[{"citation":{"ista":"Kusakabe H, Verhamme A, Blaizot J, Garel T, Wisotzki L, Leclercq F, Bacon R, Schaye J, Gallego SG, Kerutt J, Matthee JJ, Maseda M, Nanayakkara T, Pelló R, Richard J, Tresse L, Urrutia T, Vitte E. 2022. The MUSE eXtremely Deep Field: Individual detections of Lyα haloes around rest-frame UV-selected galaxies at z ≃ 2.9–4.4. Astronomy & Astrophysics. 660, A44.","chicago":"Kusakabe, Haruka, Anne Verhamme, Jérémy Blaizot, Thibault Garel, Lutz Wisotzki, Floriane Leclercq, Roland Bacon, et al. “The MUSE EXtremely Deep Field: Individual Detections of Lyα Haloes around Rest-Frame UV-Selected Galaxies at z ≃ 2.9–4.4.” Astronomy & Astrophysics. EDP Sciences, 2022. https://doi.org/10.1051/0004-6361/202142302.","mla":"Kusakabe, Haruka, et al. “The MUSE EXtremely Deep Field: Individual Detections of Lyα Haloes around Rest-Frame UV-Selected Galaxies at z ≃ 2.9–4.4.” Astronomy & Astrophysics, vol. 660, A44, EDP Sciences, 2022, doi:10.1051/0004-6361/202142302.","apa":"Kusakabe, H., Verhamme, A., Blaizot, J., Garel, T., Wisotzki, L., Leclercq, F., … Vitte, E. (2022). The MUSE eXtremely Deep Field: Individual detections of Lyα haloes around rest-frame UV-selected galaxies at z ≃ 2.9–4.4. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202142302","ama":"Kusakabe H, Verhamme A, Blaizot J, et al. The MUSE eXtremely Deep Field: Individual detections of Lyα haloes around rest-frame UV-selected galaxies at z ≃ 2.9–4.4. Astronomy & Astrophysics. 2022;660. doi:10.1051/0004-6361/202142302","short":"H. Kusakabe, A. Verhamme, J. Blaizot, T. Garel, L. Wisotzki, F. Leclercq, R. Bacon, J. Schaye, S.G. Gallego, J. Kerutt, J.J. Matthee, M. Maseda, T. Nanayakkara, R. Pelló, J. Richard, L. Tresse, T. Urrutia, E. Vitte, Astronomy & Astrophysics 660 (2022).","ieee":"H. Kusakabe et al., “The MUSE eXtremely Deep Field: Individual detections of Lyα haloes around rest-frame UV-selected galaxies at z ≃ 2.9–4.4,” Astronomy & Astrophysics, vol. 660. EDP Sciences, 2022."},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa":1,"language":[{"iso":"eng"}],"article_number":"A44","arxiv":1,"month":"04","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"publication_status":"published","abstract":[{"text":"Hydrogen Lyα haloes (LAHs) are commonly used as a tracer of the circumgalactic medium (CGM) at high redshifts. In this work, we aim to explore the existence of Lyα haloes around individual UV-selected galaxies, rather than around Lyα emitters (LAEs), at high redshifts. Our sample was continuum-selected with F775W ≤ 27.5, and spectroscopic redshifts were assigned or constrained for all the sources thanks to the deepest (100- to 140-h) existing Very Large Telescope (VLT)/Multi-Unit Spectroscopic Explorer (MUSE) data with adaptive optics. The final sample includes 21 galaxies that are purely F775W-magnitude selected within the redshift range z ≈ 2.9 − 4.4 and within a UV magnitude range −20 ≤ M1500 ≤ −18, thus avoiding any bias toward LAEs. We tested whether galaxy’s Lyα emission is significantly more extended than the MUSE PSF-convolved continuum component. We find 17 LAHs and four non-LAHs. We report the first individual detections of extended Lyα emission around non-LAEs. The Lyα halo fraction is thus as high as 81.0−11.2+10.3%, which is close to that for LAEs at z = 3 − 6 in the literature. This implies that UV-selected galaxies generally have a large amount of hydrogen in their CGM. We derived the mean surface brightness (SB) profile for our LAHs with cosmic dimming corrections and find that Lyα emission extends to 5.4 arcsec (≃40 physical kpc at the midpoint redshift z = 3.6) above the typical 1σ SB limit. The incidence rate of surrounding gas detected in Lyα per one-dimensional line of sight per unit redshift, dn/dz, is estimated to be 0.76−0.09+0.09 for galaxies with M1500 ≤ −18 mag at z ≃ 3.7. Assuming that Lyα emission and absorption arise in the same gas, this suggests, based on abundance matching, that LAHs trace the same gas as damped Lyα systems (DLAs) and sub-DLAs.","lang":"eng"}],"intvolume":" 660","volume":660,"date_created":"2022-07-05T14:27:26Z","article_type":"original","scopus_import":"1","day":"07","author":[{"last_name":"Kusakabe","full_name":"Kusakabe, Haruka","first_name":"Haruka"},{"last_name":"Verhamme","full_name":"Verhamme, Anne","first_name":"Anne"},{"first_name":"Jérémy","full_name":"Blaizot, Jérémy","last_name":"Blaizot"},{"first_name":"Thibault","full_name":"Garel, Thibault","last_name":"Garel"},{"last_name":"Wisotzki","full_name":"Wisotzki, Lutz","first_name":"Lutz"},{"full_name":"Leclercq, Floriane","last_name":"Leclercq","first_name":"Floriane"},{"first_name":"Roland","last_name":"Bacon","full_name":"Bacon, Roland"},{"first_name":"Joop","full_name":"Schaye, Joop","last_name":"Schaye"},{"full_name":"Gallego, Sofia G.","last_name":"Gallego","first_name":"Sofia G."},{"full_name":"Kerutt, Josephine","last_name":"Kerutt","first_name":"Josephine"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"},{"first_name":"Michael","last_name":"Maseda","full_name":"Maseda, Michael"},{"full_name":"Nanayakkara, Themiya","last_name":"Nanayakkara","first_name":"Themiya"},{"first_name":"Roser","full_name":"Pelló, Roser","last_name":"Pelló"},{"first_name":"Johan","full_name":"Richard, Johan","last_name":"Richard"},{"last_name":"Tresse","full_name":"Tresse, Laurence","first_name":"Laurence"},{"first_name":"Tanya","last_name":"Urrutia","full_name":"Urrutia, Tanya"},{"first_name":"Eloïse","last_name":"Vitte","full_name":"Vitte, Eloïse"}],"title":"The MUSE eXtremely Deep Field: Individual detections of Lyα haloes around rest-frame UV-selected galaxies at z ≃ 2.9–4.4","oa_version":"Published Version","acknowledgement":"We thank the anonymous referee for constructive comments and suggestions. We would like to express our gratitude to Edmund Christian Herenz, Leindert Boogard, Miroslava Dessauges, Moupiya Maji, Valentin Mauerhofer, Charlotte Paola Simmonds Wagemann, Masami Ouchi, Kazuhiro Shimasaku, Akio Inoue, and Rieko Momose for giving insightful comments and suggestions. H.K. is grateful to Liam McCarney for useful suggestions on English writing through the UniGE’s Tandems linguistiques. H.K. acknowledges support from Swiss Government Excellence Scholarships and Japan Society for the Promotion of Science (JSPS) Overseas Research Fellowship. H.K., F.L., and A.V. are supported by the SNF grant PP00P2 176808. A.V. and T.G. are supported by the ERC Starting Grant 757258“TRIPLE”. This work was supported by the Programme National Cosmology et Galaxies (PNCG) of CNRS/INSU with INP and IN2P3, co-funded by CEA and CNES. This work is based on observations taken by VLT, which is operated by European Southern Observatory. This research made use of Astropy, which is a community-developed core Python package for Astronomy (Astropy Collaboration 2013, 2018), and other software and packages: MARZ, MPDAF (Piqueras et al. 2019), PHOTUTILS, Numpy (Harris et al. 2020), Scipy (Virtanen et al. 2020), and matplotlib (Hunter 2007).","date_published":"2022-04-07T00:00:00Z","status":"public","publication":"Astronomy & Astrophysics","extern":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift / galaxies: formation / galaxies: evolution / cosmology: observations"],"year":"2022","external_id":{"arxiv":["2201.07257"]},"main_file_link":[{"url":"https://arxiv.org/abs/2201.07257","open_access":"1"}],"quality_controlled":"1","_id":"11488","date_updated":"2022-07-19T09:33:24Z","type":"journal_article","article_processing_charge":"No","doi":"10.1051/0004-6361/202142302","publisher":"EDP Sciences"},{"main_file_link":[{"url":"https://arxiv.org/abs/2202.06642","open_access":"1"}],"quality_controlled":"1","_id":"11497","date_updated":"2022-07-19T09:47:16Z","type":"journal_article","article_processing_charge":"No","doi":"10.1051/0004-6361/202141900","publisher":"EDP Sciences","date_published":"2022-03-25T00:00:00Z","acknowledgement":"We thank the referee for thoughtful and constructive comments that have improved the quality of this manuscript. Based on observations collected at the European Southern Observatory under ESO programme 1101.A-0127. This work made use of v2.2.1 of the Binary Population and Spectral Synthesis (BPASS) models as described in Eldridge et al. (2017) and Stanway & Eldridge (2018). A.F. acknowledges the support from grant PRIN MIUR2017-20173ML3WW_001. T.N. acknowledges support from Australian Research Council Laureate Fellowship FL180100060.","extern":"1","status":"public","publication":"Astronomy & Astrophysics","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift / galaxies: formation / galaxies: evolution / cosmology: observations"],"year":"2022","external_id":{"arxiv":["2202.06642"]},"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"publication_status":"published","abstract":[{"lang":"eng","text":"Context. The hydrogen Lyman α line is often the only measurable feature in optical spectra of high-redshift galaxies. Its shape and strength are influenced by radiative transfer processes and the properties of the underlying stellar population. High equivalent widths of several hundred Å are especially hard to explain by models and could point towards unusual stellar populations, for example with low metallicities, young stellar ages, and a top-heavy initial mass function. Other aspects influencing equivalent widths are the morphology of the galaxy and its gas properties.\r\nAims. The aim of this study is to better understand the connection between the Lyman α rest-frame equivalent width (EW0) and spectral properties as well as ultraviolet (UV) continuum morphology by obtaining reliable EW0 histograms for a statistical sample of galaxies and by assessing the fraction of objects with large equivalent widths.\r\nMethods. We used integral field spectroscopy from the Multi Unit Spectroscopic Explorer (MUSE) combined with broad-band data from the Hubble Space Telescope (HST) to measure EW0. We analysed the emission lines of 1920 Lyman α emitters (LAEs) detected in the full MUSE-Wide (one hour exposure time) and MUSE-Deep (ten hour exposure time) surveys and found UV continuum counterparts in archival HST data. We fitted the UV continuum photometric images using the Galfit software to gain morphological information on the rest-UV emission and fitted the spectra obtained from MUSE to determine the double peak fraction, asymmetry, full-width at half maximum, and flux of the Lyman α line.\r\nResults. The two surveys show different histograms of Lyman α EW0. In MUSE-Wide, 20% of objects have EW0 > 240 Å, while this fraction is only 11% in MUSE-Deep and ≈16% for the full sample. This includes objects without HST continuum counterparts (one-third of our sample), for which we give lower limits for EW0. The object with the highest securely measured EW0 has EW0 = 589 ± 193 Å (the highest lower limit being EW0 = 4464 Å). We investigate the connection between EW0 and Lyman α spectral or UV continuum morphological properties.\r\nConclusions. The survey depth has to be taken into account when studying EW0 distributions. We find that in general, high EW0 objects can have a wide range of spectral and UV morphological properties, which might reflect that the underlying causes for high EW0 values are equally varied."}],"intvolume":" 659","volume":659,"date_created":"2022-07-06T08:17:27Z","article_type":"original","day":"25","scopus_import":"1","author":[{"last_name":"Kerutt","full_name":"Kerutt, J.","first_name":"J."},{"first_name":"L.","last_name":"Wisotzki","full_name":"Wisotzki, L."},{"first_name":"A.","last_name":"Verhamme","full_name":"Verhamme, A."},{"full_name":"Schmidt, K. B.","last_name":"Schmidt","first_name":"K. B."},{"first_name":"F.","full_name":"Leclercq, F.","last_name":"Leclercq"},{"first_name":"E. C.","full_name":"Herenz, E. C.","last_name":"Herenz"},{"full_name":"Urrutia, T.","last_name":"Urrutia","first_name":"T."},{"full_name":"Garel, T.","last_name":"Garel","first_name":"T."},{"first_name":"T.","last_name":"Hashimoto","full_name":"Hashimoto, T."},{"full_name":"Maseda, M.","last_name":"Maseda","first_name":"M."},{"last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","first_name":"Jorryt J"},{"first_name":"H.","last_name":"Kusakabe","full_name":"Kusakabe, H."},{"last_name":"Schaye","full_name":"Schaye, J.","first_name":"J."},{"first_name":"J.","last_name":"Richard","full_name":"Richard, J."},{"first_name":"B.","last_name":"Guiderdoni","full_name":"Guiderdoni, B."},{"first_name":"V.","last_name":"Mauerhofer","full_name":"Mauerhofer, V."},{"first_name":"T.","last_name":"Nanayakkara","full_name":"Nanayakkara, T."},{"full_name":"Vitte, E.","last_name":"Vitte","first_name":"E."}],"title":"Equivalent widths of Lyman α emitters in MUSE-Wide and MUSE-Deep","oa_version":"Published Version","citation":{"apa":"Kerutt, J., Wisotzki, L., Verhamme, A., Schmidt, K. B., Leclercq, F., Herenz, E. C., … Vitte, E. (2022). Equivalent widths of Lyman α emitters in MUSE-Wide and MUSE-Deep. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202141900","mla":"Kerutt, J., et al. “Equivalent Widths of Lyman α Emitters in MUSE-Wide and MUSE-Deep.” Astronomy & Astrophysics, vol. 659, 183, EDP Sciences, 2022, doi:10.1051/0004-6361/202141900.","ista":"Kerutt J, Wisotzki L, Verhamme A, Schmidt KB, Leclercq F, Herenz EC, Urrutia T, Garel T, Hashimoto T, Maseda M, Matthee JJ, Kusakabe H, Schaye J, Richard J, Guiderdoni B, Mauerhofer V, Nanayakkara T, Vitte E. 2022. Equivalent widths of Lyman α emitters in MUSE-Wide and MUSE-Deep. Astronomy & Astrophysics. 659, 183.","chicago":"Kerutt, J., L. Wisotzki, A. Verhamme, K. B. Schmidt, F. Leclercq, E. C. Herenz, T. Urrutia, et al. “Equivalent Widths of Lyman α Emitters in MUSE-Wide and MUSE-Deep.” Astronomy & Astrophysics. EDP Sciences, 2022. https://doi.org/10.1051/0004-6361/202141900.","ieee":"J. Kerutt et al., “Equivalent widths of Lyman α emitters in MUSE-Wide and MUSE-Deep,” Astronomy & Astrophysics, vol. 659. EDP Sciences, 2022.","short":"J. Kerutt, L. Wisotzki, A. Verhamme, K.B. Schmidt, F. Leclercq, E.C. Herenz, T. Urrutia, T. Garel, T. Hashimoto, M. Maseda, J.J. Matthee, H. Kusakabe, J. Schaye, J. Richard, B. Guiderdoni, V. Mauerhofer, T. Nanayakkara, E. Vitte, Astronomy & Astrophysics 659 (2022).","ama":"Kerutt J, Wisotzki L, Verhamme A, et al. Equivalent widths of Lyman α emitters in MUSE-Wide and MUSE-Deep. Astronomy & Astrophysics. 2022;659. doi:10.1051/0004-6361/202141900"},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa":1,"language":[{"iso":"eng"}],"article_number":"183","arxiv":1,"month":"03"},{"volume":512,"article_type":"original","date_created":"2022-07-07T09:21:30Z","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"},{"full_name":"Naidu, Rohan P.","last_name":"Naidu","first_name":"Rohan P."},{"first_name":"Gabriele","full_name":"Pezzulli, Gabriele","last_name":"Pezzulli"},{"last_name":"Gronke","full_name":"Gronke, Max","first_name":"Max"},{"first_name":"David","full_name":"Sobral, David","last_name":"Sobral"},{"last_name":"Oesch","full_name":"Oesch, Pascal A.","first_name":"Pascal A."