_name":"A"},{"first_name":"A","last_name":"Grazian","full_name":"Grazian, A"},{"last_name":"Guaita","first_name":"L","full_name":"Guaita, L"}],"publication":"Monthly Notices of the Royal Astronomical Society","issue":"1","acknowledgement":"This paper makes use of the following ALMA data:\r\nADS/JAO.ALMA#2012.1.00719.S, ADS/JAO.ALMA#2012.A.00040.S,\r\nADS/JAO.ALMA#2013.A.00433.S, ADS/JAO.ALMA#2011.0.00115.S,\r\nADS/JAO.ALMA#2012.1.00033.S, ADS/JAO.ALMA#2012.1.00523.S,\r\nADS/JAO.ALMA#2013.1.00815.S, ADS/JAO.ALMA#2015.1.00834.S.,\r\nADS/JAO.ALMA#2015.1.01105.S, AND ADS/JAO.ALMA#2016.1.01240.S\r\nwhich can be retrieved from the ALMA data archive:\r\nhttps://almascience.eso.org/ alma-data/archive. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. We are grateful to G. Jones to for providing his [C II] flux maps. RM and SC acknowledge support by the Science and Technology Facilities Council (STFC). RM acknowledges ERC Advanced Grant 695671 ‘QUENCH’. AF acknowledges support from the ERC Advanced Grant INTERSTELLAR H2020/740120.","volume":478,"month":"07","page":"1170-1184","date_published":"2018-07-01T00:00:00Z","citation":{"ista":"Carniani S, Maiolino R, Amorin R, Pentericci L, Pallottini A, Ferrara A, Willott CJ, Smit R, Matthee JJ, Sobral D, Santini P, Castellano M, De Barros S, Fontana A, Grazian A, Guaita L. 2018. Kiloparsec-scale gaseous clumps and star formation at z = 5–7. Monthly Notices of the Royal Astronomical Society. 478(1), 1170–1184.","ama":"Carniani S, Maiolino R, Amorin R, et al. Kiloparsec-scale gaseous clumps and star formation at z = 5–7. Monthly Notices of the Royal Astronomical Society. 2018;478(1):1170-1184. doi:10.1093/mnras/sty1088","chicago":"Carniani, S, R Maiolino, R Amorin, L Pentericci, A Pallottini, A Ferrara, C J Willott, et al. “Kiloparsec-Scale Gaseous Clumps and Star Formation at z = 5–7.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2018. https://doi.org/10.1093/mnras/sty1088.","short":"S. Carniani, R. Maiolino, R. Amorin, L. Pentericci, A. Pallottini, A. Ferrara, C.J. Willott, R. Smit, J.J. Matthee, D. Sobral, P. Santini, M. Castellano, S. De Barros, A. Fontana, A. Grazian, L. Guaita, Monthly Notices of the Royal Astronomical Society 478 (2018) 1170–1184.","mla":"Carniani, S., et al. “Kiloparsec-Scale Gaseous Clumps and Star Formation at z = 5–7.” Monthly Notices of the Royal Astronomical Society, vol. 478, no. 1, Oxford University Press, 2018, pp. 1170–84, doi:10.1093/mnras/sty1088.","ieee":"S. Carniani et al., “Kiloparsec-scale gaseous clumps and star formation at z = 5–7,” Monthly Notices of the Royal Astronomical Society, vol. 478, no. 1. Oxford University Press, pp. 1170–1184, 2018.","apa":"Carniani, S., Maiolino, R., Amorin, R., Pentericci, L., Pallottini, A., Ferrara, A., … Guaita, L. (2018). Kiloparsec-scale gaseous clumps and star formation at z = 5–7. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/sty1088"},"abstract":[{"text":"We investigate the morphology of the [C II] emission in a sample of ‘normal’ star-forming galaxies at 5 < z < 7.2 in relation to their UV (rest-frame) counterpart. We use new Atacama Large Millimetre/submillimetre Array (ALMA) observations of galaxies at z ∼ 6–7, as well as a careful re-analysis of archival ALMA data. In total 29 galaxies were analysed, 21 of which are detected in [C II]. For several of the latter the [C II] emission breaks into multiple components. Only a fraction of these [C II] components, if any, is associated with the primary UV systems, while the bulk of the [C II] emission is associated either with fainter UV components, or not associated with any UV counterpart at the current limits. By taking into account the presence of all these components, we find that the L[CII]–SFR (star formation rate) relation at early epochs is fully consistent with the local relation, but it has a dispersion of 0.48 ± 0.07 dex, which is about two times larger than observed locally. We also find that the deviation from the local L[CII]–SFR relation has a weak anticorrelation with the EW(Ly α). The morphological analysis also reveals that [C II] emission is generally much more extended than the UV emission. As a consequence, these primordial galaxies are characterized by a [C II] surface brightness generally much lower than expected from the local Σ[CII]−ΣSFR relation. These properties are likely a consequence of a combination of different effects, namely gas metallicity, [C II] emission from obscured star-forming regions, strong variations of the ionization parameter, and circumgalactic gas in accretion or ejected by these primeval galaxies.","lang":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","galaxies: ISM","galaxies: formation"],"intvolume":" 478","extern":"1","date_updated":"2022-08-19T06:58:06Z"},{"quality_controlled":"1","date_created":"2022-07-12T07:18:02Z","language":[{"iso":"eng"}],"article_type":"original","_id":"11557","scopus_import":"1","oa_version":"Preprint","doi":"10.1093/mnras/sty782","article_processing_charge":"No","title":"The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN","arxiv":1,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1802.10102"}],"year":"2018","publication_status":"published","publisher":"Oxford University Press","day":"01","external_id":{"arxiv":["1802.10102"]},"oa":1,"type":"journal_article","intvolume":" 477","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: active","galaxies: evolution","galaxies: high-redshift","galaxies: ISM","galaxies: starburst","cosmology: observations"],"date_updated":"2022-08-19T07:01:08Z","extern":"1","date_published":"2018-06-01T00:00:00Z","abstract":[{"text":"Deep narrow-band surveys have revealed a large population of faint Ly α emitters (LAEs) in the distant Universe, but relatively little is known about the most luminous sources (LLyα≳1042.7 erg s−1; LLyα≳L∗Lyα). Here we present the spectroscopic follow-up of 21 luminous LAEs at z ∼ 2–3 found with panoramic narrow-band surveys over five independent extragalactic fields (≈4 × 106 Mpc3 surveyed at z ∼ 2.2 and z ∼ 3.1). We use WHT/ISIS, Keck/DEIMOS, and VLT/X-SHOOTER to study these sources using high ionization UV lines. Luminous LAEs at z ∼ 2–3 have blue UV slopes (β=−2.0+0.3−0.1) and high Ly α escape fractions (50+20−15 per cent) and span five orders of magnitude in UV luminosity (MUV ≈ −19 to −24). Many (70 per cent) show at least one high ionization rest-frame UV line such as C IV, N V, C III], He II or O III], typically blue-shifted by ≈100–200 km s−1 relative to Ly α. Their Ly α profiles reveal a wide variety of shapes, including significant blue-shifted components and widths from 200 to 4000 km s−1. Overall, 60 ± 11 per cent appear to be active galactic nucleus (AGN) dominated, and at LLyα > 1043.3 erg s−1 and/or MUV < −21.5 virtually all LAEs are AGNs with high ionization parameters (log U = 0.6 ± 0.5) and with metallicities of ≈0.5 − 1 Z⊙. Those lacking signatures of AGNs (40 ± 11 per cent) have lower ionization parameters (logU=−3.0+1.6−0.9 and log ξion = 25.4 ± 0.2) and are apparently metal-poor sources likely powered by young, dust-poor ‘maximal’ starbursts. Our results show that luminous LAEs at z ∼ 2–3 are a diverse population and that 2×L∗Lyα and 2×M∗UV mark a sharp transition in the nature of LAEs, from star formation dominated to AGN dominated.","lang":"eng"}],"citation":{"ista":"Sobral D, Matthee JJ, Darvish B, Smail I, Best PN, Alegre L, Röttgering H, Mobasher B, Paulino-Afonso A, Stroe A, Oteo I. 2018. The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN. Monthly Notices of the Royal Astronomical Society. 477(2), 2817–2840.","mla":"Sobral, David, et al. “The Nature of Luminous Ly α Emitters at z ∼ 2–3: Maximal Dust-Poor Starbursts and Highly Ionizing AGN.” Monthly Notices of the Royal Astronomical Society, vol. 477, no. 2, Oxford University Press, 2018, pp. 2817–40, doi:10.1093/mnras/sty782.","ieee":"D. Sobral et al., “The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN,” Monthly Notices of the Royal Astronomical Society, vol. 477, no. 2. Oxford University Press, pp. 2817–2840, 2018.","short":"D. Sobral, J.J. Matthee, B. Darvish, I. Smail, P.N. Best, L. Alegre, H. Röttgering, B. Mobasher, A. Paulino-Afonso, A. Stroe, I. Oteo, Monthly Notices of the Royal Astronomical Society 477 (2018) 2817–2840.","apa":"Sobral, D., Matthee, J. J., Darvish, B., Smail, I., Best, P. N., Alegre, L., … Oteo, I. (2018). The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/sty782","ama":"Sobral D, Matthee JJ, Darvish B, et al. The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN. Monthly Notices of the Royal Astronomical Society. 2018;477(2):2817-2840. doi:10.1093/mnras/sty782","chicago":"Sobral, David, Jorryt J Matthee, Behnam Darvish, Ian Smail, Philip N Best, Lara Alegre, Huub Röttgering, et al. “The Nature of Luminous Ly α Emitters at z ∼ 2–3: Maximal Dust-Poor Starbursts and Highly Ionizing AGN.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2018. https://doi.org/10.1093/mnras/sty782."},"month":"06","acknowledgement":"We thank the anonymous reviewer for their timely and constructive comments that greatly helped us to improve the manuscript. DS acknowledges financial support from the Netherlands Organization for Scientific research (NWO) through a Veni fellowship and from Lancaster University through an Early Career Internal Grant A100679. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. BD acknowledges financial support from NASA through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G, and the National Science Foundation, grant number 1716907. IRS acknowledges support from the ERC Advanced Grant DUSTYGAL (321334), STFC (ST/P000541/1), and a Royal Society/Wolfson Merit Award. PNB is grateful for support from STFC via grant ST/M001229/1. We thank Anne Verhamme, Kimihiko Nakajima, Ryan Trainor, Sangeeta Malhotra, Max Gronke, James Rhoads, Fang Xia An, Matthew Hayes, Takashi Kojima, Mark Dijkstra, and Anne Jaskot for many helpful and engaging discussions, particularly during the SnowCLAW Ly α workshop. We thank Bruno Ribeiro, Stephane Charlot, and Joseph Caruana for comments on the manuscript. The authors would also like to thank Ingrid Tengs, Meg Singleton, Ali Khostovan, and Sara Perez for participating in part of the observations. We also thank Joao Calhau, Leah Morabito, Sergio Santos, and Aayush Saxena for their assistance with the narrow-band observations which allowed to select some of the sour ces. Based on observations obtained with the William Herschel Telescope, program: W16AN004; the Very Large Telescope, programs: 098.A-0819 & 099.A-0254; and the Keck II telescope, program: C267D. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme IDs 294.A-5018, 294.A-5039, 092.A-0786, 093.A-0561, 097.A-0943, 098.A-0819, 099.A-0254 and 179.A-2005. The authors acknowledge the award of service time (SW2014b20) on the WHT. WHT and its service programme are operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. The authors would also like to thank all the extremely helpful observatory staff that have greatly contributed towards our observations, particularly Fiona Riddick, Lilian Dominguez, Florencia Jimenez, and Ian Skillen. We have benefited greatly from the publicly available programming language PYTHON, including the NUMPY & SCIPY (Van Der Walt, Colbert & Varoquaux 2011; Jones et al. 2001), MATPLOTLIB (Hunter 2007), ASTROPY (Astropy Collaboration et al. 2013), and the TOPCAT analysis program (Taylor 2013). This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France.","volume":477,"page":"2817-2840","status":"public","author":[{"full_name":"Sobral, David","last_name":"Sobral","first_name":"David"},{"full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X"},{"first_name":"Behnam","last_name":"Darvish","full_name":"Darvish, Behnam"},{"last_name":"Smail","first_name":"Ian","full_name":"Smail, Ian"},{"full_name":"Best, Philip N","last_name":"Best","first_name":"Philip N"},{"last_name":"Alegre","first_name":"Lara","full_name":"Alegre, Lara"},{"full_name":"Röttgering, Huub","first_name":"Huub","last_name":"Röttgering"},{"full_name":"Mobasher, Bahram","last_name":"Mobasher","first_name":"Bahram"},{"last_name":"Paulino-Afonso","first_name":"Ana","full_name":"Paulino-Afonso, Ana"},{"first_name":"Andra","last_name":"Stroe","full_name":"Stroe, Andra"},{"last_name":"Oteo","first_name":"Iván","full_name":"Oteo, Iván"}],"publication":"Monthly Notices of the Royal Astronomical Society","issue":"2"},{"status":"public","author":[{"full_name":"Sobral, David","first_name":"David","last_name":"Sobral"},{"last_name":"Santos","first_name":"Sérgio","full_name":"Santos, Sérgio"},{"orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Paulino-Afonso","first_name":"Ana","full_name":"Paulino-Afonso, Ana"},{"first_name":"Bruno","last_name":"Ribeiro","full_name":"Ribeiro, Bruno"},{"full_name":"Calhau, João","first_name":"João","last_name":"Calhau"},{"full_name":"Khostovan, Ali A","first_name":"Ali A","last_name":"Khostovan"}],"publication":"Monthly Notices of the Royal Astronomical Society","issue":"4","month":"06","volume":476,"acknowledgement":"We thank the anonymous referee for their constructive comments that helped us improve the manuscript. DS acknowledges the hospitality of the IAC and a Severo Ochoa visiting grant. SS and JC acknowledge studentships from the Lancaster University. JM acknowledges a Huygens PhD fellowship from Leiden University. APA acknowledges financial support from the Science and Technology Foundation (FCT, Portugal) through research grants UID/FIS/04434/2013 and fellowship PD/BD/52706/2014. The authors thank Alyssa Drake, Kimihiko Nakajima, Yuichi Harikane, Max Gronke, Irene Shivaei, Helmut Dannerbauer, Huub Rottgering, ¨ Marius Eide, and Masami Ouchi for many engaging and stimulating discussions. We also thank Sara Perez, Alex Bennett, and Tom Rose for their involvement in the early stages of this project. Based on data products from observations made with European Southern Observatory (ESO) Telescopes at the La Silla Paranal Observatory under ESO programme IDs 294.A-5018, 097.A 0943,\r\n098.A-0819, 099.A-0254, and 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. Based on observations using the WFC on the 2.5 m INT, as part of programmes 2013AN002, 2013BN008, 2014AC88, 2014AN002, 2014BN006, 2014BC118, and 2016AN001. The INT is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. This work is based in part on data products produced at TERAPIX available at the Canadian Astronomy Data Centre as part of the Canada–France– Hawaii Telescope Legacy Survey (CFHTLS), a collaborative project of NRC and CNRS.\r\nWe are grateful to the CFHTLS, COSMOS-UltraVISTA, and COSMOS survey teams. We are also unmeasurably thankful to the pioneering and continuous work from previous Ly α surveys’ teams. Without these previous Ly α and the wider reach legacy surveys, this research would have been impossible. We also thank the VUDS team for making available spectroscopic redshifts from data obtained with VIMOS at the European Southern Observatory Very Large Telescope, Paranal, Chile, under Large Programme 185.A-0791. Finally, the authors acknowledge the unique value of the publicly available programming language PYTHON, including the NUMPY and SCIPY (Van Der Walt, Colbert & Varoquaux 2011; Jones et al. 2001), MATPLOTLIB (Hunter 2007), ASTROPY (Astropy Collaboration et al. 2013), and the TOPCAT analysis program (Taylor 2005). We publicly release a catalogue with all LAEs used in this paper (SC4K), so it can be freely explored by the community (see five example entries in Table A1).","page":"4725-4752","date_published":"2018-06-01T00:00:00Z","abstract":[{"lang":"eng","text":"We present and explore deep narrow- and medium-band data obtained with the Subaru and the Isaac Newton Telescopes in the ∼2 deg2 COSMOS field. We use these data as an extremely wide, low-resolution (R ∼ 20–80) Integral Field Unit survey to slice through the COSMOS field and obtain a large sample of ∼4000 Ly α emitters (LAEs) from z ∼ 2 to 6 in 16 redshift slices (SC4K). We present new Ly α luminosity functions (LFs) covering a comoving volume of ∼108 Mpc3. SC4K extensively complements ultradeep surveys, jointly covering over 4 dex in Ly α luminosity and revealing a global (2.5 < z < 6) synergy LF with α=−1.93+0.12−0.12, log10Φ∗Lyα=−3.45+0.22−0.29 Mpc−3, and log10L∗Lyα=42.93+0.15−0.11 erg s−1. The Schechter component of the Ly α LF reveals a factor ∼5 rise in L∗Lyα and a ∼7 × decline in Φ∗Lyα from z ∼ 2 to 6. The data reveal an extra power-law (or Schechter) component above LLy α ≈ 1043.3 erg s−1 at z ∼ 2.2–3.5 and we show that it is partially driven by X-ray and radio active galactic nucleus (AGN), as their Ly α LF resembles the excess. The power-law component vanishes and/or is below our detection limits above z > 3.5, likely linked with the evolution of the AGN population. The Ly α luminosity density rises by a factor ∼2 from z ∼ 2 to 3 but is then found to be roughly constant (1.1+0.2−0.2×1040 erg s−1 Mpc−3) to z ∼ 6, despite the ∼0.7 dex drop in ultraviolet (UV) luminosity density. The Ly α/UV luminosity density ratio rises from 4 ± 1 per cent to 30 ± 6 per cent from z ∼ 2.2 to 6. Our results imply a rise of a factor of ≈2 in the global ionization efficiency (ξion) and a factor ≈4 ± 1 in the Ly α escape fraction from z ∼ 2 to 6, hinting for evolution in both the typical burstiness/stellar populations and even more so in the typical interstellar medium conditions allowing Ly α photons to escape."}],"citation":{"ista":"Sobral D, Santos S, Matthee JJ, Paulino-Afonso A, Ribeiro B, Calhau J, Khostovan AA. 2018. Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6. Monthly Notices of the Royal Astronomical Society. 476(4), 4725–4752.","apa":"Sobral, D., Santos, S., Matthee, J. J., Paulino-Afonso, A., Ribeiro, B., Calhau, J., & Khostovan, A. A. (2018). Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/sty378","short":"D. Sobral, S. Santos, J.J. Matthee, A. Paulino-Afonso, B. Ribeiro, J. Calhau, A.A. Khostovan, Monthly Notices of the Royal Astronomical Society 476 (2018) 4725–4752.","ieee":"D. Sobral et al., “Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6,” Monthly Notices of the Royal Astronomical Society, vol. 476, no. 4. Oxford University Press, pp. 4725–4752, 2018.","mla":"Sobral, David, et al. “Slicing COSMOS with SC4K: The Evolution of Typical Ly α Emitters and the Ly α Escape Fraction from z ∼ 2 to 6.” Monthly Notices of the Royal Astronomical Society, vol. 476, no. 4, Oxford University Press, 2018, pp. 4725–52, doi:10.1093/mnras/sty378.","chicago":"Sobral, David, Sérgio Santos, Jorryt J Matthee, Ana Paulino-Afonso, Bruno Ribeiro, João Calhau, and Ali A Khostovan. “Slicing COSMOS with SC4K: The Evolution of Typical Ly α Emitters and the Ly α Escape Fraction from z ∼ 2 to 6.