[{"user_id":"72615eeb-f1f3-11ec-aa25-d4573ddc34fd","citation":{"ista":"Hatch EM, Hetzer M. 2015. Chromothripsis. Current Biology. 25(10), PR397-R399.","chicago":"Hatch, Emily M., and Martin Hetzer. “Chromothripsis.” Current Biology. Elsevier, 2015. https://doi.org/10.1016/j.cub.2015.02.033.","apa":"Hatch, E. M., & Hetzer, M. (2015). Chromothripsis. Current Biology. Elsevier. https://doi.org/10.1016/j.cub.2015.02.033","ama":"Hatch EM, Hetzer M. Chromothripsis. Current Biology. 2015;25(10):PR397-R399. doi:10.1016/j.cub.2015.02.033","ieee":"E. M. Hatch and M. Hetzer, “Chromothripsis,” Current Biology, vol. 25, no. 10. Elsevier, pp. PR397-R399, 2015.","short":"E.M. Hatch, M. Hetzer, Current Biology 25 (2015) PR397-R399.","mla":"Hatch, Emily M., and Martin Hetzer. “Chromothripsis.” Current Biology, vol. 25, no. 10, Elsevier, 2015, pp. PR397-R399, doi:10.1016/j.cub.2015.02.033."},"title":"Chromothripsis","article_processing_charge":"No","external_id":{"pmid":["25989073"]},"author":[{"last_name":"Hatch","full_name":"Hatch, Emily M.","first_name":"Emily M."},{"last_name":"HETZER","full_name":"HETZER, Martin W","orcid":"0000-0002-2111-992X","first_name":"Martin W","id":"86c0d31b-b4eb-11ec-ac5a-eae7b2e135ed"}],"oa":1,"quality_controlled":"1","publisher":"Elsevier","publication":"Current Biology","day":"18","year":"2015","date_created":"2022-04-07T07:49:00Z","date_published":"2015-05-18T00:00:00Z","doi":"10.1016/j.cub.2015.02.033","page":"PR397-R399","_id":"11074","keyword":["General Agricultural and Biological Sciences","General Biochemistry","Genetics and Molecular Biology"],"status":"public","article_type":"original","type":"journal_article","extern":"1","date_updated":"2022-07-18T08:34:34Z","oa_version":"Published Version","pmid":1,"intvolume":" 25","month":"05","main_file_link":[{"url":"https://doi.org/10.1016/j.cub.2015.02.033","open_access":"1"}],"scopus_import":"1","language":[{"iso":"eng"}],"publication_status":"published","publication_identifier":{"issn":["0960-9822"]},"volume":25,"issue":"10"},{"_id":"11519","status":"public","keyword":["Space and Planetary Science","Astronomy and Astrophysics","dark ages","reionization","first stars – early universe – galaxies: evolution"],"type":"journal_article","article_type":"original","extern":"1","date_updated":"2022-08-18T10:30:13Z","oa_version":"Preprint","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"}],"month":"07","intvolume":" 808","scopus_import":"1","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1504.01734"}],"language":[{"iso":"eng"}],"publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"publication_status":"published","volume":808,"issue":"2","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"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.","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","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","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.","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.","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."},"title":"Evidence for PopIII-like stellar populations in the most luminous Lyα emitters at the epoch of reionisation: Spectroscopic confirmation","author":[{"first_name":"David","last_name":"Sobral","full_name":"Sobral, David"},{"last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J"},{"last_name":"Darvish","full_name":"Darvish, Behnam","first_name":"Behnam"},{"last_name":"Schaerer","full_name":"Schaerer, Daniel","first_name":"Daniel"},{"first_name":"Bahram","last_name":"Mobasher","full_name":"Mobasher, Bahram"},{"full_name":"Röttgering, Huub","last_name":"Röttgering","first_name":"Huub"},{"full_name":"Santos, Sérgio","last_name":"Santos","first_name":"Sérgio"},{"last_name":"Hemmati","full_name":"Hemmati, Shoubaneh","first_name":"Shoubaneh"}],"article_processing_charge":"No","external_id":{"arxiv":["1504.01734"]},"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.","quality_controlled":"1","publisher":"IOP Publishing","oa":1,"day":"28","publication":"The Astrophysical Journal","year":"2015","date_published":"2015-07-28T00:00:00Z","doi":"10.1088/0004-637X/808/2/139","date_created":"2022-07-07T09:00:58Z","page":"139"},{"_id":"11580","type":"journal_article","article_type":"original","status":"public","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: formation","galaxies: luminosity function","mass function","cosmology: observations","early Universe","large-scale structure of Universe"],"date_updated":"2022-08-19T08:23:18Z","extern":"1","abstract":[{"lang":"eng","text":"We present results from the largest contiguous narrow-band survey in the near-infrared. We have used the wide-field infrared camera/Canada–France–Hawaii Telescope and the lowOH2 filter (1.187 ± 0.005 μm) to survey ≈10 deg2 of contiguous extragalactic sky in the SA22 field. A total of ∼6000 candidate emission-line galaxies are found. We use deep ugrizJK data to obtain robust photometric redshifts. We combine our data with the High-redshift(Z) Emission Line Survey (HiZELS), explore spectroscopic surveys (VVDS, VIPERS) and obtain our own spectroscopic follow-up with KMOS, FMOS and MOSFIRE to derive large samples of high-redshift emission-line selected galaxies: 3471 Hα emitters at z = 0.8, 1343 [O III] + Hβ emitters at z = 1.4 and 572 [O II] emitters at z = 2.2. We probe comoving volumes of >106 Mpc3 and find significant overdensities, including an 8.5σ (spectroscopically confirmed) overdensity of Hα emitters at z = 0.81. We derive Hα, [O III] + Hβ and [O II] luminosity functions at z = 0.8, 1.4, 2.2, respectively, and present implications for future surveys such as Euclid. Our uniquely large volumes/areas allow us to subdivide the samples in thousands of randomized combinations of areas and provide a robust empirical measurement of sample/cosmic variance. We show that surveys for star-forming/emission-line galaxies at a depth similar to ours can only overcome cosmic-variance (errors <10 per cent) if they are based on volumes >5 × 105 Mpc3; errors on L* and ϕ* due to sample (cosmic) variance on surveys probing ∼104 and ∼105 Mpc3 are typically very high: ∼300 and ∼40–60 per cent, respectively."}],"oa_version":"Preprint","scopus_import":"1","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1502.06602"}],"month":"08","intvolume":" 451","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"publication_status":"published","language":[{"iso":"eng"}],"issue":"3","volume":451,"citation":{"mla":"Sobral, D., et al. “CF-HiZELS, an ∼10 Deg2 Emission-Line Survey with Spectroscopic Follow-up: Hα, [O III] + Hβ and [O II] Luminosity Functions at z = 0.8, 1.4 and 2.2 .” Monthly Notices of the Royal Astronomical Society, vol. 451, no. 3, Oxford University Press, 2015, pp. 2303–23, doi:10.1093/mnras/stv1076.","apa":"Sobral, D., Matthee, J. J., Best, P. N., Smail, I., Khostovan, A. A., Milvang-Jensen, B., … Mobasher, B. (2015). CF-HiZELS, an ∼10 deg2 emission-line survey with spectroscopic follow-up: Hα, [O III] + Hβ and [O II] luminosity functions at z = 0.8, 1.4 and 2.2 . Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stv1076","ama":"Sobral D, Matthee JJ, Best PN, et al. CF-HiZELS, an ∼10 deg2 emission-line survey with spectroscopic follow-up: Hα, [O III] + Hβ and [O II] luminosity functions at z = 0.8, 1.4 and 2.2 . Monthly Notices of the Royal Astronomical Society. 2015;451(3):2303-2323. doi:10.1093/mnras/stv1076","ieee":"D. Sobral et al., “CF-HiZELS, an ∼10 deg2 emission-line survey with spectroscopic follow-up: Hα, [O III] + Hβ and [O II] luminosity functions at z = 0.8, 1.4 and 2.2 ,” Monthly Notices of the Royal Astronomical Society, vol. 451, no. 3. Oxford University Press, pp. 2303–2323, 2015.","short":"D. Sobral, J.J. Matthee, P.N. Best, I. Smail, A.A. Khostovan, B. Milvang-Jensen, J.-W. Kim, J. Stott, J. Calhau, H. Nayyeri, B. Mobasher, Monthly Notices of the Royal Astronomical Society 451 (2015) 2303–2323.","chicago":"Sobral, D., Jorryt J Matthee, P. N. Best, I. Smail, A. A. Khostovan, B. Milvang-Jensen, J.-W. Kim, et al. “CF-HiZELS, an ∼10 Deg2 Emission-Line Survey with Spectroscopic Follow-up: Hα, [O III] + Hβ and [O II] Luminosity Functions at z = 0.8, 1.4 and 2.2 .” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2015. https://doi.org/10.1093/mnras/stv1076.","ista":"Sobral D, Matthee JJ, Best PN, Smail I, Khostovan AA, Milvang-Jensen B, Kim J-W, Stott J, Calhau J, Nayyeri H, Mobasher B. 2015. CF-HiZELS, an ∼10 deg2 emission-line survey with spectroscopic follow-up: Hα, [O III] + Hβ and [O II] luminosity functions at z = 0.8, 1.4 and 2.2 . Monthly Notices of the Royal Astronomical Society. 