[{"acknowledgement":"We are grateful to J. Zhu for fruitful discussions. A.F.Y. acknowledges support from the Office of Naval Research under award N00014-20-1-2609, and the Gordon and Betty Moore Foundation under award GBMF9471. M.P.Z. acknowledges support from the ARO under MURI W911NF-16-1-0361. K.W. and T.T. acknowledge support from the Elemental Strategy Initiative conducted by the MEXT, Japan, via grant no. JPMXP0112101001; JSPS KAKENHI grant no. JP20H00354; and the CREST(JPMJCR15F3), JST. A.V. was supported by a Simons Investigator Award. P.L. was supported by the Department of Defense (DoD) through the National Defense Science and Engineering Graduate Fellowship (NDSEG) Program.","doi":"10.1038/s41567-021-01418-6","keyword":["general physics","astronomy"],"language":[{"iso":"eng"}],"title":"Topological charge density waves at half-integer filling of a moiré superlattice","citation":{"ista":"Polshyn H, Zhang Y, Kumar MA, Soejima T, Ledwith P, Watanabe K, Taniguchi T, Vishwanath A, Zaletel MP, Young AF. 2021. Topological charge density waves at half-integer filling of a moiré superlattice. Nature Physics.","ieee":"H. Polshyn et al., “Topological charge density waves at half-integer filling of a moiré superlattice,” Nature Physics. Springer Nature, 2021.","chicago":"Polshyn, Hryhoriy, Y. Zhang, M. A. Kumar, T. Soejima, P. Ledwith, K. Watanabe, T. Taniguchi, A. Vishwanath, M. P. Zaletel, and A. F. Young. “Topological Charge Density Waves at Half-Integer Filling of a Moiré Superlattice.” Nature Physics. Springer Nature, 2021. https://doi.org/10.1038/s41567-021-01418-6.","mla":"Polshyn, Hryhoriy, et al. “Topological Charge Density Waves at Half-Integer Filling of a Moiré Superlattice.” Nature Physics, Springer Nature, 2021, doi:10.1038/s41567-021-01418-6.","short":"H. Polshyn, Y. Zhang, M.A. Kumar, T. Soejima, P. Ledwith, K. Watanabe, T. Taniguchi, A. Vishwanath, M.P. Zaletel, A.F. Young, Nature Physics (2021).","apa":"Polshyn, H., Zhang, Y., Kumar, M. A., Soejima, T., Ledwith, P., Watanabe, K., … Young, A. F. (2021). Topological charge density waves at half-integer filling of a moiré superlattice. Nature Physics. Springer Nature. https://doi.org/10.1038/s41567-021-01418-6","ama":"Polshyn H, Zhang Y, Kumar MA, et al. Topological charge density waves at half-integer filling of a moiré superlattice. Nature Physics. 2021. doi:10.1038/s41567-021-01418-6"},"author":[{"orcid":"0000-0001-8223-8896","id":"edfc7cb1-526e-11ec-b05a-e6ecc27e4e48","first_name":"Hryhoriy","full_name":"Polshyn, Hryhoriy","last_name":"Polshyn"},{"full_name":"Zhang, Y.","first_name":"Y.","last_name":"Zhang"},{"last_name":"Kumar","full_name":"Kumar, M. A.","first_name":"M. A."},{"last_name":"Soejima","first_name":"T.","full_name":"Soejima, T."},{"full_name":"Ledwith, P.","first_name":"P.","last_name":"Ledwith"},{"first_name":"K.","full_name":"Watanabe, K.","last_name":"Watanabe"},{"last_name":"Taniguchi","full_name":"Taniguchi, T.","first_name":"T."},{"last_name":"Vishwanath","first_name":"A.","full_name":"Vishwanath, A."},{"first_name":"M. P.","full_name":"Zaletel, M. P.","last_name":"Zaletel"},{"last_name":"Young","first_name":"A. F.","full_name":"Young, A. F."}],"type":"journal_article","day":"09","publisher":"Springer Nature","status":"public","publication":"Nature Physics","quality_controlled":"1","date_created":"2022-01-13T12:30:47Z","month":"12","extern":"1","publication_identifier":{"eissn":["1745-2481"],"issn":["1745-2473"]},"scopus_import":"1","external_id":{"arxiv":["2104.01178"]},"user_id":"8b945eb4-e2f2-11eb-945a-df72226e66a9","date_updated":"2022-01-13T14:11:31Z","oa_version":"Preprint","year":"2021","article_type":"original","main_file_link":[{"url":"https://arxiv.org/abs/2104.01178","open_access":"1"}],"oa":1,"publication_status":"published","article_processing_charge":"No","arxiv":1,"date_published":"2021-12-09T00:00:00Z","_id":"10617","abstract":[{"text":"When a flat band is partially filled with electrons, strong Coulomb interactions between them may lead to the emergence of topological gapped states with quantized Hall conductivity. Such emergent topological states have been found in partially filled Landau levels1 and Hofstadter bands2,3; however, in both cases, a large magnetic field is required to produce the underlying flat band. The recent observation of quantum anomalous Hall effects in narrow-band moiré materials4,5,6,7 has led to the theoretical prediction that such phases could be realized at zero magnetic field8,9,10,11,12. Here we report the observation of insulators with Chern number C = 1 in the zero-magnetic-field limit at half-integer filling of the moiré superlattice unit cell in twisted monolayer–bilayer graphene7,13,14,15. Chern insulators in a half-filled band suggest the spontaneous doubling of the superlattice unit cell2,3,16, and our calculations find a ground state of the topological charge density wave at half-filling of the underlying band. The discovery of these topological phases at fractional superlattice filling enables the further pursuit of zero-magnetic-field phases that have fractional statistics that exist either as elementary excitations or bound to lattice dislocations.","lang":"eng"}]},{"year":"2021","oa_version":"Published Version","article_type":"original","publication_identifier":{"issn":["2041-1723"]},"scopus_import":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2023-02-28T13:21:51Z","_id":"12585","abstract":[{"lang":"eng","text":"Glaciers in High Mountain Asia generate meltwater that supports the water needs of 250 million people, but current knowledge of annual accumulation and ablation is limited to sparse field measurements biased in location and glacier size. Here, we present altitudinally-resolved specific mass balances (surface, internal, and basal combined) for 5527 glaciers in High Mountain Asia for 2000–2016, derived by correcting observed glacier thinning patterns for mass redistribution due to ice flow. We find that 41% of glaciers accumulated mass over less than 20% of their area, and only 60% ± 10% of regional annual ablation was compensated by accumulation. Even without 21st century warming, 21% ± 1% of ice volume will be lost by 2100 due to current climatic-geometric imbalance, representing a reduction in glacier ablation into rivers of 28% ± 1%. The ablation of glaciers in the Himalayas and Tien Shan was mostly unsustainable and ice volume in these regions will reduce by at least 30% by 2100. The most important and vulnerable glacier-fed river basins (Amu Darya, Indus, Syr Darya, Tarim Interior) were supplied with >50% sustainable glacier ablation but will see long-term reductions in ice mass and glacier meltwater supply regardless of the Karakoram Anomaly."}],"date_published":"2021-05-17T00:00:00Z","article_number":"2868","article_processing_charge":"No","volume":12,"oa":1,"main_file_link":[{"url":"https://doi.org/10.1038/s41467-021-23073-4","open_access":"1"}],"publication_status":"published","author":[{"first_name":"Evan","full_name":"Miles, Evan","last_name":"Miles"},{"full_name":"McCarthy, Michael","first_name":"Michael","last_name":"McCarthy"},{"last_name":"Dehecq","full_name":"Dehecq, Amaury","first_name":"Amaury"},{"full_name":"Kneib, Marin","first_name":"Marin","last_name":"Kneib"},{"last_name":"Fugger","first_name":"Stefan","full_name":"Fugger, Stefan"},{"last_name":"Pellicciotti","first_name":"Francesca","full_name":"Pellicciotti, Francesca","id":"b28f055a-81ea-11ed-b70c-a9fe7f7b0e70"}],"type":"journal_article","day":"17","title":"Health and sustainability of glaciers in High Mountain Asia","citation":{"short":"E. Miles, M. McCarthy, A. Dehecq, M. Kneib, S. Fugger, F. Pellicciotti, Nature Communications 12 (2021).","apa":"Miles, E., McCarthy, M., Dehecq, A., Kneib, M., Fugger, S., & Pellicciotti, F. (2021). Health and sustainability of glaciers in High Mountain Asia. Nature Communications. Springer Nature. https://doi.org/10.1038/s41467-021-23073-4","ama":"Miles E, McCarthy M, Dehecq A, Kneib M, Fugger S, Pellicciotti F. Health and sustainability of glaciers in High Mountain Asia. Nature Communications. 2021;12. doi:10.1038/s41467-021-23073-4","ista":"Miles E, McCarthy M, Dehecq A, Kneib M, Fugger S, Pellicciotti F. 2021. Health and sustainability of glaciers in High Mountain Asia. Nature Communications. 12, 2868.","ieee":"E. Miles, M. McCarthy, A. Dehecq, M. Kneib, S. Fugger, and F. Pellicciotti, “Health and sustainability of glaciers in High Mountain Asia,” Nature Communications, vol. 12. Springer Nature, 2021.","chicago":"Miles, Evan, Michael McCarthy, Amaury Dehecq, Marin Kneib, Stefan Fugger, and Francesca Pellicciotti. “Health and Sustainability of Glaciers in High Mountain Asia.” Nature Communications. Springer Nature, 2021. https://doi.org/10.1038/s41467-021-23073-4.","mla":"Miles, Evan, et al. “Health and Sustainability of Glaciers in High Mountain Asia.” Nature Communications, vol. 12, 2868, Springer Nature, 2021, doi:10.1038/s41467-021-23073-4."},"doi":"10.1038/s41467-021-23073-4","keyword":["General Physics and Astronomy","General Biochemistry","Genetics and Molecular Biology","General Chemistry","Multidisciplinary"],"language":[{"iso":"eng"}],"date_created":"2023-02-20T08:11:29Z","month":"05","extern":"1","intvolume":" 12","status":"public","publication":"Nature Communications","quality_controlled":"1","publisher":"Springer Nature"},{"user_id":"4359f0d1-fa6c-11eb-b949-802e58b17ae8","date_updated":"2023-08-10T14:16:16Z","external_id":{"isi":["000655481800014"]},"scopus_import":"1","publication_identifier":{"issn":["2041-1723"]},"acknowledged_ssus":[{"_id":"SSU"}],"article_type":"original","has_accepted_license":"1","year":"2021","oa_version":"Published Version","file_date_updated":"2021-12-17T11:34:50Z","volume":12,"tmp":{"legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","short":"CC BY (4.0)"},"publication_status":"published","oa":1,"file":[{"creator":"kschuh","file_size":3108845,"file_name":"2021_NatureCommunications_Vandael.pdf","checksum":"6036a8cdae95e1707c2a04d54e325ff4","access_level":"open_access","date_updated":"2021-12-17T11:34:50Z","file_id":"10563","relation":"main_file","content_type":"application/pdf","date_created":"2021-12-17T11:34:50Z","success":1}],"article_number":"2912","_id":"9778","date_published":"2021-05-18T00:00:00Z","abstract":[{"text":"The hippocampal mossy fiber synapse is a key synapse of the trisynaptic circuit. Post-tetanic potentiation (PTP) is the most powerful form of plasticity at this synaptic connection. It is widely believed that mossy fiber PTP is an entirely presynaptic phenomenon, implying that PTP induction is input-specific, and requires neither activity of multiple inputs nor stimulation of postsynaptic neurons. To directly test cooperativity and associativity, we made paired recordings between single mossy fiber terminals and postsynaptic CA3 pyramidal neurons in rat brain slices. By stimulating non-overlapping mossy fiber inputs converging onto single CA3 neurons, we confirm that PTP is input-specific and non-cooperative. Unexpectedly, mossy fiber PTP exhibits anti-associative induction properties. EPSCs show only minimal PTP after combined pre- and postsynaptic high-frequency stimulation with intact postsynaptic Ca2+ signaling, but marked PTP in the absence of postsynaptic spiking and after suppression of postsynaptic Ca2+ signaling (10 mM EGTA). PTP is largely recovered by inhibitors of voltage-gated R- and L-type Ca2+ channels, group II mGluRs, and vacuolar-type H+-ATPase, suggesting the involvement of retrograde vesicular glutamate signaling. Transsynaptic regulation of PTP extends the repertoire of synaptic computations, implementing a brake on mossy fiber detonation and a “smart teacher” function of hippocampal mossy fiber synapses.","lang":"eng"}],"issue":"1","article_processing_charge":"No","language":[{"iso":"eng"}],"keyword":["general physics and astronomy","general biochemistry","genetics and molecular biology","general chemistry"],"doi":"10.1038/s41467-021-23153-5","ddc":["570"],"acknowledgement":"We thank Drs. Carolina Borges-Merjane and Jose Guzman for critically reading the manuscript, and Pablo Castillo for discussions. We are grateful to Alois Schlögl for help with analysis, Florian Marr for excellent technical assistance and cell reconstruction, Christina Altmutter for technical help, Eleftheria Kralli-Beller for manuscript editing, and the Scientific Service Units of IST Austria for support. This project received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (grant agreement No 692692) and the Fond zur Förderung der Wissenschaftlichen Forschung (Z 312-B27, Wittgenstein award), both to P.J.","related_material":{"link":[{"relation":"press_release","url":"https://ist.ac.at/en/news/synaptic-transmission-not-a-one-way-street/","description":"News on IST Homepage"}]},"project":[{"_id":"25B7EB9E-B435-11E9-9278-68D0E5697425","call_identifier":"H2020","grant_number":"692692","name":"Biophysics and circuit function of a giant cortical glumatergic synapse"},{"_id":"25C5A090-B435-11E9-9278-68D0E5697425","call_identifier":"FWF","grant_number":"Z00312","name":"The Wittgenstein Prize"}],"day":"18","type":"journal_article","author":[{"id":"3AE48E0A-F248-11E8-B48F-1D18A9856A87","orcid":"0000-0001-7577-1676","full_name":"Vandael, David H","first_name":"David H","last_name":"Vandael"},{"id":"3337E116-F248-11E8-B48F-1D18A9856A87","orcid":"0000-0003-0408-6094","first_name":"Yuji","full_name":"Okamoto, Yuji","last_name":"Okamoto"},{"orcid":"0000-0001-5001-4804","id":"353C1B58-F248-11E8-B48F-1D18A9856A87","last_name":"Jonas","full_name":"Jonas, Peter M","first_name":"Peter M"}],"ec_funded":1,"citation":{"mla":"Vandael, David H., et al. “Transsynaptic Modulation of Presynaptic Short-Term Plasticity in Hippocampal Mossy Fiber Synapses.” Nature Communications, vol. 12, no. 1, 2912, Springer, 2021, doi:10.1038/s41467-021-23153-5.","ista":"Vandael DH, Okamoto Y, Jonas PM. 2021. Transsynaptic modulation of presynaptic short-term plasticity in hippocampal mossy fiber synapses. Nature Communications. 12(1), 2912.","ieee":"D. H. Vandael, Y. Okamoto, and P. M. Jonas, “Transsynaptic modulation of presynaptic short-term plasticity in hippocampal mossy fiber synapses,” Nature Communications, vol. 12, no. 1. Springer, 2021.","chicago":"Vandael, David H, Yuji Okamoto, and Peter M Jonas. “Transsynaptic Modulation of Presynaptic Short-Term Plasticity in Hippocampal Mossy Fiber Synapses.” Nature Communications. Springer, 2021. https://doi.org/10.1038/s41467-021-23153-5.","apa":"Vandael, D. H., Okamoto, Y., & Jonas, P. M. (2021). Transsynaptic modulation of presynaptic short-term plasticity in hippocampal mossy fiber synapses. Nature Communications. Springer. https://doi.org/10.1038/s41467-021-23153-5","ama":"Vandael DH, Okamoto Y, Jonas PM. Transsynaptic modulation of presynaptic short-term plasticity in hippocampal mossy fiber synapses. Nature Communications. 2021;12(1). doi:10.1038/s41467-021-23153-5","short":"D.H. Vandael, Y. Okamoto, P.M. Jonas, Nature Communications 12 (2021)."},"title":"Transsynaptic modulation of presynaptic short-term plasticity in hippocampal mossy fiber synapses","department":[{"_id":"PeJo"}],"quality_controlled":"1","publication":"Nature Communications","status":"public","intvolume":" 12","publisher":"Springer","isi":1,"month":"05","date_created":"2021-08-06T07:22:55Z"},{"publication":"SciPost Physics","department":[{"_id":"MaSe"}],"quality_controlled":"1","status":"public","intvolume":" 11","publisher":"SciPost","isi":1,"month":"09","date_created":"2021-09-02T11:49:47Z","keyword":["General Physics and Astronomy"],"language":[{"iso":"eng"}],"doi":"10.21468/scipostphys.11.3.048","ddc":["519"],"project":[{"call_identifier":"H2020","_id":"260C2330-B435-11E9-9278-68D0E5697425","name":"ISTplus - Postdoctoral Fellowships","grant_number":"754411"}],"day":"02","type":"journal_article","author":[{"first_name":"Stefano","full_name":"De Nicola, Stefano","last_name":"De Nicola","id":"42832B76-F248-11E8-B48F-1D18A9856A87","orcid":"0000-0002-4842-6671"}],"citation":{"ieee":"S. De Nicola, “Importance sampling scheme for the stochastic simulation of quantum spin dynamics,” SciPost Physics, vol. 11, no. 3. SciPost, 2021.","ista":"De Nicola S. 2021. Importance sampling scheme for the stochastic simulation of quantum spin dynamics. SciPost Physics. 11(3), 048.","chicago":"De Nicola, Stefano. “Importance Sampling Scheme for the Stochastic Simulation of Quantum Spin Dynamics.” SciPost Physics. SciPost, 2021. https://doi.org/10.21468/scipostphys.11.3.048.","mla":"De Nicola, Stefano. “Importance Sampling Scheme for the Stochastic Simulation of Quantum Spin Dynamics.” SciPost Physics, vol. 11, no. 3, 048, SciPost, 2021, doi:10.21468/scipostphys.11.3.048.","short":"S. De Nicola, SciPost Physics 11 (2021).","apa":"De Nicola, S. (2021). Importance sampling scheme for the stochastic simulation of quantum spin dynamics. SciPost Physics. SciPost. https://doi.org/10.21468/scipostphys.11.3.048","ama":"De Nicola S. Importance sampling scheme for the stochastic simulation of quantum spin dynamics. SciPost Physics. 2021;11(3). doi:10.21468/scipostphys.11.3.048"},"ec_funded":1,"title":"Importance sampling scheme for the stochastic simulation of quantum spin dynamics","file_date_updated":"2021-09-02T14:05:43Z","tmp":{"legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","short":"CC BY (4.0)"},"volume":11,"publication_status":"published","oa":1,"article_number":"048","file":[{"checksum":"e4ec69d893e31811efc6093cb6ea8eb7","access_level":"open_access","date_updated":"2021-09-02T14:05:43Z","creator":"cchlebak","file_size":373833,"file_name":"2021_SciPostPhys_DeNicola.pdf","date_created":"2021-09-02T14:05:43Z","success":1,"file_id":"9984","relation":"main_file","content_type":"application/pdf"}],"abstract":[{"lang":"eng","text":"The numerical simulation of dynamical phenomena in interacting quantum systems is a notoriously hard problem. Although a number of promising numerical methods exist, they often have limited applicability due to the growth of entanglement or the presence of the so-called sign problem. In this work, we develop an importance sampling scheme for the simulation of quantum spin dynamics, building on a recent approach mapping quantum spin systems to classical stochastic processes. The importance sampling scheme is based on identifying the classical trajectory that yields the largest contribution to a given quantum observable. An exact transformation is then carried out to preferentially sample trajectories that are close to the dominant one. We demonstrate that this approach is capable of reducing the temporal growth of fluctuations in the stochastic quantities, thus extending the range of accessible times and system sizes compared to direct sampling. We discuss advantages and limitations of the proposed approach, outlining directions\r\nfor further developments."