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2018. https://doi.org/10.1093/mnras/sty378.","ama":"Sobral D, Santos S, Matthee JJ, et al. Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6. Monthly Notices of the Royal Astronomical Society. 2018;476(4):4725-4752. doi:10.1093/mnras/sty378"},"intvolume":" 476","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: formation","galaxies: high-redshift","galaxies: luminosity function","mass function","galaxies: statistics"],"extern":"1","date_updated":"2022-08-19T07:04:45Z","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1712.04451"}],"year":"2018","publication_status":"published","publisher":"Oxford University Press","day":"01","external_id":{"arxiv":["1712.04451"]},"oa":1,"type":"journal_article","article_processing_charge":"No","title":"Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6","arxiv":1,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"article_type":"original","_id":"11558","oa_version":"Preprint","scopus_import":"1","doi":"10.1093/mnras/sty378","quality_controlled":"1","date_created":"2022-07-12T10:41:08Z"},{"article_processing_charge":"No","title":"Star-forming galaxies are predicted to lie on a fundamental plane of mass, star formation rate, and α-enhancement","arxiv":1,"publication_identifier":{"eissn":["1745-3933"],"issn":["1745-3925"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"url":"https://arxiv.org/abs/1802.06786","open_access":"1"}],"year":"2018","publication_status":"published","publisher":"Oxford University Press","day":"01","external_id":{"arxiv":["1802.06786"]},"oa":1,"type":"journal_article","quality_controlled":"1","date_created":"2022-07-14T12:49:47Z","language":[{"iso":"eng"}],"article_type":"original","_id":"11584","scopus_import":"1","oa_version":"Preprint","doi":"10.1093/mnrasl/sly093","month":"09","volume":479,"acknowledgement":"We thank the anonymous referee for their constructive comments. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. We thank Jarle Brinchmann, Rob Crain and David Sobral for discussions. We acknowledge the use of the TOPCAT software (Taylor 2013) for assisting in rapid exploration of multidimensional data sets and the use of PYTHON and its NUMPY, MATPLOTLIB, and PANDAS packages.","page":"L34 - L39","status":"public","author":[{"orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"first_name":"Joop","last_name":"Schaye","full_name":"Schaye, Joop"}],"issue":"1","publication":"Monthly Notices of the Royal Astronomical Society: Letters","intvolume":" 479","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: abundances","galaxies: evolution","galaxies: formation","galaxies: star formation"],"extern":"1","date_updated":"2024-10-14T11:37:53Z","date_published":"2018-09-01T00:00:00Z","citation":{"ista":"Matthee JJ, Schaye J. 2018. Star-forming galaxies are predicted to lie on a fundamental plane of mass, star formation rate, and α-enhancement. Monthly Notices of the Royal Astronomical Society: Letters. 479(1), L34–L39.","apa":"Matthee, J. J., & Schaye, J. (2018). Star-forming galaxies are predicted to lie on a fundamental plane of mass, star formation rate, and α-enhancement. Monthly Notices of the Royal Astronomical Society: Letters. Oxford University Press. https://doi.org/10.1093/mnrasl/sly093","mla":"Matthee, Jorryt J., and Joop Schaye. “Star-Forming Galaxies Are Predicted to Lie on a Fundamental Plane of Mass, Star Formation Rate, and α-Enhancement.” Monthly Notices of the Royal Astronomical Society: Letters, vol. 479, no. 1, Oxford University Press, 2018, pp. L34–39, doi:10.1093/mnrasl/sly093.","short":"J.J. Matthee, J. Schaye, Monthly Notices of the Royal Astronomical Society: Letters 479 (2018) L34–L39.","ieee":"J. J. Matthee and J. Schaye, “Star-forming galaxies are predicted to lie on a fundamental plane of mass, star formation rate, and α-enhancement,” Monthly Notices of the Royal Astronomical Society: Letters, vol. 479, no. 1. Oxford University Press, pp. L34–L39, 2018.","chicago":"Matthee, Jorryt J, and Joop Schaye. “Star-Forming Galaxies Are Predicted to Lie on a Fundamental Plane of Mass, Star Formation Rate, and α-Enhancement.” Monthly Notices of the Royal Astronomical Society: Letters. Oxford University Press, 2018. https://doi.org/10.1093/mnrasl/sly093.","ama":"Matthee JJ, Schaye J. Star-forming galaxies are predicted to lie on a fundamental plane of mass, star formation rate, and α-enhancement. Monthly Notices of the Royal Astronomical Society: Letters. 2018;479(1):L34-L39. doi:10.1093/mnrasl/sly093"},"abstract":[{"text":"Observations show that star-forming galaxies reside on a tight 3D plane between mass, gas-phase metallicity, and star formation rate (SFR), which can be explained by the interplay between metal-poor gas inflows, SFR and outflows. However, different metals are released on different time-scales, which may affect the slope of this relation. Here, we use central, star-forming galaxies with Mstar = 109.0–10.5 M⊙ from the EAGLE hydrodynamical simulation to examine 3D relations between mass, SFR, and chemical enrichment using absolute and relative C, N, O, and Fe abundances. We show that the scatter is smaller when gas-phase α-enhancement is used rather than metallicity. A similar plane also exists for stellar α-enhancement, implying that present-day specific SFRs are correlated with long time-scale star formation histories. Between z = 0 and 1, the α-enhancement plane is even more insensitive to redshift than the plane using metallicity. However, it evolves at z > 1 due to lagging iron yields. At fixed mass, galaxies with higher SFRs have star formation histories shifted towards late times, are more α-enhanced, and this α-enhancement increases with redshift as observed. These findings suggest that relations between physical properties inferred from observations may be affected by systematic variations in α-enhancements.","lang":"eng"}]},{"date_published":"2018-12-01T00:00:00Z","citation":{"ista":"Bugnet LA, García RA, Davies GR, Mathur S, Corsaro E, Hall OJ, Rendle BM. 2018. FliPer: A global measure of power density to estimate surface gravities of main-sequence solar-like stars and red giants. Astronomy & Astrophysics. 620, A38.","chicago":"Bugnet, Lisa Annabelle, R. A. García, G. R. Davies, S. Mathur, E. Corsaro, O. J. Hall, and B. M. Rendle. “FliPer: A Global Measure of Power Density to Estimate Surface Gravities of Main-Sequence Solar-like Stars and Red Giants.” Astronomy & Astrophysics. EDP Sciences, 2018. https://doi.org/10.1051/0004-6361/201833106.","ama":"Bugnet LA, García RA, Davies GR, et al. FliPer: A global measure of power density to estimate surface gravities of main-sequence solar-like stars and red giants. Astronomy & Astrophysics. 2018;620. doi:10.1051/0004-6361/201833106","apa":"Bugnet, L. A., García, R. A., Davies, G. R., Mathur, S., Corsaro, E., Hall, O. J., & Rendle, B. M. (2018). FliPer: A global measure of power density to estimate surface gravities of main-sequence solar-like stars and red giants. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201833106","short":"L.A. Bugnet, R.A. García, G.R. Davies, S. Mathur, E. Corsaro, O.J. Hall, B.M. Rendle, Astronomy & Astrophysics 620 (2018).","mla":"Bugnet, Lisa Annabelle, et al. “FliPer: A Global Measure of Power Density to Estimate Surface Gravities of Main-Sequence Solar-like Stars and Red Giants.” Astronomy & Astrophysics, vol. 620, A38, EDP Sciences, 2018, doi:10.1051/0004-6361/201833106.","ieee":"L. A. Bugnet et al., “FliPer: A global measure of power density to estimate surface gravities of main-sequence solar-like stars and red giants,” Astronomy & Astrophysics, vol. 620. EDP Sciences, 2018."},"abstract":[{"text":"Asteroseismology provides global stellar parameters such as masses, radii, or surface gravities using mean global seismic parameters and effective temperature for thousands of low-mass stars (0.8 M⊙ < M < 3 M⊙). This methodology has been successfully applied to stars in which acoustic modes excited by turbulent convection are measured. Other methods such as the Flicker technique can also be used to determine stellar surface gravities, but only works for log g above 2.5 dex. In this work, we present a new metric called FliPer (Flicker in spectral power density, in opposition to the standard Flicker measurement which is computed in the time domain); it is able to extend the range for which reliable surface gravities can be obtained (0.1 < log g < 4.6 dex) without performing any seismic analysis for stars brighter than Kp < 14. FliPer takes into account the average variability of a star measured in the power density spectrum in a given range of frequencies. However, FliPer values calculated on several ranges of frequency are required to better characterize a star. Using a large set of asteroseismic targets it is possible to calibrate the behavior of surface gravity with FliPer through machine learning. This calibration made with a random forest regressor covers a wide range of surface gravities from main-sequence stars to subgiants and red giants, with very small uncertainties from 0.04 to 0.1 dex. FliPer values can be inserted in automatic global seismic pipelines to either give an estimation of the stellar surface gravity or to assess the quality of the seismic results by detecting any outliers in the obtained νmax values. FliPer also constrains the surface gravities of main-sequence dwarfs using only long-cadence data for which the Nyquist frequency is too low to measure the acoustic-mode properties.","lang":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","asteroseismology / methods","data analysis / stars","oscillations"],"intvolume":" 620","extern":"1","date_updated":"2024-10-14T11:40:17Z","status":"public","author":[{"full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","first_name":"Lisa Annabelle","last_name":"Bugnet","orcid":"0000-0003-0142-4000"},{"last_name":"García","first_name":"R. A.","full_name":"García, R. A."