451(3), 2303–2323."},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","author":[{"first_name":"D.","full_name":"Sobral, D.","last_name":"Sobral"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J"},{"first_name":"P. N.","last_name":"Best","full_name":"Best, P. N."},{"first_name":"I.","last_name":"Smail","full_name":"Smail, I."},{"last_name":"Khostovan","full_name":"Khostovan, A. A.","first_name":"A. A."},{"last_name":"Milvang-Jensen","full_name":"Milvang-Jensen, B.","first_name":"B."},{"full_name":"Kim, J.-W.","last_name":"Kim","first_name":"J.-W."},{"last_name":"Stott","full_name":"Stott, J.","first_name":"J."},{"last_name":"Calhau","full_name":"Calhau, J.","first_name":"J."},{"last_name":"Nayyeri","full_name":"Nayyeri, H.","first_name":"H."},{"first_name":"B.","full_name":"Mobasher, B.","last_name":"Mobasher"}],"external_id":{"arxiv":["1502.06602"]},"article_processing_charge":"No","title":"CF-HiZELS, an ∼10 deg2 emission-line survey with spectroscopic follow-up: Hα, [O III] + Hβ and [O II] luminosity functions at z = 0.8, 1.4 and 2.2 ","acknowledgement":"The authors wish to thank the anonymous reviewer for many helpful comments and suggestions which greatly improved the clarity and quality of this work. DS acknowledges financial support from the Netherlands Organization for Scientific research (NWO) through a Veni fellowship, from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010), from FCT grant PEst-OE/FIS/UI2751/2014, and from LSF and LKBF. JM acknowledges the award of a Huygens PhD fellowship. PNB is grateful for support from STFC. IRS acknowledges support from STFC, a Leverhulme Fellowship, the ERC Advanced Investigator programme DUSTYGAL and a Royal Society/Wolfson Merit Award. BMJ acknowledges support from the ERC-StG grant EGGS-278202. The Dark Cosmology Centre is funded by the DNRF. The Dark Cosmology Centre is funded by the DNRF. JWK acknowledges support from the National Research Foundation of Korea (NRF) grant, no. 2008-0060544, funded by the Korea government (MSIP). JPS acknowledges support from STFC (ST/I001573/1). JC acknowledges support from the FCT-IF grant IF/01154/2012/CP0189/CT0010. The work was only possible due to OPTICON/FP7 and the invaluable access that it granted to the CFHT telescope. We would also like to acknowledge the excellent work done by CFHT staff in conducting the observations in service mode, and on delivering truly excellent data. We are also tremendously thankful to Kentaro Aoki for the incredible support while observing at Subaru with FMOS, and also to the Keck staff for the help with the observations with MOSFIRE. This work is based on observations obtained with WIRCam on the CFHT, OPTICON programme 2011B/029, 2012A019 and 2012B/016. Based on observations made with ESO telescopes at the La Silla Paranal Observatory under programmes IDs 60.A-9460 (data can be accessed through the ESO data archive), 087.A 0337 and 089.A-0965. Based on observations done with FMOS on Subaru under programme S14A-084, and on MOSFIRE/Keck observations under programme U066M. Part of the data on which this analysis is based are available from Sobral et al. (2013a). Dedicated to the memory of C. M. Sobral (1953-2014).","publisher":"Oxford University Press","quality_controlled":"1","oa":1,"year":"2015","day":"11","publication":"Monthly Notices of the Royal Astronomical Society","page":"2303-2323","date_published":"2015-08-11T00:00:00Z","doi":"10.1093/mnras/stv1076","date_created":"2022-07-14T09:02:22Z"},{"publication":"Monthly Notices of the Royal Astronomical Society","day":"21","year":"2015","date_created":"2022-07-14T11:57:03Z","date_published":"2015-07-21T00:00:00Z","doi":"10.1093/mnras/stv947","page":"400-417","acknowledgement":"We thank the anonymous referee for the comments and suggestions which have improved the quality of this work. We thank Masami Ouchi for his useful comments on an earlier version of this paper. JM acknowledges the support of a Huygens PhD fellowship from Leiden University and is thankful for the hospitality of the Center for Astronomy and Astrophysics of the University of Lisbon where part of this research has been done. DS acknowledges financial support from the Netherlands Organization 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) and from FCT grant PEstOE/FIS/UI2751/2014. HR acknowledges support from the ERC Advanced Investigator programme NewClusters 321271. We acknowledge the award of ESO DDT time (294.A-5018) for providing the possibility of a timely publication of this work.