}],"_id":"9981","date_published":"2021-09-02T00:00:00Z","arxiv":1,"article_processing_charge":"No","issue":"3","external_id":{"isi":["000692534200001"],"arxiv":["2103.16468"]},"user_id":"4359f0d1-fa6c-11eb-b949-802e58b17ae8","date_updated":"2023-08-11T10:59:29Z","publication_identifier":{"eissn":["2666-9366"],"issn":["2542-4653"]},"article_type":"original","year":"2021","has_accepted_license":"1","oa_version":"Published Version"},{"publisher":"EDP Sciences","quality_controlled":"1","publication":"Astronomy & Astrophysics","status":"public","intvolume":" 641","extern":"1","month":"09","date_created":"2022-07-06T09:38:16Z","acknowledgement":"We thank Margherita Talia, Stéphane Charlot, Adele Plat and Alba Vidal-García for helpful discussions. This work is supported by the ERC advanced grant 339659-MUSICOS (R. Bacon). AF acknowledges the support from grant PRIN MIUR 2017 20173ML3WW. MVM and JP would like to thank the Leiden/ESA Astrophysics Program for Summer Students (LEAPS) for funding at the outset of this project. FL, HK, and AV acknowledge support from the ERC starting grant ERC-757258-TRIPLE. TH was supported by Leading Initiative for Excellent Young Researchers, MEXT, Japan. JB acknowledges support by FCT/MCTES through national funds by the grant UID/FIS/04434/2019, UIDB/04434/2020 and UIDP/04434/2020 and through the Investigador FCT Contract No. IF/01654/2014/CP1215/CT0003. HI acknowledges support from JSPS KAKENHI Grant Number JP19K23462. We would also like to thank the organizers and participants of the Leiden Lorentz Center workshop: Revolutionary Spectroscopy of Today as a Springboard to Webb. This work made use of several open source python packages: NUMPY (van der Walt et al. 2011), MATPLOTLIB (Hunter 2007), ASTROPY (Astropy Collaboration 2013) and MPDAF (MUSE Python Data Analysis Framework, Piqueras et al. 2019).","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution / galaxies: high-redshift / ISM: lines and bands / ultraviolet: ISM / ultraviolet: galaxies"],"doi":"10.1051/0004-6361/202038133","citation":{"chicago":"Feltre, Anna, Michael V. Maseda, Roland Bacon, Jayadev Pradeep, Floriane Leclercq, Haruka Kusakabe, Lutz Wisotzki, et al. “The MUSE Hubble Ultra Deep Field Survey: XV. The Mean Rest-UV Spectra of Lyα Emitters at z > 3.” Astronomy & Astrophysics. EDP Sciences, 2020. https://doi.org/10.1051/0004-6361/202038133.","ieee":"A. Feltre et al., “The MUSE Hubble Ultra Deep Field Survey: XV. The mean rest-UV spectra of Lyα emitters at z > 3,” Astronomy & Astrophysics, vol. 641. EDP Sciences, 2020.","ista":"Feltre A, Maseda MV, Bacon R, Pradeep J, Leclercq F, Kusakabe H, Wisotzki L, Hashimoto T, Schmidt KB, Blaizot J, Brinchmann J, Boogaard L, Cantalupo S, Carton D, Inami H, Kollatschny W, Marino RA, Matthee JJ, Nanayakkara T, Richard J, Schaye J, Tresse L, Urrutia T, Verhamme A, Weilbacher PM. 2020. The MUSE Hubble Ultra Deep Field Survey: XV. The mean rest-UV spectra of Lyα emitters at z > 3. Astronomy & Astrophysics. 641, A118.","mla":"Feltre, Anna, et al. “The MUSE Hubble Ultra Deep Field Survey: XV. The Mean Rest-UV Spectra of Lyα Emitters at z > 3.” Astronomy & Astrophysics, vol. 641, A118, EDP Sciences, 2020, doi:10.1051/0004-6361/202038133.","short":"A. Feltre, M.V. Maseda, R. Bacon, J. Pradeep, F. Leclercq, H. Kusakabe, L. Wisotzki, T. Hashimoto, K.B. Schmidt, J. Blaizot, J. Brinchmann, L. Boogaard, S. Cantalupo, D. Carton, H. Inami, W. Kollatschny, R.A. Marino, J.J. Matthee, T. Nanayakkara, J. Richard, J. Schaye, L. Tresse, T. Urrutia, A. Verhamme, P.M. Weilbacher, Astronomy & Astrophysics 641 (2020).","ama":"Feltre A, Maseda MV, Bacon R, et al. The MUSE Hubble Ultra Deep Field Survey: XV. The mean rest-UV spectra of Lyα emitters at z > 3. Astronomy & Astrophysics. 2020;641. doi:10.1051/0004-6361/202038133","apa":"Feltre, A., Maseda, M. V., Bacon, R., Pradeep, J., Leclercq, F., Kusakabe, H., … Weilbacher, P. M. (2020). The MUSE Hubble Ultra Deep Field Survey: XV. The mean rest-UV spectra of Lyα emitters at z > 3. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202038133"},"title":"The MUSE Hubble Ultra Deep Field Survey: XV. The mean rest-UV spectra of Lyα emitters at z > 3","day":"18","author":[{"last_name":"Feltre","first_name":"Anna","full_name":"Feltre, Anna"},{"last_name":"Maseda","full_name":"Maseda, Michael V.","first_name":"Michael V."},{"last_name":"Bacon","first_name":"Roland","full_name":"Bacon, Roland"},{"full_name":"Pradeep, Jayadev","first_name":"Jayadev","last_name":"Pradeep"},{"full_name":"Leclercq, Floriane","first_name":"Floriane","last_name":"Leclercq"},{"full_name":"Kusakabe, Haruka","first_name":"Haruka","last_name":"Kusakabe"},{"last_name":"Wisotzki","full_name":"Wisotzki, Lutz","first_name":"Lutz"},{"first_name":"Takuya","full_name":"Hashimoto, Takuya","last_name":"Hashimoto"},{"full_name":"Schmidt, Kasper B.","first_name":"Kasper B.","last_name":"Schmidt"},{"last_name":"Blaizot","first_name":"Jeremy","full_name":"Blaizot, Jeremy"},{"last_name":"Brinchmann","first_name":"Jarle","full_name":"Brinchmann, Jarle"},{"last_name":"Boogaard","full_name":"Boogaard, Leindert","first_name":"Leindert"},{"last_name":"Cantalupo","full_name":"Cantalupo, Sebastiano","first_name":"Sebastiano"},{"last_name":"Carton","full_name":"Carton, David","first_name":"David"},{"last_name":"Inami","full_name":"Inami, Hanae","first_name":"Hanae"},{"last_name":"Kollatschny","first_name":"Wolfram","full_name":"Kollatschny, Wolfram"},{"full_name":"Marino, Raffaella A.","first_name":"Raffaella A.","last_name":"Marino"},{"last_name":"Matthee","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"full_name":"Nanayakkara, Themiya","first_name":"Themiya","last_name":"Nanayakkara"},{"first_name":"Johan","full_name":"Richard, Johan","last_name":"Richard"},{"last_name":"Schaye","full_name":"Schaye, Joop","first_name":"Joop"},{"last_name":"Tresse","first_name":"Laurence","full_name":"Tresse, Laurence"},{"full_name":"Urrutia, Tanya","first_name":"Tanya","last_name":"Urrutia"},{"full_name":"Verhamme, Anne","first_name":"Anne","last_name":"Verhamme"},{"last_name":"Weilbacher","full_name":"Weilbacher, Peter M.","first_name":"Peter M."}],"type":"journal_article","publication_status":"published","oa":1,"main_file_link":[{"url":"https://arxiv.org/abs/2007.01878","open_access":"1"}],"volume":641,"arxiv":1,"article_processing_charge":"No","article_number":"A118","_id":"11501","abstract":[{"lang":"eng","text":"We investigated the ultraviolet (UV) spectral properties of faint Lyman-α emitters (LAEs) in the redshift range 2.9 ≤ z ≤ 4.6, and we provide material to prepare future observations of the faint Universe. We used data from the MUSE Hubble Ultra Deep Survey to construct mean rest-frame spectra of continuum-faint (median MUV of −18 and down to MUV of −16), low stellar mass (median value of 108.4 M⊙ and down to 107 M⊙) LAEs at redshift z ≳ 3. We computed various averaged spectra of LAEs, subsampled on the basis of their observational (e.g., Lyα strength, UV magnitude and spectral slope) and physical (e.g., stellar mass and star-formation rate) properties. We searched for UV spectral features other than Lyα, such as higher ionization nebular emission lines and absorption features. We successfully observed the O III]λ1666 and [C III]λ1907+C III]λ1909 collisionally excited emission lines and the He IIλ1640 recombination feature, as well as the resonant C IVλλ1548,1551 doublet either in emission or P-Cygni. We compared the observed spectral properties of the different mean spectra and find the emission lines to vary with the observational and physical properties of the LAEs. In particular, the mean spectra of LAEs with larger Lyα equivalent widths, fainter UV magnitudes, bluer UV spectral slopes, and lower stellar masses show the strongest nebular emission. The line ratios of these lines are similar to those measured in the spectra of local metal-poor galaxies, while their equivalent widths are weaker compared to the handful of extreme values detected in individual spectra of z > 2 galaxies. This suggests that weak UV features are likely ubiquitous in high z, low-mass, and faint LAEs. We publicly released the stacked spectra, as they can serve as empirical templates for the design of future observations, such as those with the James Webb Space Telescope and the Extremely Large Telescope."}],"date_published":"2020-09-18T00:00:00Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2022-07-19T09:35:43Z","scopus_import":"1","external_id":{"arxiv":["2007.01878"]},"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"article_type":"original","year":"2020","oa_version":"Published Version"},{"_id":"11503","abstract":[{"lang":"eng","text":"Context. The Lyα emitter (LAE) fraction, XLAE, is a potentially powerful probe of the evolution of the intergalactic neutral hydrogen gas fraction. However, uncertainties in the measurement of XLAE are still under debate.\r\nAims. Thanks to deep data obtained with the integral field spectrograph Multi Unit Spectroscopic Explorer (MUSE), we can measure the evolution of the LAE fraction homogeneously over a wide redshift range of z ≈ 3–6 for UV-faint galaxies (down to UV magnitudes of M1500 ≈ −17.75). This is a significantly fainter range than in former studies (M1500 ≤ −18.75) and it allows us to probe the bulk of the population of high-redshift star-forming galaxies.\r\nMethods. We constructed a UV-complete photometric-redshift sample following UV luminosity functions and measured the Lyα emission with MUSE using the latest (second) data release from the MUSE Hubble Ultra Deep Field Survey.\r\nResults. We derived the redshift evolution of XLAE for M1500 ∈ [ − 21.75; −17.75] for the first time with a equivalent width range EW(Lyα) ≥ 65 Å and found low values of XLAE ≲ 30% at z ≲ 6. The best-fit linear relation is XLAE = 0.07+0.06−0.03z − 0.22+0.12−0.24. For M1500 ∈ [ − 20.25; −18.75] and EW(Lyα) ≥ 25 Å, our XLAE values are consistent with those in the literature within 1σ at z ≲ 5, but our median values are systematically lower than reported values over the whole redshift range. In addition, we do not find a significant dependence of XLAE on M1500 for EW(Lyα) ≥ 50 Å at z ≈ 3–4, in contrast with previous work. The differences in XLAE mainly arise from selection biases for Lyman Break Galaxies (LBGs) in the literature: UV-faint LBGs are more easily selected if they have strong Lyα emission, hence XLAE is biased towards higher values when those samples are used.\r\nConclusions. Our results suggest either a lower increase of XLAE towards z ≈ 6 than previously suggested, or even a turnover of XLAE at z ≈ 5.5, which may be the signature of a late or patchy reionization process. We compared our results with predictions from a cosmological galaxy evolution model. We find that a model with a bursty star formation (SF) can reproduce our observed LAE fractions much better than models where SF is a smooth function of time."}],"date_published":"2020-06-03T00:00:00Z","article_number":"A12","article_processing_charge":"No","arxiv":1,"volume":638,"main_file_link":[{"url":"https://arxiv.org/abs/2003.12083","open_access":"1"}],"oa":1,"publication_status":"published","year":"2020","oa_version":"Published Version","article_type":"original","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"external_id":{"arxiv":["2003.12083"]},"scopus_import":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2022-07-19T09:35:20Z","date_created":"2022-07-06T09:50:48Z","month":"06","extern":"1","status":"public","intvolume":" 638","publication":"Astronomy & Astrophysics","quality_controlled":"1","publisher":"EDP Sciences","author":[{"last_name":"Kusakabe","full_name":"Kusakabe, Haruka","first_name":"Haruka"},{"last_name":"Blaizot","full_name":"Blaizot, Jérémy","first_name":"Jérémy"},{"first_name":"Thibault","full_name":"Garel, Thibault","last_name":"Garel"},{"full_name":"Verhamme, Anne","first_name":"Anne","last_name":"Verhamme"},{"last_name":"Bacon","full_name":"Bacon, Roland","first_name":"Roland"},{"last_name":"Richard","full_name":"Richard, Johan","first_name":"Johan"},{"first_name":"Takuya","full_name":"Hashimoto, Takuya","last_name":"Hashimoto"},{"last_name":"Inami","full_name":"Inami, Hanae","first_name":"Hanae"},{"full_name":"Conseil, Simon","first_name":"Simon","last_name":"Conseil"},{"last_name":"Guiderdoni","full_name":"Guiderdoni, Bruno","first_name":"Bruno"},{"full_name":"Drake, Alyssa B.","first_name":"Alyssa B.","last_name":"Drake"},{"last_name":"Christian Herenz","first_name":"Edmund","full_name":"Christian Herenz, Edmund"},{"full_name":"Schaye, Joop","first_name":"Joop","last_name":"Schaye"},{"full_name":"Oesch, Pascal","first_name":"Pascal","last_name":"Oesch"},{"first_name":"Jorryt J","full_name":"Matthee, Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X"},{"last_name":"Anna Marino","first_name":"Raffaella","full_name":"Anna Marino, Raffaella"},{"first_name":"Kasper","full_name":"Borello Schmidt, Kasper","last_name":"Borello Schmidt"},{"last_name":"Pelló","first_name":"Roser","full_name":"Pelló, Roser"},{"first_name":"Michael","full_name":"Maseda, Michael","last_name":"Maseda"},{"full_name":"Leclercq, Floriane","first_name":"Floriane","last_name":"Leclercq"},{"full_name":"Kerutt, Josephine","first_name":"Josephine","last_name":"Kerutt"},{"full_name":"Mahler, Guillaume","first_name":"Guillaume","last_name":"Mahler"}],"type":"journal_article","day":"03","title":"The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6","citation":{"apa":"Kusakabe, H., Blaizot, J., Garel, T., Verhamme, A., Bacon, R., Richard, J., … Mahler, G. (2020). The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201937340","ama":"Kusakabe H, Blaizot J, Garel T, et al. The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6. Astronomy & Astrophysics. 2020;638. doi:10.1051/0004-6361/201937340","short":"H. Kusakabe, J. Blaizot, T. Garel, A. Verhamme, R. Bacon, J. Richard, T. Hashimoto, H. Inami, S. Conseil, B. Guiderdoni, A.B. Drake, E. Christian Herenz, J. Schaye, P. Oesch, J.J. Matthee, R. Anna Marino, K. Borello Schmidt, R. Pelló, M. Maseda, F. Leclercq, J. Kerutt, G. Mahler, Astronomy & Astrophysics 638 (2020).","mla":"Kusakabe, Haruka, et al. “The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα Emitter Fraction from z = 3 to z = 6.” Astronomy & Astrophysics, vol. 638, A12, EDP Sciences, 2020, doi:10.1051/0004-6361/201937340.","ieee":"H. Kusakabe et al., “The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6,” Astronomy & Astrophysics, vol. 638. EDP Sciences, 2020.","ista":"Kusakabe H, Blaizot J, Garel T, Verhamme A, Bacon R, Richard J, Hashimoto T, Inami H, Conseil S, Guiderdoni B, Drake AB, Christian Herenz E, Schaye J, Oesch P, Matthee JJ, Anna Marino R, Borello Schmidt K, Pelló R, Maseda M, Leclercq F, Kerutt J, Mahler G. 2020. The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6. Astronomy & Astrophysics. 638, A12.","chicago":"Kusakabe, Haruka, Jérémy Blaizot, Thibault Garel, Anne Verhamme, Roland Bacon, Johan Richard, Takuya Hashimoto, et al. “The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα Emitter Fraction from z = 3 to z = 6.” Astronomy & Astrophysics. EDP Sciences, 2020. https://doi.org/10.1051/0004-6361/201937340."},"doi":"10.1051/0004-6361/201937340","keyword":["Space and Planetary Science","Astronomy and Astrophysics","dark ages / reionization / first stars / early Universe / cosmology: observations / galaxies: evolution / galaxies: high-redshift / intergalactic medium"],"language":[{"iso":"eng"}],"acknowledgement":"We thank the anonymous referee for constructive comments and suggestions. We would like to express our gratitude to Stephane De Barros and Pablo Arrabal Haro for kindly providing their data plotted in Figs. 1, 2, and 8. We are grateful to Kazuhiro Shimasaku, Masami Ouchi, Rieko Momose, Daniel Schaerer, Hidenobu Yajima, Taku Okamura, Makoto Ando, and Hinako Goto for giving insightful comments and suggestions. This work is based on observations taken by VLT, which is operated by European Southern Observatory. This research made use of Astropy (http://www.astropy.org), which is a community-developed core Python package for Astronomy (Astropy Collaboration 2013, 2018), MARZ, MPDAF, and matplotlib (Hunter 2007). H.K. acknowledges support from Japan Society for the Promotion of Science (JSPS) through the JSPS Research Fellowship for Young Scientists and Overseas Challenge Program for Young Researchers. AV acknowledges support from the ERC starting grant 757258-TRIPLE and the SNF Professorship 176808-TRIPLE. This work was supported by the project FOGHAR (Agence Nationale de la Recherche, ANR-13-BS05-0010-02). JB acknowledges support from the ORAGE project from the Agence Nationale de la Recherche under grant ANR-14-CE33-0016-03. JR acknowledges support from the ERC starting grant 336736-CALENDS. T. H. acknowledges supports by the Grant-inAid for Scientic Research 19J01620."