},{"full_name":"Davies, G. R.","first_name":"G. R.","last_name":"Davies"},{"full_name":"Mathur, S.","last_name":"Mathur","first_name":"S."},{"first_name":"E.","last_name":"Corsaro","full_name":"Corsaro, E."},{"full_name":"Hall, O. J.","last_name":"Hall","first_name":"O. J."},{"first_name":"B. M.","last_name":"Rendle","full_name":"Rendle, B. M."}],"publication":"Astronomy & Astrophysics","acknowledgement":"We thank the anonymous referee for the very useful comments. We would also like to thank M. Benbakoura for his help in analyzing the light curves of several binary systems included in our set of stars. L.B. and R.A.G. acknowledge the support from PLATO and GOLF CNES grants. S.M. acknowledges support from the National Aeronautics and Space Administration under Grant NNX15AF13G, the National Science Foundation grant AST-1411685, and the Ramon y Cajal fellowship no. RYC-2015-17697. E.C. is funded by the European Union’s Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement no. 664931. O.J.H and B.M.R. acknowledge the support of the UK Science and Technology Facilities Council (STFC). Funding for the Stellar Astrophysics Centre is provided by the Danish National Research Foundation (Grant DNRF106). This research has made use of NASA’s Astrophysics Data System. Data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555.","volume":620,"article_number":"A38","month":"12","article_type":"original","language":[{"iso":"eng"}],"doi":"10.1051/0004-6361/201833106","_id":"11618","oa_version":"Preprint","scopus_import":"1","quality_controlled":"1","date_created":"2022-07-18T14:37:39Z","publication_status":"published","year":"2018","publisher":"EDP Sciences","main_file_link":[{"url":"https://arxiv.org/abs/1809.05105","open_access":"1"}],"type":"journal_article","day":"01","external_id":{"arxiv":["1809.05105"]},"oa":1,"article_processing_charge":"No","title":"FliPer: A global measure of power density to estimate surface gravities of main-sequence solar-like stars and red giants","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","arxiv":1},{"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1809.07573"}],"publisher":"EDP Sciences","publication_status":"published","year":"2018","oa":1,"day":"22","external_id":{"arxiv":["1809.07573"]},"type":"journal_article","title":"TESS’s first planet: A super-Earth transiting the naked-eye star π Mensae","article_processing_charge":"No","arxiv":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"language":[{"iso":"eng"}],"article_type":"letter_note","oa_version":"Preprint","scopus_import":"1","_id":"11619","doi":"10.1051/0004-6361/201834289","quality_controlled":"1","date_created":"2022-07-18T14:41:16Z","author":[{"last_name":"Gandolfi","first_name":"D.","full_name":"Gandolfi, D."},{"full_name":"Barragán, O.","last_name":"Barragán","first_name":"O."},{"full_name":"Livingston, J. H.","first_name":"J. H.","last_name":"Livingston"},{"full_name":"Fridlund, M.","first_name":"M.","last_name":"Fridlund"},{"last_name":"Justesen","first_name":"A. B.","full_name":"Justesen, A. B."},{"full_name":"Redfield, S.","last_name":"Redfield","first_name":"S."},{"full_name":"Fossati, L.","last_name":"Fossati","first_name":"L."},{"last_name":"Mathur","first_name":"S.","full_name":"Mathur, S."},{"full_name":"Grziwa, S.","last_name":"Grziwa","first_name":"S."},{"last_name":"Cabrera","first_name":"J.","full_name":"Cabrera, J."},{"full_name":"García, R. A.","first_name":"R. A.","last_name":"García"},{"full_name":"Persson, C. M.","last_name":"Persson","first_name":"C. M."},{"full_name":"Van Eylen, V.","first_name":"V.","last_name":"Van Eylen"},{"full_name":"Hatzes, A. P.","first_name":"A. P.","last_name":"Hatzes"},{"first_name":"D.","last_name":"Hidalgo","full_name":"Hidalgo, D."},{"first_name":"S.","last_name":"Albrecht","full_name":"Albrecht, S."},{"orcid":"0000-0003-0142-4000","last_name":"Bugnet","first_name":"Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","full_name":"Bugnet, Lisa Annabelle"},{"last_name":"Cochran","first_name":"W. D.","full_name":"Cochran, W. D."},{"last_name":"Csizmadia","first_name":"Sz.","full_name":"Csizmadia, Sz."},{"full_name":"Deeg, H.","first_name":"H.","last_name":"Deeg"},{"last_name":"Eigmüller","first_name":"Ph.","full_name":"Eigmüller, Ph."},{"full_name":"Endl, M.","first_name":"M.","last_name":"Endl"},{"last_name":"Erikson","first_name":"A.","full_name":"Erikson, A."},{"first_name":"M.","last_name":"Esposito","full_name":"Esposito, M."},{"first_name":"E.","last_name":"Guenther","full_name":"Guenther, E."},{"last_name":"Korth","first_name":"J.","full_name":"Korth, J."},{"full_name":"Luque, R.","first_name":"R.","last_name":"Luque"},{"last_name":"Montañes Rodríguez","first_name":"P.","full_name":"Montañes Rodríguez, P."},{"full_name":"Nespral, D.","last_name":"Nespral","first_name":"D."},{"last_name":"Nowak","first_name":"G.","full_name":"Nowak, G."},{"full_name":"Pätzold, M.","first_name":"M.","last_name":"Pätzold"},{"full_name":"Prieto-Arranz, J.","first_name":"J.","last_name":"Prieto-Arranz"}],"status":"public","publication":"Astronomy & Astrophysics","month":"11","article_number":"L10","volume":619,"date_published":"2018-11-22T00:00:00Z","citation":{"ista":"Gandolfi D, Barragán O, Livingston JH, Fridlund M, Justesen AB, Redfield S, Fossati L, Mathur S, Grziwa S, Cabrera J, García RA, Persson CM, Van Eylen V, Hatzes AP, Hidalgo D, Albrecht S, Bugnet LA, Cochran WD, Csizmadia S, Deeg H, Eigmüller P, Endl M, Erikson A, Esposito M, Guenther E, Korth J, Luque R, Montañes Rodríguez P, Nespral D, Nowak G, Pätzold M, Prieto-Arranz J. 2018. TESS’s first planet: A super-Earth transiting the naked-eye star π Mensae. Astronomy & Astrophysics. 619, L10.","ama":"Gandolfi D, Barragán O, Livingston JH, et al. TESS’s first planet: A super-Earth transiting the naked-eye star π Mensae. Astronomy & Astrophysics. 2018;619. doi:10.1051/0004-6361/201834289","chicago":"Gandolfi, D., O. Barragán, J. H. Livingston, M. Fridlund, A. B. Justesen, S. Redfield, L. Fossati, et al. “TESS’s First Planet: A Super-Earth Transiting the Naked-Eye Star π Mensae.” Astronomy & Astrophysics. EDP Sciences, 2018. https://doi.org/10.1051/0004-6361/201834289.","mla":"Gandolfi, D., et al. “TESS’s First Planet: A Super-Earth Transiting the Naked-Eye Star π Mensae.” Astronomy & Astrophysics, vol. 619, L10, EDP Sciences, 2018, doi:10.1051/0004-6361/201834289.","short":"D. Gandolfi, O. Barragán, J.H. Livingston, M. Fridlund, A.B. Justesen, S. Redfield, L. Fossati, S. Mathur, S. Grziwa, J. Cabrera, R.A. García, C.M. Persson, V. Van Eylen, A.P. Hatzes, D. Hidalgo, S. Albrecht, L.A. Bugnet, W.D. Cochran, S. Csizmadia, H. Deeg, P. Eigmüller, M. Endl, A. Erikson, M. Esposito, E. Guenther, J. Korth, R. Luque, P. Montañes Rodríguez, D. Nespral, G. Nowak, M. Pätzold, J. Prieto-Arranz, Astronomy & Astrophysics 619 (2018).","ieee":"D. Gandolfi et al., “TESS’s first planet: A super-Earth transiting the naked-eye star π Mensae,” Astronomy & Astrophysics, vol. 619. EDP Sciences, 2018.","apa":"Gandolfi, D., Barragán, O., Livingston, J. H., Fridlund, M., Justesen, A. B., Redfield, S., … Prieto-Arranz, J. (2018). TESS’s first planet: A super-Earth transiting the naked-eye star π Mensae. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201834289"},"abstract":[{"lang":"eng","text":"We report on the confirmation and mass determination of π Men c, the first transiting planet discovered by NASA’s TESS space mission. π Men is a naked-eye (V = 5.65 mag), quiet G0 V star that was previously known to host a sub-stellar companion (π Men b) on a longperiod (Porb = 2091 days), eccentric (e = 0.64) orbit. Using TESS time-series photometry, combined with Gaia data, published UCLES at AAT Doppler measurements, and archival HARPS at ESO-3.6m radial velocities, we found that π Men c is a close-in planet with an orbital period of Porb = 6.27 days, a mass of Mc = 4.52 ± 0.81 M⊕, and a radius of Rc = 2.06 ± 0.03 R⊕. Based on the planet’s orbital period and size, π Men c is a super-Earth located at, or close to, the radius gap, while its mass and bulk density suggest it may have held on to a significant atmosphere. Because of the brightness of the host star, this system is highly suitable for a wide range of further studies to characterize the planetary atmosphere and dynamical properties. We also performed an asteroseismic analysis of the TESS data and detected a hint of power excess consistent with the seismic values expected for this star, although this result depends on the photometric aperture used to extract the light curve. This marginal detection is expected from pre-launch simulations hinting at the asteroseismic potential of the TESS mission for longer, multi-sector observations and/or for more evolved bright stars."