[{"article_type":"original","publisher":"EDP Sciences","quality_controlled":"1","title":"The MUSE eXtremely Deep Field: Individual detections of Lyα haloes around rest-frame UV-selected galaxies at z ≃ 2.9–4.4","intvolume":" 660","publication_status":"published","date_created":"2022-07-05T14:27:26Z","article_processing_charge":"No","author":[{"first_name":"Haruka","last_name":"Kusakabe","full_name":"Kusakabe, Haruka"},{"last_name":"Verhamme","first_name":"Anne","full_name":"Verhamme, Anne"},{"full_name":"Blaizot, Jérémy","last_name":"Blaizot","first_name":"Jérémy"},{"full_name":"Garel, Thibault","last_name":"Garel","first_name":"Thibault"},{"last_name":"Wisotzki","first_name":"Lutz","full_name":"Wisotzki, Lutz"},{"full_name":"Leclercq, Floriane","first_name":"Floriane","last_name":"Leclercq"},{"full_name":"Bacon, Roland","last_name":"Bacon","first_name":"Roland"},{"full_name":"Schaye, Joop","last_name":"Schaye","first_name":"Joop"},{"first_name":"Sofia G.","last_name":"Gallego","full_name":"Gallego, Sofia G."},{"full_name":"Kerutt, Josephine","last_name":"Kerutt","first_name":"Josephine"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","last_name":"Matthee"},{"full_name":"Maseda, Michael","first_name":"Michael","last_name":"Maseda"},{"full_name":"Nanayakkara, Themiya","first_name":"Themiya","last_name":"Nanayakkara"},{"full_name":"Pelló, Roser","last_name":"Pelló","first_name":"Roser"},{"full_name":"Richard, Johan","first_name":"Johan","last_name":"Richard"},{"full_name":"Tresse, Laurence","last_name":"Tresse","first_name":"Laurence"},{"last_name":"Urrutia","first_name":"Tanya","full_name":"Urrutia, Tanya"},{"first_name":"Eloïse","last_name":"Vitte","full_name":"Vitte, Eloïse"}],"_id":"11488","scopus_import":"1","extern":"1","volume":660,"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).","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"}],"doi":"10.1051/0004-6361/202142302","arxiv":1,"day":"07","external_id":{"arxiv":["2201.07257"]},"date_updated":"2022-07-19T09:33:24Z","year":"2022","citation":{"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","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.","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.","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.","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).","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."},"language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift / galaxies: formation / galaxies: evolution / cosmology: observations"],"month":"04","article_number":"A44","oa_version":"Published Version","publication":"Astronomy & Astrophysics","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2201.07257"}],"oa":1,"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"date_published":"2022-04-07T00:00:00Z","type":"journal_article"},{"extern":"1","volume":659,"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.","external_id":{"arxiv":["2202.06642"]},"citation":{"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","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","ieee":"J. Kerutt et al., “Equivalent widths of Lyman α emitters in MUSE-Wide and MUSE-Deep,” Astronomy & Astrophysics, vol. 659. EDP Sciences, 2022.","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.","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).","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."},"year":"2022","date_updated":"2022-07-19T09:47:16Z","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."}],"day":"25","arxiv":1,"doi":"10.1051/0004-6361/202141900","quality_controlled":"1","article_type":"original","publisher":"EDP Sciences","author":[{"full_name":"Kerutt, J.","first_name":"J.","last_name":"Kerutt"},{"first_name":"L.","last_name":"Wisotzki","full_name":"Wisotzki, L."},{"last_name":"Verhamme","first_name":"A.","full_name":"Verhamme, A."},{"full_name":"Schmidt, K. B.","first_name":"K. B.","last_name":"Schmidt"},{"full_name":"Leclercq, F.","last_name":"Leclercq","first_name":"F."},{"full_name":"Herenz, E. C.","last_name":"Herenz","first_name":"E. C."},{"last_name":"Urrutia","first_name":"T.","full_name":"Urrutia, T."},{"first_name":"T.","last_name":"Garel","full_name":"Garel, T."},{"first_name":"T.","last_name":"Hashimoto","full_name":"Hashimoto, T."