},{"status":"public","intvolume":" 635","quality_controlled":"1","publication":"Astronomy & Astrophysics","publisher":"EDP Sciences","date_created":"2022-07-06T09:56:20Z","extern":"1","month":"03","doi":"10.1051/0004-6361/201937339","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics galaxies: high-redshift / galaxies: formation / galaxies: evolution / cosmology: observations"],"acknowledgement":"F.L., R.B., and S.C. acknowledge support from the ERC advanced grant 339659-MUSICOS. F.L., T.G., H.K., and A.V. acknowledge support from the ERC starting grant ERC-757258-TRIPLE. A.C. and J.R. acknowledge support from the ERC starting grant 336736-CALENDS. J.B. acknowledges support by FCT/MCTES through national funds (PID-DAC) by grant UID/FIS/04434/2019 and through Investigador FCT Contract No.IF/01654/2014/CP1215/CT0003. T.H. was supported by Leading Initiative for Excellent Young Researchers, MEXT, Japan.","type":"journal_article","author":[{"full_name":"Leclercq, Floriane","first_name":"Floriane","last_name":"Leclercq"},{"first_name":"Roland","full_name":"Bacon, Roland","last_name":"Bacon"},{"full_name":"Verhamme, Anne","first_name":"Anne","last_name":"Verhamme"},{"last_name":"Garel","first_name":"Thibault","full_name":"Garel, Thibault"},{"first_name":"Jérémy","full_name":"Blaizot, Jérémy","last_name":"Blaizot"},{"first_name":"Jarle","full_name":"Brinchmann, Jarle","last_name":"Brinchmann"},{"last_name":"Cantalupo","full_name":"Cantalupo, Sebastiano","first_name":"Sebastiano"},{"last_name":"Claeyssens","first_name":"Adélaïde","full_name":"Claeyssens, Adélaïde"},{"full_name":"Conseil, Simon","first_name":"Simon","last_name":"Conseil"},{"last_name":"Contini","full_name":"Contini, Thierry","first_name":"Thierry"},{"last_name":"Hashimoto","first_name":"Takuya","full_name":"Hashimoto, Takuya"},{"full_name":"Herenz, Edmund Christian","first_name":"Edmund Christian","last_name":"Herenz"},{"last_name":"Kusakabe","full_name":"Kusakabe, Haruka","first_name":"Haruka"},{"last_name":"Marino","first_name":"Raffaella Anna","full_name":"Marino, Raffaella Anna"},{"full_name":"Maseda, Michael","first_name":"Michael","last_name":"Maseda"},{"full_name":"Matthee, Jorryt J","first_name":"Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X"},{"first_name":"Peter","full_name":"Mitchell, Peter","last_name":"Mitchell"},{"last_name":"Pezzulli","first_name":"Gabriele","full_name":"Pezzulli, Gabriele"},{"full_name":"Richard, Johan","first_name":"Johan","last_name":"Richard"},{"full_name":"Schmidt, Kasper Borello","first_name":"Kasper Borello","last_name":"Schmidt"},{"last_name":"Wisotzki","first_name":"Lutz","full_name":"Wisotzki, Lutz"}],"day":"11","title":"The MUSE Hubble Ultra Deep field survey: XIII. Spatially resolved spectral properties of Lyman α haloes around star-forming galaxies at z > 3","citation":{"chicago":"Leclercq, Floriane, Roland Bacon, Anne Verhamme, Thibault Garel, Jérémy Blaizot, Jarle Brinchmann, Sebastiano Cantalupo, et al. “The MUSE Hubble Ultra Deep Field Survey: XIII. Spatially Resolved Spectral Properties of Lyman α Haloes around Star-Forming Galaxies at z > 3.” Astronomy & Astrophysics. EDP Sciences, 2020. https://doi.org/10.1051/0004-6361/201937339.","ista":"Leclercq F, Bacon R, Verhamme A, Garel T, Blaizot J, Brinchmann J, Cantalupo S, Claeyssens A, Conseil S, Contini T, Hashimoto T, Herenz EC, Kusakabe H, Marino RA, Maseda M, Matthee JJ, Mitchell P, Pezzulli G, Richard J, Schmidt KB, Wisotzki L. 2020. The MUSE Hubble Ultra Deep field survey: XIII. Spatially resolved spectral properties of Lyman α haloes around star-forming galaxies at z > 3. Astronomy & Astrophysics. 635, A82.","ieee":"F. Leclercq et al., “The MUSE Hubble Ultra Deep field survey: XIII. Spatially resolved spectral properties of Lyman α haloes around star-forming galaxies at z > 3,” Astronomy & Astrophysics, vol. 635. EDP Sciences, 2020.","mla":"Leclercq, Floriane, et al. “The MUSE Hubble Ultra Deep Field Survey: XIII. Spatially Resolved Spectral Properties of Lyman α Haloes around Star-Forming Galaxies at z > 3.” Astronomy & Astrophysics, vol. 635, A82, EDP Sciences, 2020, doi:10.1051/0004-6361/201937339.","short":"F. Leclercq, R. Bacon, A. Verhamme, T. Garel, J. Blaizot, J. Brinchmann, S. Cantalupo, A. Claeyssens, S. Conseil, T. Contini, T. Hashimoto, E.C. Herenz, H. Kusakabe, R.A. Marino, M. Maseda, J.J. Matthee, P. Mitchell, G. Pezzulli, J. Richard, K.B. Schmidt, L. Wisotzki, Astronomy & Astrophysics 635 (2020).","ama":"Leclercq F, Bacon R, Verhamme A, et al. The MUSE Hubble Ultra Deep field survey: XIII. Spatially resolved spectral properties of Lyman α haloes around star-forming galaxies at z > 3. Astronomy & Astrophysics. 2020;635. doi:10.1051/0004-6361/201937339","apa":"Leclercq, F., Bacon, R., Verhamme, A., Garel, T., Blaizot, J., Brinchmann, J., … Wisotzki, L. (2020). The MUSE Hubble Ultra Deep field survey: XIII. Spatially resolved spectral properties of Lyman α haloes around star-forming galaxies at z > 3. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201937339"},"volume":635,"oa":1,"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2002.05731"}],"publication_status":"published","_id":"11504","date_published":"2020-03-11T00:00:00Z","abstract":[{"lang":"eng","text":"We present spatially resolved maps of six individually-detected Lyman α haloes (LAHs) as well as a first statistical analysis of the Lyman α (Lyα) spectral signature in the circum-galactic medium of high-redshift star-forming galaxies (−17.5 > MUV > −21.5) using the Multi-Unit Spectroscopic Explorer. Our resolved spectroscopic analysis of the LAHs reveals significant intrahalo variations of the Lyα line profile. Using a three-dimensional two-component model for the Lyα emission, we measured the full width at half maximum (FWHM), the peak velocity shift, and the asymmetry of the Lyα line in the core and in the halo of 19 galaxies. We find that the Lyα line shape is statistically different in the halo compared to the core (in terms of width, peak wavelength, and asymmetry) for ≈40% of our galaxies. Similarly to object-by-object based studies and a recent resolved study using lensing, we find a correlation between the peak velocity shift and the width of the Lyα line both at the interstellar and circum-galactic scales. This trend has been predicted by radiative transfer simulations of galactic winds as a result of resonant scattering in outflows. While there is a lack of correlation between the spectral properties and the spatial scale lengths of our LAHs, we find a correlation between the width of the line in the LAH and the halo flux fraction. Interestingly, UV bright galaxies (MUV < −20) show broader, more redshifted, and less asymmetric Lyα lines in their haloes. The most significant correlation found is for the FWHM of the line and the UV continuum slope of the galaxy, suggesting that the redder galaxies have broader Lyα lines. The generally broad and red line shapes found in the halo component suggest that the Lyα haloes are powered either by scattering processes through an outflowing medium, fluorescent emission from outflowing cold clumps of gas, or a mix of both. Considering the large diversity of the Lyα line profiles observed in our sample and the lack of strong correlation, the interpretation of our results is still broadly open and underlines the need for realistic spatially resolved models of the LAHs."}],"article_number":"A82","article_processing_charge":"No","arxiv":1,"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"date_updated":"2022-07-19T09:36:58Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","scopus_import":"1","external_id":{"arxiv":["2002.05731"]},"oa_version":"Published Version","year":"2020","article_type":"original"},{"doi":"10.3847/1538-4357/ab75c3","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"acknowledgement":"We are thankful to the anonymous referee for useful comments and suggestions that improved the quality of this paper. B.D. acknowledges financial support from NASA through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G, and the National Science Foundation, grant number 1716907. B.D. is thankful to Andreas Faisst, Laura Danly, and Matthew Burlando for their companionship during the observing run. B.D. is grateful to the COSMOS team for their useful comments during the team meeting in New York City 2019 May 14–17. A.R. research was made possible by Friends of W. M. Keck Observatory who philanthropically support the Keck Science Collaborative (KSC) fund. The observations presented herein were obtained at the W. M. Keck Observatory (program C236, PI Scoville), which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors would like to recognize and acknowledge the very prominent cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are fortunate to have the opportunity to perform observations from this mountain.","type":"journal_article","author":[{"full_name":"Darvish, Behnam","first_name":"Behnam","last_name":"Darvish"},{"first_name":"Nick Z.","full_name":"Scoville, Nick Z.","last_name":"Scoville"},{"first_name":"Christopher","full_name":"Martin, Christopher","last_name":"Martin"},{"first_name":"David","full_name":"Sobral, David","last_name":"Sobral"},{"full_name":"Mobasher, Bahram","first_name":"Bahram","last_name":"Mobasher"},{"full_name":"Rettura, Alessandro","first_name":"Alessandro","last_name":"Rettura"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","last_name":"Matthee"},{"last_name":"Capak","first_name":"Peter","full_name":"Capak, Peter"},{"last_name":"Chartab","full_name":"Chartab, Nima","first_name":"Nima"},{"first_name":"Shoubaneh","full_name":"Hemmati, Shoubaneh","last_name":"Hemmati"},{"last_name":"Masters","first_name":"Daniel","full_name":"Masters, Daniel"},{"first_name":"Hooshang","full_name":"Nayyeri, Hooshang","last_name":"Nayyeri"},{"last_name":"O’Sullivan","full_name":"O’Sullivan, Donal","first_name":"Donal"},{"last_name":"Paulino-Afonso","first_name":"Ana","full_name":"Paulino-Afonso, Ana"},{"full_name":"Sattari, Zahra","first_name":"Zahra","last_name":"Sattari"},{"last_name":"Shahidi","full_name":"Shahidi, Abtin","first_name":"Abtin"},{"last_name":"Salvato","first_name":"Mara","full_name":"Salvato, Mara"},{"first_name":"Brian C.","full_name":"Lemaux, Brian C.","last_name":"Lemaux"},{"last_name":"Fèvre","first_name":"Olivier Le","full_name":"Fèvre, Olivier Le"},{"last_name":"Cucciati","full_name":"Cucciati, Olga","first_name":"Olga"}],"day":"19","title":"Spectroscopic confirmation of a coma cluster progenitor at z ∼ 2.2","citation":{"mla":"Darvish, Behnam, et al. “Spectroscopic Confirmation of a Coma Cluster Progenitor at z ∼ 2.2.” The Astrophysical Journal, vol. 892, no. 1, 8, IOP Publishing, 2020, doi:10.3847/1538-4357/ab75c3.","ieee":"B. Darvish et al., “Spectroscopic confirmation of a coma cluster progenitor at z ∼ 2.2,” The Astrophysical Journal, vol. 892, no. 1. IOP Publishing, 2020.","ista":"Darvish B, Scoville NZ, Martin C, Sobral D, Mobasher B, Rettura A, Matthee JJ, Capak P, Chartab N, Hemmati S, Masters D, Nayyeri H, O’Sullivan D, Paulino-Afonso A, Sattari Z, Shahidi A, Salvato M, Lemaux BC, Fèvre OL, Cucciati O. 2020. Spectroscopic confirmation of a coma cluster progenitor at z ∼ 2.2. The Astrophysical Journal. 892(1), 8.","chicago":"Darvish, Behnam, Nick Z. Scoville, Christopher Martin, David Sobral, Bahram Mobasher, Alessandro Rettura, Jorryt J Matthee, et al. “Spectroscopic Confirmation of a Coma Cluster Progenitor at z ∼ 2.2.” The Astrophysical Journal. IOP Publishing, 2020. https://doi.org/10.3847/1538-4357/ab75c3.","apa":"Darvish, B., Scoville, N. Z., Martin, C., Sobral, D., Mobasher, B., Rettura, A., … Cucciati, O. (2020). Spectroscopic confirmation of a coma cluster progenitor at z ∼ 2.2. The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/ab75c3","ama":"Darvish B, Scoville NZ, Martin C, et al. Spectroscopic confirmation of a coma cluster progenitor at z ∼ 2.2. The Astrophysical Journal. 2020;892(1). doi:10.3847/1538-4357/ab75c3","short":"B. Darvish, N.Z. Scoville, C. Martin, D. Sobral, B. Mobasher, A. Rettura, J.J. Matthee, P. Capak, N. Chartab, S. Hemmati, D. Masters, H. Nayyeri, D. O’Sullivan, A. Paulino-Afonso, Z. Sattari, A. Shahidi, M. Salvato, B.C. Lemaux, O.L. Fèvre, O. Cucciati, The Astrophysical Journal 892 (2020)."},"intvolume":" 892","status":"public","quality_controlled":"1","publication":"The Astrophysical Journal","publisher":"IOP Publishing","date_created":"2022-07-06T13:10:51Z","extern":"1","month":"03","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"date_updated":"2022-07-19T09:31:35Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","scopus_import":"1","external_id":{"arxiv":["2002.06207"]},"year":"2020","oa_version":"Preprint","article_type":"original","volume":892,"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2002.06207"}],"oa":1,"publication_status":"published","date_published":"2020-03-19T00:00:00Z","_id":"11513","abstract":[{"lang":"eng","text":"We report the spectroscopic confirmation of a new protocluster in the COSMOS field at z ∼ 2.2, COSMOS Cluster 2.2 (CC2.2), originally identified as an overdensity of narrowband selected Hα emitting candidates. With only two masks of Keck/MOSFIRE near-IR spectroscopy in both H (∼1.47–1.81 μm) and K (∼1.92–2.40 μm) bands (∼1.5 hr each), we confirm 35 unique protocluster members with at least two emission lines detected with S/N > 3. Combined with 12 extra members from the zCOSMOS-deep spectroscopic survey (47 in total), we estimate a mean redshift and a line-of-sight velocity dispersion of zmean = 2.23224 ± 0.00101 and σlos = 645 ± 69 km s−1 for this protocluster, respectively. Assuming virialization and spherical symmetry for the system, we estimate a total mass of Mvir ∼ (1–2) ×1014M⊙ for the structure. We evaluate a number density enhancement of δg ∼ 7 for this system and we argue that the structure is likely not fully virialized at z ∼ 2.2. However, in a spherical collapse model, δg is expected to grow to a linear matter enhancement of ∼1.9 by z = 0, exceeding the collapse threshold of 1.69, and leading to a fully collapsed and virialized Coma-type structure with a total mass of Mdyn(z = 0) ∼ 9.2 × 1014M⊙ by now. This observationally efficient confirmation suggests that large narrowband emission-line galaxy surveys, when combined with ancillary photometric data, can be used to effectively trace the large-scale structure and protoclusters at a time when they are mostly dominated by star-forming galaxies."}],"article_number":"8","issue":"1","article_processing_charge":"No","arxiv":1},{"status":"public","intvolume":" 496","publication":"Monthly Notices of the Royal Astronomical Society","quality_controlled":"1","publisher":"Oxford University Press","date_created":"2022-07-07T10:20:11Z","month":"08","extern":"1","page":"1013-1022","doi":"10.1093/mnras/staa1347","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: haloes","galaxies: high-redshift","quasars: absorption lines"],"language":[{"iso":"eng"}],"related_material":{"link":[{"relation":"erratum","url":"https://doi.org/10.1093/mnras/staa2668"}]},"acknowledgement":"We thank the anonymous referee for useful suggestions. This study is based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programme(s): 094.A-0131(B), 095.A 0200(A), 096.A0222(A), 097.A-0089(A), and 099.A-0159(A). SM acknowledges support from the Alexander von Humboldt Foundation, Germany. SM thanks Christian Herenz for useful discussion. SC gratefully acknowledges support from Swiss National Science Foundation grant PP00P2 163824. JB acknowledges support by FCT/MCTES through national funds by grant UID/FIS/04434/2019 and through Investigador FCT Contract No. IF/01654/2014/CP1215/CT0003. NB and JZ acknowledge support from ANR grant ANR-17-CE31- 0017 (3DGasFlows). AC and JR acknowledge support from the ERC starting grant 336736-CALENDS. MA acknowledges support from European Union’s H2020 Marie Skłodowska-Curie Actions grant 721463 to the SUNDIAL ITN, and from the Spanish Ministry of Economy and Competitiveness (MINECO) under grant number AYA2016-76219-P. MA also acknowledges support from the Fundacion BBVA under its 2017 programme of assistance to ´scientific research groups, for the project ‘Using machine-learning techniques to drag galaxies from the noise in deep imaging’. FL and AV acknowledge support from the ERC starting grant ERC757258-TRIPLE.","type":"journal_article","author":[{"last_name":"Muzahid","full_name":"Muzahid, Sowgat","first_name":"Sowgat"},{"full_name":"Schaye, Joop","first_name":"Joop","last_name":"Schaye"},{"full_name":"Marino, Raffaella Anna","first_name":"Raffaella Anna","last_name":"Marino"},{"full_name":"Cantalupo, Sebastiano","first_name":"Sebastiano","last_name":"Cantalupo"},{"last_name":"Brinchmann","full_name":"Brinchmann, Jarle","first_name":"Jarle"},{"last_name":"Contini","first_name":"Thierry","full_name":"Contini, Thierry"},{"full_name":"Wendt, Martin","first_name":"Martin","last_name":"Wendt"},{"last_name":"Wisotzki","full_name":"Wisotzki, Lutz","first_name":"Lutz"},{"last_name":"Zabl","full_name":"Zabl, Johannes","first_name":"Johannes"},{"full_name":"Bouché, Nicolas","first_name":"Nicolas","last_name":"Bouché"},{"last_name":"Akhlaghi","first_name":"Mohammad","full_name":"Akhlaghi, Mohammad"},{"last_name":"Chen","first_name":"Hsiao-Wen","full_name":"Chen, Hsiao-Wen"},{"last_name":"Claeyssens","full_name":"Claeyssens, Adélaîde","first_name":"Adélaîde"},{"last_name":"Johnson","full_name":"Johnson, Sean","first_name":"Sean"},{"last_name":"Leclercq","first_name":"Floriane","full_name":"Leclercq, Floriane"},{"full_name":"Maseda, Michael","first_name":"Michael","last_name":"Maseda"},{"orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","full_name":"Matthee, Jorryt J","first_name":"Jorryt J"},{"last_name":"Richard","first_name":"Johan","full_name":"Richard, Johan"},{"last_name":"Urrutia","full_name":"Urrutia, Tanya","first_name":"Tanya"},{"full_name":"Verhamme, Anne","first_name":"Anne","last_name":"Verhamme"}],"day":"01","title":"MUSEQuBES: Calibrating the redshifts of Lyα emitters using stacked circumgalactic medium absorption profiles","citation":{"mla":"Muzahid, Sowgat, et al. “MUSEQuBES: Calibrating the Redshifts of Lyα Emitters Using Stacked Circumgalactic Medium Absorption Profiles.” Monthly Notices of the Royal Astronomical Society, vol. 496, no. 2, Oxford University Press, 2020, pp. 1013–22, doi:10.1093/mnras/staa1347.","ieee":"S. Muzahid et al., “MUSEQuBES: Calibrating the redshifts of Lyα emitters using stacked circumgalactic medium absorption profiles,” Monthly Notices of the Royal Astronomical Society, vol. 496, no. 2. Oxford University Press, pp. 1013–1022, 2020.","ista":"Muzahid S, Schaye J, Marino RA, Cantalupo S, Brinchmann J, Contini T, Wendt M, Wisotzki L, Zabl J, Bouché N, Akhlaghi M, Chen H-W, Claeyssens A, Johnson S, Leclercq F, Maseda M, Matthee JJ, Richard J, Urrutia T, Verhamme A. 2020. MUSEQuBES: Calibrating the redshifts of Lyα emitters using stacked circumgalactic medium absorption profiles. Monthly Notices of the Royal Astronomical Society. 