}],"intvolume":" 619","keyword":["Space and Planetary Science","Astronomy and Astrophysics","planetary systems / planets and satellites","detection / planets and satellites","fundamental parameters / planets and satellites","terrestrial planets / stars","fundamental parameters"],"date_updated":"2022-08-22T07:43:29Z","extern":"1"},{"date_published":"2018-08-01T00:00:00Z","citation":{"apa":"Van Eylen, V., Dai, F., Mathur, S., Gandolfi, D., Albrecht, S., Fridlund, M., … Smith, A. M. S. (2018). HD 89345: A bright oscillating star hosting a transiting warm Saturn-sized planet observed by K2. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/sty1390","ieee":"V. Van Eylen et al., “HD 89345: A bright oscillating star hosting a transiting warm Saturn-sized planet observed by K2,” Monthly Notices of the Royal Astronomical Society, vol. 478, no. 4. Oxford University Press, pp. 4866–4880, 2018.","short":"V. Van Eylen, F. Dai, S. Mathur, D. Gandolfi, S. Albrecht, M. Fridlund, R.A. García, E. Guenther, M. Hjorth, A.B. Justesen, J. Livingston, M.N. Lund, F. Pérez Hernández, J. Prieto-Arranz, C. Regulo, L.A. Bugnet, M.E. Everett, T. Hirano, D. Nespral, G. Nowak, E. Palle, V. Silva Aguirre, T. Trifonov, J.N. Winn, O. Barragán, P.G. Beck, W.J. Chaplin, W.D. Cochran, S. Csizmadia, H. Deeg, M. Endl, P. Heeren, S. Grziwa, A.P. Hatzes, D. Hidalgo, J. Korth, S. Mathis, P. Montañes Rodriguez, N. Narita, M. Patzold, C.M. Persson, F. Rodler, A.M.S. Smith, Monthly Notices of the Royal Astronomical Society 478 (2018) 4866–4880.","mla":"Van Eylen, V., et al. “HD 89345: A Bright Oscillating Star Hosting a Transiting Warm Saturn-Sized Planet Observed by K2.” Monthly Notices of the Royal Astronomical Society, vol. 478, no. 4, Oxford University Press, 2018, pp. 4866–80, doi:10.1093/mnras/sty1390.","chicago":"Van Eylen, V, F Dai, S Mathur, D Gandolfi, S Albrecht, M Fridlund, R A García, et al. “HD 89345: A Bright Oscillating Star Hosting a Transiting Warm Saturn-Sized Planet Observed by K2.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2018. https://doi.org/10.1093/mnras/sty1390.","ama":"Van Eylen V, Dai F, Mathur S, et al. HD 89345: A bright oscillating star hosting a transiting warm Saturn-sized planet observed by K2. Monthly Notices of the Royal Astronomical Society. 2018;478(4):4866-4880. doi:10.1093/mnras/sty1390","ista":"Van Eylen V, Dai F, Mathur S, Gandolfi D, Albrecht S, Fridlund M, García RA, Guenther E, Hjorth M, Justesen AB, Livingston J, Lund MN, Pérez Hernández F, Prieto-Arranz J, Regulo C, Bugnet LA, Everett ME, Hirano T, Nespral D, Nowak G, Palle E, Silva Aguirre V, Trifonov T, Winn JN, Barragán O, Beck PG, Chaplin WJ, Cochran WD, Csizmadia S, Deeg H, Endl M, Heeren P, Grziwa S, Hatzes AP, Hidalgo D, Korth J, Mathis S, Montañes Rodriguez P, Narita N, Patzold M, Persson CM, Rodler F, Smith AMS. 2018. HD 89345: A bright oscillating star hosting a transiting warm Saturn-sized planet observed by K2. Monthly Notices of the Royal Astronomical Society. 478(4), 4866–4880."},"abstract":[{"text":"We report the discovery and characterization of HD 89345b (K2-234b; EPIC 248777106b), a Saturn-sized planet orbiting a slightly evolved star. HD 89345 is a bright star (V = 9.3 mag) observed by the K2 mission with 1 min time sampling. It exhibits solar-like oscillations. We conducted asteroseismology to determine the parameters of the star, finding the mass and radius to be 1.12+0.04−0.01M⊙ and 1.657+0.020−0.004R⊙, respectively. The star appears to have recently left the main sequence, based on the inferred age, 9.4+0.4−1.3Gyr, and the non-detection of mixed modes. The star hosts a ‘warm Saturn’ (P = 11.8 d, Rp = 6.86 ± 0.14 R⊕). Radial-velocity follow-up observations performed with the FIbre-fed Echelle Spectrograph, HARPS, and HARPS-N spectrographs show that the planet has a mass of 35.7 ± 3.3 M⊕. The data also show that the planet’s orbit is eccentric (e ≈ 0.2). An investigation of the rotational splitting of the oscillation frequencies of the star yields no conclusive evidence on the stellar inclination angle. We further obtained Rossiter–McLaughlin observations, which result in a broad posterior of the stellar obliquity. The planet seems to confirm to the same patterns that have been observed for other sub-Saturns regarding planet mass and multiplicity, orbital eccentricity, and stellar metallicity.","lang":"eng"}],"intvolume":" 478","keyword":["Space and Planetary Science","Astronomy and Astrophysics","asteroseismology","planets and satellites: composition","planets and satellites: formation","planets and satellites: fundamental parameters"],"date_updated":"2022-08-22T07:45:38Z","extern":"1","author":[{"last_name":"Van Eylen","first_name":"V","full_name":"Van Eylen, V"},{"first_name":"F","last_name":"Dai","full_name":"Dai, F"},{"full_name":"Mathur, S","last_name":"Mathur","first_name":"S"},{"full_name":"Gandolfi, D","last_name":"Gandolfi","first_name":"D"},{"full_name":"Albrecht, S","first_name":"S","last_name":"Albrecht"},{"last_name":"Fridlund","first_name":"M","full_name":"Fridlund, M"},{"full_name":"García, R A","first_name":"R A","last_name":"García"},{"full_name":"Guenther, E","last_name":"Guenther","first_name":"E"},{"full_name":"Hjorth, M","first_name":"M","last_name":"Hjorth"},{"full_name":"Justesen, A B","first_name":"A B","last_name":"Justesen"},{"full_name":"Livingston, J","last_name":"Livingston","first_name":"J"},{"last_name":"Lund","first_name":"M N","full_name":"Lund, M N"},{"full_name":"Pérez Hernández, F","last_name":"Pérez Hernández","first_name":"F"},{"last_name":"Prieto-Arranz","first_name":"J","full_name":"Prieto-Arranz, J"},{"last_name":"Regulo","first_name":"C","full_name":"Regulo, C"},{"last_name":"Bugnet","orcid":"0000-0003-0142-4000","first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501"},{"first_name":"M E","last_name":"Everett","full_name":"Everett, M E"},{"last_name":"Hirano","first_name":"T","full_name":"Hirano, T"},{"full_name":"Nespral, D","last_name":"Nespral","first_name":"D"},{"full_name":"Nowak, G","last_name":"Nowak","first_name":"G"},{"full_name":"Palle, E","first_name":"E","last_name":"Palle"},{"last_name":"Silva Aguirre","first_name":"V","full_name":"Silva Aguirre, V"},{"full_name":"Trifonov, T","last_name":"Trifonov","first_name":"T"},{"full_name":"Winn, J N","first_name":"J N","last_name":"Winn"},{"first_name":"O","last_name":"Barragán","full_name":"Barragán, O"},{"first_name":"P G","last_name":"Beck","full_name":"Beck, P G"},{"first_name":"W J","last_name":"Chaplin","full_name":"Chaplin, W J"},{"first_name":"W D","last_name":"Cochran","full_name":"Cochran, W D"},{"full_name":"Csizmadia, S","first_name":"S","last_name":"Csizmadia"},{"first_name":"H","last_name":"Deeg","full_name":"Deeg, H"},{"full_name":"Endl, M","last_name":"Endl","first_name":"M"},{"first_name":"P","last_name":"Heeren","full_name":"Heeren, P"},{"full_name":"Grziwa, S","first_name":"S","last_name":"Grziwa"},{"full_name":"Hatzes, A P","last_name":"Hatzes","first_name":"A P"},{"last_name":"Hidalgo","first_name":"D","full_name":"Hidalgo, D"},{"last_name":"Korth","first_name":"J","full_name":"Korth, J"},{"first_name":"S","last_name":"Mathis","full_name":"Mathis, S"},{"first_name":"P","last_name":"Montañes Rodriguez","full_name":"Montañes Rodriguez, P"},{"full_name":"Narita, N","last_name":"Narita","first_name":"N"},{"full_name":"Patzold, M","first_name":"M","last_name":"Patzold"},{"first_name":"C M","last_name":"Persson","full_name":"Persson, C M"},{"last_name":"Rodler","first_name":"F","full_name":"Rodler, F"},{"full_name":"Smith, A M S","first_name":"A M S","last_name":"Smith"}],"status":"public","publication":"Monthly Notices of the Royal Astronomical Society","issue":"4","month":"08","volume":478,"acknowledgement":"We gratefully acknowledge many helpful suggestions by the anonymous referee. Based on observations made with a) the Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos; b) the ESO-3.6m telescope at La Silla Observatory under programme ID 0100.C-0808; c) the Italian Telescopio Nazionale Galileo operated on the island of La Palma by the Fundación Galileo Galilei of the Istituto Nazionale di Astrofisica. NESSI was funded by the NASA Exoplanet Exploration Program and the NASA Ames Research Center. NESSI was built at the Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. This project has received funding from the European Union’s Horizon 2020 research and innovation programme under grant agreement No 730890. This material reflects only the authors views and the Commission is not liable for any use that may be made of the information contained therein. DG gratefully acknowledges the financial support of the Programma Giovani Ricercatori – Rita Levi Montalcini – Rientro dei Cervelli (2012) awarded by the Italian Ministry of Education, Universities and Research (MIUR). SaM would like to acknowledge support from the Ramon y Cajal fellowship number RYC-2015-17697. AJ, MH, and SA acknowledge support by the Danish Council for Independent Research, through a DFF Sapere Aude Starting Grant nr. 4181-00487B. SzCs, APH, MP, and HR acknowledge the support of the DFG priority program SPP 1992Exploring the Diversity of Extrasolar Planets (grants HA 3279/12-1, PA 525/18-1, PA5 25/19-1 and PA525/20-1, RA 714/14-1) HD, CR, and FPH acknowledge the financial support from MINECO under grants ESP2015-65712-C5-4-R and AYA2016-76378-P. This paper has made use of the IAC Supercomputing facility HTCondor (http://research.cs.wisc.edu/htcondor/), partly financed by the Ministry of Economy and Competitiveness with FEDER funds, code IACA13-3E-2493. MF and CMP gratefully acknowledge the support of the Swedish National Space Board. RAG and StM thanks the support of the CNES PLATO grant. PGB is a postdoctoral fellow in the MINECO-programme ’Juan de la Cierva Incorporacion’ (IJCI-2015-26034). StM acknowledges support from ERC through SPIRE grant (647383) and from ISSI through the ENCELADE 2.0 team. VSA acknowledges support from VILLUM FONDEN (research grant 10118). MNL acknowledges support from the ESA-PRODEX programme. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (Grant agreement no.: DNRF106) This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This research was made with the use of NASA’s Astrophysics Data System and the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program.","page":"4866-4880","language":[{"iso":"eng"}],"article_type":"original","oa_version":"Preprint","scopus_import":"1","_id":"11620","doi":"10.1093/mnras/sty1390","quality_controlled":"1","date_created":"2022-07-18T14:43:17Z","main_file_link":[{"url":"https://arxiv.org/abs/1805.01860","open_access":"1"}],"publisher":"Oxford University Press","publication_status":"published","year":"2018","oa":1,"day":"01","external_id":{"arxiv":["1805.01860"]},"type":"journal_article","title":"HD 89345: A bright oscillating star hosting a transiting warm Saturn-sized planet observed by K2","article_processing_charge":"No","arxiv":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]}},{"arxiv":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","month":"11","article_processing_charge":"No","article_number":"1811.12140","title":"FliPer: Classifying TESS pulsating stars","day":"29","external_id":{"arxiv":["1811.12140"]},"oa":1,"publication":"arXiv","type":"preprint","main_file_link":[{"url":" https://doi.org/10.48550/arXiv.1811.12140","open_access":"1"}],"status":"public","author":[{"full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","first_name":"Lisa Annabelle","last_name":"Bugnet","orcid":"0000-0003-0142-4000"},{"full_name":"García, R. A.","last_name":"García","first_name":"R. A."},{"last_name":"Davies","first_name":"G. R.","full_name":"Davies, G. R."},{"full_name":"Mathur, S.","first_name":"S.","last_name":"Mathur"},{"last_name":"Hall","first_name":"O. J.","full_name":"Hall, O. J."},{"full_name":"Rendle, B. M.","last_name":"Rendle","first_name":"B. M."}],"publication_status":"submitted","year":"2018","date_updated":"2022-08-22T08:41:55Z","extern":"1","date_created":"2022-07-21T07:05:23Z","keyword":["asteroseismology - methods","data analysis - stars","oscillations"],"_id":"11631","citation":{"ista":"Bugnet LA, García RA, Davies GR, Mathur S, Hall OJ, Rendle BM. FliPer: Classifying TESS pulsating stars. arXiv, 1811.12140.","chicago":"Bugnet, Lisa Annabelle, R. A. García, G. R. Davies, S. Mathur, O. J. Hall, and B. M. Rendle. “FliPer: Classifying TESS Pulsating Stars.” ArXiv, n.d. https://doi.org/10.48550/arXiv.1811.12140.","ama":"Bugnet LA, García RA, Davies GR, Mathur S, Hall OJ, Rendle BM. FliPer: Classifying TESS pulsating stars. arXiv. doi:10.48550/arXiv.1811.12140","apa":"Bugnet, L. A., García, R. A., Davies, G. R., Mathur, S., Hall, O. J., & Rendle, B. M. (n.d.). FliPer: Classifying TESS pulsating stars. arXiv. https://doi.org/10.48550/arXiv.1811.12140","short":"L.A. Bugnet, R.A. García, G.R. Davies, S. Mathur, O.J. Hall, B.M. Rendle, ArXiv (n.d.).","ieee":"L. A. Bugnet, R. A. García, G. R. Davies, S. Mathur, O. J. Hall, and B. M. Rendle, “FliPer: Classifying TESS pulsating stars,” arXiv. .","mla":"Bugnet, Lisa Annabelle, et al. “FliPer: Classifying TESS Pulsating Stars.” ArXiv, 1811.12140, doi:10.48550/arXiv.1811.12140."},"abstract":[{"lang":"eng","text":"The recently launched NASA Transiting Exoplanet Survey Satellite (TESS) mission is going to collect lightcurves for a few hundred million of stars and we expect to increase the number of pulsating stars to analyze compared to the few thousand stars observed by the CoRoT, Kepler and K2 missions. However, most of the TESS targets have not yet been properly classified and characterized. In order to improve the analysis of the TESS data, it is crucial to determine the type of stellar pulsations in a timely manner. We propose an automatic method to classify stars attending to their pulsation properties, in particular, to identify solar-like pulsators among all TESS targets. It relies on the use of the global amount of power contained in the power spectrum (already known as the FliPer method) as a key parameter, along with\r\nthe effective temperature, to feed into a machine learning classifier. Our study, based on TESS simulated datasets, shows that we are able to classify pulsators with a 98% accuracy."}],"oa_version":"Preprint","doi":"10.48550/arXiv.1811.12140","date_published":"2018-11-29T00:00:00Z","language":[{"iso":"eng"}]},{"publisher":"Association for Computing Machinery","publication_status":"published","year":"2018","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1708.06127"}],"type":"journal_article","oa":1,"day":"01","external_id":{"arxiv":["1708.06127"]},"title":"Practical minimum cut algorithms","article_processing_charge":"No","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_identifier":{"eissn":["1084-6654"],"issn":["1084-6654"]},"arxiv":1,"article_type":"original","language":[{"iso":"eng"}],"doi":"10.1145/3274662","oa_version":"Preprint","scopus_import":"1","_id":"11657","quality_controlled":"1","date_created":"2022-07-27T08:28:26Z","author":[{"id":"540c9bbd-f2de-11ec-812d-d04a5be85630","full_name":"Henzinger, Monika H","first_name":"Monika H","orcid":"0000-0002-5008-6530","last_name":"Henzinger"},{"full_name":"Noe, Alexander","last_name":"Noe","first_name":"Alexander"},{"first_name":"Christian","last_name":"Schulz","full_name":"Schulz, Christian"},{"last_name":"Strash","first_name":"Darren","full_name":"Strash, Darren"}],"status":"public","publication":"ACM Journal of Experimental Algorithmics","volume":23,"month":"10","page":"1-22","date_published":"2018-10-01T00:00:00Z","abstract":[{"lang":"eng","text":"The minimum cut problem for an undirected edge-weighted graph asks us to divide its set of nodes into two blocks while minimizing the weight sum of the cut edges. Here, we introduce a linear-time algorithm to compute near-minimum cuts. Our algorithm is based on cluster contraction using label propagation and Padberg and Rinaldi’s contraction heuristics [SIAM Review, 1991]. We give both sequential and shared-memory parallel implementations of our algorithm. Extensive experiments on both real-world and generated instances show that our algorithm finds the optimal cut on nearly all instances significantly faster than other state-of-the-art exact algorithms, and our error rate is lower than that of other heuristic algorithms. In addition, our parallel algorithm runs a factor 7.5× faster on average when using 32 threads. To further speed up computations, we also give a version of our algorithm that performs random edge contractions as preprocessing. This version achieves a lower running time and better parallel scalability at the expense of a higher error rate."}],"citation":{"ama":"Henzinger M, Noe A, Schulz C, Strash D. Practical minimum cut algorithms. ACM Journal of Experimental Algorithmics. 2018;23:1-22. doi:10.1145/3274662","chicago":"Henzinger, Monika, Alexander Noe, Christian Schulz, and Darren Strash. “Practical Minimum Cut Algorithms.” ACM Journal of Experimental Algorithmics. Association for Computing Machinery, 2018. https://doi.org/10.1145/3274662.","mla":"Henzinger, Monika, et al. “Practical Minimum Cut Algorithms.” ACM Journal of Experimental Algorithmics, vol. 23, Association for Computing Machinery, 2018, pp. 1–22, doi:10.1145/3274662.","short":"M. Henzinger, A. Noe, C. Schulz, D. Strash, ACM Journal of Experimental Algorithmics 23 (2018) 1–22.","ieee":"M. Henzinger, A. Noe, C. Schulz, and D. Strash, “Practical minimum cut algorithms,” ACM Journal of Experimental Algorithmics, vol. 23. Association for Computing Machinery, pp. 1–22, 2018.","apa":"Henzinger, M., Noe, A., Schulz, C., & Strash, D. (2018). Practical minimum cut algorithms. ACM Journal of Experimental Algorithmics. Association for Computing Machinery. https://doi.org/10.1145/3274662","ista":"Henzinger M, Noe A, Schulz C, Strash D. 2018. Practical minimum cut algorithms. ACM Journal of Experimental Algorithmics. 23, 1–22."