},{"first_name":"Matthew","full_name":"Hayes, Matthew","last_name":"Hayes"},{"full_name":"Erb, Dawn","last_name":"Erb","first_name":"Dawn"},{"last_name":"Schaerer","full_name":"Schaerer, Daniel","first_name":"Daniel"},{"first_name":"Ricardo","last_name":"Amorín","full_name":"Amorín, Ricardo"},{"last_name":"Tacchella","full_name":"Tacchella, Sandro","first_name":"Sandro"},{"last_name":"Ana Paulino-Afonso","full_name":"Ana Paulino-Afonso, Ana Paulino-Afonso","first_name":"Ana Paulino-Afonso"},{"first_name":"Mario","last_name":"Llerena","full_name":"Llerena, Mario"},{"full_name":"Calhau, João","last_name":"Calhau","first_name":"João"},{"full_name":"Röttgering, Huub","last_name":"Röttgering","first_name":"Huub"}],"day":"01","scopus_import":"1","oa_version":"Preprint","title":"(Re)Solving reionization with Lyα: How bright Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"publication_status":"published","abstract":[{"lang":"eng","text":"The cosmic ionizing emissivity from star-forming galaxies has long been anchored to UV luminosity functions. Here, we introduce an emissivity framework based on Lyα emitters (LAEs), which naturally hones in on the subset of galaxies responsible for the ionizing background due to the intimate connection between production and escape of Lyα and LyC photons. Using constraints on the escape fractions of bright LAEs (LLyα > 0.2L*) at z ≈ 2 obtained from resolved Lyα profiles, and arguing for their redshift-invariance, we show that: (i) quasars and LAEs together reproduce the relatively flat emissivity at z ≈ 2–6, which is non-trivial given the strong evolution in both the star formation density and quasar number density at these epochs and (ii) LAEs produce late and rapid reionization between z ≈ 6−9 under plausible assumptions. Within this framework, the >10 × rise in the UV population-averaged fesc between z ≈ 3–7 naturally arises due to the same phenomena that drive the growing LAE fraction with redshift. Generally, a LAE dominated emissivity yields a peak in the distribution of the ionizing budget with UV luminosity as reported in latest simulations. Using our adopted parameters (fesc=50 per cent, ξion = 1025.9 Hz erg−1 for half the bright LAEs), a highly ionizing minority of galaxies with MUV < −17 accounts for the entire ionizing budget from star-forming galaxies. Rapid flashes of LyC from such rare galaxies produce a ‘disco’ ionizing background. We conclude proposing tests to further develop our suggested Lyα-anchored formalism."}],"intvolume":" 512","month":"06","arxiv":1,"issue":"4","citation":{"mla":"Matthee, Jorryt J., et al. “(Re)Solving Reionization with Lyα: How Bright Lyα Emitters Account for the z ≈ 2 − 8 Cosmic Ionizing Background.” Monthly Notices of the Royal Astronomical Society, vol. 512, no. 4, Oxford University Press, 2022, pp. 5960–77, doi:10.1093/mnras/stac801.","apa":"Matthee, J. J., Naidu, R. P., Pezzulli, G., Gronke, M., Sobral, D., Oesch, P. A., … Röttgering, H. (2022). (Re)Solving reionization with Lyα: How bright Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stac801","ista":"Matthee JJ, Naidu RP, Pezzulli G, Gronke M, Sobral D, Oesch PA, Hayes M, Erb D, Schaerer D, Amorín R, Tacchella S, Ana Paulino-Afonso AP-A, Llerena M, Calhau J, Röttgering H. 2022. (Re)Solving reionization with Lyα: How bright Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background. Monthly Notices of the Royal Astronomical Society. 512(4), 5960–5977.","chicago":"Matthee, Jorryt J, Rohan P. Naidu, Gabriele Pezzulli, Max Gronke, David Sobral, Pascal A. Oesch, Matthew Hayes, et al. “(Re)Solving Reionization with Lyα: How Bright Lyα Emitters Account for the z ≈ 2 − 8 Cosmic Ionizing Background.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2022. https://doi.org/10.1093/mnras/stac801.","short":"J.J. Matthee, R.P. Naidu, G. Pezzulli, M. Gronke, D. Sobral, P.A. Oesch, M. Hayes, D. Erb, D. Schaerer, R. Amorín, S. Tacchella, A.P.-A. Ana Paulino-Afonso, M. Llerena, J. Calhau, H. Röttgering, Monthly Notices of the Royal Astronomical Society 512 (2022) 5960–5977.","ieee":"J. J. Matthee et al., “(Re)Solving reionization with Lyα: How bright Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background,” Monthly Notices of the Royal Astronomical Society, vol. 512, no. 4. Oxford University Press, pp. 5960–5977, 2022.","ama":"Matthee JJ, Naidu RP, Pezzulli G, et al. (Re)Solving reionization with Lyα: How bright Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background. Monthly Notices of the Royal Astronomical Society. 2022;512(4):5960-5977. doi:10.1093/mnras/stac801"},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa":1,"language":[{"iso":"eng"}],"date_updated":"2022-08-18T10:42:47Z","_id":"11521","type":"journal_article","doi":"10.1093/mnras/stac801","article_processing_charge":"No","publisher":"Oxford University Press","main_file_link":[{"url":"https://arxiv.org/abs/2110.11967","open_access":"1"}],"quality_controlled":"1","page":"5960-5977","keyword":["galaxies: high-redshift","intergalactic medium","cosmology: observations","dark ages","reionization","first stars","ultraviolet: galaxies"],"year":"2022","external_id":{"arxiv":["2110.11967"]},"date_published":"2022-06-01T00:00:00Z","acknowledgement":"We thank an anonymous referee for an encouraging and constructive report that helped improving the quality of this work. We acknowledge illuminating conversations with Xiaohan Wu, Chris Cain, Anna-Christina Eilers, Simon Lilly and Ruari Mackenzie. RPN gratefully acknowledges an Ashford Fellowship granted by Harvard University. MG was supported by NASA through the NASA Hubble Fellowship grant HST-HF2-51409. PO acknowledges support from the Swiss National Science Foundation through the SNSF Professorship grant 190079. GP acknowledges support from the Netherlands Research School for Astronomy (NOVA). MH is fellow of the Knut and Alice Wallenberg Foundation. DE is supported by the US National Science Foundation (NSF) through Astronomy & Astrophysics grant AST-1909198. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant No. 140. RA acknowledges support from Fondecyt Regular Grant 1202007. ST is supported by the 2021 Research Fund 1.210134.01 of UNIST (Ulsan National Institute of Science & Technology). MLl acknowledges support from the ANID/Scholarship Program/Doctorado Nacional/2019-21191036. JC acknowledges support from the Spanish Ministry of Science and Innovation, project PID2019-107408GB-C43 (ESTALLIDOS) and from Gobierno de Canarias through EU FEDER funding, project PID2020010050.","extern":"1","publication":"Monthly Notices of the Royal Astronomical Society","status":"public"},{"extern":"1","status":"public","publication":"Astronomy & Astrophysics","acknowledgement":"We warmly thank ESO Paranal staff for their great professional support during all MXDF GTO observing runs. We thank the anonymous referee for a careful reading of the manuscript and helpful comments. We also thank Matthew Lehnert for fruitful discussions. RB, AF, SC acknowledge support from the ERC advanced grant 339659-MUSICOS. JB acknowledges support by Fundação para a Ciência e a Tecnologia (FCT) through the research grants UID/FIS/04434/2019, UIDB/04434/2020, UIDP/04434/2020 and through the Investigador FCT Contract No. IF/01654/2014/CP1215/CT0003. TG, AV acknowledges support from the European Research Council under grant agreement ERC-stg-757258 (TRIPLE). DM acknowledges A. Dabbech for useful interactions about IUWT and support from the GDR ISIS through the Projets exploratoires program (project TASTY). AF acknowledges the support from grant PRIN MIUR2017-20173ML3WW_001. SLZ acknowledges support by The Netherlands Organisation for Scientific Research (NWO) through a TOP Grant Module 1 under project number 614.001.652. This research made use of the following open-source software and we are thankful to the developers of these: GNU Octave (Eaton et al. 2018) and its statistics, signal and image packages, the Python packages Matplotlib (Hunter 2007), Numpy (van der Walt et al. 2010), MPDAF (Piqueras et al. 2017), Astropy (Astropy Collaboration 2018), PyWavelets (Lee et al. 2019).","date_published":"2021-03-18T00:00:00Z","external_id":{"arxiv":["2102.05516"]},"year":"2021","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift / galaxies: groups: general / cosmology: observations"],"quality_controlled":"1","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2102.05516"}],"publisher":"EDP Sciences","article_processing_charge":"No","doi":"10.1051/0004-6361/202039887","type":"journal_article","_id":"11500","date_updated":"2022-07-19T09:34:57Z","language":[{"iso":"eng"}],"oa":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"ama":"Bacon R, Mary D, Garel T, et al. The MUSE Extremely Deep Field: The cosmic web in emission at high redshift. Astronomy & Astrophysics. 2021;647. doi:10.1051/0004-6361/202039887","short":"R. Bacon, D. Mary, T. Garel, J. Blaizot, M. Maseda, J. Schaye, L. Wisotzki, S. Conseil, J. Brinchmann, F. Leclercq, V. Abril-Melgarejo, L. Boogaard, N.F. Bouché, T. Contini, A. Feltre, B. Guiderdoni, C. Herenz, W. Kollatschny, H. Kusakabe, J.J. Matthee, L. Michel-Dansac, T. Nanayakkara, J. Richard, M. Roth, K.B. Schmidt, M. Steinmetz, L. Tresse, T. Urrutia, A. Verhamme, P.M. Weilbacher, J. Zabl, S.L. Zoutendijk, Astronomy & Astrophysics 647 (2021).","ieee":"R. Bacon et al., “The MUSE Extremely Deep Field: The cosmic web in emission at high redshift,” Astronomy & Astrophysics, vol. 647. EDP Sciences, 2021.","chicago":"Bacon, R., D. Mary, T. Garel, J. Blaizot, M. Maseda, J. Schaye, L. Wisotzki, et al. “The MUSE Extremely Deep Field: The Cosmic Web in Emission at High Redshift.” Astronomy & Astrophysics. EDP Sciences, 2021. https://doi.org/10.1051/0004-6361/202039887.","ista":"Bacon R, Mary D, Garel T, Blaizot J, Maseda M, Schaye J, Wisotzki L, Conseil S, Brinchmann J, Leclercq F, Abril-Melgarejo V, Boogaard L, Bouché NF, Contini T, Feltre A, Guiderdoni B, Herenz C, Kollatschny W, Kusakabe H, Matthee JJ, Michel-Dansac L, Nanayakkara T, Richard J, Roth M, Schmidt KB, Steinmetz M, Tresse L, Urrutia T, Verhamme A, Weilbacher PM, Zabl J, Zoutendijk SL. 2021. The MUSE Extremely Deep Field: The cosmic web in emission at high redshift. Astronomy & Astrophysics. 647, A107.","mla":"Bacon, R., et al. “The MUSE Extremely Deep Field: The Cosmic Web in Emission at High Redshift.” Astronomy & Astrophysics, vol. 647, A107, EDP Sciences, 2021, doi:10.1051/0004-6361/202039887.","apa":"Bacon, R., Mary, D., Garel, T., Blaizot, J., Maseda, M., Schaye, J., … Zoutendijk, S. L. (2021). The MUSE Extremely Deep Field: The cosmic web in emission at high redshift. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202039887"},"arxiv":1,"month":"03","article_number":"A107","intvolume":" 647","abstract":[{"text":"We report the discovery of diffuse extended Lyα emission from redshift 3.1 to 4.5, tracing cosmic web filaments on scales of 2.5−4 cMpc. These structures have been observed in overdensities of Lyα emitters in the MUSE Extremely Deep Field, a 140 h deep MUSE observation located in the Hubble Ultra-Deep Field. Among the 22 overdense regions identified, five are likely to harbor very extended Lyα emission at high significance with an average surface brightness of 5 × 10−20 erg s−1 cm−2 arcsec−2. Remarkably, 70% of the total Lyα luminosity from these filaments comes from beyond the circumgalactic medium of any identified Lyα emitter. Fluorescent Lyα emission powered by the cosmic UV background can only account for less than 34% of this emission at z ≈ 3 and for not more than 10% at higher redshift. We find that the bulk of this diffuse emission can be reproduced by the unresolved Lyα emission of a large population of ultra low-luminosity Lyα emitters (< 1040 erg s−1), provided that the faint end of the Lyα luminosity function is steep (α ⪅ −1.8), it extends down to luminosities lower than 1038 − 1037 erg s−1, and the clustering of these Lyα emitters is significant (filling factor < 1/6). If these Lyα emitters are powered by star formation, then this implies their luminosity function needs to extend down to star formation rates < 10−4 M⊙ yr−1. These observations provide the first detection of the cosmic web in Lyα emission in typical filamentary environments and the first observational clue indicating the existence of a large population of ultra low-luminosity Lyα emitters at high redshift.","lang":"eng"}],"publication_status":"published","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"oa_version":"Published Version","title":"The MUSE Extremely Deep Field: The cosmic web in emission at high redshift","scopus_import":"1","day":"18","author":[{"last_name":"Bacon","full_name":"Bacon, R.","first_name":"R."},{"full_name":"Mary, D.","last_name":"Mary","first_name":"D."},{"first_name":"T.","full_name":"Garel, T.","last_name":"Garel"},{"first_name":"J.","full_name":"Blaizot, J.","last_name":"Blaizot"},{"first_name":"M.","last_name":"Maseda","full_name":"Maseda, M."},{"first_name":"J.","full_name":"Schaye, J.","last_name":"Schaye"},{"first_name":"L.","full_name":"Wisotzki, L.","last_name":"Wisotzki"},{"first_name":"S.","last_name":"Conseil","full_name":"Conseil, S."},{"full_name":"Brinchmann, J.","last_name":"Brinchmann","first_name":"J."},{"full_name":"Leclercq, F.","last_name":"Leclercq","first_name":"F."},{"first_name":"V.","full_name":"Abril-Melgarejo, V.","last_name":"Abril-Melgarejo"},{"last_name":"Boogaard","full_name":"Boogaard, L.","first_name":"L."},{"first_name":"N. F.","last_name":"Bouché","full_name":"Bouché, N. F."},{"full_name":"Contini, T.","last_name":"Contini","first_name":"T."},{"last_name":"Feltre","full_name":"Feltre, A.","first_name":"A."},{"first_name":"B.","full_name":"Guiderdoni, B.","last_name":"Guiderdoni"},{"full_name":"Herenz, C.","last_name":"Herenz","first_name":"C."},{"full_name":"Kollatschny, W.","last_name":"Kollatschny","first_name":"W."},{"full_name":"Kusakabe, H.","last_name":"Kusakabe","first_name":"H."},{"first_name":"Jorryt J","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee"},{"full_name":"Michel-Dansac, L.","last_name":"Michel-Dansac","first_name":"L."},{"full_name":"Nanayakkara, T.","last_name":"Nanayakkara","first_name":"T."},{"first_name":"J.","full_name":"Richard, J.","last_name":"Richard"},{"last_name":"Roth","full_name":"Roth, M.","first_name":"M."},{"first_name":"K. B.","full_name":"Schmidt, K. B.","last_name":"Schmidt"},{"first_name":"M.","full_name":"Steinmetz, M.","last_name":"Steinmetz"},{"first_name":"L.","last_name":"Tresse","full_name":"Tresse, L."},{"first_name":"T.","last_name":"Urrutia","full_name":"Urrutia, T."},{"last_name":"Verhamme","full_name":"Verhamme, A.","first_name":"A."},{"first_name":"P. M.","last_name":"Weilbacher","full_name":"Weilbacher, P. M."},{"last_name":"Zabl","full_name":"Zabl, J.","first_name":"J."},{"first_name":"S. L.","full_name":"Zoutendijk, S. L.","last_name":"Zoutendijk"}],"date_created":"2022-07-06T09:31:50Z","article_type":"original","volume":647},{"title":"The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6","oa_version":"Published Version","author":[{"first_name":"Haruka","last_name":"Kusakabe","full_name":"Kusakabe, Haruka"},{"full_name":"Blaizot, Jérémy","last_name":"Blaizot","first_name":"Jérémy"},{"full_name":"Garel, Thibault","last_name":"Garel","first_name":"Thibault"},{"full_name":"Verhamme, Anne","last_name":"Verhamme","first_name":"Anne"},{"last_name":"Bacon","full_name":"Bacon, Roland","first_name":"Roland"},{"last_name":"Richard","full_name":"Richard, Johan","first_name":"Johan"},{"full_name":"Hashimoto, Takuya","last_name":"Hashimoto","first_name":"Takuya"},{"first_name":"Hanae","last_name":"Inami","full_name":"Inami, Hanae"},{"full_name":"Conseil, Simon","last_name":"Conseil","first_name":"Simon"},{"last_name":"Guiderdoni","full_name":"Guiderdoni, Bruno","first_name":"Bruno"},{"first_name":"Alyssa B.","full_name":"Drake, Alyssa B.","last_name":"Drake"},{"last_name":"Christian Herenz","full_name":"Christian Herenz, Edmund","first_name":"Edmund"},{"first_name":"Joop","last_name":"Schaye","full_name":"Schaye, Joop"},{"last_name":"Oesch","full_name":"Oesch, Pascal","first_name":"Pascal"},{"last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","first_name":"Jorryt J"},{"first_name":"Raffaella","full_name":"Anna Marino, Raffaella","last_name":"Anna Marino"},{"full_name":"Borello Schmidt, Kasper","last_name":"Borello Schmidt","first_name":"Kasper"},{"full_name":"Pelló, Roser","last_name":"Pelló","first_name":"Roser"},{"first_name":"Michael","full_name":"Maseda, Michael","last_name":"Maseda"},{"first_name":"Floriane","full_name":"Leclercq, Floriane","last_name":"Leclercq"},{"last_name":"Kerutt","full_name":"Kerutt, Josephine","first_name":"Josephine"},{"last_name":"Mahler","full_name":"Mahler, Guillaume","first_name":"Guillaume"}],"scopus_import":"1","day":"03","article_type":"original","date_created":"2022-07-06T09:50:48Z","volume":638,"abstract":[{"text":"Context. The Lyα emitter (LAE) fraction, XLAE, is a potentially powerful probe of the evolution of the intergalactic neutral hydrogen gas fraction. However, uncertainties in the measurement of XLAE are still under debate.