496(2), 1013–1022.","chicago":"Muzahid, Sowgat, Joop Schaye, Raffaella Anna Marino, Sebastiano Cantalupo, Jarle Brinchmann, Thierry Contini, Martin Wendt, et al. “MUSEQuBES: Calibrating the Redshifts of Lyα Emitters Using Stacked Circumgalactic Medium Absorption Profiles.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2020. https://doi.org/10.1093/mnras/staa1347.","apa":"Muzahid, S., Schaye, J., Marino, R. A., Cantalupo, S., Brinchmann, J., Contini, T., … Verhamme, A. (2020). MUSEQuBES: Calibrating the redshifts of Lyα emitters using stacked circumgalactic medium absorption profiles. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staa1347","ama":"Muzahid S, Schaye J, Marino RA, et al. MUSEQuBES: Calibrating the redshifts of Lyα emitters using stacked circumgalactic medium absorption profiles. Monthly Notices of the Royal Astronomical Society. 2020;496(2):1013-1022. doi:10.1093/mnras/staa1347","short":"S. Muzahid, J. Schaye, R.A. Marino, S. Cantalupo, J. Brinchmann, T. Contini, M. Wendt, L. Wisotzki, J. Zabl, N. Bouché, M. Akhlaghi, H.-W. Chen, A. Claeyssens, S. Johnson, F. Leclercq, M. Maseda, J.J. Matthee, J. Richard, T. Urrutia, A. Verhamme, Monthly Notices of the Royal Astronomical Society 496 (2020) 1013–1022."},"volume":496,"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1910.03593"}],"oa":1,"publication_status":"published","date_published":"2020-08-01T00:00:00Z","_id":"11528","abstract":[{"text":"Ly α emission lines are typically found to be redshifted with respect to the systemic redshifts of galaxies, likely due to resonant scattering of Ly α photons. Here, we measure the average velocity offset for a sample of 96 z ≈ 3.3 Ly α emitters (LAEs) with a median Ly α flux (luminosity) of ≈10−17 erg cm−2 s−1 (≈1042 erg s−1) and a median star formation rate (SFR) of ≈1.3 M⊙ yr−1 (not corrected for possible dust extinction), detected by the Multi-Unit Spectroscopic Explorer as part of our MUSEQuBES circumgalactic medium (CGM) survey. By postulating that the stacked CGM absorption profiles of these LAEs, probed by eight background quasars, must be centred on the systemic redshift, we measure an average velocity offset, Voffset = 171\\pm 8 km s−1, between the Ly α emission peak and the systemic redshift. The observed Voffset is lower by factors of ≈1.4 and ≈2.6 compared to the velocity offsets measured for narrow-band-selected LAEs and Lyman break galaxies, respectively, which probe galaxies with higher masses and SFRs. Consistent with earlier studies based on direct measurements for individual objects, we find that the Voffset is correlated with the full width at half-maximum of the red peak of the Ly α line, and anticorrelated with the rest-frame equivalent width. Moreover, we find that Voffset is correlated with SFR with a sub-linear scaling relation, Voffset∝SFR0.16±0.03. Adopting the mass scaling for main-sequence galaxies, such a relation suggests that Voffset scales with the circular velocity of the dark matter haloes hosting the LAEs.","lang":"eng"}],"article_processing_charge":"No","issue":"2","arxiv":1,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"external_id":{"arxiv":["1910.03593"]},"scopus_import":"1","date_updated":"2022-08-18T11:00:24Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","year":"2020","oa_version":"Preprint","article_type":"original"},{"year":"2020","oa_version":"Preprint","article_type":"original","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"scopus_import":"1","external_id":{"arxiv":["2008.01731"]},"date_updated":"2022-08-18T11:04:05Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","_id":"11529","date_published":"2020-10-01T00:00:00Z","abstract":[{"text":"CR7 is among the most luminous Ly α emitters (LAEs) known at z = 6.6 and consists of at least three UV components that are surrounded by Ly α emission. Previous studies have suggested that it may host an extreme ionizing source. Here, we present deep integral field spectroscopy of CR7 with VLT/Multi Unit Spectroscopic Explorer (MUSE). We measure extended emission with a similar halo scale length as typical LAEs at z ≈ 5. CR7’s Ly α halo is clearly elongated along the direction connecting the multiple components, likely tracing the underlying gas distribution. The Ly α emission originates almost exclusively from the brightest UV component, but we also identify a faint kinematically distinct Ly α emitting region nearby a fainter component. Combined with new near-infrared data, the MUSE data show that the rest-frame Ly α equivalent width (EW) is ≈100 Å. This is a factor 4 higher than the EW measured in low-redshift analogues with carefully matched Ly α profiles (and thus arguably H I column density), but this EW can plausibly be explained by star formation. Alternative scenarios requiring active galactic nucleus (AGN) powering are also disfavoured by the narrower and steeper Ly α spectrum and much smaller IR to UV ratio compared to obscured AGN in other Ly α blobs. CR7’s Ly α emission, while extremely luminous, resembles the emission in more common LAEs at lower redshifts very well and is likely powered by a young metal-poor starburst.","lang":"eng"}],"article_processing_charge":"No","issue":"2","arxiv":1,"volume":498,"oa":1,"main_file_link":[{"url":"https://arxiv.org/abs/2008.01731","open_access":"1"}],"publication_status":"published","type":"journal_article","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J","first_name":"Jorryt J"},{"first_name":"Gabriele","full_name":"Pezzulli, Gabriele","last_name":"Pezzulli"},{"last_name":"Mackenzie","first_name":"Ruari","full_name":"Mackenzie, Ruari"},{"first_name":"Sebastiano","full_name":"Cantalupo, Sebastiano","last_name":"Cantalupo"},{"full_name":"Kusakabe, Haruka","first_name":"Haruka","last_name":"Kusakabe"},{"first_name":"Floriane","full_name":"Leclercq, Floriane","last_name":"Leclercq"},{"last_name":"Sobral","first_name":"David","full_name":"Sobral, David"},{"first_name":"Johan","full_name":"Richard, Johan","last_name":"Richard"},{"last_name":"Wisotzki","full_name":"Wisotzki, Lutz","first_name":"Lutz"},{"last_name":"Lilly","full_name":"Lilly, Simon","first_name":"Simon"},{"last_name":"Boogaard","full_name":"Boogaard, Leindert","first_name":"Leindert"},{"full_name":"Marino, Raffaella","first_name":"Raffaella","last_name":"Marino"},{"last_name":"Maseda","first_name":"Michael","full_name":"Maseda, Michael"},{"last_name":"Nanayakkara","first_name":"Themiya","full_name":"Nanayakkara, Themiya"}],"day":"01","title":"The nature of CR7 revealed with MUSE: A young starburst powering extended Ly α emission at z = 6.6","citation":{"ama":"Matthee JJ, Pezzulli G, Mackenzie R, et al. The nature of CR7 revealed with MUSE: A young starburst powering extended Ly α emission at z = 6.6. Monthly Notices of the Royal Astronomical Society. 2020;498(2):3043-3059. doi:10.1093/mnras/staa2550","apa":"Matthee, J. J., Pezzulli, G., Mackenzie, R., Cantalupo, S., Kusakabe, H., Leclercq, F., … Nanayakkara, T. (2020). The nature of CR7 revealed with MUSE: A young starburst powering extended Ly α emission at z = 6.6. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staa2550","short":"J.J. Matthee, G. Pezzulli, R. Mackenzie, S. Cantalupo, H. Kusakabe, F. Leclercq, D. Sobral, J. Richard, L. Wisotzki, S. Lilly, L. Boogaard, R. Marino, M. Maseda, T. Nanayakkara, Monthly Notices of the Royal Astronomical Society 498 (2020) 3043–3059.","mla":"Matthee, Jorryt J., et al. “The Nature of CR7 Revealed with MUSE: A Young Starburst Powering Extended Ly α Emission at z = 6.6.” Monthly Notices of the Royal Astronomical Society, vol. 498, no. 2, Oxford University Press, 2020, pp. 3043–59, doi:10.1093/mnras/staa2550.","chicago":"Matthee, Jorryt J, Gabriele Pezzulli, Ruari Mackenzie, Sebastiano Cantalupo, Haruka Kusakabe, Floriane Leclercq, David Sobral, et al. “The Nature of CR7 Revealed with MUSE: A Young Starburst Powering Extended Ly α Emission at z = 6.6.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2020. https://doi.org/10.1093/mnras/staa2550.","ista":"Matthee JJ, Pezzulli G, Mackenzie R, Cantalupo S, Kusakabe H, Leclercq F, Sobral D, Richard J, Wisotzki L, Lilly S, Boogaard L, Marino R, Maseda M, Nanayakkara T. 2020. The nature of CR7 revealed with MUSE: A young starburst powering extended Ly α emission at z = 6.6. Monthly Notices of the Royal Astronomical Society. 498(2), 3043–3059.","ieee":"J. J. Matthee et al., “The nature of CR7 revealed with MUSE: A young starburst powering extended Ly α emission at z = 6.6,” Monthly Notices of the Royal Astronomical Society, vol. 498, no. 2. Oxford University Press, pp. 3043–3059, 2020."},"doi":"10.1093/mnras/staa2550","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","dark ages","reionization","first stars","cosmology: observations"],"language":[{"iso":"eng"}],"date_created":"2022-07-07T10:36:01Z","month":"10","extern":"1","page":"3043-3059","status":"public","intvolume":" 498","publication":"Monthly Notices of the Royal Astronomical Society","quality_controlled":"1","publisher":"Oxford University Press"},{"article_type":"original","year":"2020","oa_version":"Preprint","date_updated":"2022-08-18T11:17:47Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","scopus_import":"1","external_id":{"arxiv":["2005.01732"]},"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"arxiv":1,"issue":"2","article_processing_charge":"No","date_published":"2020-06-01T00:00:00Z","_id":"11530","abstract":[{"lang":"eng","text":"A prediction of the classic active galactic nucleus (AGN) unification model is the presence of ionization cones with different orientations depending on the AGN type. Confirmations of this model exist for present times, but it is less clear in the early Universe. Here, we use the morphology of giant Ly α nebulae around AGNs at redshift z ∼ 3 to probe AGN emission and therefore the validity of the AGN unification model at this redshift. We compare the spatial morphology of 19 nebulae previously found around type I AGNs with a new sample of four Ly α nebulae detected around type II AGNs. Using two independent techniques, we find that nebulae around type II AGNs are more asymmetric than around type I, at least at radial distances r > 30 physical kpc (pkpc) from the ionizing source. We conclude that the type I and type II AGNs in our sample show evidence of different surrounding ionizing geometries. This suggests that the classical AGN unification model is also valid for high-redshift sources. Finally, we discuss how the lack of asymmetry in the inner parts (r ≲ 30 pkpc) and the associated high values of the He II to Ly α ratios in these regions could indicate additional sources of (hard) ionizing radiation originating within or in proximity of the AGN host galaxies. This work demonstrates that the morphologies of giant Ly α nebulae can be used to understand and study the geometry of high-redshift AGNs on circumnuclear scales and it lays the foundation for future studies using much larger statistical samples."}],"publication_status":"published","main_file_link":[{"url":"https://arxiv.org/abs/2005.01732","open_access":"1"}],"oa":1,"volume":495,"citation":{"chicago":"den Brok, J S, S Cantalupo, R Mackenzie, R A Marino, G Pezzulli, Jorryt J Matthee, S D Johnson, M Krumpe, T Urrutia, and W Kollatschny. “Probing the AGN Unification Model at Redshift z ∼ 3 with MUSE Observations of Giant Lyα Nebulae.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2020. https://doi.org/10.1093/mnras/staa1269.","ista":"den Brok JS, Cantalupo S, Mackenzie R, Marino RA, Pezzulli G, Matthee JJ, Johnson SD, Krumpe M, Urrutia T, Kollatschny W. 2020. Probing the AGN unification model at redshift z ∼ 3 with MUSE observations of giant Lyα nebulae. Monthly Notices of the Royal Astronomical Society. 495(2), 1874–1887.","ieee":"J. S. den Brok et al., “Probing the AGN unification model at redshift z ∼ 3 with MUSE observations of giant Lyα nebulae,” Monthly Notices of the Royal Astronomical Society, vol. 495, no. 2. Oxford University Press, pp. 1874–1887, 2020.","mla":"den Brok, J. S., et al. “Probing the AGN Unification Model at Redshift z ∼ 3 with MUSE Observations of Giant Lyα Nebulae.” Monthly Notices of the Royal Astronomical Society, vol. 495, no. 2, Oxford University Press, 2020, pp. 1874–87, doi:10.1093/mnras/staa1269.","short":"J.S. den Brok, S. Cantalupo, R. Mackenzie, R.A. Marino, G. Pezzulli, J.J. Matthee, S.D. Johnson, M. Krumpe, T. Urrutia, W. Kollatschny, Monthly Notices of the Royal Astronomical Society 495 (2020) 1874–1887.","ama":"den Brok JS, Cantalupo S, Mackenzie R, et al. Probing the AGN unification model at redshift z ∼ 3 with MUSE observations of giant Lyα nebulae. Monthly Notices of the Royal Astronomical Society. 2020;495(2):1874-1887. doi:10.1093/mnras/staa1269","apa":"den Brok, J. S., Cantalupo, S., Mackenzie, R., Marino, R. A., Pezzulli, G., Matthee, J. J., … Kollatschny, W. (2020). Probing the AGN unification model at redshift z ∼ 3 with MUSE observations of giant Lyα nebulae. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staa1269"},"title":"Probing the AGN unification model at redshift z ∼ 3 with MUSE observations of giant Lyα nebulae","day":"01","author":[{"last_name":"den Brok","full_name":"den Brok, J S","first_name":"J S"},{"last_name":"Cantalupo","first_name":"S","full_name":"Cantalupo, S"},{"last_name":"Mackenzie","first_name":"R","full_name":"Mackenzie, R"},{"last_name":"Marino","full_name":"Marino, R A","first_name":"R A"},{"last_name":"Pezzulli","first_name":"G","full_name":"Pezzulli, G"},{"first_name":"Jorryt J","full_name":"Matthee, Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X"},{"last_name":"Johnson","full_name":"Johnson, S D","first_name":"S D"},{"last_name":"Krumpe","full_name":"Krumpe, M","first_name":"M"},{"last_name":"Urrutia","first_name":"T","full_name":"Urrutia, T"},{"first_name":"W","full_name":"Kollatschny, W","last_name":"Kollatschny"}],"type":"journal_article","acknowledgement":"SC and GP gratefully acknowledge support from Swiss National Science Foundation grant PP00P2 163824. MK acknowledges support by DLR500R1904.","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: active","galaxies: high-redshift","intergalactic medium","quasars: emission lines","quasars: general"],"doi":"10.1093/mnras/staa1269","page":"1874-1887","extern":"1","month":"06","date_created":"2022-07-07T10:40:17Z","publisher":"Oxford University Press","quality_controlled":"1","publication":"Monthly Notices of the Royal Astronomical Society","status":"public","intvolume":" 495"},{"volume":493,"main_file_link":[{"url":"https://doi.org/10.1093/mnras/staa622","open_access":"1"}],"oa":1,"publication_status":"published","abstract":[{"lang":"eng","text":"While low-luminosity galaxies dominate number counts at all redshifts, their contribution to cosmic reionization is poorly understood due to a lack of knowledge of their physical properties. We isolate a sample of 35 z ≈ 4–5 continuum-faint Lyman-α emitters from deep VLT/MUSE spectroscopy and directly measure their H α emission using stacked Spitzer/IRAC Ch. 1 photometry. Based on Hubble Space Telescope imaging, we determine that the average UV continuum magnitude is fainter than −16 (≈ 0.01 L⋆), implying a median Lyman-α equivalent width of 259 Å. By combining the H α measurement with the UV magnitude, we determine the ionizing photon production efficiency, ξion, a first for such faint galaxies. The measurement of log10 (ξion [Hz erg−1]) = 26.28 (+0.28−0.40) is in excess of literature measurements of both continuum- and emission line-selected samples, implying a more efficient production of ionizing photons in these lower luminosity, Lyman-α-selected systems. We conclude that this elevated efficiency can be explained by stellar populations with metallicities between 4 × 10−4 and 0.008, with light-weighted ages less than 3 Myr."}],"_id":"11531","date_published":"2020-04-01T00:00:00Z","issue":"4","article_processing_charge":"No","arxiv":1,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2022-08-18T11:23:27Z","external_id":{"arxiv":["2002.11117"]},"scopus_import":"1","oa_version":"Published Version","year":"2020","article_type":"original","status":"public","intvolume":" 493","quality_controlled":"1","publication":"Monthly Notices of the Royal Astronomical Society","publisher":"Oxford University Press","date_created":"2022-07-07T10:46:41Z","extern":"1","month":"04","page":"5120-5130","doi":"10.1093/mnras/staa622","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","Galaxies: evolution","Galaxies: high-redshift","Galaxies: ISM"],"acknowledgement":"We would like to thank the anonymous referee for a thoughtful report and suggestions that have improved this manuscript. We are also grateful to everyone involved in the Spitzer Space Telescope mission and everyone at the Spitzer Science Center: we are truly fortunate to have been able to use data from this facility. J. B. acknowledges support by FCT/MCTES through national funds by this grant UID/FIS/04434/2019 and through the Investigador FCT contract no. IF/01654/2014/CP1215/CT0003. S. C. gratefully acknowledges support from Swiss National Science Foundation grant PP00P2 163824. We would also like to thank Mauro Stefanon for his assistance with de-blending the IRAC photometry, Pieter van Dokkum for a number of useful suggestions, and Daniel Schaerer for information regarding the stellar population models. This study is based on observations made with ESO telescopes at the La Silla Paranal Observatory under programs IDs 094.A-2089(B), 095.A0010(A), 096.A-0045(A), and 096.A-0045(B).","type":"journal_article","author":[{"first_name":"Michael V","full_name":"Maseda, Michael V","last_name":"Maseda"},{"full_name":"Bacon, Roland","first_name":"Roland","last_name":"Bacon"},{"last_name":"Lam","full_name":"Lam, Daniel","first_name":"Daniel"},{"last_name":"Matthee","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Brinchmann","first_name":"Jarle","full_name":"Brinchmann, Jarle"},{"first_name":"Joop","full_name":"Schaye, Joop","last_name":"Schaye"},{"last_name":"Labbe","full_name":"Labbe, Ivo","first_name":"Ivo"},{"last_name":"Schmidt","full_name":"Schmidt, Kasper B","first_name":"Kasper B"},{"full_name":"Boogaard, Leindert","first_name":"Leindert","last_name":"Boogaard"},{"first_name":"Rychard","full_name":"Bouwens, Rychard","last_name":"Bouwens"},{"last_name":"Cantalupo","first_name":"Sebastiano","full_name":"Cantalupo, Sebastiano"},{"last_name":"Franx","first_name":"Marijn","full_name":"Franx, Marijn"},{"last_name":"Hashimoto","full_name":"Hashimoto, Takuya","first_name":"Takuya"},{"first_name":"Hanae","full_name":"Inami, Hanae","last_name":"Inami"},{"last_name":"Kusakabe","first_name":"Haruka","full_name":"Kusakabe, Haruka"},{"first_name":"Guillaume","full_name":"Mahler, Guillaume","last_name":"Mahler"},{"last_name":"Nanayakkara","first_name":"Themiya","full_name":"Nanayakkara, Themiya"},{"last_name":"Richard","first_name":"Johan","full_name":"Richard, Johan"},{"last_name":"Wisotzki","first_name":"Lutz","full_name":"Wisotzki, Lutz"}],"day":"01","title":"Elevated ionizing photon production efficiency in faint high-equivalent-width Lyman-α emitters","citation":{"mla":"Maseda, Michael V., et al. “Elevated Ionizing Photon Production Efficiency in Faint High-Equivalent-Width Lyman-α Emitters.” Monthly Notices of the Royal Astronomical Society, vol. 493, no. 4, Oxford University Press, 2020, pp. 5120–30, doi:10.1093/mnras/staa622.","chicago":"Maseda, Michael V, Roland Bacon, Daniel Lam, Jorryt J Matthee, Jarle Brinchmann, Joop Schaye, Ivo Labbe, et al. “Elevated Ionizing Photon Production Efficiency in Faint High-Equivalent-Width Lyman-α Emitters.