[{"year":"2018","type":"journal_article","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift / galaxies: formation / dark ages / reionization / first stars / techniques: spectroscopic / intergalactic medium"],"day":"19","month":"11","publisher":"EDP Sciences","date_updated":"2024-10-14T11:31:36Z","language":[{"iso":"eng"}],"publication":"Astronomy & Astrophysics","article_processing_charge":"No","status":"public","article_number":"A136","external_id":{"arxiv":["1805.11621"]},"article_type":"original","volume":619,"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"acknowledgement":"JM acknowledges the award of a Huygens PhD fellowship from Leiden University. MG acknowledges support from NASA grant NNX17AK58G. APA, PhD::SPACE fellow, acknowledges support from the FCT through the fellowship PD/BD/52706/2014. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 294.A-5018, 098.A-0819, 099.A-0254 and 0100.A-0213. We are grateful for the excellent data-sets from the COSMOS and UltraVISTA survey teams. This research was supported by the Munich Institute for Astro- and Particle Physics (MIAPP) of the DFG cluster of excellence “Origin and Structure of the Universe”. We thank the referee for their comments that improved the paper. We also thank Christoph Behrens, Len Cowie, Koki Kakiichi, Peter Laursen, Charlotte Mason, Eros Vanzella, Lewis Weinberger and Johannes Zabl for discussions. We have benefited from the public available programming language Python, including the numpy, matplotlib, scipy and astropy packages (Hunter 2007; Astropy Collaboration 2013), the astronomical imaging tools Swarp (Bertin 2010) and ds9 and the Topcat analysis tool (Taylor 2013).","intvolume":" 619","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","arxiv":1,"citation":{"apa":"Matthee, J. J., Sobral, D., Gronke, M., Paulino-Afonso, A., Stefanon, M., & Röttgering, H. (2018). Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly contributing to the reionisation of the universe. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201833528","chicago":"Matthee, Jorryt J, David Sobral, Max Gronke, Ana Paulino-Afonso, Mauro Stefanon, and Huub Röttgering. “Confirmation of Double Peaked Lyα Emission at z = 6.593: Witnessing a Galaxy Directly Contributing to the Reionisation of the Universe.” Astronomy & Astrophysics. EDP Sciences, 2018. https://doi.org/10.1051/0004-6361/201833528.","mla":"Matthee, Jorryt J., et al. “Confirmation of Double Peaked Lyα Emission at z = 6.593: Witnessing a Galaxy Directly Contributing to the Reionisation of the Universe.” Astronomy & Astrophysics, vol. 619, A136, EDP Sciences, 2018, doi:10.1051/0004-6361/201833528.","short":"J.J. Matthee, D. Sobral, M. Gronke, A. Paulino-Afonso, M. Stefanon, H. Röttgering, Astronomy & Astrophysics 619 (2018).","ama":"Matthee JJ, Sobral D, Gronke M, Paulino-Afonso A, Stefanon M, Röttgering H. Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly contributing to the reionisation of the universe. Astronomy & Astrophysics. 2018;619. doi:10.1051/0004-6361/201833528","ieee":"J. J. Matthee, D. Sobral, M. Gronke, A. Paulino-Afonso, M. Stefanon, and H. Röttgering, “Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly contributing to the reionisation of the universe,” Astronomy & Astrophysics, vol. 619. EDP Sciences, 2018.","ista":"Matthee JJ, Sobral D, Gronke M, Paulino-Afonso A, Stefanon M, Röttgering H. 2018. Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly contributing to the reionisation of the universe. Astronomy & Astrophysics. 619, A136."},"oa":1,"date_published":"2018-11-19T00:00:00Z","scopus_import":"1","_id":"11508","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","first_name":"Jorryt J"},{"last_name":"Sobral","first_name":"David","full_name":"Sobral, David"},{"first_name":"Max","last_name":"Gronke","full_name":"Gronke, Max"},{"full_name":"Paulino-Afonso, Ana","last_name":"Paulino-Afonso","first_name":"Ana"},{"first_name":"Mauro","last_name":"Stefanon","full_name":"Stefanon, Mauro"},{"full_name":"Röttgering, Huub","first_name":"Huub","last_name":"Röttgering"}],"date_created":"2022-07-06T11:14:23Z","doi":"10.1051/0004-6361/201833528","extern":"1","title":"Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly contributing to the reionisation of the universe","oa_version":"Published Version","publication_status":"published","abstract":[{"lang":"eng","text":"Distant luminous Lyman-α emitters (LAEs) are excellent targets for spectroscopic observations of galaxies in the epoch of reionisation (EoR). We present deep high-resolution (R = 5000) VLT/X-shooter observations, along with an extensive collection of photometric data of COLA1, a proposed double peaked LAE at z = 6.6. We rule out the possibility that COLA1’s emission line is an [OII] doublet at z = 1.475 on the basis of i) the asymmetric red line-profile and flux ratio of the peaks (blue/red=0.31 ± 0.03) and ii) an unphysical [OII]/Hα ratio ([OII]/Hα > 22). We show that COLA1’s observed B-band flux is explained by a faint extended foreground LAE, for which we detect Lyα and [OIII] at z = 2.142. We thus conclude that COLA1 is a real double-peaked LAE at z = 6.593, the first discovered at z > 6. COLA1 is UV luminous (M1500 = −21.6 ± 0.3), has a high equivalent width (EW0,Lyα = 120−40+50 Å) and very compact Lyα emission (r50,Lyα = 0.33−0.04+0.07 kpc). Relatively weak inferred Hβ+[OIII] line-emission from Spitzer/IRAC indicates an extremely low metallicity of Z < 1/20 Z⊙ or reduced strength of nebular lines due to high escape of ionising photons. The small Lyα peak separation of 220 ± 20 km s−1 implies a low HI column density and an ionising photon escape fraction of ≈15 − 30%, providing the first direct evidence that such galaxies contribute actively to the reionisation of the Universe at z > 6. Based on simple estimates, we find that COLA1 could have provided just enough photons to reionise its own ≈0.3 pMpc (2.3 cMpc) bubble, allowing the blue Lyα line to be observed. However, we also discuss alternative scenarios explaining the detected double peaked nature of COLA1. Our results show that future high-resolution observations of statistical samples of double peaked LAEs at z > 5 are a promising probe of the occurrence of ionised regions around galaxies in the EoR."}],"quality_controlled":"1","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1805.11621"}]},{"title":"FliPer: A global measure of power density to estimate surface gravities of main-sequence solar-like stars and red giants","oa_version":"Preprint","publication_status":"published","abstract":[{"lang":"eng","text":"Asteroseismology provides global stellar parameters such as masses, radii, or surface gravities using mean global seismic parameters and effective temperature for thousands of low-mass stars (0.8 M⊙ < M < 3 M⊙). This methodology has been successfully applied to stars in which acoustic modes excited by turbulent convection are measured. Other methods such as the Flicker technique can also be used to determine stellar surface gravities, but only works for log g above 2.5 dex. In this work, we present a new metric called FliPer (Flicker in spectral power density, in opposition to the standard Flicker measurement which is computed in the time domain); it is able to extend the range for which reliable surface gravities can be obtained (0.1 < log g < 4.6 dex) without performing any seismic analysis for stars brighter than Kp < 14. FliPer takes into account the average variability of a star measured in the power density spectrum in a given range of frequencies. However, FliPer values calculated on several ranges of frequency are required to better characterize a star. Using a large set of asteroseismic targets it is possible to calibrate the behavior of surface gravity with FliPer through machine learning. This calibration made with a random forest regressor covers a wide range of surface gravities from main-sequence stars to subgiants and red giants, with very small uncertainties from 0.04 to 0.1 dex. FliPer values can be inserted in automatic global seismic pipelines to either give an estimation of the stellar surface gravity or to assess the quality of the seismic results by detecting any outliers in the obtained νmax values. FliPer also constrains the surface gravities of main-sequence dwarfs using only long-cadence data for which the Nyquist frequency is too low to measure the acoustic-mode properties."}],"quality_controlled":"1","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1809.05105"}],"volume":620,"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"article_type":"original","intvolume":" 620","acknowledgement":"We thank the anonymous referee for the very useful comments. We would also like to thank M. Benbakoura for his help in analyzing the light curves of several binary systems included in our set of stars. L.B. and R.A.G. acknowledge the support from PLATO and GOLF CNES grants. S.M. acknowledges support from the National Aeronautics and Space Administration under Grant NNX15AF13G, the National Science Foundation grant AST-1411685, and the Ramon y Cajal fellowship no. RYC-2015-17697. E.C. is funded by the European Union’s Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement no. 664931. O.J.H and B.M.R. acknowledge the support of the UK Science and Technology Facilities Council (STFC). Funding for the Stellar Astrophysics Centre is provided by the Danish National Research Foundation (Grant DNRF106). This research has made use of NASA’s Astrophysics Data System. Data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555.","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa":1,"date_published":"2018-12-01T00:00:00Z","citation":{"ieee":"L. A. Bugnet et al., “FliPer: A global measure of power density to estimate surface gravities of main-sequence solar-like stars and red giants,” Astronomy & Astrophysics, vol. 620. EDP Sciences, 2018.","ista":"Bugnet LA, García RA, Davies GR, Mathur S, Corsaro E, Hall OJ, Rendle BM. 2018. FliPer: A global measure of power density to estimate surface gravities of main-sequence solar-like stars and red giants. Astronomy & Astrophysics. 