\r\nAims. Thanks to deep data obtained with the integral field spectrograph Multi Unit Spectroscopic Explorer (MUSE), we can measure the evolution of the LAE fraction homogeneously over a wide redshift range of z ≈ 3–6 for UV-faint galaxies (down to UV magnitudes of M1500 ≈ −17.75). This is a significantly fainter range than in former studies (M1500 ≤ −18.75) and it allows us to probe the bulk of the population of high-redshift star-forming galaxies.\r\nMethods. We constructed a UV-complete photometric-redshift sample following UV luminosity functions and measured the Lyα emission with MUSE using the latest (second) data release from the MUSE Hubble Ultra Deep Field Survey.\r\nResults. We derived the redshift evolution of XLAE for M1500 ∈ [ − 21.75; −17.75] for the first time with a equivalent width range EW(Lyα) ≥ 65 Å and found low values of XLAE ≲ 30% at z ≲ 6. The best-fit linear relation is XLAE = 0.07+0.06−0.03z − 0.22+0.12−0.24. For M1500 ∈ [ − 20.25; −18.75] and EW(Lyα) ≥ 25 Å, our XLAE values are consistent with those in the literature within 1σ at z ≲ 5, but our median values are systematically lower than reported values over the whole redshift range. In addition, we do not find a significant dependence of XLAE on M1500 for EW(Lyα) ≥ 50 Å at z ≈ 3–4, in contrast with previous work. The differences in XLAE mainly arise from selection biases for Lyman Break Galaxies (LBGs) in the literature: UV-faint LBGs are more easily selected if they have strong Lyα emission, hence XLAE is biased towards higher values when those samples are used.\r\nConclusions. Our results suggest either a lower increase of XLAE towards z ≈ 6 than previously suggested, or even a turnover of XLAE at z ≈ 5.5, which may be the signature of a late or patchy reionization process. We compared our results with predictions from a cosmological galaxy evolution model. We find that a model with a bursty star formation (SF) can reproduce our observed LAE fractions much better than models where SF is a smooth function of time.","lang":"eng"}],"intvolume":" 638","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"publication_status":"published","arxiv":1,"month":"06","article_number":"A12","language":[{"iso":"eng"}],"oa":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"ieee":"H. Kusakabe et al., “The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6,” Astronomy & Astrophysics, vol. 638. EDP Sciences, 2020.","short":"H. Kusakabe, J. Blaizot, T. Garel, A. Verhamme, R. Bacon, J. Richard, T. Hashimoto, H. Inami, S. Conseil, B. Guiderdoni, A.B. Drake, E. Christian Herenz, J. Schaye, P. Oesch, J.J. Matthee, R. Anna Marino, K. Borello Schmidt, R. Pelló, M. Maseda, F. Leclercq, J. Kerutt, G. Mahler, Astronomy & Astrophysics 638 (2020).","ama":"Kusakabe H, Blaizot J, Garel T, et al. The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6. Astronomy & Astrophysics. 2020;638. doi:10.1051/0004-6361/201937340","apa":"Kusakabe, H., Blaizot, J., Garel, T., Verhamme, A., Bacon, R., Richard, J., … Mahler, G. (2020). The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201937340","mla":"Kusakabe, Haruka, et al. “The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα Emitter Fraction from z = 3 to z = 6.” Astronomy & Astrophysics, vol. 638, A12, EDP Sciences, 2020, doi:10.1051/0004-6361/201937340.","chicago":"Kusakabe, Haruka, Jérémy Blaizot, Thibault Garel, Anne Verhamme, Roland Bacon, Johan Richard, Takuya Hashimoto, et al. “The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα Emitter Fraction from z = 3 to z = 6.” Astronomy & Astrophysics. EDP Sciences, 2020. https://doi.org/10.1051/0004-6361/201937340.","ista":"Kusakabe H, Blaizot J, Garel T, Verhamme A, Bacon R, Richard J, Hashimoto T, Inami H, Conseil S, Guiderdoni B, Drake AB, Christian Herenz E, Schaye J, Oesch P, Matthee JJ, Anna Marino R, Borello Schmidt K, Pelló R, Maseda M, Leclercq F, Kerutt J, Mahler G. 2020. The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6. Astronomy & Astrophysics. 638, A12."},"publisher":"EDP Sciences","doi":"10.1051/0004-6361/201937340","article_processing_charge":"No","type":"journal_article","date_updated":"2022-07-19T09:35:20Z","_id":"11503","quality_controlled":"1","main_file_link":[{"url":"https://arxiv.org/abs/2003.12083","open_access":"1"}],"external_id":{"arxiv":["2003.12083"]},"year":"2020","keyword":["Space and Planetary Science","Astronomy and Astrophysics","dark ages / reionization / first stars / early Universe / cosmology: observations / galaxies: evolution / galaxies: high-redshift / intergalactic medium"],"publication":"Astronomy & Astrophysics","status":"public","extern":"1","date_published":"2020-06-03T00:00:00Z","acknowledgement":"We thank the anonymous referee for constructive comments and suggestions. We would like to express our gratitude to Stephane De Barros and Pablo Arrabal Haro for kindly providing their data plotted in Figs. 1, 2, and 8. We are grateful to Kazuhiro Shimasaku, Masami Ouchi, Rieko Momose, Daniel Schaerer, Hidenobu Yajima, Taku Okamura, Makoto Ando, and Hinako Goto for giving insightful comments and suggestions. This work is based on observations taken by VLT, which is operated by European Southern Observatory. This research made use of Astropy (http://www.astropy.org), which is a community-developed core Python package for Astronomy (Astropy Collaboration 2013, 2018), MARZ, MPDAF, and matplotlib (Hunter 2007). H.K. acknowledges support from Japan Society for the Promotion of Science (JSPS) through the JSPS Research Fellowship for Young Scientists and Overseas Challenge Program for Young Researchers. AV acknowledges support from the ERC starting grant 757258-TRIPLE and the SNF Professorship 176808-TRIPLE. This work was supported by the project FOGHAR (Agence Nationale de la Recherche, ANR-13-BS05-0010-02). JB acknowledges support from the ORAGE project from the Agence Nationale de la Recherche under grant ANR-14-CE33-0016-03. JR acknowledges support from the ERC starting grant 336736-CALENDS. T. H. acknowledges supports by the Grant-inAid for Scientic Research 19J01620."},{"status":"public","extern":"1","publication":"Astronomy & Astrophysics","acknowledgement":"F.L., R.B., and S.C. acknowledge support from the ERC advanced grant 339659-MUSICOS. F.L., T.G., H.K., and A.V. acknowledge support from the ERC starting grant ERC-757258-TRIPLE. A.C. and J.R. acknowledge support from the ERC starting grant 336736-CALENDS. J.B. acknowledges support by FCT/MCTES through national funds (PID-DAC) by grant UID/FIS/04434/2019 and through Investigador FCT Contract No.IF/01654/2014/CP1215/CT0003. T.H. was supported by Leading Initiative for Excellent Young Researchers, MEXT, Japan.","date_published":"2020-03-11T00:00:00Z","external_id":{"arxiv":["2002.05731"]},"year":"2020","keyword":["Space and Planetary Science","Astronomy and Astrophysics galaxies: high-redshift / galaxies: formation / galaxies: evolution / cosmology: observations"],"quality_controlled":"1","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2002.05731"}],"publisher":"EDP Sciences","doi":"10.1051/0004-6361/201937339","article_processing_charge":"No","type":"journal_article","date_updated":"2022-07-19T09:36:58Z","_id":"11504","language":[{"iso":"eng"}],"oa":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"chicago":"Leclercq, Floriane, Roland Bacon, Anne Verhamme, Thibault Garel, Jérémy Blaizot, Jarle Brinchmann, Sebastiano Cantalupo, et al. “The MUSE Hubble Ultra Deep Field Survey: XIII. Spatially Resolved Spectral Properties of Lyman α Haloes around Star-Forming Galaxies at z > 3.” Astronomy & Astrophysics. EDP Sciences, 2020. https://doi.org/10.1051/0004-6361/201937339.","ista":"Leclercq F, Bacon R, Verhamme A, Garel T, Blaizot J, Brinchmann J, Cantalupo S, Claeyssens A, Conseil S, Contini T, Hashimoto T, Herenz EC, Kusakabe H, Marino RA, Maseda M, Matthee JJ, Mitchell P, Pezzulli G, Richard J, Schmidt KB, Wisotzki L. 2020. The MUSE Hubble Ultra Deep field survey: XIII. Spatially resolved spectral properties of Lyman α haloes around star-forming galaxies at z > 3. Astronomy & Astrophysics. 635, A82.","mla":"Leclercq, Floriane, et al. “The MUSE Hubble Ultra Deep Field Survey: XIII. Spatially Resolved Spectral Properties of Lyman α Haloes around Star-Forming Galaxies at z > 3.” Astronomy & Astrophysics, vol. 635, A82, EDP Sciences, 2020, doi:10.1051/0004-6361/201937339.","apa":"Leclercq, F., Bacon, R., Verhamme, A., Garel, T., Blaizot, J., Brinchmann, J., … Wisotzki, L. (2020). The MUSE Hubble Ultra Deep field survey: XIII. Spatially resolved spectral properties of Lyman α haloes around star-forming galaxies at z > 3. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201937339","ama":"Leclercq F, Bacon R, Verhamme A, et al. The MUSE Hubble Ultra Deep field survey: XIII. Spatially resolved spectral properties of Lyman α haloes around star-forming galaxies at z > 3. Astronomy & Astrophysics. 2020;635. doi:10.1051/0004-6361/201937339","short":"F. Leclercq, R. Bacon, A. Verhamme, T. Garel, J. Blaizot, J. Brinchmann, S. Cantalupo, A. Claeyssens, S. Conseil, T. Contini, T. Hashimoto, E.C. Herenz, H. Kusakabe, R.A. Marino, M. Maseda, J.J. Matthee, P. Mitchell, G. Pezzulli, J. Richard, K.B. Schmidt, L. Wisotzki, Astronomy & Astrophysics 635 (2020).","ieee":"F. Leclercq et al., “The MUSE Hubble Ultra Deep field survey: XIII. Spatially resolved spectral properties of Lyman α haloes around star-forming galaxies at z > 3,” Astronomy & Astrophysics, vol. 635. EDP Sciences, 2020."},"month":"03","arxiv":1,"article_number":"A82","intvolume":" 635","abstract":[{"lang":"eng","text":"We present spatially resolved maps of six individually-detected Lyman α haloes (LAHs) as well as a first statistical analysis of the Lyman α (Lyα) spectral signature in the circum-galactic medium of high-redshift star-forming galaxies (−17.5 > MUV > −21.5) using the Multi-Unit Spectroscopic Explorer. Our resolved spectroscopic analysis of the LAHs reveals significant intrahalo variations of the Lyα line profile. Using a three-dimensional two-component model for the Lyα emission, we measured the full width at half maximum (FWHM), the peak velocity shift, and the asymmetry of the Lyα line in the core and in the halo of 19 galaxies. We find that the Lyα line shape is statistically different in the halo compared to the core (in terms of width, peak wavelength, and asymmetry) for ≈40% of our galaxies. Similarly to object-by-object based studies and a recent resolved study using lensing, we find a correlation between the peak velocity shift and the width of the Lyα line both at the interstellar and circum-galactic scales. This trend has been predicted by radiative transfer simulations of galactic winds as a result of resonant scattering in outflows. While there is a lack of correlation between the spectral properties and the spatial scale lengths of our LAHs, we find a correlation between the width of the line in the LAH and the halo flux fraction. Interestingly, UV bright galaxies (MUV < −20) show broader, more redshifted, and less asymmetric Lyα lines in their haloes. The most significant correlation found is for the FWHM of the line and the UV continuum slope of the galaxy, suggesting that the redder galaxies have broader Lyα lines. The generally broad and red line shapes found in the halo component suggest that the Lyα haloes are powered either by scattering processes through an outflowing medium, fluorescent emission from outflowing cold clumps of gas, or a mix of both. Considering the large diversity of the Lyα line profiles observed in our sample and the lack of strong correlation, the interpretation of our results is still broadly open and underlines the need for realistic spatially resolved models of the LAHs."}],"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"publication_status":"published","title":"The MUSE Hubble Ultra Deep field survey: XIII. Spatially resolved spectral properties of Lyman α haloes around star-forming galaxies at z > 3","oa_version":"Published Version","author":[{"first_name":"Floriane","full_name":"Leclercq, Floriane","last_name":"Leclercq"},{"first_name":"Roland","full_name":"Bacon, Roland","last_name":"Bacon"},{"first_name":"Anne","full_name":"Verhamme, Anne","last_name":"Verhamme"},{"last_name":"Garel","full_name":"Garel, Thibault","first_name":"Thibault"},{"full_name":"Blaizot, Jérémy","last_name":"Blaizot","first_name":"Jérémy"},{"full_name":"Brinchmann, Jarle","last_name":"Brinchmann","first_name":"Jarle"},{"first_name":"Sebastiano","last_name":"Cantalupo","full_name":"Cantalupo, Sebastiano"},{"last_name":"Claeyssens","full_name":"Claeyssens, Adélaïde","first_name":"Adélaïde"},{"full_name":"Conseil, Simon","last_name":"Conseil","first_name":"Simon"},{"first_name":"Thierry","last_name":"Contini","full_name":"Contini, Thierry"},{"full_name":"Hashimoto, Takuya","last_name":"Hashimoto","first_name":"Takuya"},{"first_name":"Edmund Christian","last_name":"Herenz","full_name":"Herenz, Edmund Christian"},{"full_name":"Kusakabe, Haruka","last_name":"Kusakabe","first_name":"Haruka"},{"first_name":"Raffaella Anna","full_name":"Marino, Raffaella Anna","last_name":"Marino"},{"last_name":"Maseda","full_name":"Maseda, Michael","first_name":"Michael"},{"last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","first_name":"Jorryt J"},{"first_name":"Peter","full_name":"Mitchell, Peter","last_name":"Mitchell"},{"first_name":"Gabriele","last_name":"Pezzulli","full_name":"Pezzulli, Gabriele"},{"last_name":"Richard","full_name":"Richard, Johan","first_name":"Johan"},{"last_name":"Schmidt","full_name":"Schmidt, Kasper Borello","first_name":"Kasper Borello"},{"first_name":"Lutz","last_name":"Wisotzki","full_name":"Wisotzki, Lutz"}],"scopus_import":"1","day":"11","article_type":"original","date_created":"2022-07-06T09:56:20Z","volume":635},{"type":"journal_article","date_updated":"2022-08-18T11:04:05Z","_id":"11529","publisher":"Oxford University Press","doi":"10.1093/mnras/staa2550","article_processing_charge":"No","quality_controlled":"1","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2008.01731"}],"page":"3043-3059","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","dark ages","reionization","first stars","cosmology: observations"],"external_id":{"arxiv":["2008.01731"]},"year":"2020","date_published":"2020-10-01T00:00:00Z","extern":"1","publication":"Monthly Notices of the Royal Astronomical Society","status":"public","article_type":"original","date_created":"2022-07-07T10:36:01Z","volume":498,"oa_version":"Preprint","title":"The nature of CR7 revealed with MUSE: A young starburst powering extended Ly α emission at z = 