\r\nBased on observations with the Subaru Telescope (Programme IDs: our observations: S14A-086; archival: S05B-027, S06A-025, S06B-010, S07A-013, S07B-008, S08B-008 and S09A-017) and the W.M. Keck Observatory. The Subaru telescope is operated by the National Astronomical Observatory of Japan. The W.M. Keck Observatory is operated as a scientific partnership among 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 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 CFHT 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.\r\nIn addition to the CFHT-LS and COSMOS-UltraVISTA surveys, we are grateful for the excellent data sets from the UKIRT-DXS, SXDF and S-COSMOS survey teams, without these legacy surveys, this research would have been impossible. We have benefited greatly 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 indispensable TOPCAT analysis tool (Taylor 2013)","oa":1,"publisher":"Oxford University Press","quality_controlled":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"ista":"Matthee JJ, Sobral D, Santos S, Röttgering H, Darvish B, Mobasher B. 2015. Identification of the brightest Lyα emitters at z = 6.6: implications for the evolution of the luminosity function in the reionization era. Monthly Notices of the Royal Astronomical Society. 451(1), 400–417.","chicago":"Matthee, Jorryt J, David Sobral, Sérgio Santos, Huub Röttgering, Behnam Darvish, and Bahram Mobasher. “Identification of the Brightest Lyα Emitters at z = 6.6: Implications for the Evolution of the Luminosity Function in the Reionization Era.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2015. https://doi.org/10.1093/mnras/stv947.","ieee":"J. J. Matthee, D. Sobral, S. Santos, H. Röttgering, B. Darvish, and B. Mobasher, “Identification of the brightest Lyα emitters at z = 6.6: implications for the evolution of the luminosity function in the reionization era,” Monthly Notices of the Royal Astronomical Society, vol. 451, no. 1. Oxford University Press, pp. 400–417, 2015.","short":"J.J. Matthee, D. Sobral, S. Santos, H. Röttgering, B. Darvish, B. Mobasher, Monthly Notices of the Royal Astronomical Society 451 (2015) 400–417.","apa":"Matthee, J. J., Sobral, D., Santos, S., Röttgering, H., Darvish, B., & Mobasher, B. (2015). Identification of the brightest Lyα emitters at z = 6.6: implications for the evolution of the luminosity function in the reionization era. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stv947","ama":"Matthee JJ, Sobral D, Santos S, Röttgering H, Darvish B, Mobasher B. Identification of the brightest Lyα emitters at z = 6.6: implications for the evolution of the luminosity function in the reionization era. Monthly Notices of the Royal Astronomical Society. 2015;451(1):400-417. doi:10.1093/mnras/stv947","mla":"Matthee, Jorryt J., et al. “Identification of the Brightest Lyα Emitters at z = 6.6: Implications for the Evolution of the Luminosity Function in the Reionization Era.” Monthly Notices of the Royal Astronomical Society, vol. 451, no. 1, Oxford University Press, 2015, pp. 400–17, doi:10.1093/mnras/stv947."},"title":"Identification of the brightest Lyα emitters at z = 6.6: implications for the evolution of the luminosity function in the reionization era","external_id":{"arxiv":["1502.07355"]},"article_processing_charge":"No","author":[{"last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"first_name":"David","last_name":"Sobral","full_name":"Sobral, David"},{"last_name":"Santos","full_name":"Santos, Sérgio","first_name":"Sérgio"},{"first_name":"Huub","full_name":"Röttgering, Huub","last_name":"Röttgering"},{"last_name":"Darvish","full_name":"Darvish, Behnam","first_name":"Behnam"},{"full_name":"Mobasher, Bahram","last_name":"Mobasher","first_name":"Bahram"}],"language":[{"iso":"eng"}],"publication_status":"published","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"issue":"1","volume":451,"oa_version":"Preprint","abstract":[{"text":"Using