[{"quality_controlled":"1","main_file_link":[{"url":"https://arxiv.org/abs/1610.04908","open_access":"1"}],"type":"journal_article","date_updated":"2023-09-20T11:30:58Z","_id":"1120","publisher":"American Physical Society","doi":"10.1103/PhysRevA.95.033608","article_processing_charge":"No","date_published":"2017-03-06T00:00:00Z","ec_funded":1,"project":[{"call_identifier":"H2020","name":"Analysis of quantum many-body systems","grant_number":"694227","_id":"25C6DC12-B435-11E9-9278-68D0E5697425"},{"grant_number":"P27533_N27","name":"Structure of the Excitation Spectrum for Many-Body Quantum Systems","call_identifier":"FWF","_id":"25C878CE-B435-11E9-9278-68D0E5697425"},{"_id":"26031614-B435-11E9-9278-68D0E5697425","call_identifier":"FWF","grant_number":"P29902","name":"Quantum rotations in the presence of a many-body environment"}],"publication":"Physical Review A","status":"public","publist_id":"6242","external_id":{"isi":["000395981900009"]},"related_material":{"record":[{"status":"public","relation":"dissertation_contains","id":"8958"}]},"isi":1,"year":"2017","publication_identifier":{"issn":["24699926"]},"publication_status":"published","intvolume":"        95","abstract":[{"lang":"eng","text":"The existence of a self-localization transition in the polaron problem has been under an active debate ever since Landau suggested it 83 years ago. Here we reveal the self-localization transition for the rotational analogue of the polaron -- the angulon quasiparticle. We show that, unlike for the polarons, self-localization of angulons occurs at finite impurity-bath coupling already at the mean-field level. The transition is accompanied by the spherical-symmetry breaking of the angulon ground state and a discontinuity in the first derivative of the ground-state energy. Moreover, the type of the symmetry breaking is dictated by the symmetry of the microscopic impurity-bath interaction, which leads to a number of distinct self-localized states. The predicted effects can potentially be addressed in experiments on cold molecules trapped in superfluid helium droplets and ultracold quantum gases, as well as on electronic excitations in solids and Bose-Einstein condensates. "}],"date_created":"2018-12-11T11:50:15Z","volume":95,"oa_version":"Published Version","title":"Angular self-localization of impurities rotating in a bosonic bath","author":[{"last_name":"Li","id":"4B7E523C-F248-11E8-B48F-1D18A9856A87","full_name":"Li, Xiang","first_name":"Xiang"},{"orcid":"0000-0002-6781-0521","first_name":"Robert","last_name":"Seiringer","id":"4AFD0470-F248-11E8-B48F-1D18A9856A87","full_name":"Seiringer, Robert"},{"orcid":"0000-0002-6990-7802","first_name":"Mikhail","id":"37CB05FA-F248-11E8-B48F-1D18A9856A87","full_name":"Lemeshko, Mikhail","last_name":"Lemeshko"}],"scopus_import":"1","day":"06","user_id":"c635000d-4b10-11ee-a964-aac5a93f6ac1","issue":"3","citation":{"chicago":"Li, Xiang, Robert Seiringer, and Mikhail Lemeshko. “Angular Self-Localization of Impurities Rotating in a Bosonic Bath.” <i>Physical Review A</i>. American Physical Society, 2017. <a href=\"https://doi.org/10.1103/PhysRevA.95.033608\">https://doi.org/10.1103/PhysRevA.95.033608</a>.","ista":"Li X, Seiringer R, Lemeshko M. 2017. Angular self-localization of impurities rotating in a bosonic bath. Physical Review A. 95(3), 033608.","mla":"Li, Xiang, et al. “Angular Self-Localization of Impurities Rotating in a Bosonic Bath.” <i>Physical Review A</i>, vol. 95, no. 3, 033608, American Physical Society, 2017, doi:<a href=\"https://doi.org/10.1103/PhysRevA.95.033608\">10.1103/PhysRevA.95.033608</a>.","apa":"Li, X., Seiringer, R., &#38; Lemeshko, M. (2017). Angular self-localization of impurities rotating in a bosonic bath. <i>Physical Review A</i>. American Physical Society. <a href=\"https://doi.org/10.1103/PhysRevA.95.033608\">https://doi.org/10.1103/PhysRevA.95.033608</a>","ama":"Li X, Seiringer R, Lemeshko M. Angular self-localization of impurities rotating in a bosonic bath. <i>Physical Review A</i>. 2017;95(3). doi:<a href=\"https://doi.org/10.1103/PhysRevA.95.033608\">10.1103/PhysRevA.95.033608</a>","short":"X. Li, R. Seiringer, M. Lemeshko, Physical Review A 95 (2017).","ieee":"X. Li, R. Seiringer, and M. Lemeshko, “Angular self-localization of impurities rotating in a bosonic bath,” <i>Physical Review A</i>, vol. 95, no. 3. American Physical Society, 2017."},"language":[{"iso":"eng"}],"oa":1,"article_number":"033608","department":[{"_id":"MiLe"},{"_id":"RoSe"}],"month":"03"},{"ddc":["580"],"page":"131","type":"dissertation","_id":"1127","date_updated":"2025-05-07T11:12:27Z","publisher":"Institute of Science and Technology Austria","article_processing_charge":"No","alternative_title":["ISTA Thesis"],"date_published":"2017-01-12T00:00:00Z","acknowledgement":"I would like to first acknowledge my supervisor Jiří Friml for support, kind advice and patience. It was a pleasure to be a part of your lab, Jiří. I will remember the atmosphere present in auxin lab at VIB in Ghent and at IST in Klosterneuburg forever. I would like to thank all past and present lab members for the friendship and friendly and scientific environment in the groups. It was so nice to cooperate with you, guys. There was always someone who helped me with experiments, troubleshoot issues coming from our work etc. At this place, I would like to thank especially to Gergo Molnár. I’m happy (and lucky) that I have met him; he naturally became my tutor and guide through my PhD. From no one else during my entire professional career, I’ve learned that much.","status":"public","degree_awarded":"PhD","publist_id":"6233","related_material":{"record":[{"id":"449","relation":"part_of_dissertation","status":"public"}]},"year":"2017","file_date_updated":"2021-02-22T11:52:56Z","publication_identifier":{"issn":["2663-337X"]},"publication_status":"published","abstract":[{"text":"Plant hormone auxin and its transport between cells belong to the most important\r\nmechanisms controlling plant development. Auxin itself could change localization of PINs and\r\nthereby control direction of its own flow. We performed an expression profiling experiment\r\nin Arabidopsis roots to identify potential regulators of PIN polarity which are transcriptionally\r\nregulated by auxin signalling. We identified several novel regulators and performed a detailed\r\ncharacterization of the transcription factor WRKY23 (At2g47260) and its role in auxin\r\nfeedback on PIN polarity. Gain-of-function and dominant-negative mutants revealed that\r\nWRKY23 plays a crucial role in mediating the auxin effect on PIN polarity. In concordance,\r\ntypical polar auxin transport processes such as gravitropism and leaf vascular pattern\r\nformation were disturbed by interfering with WRKY23 function.\r\nIn order to identify direct targets of WRKY23, we performed consequential expression\r\nprofiling experiments using a WRKY23 inducible gain-of-function line and dominant-negative\r\nWRKY23 line that is defunct in PIN re-arrangement. Among several genes mostly related to\r\nthe groups of cell wall and defense process regulators, we identified LYSINE-HISTIDINE\r\nTRANSPORTER 1 (LHT1; At5g40780), a small amino acid permease gene from the amino\r\nacid/auxin permease family (AAAP), we present its detailed characterisation in auxin feedback\r\non PIN repolarization, identified its transcriptional regulation, we propose a potential\r\nmechanism of its action. Moreover, we identified also a member of receptor-like protein\r\nkinase LRR-RLK (LEUCINE-RICH REPEAT TRANSMEMBRANE PROTEIN KINASE PROTEIN 1;\r\nLRRK1; At1g05700), which also affects auxin-dependent PIN re-arrangement. We described\r\nits transcriptional behaviour, subcellular localization. Based on global expression data, we\r\ntried to identify ligand responsible for mechanism of signalling and suggest signalling partner\r\nand interactors. Additionally, we described role of novel phytohormone group, strigolactone,\r\nin auxin-dependent PIN re-arrangement, that could be a fundament for future studies in this\r\nfield.\r\nOur results provide first insights into an auxin transcriptional network targeting PIN\r\nlocalization and thus regulating plant development. We highlighted WRKY23 transcriptional\r\nnetwork and characterised its mediatory role in plant development. We identified direct\r\neffectors of this network, LHT1 and LRRK1, and describe their roles in PIN re-arrangement and\r\nPIN-dependent auxin transport processes.","lang":"eng"}],"has_accepted_license":"1","date_created":"2018-12-11T11:50:17Z","title":"Identification of novel regulators of PIN polarity and development of novel auxin sensor","oa_version":"Published Version","day":"12","author":[{"full_name":"Prat, Tomas","id":"3DA3BFEE-F248-11E8-B48F-1D18A9856A87","last_name":"Prat","first_name":"Tomas"}],"user_id":"c635000d-4b10-11ee-a964-aac5a93f6ac1","citation":{"mla":"Prat, Tomas. <i>Identification of Novel Regulators of PIN Polarity and Development of Novel Auxin Sensor</i>. Institute of Science and Technology Austria, 2017.","apa":"Prat, T. (2017). <i>Identification of novel regulators of PIN polarity and development of novel auxin sensor</i>. Institute of Science and Technology Austria.","chicago":"Prat, Tomas. “Identification of Novel Regulators of PIN Polarity and Development of Novel Auxin Sensor.” Institute of Science and Technology Austria, 2017.","ista":"Prat T. 2017. Identification of novel regulators of PIN polarity and development of novel auxin sensor. Institute of Science and Technology Austria.","short":"T. Prat, Identification of Novel Regulators of PIN Polarity and Development of Novel Auxin Sensor, Institute of Science and Technology Austria, 2017.","ieee":"T. Prat, “Identification of novel regulators of PIN polarity and development of novel auxin sensor,” Institute of Science and Technology Austria, 2017.","ama":"Prat T. Identification of novel regulators of PIN polarity and development of novel auxin sensor. 2017."},"language":[{"iso":"eng"}],"oa":1,"file":[{"file_size":10285946,"date_created":"2019-04-05T08:45:14Z","date_updated":"2019-04-05T08:45:14Z","creator":"dernst","file_id":"6209","file_name":"IST_Austria_Thesis_Tomáš_Prát.pdf","content_type":"application/pdf","access_level":"closed","relation":"main_file","checksum":"d192c7c6c5ea32c8432437286dc4909e"},{"checksum":"bab18b52cf98145926042d8ed99fdb3b","relation":"main_file","content_type":"application/pdf","access_level":"open_access","file_name":"2017_Thesis_Prat.pdf","success":1,"file_id":"9185","creator":"dernst","date_updated":"2021-02-22T11:52:56Z","file_size":9802991,"date_created":"2021-02-22T11:52:56Z"}],"department":[{"_id":"JiFr"}],"month":"01","supervisor":[{"last_name":"Friml","id":"4159519E-F248-11E8-B48F-1D18A9856A87","full_name":"Friml, Jiří","orcid":"0000-0002-8302-7596","first_name":"Jiří"}]},{"has_accepted_license":"1","intvolume":"       355","abstract":[{"lang":"eng","text":"The hippocampus is thought to initiate systems-wide mnemonic processes through the reactivation of previously acquired spatial and episodic memory traces, which can recruit the entorhinal cortex as a first stage of memory redistribution to other brain areas. Hippocampal reactivation occurs during sharp wave-ripples, in which synchronous network firing encodes sequences of places.We investigated the coordination of this replay by recording assembly activity simultaneously in the CA1 region of the hippocampus and superficial layers of the medial entorhinal cortex. We found that entorhinal cell assemblies can replay trajectories independently of the hippocampus and sharp wave-ripples. This suggests that the hippocampus is not the sole initiator of spatial and episodic memory trace reactivation. Memory systems involved in these processes may include nonhierarchical, parallel components."}],"publication_status":"published","publication_identifier":{"issn":["00368075"]},"file_date_updated":"2018-12-12T10:10:22Z","author":[{"first_name":"Joseph","full_name":"O'Neill, Joseph","id":"426376DC-F248-11E8-B48F-1D18A9856A87","last_name":"O'Neill"},{"full_name":"Boccara, Charlotte","id":"3FC06552-F248-11E8-B48F-1D18A9856A87","last_name":"Boccara","orcid":"0000-0001-7237-5109","first_name":"Charlotte"},{"orcid":"0000-0001-9439-3148","first_name":"Federico","last_name":"Stella","full_name":"Stella, Federico","id":"39AF1E74-F248-11E8-B48F-1D18A9856A87"},{"first_name":"Philipp","full_name":"Schönenberger, Philipp","id":"3B9D816C-F248-11E8-B48F-1D18A9856A87","last_name":"Schönenberger"},{"last_name":"Csicsvari","full_name":"Csicsvari, Jozsef L","id":"3FA14672-F248-11E8-B48F-1D18A9856A87","first_name":"Jozsef L","orcid":"0000-0002-5193-4036"}],"scopus_import":"1","day":"13","title":"Superficial layers of the medial entorhinal cortex replay independently of the hippocampus","oa_version":"Submitted Version","volume":355,"date_created":"2018-12-11T11:50:19Z","oa":1,"language":[{"iso":"eng"}],"pubrep_id":"976","issue":"6321","citation":{"mla":"O’Neill, Joseph, et al. “Superficial Layers of the Medial Entorhinal Cortex Replay Independently of the Hippocampus.” <i>Science</i>, vol. 355, no. 6321, American Association for the Advancement of Science, 2017, pp. 184–88, doi:<a href=\"https://doi.org/10.1126/science.aag2787\">10.1126/science.aag2787</a>.","apa":"O’Neill, J., Boccara, C. N., Stella, F., Schönenberger, P., &#38; Csicsvari, J. L. (2017). Superficial layers of the medial entorhinal cortex replay independently of the hippocampus. <i>Science</i>. American Association for the Advancement of Science. <a href=\"https://doi.org/10.1126/science.aag2787\">https://doi.org/10.1126/science.aag2787</a>","ista":"O’Neill J, Boccara CN, Stella F, Schönenberger P, Csicsvari JL. 2017. Superficial layers of the medial entorhinal cortex replay independently of the hippocampus. Science. 