6.6","author":[{"last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"},{"first_name":"Gabriele","last_name":"Pezzulli","full_name":"Pezzulli, Gabriele"},{"last_name":"Mackenzie","full_name":"Mackenzie, Ruari","first_name":"Ruari"},{"first_name":"Sebastiano","last_name":"Cantalupo","full_name":"Cantalupo, Sebastiano"},{"first_name":"Haruka","full_name":"Kusakabe, Haruka","last_name":"Kusakabe"},{"full_name":"Leclercq, Floriane","last_name":"Leclercq","first_name":"Floriane"},{"first_name":"David","full_name":"Sobral, David","last_name":"Sobral"},{"full_name":"Richard, Johan","last_name":"Richard","first_name":"Johan"},{"last_name":"Wisotzki","full_name":"Wisotzki, Lutz","first_name":"Lutz"},{"full_name":"Lilly, Simon","last_name":"Lilly","first_name":"Simon"},{"last_name":"Boogaard","full_name":"Boogaard, Leindert","first_name":"Leindert"},{"last_name":"Marino","full_name":"Marino, Raffaella","first_name":"Raffaella"},{"first_name":"Michael","full_name":"Maseda, Michael","last_name":"Maseda"},{"last_name":"Nanayakkara","full_name":"Nanayakkara, Themiya","first_name":"Themiya"}],"scopus_import":"1","day":"01","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"publication_status":"published","intvolume":" 498","abstract":[{"lang":"eng","text":"CR7 is among the most luminous Ly α emitters (LAEs) known at z = 6.6 and consists of at least three UV components that are surrounded by Ly α emission. Previous studies have suggested that it may host an extreme ionizing source. Here, we present deep integral field spectroscopy of CR7 with VLT/Multi Unit Spectroscopic Explorer (MUSE). We measure extended emission with a similar halo scale length as typical LAEs at z ≈ 5. CR7’s Ly α halo is clearly elongated along the direction connecting the multiple components, likely tracing the underlying gas distribution. The Ly α emission originates almost exclusively from the brightest UV component, but we also identify a faint kinematically distinct Ly α emitting region nearby a fainter component. Combined with new near-infrared data, the MUSE data show that the rest-frame Ly α equivalent width (EW) is ≈100 Å. This is a factor 4 higher than the EW measured in low-redshift analogues with carefully matched Ly α profiles (and thus arguably H I column density), but this EW can plausibly be explained by star formation. Alternative scenarios requiring active galactic nucleus (AGN) powering are also disfavoured by the narrower and steeper Ly α spectrum and much smaller IR to UV ratio compared to obscured AGN in other Ly α blobs. CR7’s Ly α emission, while extremely luminous, resembles the emission in more common LAEs at lower redshifts very well and is likely powered by a young metal-poor starburst."}],"month":"10","arxiv":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","issue":"2","citation":{"ama":"Matthee JJ, Pezzulli G, Mackenzie R, et al. The nature of CR7 revealed with MUSE: A young starburst powering extended Ly α emission at z = 6.6. Monthly Notices of the Royal Astronomical Society. 2020;498(2):3043-3059. doi:10.1093/mnras/staa2550","ieee":"J. J. Matthee et al., “The nature of CR7 revealed with MUSE: A young starburst powering extended Ly α emission at z = 6.6,” Monthly Notices of the Royal Astronomical Society, vol. 498, no. 2. Oxford University Press, pp. 3043–3059, 2020.","short":"J.J. Matthee, G. Pezzulli, R. Mackenzie, S. Cantalupo, H. Kusakabe, F. Leclercq, D. Sobral, J. Richard, L. Wisotzki, S. Lilly, L. Boogaard, R. Marino, M. Maseda, T. Nanayakkara, Monthly Notices of the Royal Astronomical Society 498 (2020) 3043–3059.","ista":"Matthee JJ, Pezzulli G, Mackenzie R, Cantalupo S, Kusakabe H, Leclercq F, Sobral D, Richard J, Wisotzki L, Lilly S, Boogaard L, Marino R, Maseda M, Nanayakkara T. 2020. The nature of CR7 revealed with MUSE: A young starburst powering extended Ly α emission at z = 6.6. Monthly Notices of the Royal Astronomical Society. 498(2), 3043–3059.","chicago":"Matthee, Jorryt J, Gabriele Pezzulli, Ruari Mackenzie, Sebastiano Cantalupo, Haruka Kusakabe, Floriane Leclercq, David Sobral, et al. “The Nature of CR7 Revealed with MUSE: A Young Starburst Powering Extended Ly α Emission at z = 6.6.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2020. https://doi.org/10.1093/mnras/staa2550.","apa":"Matthee, J. J., Pezzulli, G., Mackenzie, R., Cantalupo, S., Kusakabe, H., Leclercq, F., … Nanayakkara, T. (2020). The nature of CR7 revealed with MUSE: A young starburst powering extended Ly α emission at z = 6.6. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staa2550","mla":"Matthee, Jorryt J., et al. “The Nature of CR7 Revealed with MUSE: A Young Starburst Powering Extended Ly α Emission at z = 6.6.” Monthly Notices of the Royal Astronomical Society, vol. 498, no. 2, Oxford University Press, 2020, pp. 3043–59, doi:10.1093/mnras/staa2550."},"language":[{"iso":"eng"}],"oa":1},{"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"publication_status":"published","abstract":[{"text":"The observed properties of the Lyman-α (Ly α) emission line are a powerful probe of neutral gas in and around galaxies. We present spatially resolved Ly α spectroscopy with VLT/MUSE targeting VR7, a UV-luminous galaxy at z = 6.532 with moderate Ly α equivalent width (EW0 ≈ 38 Å). These data are combined with deep resolved [CII]158μm spectroscopy obtained with ALMA and UV imaging from HST and we also detect UV continuum with MUSE. Ly α emission is clearly detected with S/N ≈ 40 and FWHM of 374 km s−1. Ly α and [C II] are similarly extended beyond the UV, with effective radius reff = 2.1 ± 0.2 kpc for a single exponential model or reff,Lyα,halo=3.45+1.08−0.87 kpc when measured jointly with the UV continuum. The Ly α profile is broader and redshifted with respect to the [C II] line (by 213 km s−1), but there are spatial variations that are qualitatively similar in both lines and coincide with resolved UV components. This suggests that the emission originates from two components with plausibly different H I column densities. We place VR7 in the context of other galaxies at similar and lower redshift. The Ly α halo scale length is similar at different redshifts and velocity shifts with respect to the systemic are typically smaller. Overall, we find little indications of a more neutral vicinity at higher redshift. This means that the local (∼10 kpc) neutral gas conditions that determine the observed Ly α properties in VR7 resemble the conditions in post-reionization galaxies.","lang":"eng"}],"intvolume":" 492","volume":492,"article_type":"original","date_created":"2022-07-07T12:21:36Z","author":[{"orcid":"0000-0003-2871-127X","first_name":"Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J"},{"full_name":"Sobral, David","last_name":"Sobral","first_name":"David"},{"last_name":"Gronke","full_name":"Gronke, Max","first_name":"Max"},{"full_name":"Pezzulli, Gabriele","last_name":"Pezzulli","first_name":"Gabriele"},{"full_name":"Cantalupo, Sebastiano","last_name":"Cantalupo","first_name":"Sebastiano"},{"last_name":"Röttgering","full_name":"Röttgering, Huub","first_name":"Huub"},{"first_name":"Behnam","last_name":"Darvish","full_name":"Darvish, Behnam"},{"first_name":"Sérgio","last_name":"Santos","full_name":"Santos, Sérgio"}],"scopus_import":"1","day":"01","oa_version":"Preprint","title":"Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 ","issue":"2","citation":{"chicago":"Matthee, Jorryt J, David Sobral, Max Gronke, Gabriele Pezzulli, Sebastiano Cantalupo, Huub Röttgering, Behnam Darvish, and Sérgio Santos. “Resolved Lyman-α Properties of a Luminous Lyman-Break Galaxy in a Large Ionized Bubble at z = 6.53 .” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2020. https://doi.org/10.1093/mnras/stz3554.","ista":"Matthee JJ, Sobral D, Gronke M, Pezzulli G, Cantalupo S, Röttgering H, Darvish B, Santos S. 2020. Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 . Monthly Notices of the Royal Astronomical Society. 492(2), 1778–1790.","mla":"Matthee, Jorryt J., et al. “Resolved Lyman-α Properties of a Luminous Lyman-Break Galaxy in a Large Ionized Bubble at z = 6.53 .” Monthly Notices of the Royal Astronomical Society, vol. 492, no. 2, Oxford University Press, 2020, pp. 1778–90, doi:10.1093/mnras/stz3554.","apa":"Matthee, J. J., Sobral, D., Gronke, M., Pezzulli, G., Cantalupo, S., Röttgering, H., … Santos, S. (2020). Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 . Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stz3554","ama":"Matthee JJ, Sobral D, Gronke M, et al. Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 . Monthly Notices of the Royal Astronomical Society. 2020;492(2):1778-1790. doi:10.1093/mnras/stz3554","short":"J.J. Matthee, D. Sobral, M. Gronke, G. Pezzulli, S. Cantalupo, H. Röttgering, B. Darvish, S. Santos, Monthly Notices of the Royal Astronomical Society 492 (2020) 1778–1790.","ieee":"J. J. Matthee et al., “Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 ,” Monthly Notices of the Royal Astronomical Society, vol. 492, no. 2. Oxford University Press, pp. 1778–1790, 2020."},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa":1,"language":[{"iso":"eng"}],"arxiv":1,"month":"02","main_file_link":[{"url":"https://arxiv.org/abs/1909.06376","open_access":"1"}],"quality_controlled":"1","page":"1778-1790","date_updated":"2022-08-18T11:29:53Z","_id":"11534","type":"journal_article","doi":"10.1093/mnras/stz3554","article_processing_charge":"No","publisher":"Oxford University Press","date_published":"2020-02-01T00:00:00Z","acknowledgement":"We thank the referee for their suggestions and constructive comments that helped to improve the presentation of our results. Based on observations obtained with the Very Large Telescope, program 99.A-0462. Based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program #14699. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2017.1.01451.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan) and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. MG acknowledges support from NASA grant NNX17AK58G. GP and SC gratefully acknowledge support from Swiss National Science Foundation grant PP00P2 163824. BD acknowledges financial support from the National Science Foundation, grant number 1716907. We have benefited greatly from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, SCIPY (Jones et al. 2001; Hunter 2007; van der Walt, Colbert & Varoquaux 2011) and ASTROPY (Astropy Collaboration 2013) packages, the astronomical imaging tools SEXTRACTOR, SWARP, and SCAMP (Bertin & Arnouts 1996; Bertin 2006, 2010) and the TOPCAT analysis tool (Taylor 2013).","extern":"1","publication":"Monthly Notices of the Royal Astronomical Society","status":"public","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","dark ages","reionization","first stars","cosmology: observations"],"year":"2020","external_id":{"arxiv":["1909.06376"]}},{"month":"04","arxiv":1,"oa":1,"language":[{"iso":"eng"}],"citation":{"chicago":"Calhau, João, David Sobral, Sérgio Santos, Jorryt J Matthee, Ana Paulino-Afonso, Andra Stroe, Brooke Simmons, Cassandra Barlow-Hall, and Benjamin Adams. “The X-Ray and Radio Activity of Typical and Luminous Ly α Emitters from z ∼ 2 to z ∼ 6: Evidence for a Diverse, Evolving Population.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2020. https://doi.org/10.1093/mnras/staa476.","ista":"Calhau J, Sobral D, Santos S, Matthee JJ, Paulino-Afonso A, Stroe A, Simmons B, Barlow-Hall C, Adams B. 2020. The X-ray and radio activity of typical and luminous Ly α emitters from z ∼ 2 to z ∼ 6: Evidence for a diverse, evolving population. Monthly Notices of the Royal Astronomical Society. 493(3), 3341–3362.","apa":"Calhau, J., Sobral, D., Santos, S., Matthee, J. J., Paulino-Afonso, A., Stroe, A., … Adams, B. (2020). The X-ray and radio activity of typical and luminous Ly α emitters from z ∼ 2 to z ∼ 6: Evidence for a diverse, evolving population. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staa476","mla":"Calhau, João, et al. “The X-Ray and Radio Activity of Typical and Luminous Ly α Emitters from z ∼ 2 to z ∼ 6: Evidence for a Diverse, Evolving Population.” Monthly Notices of the Royal Astronomical Society, vol. 493, no. 3, Oxford University Press, 2020, pp. 3341–62, doi:10.1093/mnras/staa476.","ama":"Calhau J, Sobral D, Santos S, et al. The X-ray and radio activity of typical and luminous Ly α emitters from z ∼ 2 to z ∼ 6: Evidence for a diverse, evolving population. Monthly Notices of the Royal Astronomical Society. 2020;493(3):3341-3362. doi:10.1093/mnras/staa476","ieee":"J. Calhau et al., “The X-ray and radio activity of typical and luminous Ly α emitters from z ∼ 2 to z ∼ 6: Evidence for a diverse, evolving population,” Monthly Notices of the Royal Astronomical Society, vol. 493, no. 3. Oxford University Press, pp. 3341–3362, 2020.","short":"J. Calhau, D. Sobral, S. Santos, J.J. Matthee, A. Paulino-Afonso, A. Stroe, B. Simmons, C. Barlow-Hall, B. Adams, Monthly Notices of the Royal Astronomical Society 493 (2020) 3341–3362."},"issue":"3","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","day":"01","scopus_import":"1","author":[{"last_name":"Calhau","full_name":"Calhau, João","first_name":"João"},{"first_name":"David","last_name":"Sobral","full_name":"Sobral, David"},{"last_name":"Santos","full_name":"Santos, Sérgio","first_name":"Sérgio"},{"first_name":"Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee"},{"first_name":"Ana","full_name":"Paulino-Afonso, Ana","last_name":"Paulino-Afonso"},{"first_name":"Andra","full_name":"Stroe, Andra","last_name":"Stroe"},{"last_name":"Simmons","full_name":"Simmons, Brooke","first_name":"Brooke"},{"first_name":"Cassandra","full_name":"Barlow-Hall, Cassandra","last_name":"Barlow-Hall"},{"last_name":"Adams","full_name":"Adams, Benjamin","first_name":"Benjamin"}],"title":"The X-ray and radio activity of typical and luminous Ly α emitters from z ∼ 2 to z ∼ 6: Evidence for a diverse, evolving population","oa_version":"Preprint","volume":493,"date_created":"2022-07-08T07:34:10Z","article_type":"original","abstract":[{"lang":"eng","text":"Despite recent progress in understanding Ly α emitters (LAEs), relatively little is known regarding their typical black hole activity across cosmic time. Here, we study the X-ray and radio properties of ∼4000 LAEs at 2.2 < z < 6 from the SC4K survey in the COSMOS field. We detect 254 (6.8per cent±0.4per cent) LAEs individually in the X-rays (S/N > 3) with an average luminosity of 1044.31±0.01ergs−1 and average black hole accretion rate (BHAR) of 0.72±0.01 M⊙ yr−1, consistent with moderate to high accreting active galactic neuclei (AGNs). We detect 120 sources in deep radio data (radio AGN fraction of 3.2per cent±0.3per cent). The global AGN fraction (8.6per cent±0.4per cent) rises with Ly α luminosity and declines with increasing redshift. For X-ray-detected LAEs, Ly α luminosities correlate with the BHARs, suggesting that Ly α luminosity becomes a BHAR indicator. Most LAEs (93.1per cent±0.6per cent) at 2 < z < 6 have no detectable X-ray emission (BHARs < 0.017 M⊙ yr−1). The median star formation rate (SFR) of star-forming LAEs from Ly α and radio luminosities is 7.6+6.6−2.8 M⊙ yr−1. The black hole to galaxy growth ratio (BHAR/SFR) for LAEs is <0.0022, consistent with typical star-forming galaxies and the local BHAR/SFR relation. We conclude that LAEs at 2 < z < 6 include two different populations: an AGN population, where Ly α luminosity traces BHAR, and another with low SFRs which remain undetected in even the deepest X-ray stacks but is detected in the radio stacks."