620, A38.","apa":"Bugnet, L. A., García, R. A., Davies, G. R., Mathur, S., Corsaro, E., Hall, O. J., & Rendle, B. M. (2018). FliPer: A global measure of power density to estimate surface gravities of main-sequence solar-like stars and red giants. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201833106","ama":"Bugnet LA, García RA, Davies GR, et al. FliPer: A global measure of power density to estimate surface gravities of main-sequence solar-like stars and red giants. Astronomy & Astrophysics. 2018;620. doi:10.1051/0004-6361/201833106","mla":"Bugnet, Lisa Annabelle, et al. “FliPer: A Global Measure of Power Density to Estimate Surface Gravities of Main-Sequence Solar-like Stars and Red Giants.” Astronomy & Astrophysics, vol. 620, A38, EDP Sciences, 2018, doi:10.1051/0004-6361/201833106.","short":"L.A. Bugnet, R.A. García, G.R. Davies, S. Mathur, E. Corsaro, O.J. Hall, B.M. Rendle, Astronomy & Astrophysics 620 (2018).","chicago":"Bugnet, Lisa Annabelle, R. A. García, G. R. Davies, S. Mathur, E. Corsaro, O. J. Hall, and B. M. Rendle. “FliPer: A Global Measure of Power Density to Estimate Surface Gravities of Main-Sequence Solar-like Stars and Red Giants.” Astronomy & Astrophysics. EDP Sciences, 2018. https://doi.org/10.1051/0004-6361/201833106."},"arxiv":1,"_id":"11618","scopus_import":"1","doi":"10.1051/0004-6361/201833106","author":[{"id":"d9edb345-f866-11ec-9b37-d119b5234501","full_name":"Bugnet, Lisa Annabelle","orcid":"0000-0003-0142-4000","last_name":"Bugnet","first_name":"Lisa Annabelle"},{"full_name":"García, R. A.","last_name":"García","first_name":"R. A."},{"first_name":"G. R.","last_name":"Davies","full_name":"Davies, G. R."},{"full_name":"Mathur, S.","last_name":"Mathur","first_name":"S."},{"full_name":"Corsaro, E.","last_name":"Corsaro","first_name":"E."},{"full_name":"Hall, O. J.","first_name":"O. J.","last_name":"Hall"},{"full_name":"Rendle, B. M.","last_name":"Rendle","first_name":"B. M."}],"extern":"1","date_created":"2022-07-18T14:37:39Z","date_updated":"2024-10-14T11:40:17Z","language":[{"iso":"eng"}],"publication":"Astronomy & Astrophysics","article_processing_charge":"No","status":"public","external_id":{"arxiv":["1809.05105"]},"article_number":"A38","year":"2018","type":"journal_article","keyword":["Space and Planetary Science","Astronomy and Astrophysics","asteroseismology / methods","data analysis / stars","oscillations"],"day":"01","month":"12","publisher":"EDP Sciences"},{"language":[{"iso":"eng"}],"date_updated":"2022-08-22T07:43:29Z","status":"public","article_number":"L10","external_id":{"arxiv":["1809.07573"]},"publication":"Astronomy & Astrophysics","article_processing_charge":"No","keyword":["Space and Planetary Science","Astronomy and Astrophysics","planetary systems / planets and satellites","detection / planets and satellites","fundamental parameters / planets and satellites","terrestrial planets / stars","fundamental parameters"],"year":"2018","type":"journal_article","month":"11","publisher":"EDP Sciences","day":"22","abstract":[{"text":"We report on the confirmation and mass determination of π Men c, the first transiting planet discovered by NASA’s TESS space mission. π Men is a naked-eye (V = 5.65 mag), quiet G0 V star that was previously known to host a sub-stellar companion (π Men b) on a longperiod (Porb = 2091 days), eccentric (e = 0.64) orbit. Using TESS time-series photometry, combined with Gaia data, published UCLES at AAT Doppler measurements, and archival HARPS at ESO-3.6m radial velocities, we found that π Men c is a close-in planet with an orbital period of Porb = 6.27 days, a mass of Mc = 4.52 ± 0.81 M⊕, and a radius of Rc = 2.06 ± 0.03 R⊕. Based on the planet’s orbital period and size, π Men c is a super-Earth located at, or close to, the radius gap, while its mass and bulk density suggest it may have held on to a significant atmosphere. Because of the brightness of the host star, this system is highly suitable for a wide range of further studies to characterize the planetary atmosphere and dynamical properties. We also performed an asteroseismic analysis of the TESS data and detected a hint of power excess consistent with the seismic values expected for this star, although this result depends on the photometric aperture used to extract the light curve. This marginal detection is expected from pre-launch simulations hinting at the asteroseismic potential of the TESS mission for longer, multi-sector observations and/or for more evolved bright stars.","lang":"eng"}],"oa_version":"Preprint","title":"TESS’s first planet: A super-Earth transiting the naked-eye star π Mensae","publication_status":"published","main_file_link":[{"url":"https://arxiv.org/abs/1809.07573","open_access":"1"}],"quality_controlled":"1","intvolume":" 619","article_type":"letter_note","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"volume":619,"scopus_import":"1","_id":"11619","author":[{"full_name":"Gandolfi, D.","first_name":"D.","last_name":"Gandolfi"},{"full_name":"Barragán, O.","last_name":"Barragán","first_name":"O."},{"full_name":"Livingston, J. H.","first_name":"J. H.","last_name":"Livingston"},{"full_name":"Fridlund, M.","first_name":"M.","last_name":"Fridlund"},{"full_name":"Justesen, A. B.","last_name":"Justesen","first_name":"A. B."},{"last_name":"Redfield","first_name":"S.","full_name":"Redfield, S."},{"first_name":"L.","last_name":"Fossati","full_name":"Fossati, L."},{"full_name":"Mathur, S.","first_name":"S.","last_name":"Mathur"},{"first_name":"S.","last_name":"Grziwa","full_name":"Grziwa, S."},{"full_name":"Cabrera, J.","last_name":"Cabrera","first_name":"J."},{"first_name":"R. A.","last_name":"García","full_name":"García, R. A."},{"full_name":"Persson, C. M.","last_name":"Persson","first_name":"C. M."},{"full_name":"Van Eylen, V.","last_name":"Van Eylen","first_name":"V."},{"last_name":"Hatzes","first_name":"A. P.","full_name":"Hatzes, A. P."},{"full_name":"Hidalgo, D.","first_name":"D.","last_name":"Hidalgo"},{"last_name":"Albrecht","first_name":"S.","full_name":"Albrecht, S."},{"first_name":"Lisa Annabelle","orcid":"0000-0003-0142-4000","last_name":"Bugnet","full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501"},{"full_name":"Cochran, W. D.","last_name":"Cochran","first_name":"W. D."},{"first_name":"Sz.","last_name":"Csizmadia","full_name":"Csizmadia, Sz."},{"full_name":"Deeg, H.","last_name":"Deeg","first_name":"H."},{"full_name":"Eigmüller, Ph.","last_name":"Eigmüller","first_name":"Ph."},{"last_name":"Endl","first_name":"M.","full_name":"Endl, M."},{"full_name":"Erikson, A.","first_name":"A.","last_name":"Erikson"},{"last_name":"Esposito","first_name":"M.","full_name":"Esposito, M."},{"full_name":"Guenther, E.","first_name":"E.","last_name":"Guenther"},{"last_name":"Korth","first_name":"J.","full_name":"Korth, J."},{"full_name":"Luque, R.","first_name":"R.","last_name":"Luque"},{"full_name":"Montañes Rodríguez, P.","first_name":"P.","last_name":"Montañes Rodríguez"},{"full_name":"Nespral, D.","first_name":"D.","last_name":"Nespral"},{"full_name":"Nowak, G.","last_name":"Nowak","first_name":"G."},{"first_name":"M.","last_name":"Pätzold","full_name":"Pätzold, M."},{"full_name":"Prieto-Arranz, J.","first_name":"J.","last_name":"Prieto-Arranz"}],"doi":"10.1051/0004-6361/201834289","extern":"1","date_created":"2022-07-18T14:41:16Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"mla":"Gandolfi, D., et al. “TESS’s First Planet: A Super-Earth Transiting the Naked-Eye Star π Mensae.” Astronomy & Astrophysics, vol. 619, L10, EDP Sciences, 2018, doi:10.1051/0004-6361/201834289.","chicago":"Gandolfi, D., O. Barragán, J. H. Livingston, M. Fridlund, A. B. Justesen, S. Redfield, L. Fossati, et al. “TESS’s First Planet: A Super-Earth Transiting the Naked-Eye Star π Mensae.” Astronomy & Astrophysics. EDP Sciences, 2018. https://doi.org/10.1051/0004-6361/201834289.","short":"D. Gandolfi, O. Barragán, J.H. Livingston, M. Fridlund, A.B. Justesen, S. Redfield, L. Fossati, S. Mathur, S. Grziwa, J. Cabrera, R.A. García, C.M. Persson, V. Van Eylen, A.P. Hatzes, D. Hidalgo, S. Albrecht, L.A. Bugnet, W.D. Cochran, S. Csizmadia, H. Deeg, P. Eigmüller, M. Endl, A. Erikson, M. Esposito, E. Guenther, J. Korth, R. Luque, P. Montañes Rodríguez, D. Nespral, G. Nowak, M. Pätzold, J. Prieto-Arranz, Astronomy & Astrophysics 619 (2018).","ama":"Gandolfi D, Barragán O, Livingston JH, et al. TESS’s first planet: A super-Earth transiting the naked-eye star π Mensae. Astronomy & Astrophysics. 2018;619. doi:10.1051/0004-6361/201834289","apa":"Gandolfi, D., Barragán, O., Livingston, J. H., Fridlund, M., Justesen, A. B., Redfield, S., … Prieto-Arranz, J. (2018). TESS’s first planet: A super-Earth transiting the naked-eye star π Mensae. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201834289","ista":"Gandolfi D, Barragán O, Livingston JH, Fridlund M, Justesen AB, Redfield S, Fossati L, Mathur S, Grziwa S, Cabrera J, García RA, Persson CM, Van Eylen V, Hatzes AP, Hidalgo D, Albrecht S, Bugnet LA, Cochran WD, Csizmadia S, Deeg H, Eigmüller P, Endl M, Erikson A, Esposito M, Guenther E, Korth J, Luque R, Montañes Rodríguez P, Nespral D, Nowak G, Pätzold M, Prieto-Arranz J. 2018. TESS’s first planet: A super-Earth transiting the naked-eye star π Mensae. Astronomy & Astrophysics. 619, L10.","ieee":"D. Gandolfi et al., “TESS’s first planet: A super-Earth transiting the naked-eye star π Mensae,” Astronomy & Astrophysics, vol. 619. EDP Sciences, 2018."