wide-field narrow-band surveys, we provide a new measurement of the z = 6.6 Lymanα emitter (LAE) luminosity function (LF), which constraints the bright end for the first time. We use a combination of archival narrow-band NB921 data in UDS and new NB921 measurements in SA22 and COSMOS/UltraVISTA, all observed with the Subaru telescope, with a total area of ∼5 deg2. We exclude lower redshift interlopers by using broad-band optical and near-infrared photometry and also exclude three supernovae with data split over multiple epochs. Combining the UDS and COSMOS samples, we find no evolution of the bright end of the Lyα LF between z = 5.7 and 6.6, which is supported by spectroscopic follow-up, and conclude that sources with Himiko-like luminosity are not as rare as previously thought, with number densities of ∼1.5 × 10−5 Mpc−3. Combined with our wide-field SA22 measurements, our results indicate a non-Schechter-like bright end of the LF at z = 6.6 and a different evolution of observed faint and bright LAEs, overcoming cosmic variance. This differential evolution is also seen in the spectroscopic follow-up of UV-selected galaxies and is now also confirmed for LAEs, and we argue that it may be an effect of reionization. Using a toy model, we show that such differential evolution of the LF is expected, since brighter sources are able to ionize their surroundings earlier, such that Lyα photons are able to escape. Our targets are excellent candidates for detailed follow-up studies and provide the possibility to give a unique view on the earliest stages in the formation of galaxies and reionization process.","lang":"eng"}],"intvolume":" 451","month":"07","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1502.07355"}],"scopus_import":"1","extern":"1","date_updated":"2022-08-19T08:25:25Z","_id":"11581","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"status":"public","type":"journal_article","article_type":"original"},{"oa_version":"Preprint","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"}],"intvolume":" 453","month":"11","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1506.07173"}],"scopus_import":"1","language":[{"iso":"eng"}],"publication_status":"published","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"volume":453,"issue":"3","_id":"11579","keyword":["Space and Planetary Science","Astronomy and Astrophysics","black hole physics","stars: Population III","galaxies: high-redshift"],"status":"public","article_type":"original","type":"journal_article","extern":"1","date_updated":"2022-08-19T08:19:23Z","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.","oa":1,"publisher":"Oxford University Press","quality_controlled":"1","publication":"Monthly Notices of the Royal Astronomical Society","day":"01","year":"2015","date_created":"2022-07-14T08:58:36Z","date_published":"2015-11-01T00:00:00Z","doi":"10.1093/mnras/stv1795","page":"2465-2470","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"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.","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.","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","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","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.","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.","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."},"title":"The brightest Lyα emitter: Pop III or black hole?","external_id":{"arxiv":["1506.07173"]},"article_processing_charge":"No","author":[{"last_name":"Pallottini","full_name":"Pallottini, A.","first_name":"A."},{"first_name":"A.","full_name":"Ferrara, A.","last_name":"Ferrara"},{"full_name":"Pacucci, F.","last_name":"Pacucci","first_name":"F."},{"first_name":"S.","full_name":"Gallerani, S.","last_name":"Gallerani"},{"first_name":"S.","full_name":"Salvadori, S.","last_name":"Salvadori"},{"first_name":"R.","last_name":"Schneider","full_name":"Schneider, R."},{"first_name":"D.","full_name":"Schaerer, D.","last_name":"Schaerer"},{"first_name":"D.","full_name":"Sobral, D.","last_name":"Sobral"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee"}]}]