},{"first_name":"M.","last_name":"Maseda","full_name":"Maseda, M."},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J"},{"last_name":"Kusakabe","first_name":"H.","full_name":"Kusakabe, H."},{"first_name":"J.","last_name":"Schaye","full_name":"Schaye, J."},{"full_name":"Richard, J.","last_name":"Richard","first_name":"J."},{"last_name":"Guiderdoni","first_name":"B.","full_name":"Guiderdoni, B."},{"full_name":"Mauerhofer, V.","last_name":"Mauerhofer","first_name":"V."},{"first_name":"T.","last_name":"Nanayakkara","full_name":"Nanayakkara, T."},{"last_name":"Vitte","first_name":"E.","full_name":"Vitte, E."}],"scopus_import":"1","_id":"11497","intvolume":" 659","title":"Equivalent widths of Lyman α emitters in MUSE-Wide and MUSE-Deep","date_created":"2022-07-06T08:17:27Z","article_processing_charge":"No","publication_status":"published","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","main_file_link":[{"url":"https://arxiv.org/abs/2202.06642","open_access":"1"}],"type":"journal_article","date_published":"2022-03-25T00:00:00Z","oa":1,"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift / galaxies: formation / galaxies: evolution / cosmology: observations"],"language":[{"iso":"eng"}],"publication":"Astronomy & Astrophysics","article_number":"183","month":"03","oa_version":"Published Version"},{"scopus_import":"1","_id":"11524","issue":"1","author":[{"full_name":"Santos, S","first_name":"S","last_name":"Santos"},{"last_name":"Sobral","first_name":"D","full_name":"Sobral, D"},{"first_name":"J","last_name":"Butterworth","full_name":"Butterworth, J"},{"last_name":"Paulino-Afonso","first_name":"A","full_name":"Paulino-Afonso, A"},{"last_name":"Ribeiro","first_name":"B","full_name":"Ribeiro, B"},{"full_name":"da Cunha, E","last_name":"da Cunha","first_name":"E"},{"full_name":"Calhau, J","last_name":"Calhau","first_name":"J"},{"last_name":"Khostovan","first_name":"A A","full_name":"Khostovan, A A"},{"full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"full_name":"Arrabal Haro, P","last_name":"Arrabal Haro","first_name":"P"}],"article_processing_charge":"No","date_created":"2022-07-07T10:02:59Z","publication_status":"published","intvolume":" 505","title":"The evolution of the UV luminosity and stellar mass functions of Lyman-α emitters from z ∼ 2 to z ∼ 6","quality_controlled":"1","page":"1117-1134","publisher":"Oxford University Press","article_type":"original","year":"2021","citation":{"apa":"Santos, S., Sobral, D., Butterworth, J., Paulino-Afonso, A., Ribeiro, B., da Cunha, E., … Arrabal Haro, P. (2021). The evolution of the UV luminosity and stellar mass functions of Lyman-α emitters from z ∼ 2 to z ∼ 6. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stab1218","ama":"Santos S, Sobral D, Butterworth J, et al. The evolution of the UV luminosity and stellar mass functions of Lyman-α emitters from z ∼ 2 to z ∼ 6. Monthly Notices of the Royal Astronomical Society. 2021;505(1):1117-1134. doi:10.1093/mnras/stab1218","chicago":"Santos, S, D Sobral, J Butterworth, A Paulino-Afonso, B Ribeiro, E da Cunha, J Calhau, A A Khostovan, Jorryt J Matthee, and P Arrabal Haro. “The Evolution of the UV Luminosity and Stellar Mass Functions of Lyman-α Emitters from z ∼ 2 to z ∼ 6.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2021. https://doi.org/10.1093/mnras/stab1218.","ieee":"S. Santos et al., “The evolution of the UV luminosity and stellar mass functions of Lyman-α emitters from z ∼ 2 to z ∼ 6,” Monthly Notices of the Royal Astronomical Society, vol. 505, no. 1. Oxford University Press, pp. 1117–1134, 2021.","short":"S. Santos, D. Sobral, J. Butterworth, A. Paulino-Afonso, B. Ribeiro, E. da Cunha, J. Calhau, A.A. Khostovan, J.J. Matthee, P. Arrabal Haro, Monthly Notices of the Royal Astronomical Society 505 (2021) 1117–1134.","mla":"Santos, S., et al. “The Evolution of the UV Luminosity and Stellar Mass Functions of Lyman-α Emitters from z ∼ 2 to z ∼ 6.” Monthly Notices of the Royal Astronomical Society, vol. 505, no. 1, Oxford University Press, 2021, pp. 1117–34, doi:10.1093/mnras/stab1218.","ista":"Santos S, Sobral D, Butterworth J, Paulino-Afonso A, Ribeiro B, da Cunha E, Calhau J, Khostovan AA, Matthee JJ, Arrabal Haro P. 2021. The evolution of the UV luminosity and stellar mass functions of Lyman-α emitters from z ∼ 2 to z ∼ 6. Monthly Notices of the Royal Astronomical Society. 