}],"intvolume":" 493","publication_status":"published","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"year":"2020","external_id":{"arxiv":["1909.11672"]},"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: active","galaxies: evolution","galaxies: high-redshift","quasars: supermassive black holes","galaxies: star formation","cosmology: observations","X-rays: galaxies"],"status":"public","publication":"Monthly Notices of the Royal Astronomical Society","extern":"1","date_published":"2020-04-01T00:00:00Z","acknowledgement":"JM acknowledges the support of a Huygens PhD fellowship from Leiden University. We thank Camila Correa for help analysing snipshot merger trees. We thank the anonymous referee for constructive comments. We also thank Jarle Brinchmann, Rob Crain, Antonios Katsianis, Paola Popesso, and David Sobral for discussions and suggestions. We also thank the participants of the Lorentz Center workshop ‘A Decade of the Star-Forming Main Sequence’ held on 2017 September 4–8, for discussions and ideas. We have benefited from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, and SCIPY (Hunter 2007) packages and the TOPCAT analysis tool (Taylor 2013).","article_processing_charge":"No","doi":"10.1093/mnras/staa476","publisher":"Oxford University Press","_id":"11539","date_updated":"2022-08-18T11:25:31Z","type":"journal_article","page":"3341-3362","main_file_link":[{"url":"https://arxiv.org/abs/1909.11672","open_access":"1"}],"quality_controlled":"1"},{"date_created":"2022-07-07T13:01:03Z","article_type":"original","volume":489,"title":"The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities","oa_version":"Preprint","scopus_import":"1","day":"01","author":[{"first_name":"A A","full_name":"Khostovan, A A","last_name":"Khostovan"},{"full_name":"Sobral, D","last_name":"Sobral","first_name":"D"},{"full_name":"Mobasher, B","last_name":"Mobasher","first_name":"B"},{"orcid":"0000-0003-2871-127X","first_name":"Jorryt J","last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"first_name":"R K","last_name":"Cochrane","full_name":"Cochrane, R K"},{"first_name":"N","full_name":"Chartab, N","last_name":"Chartab"},{"full_name":"Jafariyazani, M","last_name":"Jafariyazani","first_name":"M"},{"first_name":"A","last_name":"Paulino-Afonso","full_name":"Paulino-Afonso, A"},{"first_name":"S","last_name":"Santos","full_name":"Santos, S"},{"first_name":"J","full_name":"Calhau, J","last_name":"Calhau"}],"publication_status":"published","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"abstract":[{"lang":"eng","text":"We investigate the clustering and halo properties of ∼5000 Ly α-selected emission-line galaxies (LAEs) from the Slicing COSMOS 4K (SC4K) and from archival NB497 imaging of SA22 split in 15 discrete redshift slices between z ∼ 2.5 and 6. We measure clustering lengths of r0 ∼ 3–6 h−1 Mpc and typical halo masses of ∼1011 M⊙ for our narrowband-selected LAEs with typical LLy α ∼ 1042–43 erg s−1. The intermediate-band-selected LAEs are observed to have r0 ∼ 3.5–15 h−1 Mpc with typical halo masses of ∼1011–12 M⊙ and typical LLy α ∼ 1043–43.6 erg s−1. We find a strong, redshift-independent correlation between halo mass and Ly α luminosity normalized by the characteristic Ly α luminosity, L⋆(z). The faintest LAEs (L ∼ 0.1 L⋆(z)) typically identified by deep narrowband surveys are found in 1010 M⊙ haloes and the brightest LAEs (L ∼ 7 L⋆(z)) are found in ∼5 × 1012 M⊙ haloes. A dependency on the rest-frame 1500 Å UV luminosity, MUV, is also observed where the halo masses increase from 1011 to 1013 M⊙ for MUV ∼ −19 to −23.5 mag. Halo mass is also observed to increase from 109.8 to 1012 M⊙ for dust-corrected UV star formation rates from ∼0.6 to 10 M⊙ yr−1 and continues to increase up to 1013 M⊙ in halo mass, where the majority of those sources are active galactic nuclei. All the trends we observe are found to be redshift independent. Our results reveal that LAEs are the likely progenitors of a wide range of galaxies depending on their luminosity, from dwarf-like, to Milky Way-type, to bright cluster galaxies. LAEs therefore provide unique insight into the early formation and evolution of the galaxies we observe in the local Universe."}],"intvolume":" 489","month":"10","arxiv":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"ama":"Khostovan AA, Sobral D, Mobasher B, et al. The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities. Monthly Notices of the Royal Astronomical Society. 2019;489(1):555-573. doi:10.1093/mnras/stz2149","short":"A.A. Khostovan, D. Sobral, B. Mobasher, J.J. Matthee, R.K. Cochrane, N. Chartab, M. Jafariyazani, A. Paulino-Afonso, S. Santos, J. Calhau, Monthly Notices of the Royal Astronomical Society 489 (2019) 555–573.","ieee":"A. A. Khostovan et al., “The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities,” Monthly Notices of the Royal Astronomical Society, vol. 489, no. 1. Oxford University Press, pp. 555–573, 2019.","ista":"Khostovan AA, Sobral D, Mobasher B, Matthee JJ, Cochrane RK, Chartab N, Jafariyazani M, Paulino-Afonso A, Santos S, Calhau J. 2019. The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities. Monthly Notices of the Royal Astronomical Society. 489(1), 555–573.","chicago":"Khostovan, A A, D Sobral, B Mobasher, Jorryt J Matthee, R K Cochrane, N Chartab, M Jafariyazani, A Paulino-Afonso, S Santos, and J Calhau. “The Clustering of Typical Ly α Emitters from z ∼ 2.5–6: Host Halo Masses Depend on Ly α and UV Luminosities.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2019. https://doi.org/10.1093/mnras/stz2149.","mla":"Khostovan, A. A., et al. “The Clustering of Typical Ly α Emitters from z ∼ 2.5–6: Host Halo Masses Depend on Ly α and UV Luminosities.” Monthly Notices of the Royal Astronomical Society, vol. 489, no. 1, Oxford University Press, 2019, pp. 555–73, doi:10.1093/mnras/stz2149.","apa":"Khostovan, A. A., Sobral, D., Mobasher, B., Matthee, J. J., Cochrane, R. K., Chartab, N., … Calhau, J. (2019). The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stz2149"},"issue":"1","language":[{"iso":"eng"}],"oa":1,"type":"journal_article","_id":"11535","date_updated":"2022-08-19T06:38:42Z","publisher":"Oxford University Press","article_processing_charge":"No","doi":"10.1093/mnras/stz2149","quality_controlled":"1","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1811.00556"}],"page":"555-573","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: haloes","galaxies: high-redshift","galaxies: star formation","cosmology: observations","large-scale structure of Universe"],"external_id":{"arxiv":["1811.00556"]},"year":"2019","acknowledgement":"We thank the anonymous referee for their useful comments and suggestions that helped improve this study. AAK acknowledges that this work was supported by NASA Headquarters under the NASA Earth and Space Science Fellowship Program – Grant NNX16AO92H. JM acknowledges support from the ETH Zwicky fellowship. RKC acknowledges funding from STFC via a studentship. APA acknowledges support from the Fundac¸ao para a Ci ˜ encia e a Tecnologia FCT through the fellowship PD/BD/52706/2014 and the research grant UID/FIS/04434/2013. JC and SS both acknowledge their support from the Lancaster University PhD Fellowship. We have benefited greatly from the publicly available programming language PYTHON, including the NUMPY, SCIPY, MATPLOTLIB, SCIKIT-LEARN, and ASTROPY packages, as well as the TOPCAT analysis program. The SC4K samples used in this paper are all publicly available for use by the community (Sobral et al. 2018a). The catalogue is also available on the COSMOS IPAC website (https://irsa.ipac.caltech.edu/data/COSMOS/overview.html).","date_published":"2019-10-01T00:00:00Z","publication":"Monthly Notices of the Royal Astronomical Society","extern":"1","status":"public"},{"oa":1,"language":[{"iso":"eng"}],"citation":{"apa":"Sobral, D., Matthee, J. J., Brammer, G., Ferrara, A., Alegre, L., Röttgering, H., … Darvish, B. (2019). On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/sty2779","mla":"Sobral, David, et al. “On the Nature and Physical Conditions of the Luminous Ly α Emitter CR7 and Its Rest-Frame UV Components.” Monthly Notices of the Royal Astronomical Society, vol. 482, no. 2, Oxford University Press, 2019, pp. 2422–41, doi:10.1093/mnras/sty2779.","chicago":"Sobral, David, Jorryt J Matthee, Gabriel Brammer, Andrea Ferrara, Lara Alegre, Huub Röttgering, Daniel Schaerer, Bahram Mobasher, and Behnam Darvish. “On the Nature and Physical Conditions of the Luminous Ly α Emitter CR7 and Its Rest-Frame UV Components.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2019. https://doi.org/10.1093/mnras/sty2779.","ista":"Sobral D, Matthee JJ, Brammer G, Ferrara A, Alegre L, Röttgering H, Schaerer D, Mobasher B, Darvish B. 2019. On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components. Monthly Notices of the Royal Astronomical Society. 482(2), 2422–2441.","ieee":"D. Sobral et al., “On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components,” Monthly Notices of the Royal Astronomical Society, vol. 482, no. 2. Oxford University Press, pp. 2422–2441, 2019.","short":"D. Sobral, J.J. Matthee, G. Brammer, A. Ferrara, L. Alegre, H. Röttgering, D. Schaerer, B. Mobasher, B. Darvish, Monthly Notices of the Royal Astronomical Society 482 (2019) 2422–2441.","ama":"Sobral D, Matthee JJ, Brammer G, et al. On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components. Monthly Notices of the Royal Astronomical Society. 2019;482(2):2422-2441. doi:10.1093/mnras/sty2779"},"issue":"2","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","arxiv":1,"month":"01","abstract":[{"lang":"eng","text":"We present new Hubble Space Telescope (HST)/WFC3 observations and re-analyse VLT data to unveil the continuum, variability, and rest-frame ultraviolet (UV) lines of the multiple UV clumps of the most luminous Lyα emitter at z = 6.6, CR7 (COSMOS Redshift 7). Our re-reduced, flux-calibrated X-SHOOTER spectra of CR7 reveal an He II emission line in observations obtained along the major axis of Lyα emission with the best seeing conditions. He II is spatially offset by ≈+0.8 arcsec from the peak of Lyα emission, and it is found towards clump B. Our WFC3 grism spectra detects the UV continuum of CR7’s clump A, yielding a power law with β=−2.5+0.6−0.7 and MUV=−21.87+0.25−0.20. No significant variability is found for any of the UV clumps on their own, but there is tentative (≈2.2 σ) brightening of CR7 in F110W as a whole from 2012 to 2017. HST grism data fail to robustly detect rest-frame UV lines in any of the clumps, implying fluxes ≲2×10−17 erg s−1 cm−2 (3σ). We perform CLOUDY modelling to constrain the metallicity and the ionizing nature of CR7. CR7 seems to be actively forming stars without any clear active galactic nucleus activity in clump A, consistent with a metallicity of ∼0.05–0.2 Z⊙. Component C or an interclump component between B and C may host a high ionization source. Our results highlight the need for spatially resolved information to study the formation and assembly of early galaxies."}],"intvolume":" 482","publication_status":"published","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"scopus_import":"1","day":"01","author":[{"first_name":"David","full_name":"Sobral, David","last_name":"Sobral"},{"last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"},{"full_name":"Brammer, Gabriel","last_name":"Brammer","first_name":"Gabriel"},{"full_name":"Ferrara, Andrea","last_name":"Ferrara","first_name":"Andrea"},{"full_name":"Alegre, Lara","last_name":"Alegre","first_name":"Lara"},{"last_name":"Röttgering","full_name":"Röttgering, Huub","first_name":"Huub"},{"full_name":"Schaerer, Daniel","last_name":"Schaerer","first_name":"Daniel"},{"first_name":"Bahram","last_name":"Mobasher","full_name":"Mobasher, Bahram"},{"full_name":"Darvish, Behnam","last_name":"Darvish","first_name":"Behnam"}],"title":"On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components","oa_version":"Preprint","volume":482,"date_created":"2022-07-08T10:40:05Z","article_type":"original","publication":"Monthly Notices of the Royal Astronomical Society","status":"public","extern":"1","date_published":"2019-01-01T00:00:00Z","acknowledgement":"We thank the anonymous reviewer for the numerous detailed comments that led us to greatly improve the quality, extent, and statistical robustness of this work. DS acknowledges financial support from the Netherlands Organisation for Scientific research through a Veni fellowship. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. AF acknowledges support from the ERC Advanced Grant INTERSTELLAR H2020/740120. BD acknowledges financial support from NASA through the Astrophysics Data Analysis Program, grant number NNX12AE20G and the National Science Foundation, grant number 1716907. We are thankful for several discussions and constructive comments from Johannes Zabl, Eros Vanzella, Bo Milvang-Jensen, Henry McCracken, Max Gronke, Mark Dijkstra, Richard Ellis, and Nicolas Laporte. We also thank Umar Burhanudin and Izzy Garland for taking part in the XGAL internship in Lancaster and for exploring the HST grism data independently. Based on observations obtained with HST/WFC3 programs 12578, 14495, and 14596. Based on observations of the National Japanese Observatory with the Suprime-Cam on the Subaru telescope (S14A-086) on the big island 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, 092.A 0786, 093.A-0561, 097.A0043, 097.A-0943, 098.A-0819, 298.A-5012, 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. This research was supported by the Munich Institute for Astro- and Particle Physics of the DFG cluster of excellence ‘Origin and Structure of the Universe’. We have benefitted immensely from the public available programming language PYTHON, including NUMPY and SCIPY (Jones et al. 2001; Van Der Walt, Colbert & Varoquaux 2011), MATPLOTLIB (Hunter 2007), ASTROPY (Astropy Collaboration et al. 2013), and the TOPCAT analysis program (Taylor 2013). This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France. All data used for this paper are publicly available, and we make all reduced data available with the refereed paper.","year":"2019","external_id":{"arxiv":["1710.08422"]},"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","galaxies: ISM","cosmology: observations","dark ages","reionization","first stars","early Universe"],"page":"2422-2441","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1710.08422"}],"quality_controlled":"1","article_processing_charge":"No","doi":"10.1093/mnras/sty2779","publisher":"Oxford University Press","_id":"11541","date_updated":"2022-08-19T06:49:36Z","type":"journal_article"},{"type":"journal_article","_id":"11549","date_updated":"2022-08-19T06:53:39Z","publisher":"Oxford University Press","article_processing_charge":"No","doi":"10.1093/mnras/sty925","quality_controlled":"1","main_file_link":[{"url":"https://arxiv.org/abs/1705.01101"}],"page":"2999-3015","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: haloes","galaxies: high-redshift","galaxies: star formation","cosmology: observations","large-scale structure of Universe"],"external_id":{"arxiv":["1705.01101"]},"year":"2018","acknowledgement":"We thank the anonymous referee for their useful comments and suggestions that improved this study. AAK thanks Anahita Alavi and Irene Shivaei for useful discussion in the making of this paper. AAK acknowledges that this work was supported by NASA Headquarters under the NASA Earth and Space Science Fellowship Program – Grant NNX16AO92H. DS acknowledges financial support from the Netherlands Organization for Scientific Research (NWO) through a Veni fellowship and from Lancaster University through an Early Career Internal Grant A100679. PNB is grateful for support from STFC via grant STM001229/1. IRS acknowledges support from STFC (ST/L00075X/1), the ERC Advanced Grant DUSTYGAL (321334), and a Royal Society/Wolfson Merit award. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. BD acknowledges financial support from NASA through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G.","date_published":"2018-08-01T00:00:00Z","extern":"1","status":"public","publication":"Monthly Notices of the Royal Astronomical Society","date_created":"2022-07-08T11:48:48Z","article_type":"original","volume":478,"oa_version":"Published Version","title":"The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar mass","day":"01","scopus_import":"1","author":[{"last_name":"Khostovan","full_name":"Khostovan, A A","first_name":"A A"},{"first_name":"D","full_name":"Sobral, D","last_name":"Sobral"},{"full_name":"Mobasher, B","last_name":"Mobasher","first_name":"B"},{"last_name":"Best","full_name":"Best, P N","first_name":"P N"},{"last_name":"Smail","full_name":"Smail, I","first_name":"I"},{"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":"Darvish","full_name":"Darvish, B","first_name":"B"},{"first_name":"H","last_name":"Nayyeri","full_name":"Nayyeri, H"},{"first_name":"S","full_name":"Hemmati, S","last_name":"Hemmati"},{"first_name":"J P","last_name":"Stott","full_name":"Stott, J P"}],"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"publication_status":"published","intvolume":" 478","abstract":[{"text":"We investigate the clustering properties of ∼7000 H β + [O III] and [O II] narrowband-selected emitters at z ∼ 0.8–4.7 from the High-z Emission Line Survey. We find clustering lengths, r0, of 1.5–4.0 h−1 Mpc and minimum dark matter halo masses of 1010.7–12.1 M⊙ for our z = 0.8–3.2 H β + [O III] emitters and r0 ∼ 2.0–8.3 h−1 Mpc and halo masses of 1011.5–12.6 M⊙ for our z = 1.5–4.7 [O II] emitters. We find r0 to strongly increase both with increasing line luminosity and redshift. By taking into account the evolution of the characteristic line luminosity, L⋆(z), and using our model predictions of halo mass given r0, we find a strong, redshift-independent increasing trend between L/L⋆(z) and minimum halo mass. The faintest H β + [O III] emitters are found to reside in 109.5 M⊙ haloes and the brightest emitters in 1013.0 M⊙ haloes. For [O II] emitters, the faintest emitters are found in 1010.5 M⊙ haloes and the brightest emitters in 1012.6 M⊙ haloes. A redshift-independent stellar mass dependency is also observed where the halo mass increases from 1011 to 1012.5 M⊙ for stellar masses of 108.5 to 1011.5 M⊙, respectively. We investigate the interdependencies of these trends by repeating our analysis in a Lline−Mstar grid space for our most populated samples (H β + [O III] z = 0.84 and [O II] z = 1.47) and find that the line luminosity dependency is stronger than the stellar mass dependency on halo mass. For L > L⋆ emitters at all epochs, we find a relatively flat trend with halo masses of 1012.5–13 M⊙, which may be due to quenching mechanisms in massive haloes that is consistent with a transitional halo mass predicted by models.","lang":"eng"}],"month":"08","arxiv":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"ista":"Khostovan AA, Sobral D, Mobasher B, Best PN, Smail I, Matthee JJ, Darvish B, Nayyeri H, Hemmati S, Stott JP. 2018. The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar mass. Monthly Notices of the Royal Astronomical Society. 478(3), 2999–3015.","chicago":"Khostovan, A A, D Sobral, B Mobasher, P N Best, I Smail, Jorryt J Matthee, B Darvish, H Nayyeri, S Hemmati, and J P Stott. “The Clustering of H β + [O III] and [O II] Emitters since z ∼ 5: Dependencies with Line Luminosity and Stellar Mass.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2018. https://doi.org/10.1093/mnras/sty925.","mla":"Khostovan, A. A., et al. “The Clustering of H β + [O III] and [O II] Emitters since z ∼ 5: Dependencies with Line Luminosity and Stellar Mass.” Monthly Notices of the Royal Astronomical Society, vol. 478, no. 3, Oxford University Press, 2018, pp. 2999–3015, doi:10.1093/mnras/sty925.","apa":"Khostovan, A. A., Sobral, D., Mobasher, B., Best, P. N., Smail, I., Matthee, J. J., … Stott, J. P. (2018). The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar mass. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/sty925","ama":"Khostovan AA, Sobral D, Mobasher B, et al. The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar mass. Monthly Notices of the Royal Astronomical Society. 2018;478(3):2999-3015. doi:10.1093/mnras/sty925","short":"A.A. Khostovan, D. Sobral, B. Mobasher, P.N. Best, I. Smail, J.J. Matthee, B. Darvish, H. Nayyeri, S. Hemmati, J.P. Stott, Monthly Notices of the Royal Astronomical Society 478 (2018) 2999–3015.","ieee":"A. A. Khostovan et al., “The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar mass,” Monthly Notices of the Royal Astronomical Society, vol. 478, no. 3. Oxford University Press, pp. 2999–3015, 2018."},"issue":"3","language":[{"iso":"eng"}]},{"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"publication_status":"published","intvolume":" 477","abstract":[{"text":"Deep narrow-band surveys have revealed a large population of faint Ly α emitters (LAEs) in the distant Universe, but relatively little is known about the most luminous sources (LLyα≳1042.7 erg s−1; LLyα≳L∗Lyα). Here we present the spectroscopic follow-up of 21 luminous LAEs at z ∼ 2–3 found with panoramic narrow-band surveys over five independent extragalactic fields (≈4 × 106 Mpc3 surveyed at z ∼ 2.2 and z ∼ 3.1). We use WHT/ISIS, Keck/DEIMOS, and VLT/X-SHOOTER to study these sources using high ionization UV lines. Luminous LAEs at z ∼ 2–3 have blue UV slopes (β=−2.0+0.3−0.1) and high Ly α escape fractions (50+20−15 per cent) and span five orders of magnitude in UV luminosity (MUV ≈ −19 to −24). Many (70 per cent) show at least one high ionization rest-frame UV line such as C IV, N V, C III], He II or O III], typically blue-shifted by ≈100–200 km s−1 relative to Ly α. Their Ly α profiles reveal a wide variety of shapes, including significant blue-shifted components and widths from 200 to 4000 km s−1. Overall, 60 ± 11 per cent appear to be active galactic nucleus (AGN) dominated, and at LLyα > 1043.3 erg s−1 and/or MUV < −21.5 virtually all LAEs are AGNs with high ionization parameters (log U = 0.6 ± 0.5) and with metallicities of ≈0.5 − 1 Z⊙. Those lacking signatures of AGNs (40 ± 11 per cent) have lower ionization parameters (logU=−3.0+1.6−0.9 and log ξion = 25.4 ± 0.2) and are apparently metal-poor sources likely powered by young, dust-poor ‘maximal’ starbursts. Our results show that luminous LAEs at z ∼ 2–3 are a diverse population and that 2×L∗Lyα and 2×M∗UV mark a sharp transition in the nature of LAEs, from star formation dominated to AGN dominated.","lang":"eng"}],"article_type":"original","date_created":"2022-07-12T07:18:02Z","volume":477,"oa_version":"Preprint","title":"The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN","author":[{"last_name":"Sobral","full_name":"Sobral, David","first_name":"David"},{"orcid":"0000-0003-2871-127X","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee"},{"last_name":"Darvish","full_name":"Darvish, Behnam","first_name":"Behnam"},{"full_name":"Smail, Ian","last_name":"Smail","first_name":"Ian"},{"full_name":"Best, Philip N","last_name":"Best","first_name":"Philip N"},{"first_name":"Lara","last_name":"Alegre","full_name":"Alegre, Lara"},{"last_name":"Röttgering","full_name":"Röttgering, Huub","first_name":"Huub"},{"full_name":"Mobasher, Bahram","last_name":"Mobasher","first_name":"Bahram"},{"first_name":"Ana","full_name":"Paulino-Afonso, Ana","last_name":"Paulino-Afonso"},{"first_name":"Andra","full_name":"Stroe, Andra","last_name":"Stroe"},{"last_name":"Oteo","full_name":"Oteo, Iván","first_name":"Iván"}],"scopus_import":"1","day":"01","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","issue":"2","citation":{"ista":"Sobral D, Matthee JJ, Darvish B, Smail I, Best PN, Alegre L, Röttgering H, Mobasher B, Paulino-Afonso A, Stroe A, Oteo I. 2018. The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN. Monthly Notices of the Royal Astronomical Society. 477(2), 2817–2840.","chicago":"Sobral, David, Jorryt J Matthee, Behnam Darvish, Ian Smail, Philip N Best, Lara Alegre, Huub Röttgering, et al. “The Nature of Luminous Ly α Emitters at z ∼ 2–3: Maximal Dust-Poor Starbursts and Highly Ionizing AGN.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2018. https://doi.org/10.1093/mnras/sty782.","mla":"Sobral, David, et al. “The Nature of Luminous Ly α Emitters at z ∼ 2–3: Maximal Dust-Poor Starbursts and Highly Ionizing AGN.” Monthly Notices of the Royal Astronomical Society, vol. 477, no. 2, Oxford University Press, 2018, pp. 2817–40, doi:10.1093/mnras/sty782.","apa":"Sobral, D., Matthee, J. J., Darvish, B., Smail, I., Best, P. N., Alegre, L., … Oteo, I. (2018). The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/sty782","ama":"Sobral D, Matthee JJ, Darvish B, et al. The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN. Monthly Notices of the Royal Astronomical Society. 2018;477(2):2817-2840. doi:10.1093/mnras/sty782","short":"D. Sobral, J.J. Matthee, B. Darvish, I. Smail, P.N. Best, L. Alegre, H. Röttgering, B. Mobasher, A. Paulino-Afonso, A. Stroe, I. Oteo, Monthly Notices of the Royal Astronomical Society 477 (2018) 2817–2840.","ieee":"D. Sobral et al., “The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN,” Monthly Notices of the Royal Astronomical Society, vol. 477, no. 2. Oxford University Press, pp. 2817–2840, 2018."},"language":[{"iso":"eng"}],"oa":1,"arxiv":1,"month":"06","quality_controlled":"1","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1802.10102"}],"page":"2817-2840","type":"journal_article","date_updated":"2022-08-19T07:01:08Z","_id":"11557","publisher":"Oxford University Press","doi":"10.1093/mnras/sty782","article_processing_charge":"No","date_published":"2018-06-01T00:00:00Z","acknowledgement":"We thank the anonymous reviewer for their timely and constructive comments that greatly helped us to improve the manuscript. DS acknowledges financial support from the Netherlands Organization for Scientific research (NWO) through a Veni fellowship and from Lancaster University through an Early Career Internal Grant A100679. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. BD acknowledges financial support from NASA through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G, and the National Science Foundation, grant number 1716907. IRS acknowledges support from the ERC Advanced Grant DUSTYGAL (321334), STFC (ST/P000541/1), and a Royal Society/Wolfson Merit Award. PNB is grateful for support from STFC via grant ST/M001229/1. We thank Anne Verhamme, Kimihiko Nakajima, Ryan Trainor, Sangeeta Malhotra, Max Gronke, James Rhoads, Fang Xia An, Matthew Hayes, Takashi Kojima, Mark Dijkstra, and Anne Jaskot for many helpful and engaging discussions, particularly during the SnowCLAW Ly α workshop. We thank Bruno Ribeiro, Stephane Charlot, and Joseph Caruana for comments on the manuscript. The authors would also like to thank Ingrid Tengs, Meg Singleton, Ali Khostovan, and Sara Perez for participating in part of the observations. We also thank Joao Calhau, Leah Morabito, Sergio Santos, and Aayush Saxena for their assistance with the narrow-band observations which allowed to select some of the sour ces. Based on observations obtained with the William Herschel Telescope, program: W16AN004; the Very Large Telescope, programs: 098.A-0819 & 099.A-0254; and the Keck II telescope, program: C267D. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme IDs 294.A-5018, 294.A-5039, 092.A-0786, 093.A-0561, 097.A-0943, 098.A-0819, 099.A-0254 and 179.A-2005. The authors acknowledge the award of service time (SW2014b20) on the WHT. WHT and its service programme are operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. The authors would also like to thank all the extremely helpful observatory staff that have greatly contributed towards our observations, particularly Fiona Riddick, Lilian Dominguez, Florencia Jimenez, and Ian Skillen. We have benefited greatly from the publicly available programming language PYTHON, including the NUMPY & SCIPY (Van Der Walt, Colbert & Varoquaux 2011; Jones et al. 2001), MATPLOTLIB (Hunter 2007), ASTROPY (Astropy Collaboration et al. 2013), and the TOPCAT analysis program (Taylor 2013). This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France.","status":"public","extern":"1","publication":"Monthly Notices of the Royal Astronomical Society","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: active","galaxies: evolution","galaxies: high-redshift","galaxies: ISM","galaxies: starburst","cosmology: observations"],"external_id":{"arxiv":["1802.10102"]},"year":"2018"},{"page":"1242-1258","quality_controlled":"1","main_file_link":[{"url":"https://arxiv.org/abs/1609.05897","open_access":"1"}],"publisher":"Oxford University Press","article_processing_charge":"No","doi":"10.1093/mnras/stw3090","type":"journal_article","_id":"11562","date_updated":"2022-08-19T07:18:20Z","extern":"1","publication":"Monthly Notices of the Royal Astronomical Society","status":"public","acknowledgement":"We thank the reviewer for his/her helpful comments and suggestions that have greatly improved this work. DS and JM acknowledge financial support from the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship. DS also acknowledges funding from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010). PNB is grateful for support from the UK STFC via grant ST/M001229/1. IRS acknowledges support from STFC (ST/L00075X/1), the ERC Advanced Investigator programme DUSTYGAL 321334 and a Royal Society/Wolfson merit award. We thank Matthew Hayes, Ryan Trainor, Kimihiko Nakajima and Anne Verhamme for many helpful discussions and Ana Sobral, Carolina Duarte and Miguel Domingos for taking part in observations with the NB392 filter. We also thank Sergio Santos for helpful comments. This research is based on observations obtained on the Isaac Newton Telescope (INT), programs: I13AN002, I14AN002, 088-INT7/14A, I14BN006, 118-INT13/14B & I15AN008. The authors acknowledge the award of time from programmes: I13AN002, I14AN002, 088-INT7/14A, I14BN006, 118-INT13/14B, I15AN008 on the INT. INT is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 098.A 0819. We have benefited greatly from the publicly available programming language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY and ASTROPY packages, the astronomical imaging tools SEXTRACTOR, SWARP (Bertin & Arnouts 1996; Bertin 2010), SCAMP (Bertin 2006) and TOPCAT (Taylor 2005). Dedicated to the memory of M. L. Nicolau and M. C. Serrano.","date_published":"2017-04-01T00:00:00Z","external_id":{"arxiv":["1609.05897"]},"year":"2017","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: haloes","galaxies: high-redshift","galaxies: luminosity function","mass function","galaxies: statistics","cosmology: observations"],"abstract":[{"text":"We present the CAlibrating LYMan-α with Hα (CALYMHA) pilot survey and new results on Lyman α (Lyα) selected galaxies at z ∼ 2. We use a custom-built Lyα narrow-band filter at the Isaac Newton Telescope, designed to provide a matched volume coverage to the z = 2.23 Hα HiZELS survey. Here, we present the first results for the COSMOS and UDS fields. Our survey currently reaches a 3σ line flux limit of ∼4 × 10−17 erg s−1 cm−2, and a Lyα luminosity limit of ∼1042.3 erg s−1. We find 188 Lyα emitters over 7.3 × 105 Mpc3, but also find significant numbers of other line-emitting sources corresponding to He II, C III] and C IV emission lines. These sources are important contaminants, and we carefully remove them, unlike most previous studies. We find that the Lyα luminosity function at z = 2.23 is very well described by a Schechter function up to LLy α ≈ 1043 erg s−1 with L∗=1042.59+0.16−0.08 erg s−1, ϕ∗=10−3.09+0.14−0.34 Mpc−3 and α = −1.75 ± 0.25. Above LLy α ≈ 1043 erg s−1, the Lyα luminosity function becomes power-law like, driven by X-ray AGN. We find that Lyα-selected emitters have a high escape fraction of 37 ± 7 per cent, anticorrelated with Lyα luminosity and correlated with Lyα equivalent width. Lyα emitters have ubiquitous large (≈40 kpc) Lyα haloes, ∼2 times larger than their Hα extents. By directly comparing our Lyα and Hα luminosity functions, we find that the global/overall escape fraction of Lyα photons (within a 13 kpc radius) from the full population of star-forming galaxies is 5.1 ± 0.2 per cent at the peak of the star formation history. An extra 3.3 ± 0.3 per cent of Lyα photons likely still escape, but at larger radii.","lang":"eng"}],"intvolume":" 466","publication_status":"published","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"title":"The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23","oa_version":"Preprint","day":"01","scopus_import":"1","author":[{"full_name":"Sobral, David","last_name":"Sobral","first_name":"David"},{"full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"},{"full_name":"Best, Philip","last_name":"Best","first_name":"Philip"},{"first_name":"Andra","last_name":"Stroe","full_name":"Stroe, Andra"},{"last_name":"Röttgering","full_name":"Röttgering, Huub","first_name":"Huub"},{"last_name":"Oteo","full_name":"Oteo, Iván","first_name":"Iván"},{"last_name":"Smail","full_name":"Smail, Ian","first_name":"Ian"},{"first_name":"Leah","full_name":"Morabito, Leah","last_name":"Morabito"},{"full_name":"Paulino-Afonso, Ana","last_name":"Paulino-Afonso","first_name":"Ana"}],"date_created":"2022-07-12T12:04:16Z","article_type":"original","volume":466,"language":[{"iso":"eng"}],"oa":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"ama":"Sobral D, Matthee JJ, Best P, et al. The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23. Monthly Notices of the Royal Astronomical Society. 