},"arxiv":1,"oa":1,"date_published":"2018-11-22T00:00:00Z"},{"external_id":{"arxiv":["1811.12140"]},"article_number":"1811.12140","status":"public","main_file_link":[{"url":" https://doi.org/10.48550/arXiv.1811.12140","open_access":"1"}],"article_processing_charge":"No","publication":"arXiv","language":[{"iso":"eng"}],"abstract":[{"text":"The recently launched NASA Transiting Exoplanet Survey Satellite (TESS) mission is going to collect lightcurves for a few hundred million of stars and we expect to increase the number of pulsating stars to analyze compared to the few thousand stars observed by the CoRoT, Kepler and K2 missions. However, most of the TESS targets have not yet been properly classified and characterized. In order to improve the analysis of the TESS data, it is crucial to determine the type of stellar pulsations in a timely manner. We propose an automatic method to classify stars attending to their pulsation properties, in particular, to identify solar-like pulsators among all TESS targets. It relies on the use of the global amount of power contained in the power spectrum (already known as the FliPer method) as a key parameter, along with\r\nthe effective temperature, to feed into a machine learning classifier. Our study, based on TESS simulated datasets, shows that we are able to classify pulsators with a 98% accuracy.","lang":"eng"}],"publication_status":"submitted","date_updated":"2022-08-22T08:41:55Z","oa_version":"Preprint","title":"FliPer: Classifying TESS pulsating stars","extern":"1","author":[{"full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","first_name":"Lisa Annabelle","last_name":"Bugnet","orcid":"0000-0003-0142-4000"},{"full_name":"García, R. A.","first_name":"R. A.","last_name":"García"},{"full_name":"Davies, G. R.","last_name":"Davies","first_name":"G. R."},{"full_name":"Mathur, S.","last_name":"Mathur","first_name":"S."},{"full_name":"Hall, O. J.","last_name":"Hall","first_name":"O. J."},{"full_name":"Rendle, B. M.","first_name":"B. M.","last_name":"Rendle"}],"doi":"10.48550/arXiv.1811.12140","date_created":"2022-07-21T07:05:23Z","_id":"11631","month":"11","oa":1,"date_published":"2018-11-29T00:00:00Z","arxiv":1,"citation":{"apa":"Bugnet, L. A., García, R. A., Davies, G. R., Mathur, S., Hall, O. J., & Rendle, B. M. (n.d.). FliPer: Classifying TESS pulsating stars. arXiv. https://doi.org/10.48550/arXiv.1811.12140","mla":"Bugnet, Lisa Annabelle, et al. “FliPer: Classifying TESS Pulsating Stars.” ArXiv, 1811.12140, doi:10.48550/arXiv.1811.12140.","chicago":"Bugnet, Lisa Annabelle, R. A. García, G. R. Davies, S. Mathur, O. J. Hall, and B. M. Rendle. “FliPer: Classifying TESS Pulsating Stars.” ArXiv, n.d. https://doi.org/10.48550/arXiv.1811.12140.","short":"L.A. Bugnet, R.A. García, G.R. Davies, S. Mathur, O.J. Hall, B.M. Rendle, ArXiv (n.d.).","ama":"Bugnet LA, García RA, Davies GR, Mathur S, Hall OJ, Rendle BM. FliPer: Classifying TESS pulsating stars. arXiv. doi:10.48550/arXiv.1811.12140","ieee":"L. A. Bugnet, R. A. García, G. R. Davies, S. Mathur, O. J. Hall, and B. M. Rendle, “FliPer: Classifying TESS pulsating stars,” arXiv. .","ista":"Bugnet LA, García RA, Davies GR, Mathur S, Hall OJ, Rendle BM. FliPer: Classifying TESS pulsating stars. arXiv, 1811.12140."},"day":"29","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","keyword":["asteroseismology - methods","data analysis - stars","oscillations"],"type":"preprint","year":"2018"},{"main_file_link":[{"url":"https://arxiv.org/abs/1709.06569","open_access":"1"}],"quality_controlled":"1","abstract":[{"text":"We present spectroscopic follow-up observations of CR7 with ALMA, targeted at constraining the infrared (IR) continuum and [C II]158 mm line-emission at high spatial resolution matched to the HST/WFC3 imaging. CR7 is a luminous Lyα emitting galaxy at z = 6.6 that consists of three separated UV-continuum components. Our observations reveal several well-separated components of [C II] emission. The two most luminous components in [C II] coincide with the brightest UV components (A and B), blueshifted by »150 km s−1 with respect to the\r\npeak of Lyα emission. Other [C II] components are observed close to UV clumps B and C and are blueshifted by »300 and ≈80 km s−1 with respect to the systemic redshift. We do not detect FIR continuum emission due to dust with a 3σ limiting luminosity LIR T L d 35 K 3.1 10 = <´ 10 ( ) . This allows us to mitigate uncertainties in the dust-corrected SFR and derive SFRs for the three UV clumps A, B, and C of 28, 5, and 7 M yr−1. All clumps have [C II] luminosities consistent within the scatter observed in the local relation between SFR and L[ ] C II , implying that strong Lyα emission does not necessarily anti-correlate with [C II] luminosity. Combining\r\nour measurements with the literature, we show that galaxies with blue UV slopes have weaker [C II] emission at fixed SFR, potentially due to their lower metallicities and/or higher photoionization. Comparison with hydrodynamical simulations suggests that CR7ʼs clumps have metallicities of 0.1 Z Z 0.2 < < . The observed ISM structure of CR7 indicates that we are likely witnessing the build up of a central galaxy in the early universe through complex accretion of satellites.","lang":"eng"}],"publication_status":"published","oa_version":"Preprint","title":"ALMA reveals metals yet no dust within multiple components in CR7","extern":"1","doi":"10.3847/1538-4357/aa9931","date_created":"2022-07-07T08:48:04Z","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J"},{"full_name":"Sobral, D.","last_name":"Sobral","first_name":"D."},{"full_name":"Boone, F.","first_name":"F.","last_name":"Boone"},{"last_name":"Röttgering","first_name":"H.","full_name":"Röttgering, H."},{"last_name":"Schaerer","first_name":"D.","full_name":"Schaerer, D."},{"first_name":"M.","last_name":"Girard","full_name":"Girard, M."},{"full_name":"Pallottini, A.","first_name":"A.","last_name":"Pallottini"},{"full_name":"Vallini, L.","last_name":"Vallini","first_name":"L."},{"full_name":"Ferrara, A.","last_name":"Ferrara","first_name":"A."},{"last_name":"Darvish","first_name":"B.","full_name":"Darvish, B."},{"full_name":"Mobasher, B.","first_name":"B.","last_name":"Mobasher"}],"scopus_import":"1","_id":"11518","citation":{"ieee":"J. J. Matthee et al., “ALMA reveals metals yet no dust within multiple components in CR7,” The Astrophysical Journal, vol. 851, no. 2. IOP Publishing, 2017.","ista":"Matthee JJ, Sobral D, Boone F, Röttgering H, Schaerer D, Girard M, Pallottini A, Vallini L, Ferrara A, Darvish B, Mobasher B. 2017. ALMA reveals metals yet no dust within multiple components in CR7. The Astrophysical Journal. 851(2), 145.","apa":"Matthee, J. J., Sobral, D., Boone, F., Röttgering, H., Schaerer, D., Girard, M., … Mobasher, B. (2017). ALMA reveals metals yet no dust within multiple components in CR7. The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/aa9931","short":"J.J. Matthee, D. Sobral, F. Boone, H. Röttgering, D. Schaerer, M. Girard, A. Pallottini, L. Vallini, A. Ferrara, B. Darvish, B. Mobasher, The Astrophysical Journal 851 (2017).","chicago":"Matthee, Jorryt J, D. Sobral, F. Boone, H. Röttgering, D. Schaerer, M. Girard, A. Pallottini, et al. “ALMA Reveals Metals yet No Dust within Multiple Components in CR7.” The Astrophysical Journal. IOP Publishing, 2017. https://doi.org/10.3847/1538-4357/aa9931.","mla":"Matthee, Jorryt J., et al. “ALMA Reveals Metals yet No Dust within Multiple Components in CR7.” The Astrophysical Journal, vol. 851, no. 2, 145, IOP Publishing, 2017, doi:10.3847/1538-4357/aa9931.","ama":"Matthee JJ, Sobral D, Boone F, et al. ALMA reveals metals yet no dust within multiple components in CR7. The Astrophysical Journal. 2017;851(2). doi:10.3847/1538-4357/aa9931"},"arxiv":1,"date_published":"2017-12-21T00:00:00Z","oa":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","acknowledgement":"We thank the referee for their constructive comments, which have helped improve the quality and clarity of this work. We thank Raffaella Schneider for comments on an earlier version of this paper. We thank Leindert Boogaard, Steven Bos, Rychard Bouwens, and Renske Smit for discussions. J.M. acknowledges the support of a Huygens PhD fellowship from Leiden University. D.S. acknowledges financial support from the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship and from Lancaster University through an Early Career Internal Grant A100679. A.F. acknowledges support from the ERC Advanced Grant INTERSTELLAR H2020/740120. B.D. acknowledges financial support from NASA through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 294.A-5018. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2015.1.00122.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ.","intvolume":" 851","article_type":"original","volume":851,"publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"article_number":"145","external_id":{"arxiv":["1709.06569"]},"status":"public","article_processing_charge":"No","publication":"The Astrophysical Journal","language":[{"iso":"eng"}],"date_updated":"2024-10-14T11:32:14Z","publisher":"IOP Publishing","month":"12","day":"21","issue":"2","keyword":["Space and Planetary Science","Astronomy and Astrophysics","dark ages","reionization","first stars – galaxies: formation – galaxies: high-redshift – galaxies: ISM – galaxies: kinematics and dynamics"],"type":"journal_article","year":"2017"},{"abstract":[{"lang":"eng","text":"We study the production rate of ionizing photons of a sample of 588 Hα emitters (HAEs) and 160 Lyman-α emitters (LAEs) at z = 2.2 in the COSMOS field in order to assess the implied emissivity from galaxies, based on their ultraviolet (UV) luminosity. By exploring the rest-frame Lyman Continuum (LyC) with GALEX/NUV data, we find fesc < 2.8 (6.4) per cent through median (mean) stacking. By combining the Hα luminosity density with intergalactic medium emissivity measurements from absorption studies, we find a globally averaged 〈fesc〉 of 5.9+14.5−4.2 per cent at z = 2.2 if we assume HAEs are the only source of ionizing photons. We find similarly low values of the global 〈fesc〉 at z ≈ 3–5, also ruling out a high 〈fesc〉 at z < 5. These low escape fractions allow us to measure ξion, the number of produced ionizing photons per unit UV luminosity, and investigate how this depends on galaxy properties. We find a typical ξion ≈ 1024.77 ± 0.04 Hz erg−1 for HAEs and ξion ≈ 1025.14 ± 0.09 Hz erg−1 for LAEs. LAEs and low-mass HAEs at z = 2.2 show similar values of ξion as typically assumed in the reionization era, while the typical HAE is three times less ionizing. Due to an increasing ξion with increasing EW(Hα), ξion likely increases with redshift. This evolution alone is fully in line with the observed evolution of ξion between z ≈ 2 and 5, indicating a typical value of ξion ≈ 1025.4 Hz erg−1 in the reionization era."