},"keyword":["Theoretical Computer Science"],"intvolume":" 23","extern":"1","date_updated":"2024-11-06T12:05:24Z"},{"title":"Incremental exact min-cut in polylogarithmic amortized update time","article_processing_charge":"No","arxiv":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_identifier":{"issn":["1549-6325"],"eissn":["1549-6333"]},"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1611.06500"}],"publisher":"Association for Computing Machinery","year":"2018","publication_status":"published","oa":1,"external_id":{"arxiv":["1611.06500"]},"day":"01","type":"journal_article","quality_controlled":"1","date_created":"2022-07-27T11:29:39Z","language":[{"iso":"eng"}],"article_type":"original","scopus_import":"1","oa_version":"Preprint","_id":"11664","doi":"10.1145/3174803","month":"04","article_number":"17","acknowledgement":"We thank the two anonymous reviewers for their suggestions and comments, which improved the\r\nquality of the article.","volume":14,"author":[{"first_name":"Gramoz","last_name":"Goranci","full_name":"Goranci, Gramoz"},{"id":"540c9bbd-f2de-11ec-812d-d04a5be85630","full_name":"Henzinger, Monika H","orcid":"0000-0002-5008-6530","last_name":"Henzinger","first_name":"Monika H"},{"first_name":"Mikkel","last_name":"Thorup","full_name":"Thorup, Mikkel"}],"status":"public","publication":"ACM Transactions on Algorithms","issue":"2","intvolume":" 14","extern":"1","date_updated":"2024-11-06T12:05:51Z","date_published":"2018-04-01T00:00:00Z","abstract":[{"text":"We present a deterministic incremental algorithm for exactly maintaining the size of a minimum cut with O(log3 n log log2 n) amortized time per edge insertion and O(1) query time. This result partially answers an open question posed by Thorup (2007). It also stays in sharp contrast to a polynomial conditional lower bound for the fully dynamic weighted minimum cut problem. Our algorithm is obtained by combining a sparsification technique of Kawarabayashi and Thorup (2015) or its recent improvement by Henzinger, Rao, and Wang (2017), and an exact incremental algorithm of Henzinger (1997).\r\n\r\nWe also study space-efficient incremental algorithms for the minimum cut problem. Concretely, we show that there exists an O(nlog n/ε2) space Monte Carlo algorithm that can process a stream of edge insertions starting from an empty graph, and with high probability, the algorithm maintains a (1+ε)-approximation to the minimum cut. The algorithm has O((α (n) log3 n)/ε 2) amortized update time and constant query time, where α (n) stands for the inverse of Ackermann function.","lang":"eng"}],"citation":{"apa":"Goranci, G., Henzinger, M., & Thorup, M. (2018). Incremental exact min-cut in polylogarithmic amortized update time. ACM Transactions on Algorithms. Association for Computing Machinery. https://doi.org/10.1145/3174803","ieee":"G. Goranci, M. Henzinger, and M. Thorup, “Incremental exact min-cut in polylogarithmic amortized update time,” ACM Transactions on Algorithms, vol. 14, no. 2. Association for Computing Machinery, 2018.","mla":"Goranci, Gramoz, et al. “Incremental Exact Min-Cut in Polylogarithmic Amortized Update Time.” ACM Transactions on Algorithms, vol. 14, no. 2, 17, Association for Computing Machinery, 2018, doi:10.1145/3174803.","short":"G. Goranci, M. Henzinger, M. Thorup, ACM Transactions on Algorithms 14 (2018).","chicago":"Goranci, Gramoz, Monika Henzinger, and Mikkel Thorup. “Incremental Exact Min-Cut in Polylogarithmic Amortized Update Time.” ACM Transactions on Algorithms. Association for Computing Machinery, 2018. https://doi.org/10.1145/3174803.","ama":"Goranci G, Henzinger M, Thorup M. Incremental exact min-cut in polylogarithmic amortized update time. ACM Transactions on Algorithms. 2018;14(2). doi:10.1145/3174803","ista":"Goranci G, Henzinger M, Thorup M. 2018. Incremental exact min-cut in polylogarithmic amortized update time. ACM Transactions on Algorithms. 14(2), 17."}},{"author":[{"last_name":"Dütting","first_name":"Paul","full_name":"Dütting, Paul"},{"first_name":"Monika H","orcid":"0000-0002-5008-6530","last_name":"Henzinger","id":"540c9bbd-f2de-11ec-812d-d04a5be85630","full_name":"Henzinger, Monika H"},{"full_name":"Starnberger, Martin","last_name":"Starnberger","first_name":"Martin"}],"status":"public","publication":"ACM Transactions on Economics and Computation","issue":"2","article_number":"5","volume":6,"month":"05","date_published":"2018-05-01T00:00:00Z","abstract":[{"lang":"eng","text":"The focus of classic mechanism design has been on truthful direct-revelation mechanisms. In the context of combinatorial auctions, the truthful direct-revelation mechanism that maximizes social welfare is the Vickrey-Clarke-Groves mechanism. For many valuation spaces, computing the allocation and payments of the VCG mechanism, however, is a computationally hard problem. We thus study the performance of the VCG mechanism when bidders are forced to choose bids from a subspace of the valuation space for which the VCG outcome can be computed efficiently. We prove improved upper bounds on the welfare loss for restrictions to additive bids and upper and lower bounds for restrictions to non-additive bids. These bounds show that increased expressiveness can give rise to additional equilibria of poorer efficiency."}],"citation":{"ieee":"P. Dütting, M. Henzinger, and M. Starnberger, “Valuation compressions in VCG-based combinatorial auctions,” ACM Transactions on Economics and Computation, vol. 6, no. 2. Association for Computing Machinery, 2018.","short":"P. Dütting, M. Henzinger, M. Starnberger, ACM Transactions on Economics and Computation 6 (2018).","mla":"Dütting, Paul, et al. “Valuation Compressions in VCG-Based Combinatorial Auctions.” ACM Transactions on Economics and Computation, vol. 6, no. 2, 5, Association for Computing Machinery, 2018, doi:10.1145/3232860.","apa":"Dütting, P., Henzinger, M., & Starnberger, M. (2018). Valuation compressions in VCG-based combinatorial auctions. ACM Transactions on Economics and Computation. Association for Computing Machinery. https://doi.org/10.1145/3232860","ama":"Dütting P, Henzinger M, Starnberger M. Valuation compressions in VCG-based combinatorial auctions. ACM Transactions on Economics and Computation. 2018;6(2). doi:10.1145/3232860","chicago":"Dütting, Paul, Monika Henzinger, and Martin Starnberger. “Valuation Compressions in VCG-Based Combinatorial Auctions.” ACM Transactions on Economics and Computation. Association for Computing Machinery, 2018. https://doi.org/10.1145/3232860.","ista":"Dütting P, Henzinger M, Starnberger M. 2018. Valuation compressions in VCG-based combinatorial auctions. ACM Transactions on Economics and Computation. 6(2), 5."},"keyword":["Theory of computation","Algorithmic game theory and mechanism design","Applied computing","Economics","Simplified mechanisms","Combinatorial auctions with item bidding","Price of anarchy"],"intvolume":" 6","date_updated":"2024-11-06T12:06:28Z","extern":"1","publisher":"Association for Computing Machinery","publication_status":"published","year":"2018","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1310.3153"}],"type":"journal_article","oa":1,"day":"01","external_id":{"arxiv":["1310.3153"]},"title":"Valuation compressions in VCG-based combinatorial auctions","article_processing_charge":"No","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_identifier":{"issn":["2167-8375"],"eissn":["2167-8383"]},"arxiv":1,"article_type":"original","language":[{"iso":"eng"}],"doi":"10.1145/3232860","oa_version":"Preprint","scopus_import":"1","_id":"11667","quality_controlled":"1","date_created":"2022-07-27T11:46:46Z"},{"quality_controlled":"1","date_created":"2022-08-08T11:20:03Z","article_type":"original","language":[{"iso":"eng"}],"doi":"10.1016/j.ic.2018.02.005","oa_version":"Published Version","scopus_import":"1","_id":"11757","title":"Dynamic algorithms via the primal-dual method","article_processing_charge":"No","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_identifier":{"issn":["0890-5401"]},"publisher":"Elsevier","year":"2018","publication_status":"published","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1016/j.ic.2018.02.005"}],"type":"journal_article","oa":1,"day":"01","intvolume":" 261","extern":"1","date_updated":"2024-11-06T08:13:33Z","date_published":"2018-08-01T00:00:00Z","citation":{"ama":"Bhattacharya S, Henzinger M, Italiano G. Dynamic algorithms via the primal-dual method. Information and Computation. 2018;261(08):219-239. doi:10.1016/j.ic.2018.02.005","chicago":"Bhattacharya, Sayan, Monika Henzinger, and Giuseppe Italiano. “Dynamic Algorithms via the Primal-Dual Method.” Information and Computation. Elsevier, 2018. https://doi.org/10.1016/j.ic.2018.02.005.","mla":"Bhattacharya, Sayan, et al. “Dynamic Algorithms via the Primal-Dual Method.” Information and Computation, vol. 261, no. 08, Elsevier, 2018, pp. 219–39, doi:10.1016/j.ic.2018.02.005.","ieee":"S. Bhattacharya, M. Henzinger, and G. Italiano, “Dynamic algorithms via the primal-dual method,” Information and Computation, vol. 261, no. 08. Elsevier, pp. 219–239, 2018.","short":"S. Bhattacharya, M. Henzinger, G. Italiano, Information and Computation 261 (2018) 219–239.","apa":"Bhattacharya, S., Henzinger, M., & Italiano, G. (2018). Dynamic algorithms via the primal-dual method. Information and Computation. Elsevier. https://doi.org/10.1016/j.ic.2018.02.005","ista":"Bhattacharya S, Henzinger M, Italiano G. 2018. Dynamic algorithms via the primal-dual method. Information and Computation. 261(08), 219–239."},"abstract":[{"lang":"eng","text":"We develop a dynamic version of the primal-dual method for optimization problems, and apply it to obtain the following results. (1) For the dynamic set-cover problem, we maintain an O ( f 2)-approximately optimal solution in O ( f · log(m + n)) amortized update time, where f is the maximum “frequency” of an element, n is the number of sets, and m is the maximum number of elements in the universe at any point in time. (2) For the dynamic b-matching problem, we maintain an O (1)-approximately optimal solution in O (log3 n) amortized update time, where n is the number of nodes in the graph."