505(1), 1117–1134."},"date_updated":"2022-08-18T10:51:47Z","external_id":{"arxiv":["2105.00007"]},"day":"01","arxiv":1,"doi":"10.1093/mnras/stab1218","abstract":[{"lang":"eng","text":"We measure the evolution of the rest-frame UV luminosity function (LF) and the stellar mass function (SMF) of Lyman-α (Ly α) emitters (LAEs) from z ∼ 2 to z ∼ 6 by exploring ∼4000 LAEs from the SC4K sample. We find a correlation between Ly α luminosity (LLy α) and rest-frame UV (MUV), with best fit MUV=−1.6+0.2−0.3log10(LLyα/ergs−1)+47+12−11 and a shallower relation between LLy α and stellar mass (M⋆), with best fit log10(M⋆/M⊙)=0.9+0.1−0.1log10(LLyα/ergs−1)−28+4.0−3.8. An increasing LLy α cut predominantly lowers the number density of faint MUV and low M⋆ LAEs. We estimate a proxy for the full UV LFs and SMFs of LAEs with simple assumptions of the faint end slope. For the UV LF, we find a brightening of the characteristic UV luminosity (M∗UV) with increasing redshift and a decrease of the characteristic number density (Φ*). For the SMF, we measure a characteristic stellar mass (M∗⋆/M⊙) increase with increasing redshift, and a Φ* decline. However, if we apply a uniform luminosity cut of log10(LLyα/ergs−1)≥43.0, we find much milder to no evolution in the UV and SMF of LAEs. The UV luminosity density (ρUV) of the full sample of LAEs shows moderate evolution and the stellar mass density (ρM) decreases, with both being always lower than the total ρUV and ρM of more typical galaxies but slowly approaching them with increasing redshift. Overall, our results indicate that both ρUV and ρM of LAEs slowly approach the measurements of continuum-selected galaxies at z > 6, which suggests a key role of LAEs in the epoch of reionization."}],"acknowledgement":"This research made use of Astropy, a community developed core Python package for Astronomy (Astropy Collaboration et al. 2013). topcat, a graphical tool for manipulating tabular data, was also utilized in this analysis (Taylor 2005). SG would like to thank Nastasha Wijers for the discussion on the column density distribution in EAGLE. SC gratefully acknowledges support from Swiss National Science Foundation grants PP00P2 163824 and PP00P2 190092, and from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme grant agreement No 864361. GP acknowledges support from the Swiss National Science Foundation (SNF) and from the Netherlands Research School for Astronomy (NOVA).","volume":505,"extern":"1","publication":"Monthly Notices of the Royal Astronomical Society","oa_version":"Preprint","month":"07","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","galaxies: luminosity function","mass function"],"language":[{"iso":"eng"}],"type":"journal_article","date_published":"2021-07-01T00:00:00Z","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"oa":1,"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2105.00007"}],"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87"},{"scopus_import":"1","_id":"11501","author":[{"full_name":"Feltre, Anna","last_name":"Feltre","first_name":"Anna"},{"full_name":"Maseda, Michael V.","first_name":"Michael V.","last_name":"Maseda"},{"full_name":"Bacon, Roland","last_name":"Bacon","first_name":"Roland"},{"full_name":"Pradeep, Jayadev","first_name":"Jayadev","last_name":"Pradeep"},{"full_name":"Leclercq, Floriane","first_name":"Floriane","last_name":"Leclercq"},{"last_name":"Kusakabe","first_name":"Haruka","full_name":"Kusakabe, Haruka"},{"full_name":"Wisotzki, Lutz","first_name":"Lutz","last_name":"Wisotzki"},{"full_name":"Hashimoto, Takuya","last_name":"Hashimoto","first_name":"Takuya"},{"first_name":"Kasper B.","last_name":"Schmidt","full_name":"Schmidt, Kasper B."},{"first_name":"Jeremy","last_name":"Blaizot","full_name":"Blaizot, Jeremy"},{"full_name":"Brinchmann, Jarle","first_name":"Jarle","last_name":"Brinchmann"},{"full_name":"Boogaard, Leindert","first_name":"Leindert","last_name":"Boogaard"},{"full_name":"Cantalupo, Sebastiano","last_name":"Cantalupo","first_name":"Sebastiano"},{"last_name":"Carton","first_name":"David","full_name":"Carton, David"},{"first_name":"Hanae","last_name":"Inami","full_name":"Inami, Hanae"},{"first_name":"Wolfram","last_name":"Kollatschny","full_name":"Kollatschny, Wolfram"},{"full_name":"Marino, Raffaella A.","last_name":"Marino","first_name":"Raffaella A."