}],"publication_status":"published","title":"The production and escape of Lyman-Continuum radiation from star-forming galaxies at z ∼ 2 and their redshift evolution","oa_version":"Preprint","page":"3637-3655","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1605.08782"}],"quality_controlled":"1","acknowledgement":"We thank the referee for the many helpful and constructive comments which have significantly improved this paper. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. DS acknowledges financial support from the Netherlands Organization for Scientific research (NWO) through a Veni fellowship and from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010). PNB is grateful for support from the UK STFC via grant ST/M001229/1. IO acknowledges support from the European Research Council in the form of the Advanced Investigator Programme, 321302, COSMICISM. The authors thank Andreas Faisst, Michael Rutkowski and Andreas Sandberg for answering questions related to this work and Daniel Schaerer and Mark Dijkstra for discussions. We acknowledge the work that has been done by both the COSMOS team in assembling such large, state-of-the-art multi-wavelength data set, as this has been crucial for the results presented in this paper. We have benefited greatly from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY (Jones et al. 2001; Hunter 2007; Van Der Walt, Colbert & Varoquaux 2011) and ASTROPY (Astropy Collaboration et al. 2013) packages, the astronomical imaging tools SEXTRACTOR and SWARP (Bertin & Arnouts 1996;\r\nBertin 2010) and the TOPCAT analysis program (Taylor 2013).","intvolume":" 465","article_type":"original","volume":465,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"author":[{"first_name":"Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"first_name":"David","last_name":"Sobral","full_name":"Sobral, David"},{"full_name":"Best, Philip","first_name":"Philip","last_name":"Best"},{"full_name":"Khostovan, Ali Ahmad","first_name":"Ali Ahmad","last_name":"Khostovan"},{"full_name":"Oteo, Iván","last_name":"Oteo","first_name":"Iván"},{"full_name":"Bouwens, Rychard","first_name":"Rychard","last_name":"Bouwens"},{"first_name":"Huub","last_name":"Röttgering","full_name":"Röttgering, Huub"}],"doi":"10.1093/mnras/stw2973","extern":"1","date_created":"2022-07-12T12:12:14Z","scopus_import":"1","_id":"11564","arxiv":1,"citation":{"apa":"Matthee, J. J., Sobral, D., Best, P., Khostovan, A. A., Oteo, I., Bouwens, R., & Röttgering, H. (2017). The production and escape of Lyman-Continuum radiation from star-forming galaxies at z ∼ 2 and their redshift evolution. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stw2973","ama":"Matthee JJ, Sobral D, Best P, et al. The production and escape of Lyman-Continuum radiation from star-forming galaxies at z ∼ 2 and their redshift evolution. Monthly Notices of the Royal Astronomical Society. 2017;465(3):3637-3655. doi:10.1093/mnras/stw2973","short":"J.J. Matthee, D. Sobral, P. Best, A.A. Khostovan, I. Oteo, R. Bouwens, H. Röttgering, Monthly Notices of the Royal Astronomical Society 465 (2017) 3637–3655.","mla":"Matthee, Jorryt J., et al. “The Production and Escape of Lyman-Continuum Radiation from Star-Forming Galaxies at z ∼ 2 and Their Redshift Evolution.” Monthly Notices of the Royal Astronomical Society, vol. 465, no. 3, Oxford University Press, 2017, pp. 3637–55, doi:10.1093/mnras/stw2973.","chicago":"Matthee, Jorryt J, David Sobral, Philip Best, Ali Ahmad Khostovan, Iván Oteo, Rychard Bouwens, and Huub Röttgering. “The Production and Escape of Lyman-Continuum Radiation from Star-Forming Galaxies at z ∼ 2 and Their Redshift Evolution.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2017. https://doi.org/10.1093/mnras/stw2973.","ieee":"J. J. Matthee et al., “The production and escape of Lyman-Continuum radiation from star-forming galaxies at z ∼ 2 and their redshift evolution,” Monthly Notices of the Royal Astronomical Society, vol. 465, no. 3. Oxford University Press, pp. 3637–3655, 2017.","ista":"Matthee JJ, Sobral D, Best P, Khostovan AA, Oteo I, Bouwens R, Röttgering H. 2017. The production and escape of Lyman-Continuum radiation from star-forming galaxies at z ∼ 2 and their redshift evolution. Monthly Notices of the Royal Astronomical Society. 465(3), 3637–3655."},"date_published":"2017-03-01T00:00:00Z","oa":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"date_updated":"2024-10-14T11:35:49Z","external_id":{"arxiv":["1605.08782"]},"status":"public","article_processing_charge":"No","publication":"Monthly Notices of the Royal Astronomical Society","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","cosmology: observations","dark ages","reionization","first stars"],"type":"journal_article","year":"2017","publisher":"Oxford University Press","month":"03","day":"01","issue":"3"},{"intvolume":" 472","acknowledgement":"We thank the referee for a constructive report that has improved the quality and clarity of this work. The authors thank Grecco Oyarzún for discussions. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. DS acknowledges financial support from the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship and from Lancaster University through an Early Career Internal Grant A100679. BD acknowledges financial support from NASA through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G. We thank Kasper Schmidt for providing measurements. Based on observations with the W.M. Keck Observatory through programme C267D. The W.M. Keck Observatory is operated as a scientific partnership amongst the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 097.A-0943, 294.A 5018 and 098.A-0819 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. The authors acknowledge the award of observing time (W16AN004) and of service time (SW2014b20) on the William Herschel Telescope (WHT). WHT and its service programme are operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. Based on observations made with the NASA/ESA HST, obtained (from the Data Archive) at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with programme #14699. We are grateful for the excellent data sets from the COSMOS, UltraVISTA, SXDS, UDS and CFHTLS survey teams; without these legacy surveys, this research would have been impossible. We have benefited from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY and ASTROPY packages, the astronomical imaging tools SEXTRACTOR, SWARP and SCAMP and the TOPCAT analysis tool (Taylor 2013).","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"volume":472,"article_type":"original","_id":"11572","scopus_import":"1","doi":"10.1093/mnras/stx2061","date_created":"2022-07-13T09:47:39Z","extern":"1","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","first_name":"Jorryt J"},{"full_name":"Sobral, David","first_name":"David","last_name":"Sobral"},{"full_name":"Darvish, Behnam","last_name":"Darvish","first_name":"Behnam"},{"first_name":"Sérgio","last_name":"Santos","full_name":"Santos, Sérgio"},{"last_name":"Mobasher","first_name":"Bahram","full_name":"Mobasher, Bahram"},{"last_name":"Paulino-Afonso","first_name":"Ana","full_name":"Paulino-Afonso, Ana"},{"full_name":"Röttgering, Huub","last_name":"Röttgering","first_name":"Huub"},{"full_name":"Alegre, Lara","last_name":"Alegre","first_name":"Lara"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa":1,"date_published":"2017-11-01T00:00:00Z","arxiv":1,"citation":{"apa":"Matthee, J. J., Sobral, D., Darvish, B., Santos, S., Mobasher, B., Paulino-Afonso, A., … Alegre, L. (2017). Spectroscopic properties of luminous Ly α emitters at z ≈ 6–7 and comparison to the Lyman-break population. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stx2061","chicago":"Matthee, Jorryt J, David Sobral, Behnam Darvish, Sérgio Santos, Bahram Mobasher, Ana Paulino-Afonso, Huub Röttgering, and Lara Alegre. “Spectroscopic Properties of Luminous Ly α Emitters at z ≈ 6–7 and Comparison to the Lyman-Break Population.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2017. https://doi.org/10.1093/mnras/stx2061.","short":"J.J. Matthee, D. Sobral, B. Darvish, S. Santos, B. Mobasher, A. Paulino-Afonso, H. Röttgering, L. Alegre, Monthly Notices of the Royal Astronomical Society 472 (2017) 772–787.","mla":"Matthee, Jorryt J., et al. “Spectroscopic Properties of Luminous Ly α Emitters at z ≈ 6–7 and Comparison to the Lyman-Break Population.” Monthly Notices of the Royal Astronomical Society, vol. 472, no. 1, Oxford University Press, 2017, pp. 772–87, doi:10.1093/mnras/stx2061.","ama":"Matthee JJ, Sobral D, Darvish B, et al. Spectroscopic properties of luminous Ly α emitters at z ≈ 6–7 and comparison to the Lyman-break population. Monthly Notices of the Royal Astronomical Society. 