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2020. https://doi.org/10.1093/mnras/staa622.","ieee":"M. V. Maseda et al., “Elevated ionizing photon production efficiency in faint high-equivalent-width Lyman-α emitters,” Monthly Notices of the Royal Astronomical Society, vol. 493, no. 4. Oxford University Press, pp. 5120–5130, 2020.","ista":"Maseda MV, Bacon R, Lam D, Matthee JJ, Brinchmann J, Schaye J, Labbe I, Schmidt KB, Boogaard L, Bouwens R, Cantalupo S, Franx M, Hashimoto T, Inami H, Kusakabe H, Mahler G, Nanayakkara T, Richard J, Wisotzki L. 2020. Elevated ionizing photon production efficiency in faint high-equivalent-width Lyman-α emitters. Monthly Notices of the Royal Astronomical Society. 493(4), 5120–5130.","ama":"Maseda MV, Bacon R, Lam D, et al. Elevated ionizing photon production efficiency in faint high-equivalent-width Lyman-α emitters. Monthly Notices of the Royal Astronomical Society. 2020;493(4):5120-5130. doi:10.1093/mnras/staa622","apa":"Maseda, M. V., Bacon, R., Lam, D., Matthee, J. J., Brinchmann, J., Schaye, J., … Wisotzki, L. (2020). Elevated ionizing photon production efficiency in faint high-equivalent-width Lyman-α emitters. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staa622","short":"M.V. Maseda, R. Bacon, D. Lam, J.J. Matthee, J. Brinchmann, J. Schaye, I. Labbe, K.B. Schmidt, L. Boogaard, R. Bouwens, S. Cantalupo, M. Franx, T. Hashimoto, H. Inami, H. Kusakabe, G. Mahler, T. Nanayakkara, J. Richard, L. Wisotzki, Monthly Notices of the Royal Astronomical Society 493 (2020) 5120–5130."}},{"doi":"10.1093/mnras/staa093","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: formation","galaxies: high-redshift","galaxies: star formation"],"acknowledgement":"We thank the anonymous referee for the valuable feedback that significantly improved the quality and clarity of this paper. SS and JC acknowledge studentships from Lancaster University. APA acknowledges support from Fundação para a Ciência e a Tecnologia through the project PTDC/FISAST/31546/2017. The authors would like to thank Ali Khostovan, Sara Perez Sanchez, Alex Bennett and Tom Rose for contributions and discussions in the early stages of this work. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by CALET and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. Finally, the authors acknowledge the unique value of the publicly available analysis software TOPCAT (Taylor 2005) and publicly available programming language Python, including the numpy, pyfits, matplotlib, scipy and astropy (Astropy Collaboration et al. 2013) packages. This work is based on the public SC4K sample of LAEs (Sobral et al. 2018a) and we release the full catalogue with all the photometry and properties derived in this paper, in electronic format, along with the relevant tables.","type":"journal_article","author":[{"full_name":"Santos, S","first_name":"S","last_name":"Santos"},{"last_name":"Sobral","first_name":"D","full_name":"Sobral, D"},{"last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X"},{"last_name":"Calhau","first_name":"J","full_name":"Calhau, J"},{"full_name":"da Cunha, E","first_name":"E","last_name":"da Cunha"},{"full_name":"Ribeiro, B","first_name":"B","last_name":"Ribeiro"},{"last_name":"Paulino-Afonso","first_name":"A","full_name":"Paulino-Afonso, A"},{"full_name":"Arrabal Haro, P","first_name":"P","last_name":"Arrabal Haro"},{"full_name":"Butterworth, J","first_name":"J","last_name":"Butterworth"}],"day":"01","title":"The evolution of rest-frame UV properties, Ly α EWs, and the SFR–stellar mass relation at z ∼ 2–6 for SC4K LAEs","citation":{"ama":"Santos S, Sobral D, Matthee JJ, et al. The evolution of rest-frame UV properties, Ly α EWs, and the SFR–stellar mass relation at z ∼ 2–6 for SC4K LAEs. Monthly Notices of the Royal Astronomical Society. 2020;493(1):141-160. doi:10.1093/mnras/staa093","apa":"Santos, S., Sobral, D., Matthee, J. J., Calhau, J., da Cunha, E., Ribeiro, B., … Butterworth, J. (2020). The evolution of rest-frame UV properties, Ly α EWs, and the SFR–stellar mass relation at z ∼ 2–6 for SC4K LAEs. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staa093","short":"S. Santos, D. Sobral, J.J. Matthee, J. Calhau, E. da Cunha, B. Ribeiro, A. Paulino-Afonso, P. Arrabal Haro, J. Butterworth, Monthly Notices of the Royal Astronomical Society 493 (2020) 141–160.","mla":"Santos, S., et al. “The Evolution of Rest-Frame UV Properties, Ly α EWs, and the SFR–Stellar Mass Relation at z ∼ 2–6 for SC4K LAEs.” Monthly Notices of the Royal Astronomical Society, vol. 493, no. 1, Oxford University Press, 2020, pp. 141–60, doi:10.1093/mnras/staa093.","chicago":"Santos, S, D Sobral, Jorryt J Matthee, J Calhau, E da Cunha, B Ribeiro, A Paulino-Afonso, P Arrabal Haro, and J Butterworth. “The Evolution of Rest-Frame UV Properties, Ly α EWs, and the SFR–Stellar Mass Relation at z ∼ 2–6 for SC4K LAEs.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2020. https://doi.org/10.1093/mnras/staa093.","ieee":"S. Santos et al., “The evolution of rest-frame UV properties, Ly α EWs, and the SFR–stellar mass relation at z ∼ 2–6 for SC4K LAEs,” Monthly Notices of the Royal Astronomical Society, vol. 493, no. 1. Oxford University Press, pp. 141–160, 2020.","ista":"Santos S, Sobral D, Matthee JJ, Calhau J, da Cunha E, Ribeiro B, Paulino-Afonso A, Arrabal Haro P, Butterworth J. 2020. The evolution of rest-frame UV properties, Ly α EWs, and the SFR–stellar mass relation at z ∼ 2–6 for SC4K LAEs. Monthly Notices of the Royal Astronomical Society. 493(1), 141–160."},"status":"public","intvolume":" 493","quality_controlled":"1","publication":"Monthly Notices of the Royal Astronomical Society","publisher":"Oxford University Press","date_created":"2022-07-07T12:05:23Z","extern":"1","month":"03","page":"141-160","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2022-08-18T11:27:43Z","external_id":{"arxiv":["1910.02959"]},"scopus_import":"1","oa_version":"Preprint","year":"2020","article_type":"original","volume":493,"oa":1,"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1910.02959"}],"publication_status":"published","_id":"11533","date_published":"2020-03-01T00:00:00Z","abstract":[{"text":"We explore deep rest-frame UV to FIR data in the COSMOS field to measure the individual spectral energy distributions (SED) of the ∼4000 SC4K (Sobral et al.) Lyman α (Ly α) emitters (LAEs) at z ∼ 2–6. We find typical stellar masses of 109.3 ± 0.6 M⊙ and star formation rates (SFR) of SFRSED=4.4+10.5−2.4 M⊙ yr−1 and SFRLyα=5.9+6.3−2.6 M⊙ yr−1, combined with very blue UV slopes of β=−2.1+0.5−0.4, but with significant variations within the population. MUV and β are correlated in a similar way to UV-selected sources, but LAEs are consistently bluer. This suggests that LAEs are the youngest and/or most dust-poor subset of the UV-selected population. We also study the Ly α rest-frame equivalent width (EW0) and find 45 ‘extreme’ LAEs with EW0 > 240 Å (3σ), implying a low number density of (7 ± 1) × 10−7 Mpc−3. Overall, we measure little to no evolution of the Ly α EW0 and scale length parameter (w0), which are consistently high (EW0=140+280−70 Å, w0=129+11−11 Å) from z ∼ 6 to z ∼ 2 and below. However, w0 is anticorrelated with MUV and stellar mass. Our results imply that sources selected as LAEs have a high Ly α escape fraction (fesc,Ly α) irrespective of cosmic time, but fesc,Ly α is still higher for UV-fainter and lower mass LAEs. The least massive LAEs (<109.5 M⊙) are typically located above the star formation ‘main sequence’ (MS), but the offset from the MS decreases towards z ∼ 6 and towards 1010 M⊙. Our results imply a lack of evolution in the properties of LAEs across time and reveals the increasing overlap in properties of LAEs and UV-continuum selected galaxies as typical star-forming galaxies at high redshift effectively become LAEs.","lang":"eng"}],"issue":"1","article_processing_charge":"No","arxiv":1},{"article_type":"original","oa_version":"Preprint","year":"2020","date_updated":"2022-08-18T11:29:53Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","scopus_import":"1","external_id":{"arxiv":["1909.06376"]},"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"date_published":"2020-02-01T00:00:00Z","_id":"11534","abstract":[{"text":"The observed properties of the Lyman-α (Ly α) emission line are a powerful probe of neutral gas in and around galaxies. We present spatially resolved Ly α spectroscopy with VLT/MUSE targeting VR7, a UV-luminous galaxy at z = 6.532 with moderate Ly α equivalent width (EW0 ≈ 38 Å). These data are combined with deep resolved [CII]158μm spectroscopy obtained with ALMA and UV imaging from HST and we also detect UV continuum with MUSE. Ly α emission is clearly detected with S/N ≈ 40 and FWHM of 374 km s−1. Ly α and [C II] are similarly extended beyond the UV, with effective radius reff = 2.1 ± 0.2 kpc for a single exponential model or reff,Lyα,halo=3.45+1.08−0.87 kpc when measured jointly with the UV continuum. The Ly α profile is broader and redshifted with respect to the [C II] line (by 213 km s−1), but there are spatial variations that are qualitatively similar in both lines and coincide with resolved UV components. This suggests that the emission originates from two components with plausibly different H I column densities. We place VR7 in the context of other galaxies at similar and lower redshift. The Ly α halo scale length is similar at different redshifts and velocity shifts with respect to the systemic are typically smaller. Overall, we find little indications of a more neutral vicinity at higher redshift. This means that the local (∼10 kpc) neutral gas conditions that determine the observed Ly α properties in VR7 resemble the conditions in post-reionization galaxies.","lang":"eng"}],"arxiv":1,"issue":"2","article_processing_charge":"No","volume":492,"publication_status":"published","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1909.06376"}],"oa":1,"day":"01","author":[{"orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","last_name":"Matthee"},{"last_name":"Sobral","full_name":"Sobral, David","first_name":"David"},{"last_name":"Gronke","first_name":"Max","full_name":"Gronke, Max"},{"last_name":"Pezzulli","first_name":"Gabriele","full_name":"Pezzulli, Gabriele"},{"full_name":"Cantalupo, Sebastiano","first_name":"Sebastiano","last_name":"Cantalupo"},{"last_name":"Röttgering","first_name":"Huub","full_name":"Röttgering, Huub"},{"last_name":"Darvish","full_name":"Darvish, Behnam","first_name":"Behnam"},{"last_name":"Santos","full_name":"Santos, Sérgio","first_name":"Sérgio"}],"type":"journal_article","citation":{"mla":"Matthee, Jorryt J., et al. “Resolved Lyman-α Properties of a Luminous Lyman-Break Galaxy in a Large Ionized Bubble at z = 6.53 .” Monthly Notices of the Royal Astronomical Society, vol. 492, no. 2, Oxford University Press, 2020, pp. 1778–90, doi:10.1093/mnras/stz3554.","chicago":"Matthee, Jorryt J, David Sobral, Max Gronke, Gabriele Pezzulli, Sebastiano Cantalupo, Huub Röttgering, Behnam Darvish, and Sérgio Santos. “Resolved Lyman-α Properties of a Luminous Lyman-Break Galaxy in a Large Ionized Bubble at z = 6.53 .” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2020. https://doi.org/10.1093/mnras/stz3554.","ieee":"J. J. Matthee et al., “Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 ,” Monthly Notices of the Royal Astronomical Society, vol. 492, no. 2. Oxford University Press, pp. 1778–1790, 2020.","ista":"Matthee JJ, Sobral D, Gronke M, Pezzulli G, Cantalupo S, Röttgering H, Darvish B, Santos S. 2020. Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 . Monthly Notices of the Royal Astronomical Society. 492(2), 1778–1790.","ama":"Matthee JJ, Sobral D, Gronke M, et al. Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 . Monthly Notices of the Royal Astronomical Society. 2020;492(2):1778-1790. doi:10.1093/mnras/stz3554","apa":"Matthee, J. J., Sobral, D., Gronke, M., Pezzulli, G., Cantalupo, S., Röttgering, H., … Santos, S. (2020). Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 . Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stz3554","short":"J.J. Matthee, D. Sobral, M. Gronke, G. Pezzulli, S. Cantalupo, H. Röttgering, B. Darvish, S. Santos, Monthly Notices of the Royal Astronomical Society 492 (2020) 1778–1790."},"title":"Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 ","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","dark ages","reionization","first stars","cosmology: observations"],"doi":"10.1093/mnras/stz3554","acknowledgement":"We thank the referee for their suggestions and constructive comments that helped to improve the presentation of our results. Based on observations obtained with the Very Large Telescope, program 99.A-0462. Based on observations made with the NASA/ESA Hubble Space Telescope, obtained 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 program #14699. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2017.1.01451.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. MG acknowledges support from NASA grant NNX17AK58G. GP and SC gratefully acknowledge support from Swiss National Science Foundation grant PP00P2 163824. BD acknowledges financial support from the National Science Foundation, grant number 1716907. We have benefited greatly from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, SCIPY (Jones et al. 2001; Hunter 2007; van der Walt, Colbert & Varoquaux 2011) and ASTROPY (Astropy Collaboration 2013) packages, the astronomical imaging tools SEXTRACTOR, SWARP, and SCAMP (Bertin & Arnouts 1996; Bertin 2006, 2010) and the TOPCAT analysis tool (Taylor 2013).","extern":"1","month":"02","date_created":"2022-07-07T12:21:36Z","page":"1778-1790","quality_controlled":"1","publication":"Monthly Notices of the Royal Astronomical Society","intvolume":" 492","status":"public","publisher":"Oxford University Press"},{"date_updated":"2022-08-18T11:25:31Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","scopus_import":"1","external_id":{"arxiv":["1909.11672"]},"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"article_type":"original","year":"2020","oa_version":"Preprint","volume":493,"publication_status":"published","oa":1,"main_file_link":[{"url":"https://arxiv.org/abs/1909.11672","open_access":"1"}],"date_published":"2020-04-01T00:00:00Z","_id":"11539","abstract":[{"lang":"eng","text":"Despite recent progress in understanding Ly α emitters (LAEs), relatively little is known regarding their typical black hole activity across cosmic time. Here, we study the X-ray and radio properties of ∼4000 LAEs at 2.2 < z < 6 from the SC4K survey in the COSMOS field. We detect 254 (6.8per cent±0.4per cent) LAEs individually in the X-rays (S/N > 3) with an average luminosity of 1044.31±0.01ergs−1 and average black hole accretion rate (BHAR) of 0.72±0.01 M⊙ yr−1, consistent with moderate to high accreting active galactic neuclei (AGNs). We detect 120 sources in deep radio data (radio AGN fraction of 3.2per cent±0.3per cent). The global AGN fraction (8.6per cent±0.4per cent) rises with Ly α luminosity and declines with increasing redshift. For X-ray-detected LAEs, Ly α luminosities correlate with the BHARs, suggesting that Ly α luminosity becomes a BHAR indicator. Most LAEs (93.1per cent±0.6per cent) at 2 < z < 6 have no detectable X-ray emission (BHARs < 0.017 M⊙ yr−1). The median star formation rate (SFR) of star-forming LAEs from Ly α and radio luminosities is 7.6+6.6−2.8 M⊙ yr−1. The black hole to galaxy growth ratio (BHAR/SFR) for LAEs is <0.0022, consistent with typical star-forming galaxies and the local BHAR/SFR relation. We conclude that LAEs at 2 < z < 6 include two different populations: an AGN population, where Ly α luminosity traces BHAR, and another with low SFRs which remain undetected in even the deepest X-ray stacks but is detected in the radio stacks."