355(6321), 184–188.","chicago":"O’Neill, Joseph, Charlotte N. Boccara, Federico Stella, Philipp Schönenberger, and Jozsef L Csicsvari. “Superficial Layers of the Medial Entorhinal Cortex Replay Independently of the Hippocampus.” <i>Science</i>. American Association for the Advancement of Science, 2017. <a href=\"https://doi.org/10.1126/science.aag2787\">https://doi.org/10.1126/science.aag2787</a>.","short":"J. O’Neill, C.N. Boccara, F. Stella, P. Schönenberger, J.L. Csicsvari, Science 355 (2017) 184–188.","ieee":"J. O’Neill, C. N. Boccara, F. Stella, P. Schönenberger, and J. L. Csicsvari, “Superficial layers of the medial entorhinal cortex replay independently of the hippocampus,” <i>Science</i>, vol. 355, no. 6321. American Association for the Advancement of Science, pp. 184–188, 2017.","ama":"O’Neill J, Boccara CN, Stella F, Schönenberger P, Csicsvari JL. Superficial layers of the medial entorhinal cortex replay independently of the hippocampus. <i>Science</i>. 2017;355(6321):184-188. doi:<a href=\"https://doi.org/10.1126/science.aag2787\">10.1126/science.aag2787</a>"},"user_id":"c635000d-4b10-11ee-a964-aac5a93f6ac1","month":"01","department":[{"_id":"JoCs"}],"file":[{"file_id":"4809","date_updated":"2018-12-12T10:10:22Z","creator":"system","file_size":3761201,"date_created":"2018-12-12T10:10:22Z","relation":"main_file","access_level":"open_access","content_type":"application/pdf","file_name":"IST-2018-976-v1+1_2017Preprint_ONeill_Superficial_layers.pdf"}],"page":"184 - 188","ddc":["571"],"quality_controlled":"1","doi":"10.1126/science.aag2787","article_processing_charge":"No","publisher":"American Association for the Advancement of Science","date_updated":"2023-09-20T11:30:35Z","_id":"1132","type":"journal_article","project":[{"_id":"257A4776-B435-11E9-9278-68D0E5697425","call_identifier":"FP7","grant_number":"281511","name":"Memory-related information processing in neuronal circuits of the hippocampus and entorhinal cortex"}],"publication":"Science","status":"public","ec_funded":1,"date_published":"2017-01-13T00:00:00Z","year":"2017","isi":1,"external_id":{"isi":["000391743700044"]},"publist_id":"6226"},{"month":"02","article_number":"085302","department":[{"_id":"MiLe"}],"language":[{"iso":"eng"}],"oa":1,"user_id":"c635000d-4b10-11ee-a964-aac5a93f6ac1","citation":{"short":"E. Yakaboylu, M. Lemeshko, Physical Review Letters 118 (2017).","ieee":"E. Yakaboylu and M. Lemeshko, “Anomalous screening of quantum impurities by a neutral environment,” <i>Physical Review Letters</i>, vol. 118, no. 8. American Physical Society, 2017.","ama":"Yakaboylu E, Lemeshko M. Anomalous screening of quantum impurities by a neutral environment. <i>Physical Review Letters</i>. 2017;118(8). doi:<a href=\"https://doi.org/10.1103/PhysRevLett.118.085302\">10.1103/PhysRevLett.118.085302</a>","mla":"Yakaboylu, Enderalp, and Mikhail Lemeshko. “Anomalous Screening of Quantum Impurities by a Neutral Environment.” <i>Physical Review Letters</i>, vol. 118, no. 8, 085302, American Physical Society, 2017, doi:<a href=\"https://doi.org/10.1103/PhysRevLett.118.085302\">10.1103/PhysRevLett.118.085302</a>.","apa":"Yakaboylu, E., &#38; Lemeshko, M. (2017). Anomalous screening of quantum impurities by a neutral environment. <i>Physical Review Letters</i>. American Physical Society. <a href=\"https://doi.org/10.1103/PhysRevLett.118.085302\">https://doi.org/10.1103/PhysRevLett.118.085302</a>","chicago":"Yakaboylu, Enderalp, and Mikhail Lemeshko. “Anomalous Screening of Quantum Impurities by a Neutral Environment.” <i>Physical Review Letters</i>. American Physical Society, 2017. <a href=\"https://doi.org/10.1103/PhysRevLett.118.085302\">https://doi.org/10.1103/PhysRevLett.118.085302</a>.","ista":"Yakaboylu E, Lemeshko M. 2017. Anomalous screening of quantum impurities by a neutral environment. Physical Review Letters. 118(8), 085302."},"issue":"8","title":"Anomalous screening of quantum impurities by a neutral environment","oa_version":"Submitted Version","day":"22","scopus_import":"1","author":[{"last_name":"Yakaboylu","id":"38CB71F6-F248-11E8-B48F-1D18A9856A87","full_name":"Yakaboylu, Enderalp","first_name":"Enderalp","orcid":"0000-0001-5973-0874"},{"orcid":"0000-0002-6990-7802","first_name":"Mikhail","last_name":"Lemeshko","id":"37CB05FA-F248-11E8-B48F-1D18A9856A87","full_name":"Lemeshko, Mikhail"}],"date_created":"2018-12-11T11:50:19Z","volume":118,"abstract":[{"text":"It is a common knowledge that an effective interaction of a quantum impurity with an electromagnetic field can be screened by surrounding charge carriers, whether mobile or static. Here we demonstrate that very strong, \"anomalous\" screening can take place in the presence of a neutral, weakly polarizable environment, due to an exchange of orbital angular momentum between the impurity and the bath. Furthermore, we show that it is possible to generalize all phenomena related to isolated impurities in an external field to the case when a many-body environment is present, by casting the problem in terms of the angulon quasiparticle. As a result, the relevant observables such as the effective Rabi frequency, geometric phase, and impurity spatial alignment are straightforward to evaluate in terms of a single parameter: the angular-momentum-dependent screening factor.","lang":"eng"}],"intvolume":"       118","publication_status":"published","publication_identifier":{"issn":["00319007"]},"external_id":{"isi":["000394667600003"]},"isi":1,"year":"2017","publist_id":"6225","status":"public","publication":"Physical Review Letters","project":[{"_id":"25681D80-B435-11E9-9278-68D0E5697425","call_identifier":"FP7","grant_number":"291734","name":"International IST Postdoc Fellowship Programme"},{"call_identifier":"FWF","name":"Quantum rotations in the presence of a many-body environment","grant_number":"P29902","_id":"26031614-B435-11E9-9278-68D0E5697425"}],"date_published":"2017-02-22T00:00:00Z","ec_funded":1,"publisher":"American Physical Society","article_processing_charge":"No","doi":"10.1103/PhysRevLett.118.085302","type":"journal_article","_id":"1133","date_updated":"2023-09-20T11:30:08Z","quality_controlled":"1","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1612.02820"}]},{"ddc":["510"],"quality_controlled":"1","publisher":"Institute of Mathematical Statistics","doi":"10.1214/16-ECP38","type":"journal_article","date_updated":"2023-09-07T12:54:12Z","_id":"1144","project":[{"call_identifier":"FP7","grant_number":"338804","name":"Random matrices, universality and disordered quantum systems","_id":"258DCDE6-B435-11E9-9278-68D0E5697425"}],"status":"public","publication":"Electronic Communications in Probability","acknowledgement":"Partially supported by the IST Austria Excellence Scholarship.","date_published":"2017-01-02T00:00:00Z","ec_funded":1,"related_material":{"record":[{"id":"6179","status":"public","relation":"dissertation_contains"}]},"year":"2017","publist_id":"6214","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png","short":"CC BY (4.0)"},"abstract":[{"text":"We show that matrix elements of functions of N × N Wigner matrices fluctuate on a scale of order N−1/2 and we identify the limiting fluctuation. Our result holds for any function f of the matrix that has bounded variation thus considerably relaxing the regularity requirement imposed in [7, 11].","lang":"eng"}],"intvolume":"        21","has_accepted_license":"1","publication_status":"published","file_date_updated":"2018-12-12T10:18:10Z","oa_version":"Published Version","title":"Fluctuations of functions of Wigner matrices","author":[{"last_name":"Erdös","id":"4DBD5372-F248-11E8-B48F-1D18A9856A87","full_name":"Erdös, László","first_name":"László","orcid":"0000-0001-5366-9603"},{"full_name":"Schröder, Dominik J","id":"408ED176-F248-11E8-B48F-1D18A9856A87","last_name":"Schröder","orcid":"0000-0002-2904-1856","first_name":"Dominik J"}],"day":"02","scopus_import":1,"date_created":"2018-12-11T11:50:23Z","volume":21,"pubrep_id":"747","language":[{"iso":"eng"}],"oa":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"short":"L. Erdös, D.J. Schröder, Electronic Communications in Probability 21 (2017).","ieee":"L. Erdös and D. J. Schröder, “Fluctuations of functions of Wigner matrices,” <i>Electronic Communications in Probability</i>, vol. 21. Institute of Mathematical Statistics, 2017.","ama":"Erdös L, Schröder DJ. Fluctuations of functions of Wigner matrices. <i>Electronic Communications in Probability</i>. 2017;21. doi:<a href=\"https://doi.org/10.1214/16-ECP38\">10.1214/16-ECP38</a>","mla":"Erdös, László, and Dominik J. Schröder. “Fluctuations of Functions of Wigner Matrices.” <i>Electronic Communications in Probability</i>, vol. 21, 86, Institute of Mathematical Statistics, 2017, doi:<a href=\"https://doi.org/10.1214/16-ECP38\">10.1214/16-ECP38</a>.","apa":"Erdös, L., &#38; Schröder, D. J. (2017). Fluctuations of functions of Wigner matrices. <i>Electronic Communications in Probability</i>. Institute of Mathematical Statistics. <a href=\"https://doi.org/10.1214/16-ECP38\">https://doi.org/10.1214/16-ECP38</a>","chicago":"Erdös, László, and Dominik J Schröder. “Fluctuations of Functions of Wigner Matrices.” <i>Electronic Communications in Probability</i>. Institute of Mathematical Statistics, 2017. <a href=\"https://doi.org/10.1214/16-ECP38\">https://doi.org/10.1214/16-ECP38</a>.","ista":"Erdös L, Schröder DJ. 2017. Fluctuations of functions of Wigner matrices. Electronic Communications in Probability. 21, 86."},"month":"01","article_number":"86","file":[{"file_id":"5329","file_size":440770,"date_created":"2018-12-12T10:18:10Z","creator":"system","date_updated":"2018-12-12T10:18:10Z","relation":"main_file","file_name":"IST-2017-747-v1+1_euclid.ecp.1483347665.pdf","content_type":"application/pdf","access_level":"open_access"}],"department":[{"_id":"LaEr"}]},{"acknowledgement":"We thank all the participants for their contribution to this study and volunteers from the Nursing School of Dalian University for their supporting to collect blood and urine samples of the participants. We also thank Dr. Yasunori Takayama from National Institute for Physiological Sciences of Japan for his kind help.","date_published":"2017-08-01T00:00:00Z","publication":"Clinical Nutrition","status":"public","publist_id":"6212","year":"2017","quality_controlled":"1","page":"1136-1142","type":"journal_article","_id":"1146","date_updated":"2023-10-16T11:09:39Z","publisher":"Elsevier","article_processing_charge":"No","doi":"10.1016/j.clnu.2016.07.016","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"ama":"Sun W, Zhai M-Z, Li D, et al. Comparison of the effects of nicotinic acid and nicotinamide degradation on plasma betaine and choline levels. <i>Clinical Nutrition</i>. 2017;36(4):1136-1142. doi:<a href=\"https://doi.org/10.1016/j.clnu.2016.07.016\">10.1016/j.clnu.2016.07.016</a>","ieee":"W. Sun <i>et al.</i>, “Comparison of the effects of nicotinic acid and nicotinamide degradation on plasma betaine and choline levels,” <i>Clinical Nutrition</i>, vol. 36, no. 4. Elsevier, pp. 1136–1142, 2017.","short":"W. Sun, M.-Z. Zhai, D. Li, Y. Zhou, N. Chen, M. Guo, S. Zhou, Clinical Nutrition 36 (2017) 1136–1142.","ista":"Sun W, Zhai M-Z, Li D, Zhou Y, Chen N, Guo M, Zhou S. 2017. Comparison of the effects of nicotinic acid and nicotinamide degradation on plasma betaine and choline levels. Clinical Nutrition. 36(4), 1136–1142.","chicago":"Sun, Wuping, Ming-Zhu Zhai, Da Li, Yiming Zhou, Nana Chen, Ming Guo, and Shisheng Zhou. “Comparison of the Effects of Nicotinic Acid and Nicotinamide Degradation on Plasma Betaine and Choline Levels.” <i>Clinical Nutrition</i>. Elsevier, 2017. <a href=\"https://doi.org/10.1016/j.clnu.2016.07.016\">https://doi.org/10.1016/j.clnu.2016.07.016</a>.","apa":"Sun, W., Zhai, M.-Z., Li, D., Zhou, Y., Chen, N., Guo, M., &#38; Zhou, S. (2017). Comparison of the effects of nicotinic acid and nicotinamide degradation on plasma betaine and choline levels. <i>Clinical Nutrition</i>. Elsevier. <a href=\"https://doi.org/10.1016/j.clnu.2016.07.016\">https://doi.org/10.1016/j.clnu.2016.07.016</a>","mla":"Sun, Wuping, et al. “Comparison of the Effects of Nicotinic Acid and Nicotinamide Degradation on Plasma Betaine and Choline Levels.” <i>Clinical Nutrition</i>, vol. 36, no. 4, Elsevier, 2017, pp. 1136–42, doi:<a href=\"https://doi.org/10.1016/j.clnu.2016.07.016\">10.1016/j.clnu.2016.07.016</a>."