2017;472(1):772-787. doi:10.1093/mnras/stx2061","ieee":"J. J. Matthee et al., “Spectroscopic properties of luminous Ly α emitters at z ≈ 6–7 and comparison to the Lyman-break population,” Monthly Notices of the Royal Astronomical Society, vol. 472, no. 1. Oxford University Press, pp. 772–787, 2017.","ista":"Matthee JJ, Sobral D, Darvish B, Santos S, Mobasher B, Paulino-Afonso A, Röttgering H, Alegre L. 2017. Spectroscopic properties of luminous Ly α emitters at z ≈ 6–7 and comparison to the Lyman-break population. Monthly Notices of the Royal Astronomical Society. 472(1), 772–787."},"abstract":[{"text":"We present spectroscopic follow-up of candidate luminous Ly α emitters (LAEs) at z = 5.7–6.6 in the SA22 field with VLT/X-SHOOTER. We confirm two new luminous LAEs at z = 5.676 (SR6) and z = 6.532 (VR7), and also present HST follow-up of both sources. These sources have luminosities LLy α ≈ 3 × 1043 erg s−1, very high rest-frame equivalent widths of EW0 ≳ 200 Å and narrow Ly α lines (200–340 km s−1). VR7 is the most UV-luminous LAE at z > 6.5, with M1500 = −22.5, even brighter in the UV than CR7. Besides Ly α, we do not detect any other rest-frame UV lines in the spectra of SR6 and VR7, and argue that rest-frame UV lines are easier to observe in bright galaxies with low Ly α equivalent widths. We confirm that Ly α line widths increase with Ly α luminosity at z = 5.7, while there are indications that Ly α lines of faint LAEs become broader at z = 6.6, potentially due to reionization. We find a large spread of up to 3 dex in UV luminosity for >L⋆ LAEs, but find that the Ly α luminosity of the brightest LAEs is strongly related to UV luminosity at z = 6.6. Under basic assumptions, we find that several LAEs at z ≈ 6–7 have Ly α escape fractions ≳ 100 per cent, indicating bursty star formation histories, alternative Ly α production mechanisms, or dust attenuating Ly α emission differently than UV emission. Finally, we present a method to compute ξion, the production efficiency of ionizing photons, and find that LAEs at z ≈ 6–7 have high values of log10(ξion/Hz erg−1) ≈ 25.51 ± 0.09 that may alleviate the need for high Lyman-Continuum escape fractions required for reionization.","lang":"eng"}],"title":"Spectroscopic properties of luminous Ly α emitters at z ≈ 6–7 and comparison to the Lyman-break population","oa_version":"Preprint","publication_status":"published","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1706.06591"}],"page":"772-787","quality_controlled":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution – galaxies: high-redshift","dark ages","reionization","first stars","cosmology: observations"],"year":"2017","type":"journal_article","month":"11","publisher":"Oxford University Press","day":"01","issue":"1","language":[{"iso":"eng"}],"date_updated":"2024-10-14T11:36:26Z","status":"public","external_id":{"arxiv":["1706.06591"]},"publication":"Monthly Notices of the Royal Astronomical Society","article_processing_charge":"No"},{"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","day":"08","arxiv":1,"citation":{"ama":"Bugnet LA, Garcia RA, Davies GR, Mathur S, Corsaro E. FliPer: Checking the reliability of global seismic parameters from automatic pipelines. arXiv. doi:10.48550/arXiv.1711.02890","chicago":"Bugnet, Lisa Annabelle, R. A. Garcia, G. R. Davies, S. Mathur, and E. Corsaro. “FliPer: Checking the Reliability of Global Seismic Parameters from Automatic Pipelines.” ArXiv, n.d. https://doi.org/10.48550/arXiv.1711.02890.","short":"L.A. Bugnet, R.A. Garcia, G.R. Davies, S. Mathur, E. Corsaro, ArXiv (n.d.).","mla":"Bugnet, Lisa Annabelle, et al. “FliPer: Checking the Reliability of Global Seismic Parameters from Automatic Pipelines.” ArXiv, 1711.02890, doi:10.48550/arXiv.1711.02890.","apa":"Bugnet, L. A., Garcia, R. A., Davies, G. R., Mathur, S., & Corsaro, E. (n.d.). FliPer: Checking the reliability of global seismic parameters from automatic pipelines. arXiv. https://doi.org/10.48550/arXiv.1711.02890","ista":"Bugnet LA, Garcia RA, Davies GR, Mathur S, Corsaro E. FliPer: Checking the reliability of global seismic parameters from automatic pipelines. arXiv, 1711.02890.","ieee":"L. A. Bugnet, R. A. Garcia, G. R. Davies, S. Mathur, and E. Corsaro, “FliPer: Checking the reliability of global seismic parameters from automatic pipelines,” arXiv. ."},"date_published":"2017-11-08T00:00:00Z","oa":1,"month":"11","_id":"11633","doi":"10.48550/arXiv.1711.02890","extern":"1","author":[{"id":"d9edb345-f866-11ec-9b37-d119b5234501","full_name":"Bugnet, Lisa Annabelle","last_name":"Bugnet","orcid":"0000-0003-0142-4000","first_name":"Lisa Annabelle"},{"last_name":"Garcia","first_name":"R. A.","full_name":"Garcia, R. A."},{"full_name":"Davies, G. R.","last_name":"Davies","first_name":"G. R."},{"full_name":"Mathur, S.","first_name":"S.","last_name":"Mathur"},{"last_name":"Corsaro","first_name":"E.","full_name":"Corsaro, E."}],"date_created":"2022-07-21T07:13:13Z","year":"2017","type":"preprint","keyword":["asteroseismology - methods","data analysis - stars","oscillations"],"publication":"arXiv","article_processing_charge":"No","status":"public","main_file_link":[{"open_access":"1","url":"https://doi.org/10.48550/arXiv.1711.02890"}],"article_number":"1711.02890","external_id":{"arxiv":["1711.02890"]},"title":"FliPer: Checking the reliability of global seismic parameters from automatic pipelines","oa_version":"Preprint","date_updated":"2022-08-22T08:45:42Z","publication_status":"submitted","abstract":[{"lang":"eng","text":"Our understanding of stars through asteroseismic data analysis is limited by our ability to take advantage of the huge amount of observed stars provided by space missions such as CoRoT, Kepler , K2, and soon TESS and PLATO. Global seismic pipelines provide global stellar parameters such as mass and radius using the mean seismic parameters, as well as the effective temperature. These pipelines are commonly used automatically on thousands of stars observed by K2 for 3 months (and soon TESS for at least ∼ 1 month). However, pipelines are not immune from misidentifying noise peaks and stellar oscillations. Therefore, new validation techniques are required to assess the quality of these results. We present a new metric called FliPer (Flicker in Power), which takes into account the average variability at all measured time scales. The proper calibration of FliPer enables us to obtain good estimations of global stellar parameters such as surface gravity that are robust against the influence of noise peaks and hence are an excellent way to find faults in asteroseismic pipelines."}],"language":[{"iso":"eng"}]},{"article_processing_charge":"No","publication":"Monthly Notices of the Royal Astronomical Society","external_id":{"arxiv":["1606.07435"]},"status":"public","date_updated":"2022-08-19T08:09:54Z","language":[{"iso":"eng"}],"issue":"2","day":"01","publisher":"Oxford University Press","month":"12","type":"journal_article","year":"2016","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift","galaxies: luminosity function","mass function","cosmology: observations","dark ages","reionization","first stars"],"quality_controlled":"1","page":"1678-1691","main_file_link":[{"url":"https://arxiv.org/abs/1606.07435","open_access":"1"}],"publication_status":"published","title":"The Lyα luminosity function at z= 5.7–6.6 and the steep drop of the faint end: Implications for reionization","oa_version":"Preprint","abstract":[{"text":"We present new results from the widest narrow-band survey search for Lyα emitters at z = 5.7, just after reionization. We survey a total of 7 deg2 spread over the COSMOS, UDS and SA22 fields. We find over 11 000 line emitters, out of which 514 are robust Lyα candidates at z = 5.7 within a volume of 6.3 × 106 Mpc3. Our Lyα emitters span a wide range in Lyα luminosities, from faint to bright (LLyα ∼ 1042.5–44 erg s−1) and rest-frame equivalent widths (EW0 ∼ 25–1000 Å) in a single, homogeneous data set. By combining all our fields, we find that the faint end slope of the z = 5.7 Lyα luminosity function is very steep, with α=−2.3+0.4−0.3. We also present an updated z = 6.6 Lyα luminosity function, based on comparable volumes and obtained with the same methods, which we directly compare with that at z = 5.7. We find a significant decline of the number density of faint Lyα emitters from z = 5.7 to 6.6 (by 0.5 ± 0.1 dex), but no evolution at the bright end/no evolution in L*. Faint Lyα emitters at z = 6.6 show much more extended haloes than those at z = 5.7, suggesting that neutral Hydrogen plays an important role, increasing the scattering and leading to observations missing faint Lyα emission within the epoch of reionization. Altogether, our results suggest that we are observing patchy reionization which happens first around the brightest Lyα emitters, allowing the number densities of those sources to remain unaffected by the increase of neutral Hydrogen fraction from z ∼ 5 to 7.","lang":"eng"}],"date_published":"2016-12-01T00:00:00Z","oa":1,"citation":{"ama":"Santos S, Sobral D, Matthee JJ. The Lyα luminosity function at z= 5.7–6.6 and the steep drop of the faint end: Implications for reionization. Monthly Notices of the Royal Astronomical Society. 2016;463(2):1678-1691. doi:10.1093/mnras/stw2076","mla":"Santos, Sérgio, et al. “The Lyα Luminosity Function at Z= 5.7–6.6 and the Steep Drop of the Faint End: Implications for Reionization.” Monthly Notices of the Royal Astronomical Society, vol. 463, no. 2, Oxford University Press, 2016, pp. 1678–91, doi:10.1093/mnras/stw2076.","chicago":"Santos, Sérgio, David Sobral, and Jorryt J Matthee. “The Lyα Luminosity Function at Z= 5.7–6.6 and the Steep Drop of the Faint End: Implications for Reionization.