}],"arxiv":1,"issue":"3","article_processing_charge":"No","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: active","galaxies: evolution","galaxies: high-redshift","quasars: supermassive black holes","galaxies: star formation","cosmology: observations","X-rays: galaxies"],"doi":"10.1093/mnras/staa476","acknowledgement":"JM acknowledges the support of a Huygens PhD fellowship from Leiden University. We thank Camila Correa for help analysing snipshot merger trees. We thank the anonymous referee for constructive comments. We also thank Jarle Brinchmann, Rob Crain, Antonios Katsianis, Paola Popesso, and David Sobral for discussions and suggestions. We also thank the participants of the Lorentz Center workshop ‘A Decade of the Star-Forming Main Sequence’ held on 2017 September 4–8, for discussions and ideas. We have benefited from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, and SCIPY (Hunter 2007) packages and the TOPCAT analysis tool (Taylor 2013).","day":"01","type":"journal_article","author":[{"full_name":"Calhau, João","first_name":"João","last_name":"Calhau"},{"last_name":"Sobral","full_name":"Sobral, David","first_name":"David"},{"last_name":"Santos","full_name":"Santos, Sérgio","first_name":"Sérgio"},{"last_name":"Matthee","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Paulino-Afonso","first_name":"Ana","full_name":"Paulino-Afonso, Ana"},{"last_name":"Stroe","full_name":"Stroe, Andra","first_name":"Andra"},{"full_name":"Simmons, Brooke","first_name":"Brooke","last_name":"Simmons"},{"full_name":"Barlow-Hall, Cassandra","first_name":"Cassandra","last_name":"Barlow-Hall"},{"first_name":"Benjamin","full_name":"Adams, Benjamin","last_name":"Adams"}],"citation":{"mla":"Calhau, João, et al. “The X-Ray and Radio Activity of Typical and Luminous Ly α Emitters from z ∼ 2 to z ∼ 6: Evidence for a Diverse, Evolving Population.” Monthly Notices of the Royal Astronomical Society, vol. 493, no. 3, Oxford University Press, 2020, pp. 3341–62, doi:10.1093/mnras/staa476.","chicago":"Calhau, João, David Sobral, Sérgio Santos, Jorryt J Matthee, Ana Paulino-Afonso, Andra Stroe, Brooke Simmons, Cassandra Barlow-Hall, and Benjamin Adams. “The X-Ray and Radio Activity of Typical and Luminous Ly α Emitters from z ∼ 2 to z ∼ 6: Evidence for a Diverse, Evolving Population.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2020. https://doi.org/10.1093/mnras/staa476.","ista":"Calhau J, Sobral D, Santos S, Matthee JJ, Paulino-Afonso A, Stroe A, Simmons B, Barlow-Hall C, Adams B. 2020. The X-ray and radio activity of typical and luminous Ly α emitters from z ∼ 2 to z ∼ 6: Evidence for a diverse, evolving population. Monthly Notices of the Royal Astronomical Society. 493(3), 3341–3362.","ieee":"J. Calhau et al., “The X-ray and radio activity of typical and luminous Ly α emitters from z ∼ 2 to z ∼ 6: Evidence for a diverse, evolving population,” Monthly Notices of the Royal Astronomical Society, vol. 493, no. 3. Oxford University Press, pp. 3341–3362, 2020.","ama":"Calhau J, Sobral D, Santos S, et al. The X-ray and radio activity of typical and luminous Ly α emitters from z ∼ 2 to z ∼ 6: Evidence for a diverse, evolving population. Monthly Notices of the Royal Astronomical Society. 2020;493(3):3341-3362. doi:10.1093/mnras/staa476","apa":"Calhau, J., Sobral, D., Santos, S., Matthee, J. J., Paulino-Afonso, A., Stroe, A., … Adams, B. (2020). The X-ray and radio activity of typical and luminous Ly α emitters from z ∼ 2 to z ∼ 6: Evidence for a diverse, evolving population. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staa476","short":"J. Calhau, D. Sobral, S. Santos, J.J. Matthee, A. Paulino-Afonso, A. Stroe, B. Simmons, C. Barlow-Hall, B. Adams, Monthly Notices of the Royal Astronomical Society 493 (2020) 3341–3362."},"title":"The X-ray and radio activity of typical and luminous Ly α emitters from z ∼ 2 to z ∼ 6: Evidence for a diverse, evolving population","quality_controlled":"1","publication":"Monthly Notices of the Royal Astronomical Society","status":"public","intvolume":" 493","publisher":"Oxford University Press","extern":"1","month":"04","date_created":"2022-07-08T07:34:10Z","page":"3341-3362"},{"language":[{"iso":"eng"}],"keyword":["Astronomy and Astrophysics","Space and Planetary Science","galaxies: formation","galaxies: evolution","galaxies: high-redshift"],"doi":"10.1017/s1743921319009451","citation":{"mla":"Matthee, Jorryt J., and David Sobral. “Unveiling the Most Luminous Lyman-α Emitters in the Epoch of Reionisation.” Proceedings of the International Astronomical Union, vol. 15, no. S352, Cambridge University Press, 2020, pp. 21–25, doi:10.1017/s1743921319009451.","ista":"Matthee JJ, Sobral D. 2020. Unveiling the most luminous Lyman-α emitters in the epoch of reionisation. Proceedings of the International Astronomical Union. vol. 15, 21–25.","ieee":"J. J. Matthee and D. Sobral, “Unveiling the most luminous Lyman-α emitters in the epoch of reionisation,” in Proceedings of the International Astronomical Union, 2020, vol. 15, no. S352, pp. 21–25.","chicago":"Matthee, Jorryt J, and David Sobral. “Unveiling the Most Luminous Lyman-α Emitters in the Epoch of Reionisation.” In Proceedings of the International Astronomical Union, 15:21–25. Cambridge University Press, 2020. https://doi.org/10.1017/s1743921319009451.","apa":"Matthee, J. J., & Sobral, D. (2020). Unveiling the most luminous Lyman-α emitters in the epoch of reionisation. In Proceedings of the International Astronomical Union (Vol. 15, pp. 21–25). Cambridge University Press. https://doi.org/10.1017/s1743921319009451","ama":"Matthee JJ, Sobral D. Unveiling the most luminous Lyman-α emitters in the epoch of reionisation. In: Proceedings of the International Astronomical Union. Vol 15. Cambridge University Press; 2020:21-25. doi:10.1017/s1743921319009451","short":"J.J. Matthee, D. Sobral, in:, Proceedings of the International Astronomical Union, Cambridge University Press, 2020, pp. 21–25."},"title":"Unveiling the most luminous Lyman-α emitters in the epoch of reionisation","day":"04","type":"conference","author":[{"last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X"},{"last_name":"Sobral","first_name":"David","full_name":"Sobral, David"}],"publisher":"Cambridge University Press","quality_controlled":"1","publication":"Proceedings of the International Astronomical Union","status":"public","intvolume":" 15","page":"21-25","extern":"1","month":"06","date_created":"2022-07-14T14:08:41Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2022-08-19T08:41:12Z","scopus_import":"1","external_id":{"arxiv":["1911.04774"]},"publication_identifier":{"eissn":["1743-9221"],"issn":["1743-9213"]},"year":"2020","oa_version":"Preprint","publication_status":"published","main_file_link":[{"url":"https://arxiv.org/abs/1911.04774","open_access":"1"}],"oa":1,"volume":15,"arxiv":1,"issue":"S352","article_processing_charge":"No","abstract":[{"text":"Distant luminous Lyman-α emitters are excellent targets for detailed observations of galaxies in the epoch of reionisation. Spatially resolved observations of these galaxies allow us to simultaneously probe the emission from young stars, partially ionised gas in the interstellar medium and to constrain the properties of the surrounding hydrogen in the circumgalactic medium. We review recent results from (spectroscopic) follow-up studies of the rest-frame UV, Lyman-α and [CII] emission in luminous galaxies observed ∼500 Myr after the Big Bang with ALMA, HST/WFC3 and VLT/X-SHOOTER. These galaxies likely reside in early ionised bubbles and are complex systems, consisting of multiple well separated and resolved components where traces of metals are already present.","lang":"eng"}],"_id":"11586","date_published":"2020-06-04T00:00:00Z"},{"title":"The K2 galactic archaeology program data release 2: Asteroseismic results from campaigns 4, 6, and 7","citation":{"chicago":"Zinn, Joel C., Dennis Stello, Yvonne Elsworth, Rafael A. García, Thomas Kallinger, Savita Mathur, Benoît Mosser, et al. “The K2 Galactic Archaeology Program Data Release 2: Asteroseismic Results from Campaigns 4, 6, and 7.” The Astrophysical Journal Supplement Series. IOP Publishing, 2020. https://doi.org/10.3847/1538-4365/abbee3.","ieee":"J. C. Zinn et al., “The K2 galactic archaeology program data release 2: Asteroseismic results from campaigns 4, 6, and 7,” The Astrophysical Journal Supplement Series, vol. 251, no. 2. IOP Publishing, 2020.","ista":"Zinn JC, Stello D, Elsworth Y, García RA, Kallinger T, Mathur S, Mosser B, Bugnet LA, Jones C, Hon M, Sharma S, Schönrich R, Warfield JT, Luger R, Pinsonneault MH, Johnson JA, Huber D, Aguirre VS, Chaplin WJ, Davies GR, Miglio A. 2020. The K2 galactic archaeology program data release 2: Asteroseismic results from campaigns 4, 6, and 7. The Astrophysical Journal Supplement Series. 251(2), 23.","mla":"Zinn, Joel C., et al. “The K2 Galactic Archaeology Program Data Release 2: Asteroseismic Results from Campaigns 4, 6, and 7.” The Astrophysical Journal Supplement Series, vol. 251, no. 2, 23, IOP Publishing, 2020, doi:10.3847/1538-4365/abbee3.","short":"J.C. Zinn, D. Stello, Y. Elsworth, R.A. García, T. Kallinger, S. Mathur, B. Mosser, L.A. Bugnet, C. Jones, M. Hon, S. Sharma, R. Schönrich, J.T. Warfield, R. Luger, M.H. Pinsonneault, J.A. Johnson, D. Huber, V.S. Aguirre, W.J. Chaplin, G.R. Davies, A. Miglio, The Astrophysical Journal Supplement Series 251 (2020).","ama":"Zinn JC, Stello D, Elsworth Y, et al. The K2 galactic archaeology program data release 2: Asteroseismic results from campaigns 4, 6, and 7. The Astrophysical Journal Supplement Series. 2020;251(2). doi:10.3847/1538-4365/abbee3","apa":"Zinn, J. C., Stello, D., Elsworth, Y., García, R. A., Kallinger, T., Mathur, S., … Miglio, A. (2020). The K2 galactic archaeology program data release 2: Asteroseismic results from campaigns 4, 6, and 7. The Astrophysical Journal Supplement Series. IOP Publishing. https://doi.org/10.3847/1538-4365/abbee3"},"author":[{"last_name":"Zinn","full_name":"Zinn, Joel C.","first_name":"Joel C."},{"first_name":"Dennis","full_name":"Stello, Dennis","last_name":"Stello"},{"first_name":"Yvonne","full_name":"Elsworth, Yvonne","last_name":"Elsworth"},{"last_name":"García","first_name":"Rafael A.","full_name":"García, Rafael A."},{"last_name":"Kallinger","full_name":"Kallinger, Thomas","first_name":"Thomas"},{"last_name":"Mathur","full_name":"Mathur, Savita","first_name":"Savita"},{"last_name":"Mosser","full_name":"Mosser, Benoît","first_name":"Benoît"},{"first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle","last_name":"Bugnet","id":"d9edb345-f866-11ec-9b37-d119b5234501","orcid":"0000-0003-0142-4000"},{"last_name":"Jones","full_name":"Jones, Caitlin","first_name":"Caitlin"},{"first_name":"Marc","full_name":"Hon, Marc","last_name":"Hon"},{"last_name":"Sharma","full_name":"Sharma, Sanjib","first_name":"Sanjib"},{"last_name":"Schönrich","first_name":"Ralph","full_name":"Schönrich, Ralph"},{"first_name":"Jack T.","full_name":"Warfield, Jack T.","last_name":"Warfield"},{"full_name":"Luger, Rodrigo","first_name":"Rodrigo","last_name":"Luger"},{"last_name":"Pinsonneault","full_name":"Pinsonneault, Marc H.","first_name":"Marc H."},{"first_name":"Jennifer A.","full_name":"Johnson, Jennifer A.","last_name":"Johnson"},{"first_name":"Daniel","full_name":"Huber, Daniel","last_name":"Huber"},{"last_name":"Aguirre","full_name":"Aguirre, Victor Silva","first_name":"Victor Silva"},{"last_name":"Chaplin","full_name":"Chaplin, William J.","first_name":"William J."},{"full_name":"Davies, Guy R.","first_name":"Guy R.","last_name":"Davies"},{"first_name":"Andrea","full_name":"Miglio, Andrea","last_name":"Miglio"}],"type":"journal_article","day":"01","acknowledgement":"We thank the referee for comments that strengthened the manuscript. J. C. Z. and M. H. P. acknowledge support from NASA grants 80NSSC18K0391 and NNX17AJ40G. Y. E. and C. J. acknowledge the support of the UK Science and Technology Facilities Council (STFC). S. M. would like to acknowledge support from the Spanish Ministry with the Ramon y Cajal fellowship number RYC-2015-17697. R. A. G. acknowledges funding received from the PLATO CNES grant. R. S. acknowledges funding via a Royal Society University Research Fellowship. D.H. acknowledges support from the Alfred P. Sloan Foundation and the National Aeronautics and Space Administration (80NSSC19K0108). V.S.A. acknowledges support from the Independent Research Fund Denmark (Research grant 7027-00096B), and the Carlsberg foundation (grant agreement CF19-0649). This research was supported in part by the National Science Foundation under grant No. NSF PHY-1748958.\r\n\r\nFunding for the Stellar Astrophysics Centre (SAC) is provided by The Danish National Research Foundation (grant agreement No. DNRF106).\r\n\r\nThe K2 Galactic Archaeology Program is supported by the National Aeronautics and Space Administration under grant NNX16AJ17G issued through the K2 Guest Observer Program.\r\n\r\nThis publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation.\r\n\r\nThis work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.\r\n\r\nFunding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High Performance Computing at the University of Utah. The SDSS website is www.sdss.org.\r\n\r\nSDSS-IV is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration, including the Brazilian Participation Group, the Carnegie Institution for Science, Carnegie Mellon University, the Chilean Participation Group, the French Participation Group, the Harvard–Smithsonian Center for Astrophysics, Instituto de Astrofísica de Canarias, The Johns Hopkins University, Kavli Institute for the Physics and Mathematics of the Universe (IPMU)/University of Tokyo, the Korean Participation Group, Lawrence Berkeley National Laboratory, Leibniz Institut für Astrophysik Potsdam (AIP), Max-Planck-Institut für Astronomie (MPIA Heidelberg), Max-Planck-Institut für Astrophysik (MPA Garching), Max-Planck-Institut für Extraterrestrische Physik (MPE), National Astronomical Observatories of China, New Mexico State University, New York University, University of Notre Dame, Observatário Nacional/MCTI, The Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, Universidad Nacional Autónoma de México, University of Arizona, University of Colorado Boulder, University of Oxford, University of Portsmouth, University of Utah, University of Virginia, University of Washington, University of Wisconsin, Vanderbilt University, and Yale University.\r\n\r\nSoftware: asfgrid (Sharma & Stello 2016), emcee (Foreman-Mackey et al. 2013), NumPy (Walt 2011), pandas (McKinney 2010; Reback et al. 2020), Matplotlib (Hunter 2007), IPython (Pérez & Granger 2007), SciPy (Virtanen et al. 2020).","doi":"10.3847/1538-4365/abbee3","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"date_created":"2022-07-18T13:27:26Z","extern":"1","month":"12","publisher":"IOP Publishing","status":"public","intvolume":" 251","quality_controlled":"1","publication":"The Astrophysical Journal Supplement Series","oa_version":"Preprint","year":"2020","article_type":"original","publication_identifier":{"issn":["0067-0049"],"eissn":["1538-4365"]},"date_updated":"2022-08-22T07:04:45Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","scopus_import":"1","external_id":{"arxiv":["2012.04051"]},"issue":"2","article_processing_charge":"No","arxiv":1,"_id":"11610","date_published":"2020-12-01T00:00:00Z","abstract":[{"text":"Studies of Galactic structure and evolution have benefited enormously from Gaia kinematic information, though additional, intrinsic stellar parameters like age are required to best constrain Galactic models. Asteroseismology is the most precise method of providing such information for field star populations en masse, but existing samples for the most part have been limited to a few narrow fields of view by the CoRoT and Kepler missions. In an effort to provide well-characterized stellar parameters across a wide range in Galactic position, we present the second data release of red giant asteroseismic parameters for the K2 Galactic Archaeology Program (GAP). We provide ${\\nu }_{\\max }$ and ${\\rm{\\Delta }}\\nu $ based on six independent pipeline analyses; first-ascent red giant branch (RGB) and red clump (RC) evolutionary state classifications from machine learning; and ready-to-use radius and mass coefficients, κR and κM, which, when appropriately multiplied by a solar-scaled effective temperature factor, yield physical stellar radii and masses. In total, we report 4395 radius and mass coefficients, with typical uncertainties of 3.3% (stat.) ± 1% (syst.) for κR and 7.7% (stat.) ± 2% (syst.) for κM among RGB stars, and 5.0% (stat.) ± 1% (syst.) for κR and 10.5% (stat.) ± 2% (syst.) for κM among RC stars. We verify that the sample is nearly complete—except for a dearth of stars with ${\\nu }_{\\max }\\lesssim 10\\mbox{--}20\\,\\mu \\mathrm{Hz}$—by comparing to Galactic models and visual inspection. Our asteroseismic radii agree with radii derived from Gaia Data Release 2 parallaxes to within 2.2% ± 0.3% for RGB stars and 2.0% ± 0.6% for RC stars.","lang":"eng"}],"article_number":"23","main_file_link":[{"url":"https://arxiv.org/abs/2012.04051","open_access":"1"}],"oa":1,"publication_status":"published","volume":251},{"page":"382-389","extern":"1","month":"04","date_created":"2022-07-18T13:36:19Z","publisher":"Springer Nature","quality_controlled":"1","publication":"Nature Astronomy","status":"public","intvolume":" 4","citation":{"ama":"Chaplin WJ, Serenelli AM, Miglio A, et al. Age dating of an early Milky Way merger via asteroseismology of the naked-eye star ν Indi. Nature Astronomy. 2020;4(4):382-389. doi:10.1038/s41550-019-0975-9","apa":"Chaplin, W. J., Serenelli, A. M., Miglio, A., Morel, T., Mackereth, J. T., Vincenzo, F., … Yıldız, M. (2020). Age dating of an early Milky Way merger via asteroseismology of the naked-eye star ν Indi. Nature Astronomy. Springer Nature. https://doi.org/10.1038/s41550-019-0975-9","short":"W.J. Chaplin, A.M. Serenelli, A. Miglio, T. Morel, J.T. Mackereth, F. Vincenzo, H. Kjeldsen, S. Basu, W.H. Ball, A. Stokholm, K. Verma, J.R. Mosumgaard, V. Silva Aguirre, A. Mazumdar, P. Ranadive, H.M. Antia, Y. Lebreton, J. Ong, T. Appourchaux, T.R. Bedding, J. Christensen-Dalsgaard, O. Creevey, R.A. García, R. Handberg, D. Huber, S.D. Kawaler, M.N. Lund, T.S. Metcalfe, K.G. Stassun, M. Bazot, P.G. Beck, K.J. Bell, M. Bergemann, D.L. Buzasi, O. Benomar, D. Bossini, L.A. Bugnet, T.L. Campante, Z.