}],"volume":261,"month":"08","page":"219-239","author":[{"first_name":"Sayan","last_name":"Bhattacharya","full_name":"Bhattacharya, Sayan"},{"full_name":"Henzinger, Monika H","id":"540c9bbd-f2de-11ec-812d-d04a5be85630","orcid":"0000-0002-5008-6530","last_name":"Henzinger","first_name":"Monika H"},{"full_name":"Italiano, Giuseppe","first_name":"Giuseppe","last_name":"Italiano"}],"status":"public","publication":"Information and Computation","issue":"08"},{"arxiv":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_identifier":{"issn":["0004-5411"],"eissn":["1557-735X"]},"title":"Decremental single-source shortest paths on undirected graphs in near-linear total update time","article_processing_charge":"No","oa":1,"day":"01","external_id":{"arxiv":["1512.08148"]},"type":"journal_article","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1512.08148"}],"publisher":"Association for Computing Machinery","publication_status":"published","year":"2018","date_created":"2022-08-08T12:33:17Z","quality_controlled":"1","scopus_import":"1","oa_version":"Preprint","_id":"11768","doi":"10.1145/3218657","language":[{"iso":"eng"}],"article_type":"original","page":"1-40","month":"12","volume":65,"publication":"Journal of the ACM","issue":"6","author":[{"first_name":"Monika H","last_name":"Henzinger","orcid":"0000-0002-5008-6530","full_name":"Henzinger, Monika H","id":"540c9bbd-f2de-11ec-812d-d04a5be85630"},{"first_name":"Sebastian","last_name":"Krinninger","full_name":"Krinninger, Sebastian"},{"last_name":"Nanongkai","first_name":"Danupon","full_name":"Nanongkai, Danupon"}],"status":"public","extern":"1","date_updated":"2024-11-06T12:18:17Z","intvolume":" 65","abstract":[{"lang":"eng","text":"In the decremental single-source shortest paths (SSSP) problem, we want to maintain the distances between a given source node s and every other node in an n-node m-edge graph G undergoing edge deletions. While its static counterpart can be solved in near-linear time, this decremental problem is much more challenging even in the undirected unweighted case. In this case, the classic O(mn) total update time of Even and Shiloach [16] has been the fastest known algorithm for three decades. At the cost of a (1+ϵ)-approximation factor, the running time was recently improved to n2+o(1) by Bernstein and Roditty [9]. In this article, we bring the running time down to near-linear: We give a (1+ϵ)-approximation algorithm with m1+o(1) expected total update time, thus obtaining near-linear time. Moreover, we obtain m1+o(1) log W time for the weighted case, where the edge weights are integers from 1 to W. The only prior work on weighted graphs in o(mn) time is the mn0.9 + o(1)-time algorithm by Henzinger et al. [18, 19], which works for directed graphs with quasi-polynomial edge weights. The expected running time bound of our algorithm holds against an oblivious adversary.\r\n\r\nIn contrast to the previous results, which rely on maintaining a sparse emulator, our algorithm relies on maintaining a so-called sparse (h, ϵ)-hop set introduced by Cohen [12] in the PRAM literature. An (h, ϵ)-hop set of a graph G=(V, E) is a set F of weighted edges such that the distance between any pair of nodes in G can be (1+ϵ)-approximated by their h-hop distance (given by a path containing at most h edges) on G′=(V, E ∪ F). Our algorithm can maintain an (no(1), ϵ)-hop set of near-linear size in near-linear time under edge deletions. It is the first of its kind to the best of our knowledge. To maintain approximate distances using this hop set, we extend the monotone Even-Shiloach tree of Henzinger et al. [20] and combine it with the bounded-hop SSSP technique of Bernstein [4, 5] and Mądry [27]. These two new tools might be of independent interest."}],"citation":{"ama":"Henzinger M, Krinninger S, Nanongkai D. Decremental single-source shortest paths on undirected graphs in near-linear total update time. Journal of the ACM. 2018;65(6):1-40. doi:10.1145/3218657","chicago":"Henzinger, Monika, Sebastian Krinninger, and Danupon Nanongkai. “Decremental Single-Source Shortest Paths on Undirected Graphs in near-Linear Total Update Time.” Journal of the ACM. Association for Computing Machinery, 2018. https://doi.org/10.1145/3218657.","short":"M. Henzinger, S. Krinninger, D. Nanongkai, Journal of the ACM 65 (2018) 1–40.","ieee":"M. Henzinger, S. Krinninger, and D. Nanongkai, “Decremental single-source shortest paths on undirected graphs in near-linear total update time,” Journal of the ACM, vol. 65, no. 6. Association for Computing Machinery, pp. 1–40, 2018.","mla":"Henzinger, Monika, et al. “Decremental Single-Source Shortest Paths on Undirected Graphs in near-Linear Total Update Time.” Journal of the ACM, vol. 65, no. 6, Association for Computing Machinery, 2018, pp. 1–40, doi:10.1145/3218657.","apa":"Henzinger, M., Krinninger, S., & Nanongkai, D. (2018). Decremental single-source shortest paths on undirected graphs in near-linear total update time. Journal of the ACM. Association for Computing Machinery. https://doi.org/10.1145/3218657","ista":"Henzinger M, Krinninger S, Nanongkai D. 2018. Decremental single-source shortest paths on undirected graphs in near-linear total update time. Journal of the ACM. 65(6), 1–40."},"date_published":"2018-12-01T00:00:00Z","related_material":{"record":[{"id":"11855","status":"public","relation":"earlier_version"}]}},{"arxiv":1,"publication_identifier":{"isbn":["9783959770811"],"issn":["1868-8969"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","article_processing_charge":"No","title":"A tree structure for dynamic facility location","external_id":{"arxiv":["1909.06653"]},"day":"14","oa":1,"type":"conference","main_file_link":[{"open_access":"1","url":"https://doi.org/10.4230/LIPIcs.ESA.2018.39"}],"publication_status":"published","year":"2018","publisher":"Schloss Dagstuhl - Leibniz-Zentrum für Informatik","date_created":"2022-08-12T08:20:57Z","quality_controlled":"1","_id":"11827","oa_version":"Published Version","scopus_import":"1","doi":"10.4230/LIPICS.ESA.2018.39","language":[{"iso":"eng"}],"month":"08","volume":112,"article_number":"39","publication":"26th Annual European Symposium on Algorithms","alternative_title":["LIPIcs"],"status":"public","author":[{"last_name":"Goranci","first_name":"Gramoz ","full_name":"Goranci, Gramoz "},{"orcid":"0000-0002-5008-6530","last_name":"Henzinger","first_name":"Monika H","full_name":"Henzinger, Monika H","id":"540c9bbd-f2de-11ec-812d-d04a5be85630"},{"full_name":"Leniowski, Dariusz","last_name":"Leniowski","first_name":"Dariusz"}],"date_updated":"2024-11-06T11:57:41Z","extern":"1","intvolume":" 112","citation":{"ista":"Goranci G, Henzinger M, Leniowski D. 2018. A tree structure for dynamic facility location. 26th Annual European Symposium on Algorithms. ESA: Annual European Symposium on Algorithms, LIPIcs, vol. 112, 39.","apa":"Goranci, G., Henzinger, M., & Leniowski, D. (2018). A tree structure for dynamic facility location. In 26th Annual European Symposium on Algorithms (Vol. 112). Helsinki, Finland: Schloss Dagstuhl - Leibniz-Zentrum für Informatik. https://doi.org/10.4230/LIPICS.ESA.2018.39","short":"G. Goranci, M. Henzinger, D. Leniowski, in:, 26th Annual European Symposium on Algorithms, Schloss Dagstuhl - Leibniz-Zentrum für Informatik, 2018.","ieee":"G. Goranci, M. Henzinger, and D. Leniowski, “A tree structure for dynamic facility location,” in 26th Annual European Symposium on Algorithms, Helsinki, Finland, 2018, vol. 112.","mla":"Goranci, Gramoz, et al. “A Tree Structure for Dynamic Facility Location.” 26th Annual European Symposium on Algorithms, vol. 112, 39, Schloss Dagstuhl - Leibniz-Zentrum für Informatik, 2018, doi:10.4230/LIPICS.ESA.2018.39.","chicago":"Goranci, Gramoz , Monika Henzinger, and Dariusz Leniowski. “A Tree Structure for Dynamic Facility Location.” In 26th Annual European Symposium on Algorithms, Vol. 112. Schloss Dagstuhl - Leibniz-Zentrum für Informatik, 2018. https://doi.org/10.4230/LIPICS.ESA.2018.39.","ama":"Goranci G, Henzinger M, Leniowski D. A tree structure for dynamic facility location. In: 26th Annual European Symposium on Algorithms. Vol 112. Schloss Dagstuhl - Leibniz-Zentrum für Informatik; 2018. doi:10.4230/LIPICS.ESA.2018.39"},"abstract":[{"text":"We study the metric facility location problem with client insertions and deletions. This setting differs from the classic dynamic facility location problem, where the set of clients remains the same, but the metric space can change over time. We show a deterministic algorithm that maintains a constant factor approximation to the optimal solution in worst-case time O~(2^{O(kappa^2)}) per client insertion or deletion in metric spaces while answering queries about the cost in O(1) time, where kappa denotes the doubling dimension of the metric. For metric spaces with bounded doubling dimension, the update time is polylogarithmic in the parameters of the problem.","lang":"eng"}],"conference":{"location":"Helsinki, Finland","name":"ESA: Annual European Symposium on Algorithms","start_date":"2018-08-20","end_date":"2018-08-22"},"date_published":"2018-08-14T00:00:00Z"}]