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2016. https://doi.org/10.1093/mnras/stw2076.","short":"S. Santos, D. Sobral, J.J. Matthee, Monthly Notices of the Royal Astronomical Society 463 (2016) 1678–1691.","apa":"Santos, S., Sobral, D., & Matthee, J. J. (2016). The Lyα luminosity function at z= 5.7–6.6 and the steep drop of the faint end: Implications for reionization. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stw2076","ista":"Santos S, Sobral D, Matthee JJ. 2016. The Lyα luminosity function at z= 5.7–6.6 and the steep drop of the faint end: Implications for reionization. Monthly Notices of the Royal Astronomical Society. 463(2), 1678–1691.","ieee":"S. Santos, D. Sobral, and J. J. Matthee, “The Lyα luminosity function at z= 5.7–6.6 and the steep drop of the faint end: Implications for reionization,” Monthly Notices of the Royal Astronomical Society, vol. 463, no. 2. Oxford University Press, pp. 1678–1691, 2016."},"arxiv":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","author":[{"first_name":"Sérgio","last_name":"Santos","full_name":"Santos, Sérgio"},{"first_name":"David","last_name":"Sobral","full_name":"Sobral, David"},{"first_name":"Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"}],"doi":"10.1093/mnras/stw2076","extern":"1","date_created":"2022-07-13T10:08:20Z","_id":"11574","scopus_import":"1","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"volume":463,"article_type":"original","intvolume":" 463","acknowledgement":"We thank the anonymous referee for useful and constructive comments and suggestions which greatly improved the quality and clarity of our work. The authors acknowledge financial support from the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship. SS and DS acknowledge funding from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010). SS also acknowledges support from FCT through the research grants UID/FIS/04434/2013 and PTDC/FIS-AST/2194/2012. JM acknowledges a Huygens PhD fellowship from Leiden University. Based on observations with the Subaru Telescope (Program IDs: S05B-027, S06A-025, S06B-010, S07A-013, S07B-008, S08B-008, S09A-017, S14A-086). Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 294.A-5018. Based on observations obtained with MegaPrime/Megacam, a joint project of CFHT and CEA/IRFU, at the Canada–France–Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l’Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at TERAPIX available at the Canadian Astronomy Data Centre as part of the Canada–France–Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. 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 TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. We are grateful to the CFHTLS, COSMOS-UltraVISTA, UKIDSS, SXDF and COSMOS survey teams. Without these legacy surveys, this research would have been impossible. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct and explore observations from this mountain. Finally, the authors acknowledge the unique value of the publicly available programming language PYTHON, including the NUMPY, PYFITS, MATPLOTLIB, SCIPY and ASTROPY (Astropy Collaboration et al."},{"status":"public","external_id":{"arxiv":["1510.08067"]},"publication":"Monthly Notices of the Royal Astronomical Society","article_processing_charge":"No","language":[{"iso":"eng"}],"date_updated":"2022-08-19T08:12:07Z","month":"07","publisher":"Oxford University Press","day":"01","issue":"3","keyword":["Space and Planetary Science","Astronomy and Astrophysics stars: formation","ISM: evolution","galaxies: evolution","galaxies: formation","galaxies: ISM"],"year":"2016","type":"journal_article","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1510.08067"}],"page":"2632-2650","quality_controlled":"1","abstract":[{"text":"We investigate correlations between different physical properties of star-forming galaxies in the ‘Evolution and Assembly of GaLaxies and their Environments’ (EAGLE) cosmological hydrodynamical simulation suite over the redshift range 0 ≤ z ≤ 4.5. A principal component analysis reveals that neutral gas fraction (fgas,neutral), stellar mass (Mstellar) and star formation rate (SFR) account for most of the variance seen in the population, with galaxies tracing a two-dimensional, nearly flat, surface in the three-dimensional space of fgas, neutral–Mstellar–SFR with little scatter. The location of this plane varies little with redshift, whereas galaxies themselves move along the plane as their fgas, neutral and SFR drop with redshift. The positions of galaxies along the plane are highly correlated with gas metallicity. The metallicity can therefore be robustly predicted from fgas, neutral, or from the Mstellar and SFR. We argue that the appearance of this ‘Fundamental Plane of star formation’ is a consequence of self-regulation, with the plane's curvature set by the dependence of the SFR on gas density and metallicity. We analyse a large compilation of observations spanning the redshift range 0 ≲ z ≲ 3, and find that such a plane is also present in the data. The properties of the observed Fundamental Plane of star formation are in good agreement with EAGLE's predictions.","lang":"eng"}],"oa_version":"Preprint","title":"The Fundamental Plane of star formation in galaxies revealed by the EAGLE hydrodynamical simulations","publication_status":"published","scopus_import":"1","_id":"11575","date_created":"2022-07-13T10:21:24Z","doi":"10.1093/mnras/stw717","author":[{"full_name":"Lagos, Claudia del P.","first_name":"Claudia del P.","last_name":"Lagos"},{"first_name":"Tom","last_name":"Theuns","full_name":"Theuns, Tom"},{"last_name":"Schaye","first_name":"Joop","full_name":"Schaye, Joop"},{"first_name":"Michelle","last_name":"Furlong","full_name":"Furlong, Michelle"},{"first_name":"Richard G.","last_name":"Bower","full_name":"Bower, Richard G."},{"first_name":"Matthieu","last_name":"Schaller","full_name":"Schaller, Matthieu"},{"full_name":"Crain, Robert A.","last_name":"Crain","first_name":"Robert A."},{"full_name":"Trayford, James W.","first_name":"James W.","last_name":"Trayford"},{"orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J"}],"extern":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"ista":"Lagos C del P, Theuns T, Schaye J, Furlong M, Bower RG, Schaller M, Crain RA, Trayford JW, Matthee JJ. 2016. The Fundamental Plane of star formation in galaxies revealed by the EAGLE hydrodynamical simulations. Monthly Notices of the Royal Astronomical Society. 459(3), 2632–2650.","ieee":"C. del P. Lagos et al., “The Fundamental Plane of star formation in galaxies revealed by the EAGLE hydrodynamical simulations,” Monthly Notices of the Royal Astronomical Society, vol. 459, no. 3. Oxford University Press, pp. 2632–2650, 2016.","ama":"Lagos C del P, Theuns T, Schaye J, et al. The Fundamental Plane of star formation in galaxies revealed by the EAGLE hydrodynamical simulations. Monthly Notices of the Royal Astronomical Society. 2016;459(3):2632-2650. doi:10.1093/mnras/stw717","short":"C. del P. Lagos, T. Theuns, J. Schaye, M. Furlong, R.G. Bower, M. Schaller, R.A. Crain, J.W. Trayford, J.J. Matthee, Monthly Notices of the Royal Astronomical Society 459 (2016) 2632–2650.","chicago":"Lagos, Claudia del P., Tom Theuns, Joop Schaye, Michelle Furlong, Richard G. Bower, Matthieu Schaller, Robert A. Crain, James W. Trayford, and Jorryt J Matthee. “The Fundamental Plane of Star Formation in Galaxies Revealed by the EAGLE Hydrodynamical Simulations.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2016. https://doi.org/10.1093/mnras/stw717.","mla":"Lagos, Claudia del P., et al. “The Fundamental Plane of Star Formation in Galaxies Revealed by the EAGLE Hydrodynamical Simulations.” Monthly Notices of the Royal Astronomical Society, vol. 459, no. 3, Oxford University Press, 2016, pp. 2632–50, doi:10.1093/mnras/stw717.","apa":"Lagos, C. del P., Theuns, T., Schaye, J., Furlong, M., Bower, R. G., Schaller, M., … Matthee, J. J. (2016). The Fundamental Plane of star formation in galaxies revealed by the EAGLE hydrodynamical simulations. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stw717"},"arxiv":1,"date_published":"2016-07-01T00:00:00Z","oa":1,"acknowledgement":"We thank Luca Cortese, Matt Bothwell, Paola Santini and Tim Davis for providing observational data sets, and Aaron Robotham, Luca Cortese and Barbara Catinella for useful discussions. CdPL is funded by a Discovery Early Career Researcher Award (DE150100618). CdPL also thanks the MERAC Foundation for a Postdoctoral Research Award. This work used the DiRAC Data Centric system at Durham University, operated by the Institute for Computational Cosmology on behalf of the STFC DiRAC HPC Facility (www.dirac.ac.uk). This equipment was funded by BIS National E-infrastructure capital grant ST/K00042X/1, STFC capital grant ST/H008519/1, and STFC DiRAC Operations grant ST/K003267/1 and Durham University. DiRAC is part of the National E-Infrastructure. Support was also received via the Interuniversity Attraction Poles Programme initiated by the Belgian Science Policy Office ([AP P7/08 CHARM]), the National Science Foundation under grant no. NSF PHY11-25915, and the UK Science and Technology Facilities Council (grant numbers ST/F001166/1 and ST/I000976/1) via rolling and consolidating grants awarded to the ICC. The research was supported in part by the European Research Council under the European Union‘s Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement 278594-GasAroundGalaxies.","intvolume":" 459","article_type":"original","volume":459,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]}},{"oa_version":"Preprint","title":"Evidence for PopIII-like stellar populations in the most luminous Lyα emitters at the epoch of reionisation: Spectroscopic confirmation","publication_status":"published","abstract":[{"text":"Faint Lyα emitters become increasingly