},"issue":"4","language":[{"iso":"eng"}],"department":[{"_id":"RySh"}],"month":"08","publication_status":"published","publication_identifier":{"issn":["0261-5614"]},"abstract":[{"text":"Aim: The present study was to compare the effects of nicotinic acid and nicotinamide on the plasma methyl donors, choline and betaine. Methods: Thirty adult subjects were randomly divided into three groups of equal size, and orally received purified water (C group), nicotinic acid (300 mg, NA group) or nicotinamide (300 mg, NM group). Plasma nicotinamide, N 1-methylnicotinamide, homocysteine, betaine and choline levels before and 1.5-h and 3-h post-dosing, plasma normetanephrine and metanephrine concentrations at 3-h post-dosing, and the urinary excretion of N 1-methyl-2-pyridone-5-carboxamide during the test period were examined. Results: The level of 3-h plasma nicotinamide, N 1-methylnicotinamide, homocysteine, the urinary excretion of N 1-methyl-2-pyridone-5-carboxamide and pulse pressure (PP) in the NM group was 221%, 3972%, 61%, 1728% and 21.2% higher than that of the control group (P &lt; 0.01, except homocysteine and PP P &lt; 0.05), while the 3-h plasma betaine, normetanephrine and metanephrine level in the NM group was 24.4%, 9.4% and 11.7% lower (P &lt; 0.05, except betaine P &lt; 0.01), without significant difference in choline levels. Similar but less pronounced changes were observed in the NA group, with a lower level of 3-h plasma N 1-methylnicotinamide (1.90 ± 0.20 μmol/l vs. 3.62 ± 0.27 μmol/l, P &lt; 0.01) and homocysteine (12.85 ± 1.39 μmol/l vs. 18.08 ± 1.02 μmol/l, P &lt; 0.05) but a higher level of betaine (27.44 ± 0.71 μmol/l vs. 23.52 ± 0.61 μmol/l, P &lt; 0.05) than that of the NM group. Conclusion: The degradation of nicotinamide consumes more betaine than that of nicotinic acid at identical doses. This difference should be taken into consideration in niacin fortification. © 2016 Elsevier Ltd and European Society for Clinical Nutrition and Metabolism.","lang":"eng"}],"intvolume":"        36","date_created":"2018-12-11T11:50:24Z","volume":36,"oa_version":"None","title":"Comparison of the effects of nicotinic acid and nicotinamide degradation on plasma betaine and choline levels","scopus_import":"1","day":"01","author":[{"first_name":"Wuping","last_name":"Sun","full_name":"Sun, Wuping"},{"last_name":"Zhai","id":"34009CFA-F248-11E8-B48F-1D18A9856A87","full_name":"Zhai, Ming-Zhu","first_name":"Ming-Zhu"},{"first_name":"Da","full_name":"Li, Da","last_name":"Li"},{"full_name":"Zhou, Yiming","last_name":"Zhou","first_name":"Yiming"},{"first_name":"Nana","last_name":"Chen","full_name":"Chen, Nana"},{"last_name":"Guo","full_name":"Guo, Ming","first_name":"Ming"},{"full_name":"Zhou, Shisheng","last_name":"Zhou","first_name":"Shisheng"}]},{"quality_controlled":"1","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1709.06569"}],"type":"journal_article","_id":"11518","date_updated":"2022-08-18T10:23:35Z","publisher":"IOP Publishing","article_processing_charge":"No","doi":"10.3847/1538-4357/aa9931","acknowledgement":"We thank the referee for their constructive comments, which have helped improve the quality and clarity of this work. We thank Raffaella Schneider for comments on an earlier version of this paper. We thank Leindert Boogaard, Steven Bos, Rychard Bouwens, and Renske Smit for discussions. J.M. acknowledges the support of a Huygens PhD fellowship from Leiden University. D.S. acknowledges financial support from the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship and from Lancaster University through an Early Career Internal Grant A100679. A.F. acknowledges support from the ERC Advanced Grant INTERSTELLAR H2020/740120. B.D. acknowledges financial support from NASA through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 294.A-5018. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2015.1.00122.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ.","date_published":"2017-12-21T00:00:00Z","extern":"1","status":"public","publication":"The Astrophysical Journal","keyword":["Space and Planetary Science","Astronomy and Astrophysics","dark ages","reionization","first stars – galaxies: formation – galaxies: high-redshift – galaxies: ISM – galaxies: kinematics and dynamics"],"external_id":{"arxiv":["1709.06569"]},"year":"2017","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"publication_status":"published","intvolume":"       851","abstract":[{"text":"We present spectroscopic follow-up observations of CR7 with ALMA, targeted at constraining the infrared (IR) continuum and [C II]158 mm line-emission at high spatial resolution matched to the HST/WFC3 imaging. CR7 is a luminous Lyα emitting galaxy at z = 6.6 that consists of three separated UV-continuum components. Our observations reveal several well-separated components of [C II] emission. The two most luminous components in [C II] coincide with the brightest UV components (A and B), blueshifted by »150 km s−1 with respect to the\r\npeak of Lyα emission. Other [C II] components are observed close to UV clumps B and C and are blueshifted by »300 and ≈80 km s−1 with respect to the systemic redshift. We do not detect FIR continuum emission due to dust with a 3σ limiting luminosity LIR T L d 35 K 3.1 10 = <´ 10 ( ) . This allows us to mitigate uncertainties in the dust-corrected SFR and derive SFRs for the three UV clumps A, B, and C of 28, 5, and 7 M yr−1. All clumps have [C II] luminosities consistent within the scatter observed in the local relation between SFR and L[ ] C II , implying that strong Lyα emission does not necessarily anti-correlate with [C II] luminosity. Combining\r\nour measurements with the literature, we show that galaxies with blue UV slopes have weaker [C II] emission at fixed SFR, potentially due to their lower metallicities and/or higher photoionization. Comparison with hydrodynamical simulations suggests that CR7ʼs clumps have metallicities of 0.1 Z Z 0.2 < < . The observed ISM structure of CR7 indicates that we are likely witnessing the build up of a central galaxy in the early universe through complex accretion of satellites.","lang":"eng"}],"date_created":"2022-07-07T08:48:04Z","article_type":"original","volume":851,"oa_version":"Preprint","title":"ALMA reveals metals yet no dust within multiple components in CR7","scopus_import":"1","day":"21","author":[{"orcid":"0000-0003-2871-127X","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee"},{"last_name":"Sobral","full_name":"Sobral, D.","first_name":"D."},{"first_name":"F.","full_name":"Boone, F.","last_name":"Boone"},{"last_name":"Röttgering","full_name":"Röttgering, H.","first_name":"H."},{"full_name":"Schaerer, D.","last_name":"Schaerer","first_name":"D."},{"first_name":"M.","full_name":"Girard, M.","last_name":"Girard"},{"full_name":"Pallottini, A.","last_name":"Pallottini","first_name":"A."},{"first_name":"L.","full_name":"Vallini, L.","last_name":"Vallini"},{"last_name":"Ferrara","full_name":"Ferrara, A.","first_name":"A."},{"full_name":"Darvish, B.","last_name":"Darvish","first_name":"B."},{"last_name":"Mobasher","full_name":"Mobasher, B.","first_name":"B."}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"chicago":"Matthee, Jorryt J, D. Sobral, F. Boone, H. Röttgering, D. Schaerer, M. Girard, A. Pallottini, et al. “ALMA Reveals Metals yet No Dust within Multiple Components in CR7.” <i>The Astrophysical Journal</i>. IOP Publishing, 2017. <a href=\"https://doi.org/10.3847/1538-4357/aa9931\">https://doi.org/10.3847/1538-4357/aa9931</a>.","ista":"Matthee JJ, Sobral D, Boone F, Röttgering H, Schaerer D, Girard M, Pallottini A, Vallini L, Ferrara A, Darvish B, Mobasher B. 2017. ALMA reveals metals yet no dust within multiple components in CR7. The Astrophysical Journal. 851(2), 145.","mla":"Matthee, Jorryt J., et al. “ALMA Reveals Metals yet No Dust within Multiple Components in CR7.” <i>The Astrophysical Journal</i>, vol. 851, no. 2, 145, IOP Publishing, 2017, doi:<a href=\"https://doi.org/10.3847/1538-4357/aa9931\">10.3847/1538-4357/aa9931</a>.","apa":"Matthee, J. J., Sobral, D., Boone, F., Röttgering, H., Schaerer, D., Girard, M., … Mobasher, B. (2017). ALMA reveals metals yet no dust within multiple components in CR7. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/aa9931\">https://doi.org/10.3847/1538-4357/aa9931</a>","ama":"Matthee JJ, Sobral D, Boone F, et al. ALMA reveals metals yet no dust within multiple components in CR7. <i>The Astrophysical Journal</i>. 2017;851(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/aa9931\">10.3847/1538-4357/aa9931</a>","short":"J.J. Matthee, D. Sobral, F. Boone, H. Röttgering, D. Schaerer, M. Girard, A. Pallottini, L. Vallini, A. Ferrara, B. Darvish, B. Mobasher, The Astrophysical Journal 851 (2017).","ieee":"J. J. Matthee <i>et al.</i>, “ALMA reveals metals yet no dust within multiple components in CR7,” <i>The Astrophysical Journal</i>, vol. 851, no. 2. IOP Publishing, 2017."},"issue":"2","language":[{"iso":"eng"}],"oa":1,"article_number":"145","arxiv":1,"month":"12"},{"publication_identifier":{"issn":["18777503"]},"publication_status":"published","file_date_updated":"2019-01-18T08:43:16Z","abstract":[{"lang":"eng","text":"We propose a new memetic strategy that can solve the multi-physics, complex inverse problems, formulated as the multi-objective optimization ones, in which objectives are misfits between the measured and simulated states of various governing processes. The multi-deme structure of the strategy allows for both, intensive, relatively cheap exploration with a moderate accuracy and more accurate search many regions of Pareto set in parallel. The special type of selection operator prefers the coherent alternative solutions, eliminating artifacts appearing in the particular processes. The additional accuracy increment is obtained by the parallel convex searches applied to the local scalarizations of the misfit vector. The strategy is dedicated for solving ill-conditioned problems, for which inverting the single physical process can lead to the ambiguous results. The skill of the selection in artifact elimination is shown on the benchmark problem, while the whole strategy was applied for identification of oil deposits, where the misfits are related to various frequencies of the magnetic and electric waves of the magnetotelluric measurements. 2016 Elsevier B.V."}],"intvolume":"        18","has_accepted_license":"1","date_created":"2018-12-11T11:50:26Z","volume":18,"title":"A multi objective memetic inverse solver reinforced by local optimization methods","oa_version":"Submitted Version","author":[{"last_name":"Gajda-Zagorska","id":"47794CF0-F248-11E8-B48F-1D18A9856A87","full_name":"Gajda-Zagorska, Ewa P","first_name":"Ewa P"},{"first_name":"Robert","last_name":"Schaefer","full_name":"Schaefer, Robert"},{"full_name":"Smołka, Maciej","last_name":"Smołka","first_name":"Maciej"},{"first_name":"David","full_name":"Pardo, David","last_name":"Pardo"},{"first_name":"Julen","last_name":"Alvarez Aramberri","full_name":"Alvarez Aramberri, Julen"}],"scopus_import":"1","day":"01","user_id":"c635000d-4b10-11ee-a964-aac5a93f6ac1","citation":{"mla":"Gajda-Zagorska, Ewa P., et al. “A Multi Objective Memetic Inverse Solver Reinforced by Local Optimization Methods.” <i>Journal of Computational Science</i>, vol. 18, Elsevier, 2017, pp. 85–94, doi:<a href=\"https://doi.org/10.1016/j.jocs.2016.06.007\">10.1016/j.jocs.2016.06.007</a>.","apa":"Gajda-Zagorska, E. P., Schaefer, R., Smołka, M., Pardo, D., &#38; Alvarez Aramberri, J. (2017). A multi objective memetic inverse solver reinforced by local optimization methods. <i>Journal of Computational Science</i>. Elsevier. <a href=\"https://doi.org/10.1016/j.jocs.2016.06.007\">https://doi.org/10.1016/j.jocs.2016.06.007</a>","chicago":"Gajda-Zagorska, Ewa P, Robert Schaefer, Maciej Smołka, David Pardo, and Julen Alvarez Aramberri. “A Multi Objective Memetic Inverse Solver Reinforced by Local Optimization Methods.” <i>Journal of Computational Science</i>. Elsevier, 2017. <a href=\"https://doi.org/10.1016/j.jocs.2016.06.007\">https://doi.org/10.1016/j.jocs.2016.06.007</a>.","ista":"Gajda-Zagorska EP, Schaefer R, Smołka M, Pardo D, Alvarez Aramberri J. 2017. A multi objective memetic inverse solver reinforced by local optimization methods. Journal of Computational Science. 18, 85–94.","short":"E.P. Gajda-Zagorska, R. Schaefer, M. Smołka, D. Pardo, J. Alvarez Aramberri, Journal of Computational Science 18 (2017) 85–94.","ieee":"E. P. Gajda-Zagorska, R. Schaefer, M. Smołka, D. Pardo, and J. Alvarez Aramberri, “A multi objective memetic inverse solver reinforced by local optimization methods,” <i>Journal of Computational Science</i>, vol. 18. Elsevier, pp. 85–94, 2017.","ama":"Gajda-Zagorska EP, Schaefer R, Smołka M, Pardo D, Alvarez Aramberri J. A multi objective memetic inverse solver reinforced by local optimization methods. <i>Journal of Computational Science</i>. 2017;18:85-94. doi:<a href=\"https://doi.org/10.1016/j.jocs.2016.06.007\">10.1016/j.jocs.2016.06.007</a>"},"language":[{"iso":"eng"}],"oa":1,"file":[{"date_updated":"2019-01-18T08:43:16Z","creator":"dernst","file_size":1083911,"date_created":"2019-01-18T08:43:16Z","file_id":"5842","access_level":"open_access","content_type":"application/pdf","success":1,"file_name":"2016_jocs_ewa.pdf","relation":"main_file"}],"department":[{"_id":"ChWo"}],"month":"01","quality_controlled":"1","ddc":["000"],"page":"85 - 94","type":"journal_article","date_updated":"2023-09-20T11:29:44Z","_id":"1152","publisher":"Elsevier","doi":"10.1016/j.jocs.2016.06.007","article_processing_charge":"No","date_published":"2017-01-01T00:00:00Z","publication":"Journal of Computational Science","status":"public","publist_id":"6206","external_id":{"isi":["000393528700009"]},"year":"2017","isi":1},{"abstract":[{"text":"This dissertation concerns the automatic verification of probabilistic systems and programs with arrays by statistical and logical methods. Although statistical and logical methods are different in nature, we show that they can be successfully combined for system analysis. In the first part of the dissertation we present a new statistical algorithm for the verification of probabilistic systems with respect to unbounded properties, including linear temporal logic. Our algorithm often performs faster than the previous approaches, and at the same time requires less information about the system. In addition, our method can be generalized to unbounded quantitative properties such as mean-payoff bounds. In the second part, we introduce two techniques for comparing probabilistic systems. Probabilistic systems are typically compared using the notion of equivalence, which requires the systems to have the equal probability of all behaviors. However, this notion is often too strict, since probabilities are typically only empirically estimated, and any imprecision may break the relation between processes. On the one hand, we propose to replace the Boolean notion of equivalence by a quantitative distance of similarity. For this purpose, we introduce a statistical framework for estimating distances between Markov chains based on their simulation runs, and we investigate which distances can be approximated in our framework. On the other hand, we propose to compare systems with respect to a new qualitative logic, which expresses that behaviors occur with probability one or a positive probability. This qualitative analysis is robust with respect to modeling errors and applicable to many domains. In the last part, we present a new quantifier-free logic for integer arrays, which allows us to express counting. Counting properties are prevalent in array-manipulating programs, however they cannot be expressed in the quantified fragments of the theory of arrays. We present a decision procedure for our logic, and provide several complexity results.","lang":"eng"}],"has_accepted_license":"1","publication_identifier":{"issn":["2663-337X"]},"publication_status":"published","file_date_updated":"2020-07-14T12:44:34Z","oa_version":"Published Version","title":"Statistical and logical methods for property checking","author":[{"first_name":"Przemyslaw","last_name":"Daca","id":"49351290-F248-11E8-B48F-1D18A9856A87","full_name":"Daca, Przemyslaw"}],"day":"02","date_created":"2018-12-11T11:50:27Z","language":[{"iso":"eng"}],"pubrep_id":"730","oa":1,"user_id":"c635000d-4b10-11ee-a964-aac5a93f6ac1","citation":{"ama":"Daca P. Statistical and logical methods for property checking. 