Ç. Orhan, E. Corsaro, L. González-Cuesta, G.R. Davies, M.P. Di Mauro, R. Egeland, Y.P. Elsworth, P. Gaulme, H. Ghasemi, Z. Guo, O.J. Hall, A. Hasanzadeh, S. Hekker, R. Howe, J.M. Jenkins, A. Jiménez, R. Kiefer, J.S. Kuszlewicz, T. Kallinger, D.W. Latham, M.S. Lundkvist, S. Mathur, J. Montalbán, B. Mosser, A.M. Bedón, M.B. Nielsen, S. Örtel, B.M. Rendle, G.R. Ricker, T.S. Rodrigues, I.W. Roxburgh, H. Safari, M. Schofield, S. Seager, B. Smalley, D. Stello, R. Szabó, J. Tayar, N. Themeßl, A.E.L. Thomas, R.K. Vanderspek, W.E. van Rossem, M. Vrard, A. Weiss, T.R. White, J.N. Winn, M. Yıldız, Nature Astronomy 4 (2020) 382–389.","mla":"Chaplin, William J., et al. “Age Dating of an Early Milky Way Merger via Asteroseismology of the Naked-Eye Star ν Indi.” Nature Astronomy, vol. 4, no. 4, Springer Nature, 2020, pp. 382–89, doi:10.1038/s41550-019-0975-9.","chicago":"Chaplin, William J., Aldo M. Serenelli, Andrea Miglio, Thierry Morel, J. Ted Mackereth, Fiorenzo Vincenzo, Hans Kjeldsen, et al. “Age Dating of an Early Milky Way Merger via Asteroseismology of the Naked-Eye Star ν Indi.” Nature Astronomy. Springer Nature, 2020. https://doi.org/10.1038/s41550-019-0975-9.","ieee":"W. J. Chaplin et al., “Age dating of an early Milky Way merger via asteroseismology of the naked-eye star ν Indi,” Nature Astronomy, vol. 4, no. 4. Springer Nature, pp. 382–389, 2020.","ista":"Chaplin WJ, Serenelli AM, Miglio A, Morel T, Mackereth JT, Vincenzo F, Kjeldsen H, Basu S, Ball WH, Stokholm A, Verma K, Mosumgaard JR, Silva Aguirre V, Mazumdar A, Ranadive P, Antia HM, Lebreton Y, Ong J, Appourchaux T, Bedding TR, Christensen-Dalsgaard J, Creevey O, García RA, Handberg R, Huber D, Kawaler SD, Lund MN, Metcalfe TS, Stassun KG, Bazot M, Beck PG, Bell KJ, Bergemann M, Buzasi DL, Benomar O, Bossini D, Bugnet LA, Campante TL, Orhan ZÇ, Corsaro E, González-Cuesta L, Davies GR, Di Mauro MP, Egeland R, Elsworth YP, Gaulme P, Ghasemi H, Guo Z, Hall OJ, Hasanzadeh A, Hekker S, Howe R, Jenkins JM, Jiménez A, Kiefer R, Kuszlewicz JS, Kallinger T, Latham DW, Lundkvist MS, Mathur S, Montalbán J, Mosser B, Bedón AM, Nielsen MB, Örtel S, Rendle BM, Ricker GR, Rodrigues TS, Roxburgh IW, Safari H, Schofield M, Seager S, Smalley B, Stello D, Szabó R, Tayar J, Themeßl N, Thomas AEL, Vanderspek RK, van Rossem WE, Vrard M, Weiss A, White TR, Winn JN, Yıldız M. 2020. Age dating of an early Milky Way merger via asteroseismology of the naked-eye star ν Indi. Nature Astronomy. 4(4), 382–389."},"title":"Age dating of an early Milky Way merger via asteroseismology of the naked-eye star ν Indi","day":"01","author":[{"last_name":"Chaplin","full_name":"Chaplin, William J.","first_name":"William J."},{"last_name":"Serenelli","full_name":"Serenelli, Aldo M.","first_name":"Aldo M."},{"first_name":"Andrea","full_name":"Miglio, Andrea","last_name":"Miglio"},{"first_name":"Thierry","full_name":"Morel, Thierry","last_name":"Morel"},{"full_name":"Mackereth, J. Ted","first_name":"J. Ted","last_name":"Mackereth"},{"full_name":"Vincenzo, Fiorenzo","first_name":"Fiorenzo","last_name":"Vincenzo"},{"full_name":"Kjeldsen, Hans","first_name":"Hans","last_name":"Kjeldsen"},{"first_name":"Sarbani","full_name":"Basu, Sarbani","last_name":"Basu"},{"last_name":"Ball","first_name":"Warrick H.","full_name":"Ball, Warrick H."},{"last_name":"Stokholm","first_name":"Amalie","full_name":"Stokholm, Amalie"},{"full_name":"Verma, Kuldeep","first_name":"Kuldeep","last_name":"Verma"},{"last_name":"Mosumgaard","full_name":"Mosumgaard, Jakob Rørsted","first_name":"Jakob Rørsted"},{"first_name":"Victor","full_name":"Silva Aguirre, Victor","last_name":"Silva Aguirre"},{"first_name":"Anwesh","full_name":"Mazumdar, Anwesh","last_name":"Mazumdar"},{"last_name":"Ranadive","full_name":"Ranadive, Pritesh","first_name":"Pritesh"},{"full_name":"Antia, H. M.","first_name":"H. M.","last_name":"Antia"},{"last_name":"Lebreton","first_name":"Yveline","full_name":"Lebreton, Yveline"},{"last_name":"Ong","full_name":"Ong, Joel","first_name":"Joel"},{"first_name":"Thierry","full_name":"Appourchaux, Thierry","last_name":"Appourchaux"},{"last_name":"Bedding","full_name":"Bedding, Timothy R.","first_name":"Timothy R."},{"full_name":"Christensen-Dalsgaard, Jørgen","first_name":"Jørgen","last_name":"Christensen-Dalsgaard"},{"last_name":"Creevey","first_name":"Orlagh","full_name":"Creevey, Orlagh"},{"last_name":"García","full_name":"García, Rafael A.","first_name":"Rafael A."},{"first_name":"Rasmus","full_name":"Handberg, Rasmus","last_name":"Handberg"},{"full_name":"Huber, Daniel","first_name":"Daniel","last_name":"Huber"},{"last_name":"Kawaler","full_name":"Kawaler, Steven D.","first_name":"Steven D."},{"last_name":"Lund","first_name":"Mikkel N.","full_name":"Lund, Mikkel N."},{"last_name":"Metcalfe","full_name":"Metcalfe, Travis S.","first_name":"Travis S."},{"last_name":"Stassun","full_name":"Stassun, Keivan G.","first_name":"Keivan G."},{"full_name":"Bazot, Michäel","first_name":"Michäel","last_name":"Bazot"},{"last_name":"Beck","first_name":"Paul G.","full_name":"Beck, Paul G."},{"last_name":"Bell","full_name":"Bell, Keaton J.","first_name":"Keaton J."},{"last_name":"Bergemann","full_name":"Bergemann, Maria","first_name":"Maria"},{"full_name":"Buzasi, Derek L.","first_name":"Derek L.","last_name":"Buzasi"},{"last_name":"Benomar","full_name":"Benomar, Othman","first_name":"Othman"},{"last_name":"Bossini","first_name":"Diego","full_name":"Bossini, Diego"},{"orcid":"0000-0003-0142-4000","id":"d9edb345-f866-11ec-9b37-d119b5234501","last_name":"Bugnet","first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle"},{"last_name":"Campante","first_name":"Tiago L.","full_name":"Campante, Tiago L."},{"first_name":"Zeynep Çelik","full_name":"Orhan, Zeynep Çelik","last_name":"Orhan"},{"full_name":"Corsaro, Enrico","first_name":"Enrico","last_name":"Corsaro"},{"full_name":"González-Cuesta, Lucía","first_name":"Lucía","last_name":"González-Cuesta"},{"last_name":"Davies","first_name":"Guy R.","full_name":"Davies, Guy R."},{"last_name":"Di Mauro","full_name":"Di Mauro, Maria Pia","first_name":"Maria Pia"},{"full_name":"Egeland, Ricky","first_name":"Ricky","last_name":"Egeland"},{"first_name":"Yvonne P.","full_name":"Elsworth, Yvonne P.","last_name":"Elsworth"},{"full_name":"Gaulme, Patrick","first_name":"Patrick","last_name":"Gaulme"},{"first_name":"Hamed","full_name":"Ghasemi, Hamed","last_name":"Ghasemi"},{"full_name":"Guo, Zhao","first_name":"Zhao","last_name":"Guo"},{"last_name":"Hall","first_name":"Oliver J.","full_name":"Hall, Oliver J."},{"full_name":"Hasanzadeh, Amir","first_name":"Amir","last_name":"Hasanzadeh"},{"last_name":"Hekker","full_name":"Hekker, Saskia","first_name":"Saskia"},{"last_name":"Howe","first_name":"Rachel","full_name":"Howe, Rachel"},{"last_name":"Jenkins","full_name":"Jenkins, Jon M.","first_name":"Jon M."},{"last_name":"Jiménez","first_name":"Antonio","full_name":"Jiménez, Antonio"},{"first_name":"René","full_name":"Kiefer, René","last_name":"Kiefer"},{"last_name":"Kuszlewicz","full_name":"Kuszlewicz, James S.","first_name":"James S."},{"first_name":"Thomas","full_name":"Kallinger, Thomas","last_name":"Kallinger"},{"last_name":"Latham","first_name":"David W.","full_name":"Latham, David W."},{"first_name":"Mia S.","full_name":"Lundkvist, Mia S.","last_name":"Lundkvist"},{"last_name":"Mathur","full_name":"Mathur, Savita","first_name":"Savita"},{"last_name":"Montalbán","first_name":"Josefina","full_name":"Montalbán, Josefina"},{"last_name":"Mosser","full_name":"Mosser, Benoit","first_name":"Benoit"},{"last_name":"Bedón","full_name":"Bedón, Andres Moya","first_name":"Andres Moya"},{"last_name":"Nielsen","first_name":"Martin Bo","full_name":"Nielsen, Martin Bo"},{"full_name":"Örtel, Sibel","first_name":"Sibel","last_name":"Örtel"},{"first_name":"Ben M.","full_name":"Rendle, Ben M.","last_name":"Rendle"},{"last_name":"Ricker","full_name":"Ricker, George R.","first_name":"George R."},{"first_name":"Thaíse S.","full_name":"Rodrigues, Thaíse S.","last_name":"Rodrigues"},{"first_name":"Ian W.","full_name":"Roxburgh, Ian W.","last_name":"Roxburgh"},{"last_name":"Safari","full_name":"Safari, Hossein","first_name":"Hossein"},{"full_name":"Schofield, Mathew","first_name":"Mathew","last_name":"Schofield"},{"last_name":"Seager","first_name":"Sara","full_name":"Seager, Sara"},{"first_name":"Barry","full_name":"Smalley, Barry","last_name":"Smalley"},{"first_name":"Dennis","full_name":"Stello, Dennis","last_name":"Stello"},{"last_name":"Szabó","first_name":"Róbert","full_name":"Szabó, Róbert"},{"last_name":"Tayar","first_name":"Jamie","full_name":"Tayar, Jamie"},{"last_name":"Themeßl","full_name":"Themeßl, Nathalie","first_name":"Nathalie"},{"last_name":"Thomas","first_name":"Alexandra E. L.","full_name":"Thomas, Alexandra E. L."},{"first_name":"Roland K.","full_name":"Vanderspek, Roland K.","last_name":"Vanderspek"},{"last_name":"van Rossem","first_name":"Walter E.","full_name":"van Rossem, Walter E."},{"last_name":"Vrard","first_name":"Mathieu","full_name":"Vrard, Mathieu"},{"last_name":"Weiss","first_name":"Achim","full_name":"Weiss, Achim"},{"full_name":"White, Timothy R.","first_name":"Timothy R.","last_name":"White"},{"first_name":"Joshua N.","full_name":"Winn, Joshua N.","last_name":"Winn"},{"last_name":"Yıldız","first_name":"Mutlu","full_name":"Yıldız, Mutlu"}],"type":"journal_article","acknowledgement":"This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. W.J.C. acknowledges support from the UK Science and Technology Facilities Council (STFC) and UK Space Agency. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (grant agreement number DNRF106). This research was partially conducted during the Exostar19 programme at the Kavli Institute for Theoretical Physics at UC Santa Barbara, which was supported in part by the National Science Foundation under grant number NSF PHY-1748958. A.M., J.T.M., F.V. and J.M. acknowledge support from the ERC Consolidator Grant funding scheme (project ASTEROCHRONOMETRY, grant agreement number 772293). F.V. acknowledges the support of a Fellowship from the Center for Cosmology and AstroParticle Physics at The Ohio State University. W.H.B. and M.B.N. acknowledge support from the UK Space Agency. K.J.B. is supported by the National Science Foundation under award AST-1903828. M.B.N. acknowledges partial support from the NYU Abu Dhabi Center for Space Science under grant number G1502. A.M.S. is partially supported by the Spanish Government (ESP2017-82674-R) and Generalitat de Catalunya (2017-SGR-1131). T.M. acknowledges financial support from Belspo for contract PRODEX PLATO. H.K. acknowledges support from the European Social Fund via the Lithuanian Science Council grant number 09.3.3-LMT-K-712-01-0103. S.B. acknowledges support from NSF grant AST-1514676 and NASA grant 80NSSC19K0374. V.S.A. acknowledges support from the Independent Research Fund Denmark (research grant 7027-00096B). D.H. acknowledges support by the National Aeronautics and Space Administration (80NSSC18K1585, 80NSSC19K0379) awarded through the TESS Guest Investigator Program and by the National Science Foundation (AST-1717000). T.S.M. acknowledges support from a visiting fellowship at the Max Planck Institute for Solar System Research. Computational resources were provided through XSEDE allocation TG-AST090107. D.L.B. acknowledges support from NASA under grant NNX16AB76G. T.L.C. acknowledges support from the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement number 792848 (PULSATION). This work was supported by FCT/MCTES through national funds (PIDDAC) by means of grant UID/FIS/04434/2019. K.J.B., S.H., J.S.K. and N.T. are supported by the European Research Council under the European Community’s Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement number 338251 (StellarAges). E.C. is funded by the European Union’s Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement number 664931. L.G.-C. acknowledges support from the MINECO FPI-SO doctoral research project SEV-2015-0548-17-2 and predoctoral contract BES-2017-082610. P.G. is supported by the German space agency (Deutsches Zentrum für Luft- und Raumfahrt) under PLATO data grant 50OO1501. R.K. acknowledges support from the UK Science and Technology Facilities Council (STFC), under consolidated grant ST/L000733/1. M.S.L. is supported by the Carlsberg Foundation (grant agreement number CF17-076). Z.C.O., S.O. and M.Y. acknowledge support from the Scientific and Technological Research Council of Turkey (TÜBİTAK:118F352). S.M. acknowledges support from the Spanish ministry through the Ramon y Cajal fellowship number RYC-2015-17697. T.S.R. acknowledges financial support from Premiale 2015 MITiC (PI B. Garilli). R.Sz. acknowledges the support from NKFIH grant project No. K-115709, and the Lendület program of the Hungarian Academy of Science (project number 2018-7/2019). J.T. acknowledges support was provided by NASA through the NASA Hubble Fellowship grant number 51424 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. This work was supported by FEDER through COMPETE2020 (POCI-01-0145-FEDER-030389. A.M.B. acknowledges funding from the European Union’s Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement No 749962 (project THOT). A.M. and P.R. acknowledge the support of the Government of India, Department of Atomic Energy, under Project No. 12-R&D-TFR-6.04-0600. K.J.B. is an NSF Astronomy and Astrophysics Postdoctoral Fellow and DIRAC Fellow.","language":[{"iso":"eng"}],"keyword":["Astronomy and Astrophysics"],"doi":"10.1038/s41550-019-0975-9","arxiv":1,"issue":"4","article_processing_charge":"No","_id":"11611","abstract":[{"lang":"eng","text":"Over the course of its history, the Milky Way has ingested multiple smaller satellite galaxies1. Although these accreted stellar populations can be forensically identified as kinematically distinct structures within the Galaxy, it is difficult in general to date precisely the age at which any one merger occurred. Recent results have revealed a population of stars that were accreted via the collision of a dwarf galaxy, called Gaia–Enceladus1, leading to substantial pollution of the chemical and dynamical properties of the Milky Way. Here we identify the very bright, naked-eye star ν Indi as an indicator of the age of the early in situ population of the Galaxy. We combine asteroseismic, spectroscopic, astrometric and kinematic observations to show that this metal-poor, alpha-element-rich star was an indigenous member of the halo, and we measure its age to be 11.0±0.7 (stat) ±0.8 (sys) billion years. The star bears hallmarks consistent with having been kinematically heated by the Gaia–Enceladus collision. Its age implies that the earliest the merger could have begun was 11.6 and 13.2 billion years ago, at 68% and 95% confidence, respectively. Computations based on hierarchical cosmological models slightly reduce the above limits."}],"date_published":"2020-04-01T00:00:00Z","publication_status":"published","main_file_link":[{"url":"https://arxiv.org/abs/2001.04653","open_access":"1"}],"oa":1,"volume":4,"article_type":"letter_note","oa_version":"Preprint","year":"2020","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2022-08-22T07:08:29Z","external_id":{"arxiv":["2001.04653"]},"scopus_import":"1","publication_identifier":{"eissn":["2397-3366"]}},{"year":"2020","oa_version":"Preprint","article_type":"original","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"date_updated":"2022-08-22T07:25:51Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","scopus_import":"1","external_id":{"arxiv":["1912.07604"]},"_id":"11612","abstract":[{"text":"Since the onset of the \"space revolution\" of high-precision high-cadence photometry, asteroseismology has been demonstrated as a powerful tool for informing Galactic archeology investigations. The launch of the NASA Transiting Exoplanet Survey Satellite (TESS) mission has enabled seismic-based inferences to go full sky—providing a clear advantage for large ensemble studies of the different Milky Way components. Here we demonstrate its potential for investigating the Galaxy by carrying out the first asteroseismic ensemble study of red giant stars observed by TESS. We use a sample of 25 stars for which we measure their global asteroseimic observables and estimate their fundamental stellar properties, such as radius, mass, and age. Significant improvements are seen in the uncertainties of our estimates when combining seismic observables from TESS with astrometric measurements from the Gaia mission compared to when the seismology and astrometry are applied separately. Specifically, when combined we show that stellar radii can be determined to a precision of a few percent, masses to 5%–10%, and ages to the 20% level. This is comparable to the precision typically obtained using end-of-mission Kepler data.","lang":"eng"}],"date_published":"2020-02-01T00:00:00Z","article_number":"L34","issue":"2","article_processing_charge":"No","arxiv":1,"volume":889,"oa":1,"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1912.07604"}],"publication_status":"published","author":[{"last_name":"Aguirre","first_name":"Víctor Silva","full_name":"Aguirre, Víctor Silva"},{"first_name":"Dennis","full_name":"Stello, Dennis","last_name":"Stello"},{"last_name":"Stokholm","full_name":"Stokholm, Amalie","first_name":"Amalie"},{"first_name":"Jakob R.","full_name":"Mosumgaard, Jakob R.","last_name":"Mosumgaard"},{"last_name":"Ball","first_name":"Warrick H.","full_name":"Ball, Warrick H."},{"first_name":"Sarbani","full_name":"Basu, Sarbani","last_name":"Basu"},{"full_name":"Bossini, Diego","first_name":"Diego","last_name":"Bossini"},{"first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle","last_name":"Bugnet","id":"d9edb345-f866-11ec-9b37-d119b5234501","orcid":"0000-0003-0142-4000"},{"first_name":"Derek","full_name":"Buzasi, Derek","last_name":"Buzasi"},{"last_name":"Campante","full_name":"Campante, Tiago L.","first_name":"Tiago L."},{"last_name":"Carboneau","full_name":"Carboneau, Lindsey","first_name":"Lindsey"},{"first_name":"William J.","full_name":"Chaplin, William J.","last_name":"Chaplin"},{"last_name":"Corsaro","full_name":"Corsaro, Enrico","first_name":"Enrico"},{"full_name":"Davies, Guy R.","first_name":"Guy R.","last_name":"Davies"},{"first_name":"Yvonne","full_name":"Elsworth, Yvonne","last_name":"Elsworth"},{"first_name":"Rafael A.","full_name":"García, Rafael A.","last_name":"García"},{"full_name":"Gaulme, Patrick","first_name":"Patrick","last_name":"Gaulme"},{"last_name":"Hall","full_name":"Hall, Oliver J.","first_name":"Oliver J."