rarer toward the reionization epoch (z ∼ 6–7). However, observations from a very large (∼5 deg2) Lyα narrow-band survey at z = 6.6 show that this is not the case for the most luminous emitters, capable of ionizing their own local bubbles. Here we present follow-up observations of the two most luminous Lyα candidates in the COSMOS field: “MASOSA” and “CR7.” We used X-SHOOTER, SINFONI, and FORS2 on the Very Large Telescope, and DEIMOS on Keck, to confirm both candidates beyond any doubt. We find redshifts of z = 6.541 and z = 6.604 for “MASOSA” and “CR7,” respectively. MASOSA has a strong detection in Lyα with a line width of 386 ± 30 km s−1 (FWHM) and with very high EW0 (>200 Å), but undetected in the continuum, implying very low stellar mass and a likely young, metal-poor stellar population. “CR7,” with an observed Lyα luminosity of 1043.92±0.05 erg s−1 is the most luminous Lyα emitter ever found at z > 6 and is spatially extended (∼16 kpc). “CR7” reveals a narrow Lyα line with 266 ± 15 km s−1 FWHM, being detected in the near-infrared (NIR) (rest-frame UV; β = −2.3 ± 0.1) and in IRAC/Spitzer. We detect a narrow He II 1640 Å emission line (6σ, FWHM = 130 ± 30 km s−1 ) in CR7 which can explain the clear excess seen in the J-band photometry (EW0 ∼ 80 Å). We find no other emission lines from the UV to the NIR in our X-SHOOTER spectra (He II/O III] 1663 Å > 3 and He II/C III] 1908 Å > 2.5). We conclude that CR7 is best explained by a combination of a PopIII-like population, which dominates the rest-frame UV and the nebular emission, and a more normal stellar population, which presumably dominates the mass. Hubble Space Telescope/WFC3 observations show that the light is indeed spatially separated between a very blue component, coincident with Lyα and He II emission, and two red components (∼5 kpc away), which dominate the mass. Our findings are consistent with theoretical predictions of a PopIII wave, with PopIII star formation migrating away from the original sites of star formation.","lang":"eng"}],"quality_controlled":"1","main_file_link":[{"url":"https://arxiv.org/abs/1504.01734","open_access":"1"}],"page":"139","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"volume":808,"article_type":"original","intvolume":" 808","acknowledgement":"We thank the anonymous reviewer for useful and constructive comments and suggestions which greatly improved the quality and clarity of our work. D.S. acknowledges financial support from the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship, from FCT through a FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010), from FCT grant UID/FIS/04434/2013, and from LSF and LKBF. J.M. acknowledges the award of a Huygens PhD fellowship. H.R. acknowledges support from the ERC Advanced Investigator program NewClusters 321271. The authors thank Mark Dijkstra, Bhaskar Agarwal, Jarrett Johnson, Andrea Ferrara, Jarle Brinchmann, Rebecca Bowler, George Becker, Emma Curtis-Lake, Milos Milosavljevic, Raffaella Schneider, Paul Shapiro, and Erik Zackrisson for interesting, stimulating and helpful discussions. The authors are extremely grateful to ESO for the award of ESO DDT time (294.A-5018 and 294.A-5039) which allowed the spectroscopic confirmation of both sources and the detailed investigation of their nature. Observations are also based on data from W.M. Keck Observatory. The W.M. Keck Observatory is operated as a scientific partnership of Caltech, the University of California and the National Aeronautics and Space Administration. Based on observations obtained with MegaPrime/Megacam, a joint project of CFHT and CEA/IRFU, at the Canada–France–Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de lUnivers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at Terapix available at the Canadian Astronomy Data Centre as part of the Canada–France–Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme IDs 294.A-5018, 294.A-5039, and 179.A-2005, and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. The authors acknowledge the award of service time (SW2014b20) on the William Herschel Telescope (WHT). WHT and its service programme are operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias.","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa":1,"date_published":"2015-07-28T00:00:00Z","arxiv":1,"citation":{"apa":"Sobral, D., Matthee, J. J., Darvish, B., Schaerer, D., Mobasher, B., Röttgering, H., … Hemmati, S. (2015). Evidence for PopIII-like stellar populations in the most luminous Lyα emitters at the epoch of reionisation: Spectroscopic confirmation. The Astrophysical Journal. IOP Publishing. https://doi.org/10.1088/0004-637X/808/2/139","ama":"Sobral D, Matthee JJ, Darvish B, et al. Evidence for PopIII-like stellar populations in the most luminous Lyα emitters at the epoch of reionisation: Spectroscopic confirmation. The Astrophysical Journal. 2015;808(2):139. doi:10.1088/0004-637X/808/2/139","short":"D. Sobral, J.J. Matthee, B. Darvish, D. Schaerer, B. Mobasher, H. Röttgering, S. Santos, S. Hemmati, The Astrophysical Journal 808 (2015) 139.","chicago":"Sobral, David, Jorryt J Matthee, Behnam Darvish, Daniel Schaerer, Bahram Mobasher, Huub Röttgering, Sérgio Santos, and Shoubaneh Hemmati. “Evidence for PopIII-like Stellar Populations in the Most Luminous Lyα Emitters at the Epoch of Reionisation: Spectroscopic Confirmation.” The Astrophysical Journal. IOP Publishing, 2015. https://doi.org/10.1088/0004-637X/808/2/139.","mla":"Sobral, David, et al. “Evidence for PopIII-like Stellar Populations in the Most Luminous Lyα Emitters at the Epoch of Reionisation: Spectroscopic Confirmation.” The Astrophysical Journal, vol. 808, no. 2, IOP Publishing, 2015, p. 139, doi:10.1088/0004-637X/808/2/139.","ieee":"D. Sobral et al., “Evidence for PopIII-like stellar populations in the most luminous Lyα emitters at the epoch of reionisation: Spectroscopic confirmation,” The Astrophysical Journal, vol. 808, no. 2. IOP Publishing, p. 139, 2015.","ista":"Sobral D, Matthee JJ, Darvish B, Schaerer D, Mobasher B, Röttgering H, Santos S, Hemmati S. 2015. Evidence for PopIII-like stellar populations in the most luminous Lyα emitters at the epoch of reionisation: Spectroscopic confirmation. The Astrophysical Journal. 808(2), 139."},"_id":"11519","scopus_import":"1","date_created":"2022-07-07T09:00:58Z","author":[{"first_name":"David","last_name":"Sobral","full_name":"Sobral, David"},{"first_name":"Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"first_name":"Behnam","last_name":"Darvish","full_name":"Darvish, Behnam"},{"first_name":"Daniel","last_name":"Schaerer","full_name":"Schaerer, Daniel"},{"full_name":"Mobasher, Bahram","first_name":"Bahram","last_name":"Mobasher"},{"full_name":"Röttgering, Huub","first_name":"Huub","last_name":"Röttgering"},{"last_name":"Santos","first_name":"Sérgio","full_name":"Santos, Sérgio"},{"last_name":"Hemmati","first_name":"Shoubaneh","full_name":"Hemmati, Shoubaneh"}],"extern":"1","doi":"10.1088/0004-637X/808/2/139","date_updated":"2022-08-18T10:30:13Z","language":[{"iso":"eng"}],"publication":"The Astrophysical Journal","article_processing_charge":"No","status":"public","external_id":{"arxiv":["1504.01734"]},"year":"2015","type":"journal_article","keyword":["Space and Planetary Science","Astronomy and Astrophysics","dark ages","reionization","first stars – early universe – galaxies: evolution"],"day":"28","issue":"2","month":"07","publisher":"IOP Publishing"},{"volume":453,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"article_type":"original","intvolume":" 453","acknowledgement":"SS acknowledges support from the Netherlands Organization for Scientific research (NWO), VENI grant 639.041.233. RS acknowledges support from the European Research Council under the European Union (FP/2007-2013)/ERC grant agreement no. 306476. DS acknowledges (i) financial support from the NWO through a Veni fellowship and (ii) funding from FCT through a FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010) and from FCT grant PEstOE/FIS/UI2751/2014.","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa":1,"date_published":"2015-11-01T00:00:00Z","arxiv":1,"citation":{"ama":"Pallottini A, Ferrara A, Pacucci F, et al. The brightest Lyα emitter: Pop III or black hole? Monthly Notices of the Royal Astronomical Society. 2015;453(3):2465-2470. doi:10.1093/mnras/stv1795","mla":"Pallottini, A., et al. “The Brightest Lyα Emitter: Pop III or Black Hole?” Monthly Notices of the Royal Astronomical Society, vol. 453, no. 3, Oxford University Press, 2015, pp. 2465–70, doi:10.1093/mnras/stv1795.","chicago":"Pallottini, A., A. Ferrara, F. Pacucci, S. Gallerani, S. Salvadori, R. Schneider, D. Schaerer, D. Sobral, and Jorryt J Matthee. “The Brightest Lyα Emitter: Pop III or Black Hole?” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2015. https://doi.org/10.1093/mnras/stv1795.","short":"A. Pallottini, A. Ferrara, F. Pacucci, S. Gallerani, S. Salvadori, R. Schneider, D. Schaerer, D. Sobral, J.J. Matthee, Monthly Notices of the Royal Astronomical Society 453 (2015) 2465–2470.","apa":"Pallottini, A., Ferrara, A., Pacucci, F., Gallerani, S., Salvadori, S., Schneider, R., … Matthee, J. J. (2015). The brightest Lyα emitter: Pop III or black hole? Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stv1795","ista":"Pallottini A, Ferrara A, Pacucci F, Gallerani S, Salvadori S, Schneider R, Schaerer D, Sobral D, Matthee JJ. 2015. The brightest Lyα emitter: Pop III or black hole? Monthly Notices of the Royal Astronomical Society. 453(3), 2465–2470.","ieee":"A. Pallottini et al., “The brightest Lyα emitter: Pop III or black hole?,” Monthly Notices of the Royal Astronomical Society, vol. 453, no. 3. Oxford University Press, pp. 2465–2470, 2015."},"_id":"11579","scopus_import":"1","extern":"1","author":[{"last_name":"Pallottini","first_name":"A.","full_name":"Pallottini, A."