2017. doi:<a href=\"https://doi.org/10.15479/AT:ISTA:TH_730\">10.15479/AT:ISTA:TH_730</a>","ieee":"P. Daca, “Statistical and logical methods for property checking,” Institute of Science and Technology Austria, 2017.","short":"P. Daca, Statistical and Logical Methods for Property Checking, Institute of Science and Technology Austria, 2017.","chicago":"Daca, Przemyslaw. “Statistical and Logical Methods for Property Checking.” Institute of Science and Technology Austria, 2017. <a href=\"https://doi.org/10.15479/AT:ISTA:TH_730\">https://doi.org/10.15479/AT:ISTA:TH_730</a>.","ista":"Daca P. 2017. Statistical and logical methods for property checking. Institute of Science and Technology Austria.","apa":"Daca, P. (2017). <i>Statistical and logical methods for property checking</i>. Institute of Science and Technology Austria. <a href=\"https://doi.org/10.15479/AT:ISTA:TH_730\">https://doi.org/10.15479/AT:ISTA:TH_730</a>","mla":"Daca, Przemyslaw. <i>Statistical and Logical Methods for Property Checking</i>. Institute of Science and Technology Austria, 2017, doi:<a href=\"https://doi.org/10.15479/AT:ISTA:TH_730\">10.15479/AT:ISTA:TH_730</a>."},"month":"01","supervisor":[{"last_name":"Henzinger","full_name":"Henzinger, Thomas A","id":"40876CD8-F248-11E8-B48F-1D18A9856A87","first_name":"Thomas A","orcid":"0000−0002−2985−7724"}],"file":[{"file_id":"4880","date_created":"2018-12-12T10:11:26Z","file_size":1028586,"date_updated":"2020-07-14T12:44:34Z","creator":"system","relation":"main_file","checksum":"1406a681cb737508234fde34766be2c2","file_name":"IST-2017-730-v1+1_Statistical_and_Logical_Methods_for_Property_Checking.pdf","access_level":"open_access","content_type":"application/pdf"}],"department":[{"_id":"ToHe"}],"ddc":["004","005"],"page":"163","publisher":"Institute of Science and Technology Austria","doi":"10.15479/AT:ISTA:TH_730","alternative_title":["ISTA Thesis"],"article_processing_charge":"No","type":"dissertation","date_updated":"2023-09-07T11:58:34Z","_id":"1155","project":[{"_id":"25EE3708-B435-11E9-9278-68D0E5697425","grant_number":"267989","name":"Quantitative Reactive Modeling","call_identifier":"FP7"},{"_id":"25F42A32-B435-11E9-9278-68D0E5697425","grant_number":"Z211","name":"The Wittgenstein Prize","call_identifier":"FWF"},{"call_identifier":"FWF","name":"Rigorous Systems Engineering","grant_number":"S 11407_N23","_id":"25832EC2-B435-11E9-9278-68D0E5697425"}],"status":"public","degree_awarded":"PhD","date_published":"2017-01-02T00:00:00Z","acknowledgement":" First of all, I want to thank my advisor, prof. Thomas A. Henzinger, for his guidance during my PhD program. I am grateful for the freedom I was given to pursue my research interests, and his continuous support. Working with prof. Henzinger was a truly inspiring experience and taught me what it means to be a scientist. I want to express my gratitude to my collaborators: Nikola Beneš, Krishnendu Chatterjee, Martin Chmelík, Ashutosh Gupta, Willibald Krenn, Jan Kˇretínský, Dejan Nickovic, Andrey Kupriyanov, and Tatjana Petrov. I have learned a great deal from my collaborators, and without their help this thesis would not be possible. In addition, I want to thank the members of my thesis committee: Dirk Beyer, Dejan Nickovic, and Georg Weissenbacher for their advice and reviewing this dissertation. I would especially like to acknowledge the late Helmut Veith, who was a member of my committee. I will remember Helmut for his kindness, enthusiasm, and wit, as well as for being an inspiring scientist. Finally, I would like to thank my colleagues for making my stay at IST such a pleasant experience: Guy Avni, Sergiy Bogomolov, Ventsislav Chonev, Rasmus Ibsen-Jensen, Mirco Giacobbe, Bernhard Kragl, Hui Kong, Petr Novotný, Jan Otop, Andreas Pavlogiannis, Tantjana Petrov, Arjun Radhakrishna, Jakob Ruess, Thorsten Tarrach, as well as other members of groups Henzinger and Chatterjee. ","ec_funded":1,"related_material":{"record":[{"id":"1093","status":"public","relation":"part_of_dissertation"},{"relation":"part_of_dissertation","status":"public","id":"1230"},{"relation":"part_of_dissertation","status":"public","id":"1234"},{"relation":"part_of_dissertation","status":"public","id":"1391"},{"id":"1501","status":"public","relation":"part_of_dissertation"},{"status":"public","relation":"part_of_dissertation","id":"1502"},{"relation":"part_of_dissertation","status":"public","id":"2063"},{"id":"2167","status":"public","relation":"part_of_dissertation"}]},"year":"2017","publist_id":"6203"},{"date_published":"2017-10-01T00:00:00Z","publication":"Monthly Notices of the Royal Astronomical Society","extern":"1","status":"public","keyword":["Space and Planetary Science","Astronomy and Astrophysics galaxies","active","galaxies","evolution","galaxies","high-redshift","galaxies","luminosity function","mass function","galaxies: star formation"],"year":"2017","external_id":{"arxiv":["1702.04721"]},"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1702.04721"}],"quality_controlled":"1","page":"629-649","date_updated":"2022-08-19T07:15:14Z","_id":"11561","type":"journal_article","doi":"10.1093/mnras/stx1569","article_processing_charge":"No","publisher":"Oxford University Press","issue":"1","citation":{"mla":"Matthee, Jorryt J., et al. “Boötes-HiZELS: An Optical to near-Infrared Survey of Emission-Line Galaxies at z = 0.4–4.7.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 471, no. 1, Oxford University Press, 2017, pp. 629–49, doi:<a href=\"https://doi.org/10.1093/mnras/stx1569\">10.1093/mnras/stx1569</a>.","apa":"Matthee, J. J., Sobral, D., Best, P., Smail, I., Bian, F., Darvish, B., … Fan, X. (2017). Boötes-HiZELS: An optical to near-infrared survey of emission-line galaxies at z = 0.4–4.7. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stx1569\">https://doi.org/10.1093/mnras/stx1569</a>","ista":"Matthee JJ, Sobral D, Best P, Smail I, Bian F, Darvish B, Röttgering H, Fan X. 2017. Boötes-HiZELS: An optical to near-infrared survey of emission-line galaxies at z = 0.4–4.7. Monthly Notices of the Royal Astronomical Society. 471(1), 629–649.","chicago":"Matthee, Jorryt J, David Sobral, Philip Best, Ian Smail, Fuyan Bian, Behnam Darvish, Huub Röttgering, and Xiaohui Fan. “Boötes-HiZELS: An Optical to near-Infrared Survey of Emission-Line Galaxies at z = 0.4–4.7.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stx1569\">https://doi.org/10.1093/mnras/stx1569</a>.","short":"J.J. Matthee, D. Sobral, P. Best, I. Smail, F. Bian, B. Darvish, H. Röttgering, X. Fan, Monthly Notices of the Royal Astronomical Society 471 (2017) 629–649.","ieee":"J. J. Matthee <i>et al.</i>, “Boötes-HiZELS: An optical to near-infrared survey of emission-line galaxies at z = 0.4–4.7,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 471, no. 1. Oxford University Press, pp. 629–649, 2017.","ama":"Matthee JJ, Sobral D, Best P, et al. Boötes-HiZELS: An optical to near-infrared survey of emission-line galaxies at z = 0.4–4.7. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;471(1):629-649. doi:<a href=\"https://doi.org/10.1093/mnras/stx1569\">10.1093/mnras/stx1569</a>"},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa":1,"language":[{"iso":"eng"}],"arxiv":1,"month":"10","publication_status":"published","publication_identifier":{"issn":["0035-8711","1365-2966"]},"abstract":[{"lang":"eng","text":"We present a sample of ∼1000 emission-line galaxies at z = 0.4–4.7 from the ∼0.7deg2 High-z Emission-Line Survey in the Boötes field identified with a suite of six narrow-band filters at ≈0.4–2.1 μm. These galaxies have been selected on their Ly α (73), [O II] (285), H β/[O III] (387) or H α (362) emission line, and have been classified with optical to near-infrared colours. A subsample of 98 sources have reliable redshifts from multiple narrow-band (e.g. [O II]–H α) detections and/or spectroscopy. In this survey paper, we present the observations, selection and catalogues of emitters. We measure number densities of Ly α, [O II], H β/[O III] and H α and confirm strong luminosity evolution in star-forming galaxies from z ∼ 0.4 to ∼5, in agreement with previous results. To demonstrate the usefulness of dual-line emitters, we use the sample of dual [O II]–H α emitters to measure the observed [O II]/H α ratio at z = 1.47. The observed [O II]/H α ratio increases significantly from 0.40 ± 0.01 at z = 0.1 to 0.52 ± 0.05 at z = 1.47, which we attribute to either decreasing dust attenuation with redshift, or due to a bias in the (typically) fibre measurements in the local Universe that only measure the central kpc regions. At the bright end, we find that both the H α and Ly α number densities at z ≈ 2.2 deviate significantly from a Schechter form, following a power law. We show that this is driven entirely by an increasing X-ray/active galactic nucleus fraction with line luminosity, which reaches ≈100 per cent at line luminosities L ≳ 3 × 1044 erg s−1."}],"intvolume":"       471","volume":471,"article_type":"original","date_created":"2022-07-12T11:01:35Z","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","first_name":"Jorryt J"},{"first_name":"David","last_name":"Sobral","full_name":"Sobral, David"},{"first_name":"Philip","full_name":"Best, Philip","last_name":"Best"},{"first_name":"Ian","full_name":"Smail, Ian","last_name":"Smail"},{"first_name":"Fuyan","last_name":"Bian","full_name":"Bian, Fuyan"},{"last_name":"Darvish","full_name":"Darvish, Behnam","first_name":"Behnam"},{"first_name":"Huub","full_name":"Röttgering, Huub","last_name":"Röttgering"},{"last_name":"Fan","full_name":"Fan, Xiaohui","first_name":"Xiaohui"}],"scopus_import":"1","day":"01","title":"Boötes-HiZELS: An optical to near-infrared survey of emission-line galaxies at z = 0.4–4.7","oa_version":"Preprint"},{"volume":466,"article_type":"original","date_created":"2022-07-12T12:04:16Z","author":[{"last_name":"Sobral","full_name":"Sobral, David","first_name":"David"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","first_name":"Jorryt J"},{"first_name":"Philip","full_name":"Best, Philip","last_name":"Best"},{"first_name":"Andra","last_name":"Stroe","full_name":"Stroe, Andra"},{"last_name":"Röttgering","full_name":"Röttgering, Huub","first_name":"Huub"},{"first_name":"Iván","full_name":"Oteo, Iván","last_name":"Oteo"},{"full_name":"Smail, Ian","last_name":"Smail","first_name":"Ian"},{"first_name":"Leah","full_name":"Morabito, Leah","last_name":"Morabito"},{"first_name":"Ana","last_name":"Paulino-Afonso","full_name":"Paulino-Afonso, Ana"}],"day":"01","scopus_import":"1","title":"The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23","oa_version":"Preprint","publication_status":"published","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"abstract":[{"lang":"eng","text":"We present the CAlibrating LYMan-α with Hα (CALYMHA) pilot survey and new results on Lyman α (Lyα) selected galaxies at z ∼ 2. We use a custom-built Lyα narrow-band filter at the Isaac Newton Telescope, designed to provide a matched volume coverage to the z = 2.23 Hα HiZELS survey. Here, we present the first results for the COSMOS and UDS fields. Our survey currently reaches a 3σ line flux limit of ∼4 × 10−17 erg s−1 cm−2, and a Lyα luminosity limit of ∼1042.3 erg s−1. We find 188 Lyα emitters over 7.3 × 105 Mpc3, but also find significant numbers of other line-emitting sources corresponding to He II, C III] and C IV emission lines. These sources are important contaminants, and we carefully remove them, unlike most previous studies. We find that the Lyα luminosity function at z = 2.23 is very well described by a Schechter function up to LLy α ≈ 1043 erg s−1 with L∗=1042.59+0.16−0.08 erg s−1, ϕ∗=10−3.09+0.14−0.34 Mpc−3 and α = −1.75 ± 0.25. Above LLy α ≈ 1043 erg s−1, the Lyα luminosity function becomes power-law like, driven by X-ray AGN. We find that Lyα-selected emitters have a high escape fraction of 37 ± 7 per cent, anticorrelated with Lyα luminosity and correlated with Lyα equivalent width. Lyα emitters have ubiquitous large (≈40 kpc) Lyα haloes, ∼2 times larger than their Hα extents. By directly comparing our Lyα and Hα luminosity functions, we find that the global/overall escape fraction of Lyα photons (within a 13 kpc radius) from the full population of star-forming galaxies is 5.1 ± 0.2 per cent at the peak of the star formation history. An extra 3.3 ± 0.3 per cent of Lyα photons likely still escape, but at larger radii."}],"intvolume":"       466","month":"04","arxiv":1,"issue":"1","citation":{"ista":"Sobral D, Matthee JJ, Best P, Stroe A, Röttgering H, Oteo I, Smail I, Morabito L, Paulino-Afonso A. 2017. The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23. Monthly Notices of the Royal Astronomical Society. 466(1), 1242–1258.","chicago":"Sobral, David, Jorryt J Matthee, Philip Best, Andra Stroe, Huub Röttgering, Iván Oteo, Ian Smail, Leah Morabito, and Ana Paulino-Afonso. “The CALYMHA Survey: Lyα Luminosity Function and Global Escape Fraction of Lyα Photons at z = 2.23.