2017;466(1):1242-1258. doi:10.1093/mnras/stw3090","ieee":"D. Sobral et al., “The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23,” Monthly Notices of the Royal Astronomical Society, vol. 466, no. 1. Oxford University Press, pp. 1242–1258, 2017.","short":"D. Sobral, J.J. Matthee, P. Best, A. Stroe, H. Röttgering, I. Oteo, I. Smail, L. Morabito, A. Paulino-Afonso, Monthly Notices of the Royal Astronomical Society 466 (2017) 1242–1258.","ista":"Sobral D, Matthee JJ, Best P, Stroe A, Röttgering H, Oteo I, Smail I, Morabito L, Paulino-Afonso A. 2017. The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23. Monthly Notices of the Royal Astronomical Society. 466(1), 1242–1258.","chicago":"Sobral, David, Jorryt J Matthee, Philip Best, Andra Stroe, Huub Röttgering, Iván Oteo, Ian Smail, Leah Morabito, and Ana Paulino-Afonso. “The CALYMHA Survey: Lyα Luminosity Function and Global Escape Fraction of Lyα Photons at z = 2.23.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2017. https://doi.org/10.1093/mnras/stw3090.","apa":"Sobral, D., Matthee, J. J., Best, P., Stroe, A., Röttgering, H., Oteo, I., … Paulino-Afonso, A. (2017). The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stw3090","mla":"Sobral, David, et al. “The CALYMHA Survey: Lyα Luminosity Function and Global Escape Fraction of Lyα Photons at z = 2.23.” Monthly Notices of the Royal Astronomical Society, vol. 466, no. 1, Oxford University Press, 2017, pp. 1242–58, doi:10.1093/mnras/stw3090."},"issue":"1","arxiv":1,"month":"04"},{"_id":"11564","date_updated":"2022-08-19T07:53:04Z","type":"journal_article","article_processing_charge":"No","doi":"10.1093/mnras/stw2973","publisher":"Oxford University Press","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1605.08782"}],"quality_controlled":"1","page":"3637-3655","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","cosmology: observations","dark ages","reionization","first stars"],"year":"2017","external_id":{"arxiv":["1605.08782"]},"acknowledgement":"We thank the referee for the many helpful and constructive comments which have significantly improved this paper. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. DS acknowledges financial support from the Netherlands Organization for Scientific research (NWO) through a Veni fellowship and from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010). PNB is grateful for support from the UK STFC via grant ST/M001229/1. IO acknowledges support from the European Research Council in the form of the Advanced Investigator Programme, 321302, COSMICISM. The authors thank Andreas Faisst, Michael Rutkowski and Andreas Sandberg for answering questions related to this work and Daniel Schaerer and Mark Dijkstra for discussions. We acknowledge the work that has been done by both the COSMOS team in assembling such large, state-of-the-art multi-wavelength data set, as this has been crucial for the results presented in this paper. We have benefited greatly from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY (Jones et al. 2001; Hunter 2007; Van Der Walt, Colbert & Varoquaux 2011) and ASTROPY (Astropy Collaboration et al. 2013) packages, the astronomical imaging tools SEXTRACTOR and SWARP (Bertin & Arnouts 1996;\r\nBertin 2010) and the TOPCAT analysis program (Taylor 2013).","date_published":"2017-03-01T00:00:00Z","extern":"1","status":"public","publication":"Monthly Notices of the Royal Astronomical Society","volume":465,"date_created":"2022-07-12T12:12:14Z","article_type":"original","day":"01","scopus_import":"1","author":[{"orcid":"0000-0003-2871-127X","first_name":"Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J"},{"full_name":"Sobral, David","last_name":"Sobral","first_name":"David"},{"full_name":"Best, Philip","last_name":"Best","first_name":"Philip"},{"last_name":"Khostovan","full_name":"Khostovan, Ali Ahmad","first_name":"Ali Ahmad"},{"last_name":"Oteo","full_name":"Oteo, Iván","first_name":"Iván"},{"first_name":"Rychard","last_name":"Bouwens","full_name":"Bouwens, Rychard"},{"last_name":"Röttgering","full_name":"Röttgering, Huub","first_name":"Huub"}],"title":"The production and escape of Lyman-Continuum radiation from star-forming galaxies at z ∼ 2 and their redshift evolution","oa_version":"Preprint","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"publication_status":"published","abstract":[{"text":"We study the production rate of ionizing photons of a sample of 588 Hα emitters (HAEs) and 160 Lyman-α emitters (LAEs) at z = 2.2 in the COSMOS field in order to assess the implied emissivity from galaxies, based on their ultraviolet (UV) luminosity. By exploring the rest-frame Lyman Continuum (LyC) with GALEX/NUV data, we find fesc < 2.8 (6.4) per cent through median (mean) stacking. By combining the Hα luminosity density with intergalactic medium emissivity measurements from absorption studies, we find a globally averaged 〈fesc〉 of 5.9+14.5−4.2 per cent at z = 2.2 if we assume HAEs are the only source of ionizing photons. We find similarly low values of the global 〈fesc〉 at z ≈ 3–5, also ruling out a high 〈fesc〉 at z < 5. These low escape fractions allow us to measure ξion, the number of produced ionizing photons per unit UV luminosity, and investigate how this depends on galaxy properties. We find a typical ξion ≈ 1024.77 ± 0.04 Hz erg−1 for HAEs and ξion ≈ 1025.14 ± 0.09 Hz erg−1 for LAEs. LAEs and low-mass HAEs at z = 2.2 show similar values of ξion as typically assumed in the reionization era, while the typical HAE is three times less ionizing. Due to an increasing ξion with increasing EW(Hα), ξion likely increases with redshift. This evolution alone is fully in line with the observed evolution of ξion between z ≈ 2 and 5, indicating a typical value of ξion ≈ 1025.4 Hz erg−1 in the reionization era.","lang":"eng"}],"intvolume":" 465","arxiv":1,"month":"03","citation":{"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.","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.","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","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","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.","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."},"issue":"3","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa":1,"language":[{"iso":"eng"}]},{"language":[{"iso":"eng"}],"oa":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"apa":"Stroe, A., Sobral, D., Matthee, J. J., Calhau, J., & Oteo, I. (2017). A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent widths . Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stx1712","mla":"Stroe, Andra, et al. “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, Morphologies and Equivalent Widths .” Monthly Notices of the Royal Astronomical Society, vol. 471, no. 3, Oxford University Press, 2017, pp. 2558–74, doi:10.1093/mnras/stx1712.","ista":"Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. 2017. A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent widths . Monthly Notices of the Royal Astronomical Society. 471(3), 2558–2574.","chicago":"Stroe, Andra, David Sobral, Jorryt J Matthee, João Calhau, and Ivan Oteo. “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, Morphologies and Equivalent Widths .” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2017. https://doi.org/10.1093/mnras/stx1712.","ieee":"A. Stroe, D. Sobral, J. J. Matthee, J. Calhau, and I. Oteo, “A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent widths ,” Monthly Notices of the Royal Astronomical Society, vol. 471, no. 3. Oxford University Press, pp. 2558–2574, 2017.","short":"A. Stroe, D. Sobral, J.J. Matthee, J. Calhau, I. Oteo, Monthly Notices of the Royal Astronomical Society 471 (2017) 2558–2574.","ama":"Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent widths . Monthly Notices of the Royal Astronomical Society. 2017;471(3):2558-2574. doi:10.1093/mnras/stx1712"},"issue":"3","month":"11","arxiv":1,"abstract":[{"text":"While traditionally associated with active galactic nuclei (AGN), the properties of the C II] (λ = 2326 Å), C III] (λ, λ = 1907, 1909 Å) and C IV (λ, λ = 1549, 1551 Å) emission lines are still uncertain as large, unbiased samples of sources are scarce. We present the first blind, statistical study of C II], C III] and C IV emitters at z ∼ 0.68, 1.05, 1.53, respectively, uniformly selected down to a flux limit of ∼4 × 10−17 erg s−1 cm−1 through a narrow-band survey covering an area of ∼1.4 deg2 over COSMOS and UDS. We detect 16 C II], 35 C III] and 17 C IV emitters, whose nature we investigate using optical colours as well as Hubble Space Telescope (HST), X-ray, radio and far-infrared data. We find that z ∼ 0.7 C II] emitters are consistent with a mixture of blue (UV slope β = −2.0 ± 0.4) star-forming (SF) galaxies with discy HST structure and AGN with Seyfert-like morphologies. Bright C II] emitters have individual X-ray detections as well as high average black hole accretion rates (BHARs) of ∼0.1 M⊙ yr−1. C III] emitters at z ∼ 1.05 trace a general population of SF galaxies, with β = −0.8 ± 1.1, a variety of optical morphologies, including isolated and interacting galaxies and low BHAR (<0.02 M⊙ yr−1). Our C IV emitters at z ∼ 1.5 are consistent with young, blue quasars (β ∼ −1.9) with point-like optical morphologies, bright X-ray counterparts and large BHAR (0.8 M⊙ yr−1). We also find some surprising C II], C III] and C IV emitters with rest-frame equivalent widths (EWs) that could be as large as 50–100 Å. AGN or spatial offsets between the UV continuum stellar disc and the line-emitting regions may explain the large EW. These bright C II], C III] and C IV emitters are ideal candidates for spectroscopic follow-up to fully unveil their nature.","lang":"eng"}],"intvolume":" 471","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"publication_status":"published","oa_version":"Preprint","title":"A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent widths ","day":"01","scopus_import":"1","author":[{"full_name":"Stroe, Andra","last_name":"Stroe","first_name":"Andra"},{"last_name":"Sobral","full_name":"Sobral, David","first_name":"David"},{"orcid":"0000-0003-2871-127X","first_name":"Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J"},{"first_name":"João","full_name":"Calhau, João","last_name":"Calhau"},{"full_name":"Oteo, Ivan","last_name":"Oteo","first_name":"Ivan"}],"date_created":"2022-07-12T12:33:16Z","article_type":"original","volume":471,"extern":"1","status":"public","publication":"Monthly Notices of the Royal Astronomical Society","date_published":"2017-11-01T00:00:00Z","acknowledgement":"We would like to thank the anonymous referee for her/his valuable input that helped improve the clarity and interpretation of our results. DS acknowledges financial support from the Netherlands Organisation for Scientific research (NWO), through a Veni fellowship. IO acknowledges support from the European Research Council in the form of the Advanced Investigator Programme, 321302, COSMICISM. CALYMHA data are based on observations made with the Isaac Newton Telescope (proposals 13AN002, I14AN002, 088-INT7/14A, I14BN006, 118-INT13/14B, I15AN008) operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias. Also based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme IDs 098.A-0819 and 179.A-2005. We are grateful to E. L. Wright and J. Schombert for their cosmology calculator. We would like to thank the authors of NUMPY (van der Walt et al. 2011), SCIPY (Jones et al. 2001), MATPLOTLIB (Hunter 2007) and ASTROPY (Astropy Collaboration et al. 2013) for making these packages publicly available. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is ","external_id":{"arxiv":["1703.10169"]},"year":"2017","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: active","galaxies: high-redshift","quasars: emission lines","galaxies: star formation","cosmology: observations"],"page":"2558-2574","quality_controlled":"1","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1703.10169"}],"publisher":"Oxford University Press","article_processing_charge":"No","doi":"10.1093/mnras/stx1712","type":"journal_article","_id":"11566","date_updated":"2022-08-19T07:59:57Z"},{"month":"11","arxiv":1,"citation":{"ama":"Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average line ratios. Monthly Notices of the Royal Astronomical Society. 2017;471(3):2575-2586. doi:10.1093/mnras/stx1713","short":"A. Stroe, D. Sobral, J.J. Matthee, J. Calhau, I. Oteo, Monthly Notices of the Royal Astronomical Society 471 (2017) 2575–2586.","ieee":"A. Stroe, D. Sobral, J. J. Matthee, J. Calhau, and I. Oteo, “A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average line ratios,” Monthly Notices of the Royal Astronomical Society, vol. 471, no. 3. Oxford University Press, pp. 2575–2586, 2017.","ista":"Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. 2017. A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average line ratios. Monthly Notices of the Royal Astronomical Society. 471(3), 2575–2586.","chicago":"Stroe, Andra, David Sobral, Jorryt J Matthee, João Calhau, and Ivan Oteo. “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity Functions and Cosmic Average Line Ratios.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2017. https://doi.org/10.1093/mnras/stx1713.","mla":"Stroe, Andra, et al. “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity Functions and Cosmic Average Line Ratios.” Monthly Notices of the Royal Astronomical Society, vol. 471, no. 3, Oxford University Press, 2017, pp. 2575–86, doi:10.1093/mnras/stx1713.","apa":"Stroe, A., Sobral, D., Matthee, J. J., Calhau, J., & Oteo, I. (2017). A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average line ratios. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stx1713"},"issue":"3","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa":1,"language":[{"iso":"eng"}],"volume":471,"date_created":"2022-07-12T12:54:57Z","article_type":"original","day":"01","scopus_import":"1","author":[{"first_name":"Andra","full_name":"Stroe, Andra","last_name":"Stroe"},{"last_name":"Sobral","full_name":"Sobral, David","first_name":"David"},{"last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","first_name":"Jorryt J"},{"last_name":"Calhau","full_name":"Calhau, João","first_name":"João"},{"first_name":"Ivan","last_name":"Oteo","full_name":"Oteo, Ivan"}],"title":"A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average line ratios","oa_version":"Preprint","publication_status":"published","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"intvolume":" 471","abstract":[{"text":"Recently, the C III] and C IV emission lines have been observed in galaxies in the early Universe (z > 5), providing new ways to measure their redshift and study their stellar populations and active galactic nuclei (AGN). We explore the first blind C II], C III] and C IV survey (z ∼ 0.68, 1.05, 1.53, respectively) presented in Stroe et al. (2017). We derive luminosity functions (LF) and study properties of C II], C III] and C IV line emitters through comparisons to the LFs of H α and Ly α emitters, UV selected star-forming (SF) galaxies and quasars at similar redshifts. The C II] LF at z ∼ 0.68 is equally well described by a Schechter or a power-law LF, characteristic of a mixture of SF and AGN activity. The C III] LF (z ∼ 1.05) is consistent to a scaled down version of the Schechter H α and Ly α LF at their redshift, indicating a SF origin. In stark contrast, the C IV LF at z ∼ 1.53 is well fit by a power-law, quasar-like LF. We find that the brightest UV sources (MUV < −22) will universally have C III] and C IV emission. However, on average, C III] and C IV are not as abundant as H α or Ly α emitters at the same redshift, with cosmic average ratios of ∼0.02–0.06 to H α and ∼0.01–0.1 to intrinsic Ly α. We predict that the C III] and C IV lines can only be truly competitive in confirming high-redshift candidates when the hosts are intrinsically bright and the effective Ly α escape fraction is below 1 per cent. While C III] and C IV were proposed as good tracers of young, relatively low-metallicity galaxies typical of the early Universe, we find that, at least at z ∼ 1.5, C IV is exclusively hosted by AGN/quasars, especially at large line equivalent widths.","lang":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: active","galaxies: high redshift","galaxies: luminosity function","mass function","quasars: emission lines","star formation","cosmology: observations"],"year":"2017","external_id":{"arxiv":["1703.10169"]},"date_published":"2017-11-01T00:00:00Z","extern":"1","publication":"Monthly Notices of the Royal Astronomical Society","status":"public","_id":"11567","date_updated":"2022-08-19T08:02:04Z","type":"journal_article","article_processing_charge":"No","doi":"10.1093/mnras/stx1713","publisher":"Oxford University Press","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1703.10169"}],"quality_controlled":"1","page":"2575-2586"},{"external_id":{"arxiv":["1706.06591"]},"year":"2017","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution – galaxies: high-redshift","dark ages","reionization","first stars","cosmology: observations"],"publication":"Monthly Notices of the Royal Astronomical Society","status":"public","extern":"1","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).","date_published":"2017-11-01T00:00:00Z","publisher":"Oxford University Press","doi":"10.1093/mnras/stx2061","article_processing_charge":"No","type":"journal_article","date_updated":"2022-08-19T08:05:37Z","_id":"11572","page":"772-787","quality_controlled":"1","main_file_link":[{"url":"https://arxiv.org/abs/1706.06591","open_access":"1"}],"arxiv":1,"month":"11","language":[{"iso":"eng"}],"oa":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","issue":"1","citation":{"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.","short":"J.J. Matthee, D. Sobral, B. Darvish, S. Santos, B. Mobasher, A. Paulino-Afonso, H. Röttgering, L. Alegre, Monthly Notices of the Royal Astronomical Society 472 (2017) 772–787.","ama":"Matthee JJ, Sobral D, Darvish B, et al. Spectroscopic properties of luminous Ly α emitters at z ≈ 6–7 and comparison to the Lyman-break population. Monthly Notices of the Royal Astronomical Society. 2017;472(1):772-787. doi:10.1093/mnras/stx2061","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","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.","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.","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."},"oa_version":"Preprint","title":"Spectroscopic properties of luminous Ly α emitters at z ≈ 6–7 and comparison to the Lyman-break population","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","first_name":"Jorryt J"},{"first_name":"David","full_name":"Sobral, David","last_name":"Sobral"},{"first_name":"Behnam","full_name":"Darvish, Behnam","last_name":"Darvish"},{"last_name":"Santos","full_name":"Santos, Sérgio","first_name":"Sérgio"},{"full_name":"Mobasher, Bahram","last_name":"Mobasher","first_name":"Bahram"},{"first_name":"Ana","full_name":"Paulino-Afonso, Ana","last_name":"Paulino-Afonso"},{"full_name":"Röttgering, Huub","last_name":"Röttgering","first_name":"Huub"},{"first_name":"Lara","full_name":"Alegre, Lara","last_name":"Alegre"}],"scopus_import":"1","day":"01","article_type":"original","date_created":"2022-07-13T09:47:39Z","volume":472,"abstract":[{"text":"We present spectroscopic follow-up of candidate luminous Ly α emitters (LAEs) at z = 5.7–6.6 in the SA22 field with VLT/X-SHOOTER. We confirm two new luminous LAEs at z = 5.676 (SR6) and z = 6.532 (VR7), and also present HST follow-up of both sources. These sources have luminosities LLy α ≈ 3 × 1043 erg s−1, very high rest-frame equivalent widths of EW0 ≳ 200 Å and narrow Ly α lines (200–340 km s−1). VR7 is the most UV-luminous LAE at z > 6.5, with M1500 = −22.5, even brighter in the UV than CR7. Besides Ly α, we do not detect any other rest-frame UV lines in the spectra of SR6 and VR7, and argue that rest-frame UV lines are easier to observe in bright galaxies with low Ly α equivalent widths. We confirm that Ly α line widths increase with Ly α luminosity at z = 5.7, while there are indications that Ly α lines of faint LAEs become broader at z = 6.6, potentially due to reionization. We find a large spread of up to 3 dex in UV luminosity for >L⋆ LAEs, but find that the Ly α luminosity of the brightest LAEs is strongly related to UV luminosity at z = 6.6. Under basic assumptions, we find that several LAEs at z ≈ 6–7 have Ly α escape fractions ≳ 100 per cent, indicating bursty star formation histories, alternative Ly α production mechanisms, or dust attenuating Ly α emission differently than UV emission. Finally, we present a method to compute ξion, the production efficiency of ionizing photons, and find that LAEs at z ≈ 6–7 have high values of log10(ξion/Hz erg−1) ≈ 25.51 ± 0.09 that may alleviate the need for high Lyman-Continuum escape fractions required for reionization.","lang":"eng"}],"intvolume":" 472","publication_status":"published","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]}},{"month":"12","arxiv":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"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.","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","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.","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.","short":"S. Santos, D. Sobral, J.J. Matthee, Monthly Notices of the Royal Astronomical Society 463 (2016) 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.","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"},"issue":"2","language":[{"iso":"eng"}],"oa":1,"date_created":"2022-07-13T10:08:20Z","article_type":"original","volume":463,"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","day":"01","scopus_import":"1","author":[{"full_name":"Santos, Sérgio","last_name":"Santos","first_name":"Sérgio"},{"first_name":"David","full_name":"Sobral, David","last_name":"Sobral"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"}],"publication_status":"published","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"intvolume":" 463","abstract":[{"lang":"eng","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."}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift","galaxies: luminosity function","mass function","cosmology: observations","dark ages","reionization","first stars"],"external_id":{"arxiv":["1606.07435"]},"year":"2016","date_published":"2016-12-01T00:00:00Z","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.","publication":"Monthly Notices of the Royal Astronomical Society","status":"public","extern":"1","type":"journal_article","_id":"11574","date_updated":"2022-08-19T08:09:54Z","publisher":"Oxford University Press","article_processing_charge":"No","doi":"10.1093/mnras/stw2076","quality_controlled":"1","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1606.07435"}],"page":"1678-1691"},{"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"ama":"Sobral D, Kohn SA, Best PN, et al. The most luminous H α emitters at z ∼ 0.8–2.23 from HiZELS: Evolution of AGN and star-forming galaxies. Monthly Notices of the Royal Astronomical Society. 2016;457(2):1739-1752. doi:10.1093/mnras/stw022","ieee":"D. Sobral et al., “The most luminous H α emitters at z ∼ 0.8–2.23 from HiZELS: Evolution of AGN and star-forming galaxies,” Monthly Notices of the Royal Astronomical Society, vol. 457, no. 2. Oxford University Press, pp. 1739–1752, 2016.","short":"D. Sobral, S.A. Kohn, P.N. Best, I. Smail, C.M. Harrison, J. Stott, J. Calhau, J.J. Matthee, Monthly Notices of the Royal Astronomical Society 457 (2016) 1739–1752.","ista":"Sobral D, Kohn SA, Best PN, Smail I, Harrison CM, Stott J, Calhau J, Matthee JJ. 2016. The most luminous H α emitters at z ∼ 0.8–2.23 from HiZELS: Evolution of AGN and star-forming galaxies. Monthly Notices of the Royal Astronomical Society. 457(2), 1739–1752.","chicago":"Sobral, David, Saul A. Kohn, Philip N. Best, Ian Smail, Chris M. Harrison, John Stott, João Calhau, and Jorryt J Matthee. “The Most Luminous H α Emitters at z ∼ 0.8–2.23 from HiZELS: Evolution of AGN and Star-Forming Galaxies.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2016. https://doi.org/10.1093/mnras/stw022.","apa":"Sobral, D., Kohn, S. A., Best, P. N., Smail, I., Harrison, C. M., Stott, J., … Matthee, J. J. (2016). The most luminous H α emitters at z ∼ 0.8–2.23 from HiZELS: Evolution of AGN and star-forming galaxies. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stw022","mla":"Sobral, David, et al. “The Most Luminous H α Emitters at z ∼ 0.8–2.23 from HiZELS: Evolution of AGN and Star-Forming Galaxies.” Monthly Notices of the Royal Astronomical Society, vol. 457, no. 2, Oxford University Press, 2016, pp. 1739–52, doi:10.1093/mnras/stw022."},"issue":"2","language":[{"iso":"eng"}],"oa":1,"month":"04","arxiv":1,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"publication_status":"published","abstract":[{"lang":"eng","text":"We use new near-infrared spectroscopic observations to investigate the nature and evolution of the most luminous Hα emitters at z ∼ 0.8–2.23, which evolve strongly in number density over this period, and compare them to more typical Hα emitters. We study 59 luminous Hα emitters with LHα > L∗Hα, roughly equally split per redshift slice at z ∼ 0.8, 1.47 and 2.23 from the HiZELS and CF-HiZELS surveys. We find that, overall, 30 ± 8 per cent are active galactic nuclei [AGNs; 80 ± 30 per cent of these AGNs are broad-line AGNs, BL-AGNs], and we find little to no evolution in the AGN fraction with redshift, within the errors. However, the AGN fraction increases strongly with Hα luminosity and correlates best with LHα/L∗Hα(z). While LHα ≤ L∗Hα(z) Hα emitters are largely dominated by star-forming galaxies (>80 per cent), the most luminous Hα emitters (LHα>10L∗Hα(z)) at any cosmic time are essentially all BL-AGN. Using our AGN-decontaminated sample of luminous star-forming galaxies, and integrating down to a fixed Hα luminosity, we find a factor of ∼1300 evolution in the star formation rate density from z = 0 to 2.23. This is much stronger than the evolution from typical Hα star-forming galaxies and in line with the evolution seen for constant luminosity cuts used to select ‘ultraluminous’ infrared galaxies and/or sub-millimetre galaxies. By taking into account the evolution in the typical Hα luminosity, we show that the most strongly star-forming Hα-selected galaxies at any epoch (LHα>L∗Hα(z)) contribute the same fractional amount of ≈15 per cent to the total star formation rate density, at least up to z = 2.23."}],"intvolume":" 457","date_created":"2022-07-13T12:50:36Z","article_type":"original","volume":457,"oa_version":"Preprint","title":"The most luminous H α emitters at z ∼ 0.8–2.23 from HiZELS: Evolution of AGN and star-forming galaxies","day":"01","scopus_import":"1","author":[{"first_name":"David","last_name":"Sobral","full_name":"Sobral, David"},{"last_name":"Kohn","full_name":"Kohn, Saul A.","first_name":"Saul A."},{"full_name":"Best, Philip N.","last_name":"Best","first_name":"Philip N."},{"first_name":"Ian","full_name":"Smail, Ian","last_name":"Smail"},{"first_name":"Chris M.","last_name":"Harrison","full_name":"Harrison, Chris M."},{"last_name":"Stott","full_name":"Stott, John","first_name":"John"},{"first_name":"João","full_name":"Calhau, João","last_name":"Calhau"},{"full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X","first_name":"Jorryt J"}],"acknowledgement":"The authors would like to thank the anonymous reviewer for the many helpful comments and suggestions which greatly improved the clarity and quality of this work. DS and SAK acknowledge financial support from the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship. DS also acknowledges funding from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010) and from FCT grant PEst-OE/FIS/UI2751/2014. Part of this project was undertaken during the inaugural Leiden/ESA Astrophysics Program for Summer Students (LEAPS). IRS acknowledges support from STFC (ST/L00075X/1), the ERC Advanced Investigator programme DUSTYGAL 321334 and a Royal Society/Wolfson merit award. CH acknowledges support from STFC. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 087.A-0337 and ID 089.A-0965. Also based on data from the Telescopio Nazionale Galileo, with time awarded through OPTICON programmes 2011A/026 and 2012A020 and the William Herschel Telescope under programme W12BN007. The William Herschel Telescope is operated on the island of La Palma by the Isaac Newton Group in the Spanish\r\nObservatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. The authors wish to thank all the help given by the telescope staff from all the observatories used in this study: ESO staff in La Silla, and the TNG and WHT staff in La Palma. This publication makes use of data products from the Two Micron All-Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation.","date_published":"2016-04-01T00:00:00Z","publication":"Monthly Notices of the Royal Astronomical Society","extern":"1","status":"public","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","cosmology: observations"],"external_id":{"arxiv":["1601.02266"]},"year":"2016","quality_controlled":"1","main_file_link":[{"url":"https://arxiv.org/abs/1601.02266","open_access":"1"}],"page":"1739-1752","type":"journal_article","_id":"11576","date_updated":"2022-08-19T08:15:21Z","publisher":"Oxford University Press","article_processing_charge":"No","doi":"10.1093/mnras/stw022"}]