},{"full_name":"Handberg, Rasmus","first_name":"Rasmus","last_name":"Handberg"},{"last_name":"Hon","first_name":"Marc","full_name":"Hon, Marc"},{"last_name":"Kallinger","first_name":"Thomas","full_name":"Kallinger, Thomas"},{"first_name":"Liu","full_name":"Kang, Liu","last_name":"Kang"},{"first_name":"Mikkel N.","full_name":"Lund, Mikkel N.","last_name":"Lund"},{"first_name":"Savita","full_name":"Mathur, Savita","last_name":"Mathur"},{"full_name":"Mints, Alexey","first_name":"Alexey","last_name":"Mints"},{"last_name":"Mosser","first_name":"Benoit","full_name":"Mosser, Benoit"},{"last_name":"Çelik Orhan","first_name":"Zeynep","full_name":"Çelik Orhan, Zeynep"},{"full_name":"Rodrigues, Thaíse S.","first_name":"Thaíse S.","last_name":"Rodrigues"},{"last_name":"Vrard","full_name":"Vrard, Mathieu","first_name":"Mathieu"},{"last_name":"Yıldız","first_name":"Mutlu","full_name":"Yıldız, Mutlu"},{"full_name":"Zinn, Joel C.","first_name":"Joel C.","last_name":"Zinn"},{"first_name":"Sibel","full_name":"Örtel, Sibel","last_name":"Örtel"},{"first_name":"Paul G.","full_name":"Beck, Paul G.","last_name":"Beck"},{"first_name":"Keaton J.","full_name":"Bell, Keaton J.","last_name":"Bell"},{"last_name":"Guo","first_name":"Zhao","full_name":"Guo, Zhao"},{"last_name":"Jiang","full_name":"Jiang, Chen","first_name":"Chen"},{"first_name":"James S.","full_name":"Kuszlewicz, James S.","last_name":"Kuszlewicz"},{"full_name":"Kuehn, Charles A.","first_name":"Charles A.","last_name":"Kuehn"},{"first_name":"Tanda","full_name":"Li, Tanda","last_name":"Li"},{"first_name":"Mia S.","full_name":"Lundkvist, Mia S.","last_name":"Lundkvist"},{"first_name":"Marc","full_name":"Pinsonneault, Marc","last_name":"Pinsonneault"},{"first_name":"Jamie","full_name":"Tayar, Jamie","last_name":"Tayar"},{"full_name":"Cunha, Margarida S.","first_name":"Margarida S.","last_name":"Cunha"},{"last_name":"Hekker","full_name":"Hekker, Saskia","first_name":"Saskia"},{"last_name":"Huber","full_name":"Huber, Daniel","first_name":"Daniel"},{"last_name":"Miglio","full_name":"Miglio, Andrea","first_name":"Andrea"},{"full_name":"F. G. Monteiro, Mario J. P.","first_name":"Mario J. P.","last_name":"F. G. Monteiro"},{"last_name":"Slumstrup","first_name":"Ditte","full_name":"Slumstrup, Ditte"},{"last_name":"Winther","first_name":"Mark L.","full_name":"Winther, Mark L."},{"last_name":"Angelou","first_name":"George","full_name":"Angelou, George"},{"last_name":"Benomar","first_name":"Othman","full_name":"Benomar, Othman"},{"first_name":"Attila","full_name":"Bódi, Attila","last_name":"Bódi"},{"last_name":"De Moura","first_name":"Bruno L.","full_name":"De Moura, Bruno L."},{"last_name":"Deheuvels","first_name":"Sébastien","full_name":"Deheuvels, Sébastien"},{"last_name":"Derekas","first_name":"Aliz","full_name":"Derekas, Aliz"},{"first_name":"Maria Pia","full_name":"Di Mauro, Maria Pia","last_name":"Di Mauro"},{"full_name":"Dupret, Marc-Antoine","first_name":"Marc-Antoine","last_name":"Dupret"},{"full_name":"Jiménez, Antonio","first_name":"Antonio","last_name":"Jiménez"},{"last_name":"Lebreton","first_name":"Yveline","full_name":"Lebreton, Yveline"},{"first_name":"Jaymie","full_name":"Matthews, Jaymie","last_name":"Matthews"},{"last_name":"Nardetto","full_name":"Nardetto, Nicolas","first_name":"Nicolas"},{"last_name":"do Nascimento","full_name":"do Nascimento, Jose D.","first_name":"Jose D."},{"full_name":"Pereira, Filipe","first_name":"Filipe","last_name":"Pereira"},{"last_name":"Rodríguez Díaz","full_name":"Rodríguez Díaz, Luisa F.","first_name":"Luisa F."},{"first_name":"Aldo M.","full_name":"Serenelli, Aldo M.","last_name":"Serenelli"},{"first_name":"Emanuele","full_name":"Spitoni, Emanuele","last_name":"Spitoni"},{"full_name":"Stonkutė, Edita","first_name":"Edita","last_name":"Stonkutė"},{"last_name":"Suárez","first_name":"Juan Carlos","full_name":"Suárez, Juan Carlos"},{"first_name":"Robert","full_name":"Szabó, Robert","last_name":"Szabó"},{"last_name":"Van Eylen","first_name":"Vincent","full_name":"Van Eylen, Vincent"},{"first_name":"Rita","full_name":"Ventura, Rita","last_name":"Ventura"},{"last_name":"Verma","full_name":"Verma, Kuldeep","first_name":"Kuldeep"},{"first_name":"Achim","full_name":"Weiss, Achim","last_name":"Weiss"},{"full_name":"Wu, Tao","first_name":"Tao","last_name":"Wu"},{"last_name":"Barclay","full_name":"Barclay, Thomas","first_name":"Thomas"},{"full_name":"Christensen-Dalsgaard, Jørgen","first_name":"Jørgen","last_name":"Christensen-Dalsgaard"},{"first_name":"Jon M.","full_name":"Jenkins, Jon M.","last_name":"Jenkins"},{"last_name":"Kjeldsen","first_name":"Hans","full_name":"Kjeldsen, Hans"},{"last_name":"Ricker","full_name":"Ricker, George R.","first_name":"George R."},{"last_name":"Seager","full_name":"Seager, Sara","first_name":"Sara"},{"last_name":"Vanderspek","full_name":"Vanderspek, Roland","first_name":"Roland"}],"type":"journal_article","day":"01","title":"Detection and characterization of oscillating red giants: First results from the TESS satellite","citation":{"mla":"Aguirre, Víctor Silva, et al. “Detection and Characterization of Oscillating Red Giants: First Results from the TESS Satellite.” The Astrophysical Journal Letters, vol. 889, no. 2, L34, IOP Publishing, 2020, doi:10.3847/2041-8213/ab6443.","chicago":"Aguirre, Víctor Silva, Dennis Stello, Amalie Stokholm, Jakob R. Mosumgaard, Warrick H. Ball, Sarbani Basu, Diego Bossini, et al. “Detection and Characterization of Oscillating Red Giants: First Results from the TESS Satellite.” The Astrophysical Journal Letters. IOP Publishing, 2020. https://doi.org/10.3847/2041-8213/ab6443.","ieee":"V. S. Aguirre et al., “Detection and characterization of oscillating red giants: First results from the TESS satellite,” The Astrophysical Journal Letters, vol. 889, no. 2. IOP Publishing, 2020.","ista":"Aguirre VS, Stello D, Stokholm A, Mosumgaard JR, Ball WH, Basu S, Bossini D, Bugnet LA, Buzasi D, Campante TL, Carboneau L, Chaplin WJ, Corsaro E, Davies GR, Elsworth Y, García RA, Gaulme P, Hall OJ, Handberg R, Hon M, Kallinger T, Kang L, Lund MN, Mathur S, Mints A, Mosser B, Çelik Orhan Z, Rodrigues TS, Vrard M, Yıldız M, Zinn JC, Örtel S, Beck PG, Bell KJ, Guo Z, Jiang C, Kuszlewicz JS, Kuehn CA, Li T, Lundkvist MS, Pinsonneault M, Tayar J, Cunha MS, Hekker S, Huber D, Miglio A, F. G. Monteiro MJP, Slumstrup D, Winther ML, Angelou G, Benomar O, Bódi A, De Moura BL, Deheuvels S, Derekas A, Di Mauro MP, Dupret M-A, Jiménez A, Lebreton Y, Matthews J, Nardetto N, do Nascimento JD, Pereira F, Rodríguez Díaz LF, Serenelli AM, Spitoni E, Stonkutė E, Suárez JC, Szabó R, Van Eylen V, Ventura R, Verma K, Weiss A, Wu T, Barclay T, Christensen-Dalsgaard J, Jenkins JM, Kjeldsen H, Ricker GR, Seager S, Vanderspek R. 2020. Detection and characterization of oscillating red giants: First results from the TESS satellite. The Astrophysical Journal Letters. 889(2), L34.","ama":"Aguirre VS, Stello D, Stokholm A, et al. Detection and characterization of oscillating red giants: First results from the TESS satellite. The Astrophysical Journal Letters. 2020;889(2). doi:10.3847/2041-8213/ab6443","apa":"Aguirre, V. S., Stello, D., Stokholm, A., Mosumgaard, J. R., Ball, W. H., Basu, S., … Vanderspek, R. (2020). Detection and characterization of oscillating red giants: First results from the TESS satellite. The Astrophysical Journal Letters. IOP Publishing. https://doi.org/10.3847/2041-8213/ab6443","short":"V.S. Aguirre, D. Stello, A. Stokholm, J.R. Mosumgaard, W.H. Ball, S. Basu, D. Bossini, L.A. Bugnet, D. Buzasi, T.L. Campante, L. Carboneau, W.J. Chaplin, E. Corsaro, G.R. Davies, Y. Elsworth, R.A. García, P. Gaulme, O.J. Hall, R. Handberg, M. Hon, T. Kallinger, L. Kang, M.N. Lund, S. Mathur, A. Mints, B. Mosser, Z. Çelik Orhan, T.S. Rodrigues, M. Vrard, M. Yıldız, J.C. Zinn, S. Örtel, P.G. Beck, K.J. Bell, Z. Guo, C. Jiang, J.S. Kuszlewicz, C.A. Kuehn, T. Li, M.S. Lundkvist, M. Pinsonneault, J. Tayar, M.S. Cunha, S. Hekker, D. Huber, A. Miglio, M.J.P. F. G. Monteiro, D. Slumstrup, M.L. Winther, G. Angelou, O. Benomar, A. Bódi, B.L. De Moura, S. Deheuvels, A. Derekas, M.P. Di Mauro, M.-A. Dupret, A. Jiménez, Y. Lebreton, J. Matthews, N. Nardetto, J.D. do Nascimento, F. Pereira, L.F. Rodríguez Díaz, A.M. Serenelli, E. Spitoni, E. Stonkutė, J.C. Suárez, R. Szabó, V. Van Eylen, R. Ventura, K. Verma, A. Weiss, T. Wu, T. Barclay, J. Christensen-Dalsgaard, J.M. Jenkins, H. Kjeldsen, G.R. Ricker, S. Seager, R. Vanderspek, The Astrophysical Journal Letters 889 (2020)."},"doi":"10.3847/2041-8213/ab6443","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"acknowledgement":"This Letter includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). Funding for the TESS mission is provided by NASA's Science Mission directorate. Funding for the TESS Asteroseismic Science Operations Centre is provided by the Danish National Research Foundation (grant agreement No. DNRF106), ESA PRODEX (PEA 4000119301), and Stellar Astrophysics Centre (SAC) at Aarhus University. V.S.A. acknowledges support from the Independent Research Fund Denmark (Research grant 7027-00096B). D.B. is supported in the form of work contract FCT/MCTES through national funds and by FEDER through COMPETE2020 in connection to these grants: UID/FIS/04434/2019; PTDC/FIS-AST/30389/2017 & POCI-01-0145-FEDER-030389. L.B., R.A.G., and B.M. acknowledge the support from the CNES/PLATO grant. D.B. acknowledges NASA grant NNX16AB76G. T.L.C. acknowledges support from the European Union's Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement No. 792848 (PULSATION). This work was supported by FCT/MCTES through national funds (UID/FIS/04434/2019). E.C. is funded by the European Union's Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement No. 664931. R.H. and M.N.L. acknowledge the support of the ESA PRODEX programme. T.S.R. acknowledges financial support from Premiale 2015 MITiC (PI B. Garilli). K.J.B. is supported by the National Science Foundation under Award AST-1903828. M.S.L. is supported by the Carlsberg Foundation (grant agreement No. CF17-0760). M.C. is funded by FCT//MCTES through national funds and by FEDER through COMPETE2020 through these grants: UID/FIS/04434/2019, PTDC/FIS-AST/30389/2017 & POCI-01-0145-FEDER-030389, CEECIND/02619/2017. The research leading to the presented results has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement no 338251 (StellarAges). A.M. acknowledges support from the European Research Council Consolidator Grant funding scheme (project ASTEROCHRONOMETRY, grant agreement No. 772293, http://www.asterochronometry.eu). A.M.S. is partially supported by MINECO grant ESP2017-82674-R. J.C.S. acknowledges funding support from Spanish public funds for research under projects ESP2017-87676-2-2, and from project RYC-2012-09913 under the 'Ramón y Cajal' program of the Spanish Ministry of Science and Education. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products.","date_created":"2022-07-18T13:52:54Z","extern":"1","month":"02","intvolume":" 889","status":"public","quality_controlled":"1","publication":"The Astrophysical Journal Letters","publisher":"IOP Publishing"},{"date_created":"2020-09-18T10:56:20Z","month":"09","isi":1,"publisher":"Springer Nature","status":"public","intvolume":" 11","publication":"Nature Communications","department":[{"_id":"JoFi"}],"quality_controlled":"1","title":"Converting microwave and telecom photons with a silicon photonic nanomechanical interface","citation":{"mla":"Arnold, Georg M., et al. “Converting Microwave and Telecom Photons with a Silicon Photonic Nanomechanical Interface.” Nature Communications, vol. 11, 4460, Springer Nature, 2020, doi:10.1038/s41467-020-18269-z.","ista":"Arnold GM, Wulf M, Barzanjeh S, Redchenko E, Rueda Sanchez AR, Hease WJ, Hassani F, Fink JM. 2020. Converting microwave and telecom photons with a silicon photonic nanomechanical interface. Nature Communications. 11, 4460.","ieee":"G. M. Arnold et al., “Converting microwave and telecom photons with a silicon photonic nanomechanical interface,” Nature Communications, vol. 11. Springer Nature, 2020.","chicago":"Arnold, Georg M, Matthias Wulf, Shabir Barzanjeh, Elena Redchenko, Alfredo R Rueda Sanchez, William J Hease, Farid Hassani, and Johannes M Fink. “Converting Microwave and Telecom Photons with a Silicon Photonic Nanomechanical Interface.” Nature Communications. Springer Nature, 2020. https://doi.org/10.1038/s41467-020-18269-z.","apa":"Arnold, G. M., Wulf, M., Barzanjeh, S., Redchenko, E., Rueda Sanchez, A. R., Hease, W. J., … Fink, J. M. (2020). Converting microwave and telecom photons with a silicon photonic nanomechanical interface. Nature Communications. Springer Nature. https://doi.org/10.1038/s41467-020-18269-z","ama":"Arnold GM, Wulf M, Barzanjeh S, et al. Converting microwave and telecom photons with a silicon photonic nanomechanical interface. Nature Communications. 2020;11. doi:10.1038/s41467-020-18269-z","short":"G.M. Arnold, M. Wulf, S. Barzanjeh, E. Redchenko, A.R. Rueda Sanchez, W.J. Hease, F. Hassani, J.M. Fink, Nature Communications 11 (2020)."},"ec_funded":1,"type":"journal_article","author":[{"full_name":"Arnold, Georg M","first_name":"Georg M","last_name":"Arnold","orcid":"0000-0003-1397-7876","id":"3770C838-F248-11E8-B48F-1D18A9856A87"},{"first_name":"Matthias","full_name":"Wulf, Matthias","last_name":"Wulf","id":"45598606-F248-11E8-B48F-1D18A9856A87","orcid":"0000-0001-6613-1378"},{"last_name":"Barzanjeh","full_name":"Barzanjeh, Shabir","first_name":"Shabir","orcid":"0000-0003-0415-1423","id":"2D25E1F6-F248-11E8-B48F-1D18A9856A87"},{"id":"2C21D6E8-F248-11E8-B48F-1D18A9856A87","full_name":"Redchenko, Elena","first_name":"Elena","last_name":"Redchenko"},{"full_name":"Rueda Sanchez, Alfredo R","first_name":"Alfredo R","last_name":"Rueda Sanchez","orcid":"0000-0001-6249-5860","id":"3B82B0F8-F248-11E8-B48F-1D18A9856A87"},{"full_name":"Hease, William J","first_name":"William J","last_name":"Hease","id":"29705398-F248-11E8-B48F-1D18A9856A87","orcid":"0000-0001-9868-2166"},{"id":"2AED110C-F248-11E8-B48F-1D18A9856A87","orcid":"0000-0001-6937-5773","last_name":"Hassani","full_name":"Hassani, Farid","first_name":"Farid"},{"id":"4B591CBA-F248-11E8-B48F-1D18A9856A87","orcid":"0000-0001-8112-028X","first_name":"Johannes M","full_name":"Fink, Johannes M","last_name":"Fink"}],"day":"08","project":[{"grant_number":"732894","name":"Hybrid Optomechanical Technologies","call_identifier":"H2020","_id":"257EB838-B435-11E9-9278-68D0E5697425"},{"name":"A Fiber Optic Transceiver for Superconducting Qubits","grant_number":"758053","_id":"26336814-B435-11E9-9278-68D0E5697425","call_identifier":"H2020"},{"call_identifier":"H2020","_id":"260C2330-B435-11E9-9278-68D0E5697425","grant_number":"754411","name":"ISTplus - Postdoctoral Fellowships"},{"call_identifier":"H2020","_id":"237CBA6C-32DE-11EA-91FC-C7463DDC885E","grant_number":"862644","name":"Quantum readout techniques and technologies"},{"_id":"2671EB66-B435-11E9-9278-68D0E5697425","name":"Coherent on-chip conversion of superconducting qubit signals from microwaves to optical frequencies"}],"related_material":{"record":[{"id":"13056","relation":"research_data","status":"public"}],"link":[{"relation":"erratum","url":"https://doi.org/10.1038/s41467-020-18912-9"},{"relation":"press_release","description":"News on IST Homepage","url":"https://ist.ac.at/en/news/how-to-transport-microwave-quantum-information-via-optical-fiber/"}]},"acknowledgement":"We thank Yuan Chen for performing supplementary FEM simulations and Andrew Higginbotham, Ralf Riedinger, Sungkun Hong, and Lorenzo Magrini for valuable discussions. This work was supported by IST Austria, the IST nanofabrication facility (NFF), the European Union’s Horizon 2020 research and innovation program under grant agreement no. 732894 (FET Proactive HOT) and the European Research Council under grant agreement no. 758053 (ERC StG QUNNECT). G.A. is the recipient of a DOC fellowship of the Austrian Academy of Sciences at IST Austria. W.H. is the recipient of an ISTplus postdoctoral fellowship with funding from the European Union’s Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement no. 754411. J.M.F. acknowledges support from the Austrian Science Fund (FWF) through BeyondC (F71), a NOMIS foundation research grant, and the EU’s Horizon 2020 research and innovation program under grant agreement no. 862644 (FET Open QUARTET).","ddc":["530"],"doi":"10.1038/s41467-020-18269-z","keyword":["General Biochemistry","Genetics and Molecular Biology","General Physics and Astronomy","General Chemistry"],"language":[{"iso":"eng"}],"article_processing_charge":"No","date_published":"2020-09-08T00:00:00Z","_id":"8529","abstract":[{"text":"Practical quantum networks require low-loss and noise-resilient optical interconnects as well as non-Gaussian resources for entanglement distillation and distributed quantum computation. The latter could be provided by superconducting circuits but existing solutions to interface the microwave and optical domains lack either scalability or efficiency, and in most cases the conversion noise is not known. In this work we utilize the unique opportunities of silicon photonics, cavity optomechanics and superconducting circuits to demonstrate a fully integrated, coherent transducer interfacing the microwave X and the telecom S bands with a total (internal) bidirectional transduction efficiency of 1.2% (135%) at millikelvin temperatures. The coupling relies solely on the radiation pressure interaction mediated by the femtometer-scale motion of two silicon nanobeams reaching a Vπ as low as 16 μV for sub-nanowatt pump powers. Without the associated optomechanical gain, we achieve a total (internal) pure conversion efficiency of up to 0.019% (1.6%), relevant for future noise-free operation on this qubit-compatible platform.","lang":"eng"}],"file":[{"checksum":"88f92544889eb18bb38e25629a422a86","date_updated":"2020-09-18T13:02:37Z","access_level":"open_access","file_name":"2020_NatureComm_Arnold.pdf","file_size":1002818,"creator":"dernst","date_created":"2020-09-18T13:02:37Z","success":1,"content_type":"application/pdf","relation":"main_file","file_id":"8530"}],"article_number":"4460","oa":1,"publication_status":"published","tmp":{"legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","image":"/images/cc_by.png","short":"CC BY (4.0)"},"volume":11,"file_date_updated":"2020-09-18T13:02:37Z","has_accepted_license":"1","oa_version":"Published Version","year":"2020","article_type":"original","acknowledged_ssus":[{"_id":"NanoFab"}],"publication_identifier":{"issn":["2041-1723"]},"external_id":{"isi":["000577280200001"]},"date_updated":"2024-08-07T07:11:51Z","user_id":"4359f0d1-fa6c-11eb-b949-802e58b17ae8"}]