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stw3090\">https://doi.org/10.1093/mnras/stw3090</a>.","apa":"Sobral, D., Matthee, J. J., Best, P., Stroe, A., Röttgering, H., Oteo, I., … Paulino-Afonso, A. (2017). The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stw3090\">https://doi.org/10.1093/mnras/stw3090</a>","mla":"Sobral, David, et al. “The CALYMHA Survey: Lyα Luminosity Function and Global Escape Fraction of Lyα Photons at z = 2.23.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 466, no. 1, Oxford University Press, 2017, pp. 1242–58, doi:<a href=\"https://doi.org/10.1093/mnras/stw3090\">10.1093/mnras/stw3090</a>.","ama":"Sobral D, Matthee JJ, Best P, et al. The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;466(1):1242-1258. doi:<a href=\"https://doi.org/10.1093/mnras/stw3090\">10.1093/mnras/stw3090</a>","ieee":"D. Sobral <i>et al.</i>, “The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 466, no. 1. Oxford University Press, pp. 1242–1258, 2017.","short":"D. Sobral, J.J. Matthee, P. Best, A. Stroe, H. Röttgering, I. Oteo, I. Smail, L. Morabito, A. Paulino-Afonso, Monthly Notices of the Royal Astronomical Society 466 (2017) 1242–1258."},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa":1,"language":[{"iso":"eng"}],"date_updated":"2022-08-19T07:18:20Z","_id":"11562","type":"journal_article","doi":"10.1093/mnras/stw3090","article_processing_charge":"No","publisher":"Oxford University Press","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1609.05897"}],"quality_controlled":"1","page":"1242-1258","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: haloes","galaxies: high-redshift","galaxies: luminosity function","mass function","galaxies: statistics","cosmology: observations"],"year":"2017","external_id":{"arxiv":["1609.05897"]},"acknowledgement":"We thank the reviewer for his/her helpful comments and suggestions that have greatly improved this work. DS and JM acknowledge financial support from the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship. DS also acknowledges funding from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010). PNB is grateful for support from the UK STFC via grant ST/M001229/1. IRS acknowledges support from STFC (ST/L00075X/1), the ERC Advanced Investigator programme DUSTYGAL 321334 and a Royal Society/Wolfson merit award. We thank Matthew Hayes, Ryan Trainor, Kimihiko Nakajima and Anne Verhamme for many helpful discussions and Ana Sobral, Carolina Duarte and Miguel Domingos for taking part in observations with the NB392 filter. We also thank Sergio Santos for helpful comments. This research is based on observations obtained on the Isaac Newton Telescope (INT), programs: I13AN002, I14AN002, 088-INT7/14A, I14BN006, 118-INT13/14B & I15AN008. The authors acknowledge the award of time from programmes: I13AN002, I14AN002, 088-INT7/14A, I14BN006, 118-INT13/14B, I15AN008 on the INT. 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. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 098.A 0819. We have benefited greatly from the publicly available programming language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY and ASTROPY packages, the astronomical imaging tools SEXTRACTOR, SWARP (Bertin & Arnouts 1996; Bertin 2010), SCAMP (Bertin 2006) and TOPCAT (Taylor 2005). Dedicated to the memory of M. L. Nicolau and M. C. Serrano.","date_published":"2017-04-01T00:00:00Z","publication":"Monthly Notices of the Royal Astronomical Society","status":"public","extern":"1"},{"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","cosmology: observations","dark ages","reionization","first stars"],"external_id":{"arxiv":["1605.08782"]},"year":"2017","acknowledgement":"We thank the referee for the many helpful and constructive comments which have significantly improved this paper. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. DS acknowledges financial support from the Netherlands Organization for Scientific research (NWO) through a Veni fellowship and from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010). PNB is grateful for support from the UK STFC via grant ST/M001229/1. IO acknowledges support from the European Research Council in the form of the Advanced Investigator Programme, 321302, COSMICISM. The authors thank Andreas Faisst, Michael Rutkowski and Andreas Sandberg for answering questions related to this work and Daniel Schaerer and Mark Dijkstra for discussions. We acknowledge the work that has been done by both the COSMOS team in assembling such large, state-of-the-art multi-wavelength data set, as this has been crucial for the results presented in this paper. We have benefited greatly from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY (Jones et al. 2001; Hunter 2007; Van Der Walt, Colbert & Varoquaux 2011) and ASTROPY (Astropy Collaboration et al. 2013) packages, the astronomical imaging tools SEXTRACTOR and SWARP (Bertin & Arnouts 1996;\r\nBertin 2010) and the TOPCAT analysis program (Taylor 2013).","date_published":"2017-03-01T00:00:00Z","publication":"Monthly Notices of the Royal Astronomical Society","extern":"1","status":"public","type":"journal_article","_id":"11564","date_updated":"2022-08-19T07:53:04Z","publisher":"Oxford University Press","article_processing_charge":"No","doi":"10.1093/mnras/stw2973","quality_controlled":"1","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1605.08782"}],"page":"3637-3655","arxiv":1,"month":"03","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"ama":"Matthee JJ, Sobral D, Best P, et al. The production and escape of Lyman-Continuum radiation from star-forming galaxies at z ∼ 2 and their redshift evolution. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;465(3):3637-3655. doi:<a href=\"https://doi.org/10.1093/mnras/stw2973\">10.1093/mnras/stw2973</a>","short":"J.J. Matthee, D. Sobral, P. Best, A.A. Khostovan, I. Oteo, R. Bouwens, H. Röttgering, Monthly Notices of the Royal Astronomical Society 465 (2017) 3637–3655.","ieee":"J. J. Matthee <i>et al.</i>, “The production and escape of Lyman-Continuum radiation from star-forming galaxies at z ∼ 2 and their redshift evolution,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 465, no. 3. Oxford University Press, pp. 3637–3655, 2017.","chicago":"Matthee, Jorryt J, David Sobral, Philip Best, Ali Ahmad Khostovan, Iván Oteo, Rychard Bouwens, and Huub Röttgering. “The Production and Escape of Lyman-Continuum Radiation from Star-Forming Galaxies at z ∼ 2 and Their Redshift Evolution.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stw2973\">https://doi.org/10.1093/mnras/stw2973</a>.","ista":"Matthee JJ, Sobral D, Best P, Khostovan AA, Oteo I, Bouwens R, Röttgering H. 2017. The production and escape of Lyman-Continuum radiation from star-forming galaxies at z ∼ 2 and their redshift evolution. Monthly Notices of the Royal Astronomical Society. 465(3), 3637–3655.","mla":"Matthee, Jorryt J., et al. “The Production and Escape of Lyman-Continuum Radiation from Star-Forming Galaxies at z ∼ 2 and Their Redshift Evolution.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 465, no. 3, Oxford University Press, 2017, pp. 3637–55, doi:<a href=\"https://doi.org/10.1093/mnras/stw2973\">10.1093/mnras/stw2973</a>.","apa":"Matthee, J. J., Sobral, D., Best, P., Khostovan, A. A., Oteo, I., Bouwens, R., &#38; Röttgering, H. (2017). The production and escape of Lyman-Continuum radiation from star-forming galaxies at z ∼ 2 and their redshift evolution. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stw2973\">https://doi.org/10.1093/mnras/stw2973</a>"},"issue":"3","language":[{"iso":"eng"}],"oa":1,"date_created":"2022-07-12T12:12:14Z","article_type":"original","volume":465,"title":"The production and escape of Lyman-Continuum radiation from star-forming galaxies at z ∼ 2 and their redshift evolution","oa_version":"Preprint","day":"01","scopus_import":"1","author":[{"orcid":"0000-0003-2871-127X","first_name":"Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J"},{"last_name":"Sobral","full_name":"Sobral, David","first_name":"David"},{"last_name":"Best","full_name":"Best, Philip","first_name":"Philip"},{"last_name":"Khostovan","full_name":"Khostovan, Ali Ahmad","first_name":"Ali Ahmad"},{"full_name":"Oteo, Iván","last_name":"Oteo","first_name":"Iván"},{"first_name":"Rychard","full_name":"Bouwens, Rychard","last_name":"Bouwens"},{"last_name":"Röttgering","full_name":"Röttgering, Huub","first_name":"Huub"}],"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"publication_status":"published","abstract":[{"text":"We study the production rate of ionizing photons of a sample of 588 Hα emitters (HAEs) and 160 Lyman-α emitters (LAEs) at z = 2.2 in the COSMOS field in order to assess the implied emissivity from galaxies, based on their ultraviolet (UV) luminosity. By exploring the rest-frame Lyman Continuum (LyC) with GALEX/NUV data, we find fesc < 2.8 (6.4) per cent through median (mean) stacking. By combining the Hα luminosity density with intergalactic medium emissivity measurements from absorption studies, we find a globally averaged 〈fesc〉 of 5.9+14.5−4.2 per cent at z = 2.2 if we assume HAEs are the only source of ionizing photons. We find similarly low values of the global 〈fesc〉 at z ≈ 3–5, also ruling out a high 〈fesc〉 at z < 5. These low escape fractions allow us to measure ξion, the number of produced ionizing photons per unit UV luminosity, and investigate how this depends on galaxy properties. We find a typical ξion ≈ 1024.77 ± 0.04 Hz erg−1 for HAEs and ξion ≈ 1025.14 ± 0.09 Hz erg−1 for LAEs. LAEs and low-mass HAEs at z = 2.2 show similar values of ξion as typically assumed in the reionization era, while the typical HAE is three times less ionizing. Due to an increasing ξion with increasing EW(Hα), ξion likely increases with redshift. This evolution alone is fully in line with the observed evolution of ξion between z ≈ 2 and 5, indicating a typical value of ξion ≈ 1025.4 Hz erg−1 in the reionization era.","lang":"eng"}],"intvolume":"       465"},{"arxiv":1,"month":"02","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"ama":"Matthee JJ, Schaye J, Crain RA, Schaller M, Bower R, Theuns T. The origin of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE simulation. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;465(2):2381-2396. doi:<a href=\"https://doi.org/10.1093/mnras/stw2884\">10.1093/mnras/stw2884</a>","ieee":"J. J. Matthee, J. Schaye, R. A. Crain, M. Schaller, R. Bower, and T. Theuns, “The origin of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE simulation,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 465, no. 2. Oxford University Press, pp. 2381–2396, 2017.","short":"J.J. Matthee, J. Schaye, R.A. Crain, M. Schaller, R. Bower, T. Theuns, Monthly Notices of the Royal Astronomical Society 465 (2017) 2381–2396.","ista":"Matthee JJ, Schaye J, Crain RA, Schaller M, Bower R, Theuns T. 2017. The origin of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE simulation. Monthly Notices of the Royal Astronomical Society. 465(2), 2381–2396.","chicago":"Matthee, Jorryt J, Joop Schaye, Robert A. Crain, Matthieu Schaller, Richard Bower, and Tom Theuns. “The Origin of Scatter in the Stellar Mass–Halo Mass Relation of Central Galaxies in the EAGLE Simulation.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stw2884\">https://doi.org/10.1093/mnras/stw2884</a>.","apa":"Matthee, J. J., Schaye, J., Crain, R. A., Schaller, M., Bower, R., &#38; Theuns, T. (2017). The origin of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE simulation. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stw2884\">https://doi.org/10.1093/mnras/stw2884</a>","mla":"Matthee, Jorryt J., et al. “The Origin of Scatter in the Stellar Mass–Halo Mass Relation of Central Galaxies in the EAGLE Simulation.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 465, no. 2, Oxford University Press, 2017, pp. 2381–96, doi:<a href=\"https://doi.org/10.1093/mnras/stw2884\">10.1093/mnras/stw2884</a>."},"issue":"2","language":[{"iso":"eng"}],"oa":1,"date_created":"2022-07-12T12:25:08Z","article_type":"original","volume":465,"oa_version":"Preprint","title":"The origin of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE simulation","scopus_import":"1","day":"01","author":[{"orcid":"0000-0003-2871-127X","first_name":"Jorryt J","last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"first_name":"Joop","full_name":"Schaye, Joop","last_name":"Schaye"},{"first_name":"Robert A.","last_name":"Crain","full_name":"Crain, Robert A."},{"first_name":"Matthieu","full_name":"Schaller, Matthieu","last_name":"Schaller"},{"first_name":"Richard","full_name":"Bower, Richard","last_name":"Bower"},{"last_name":"Theuns","full_name":"Theuns, Tom","first_name":"Tom"}],"publication_status":"published","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"abstract":[{"lang":"eng","text":"We use the hydrodynamical EAGLE simulation to study the magnitude and origin of the scatter in the stellar mass–halo mass relation for central galaxies. We separate cause and effect by correlating stellar masses in the baryonic simulation with halo properties in a matched dark matter only (DMO) simulation. The scatter in stellar mass increases with redshift and decreases with halo mass. At z = 0.1, it declines from 0.25 dex at M200, DMO ≈ 1011 M⊙ to 0.12 dex at M200, DMO ≈ 1013 M⊙, but the trend is weak above 1012 M⊙. For M200, DMO < 1012.5 M⊙ up to 0.04 dex of the scatter is due to scatter in the halo concentration. At fixed halo mass, a larger stellar mass corresponds to a more concentrated halo. This is likely because higher concentrations imply earlier formation times and hence more time for accretion and star formation, and/or because feedback is less efficient in haloes with higher binding energies. The maximum circular velocity, Vmax, DMO, and binding energy are therefore more fundamental properties than halo mass, meaning that they are more accurate predictors of stellar mass, and we provide fitting formulae for their relations with stellar mass. However, concentration alone cannot explain the total scatter in the Mstar−M200,DMO relation, and it does not explain the scatter in Mstar–Vmax, DMO. Halo spin, sphericity, triaxiality, substructure and environment are also not responsible for the remaining scatter, which thus could be due to more complex halo properties or non-linear/stochastic baryonic effects."