},{"first_name":"A.","last_name":"Ferrara","full_name":"Ferrara, A."},{"last_name":"Pacucci","first_name":"F.","full_name":"Pacucci, F."},{"last_name":"Gallerani","first_name":"S.","full_name":"Gallerani, S."},{"full_name":"Salvadori, S.","last_name":"Salvadori","first_name":"S."},{"full_name":"Schneider, R.","first_name":"R.","last_name":"Schneider"},{"first_name":"D.","last_name":"Schaerer","full_name":"Schaerer, D."},{"full_name":"Sobral, D.","last_name":"Sobral","first_name":"D."},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J"}],"date_created":"2022-07-14T08:58:36Z","doi":"10.1093/mnras/stv1795","oa_version":"Preprint","title":"The brightest Lyα emitter: Pop III or black hole?","publication_status":"published","abstract":[{"text":"CR7 is the brightest z = 6.6 Ly α emitter (LAE) known to date, and spectroscopic follow-up by Sobral et al. suggests that CR7 might host Population (Pop) III stars. We examine this interpretation using cosmological hydrodynamical simulations. Several simulated galaxies show the same ‘Pop III wave’ pattern observed in CR7. However, to reproduce the extreme CR7 Ly α/He II1640 line luminosities (Lα/HeII) a top-heavy initial mass function and a massive ( ≳ 107 M⊙) Pop III burst with age ≲ 2 Myr are required. Assuming that the observed properties of Ly α and He II emission are typical for Pop III, we predict that in the COSMOS/UDS/SA22 fields, 14 out of the 30 LAEs at z = 6.6 with Lα > 1043.3 erg s−1 should also host Pop III stars producing an observable LHeII≳1042.7ergs−1. As an alternate explanation, we explore the possibility that CR7 is instead powered by accretion on to a direct collapse black hole. Our model predicts Lα, LHeII, and X-ray luminosities that are in agreement with the observations. In any case, the observed properties of CR7 indicate that this galaxy is most likely powered by sources formed from pristine gas. We propose that further X-ray observations can distinguish between the two above scenarios.","lang":"eng"}],"quality_controlled":"1","main_file_link":[{"url":"https://arxiv.org/abs/1506.07173","open_access":"1"}],"page":"2465-2470","year":"2015","type":"journal_article","keyword":["Space and Planetary Science","Astronomy and Astrophysics","black hole physics","stars: Population III","galaxies: high-redshift"],"issue":"3","day":"01","month":"11","publisher":"Oxford University Press","date_updated":"2022-08-19T08:19:23Z","language":[{"iso":"eng"}],"publication":"Monthly Notices of the Royal Astronomical Society","article_processing_charge":"No","status":"public","external_id":{"arxiv":["1506.07173"]}},{"status":"public","external_id":{"arxiv":["1402.6697"]},"publication":"Monthly Notices of the Royal Astronomical Society","article_processing_charge":"No","language":[{"iso":"eng"}],"date_updated":"2024-10-14T11:37:28Z","month":"05","publisher":"Oxford University Press","issue":"3","day":"21","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","cosmology: observations","dark ages","reionization","first stars"],"year":"2014","type":"journal_article","main_file_link":[{"url":"https://arxiv.org/abs/1402.6697","open_access":"1"}],"page":"2375-2387","quality_controlled":"1","abstract":[{"text":"Candidate galaxies at redshifts of z ∼ 10 are now being found in extremely deep surveys, probing very small areas. As a consequence, candidates are very faint, making spectroscopic confirmation practically impossible. In order to overcome such limitations, we have undertaken the CF-HiZELS survey, which is a large-area, medium-depth near-infrared narrow-band survey targeted at z = 8.8 Lyman α (Lyα) emitters (LAEs) and covering 10 deg2 in part of the SSA22 field with the Canada–France–Hawaii Telescope (CFHT). We surveyed a comoving volume of 4.7 × 106 Mpc3 to a Lyα luminosity limit of 6.3 × 1043舁erg舁s−1. We look for Lyα candidates by applying the following criteria: (i) clear emission-line source, (ii) no optical detections (ugriz from CFHTLS), (iii) no visible detection in the optical stack (ugriz > 27), (iv) visually checked reliable NBJ and J detections and (v) J − K ≤ 0. We compute photometric redshifts and remove a significant amount of dusty lower redshift line-emitters at z ∼ 1.4 or 2.2. A total of 13 Lyα candidates were found, of which two are marked as strong candidates, but the majority have very weak constraints on their spectral energy distributions. Using follow-up observations with SINFONI/VLT, we are able to exclude the most robust candidates as LAEs. We put a strong constraint on the Lyα luminosity function at z ∼ 9 and make realistic predictions for ongoing and future surveys. Our results show that surveys for the highest redshift LAEs are susceptible of multiple contaminations and that spectroscopic follow-up is absolutely necessary.","lang":"eng"}],"title":"A 10 deg2 Lyman α survey at z=8.8 with spectroscopic follow-up: Strong constraints on the luminosity function and implications for other surveys","oa_version":"Preprint","publication_status":"published","_id":"11583","scopus_import":"1","date_created":"2022-07-14T12:33:24Z","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","first_name":"Jorryt J"},{"full_name":"Sobral, David","first_name":"David","last_name":"Sobral"},{"last_name":"Swinbank","first_name":"A. M.","full_name":"Swinbank, A. M."},{"first_name":"Ian","last_name":"Smail","full_name":"Smail, Ian"},{"full_name":"Best, P. N.","last_name":"Best","first_name":"P. N."},{"full_name":"Kim, Jae-Woo","first_name":"Jae-Woo","last_name":"Kim"},{"full_name":"Franx, Marijn","first_name":"Marijn","last_name":"Franx"},{"full_name":"Milvang-Jensen, Bo","first_name":"Bo","last_name":"Milvang-Jensen"},{"full_name":"Fynbo, Johan","last_name":"Fynbo","first_name":"Johan"}],"extern":"1","doi":"10.1093/mnras/stu392","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa":1,"date_published":"2014-05-21T00:00:00Z","citation":{"ista":"Matthee JJ, Sobral D, Swinbank AM, Smail I, Best PN, Kim J-W, Franx M, Milvang-Jensen B, Fynbo J. 2014. A 10 deg2 Lyman α survey at z=8.8 with spectroscopic follow-up: Strong constraints on the luminosity function and implications for other surveys. Monthly Notices of the Royal Astronomical Society. 440(3), 2375–2387.","ieee":"J. J. Matthee et al., “A 10 deg2 Lyman α survey at z=8.8 with spectroscopic follow-up: Strong constraints on the luminosity function and implications for other surveys,” Monthly Notices of the Royal Astronomical Society, vol. 440, no. 3. Oxford University Press, pp. 2375–2387, 2014.","ama":"Matthee JJ, Sobral D, Swinbank AM, et al. A 10 deg2 Lyman α survey at z=8.8 with spectroscopic follow-up: Strong constraints on the luminosity function and implications for other surveys. Monthly Notices of the Royal Astronomical Society. 2014;440(3):2375-2387. doi:10.1093/mnras/stu392","mla":"Matthee, Jorryt J., et al. “A 10 Deg2 Lyman α Survey at Z=8.8 with Spectroscopic Follow-up: Strong Constraints on the Luminosity Function and Implications for Other Surveys.” Monthly Notices of the Royal Astronomical Society, vol. 440, no. 3, Oxford University Press, 2014, pp. 2375–87, doi:10.1093/mnras/stu392.","short":"J.J. Matthee, D. Sobral, A.M. Swinbank, I. Smail, P.N. Best, J.-W. Kim, M. Franx, B. Milvang-Jensen, J. Fynbo, Monthly Notices of the Royal Astronomical Society 440 (2014) 2375–2387.","chicago":"Matthee, Jorryt J, David Sobral, A. M. Swinbank, Ian Smail, P. N. Best, Jae-Woo Kim, Marijn Franx, Bo Milvang-Jensen, and Johan Fynbo. “A 10 Deg2 Lyman α Survey at Z=8.8 with Spectroscopic Follow-up: Strong Constraints on the Luminosity Function and Implications for Other Surveys.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2014. https://doi.org/10.1093/mnras/stu392.","apa":"Matthee, J. J., Sobral, D., Swinbank, A. M., Smail, I., Best, P. N., Kim, J.-W., … Fynbo, J. (2014). A 10 deg2 Lyman α survey at z=8.8 with spectroscopic follow-up: Strong constraints on the luminosity function and implications for other surveys. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stu392"},"arxiv":1,"intvolume":" 440","acknowledgement":"We thank the anonymous referee for the comments and suggestions which improved both the quality and clarity of this work. DS acknowledges financial support from the Netherlands Organisation for Scientific Research (NWO) through a Veni fellowship. IRS acknowledges support from STFC (ST/I001573/1), a Leverhulme Fellowship, the ERC Advanced Investigator programme DUSTYGAL 321334 and a Royal Society/Wolfson Merit Award. PNB acknowledges support from the Leverhulme Trust. JWK acknowledges the support from the Creative Research Initiative Program, no. 2008- 0060544, of the National Research Foundation of Korea (NRF) funded by the Korean government (MSIP). JPUF and BMJ acknowledge support from the ERC-StG grant EGGS-278202. The Dark Cosmology Centre is funded by the Danish National Research Foundation. This work is based in part on data obtained as part of the UKIRT Infrared Deep Sky Survey. Based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/IRFU, at the Canada–France–Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l’Univers of the Centre National de la Recherche Scientifique (CNRS) of France and the University of Hawaii. This work is based in part on data products produced at Terapix available at the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. This work was only possible due to OPTICON/FP7 and the access that it granted to the CFHT telescope. The authors also wish to acknowledge the CFHTLS and UKIDSS surveys for their excellent legacy and complementary value – without such high-quality data sets, this research would not have been possible.","volume":440,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"article_type":"original"}]