}],"intvolume":"       465","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: formation","galaxies: haloes","cosmology: theory"],"external_id":{"arxiv":["1608.08218"]},"year":"2017","date_published":"2017-02-01T00:00:00Z","acknowledgement":"We thank the anonymous referee for their comments. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. JM thanks David Sobral for useful discussions and help with fitting routines and Jonas Chavez Montero and Ying Zu for providing data. We thank PRACE for the access to the Curie facility in France. We have used the DiRAC system which is a part of National E-Infrastructure at Durham University, operated by the Institute for Computational Cosmology on behalf of the STFC DiRAC HPC Facility (www.dirac.ac.uk); the equipment was funded by BIS National E-infrastructure capital grant ST/K00042X/1, STFC capital grant ST/H008519/1, STFC DiRAC Operations grant ST/K003267/1 and Durham University. The study was sponsored by the Dutch National Computing Facilities Foundation (NCF) for the use of supercomputer facilities, with financial support from the Netherlands Organisation for Scientific Research (NWO), through VICI grant 639.043.409, and the European Research Council under the European Union’s Seventh Framework Programme (FP7/2007-2013)/ERC Grant agreement 278594- GasAroundGalaxies, and from the Belgian Science Policy Office ([AP P7/08 CHARM]). We have benefited greatly from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY, H5PY and RPY2 packages, and the TOPCAT analysis program (Taylor 2005).","publication":"Monthly Notices of the Royal Astronomical Society","status":"public","extern":"1","type":"journal_article","_id":"11565","date_updated":"2022-08-19T07:56:07Z","publisher":"Oxford University Press","article_processing_charge":"No","doi":"10.1093/mnras/stw2884","quality_controlled":"1","main_file_link":[{"url":"https://arxiv.org/abs/1608.08218","open_access":"1"}],"page":"2381-2396"},{"date_updated":"2022-08-19T07:59:57Z","_id":"11566","type":"journal_article","doi":"10.1093/mnras/stx1712","article_processing_charge":"No","publisher":"Oxford University Press","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1703.10169"}],"quality_controlled":"1","page":"2558-2574","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: active","galaxies: high-redshift","quasars: emission lines","galaxies: star formation","cosmology: observations"],"year":"2017","external_id":{"arxiv":["1703.10169"]},"date_published":"2017-11-01T00:00:00Z","acknowledgement":"We would like to thank the anonymous referee for her/his valuable input that helped improve the clarity and interpretation of our results. DS acknowledges financial support from the Netherlands Organisation for Scientific research (NWO), through a Veni fellowship. IO acknowledges support from the European Research Council in the form of the Advanced Investigator Programme, 321302, COSMICISM. CALYMHA data are based on observations made with the Isaac Newton Telescope (proposals 13AN002, I14AN002, 088-INT7/14A, I14BN006, 118-INT13/14B, I15AN008) 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 Astrofísica de Canarias. Also based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme IDs 098.A-0819 and 179.A-2005. We are grateful to E. L. Wright and J. Schombert for their cosmology calculator. We would like to thank the authors of NUMPY (van der Walt et al. 2011), SCIPY (Jones et al. 2001), MATPLOTLIB (Hunter 2007) and ASTROPY (Astropy Collaboration et al. 2013) for making these packages publicly available. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is ","extern":"1","publication":"Monthly Notices of the Royal Astronomical Society","status":"public","volume":471,"article_type":"original","date_created":"2022-07-12T12:33:16Z","author":[{"first_name":"Andra","last_name":"Stroe","full_name":"Stroe, Andra"},{"first_name":"David","last_name":"Sobral","full_name":"Sobral, David"},{"first_name":"Jorryt J","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee"},{"last_name":"Calhau","full_name":"Calhau, João","first_name":"João"},{"full_name":"Oteo, Ivan","last_name":"Oteo","first_name":"Ivan"}],"day":"01","scopus_import":"1","title":"A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent widths ","oa_version":"Preprint","publication_status":"published","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"intvolume":"       471","abstract":[{"text":"While traditionally associated with active galactic nuclei (AGN), the properties of the C II] (λ = 2326 Å), C III] (λ, λ = 1907, 1909 Å) and C IV (λ, λ = 1549, 1551 Å) emission lines are still uncertain as large, unbiased samples of sources are scarce. We present the first blind, statistical study of C II], C III] and C IV emitters at z ∼ 0.68, 1.05, 1.53, respectively, uniformly selected down to a flux limit of ∼4 × 10−17 erg s−1 cm−1 through a narrow-band survey covering an area of ∼1.4 deg2 over COSMOS and UDS. We detect 16 C II], 35 C III] and 17 C IV emitters, whose nature we investigate using optical colours as well as Hubble Space Telescope (HST), X-ray, radio and far-infrared data. We find that z ∼ 0.7 C II] emitters are consistent with a mixture of blue (UV slope β = −2.0 ± 0.4) star-forming (SF) galaxies with discy HST structure and AGN with Seyfert-like morphologies. Bright C II] emitters have individual X-ray detections as well as high average black hole accretion rates (BHARs) of ∼0.1 M⊙ yr−1. C III] emitters at z ∼ 1.05 trace a general population of SF galaxies, with β = −0.8 ± 1.1, a variety of optical morphologies, including isolated and interacting galaxies and low BHAR (<0.02 M⊙ yr−1). Our C IV emitters at z ∼ 1.5 are consistent with young, blue quasars (β ∼ −1.9) with point-like optical morphologies, bright X-ray counterparts and large BHAR (0.8  M⊙ yr−1). We also find some surprising C II], C III] and C IV emitters with rest-frame equivalent widths (EWs) that could be as large as 50–100 Å. AGN or spatial offsets between the UV continuum stellar disc and the line-emitting regions may explain the large EW. These bright C II], C III] and C IV emitters are ideal candidates for spectroscopic follow-up to fully unveil their nature.","lang":"eng"}],"arxiv":1,"month":"11","issue":"3","citation":{"ama":"Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent widths . <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;471(3):2558-2574. doi:<a href=\"https://doi.org/10.1093/mnras/stx1712\">10.1093/mnras/stx1712</a>","ieee":"A. Stroe, D. Sobral, J. J. Matthee, J. Calhau, and I. Oteo, “A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent widths ,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 471, no. 3. Oxford University Press, pp. 2558–2574, 2017.","short":"A. Stroe, D. Sobral, J.J. Matthee, J. Calhau, I. Oteo, Monthly Notices of the Royal Astronomical Society 471 (2017) 2558–2574.","ista":"Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. 2017. A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent widths . Monthly Notices of the Royal Astronomical Society. 471(3), 2558–2574.","chicago":"Stroe, Andra, David Sobral, Jorryt J Matthee, João Calhau, and Ivan Oteo. “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, Morphologies and Equivalent Widths .” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stx1712\">https://doi.org/10.1093/mnras/stx1712</a>.","apa":"Stroe, A., Sobral, D., Matthee, J. J., Calhau, J., &#38; Oteo, I. (2017). A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent widths . <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stx1712\">https://doi.org/10.1093/mnras/stx1712</a>","mla":"Stroe, Andra, et al. “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, Morphologies and Equivalent Widths .” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 471, no. 3, Oxford University Press, 2017, pp. 2558–74, doi:<a href=\"https://doi.org/10.1093/mnras/stx1712\">10.1093/mnras/stx1712</a>."},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa":1,"language":[{"iso":"eng"}]},{"intvolume":"       471","abstract":[{"text":"Recently, the C III] and C IV emission lines have been observed in galaxies in the early Universe (z > 5), providing new ways to measure their redshift and study their stellar populations and active galactic nuclei (AGN). We explore the first blind C II], C III] and C IV survey (z ∼ 0.68, 1.05, 1.53, respectively) presented in Stroe et al. (2017). We derive luminosity functions (LF) and study properties of C II], C III] and C IV line emitters through comparisons to the LFs of H α and Ly α emitters, UV selected star-forming (SF) galaxies and quasars at similar redshifts. The C II] LF at z ∼ 0.68 is equally well described by a Schechter or a power-law LF, characteristic of a mixture of SF and AGN activity. The C III] LF (z ∼ 1.05) is consistent to a scaled down version of the Schechter H α and Ly α LF at their redshift, indicating a SF origin. In stark contrast, the C IV LF at z ∼ 1.53 is well fit by a power-law, quasar-like LF. We find that the brightest UV sources (MUV < −22) will universally have C III] and C IV emission. However, on average, C III] and C IV are not as abundant as H α or Ly α emitters at the same redshift, with cosmic average ratios of ∼0.02–0.06 to H α and ∼0.01–0.1 to intrinsic Ly α. We predict that the C III] and C IV lines can only be truly competitive in confirming high-redshift candidates when the hosts are intrinsically bright and the effective Ly α escape fraction is below 1 per cent. While C III] and C IV were proposed as good tracers of young, relatively low-metallicity galaxies typical of the early Universe, we find that, at least at z ∼ 1.5, C IV is exclusively hosted by AGN/quasars, especially at large line equivalent widths.","lang":"eng"}],"publication_status":"published","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"day":"01","scopus_import":"1","author":[{"first_name":"Andra","last_name":"Stroe","full_name":"Stroe, Andra"},{"last_name":"Sobral","full_name":"Sobral, David","first_name":"David"},{"first_name":"Jorryt J","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee"},{"first_name":"João","last_name":"Calhau","full_name":"Calhau, João"},{"first_name":"Ivan","full_name":"Oteo, Ivan","last_name":"Oteo"}],"title":"A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average line ratios","oa_version":"Preprint","volume":471,"date_created":"2022-07-12T12:54:57Z","article_type":"original","oa":1,"language":[{"iso":"eng"}],"citation":{"short":"A. Stroe, D. Sobral, J.J. Matthee, J. Calhau, I. Oteo, Monthly Notices of the Royal Astronomical Society 471 (2017) 2575–2586.","ieee":"A. Stroe, D. Sobral, J. J. Matthee, J. Calhau, and I. Oteo, “A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average line ratios,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 471, no. 3. Oxford University Press, pp. 2575–2586, 2017.","ama":"Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average line ratios. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;471(3):2575-2586. doi:<a href=\"https://doi.org/10.1093/mnras/stx1713\">10.1093/mnras/stx1713</a>","mla":"Stroe, Andra, et al. “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity Functions and Cosmic Average Line Ratios.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 471, no. 3, Oxford University Press, 2017, pp. 2575–86, doi:<a href=\"https://doi.org/10.1093/mnras/stx1713\">10.1093/mnras/stx1713</a>.","apa":"Stroe, A., Sobral, D., Matthee, J. J., Calhau, J., &#38; Oteo, I. (2017). A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average line ratios. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stx1713\">https://doi.org/10.1093/mnras/stx1713</a>","ista":"Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. 2017. A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average line ratios. Monthly Notices of the Royal Astronomical Society. 471(3), 2575–2586.","chicago":"Stroe, Andra, David Sobral, Jorryt J Matthee, João Calhau, and Ivan Oteo. “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity Functions and Cosmic Average Line Ratios.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stx1713\">https://doi.org/10.1093/mnras/stx1713</a>."},"issue":"3","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","arxiv":1,"month":"11","page":"2575-2586","main_file_link":[{"url":"https://arxiv.org/abs/1703.10169","open_access":"1"}],"quality_controlled":"1","article_processing_charge":"No","doi":"10.1093/mnras/stx1713","publisher":"Oxford University Press","_id":"11567","date_updated":"2022-08-19T08:02:04Z","type":"journal_article","publication":"Monthly Notices of the Royal Astronomical Society","extern":"1","status":"public","date_published":"2017-11-01T00:00:00Z","year":"2017","external_id":{"arxiv":["1703.10169"]},"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: active","galaxies: high redshift","galaxies: luminosity function","mass function","quasars: emission lines","star formation","cosmology: observations"]},{"language":[{"iso":"eng"}],"oa":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","issue":"1","citation":{"apa":"Matthee, J. J., Sobral, D., Darvish, B., Santos, S., Mobasher, B., Paulino-Afonso, A., … Alegre, L. (2017). Spectroscopic properties of luminous Ly α emitters at z ≈ 6–7 and comparison to the Lyman-break population. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stx2061\">https://doi.org/10.1093/mnras/stx2061</a>","mla":"Matthee, Jorryt J., et al. “Spectroscopic Properties of Luminous Ly α Emitters at z ≈ 6–7 and Comparison to the Lyman-Break Population.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 472, no. 1, Oxford University Press, 2017, pp. 772–87, doi:<a href=\"https://doi.org/10.1093/mnras/stx2061\">10.1093/mnras/stx2061</a>.","ista":"Matthee JJ, Sobral D, Darvish B, Santos S, Mobasher B, Paulino-Afonso A, Röttgering H, Alegre L. 2017. Spectroscopic properties of luminous Ly α emitters at z ≈ 6–7 and comparison to the Lyman-break population. Monthly Notices of the Royal Astronomical Society. 472(1), 772–787.","chicago":"Matthee, Jorryt J, David Sobral, Behnam Darvish, Sérgio Santos, Bahram Mobasher, Ana Paulino-Afonso, Huub Röttgering, and Lara Alegre. “Spectroscopic Properties of Luminous Ly α Emitters at z ≈ 6–7 and Comparison to the Lyman-Break Population.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stx2061\">https://doi.org/10.1093/mnras/stx2061</a>.","ieee":"J. J. Matthee <i>et al.</i>, “Spectroscopic properties of luminous Ly α emitters at z ≈ 6–7 and comparison to the Lyman-break population,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 472, no. 1. Oxford University Press, pp. 772–787, 2017.","short":"J.J. Matthee, D. Sobral, B. Darvish, S. Santos, B. Mobasher, A. Paulino-Afonso, H. Röttgering, L. Alegre, Monthly Notices of the Royal Astronomical Society 472 (2017) 772–787.","ama":"Matthee JJ, Sobral D, Darvish B, et al. Spectroscopic properties of luminous Ly α emitters at z ≈ 6–7 and comparison to the Lyman-break population. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;472(1):772-787. doi:<a href=\"https://doi.org/10.1093/mnras/stx2061\">10.1093/mnras/stx2061</a>"},"month":"11","arxiv":1,"abstract":[{"text":"We present spectroscopic follow-up of candidate luminous Ly α emitters (LAEs) at z = 5.7–6.6 in the SA22 field with VLT/X-SHOOTER. We confirm two new luminous LAEs at z = 5.676 (SR6) and z = 6.532 (VR7), and also present HST follow-up of both sources. These sources have luminosities LLy α ≈ 3 × 1043 erg s−1, very high rest-frame equivalent widths of EW0 ≳ 200 Å and narrow Ly α lines (200–340 km s−1). VR7 is the most UV-luminous LAE at z > 6.5, with M1500 = −22.5, even brighter in the UV than CR7. Besides Ly α, we do not detect any other rest-frame UV lines in the spectra of SR6 and VR7, and argue that rest-frame UV lines are easier to observe in bright galaxies with low Ly α equivalent widths. We confirm that Ly α line widths increase with Ly α luminosity at z = 5.7, while there are indications that Ly α lines of faint LAEs become broader at z = 6.6, potentially due to reionization. We find a large spread of up to 3 dex in UV luminosity for >L⋆ LAEs, but find that the Ly α luminosity of the brightest LAEs is strongly related to UV luminosity at z = 6.6. Under basic assumptions, we find that several LAEs at z ≈ 6–7 have Ly α escape fractions ≳ 100  per cent, indicating bursty star formation histories, alternative Ly α production mechanisms, or dust attenuating Ly α emission differently than UV emission. Finally, we present a method to compute ξion, the production efficiency of ionizing photons, and find that LAEs at z ≈ 6–7 have high values of log10(ξion/Hz erg−1) ≈ 25.51 ± 0.09 that may alleviate the need for high Lyman-Continuum escape fractions required for reionization.","lang":"eng"}],"intvolume":"       472","publication_status":"published","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"title":"Spectroscopic properties of luminous Ly α emitters at z ≈ 6–7 and comparison to the Lyman-break population","oa_version":"Preprint","author":[{"orcid":"0000-0003-2871-127X","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee"},{"first_name":"David","full_name":"Sobral, David","last_name":"Sobral"},{"first_name":"Behnam","last_name":"Darvish","full_name":"Darvish, Behnam"},{"full_name":"Santos, Sérgio","last_name":"Santos","first_name":"Sérgio"},{"last_name":"Mobasher","full_name":"Mobasher, Bahram","first_name":"Bahram"},{"first_name":"Ana","full_name":"Paulino-Afonso, Ana","last_name":"Paulino-Afonso"},{"first_name":"Huub","full_name":"Röttgering, Huub","last_name":"Röttgering"},{"last_name":"Alegre","full_name":"Alegre, Lara","first_name":"Lara"}],"scopus_import":"1","day":"01","article_type":"original","date_created":"2022-07-13T09:47:39Z","volume":472,"publication":"Monthly Notices of the Royal Astronomical Society","status":"public","extern":"1","date_published":"2017-11-01T00:00:00Z","acknowledgement":"We thank the referee for a constructive report that has improved the quality and clarity of this work. The authors thank Grecco Oyarzún for discussions. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. DS acknowledges financial support from the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship and from Lancaster University through an Early Career Internal Grant A100679. BD acknowledges financial support from NASA through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G. We thank Kasper Schmidt for providing measurements. Based on observations with the W.M. Keck Observatory through programme C267D. The W.M. Keck Observatory is operated as a scientific partnership amongst the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 097.A-0943, 294.A 5018 and 098.A-0819 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. The authors acknowledge the award of observing time (W16AN004) and of service time (SW2014b20) on the William Herschel Telescope (WHT). WHT and its service programme are operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. Based on observations made with the NASA/ESA HST, obtained (from the Data Archive) at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with programme #14699. We are grateful for the excellent data sets from the COSMOS, UltraVISTA, SXDS, UDS and CFHTLS survey teams; without these legacy surveys, this research would have been impossible. We have benefited from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY and ASTROPY packages, the astronomical imaging tools SEXTRACTOR, SWARP and SCAMP and the TOPCAT analysis tool (Taylor 2013).","external_id":{"arxiv":["1706.06591"]},"year":"2017","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution – galaxies: high-redshift","dark ages","reionization","first stars","cosmology: observations"],"page":"772-787","quality_controlled":"1","main_file_link":[{"url":"https://arxiv.org/abs/1706.06591","open_access":"1"}],"publisher":"Oxford University Press","doi":"10.1093/mnras/stx2061","article_processing_charge":"No","type":"journal_article","date_updated":"2022-08-19T08:05:37Z","_id":"11572"},{"intvolume":"       471","abstract":[{"lang":"eng","text":"We present dynamical measurements from the KMOS (K-band multi-object spectrograph) Deep Survey (KDS), which comprises 77 typical star-forming galaxies at z ≃ 3.5 in the mass range 9.0 < log (M⋆/M⊙) < 10.5. These measurements constrain the internal dynamics, the intrinsic velocity dispersions (σint) and rotation velocities (VC) of galaxies in the high-redshift Universe. The mean velocity dispersion of the galaxies in our sample is σint=70.8+3.3−3.1kms−1⁠, revealing that the increasing average σint with increasing redshift, reported for z ≲ 2, continues out to z ≃ 3.5. Only 36 ± 8 per cent of our galaxies are rotation-dominated (VC/σint > 1), with the sample average VC/σint value much smaller than at lower redshift. After carefully selecting comparable star-forming samples at multiple epochs, we find that the rotation-dominated fraction evolves with redshift with a z−0.2 dependence. The rotation-dominated KDS galaxies show no clear offset from the local rotation velocity–stellar mass (i.e. VC–M⋆) relation, although a smaller fraction of the galaxies are on the relation due to the increase in the dispersion-dominated fraction. These observations are consistent with a simple equilibrium model picture, in which random motions are boosted in high-redshift galaxies by a combination of the increasing gas fractions, accretion efficiency, specific star formation rate and stellar feedback and which may provide significant pressure support against gravity on the galactic disc scale."}],"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"publication_status":"published","title":"The KMOS Deep Survey (KDS) – I. Dynamical measurements of typical star-forming galaxies at z ≃ 3.5","oa_version":"Preprint","author":[{"first_name":"O. J.","last_name":"Turner","full_name":"Turner, O. J."},{"last_name":"Cirasuolo","full_name":"Cirasuolo, M.","first_name":"M."},{"full_name":"Harrison, C. M.","last_name":"Harrison","first_name":"C. M."},{"first_name":"R. J.","last_name":"McLure","full_name":"McLure, R. J."},{"last_name":"Dunlop","full_name":"Dunlop, J. S.","first_name":"J. S."},{"last_name":"Swinbank","full_name":"Swinbank, A. M.","first_name":"A. M."},{"first_name":"H. L.","full_name":"Johnson, H. L.","last_name":"Johnson"},{"first_name":"D.","full_name":"Sobral, D.","last_name":"Sobral"},{"first_name":"Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Sharples","full_name":"Sharples, R. M.","first_name":"R. M."}],"day":"01","scopus_import":"1","article_type":"original","date_created":"2022-07-13T10:03:01Z","volume":471,"language":[{"iso":"eng"}],"oa":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","issue":"2","citation":{"ieee":"O. J. Turner <i>et al.</i>, “The KMOS Deep Survey (KDS) – I. Dynamical measurements of typical star-forming galaxies at z ≃ 3.5,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 471, no. 2. Oxford University Press, pp. 1280–1320, 2017.","short":"O.J. Turner, M. Cirasuolo, C.M. Harrison, R.J. McLure, J.S. Dunlop, A.M. Swinbank, H.L. Johnson, D. Sobral, J.J. Matthee, R.M. Sharples, Monthly Notices of the Royal Astronomical Society 471 (2017) 1280–1320.","ama":"Turner OJ, Cirasuolo M, Harrison CM, et al. The KMOS Deep Survey (KDS) – I. Dynamical measurements of typical star-forming galaxies at z ≃ 3.5. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;471(2):1280-1320. doi:<a href=\"https://doi.org/10.1093/mnras/stx1366\">10.1093/mnras/stx1366</a>","apa":"Turner, O. J., Cirasuolo, M., Harrison, C. M., McLure, R. J., Dunlop, J. S., Swinbank, A. M., … Sharples, R. M. (2017). The KMOS Deep Survey (KDS) – I. Dynamical measurements of typical star-forming galaxies at z ≃ 3.5. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stx1366\">https://doi.org/10.1093/mnras/stx1366</a>","mla":"Turner, O. J., et al. “The KMOS Deep Survey (KDS) – I. Dynamical Measurements of Typical Star-Forming Galaxies at z ≃ 3.5.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 471, no. 2, Oxford University Press, 2017, pp. 1280–320, doi:<a href=\"https://doi.org/10.1093/mnras/stx1366\">10.1093/mnras/stx1366</a>.","ista":"Turner OJ, Cirasuolo M, Harrison CM, McLure RJ, Dunlop JS, Swinbank AM, Johnson HL, Sobral D, Matthee JJ, Sharples RM. 2017. The KMOS Deep Survey (KDS) – I. Dynamical measurements of typical star-forming galaxies at z ≃ 3.5. Monthly Notices of the Royal Astronomical Society. 471(2), 1280–1320.","chicago":"Turner, O. J., M. Cirasuolo, C. M. Harrison, R. J. McLure, J. S. Dunlop, A. M. Swinbank, H. L. Johnson, D. Sobral, Jorryt J Matthee, and R. M. Sharples. “The KMOS Deep Survey (KDS) – I. Dynamical Measurements of Typical Star-Forming Galaxies at z ≃ 3.5.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stx1366\">https://doi.org/10.1093/mnras/stx1366</a>."},"month":"10","arxiv":1,"page":"1280-1320","quality_controlled":"1","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1704.06263"}],"publisher":"Oxford University Press","doi":"10.1093/mnras/stx1366","article_processing_charge":"No","type":"journal_article","date_updated":"2022-08-19T08:07:31Z","_id":"11573","status":"public","publication":"Monthly Notices of the Royal Astronomical Society","extern":"1","acknowledgement":"We wish to thank the anonymous referee for their comments, which have improved the quality and clarity of this work. OJT acknowledges the financial support of the Science and Technology Facilities Council through a studentship award. MC and OJT acknowledge the KMOS team and all the personnel of the European Southern Observatory Very Large Telescope for outstanding support during the KMOS GTO observations. CMH, AMS and RMS acknowledge the Science and Technology Facilities Council through grant code ST/L00075X/1. RJM acknowledges the support of the European Research Council via the award of a Consolidator Grant (PI: McLure). JSD acknowledges the support of the European Research Council via the award of an Advanced Grant (PI J. Dunlop), and the contribution of the EC FP7 SPACE project ASTRODEEP (Ref.No: 312725). AMS acknowledges the Leverhulme Foundation. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. DS acknowledges financial support from the Netherlands Organization for Scientific research (NWO) through a Veni fellowship and from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010). This work is based on observations taken by the CANDELS Multi-Cycle Treasury Program with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. This work is based on observations taken by the 3D HST Treasury Program (GO 12177 and 12328) with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Based on data obtained with the European Southern Observatory Very Large Telescope, Paranal, Chile, under Large Program 185.A-0791, and made available by the VUDS team at the CESAM data centre, Laboratoire d’Astrophysique de Marseille, France. Based on observations obtained at the Very Large Telescope of the European Southern Observatory. Programme IDs: 092.A 0399(A), 093.A-0122(A,B), 094.A-0214(A,B),095.A0680(A,B),096.A-0315(A,B,C).","date_published":"2017-10-01T00:00:00Z","external_id":{"arxiv":["1704.06263"]},"year":"2017","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","galaxies: kinematics and dynamics"]},{"pmid":1,"ec_funded":1,"date_published":"2017-01-01T00:00:00Z","project":[{"_id":"25716A02-B435-11E9-9278-68D0E5697425","call_identifier":"FP7","name":"Polarity and subcellular dynamics in plants","grant_number":"282300"}],"status":"public","publication":"Plant Physiology","publist_id":"6199","year":"2017","isi":1,"external_id":{"pmid":["27837086"],"isi":["000394135800041"]},"quality_controlled":"1","page":"552 - 565","ddc":["580"],"date_updated":"2025-05-07T11:12:30Z","_id":"1159","type":"journal_article","doi":"10.1104/pp.16.00943","article_processing_charge":"No","publisher":"American Society of Plant Biologists","issue":"1","citation":{"ieee":"W. Steenackers <i>et al.</i>, “Cis-cinnamic acid is a novel natural auxin efflux inhibitor that promotes lateral root formation,” <i>Plant Physiology</i>, vol. 173, no. 1. American Society of Plant Biologists, pp. 552–565, 2017.","short":"W. Steenackers, P. Klíma, M. Quareshy, I. Cesarino, R. Kumpf, S. Corneillie, P. Araújo, T. Viaene, G. Goeminne, M. Nowack, K. Ljung, J. Friml, J. Blakeslee, O. Novák, E. Zažímalová, R. Napier, W. Boerjan, B. Vanholme, Plant Physiology 173 (2017) 552–565.","ama":"Steenackers W, Klíma P, Quareshy M, et al. Cis-cinnamic acid is a novel natural auxin efflux inhibitor that promotes lateral root formation. <i>Plant Physiology</i>. 2017;173(1):552-565. doi:<a href=\"https://doi.org/10.1104/pp.16.00943\">10.1104/pp.16.00943</a>","apa":"Steenackers, W., Klíma, P., Quareshy, M., Cesarino, I., Kumpf, R., Corneillie, S., … Vanholme, B. (2017). Cis-cinnamic acid is a novel natural auxin efflux inhibitor that promotes lateral root formation. <i>Plant Physiology</i>. American Society of Plant Biologists. <a href=\"https://doi.org/10.1104/pp.16.00943\">https://doi.org/10.1104/pp.16.00943</a>","mla":"Steenackers, Ward, et al. “Cis-Cinnamic Acid Is a Novel Natural Auxin Efflux Inhibitor That Promotes Lateral Root Formation.” <i>Plant Physiology</i>, vol. 173, no. 1, American Society of Plant Biologists, 2017, pp. 552–65, doi:<a href=\"https://doi.org/10.1104/pp.16.00943\">10.1104/pp.16.00943</a>.","ista":"Steenackers W, Klíma P, Quareshy M, Cesarino I, Kumpf R, Corneillie S, Araújo P, Viaene T, Goeminne G, Nowack M, Ljung K, Friml J, Blakeslee J, Novák O, Zažímalová E, Napier R, Boerjan W, Vanholme B. 2017. Cis-cinnamic acid is a novel natural auxin efflux inhibitor that promotes lateral root formation. Plant Physiology. 173(1), 552–565.","chicago":"Steenackers, Ward, Petr Klíma, Mussa Quareshy, Igor Cesarino, Robert Kumpf, Sander Corneillie, Pedro Araújo, et al. “Cis-Cinnamic Acid Is a Novel Natural Auxin Efflux Inhibitor That Promotes Lateral Root Formation.” <i>Plant Physiology</i>. American Society of Plant Biologists, 2017. <a href=\"https://doi.org/10.1104/pp.16.00943\">https://doi.org/10.1104/pp.16.00943</a>."},"user_id":"c635000d-4b10-11ee-a964-aac5a93f6ac1","oa":1,"language":[{"iso":"eng"}],"department":[{"_id":"JiFr"}],"file":[{"relation":"main_file","checksum":"fd4d1cfe7ed70e54bb12ae3881f3fb91","file_name":"2016_PlantPhysi_Steenackers.pdf","content_type":"application/pdf","access_level":"open_access","file_id":"7040","file_size":4109142,"date_created":"2019-11-18T16:12:25Z","creator":"dernst","date_updated":"2020-07-14T12:44:36Z"}],"month":"01","publication_identifier":{"issn":["0032-0889"]},"publication_status":"published","file_date_updated":"2020-07-14T12:44:36Z","has_accepted_license":"1","intvolume":"       173","abstract":[{"lang":"eng","text":"Auxin steers numerous physiological processes in plants, making the tight control of its endogenous levels and spatiotemporal distribution a necessity. This regulation is achieved by different mechanisms, including auxin biosynthesis, metabolic conversions, degradation, and transport. Here, we introduce cis-cinnamic acid (c-CA) as a novel and unique addition to a small group of endogenous molecules affecting in planta auxin concentrations. c-CA is the photo-isomerization product of the phenylpropanoid pathway intermediate trans-CA (t-CA). When grown on c-CA-containing medium, an evolutionary diverse set of plant species were shown to exhibit phenotypes characteristic for high auxin levels, including inhibition of primary root growth, induction of root hairs, and promotion of adventitious and lateral rooting. By molecular docking and receptor binding assays, we showed that c-CA itself is neither an auxin nor an anti-auxin, and auxin profiling data revealed that c-CA does not significantly interfere with auxin biosynthesis. Single cell-based auxin accumulation assays showed that c-CA, and not t-CA, is a potent inhibitor of auxin efflux. Auxin signaling reporters detected changes in spatiotemporal distribution of the auxin response along the root of c-CA-treated plants, and long-distance auxin transport assays showed no inhibition of rootward auxin transport. Overall, these results suggest that the phenotypes of c-CA-treated plants are the consequence of a local change in auxin accumulation, induced by the inhibition of auxin efflux. This work reveals a novel mechanism how plants may regulate auxin levels and adds a novel, naturally occurring molecule to the chemical toolbox for the studies of auxin homeostasis."}],"volume":173,"article_type":"original","date_created":"2018-12-11T11:50:28Z","author":[{"first_name":"Ward","full_name":"Steenackers, Ward","last_name":"Steenackers"},{"last_name":"Klíma","full_name":"Klíma, Petr","first_name":"Petr"},{"first_name":"Mussa","full_name":"Quareshy, Mussa","last_name":"Quareshy"},{"last_name":"Cesarino","full_name":"Cesarino, Igor","first_name":"Igor"},{"full_name":"Kumpf, Robert","last_name":"Kumpf","first_name":"Robert"},{"first_name":"Sander","full_name":"Corneillie, Sander","last_name":"Corneillie"},{"last_name":"Araújo","full_name":"Araújo, Pedro","first_name":"Pedro"},{"full_name":"Viaene, Tom","last_name":"Viaene","first_name":"Tom"},{"first_name":"Geert","last_name":"Goeminne","full_name":"Goeminne, Geert"},{"full_name":"Nowack, Moritz","last_name":"Nowack","first_name":"Moritz"},{"full_name":"Ljung, Karin","last_name":"Ljung","first_name":"Karin"},{"first_name":"Jirí","orcid":"0000-0002-8302-7596","id":"4159519E-F248-11E8-B48F-1D18A9856A87","full_name":"Friml, Jirí","last_name":"Friml"},{"first_name":"Joshua","full_name":"Blakeslee, Joshua","last_name":"Blakeslee"},{"first_name":"Ondřej","full_name":"Novák, Ondřej","last_name":"Novák"},{"first_name":"Eva","full_name":"Zažímalová, Eva","last_name":"Zažímalová"},{"last_name":"Napier","full_name":"Napier, Richard","first_name":"Richard"},{"last_name":"Boerjan","full_name":"Boerjan, Wout","first_name":"Wout"},{"last_name":"Vanholme","full_name":"Vanholme, Bartel","first_name":"Bartel"}],"day":"01","scopus_import":"1","oa_version":"Submitted Version","title":"Cis-cinnamic acid is a novel natural auxin efflux inhibitor that promotes lateral root formation"},{"author":[{"first_name":"Sebastian","orcid":"0000-0001-5964-0203","last_name":"Altmeyer","id":"2EE67FDC-F248-11E8-B48F-1D18A9856A87","full_name":"Altmeyer, Sebastian"},{"full_name":"Do, Younghae","last_name":"Do","first_name":"Younghae"},{"first_name":"Ying","full_name":"Lai, Ying","last_name":"Lai"}],"scopus_import":"1","day":"06","oa_version":"Published Version","title":"Dynamics of ferrofluidic flow in the Taylor-Couette system with a small aspect ratio","volume":7,"date_created":"2018-12-11T11:50:28Z","has_accepted_license":"1","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","image":"/images/cc_by.png","short":"CC BY (4.0)"},"intvolume":"         7","abstract":[{"lang":"eng","text":"We investigate fundamental nonlinear dynamics of ferrofluidic Taylor-Couette flow - flow confined be-tween two concentric independently rotating cylinders - consider small aspect ratio by solving the ferro-hydrodynamical equations, carrying out systematic bifurcation analysis. Without magnetic field, we find steady flow patterns, previously observed with a simple fluid, such as those containing normal one- or two vortex cells, as well as anomalous one-cell and twin-cell flow states. However, when a symmetry-breaking transverse magnetic field is present, all flow states exhibit stimulated, finite two-fold mode. Various bifurcations between steady and unsteady states can occur, corresponding to the transitions between the two-cell and one-cell states. While unsteady, axially oscillating flow states can arise, we also detect the emergence of new unsteady flow states. In particular, we uncover two new states: one contains only the azimuthally oscillating solution in the configuration of the twin-cell flow state, and an-other a rotating flow state. Topologically, these flow states are a limit cycle and a quasiperiodic solution on a two-torus, respectively. Emergence of new flow states in addition to observed ones with classical fluid, indicates that richer but potentially more controllable dynamics in ferrofluidic flows, as such flow states depend on the external magnetic field."}],"publication_identifier":{"issn":["20452322"]},"publication_status":"published","file_date_updated":"2020-07-14T12:44:36Z","month":"01","department":[{"_id":"BjHo"}],"file":[{"date_created":"2018-12-12T10:10:16Z","file_size":4546835,"date_updated":"2020-07-14T12:44:36Z","creator":"system","file_id":"4802","file_name":"IST-2017-743-v1+1_srep40012.pdf","content_type":"application/pdf","access_level":"open_access","relation":"main_file","checksum":"694aa70399444570825099c1a7ec91f2"}],"article_number":"40012","oa":1,"language":[{"iso":"eng"}],"pubrep_id":"743","citation":{"apa":"Altmeyer, S., Do, Y., &#38; Lai, Y. (2017). Dynamics of ferrofluidic flow in the Taylor-Couette system with a small aspect ratio. <i>Scientific Reports</i>. Nature Publishing Group. <a href=\"https://doi.org/10.1038/srep40012\">https://doi.org/10.1038/srep40012</a>","mla":"Altmeyer, Sebastian, et al. “Dynamics of Ferrofluidic Flow in the Taylor-Couette System with a Small Aspect Ratio.” <i>Scientific Reports</i>, vol. 7, 40012, Nature Publishing Group, 2017, doi:<a href=\"https://doi.org/10.1038/srep40012\">10.1038/srep40012</a>.","ista":"Altmeyer S, Do Y, Lai Y. 2017. Dynamics of ferrofluidic flow in the Taylor-Couette system with a small aspect ratio. Scientific Reports. 7, 40012.","chicago":"Altmeyer, Sebastian, Younghae Do, and Ying Lai. “Dynamics of Ferrofluidic Flow in the Taylor-Couette System with a Small Aspect Ratio.” <i>Scientific Reports</i>. Nature Publishing Group, 2017. <a href=\"https://doi.org/10.1038/srep40012\">https://doi.org/10.1038/srep40012</a>.","ieee":"S. Altmeyer, Y. Do, and Y. Lai, “Dynamics of ferrofluidic flow in the Taylor-Couette system with a small aspect ratio,” <i>Scientific Reports</i>, vol. 7. Nature Publishing Group, 2017.","short":"S. Altmeyer, Y. Do, Y. Lai, Scientific Reports 7 (2017).","ama":"Altmeyer S, Do Y, Lai Y. Dynamics of ferrofluidic flow in the Taylor-Couette system with a small aspect ratio. <i>Scientific Reports</i>. 2017;7. doi:<a href=\"https://doi.org/10.1038/srep40012\">10.1038/srep40012</a>"},"user_id":"c635000d-4b10-11ee-a964-aac5a93f6ac1","doi":"10.1038/srep40012","article_processing_charge":"No","publisher":"Nature Publishing Group","date_updated":"2023-09-20T11:28:49Z","_id":"1160","type":"journal_article","ddc":["532"],"quality_controlled":"1","year":"2017","isi":1,"external_id":{"isi":["000391269700001"]},"publist_id":"6198","status":"public","publication":"Scientific Reports","date_published":"2017-01-06T00:00:00Z"},{"doi":"10.1016/j.cub.2016.11.035","article_processing_charge":"No","publisher":"Cell Press","date_updated":"2023-09-20T11:28:19Z","_id":"1161","type":"journal_article","page":"R24 - R25","quality_controlled":"1","year":"2017","isi":1,"external_id":{"isi":["000391902500010"]},"publist_id":"6197","publication":"Current Biology","status":"public","date_published":"2017-01-09T00:00:00Z","author":[{"first_name":"Jan","last_name":"Müller","full_name":"Müller, Jan","id":"AD07FDB4-0F61-11EA-8158-C4CC64CEAA8D"},{"last_name":"Sixt","id":"41E9FBEA-F248-11E8-B48F-1D18A9856A87","full_name":"Sixt, Michael K","orcid":"0000-0002-6620-9179","first_name":"Michael K"}],"scopus_import":"1","day":"09","title":"Cell migration: Making the waves","oa_version":"None","volume":27,"date_created":"2018-12-11T11:50:29Z","abstract":[{"text":"Coordinated changes of cell shape are often the result of the excitable, wave-like dynamics of the actin cytoskeleton. New work shows that, in migrating cells, protrusion waves arise from mechanochemical crosstalk between adhesion sites, membrane tension and the actin protrusive machinery.","lang":"eng"}],"intvolume":"        27","publication_identifier":{"issn":["09609822"]},"publication_status":"published","month":"01","department":[{"_id":"MiSi"}],"language":[{"iso":"eng"}],"issue":"1","citation":{"short":"J. Müller, M.K. Sixt, Current Biology 27 (2017) R24–R25.","ieee":"J. Müller and M. K. Sixt, “Cell migration: Making the waves,” <i>Current Biology</i>, vol. 27, no. 1. Cell Press, pp. R24–R25, 2017.","ama":"Müller J, Sixt MK. Cell migration: Making the waves. <i>Current Biology</i>. 2017;27(1):R24-R25. doi:<a href=\"https://doi.org/10.1016/j.cub.2016.11.035\">10.1016/j.cub.2016.11.035</a>","mla":"Müller, Jan, and Michael K. Sixt. “Cell Migration: Making the Waves.” <i>Current Biology</i>, vol. 27, no. 1, Cell Press, 2017, pp. R24–25, doi:<a href=\"https://doi.org/10.1016/j.cub.2016.11.035\">10.1016/j.cub.2016.11.035</a>.","apa":"Müller, J., &#38; Sixt, M. K. (2017). Cell migration: Making the waves. <i>Current Biology</i>. Cell Press. <a href=\"https://doi.org/10.1016/j.cub.2016.11.035\">https://doi.org/10.1016/j.cub.2016.11.035</a>","chicago":"Müller, Jan, and Michael K Sixt. “Cell Migration: Making the Waves.” <i>Current Biology</i>. Cell Press, 2017. <a href=\"https://doi.org/10.1016/j.cub.2016.11.035\">https://doi.org/10.1016/j.cub.2016.11.035</a>.","ista":"Müller J, Sixt MK. 2017. Cell migration: Making the waves. Current Biology. 27(1), R24–R25."},"user_id":"c635000d-4b10-11ee-a964-aac5a93f6ac1"}]