},{"last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Nanayakkara","first_name":"Themiya","full_name":"Nanayakkara, Themiya"},{"last_name":"Richard","first_name":"Johan","full_name":"Richard, Johan"},{"last_name":"Schaye","first_name":"Joop","full_name":"Schaye, Joop"},{"last_name":"Tresse","first_name":"Laurence","full_name":"Tresse, Laurence"},{"last_name":"Urrutia","first_name":"Tanya","full_name":"Urrutia, Tanya"},{"full_name":"Verhamme, Anne","first_name":"Anne","last_name":"Verhamme"},{"last_name":"Weilbacher","first_name":"Peter M.","full_name":"Weilbacher, Peter M."}],"article_processing_charge":"No","date_created":"2022-07-06T09:38:16Z","publication_status":"published","intvolume":" 641","title":"The MUSE Hubble Ultra Deep Field Survey: XV. The mean rest-UV spectra of Lyα emitters at z > 3","quality_controlled":"1","publisher":"EDP Sciences","article_type":"original","year":"2020","citation":{"ieee":"A. Feltre et al., “The MUSE Hubble Ultra Deep Field Survey: XV. The mean rest-UV spectra of Lyα emitters at z > 3,” Astronomy & Astrophysics, vol. 641. EDP Sciences, 2020.","chicago":"Feltre, Anna, Michael V. Maseda, Roland Bacon, Jayadev Pradeep, Floriane Leclercq, Haruka Kusakabe, Lutz Wisotzki, et al. “The MUSE Hubble Ultra Deep Field Survey: XV. The Mean Rest-UV Spectra of Lyα Emitters at z > 3.” Astronomy & Astrophysics. EDP Sciences, 2020. https://doi.org/10.1051/0004-6361/202038133.","apa":"Feltre, A., Maseda, M. V., Bacon, R., Pradeep, J., Leclercq, F., Kusakabe, H., … Weilbacher, P. M. (2020). The MUSE Hubble Ultra Deep Field Survey: XV. The mean rest-UV spectra of Lyα emitters at z > 3. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202038133","ama":"Feltre A, Maseda MV, Bacon R, et al. The MUSE Hubble Ultra Deep Field Survey: XV. The mean rest-UV spectra of Lyα emitters at z > 3. Astronomy & Astrophysics. 2020;641. doi:10.1051/0004-6361/202038133","ista":"Feltre A, Maseda MV, Bacon R, Pradeep J, Leclercq F, Kusakabe H, Wisotzki L, Hashimoto T, Schmidt KB, Blaizot J, Brinchmann J, Boogaard L, Cantalupo S, Carton D, Inami H, Kollatschny W, Marino RA, Matthee JJ, Nanayakkara T, Richard J, Schaye J, Tresse L, Urrutia T, Verhamme A, Weilbacher PM. 2020. The MUSE Hubble Ultra Deep Field Survey: XV. The mean rest-UV spectra of Lyα emitters at z > 3. Astronomy & Astrophysics. 641, A118.","short":"A. Feltre, M.V. Maseda, R. Bacon, J. Pradeep, F. Leclercq, H. Kusakabe, L. Wisotzki, T. Hashimoto, K.B. Schmidt, J. Blaizot, J. Brinchmann, L. Boogaard, S. Cantalupo, D. Carton, H. Inami, W. Kollatschny, R.A. Marino, J.J. Matthee, T. Nanayakkara, J. Richard, J. Schaye, L. Tresse, T. Urrutia, A. Verhamme, P.M. Weilbacher, Astronomy & Astrophysics 641 (2020).","mla":"Feltre, Anna, et al. “The MUSE Hubble Ultra Deep Field Survey: XV. The Mean Rest-UV Spectra of Lyα Emitters at z > 3.” Astronomy & Astrophysics, vol. 641, A118, EDP Sciences, 2020, doi:10.1051/0004-6361/202038133."},"date_updated":"2022-07-19T09:35:43Z","external_id":{"arxiv":["2007.01878"]},"day":"18","arxiv":1,"doi":"10.1051/0004-6361/202038133","abstract":[{"text":"We investigated the ultraviolet (UV) spectral properties of faint Lyman-α emitters (LAEs) in the redshift range 2.9 ≤ z ≤ 4.6, and we provide material to prepare future observations of the faint Universe. We used data from the MUSE Hubble Ultra Deep Survey to construct mean rest-frame spectra of continuum-faint (median MUV of −18 and down to MUV of −16), low stellar mass (median value of 108.4 M⊙ and down to 107 M⊙) LAEs at redshift z ≳ 3. We computed various averaged spectra of LAEs, subsampled on the basis of their observational (e.g., Lyα strength, UV magnitude and spectral slope) and physical (e.g., stellar mass and star-formation rate) properties. We searched for UV spectral features other than Lyα, such as higher ionization nebular emission lines and absorption features. We successfully observed the O III]λ1666 and [C III]λ1907+C III]λ1909 collisionally excited emission lines and the He IIλ1640 recombination feature, as well as the resonant C IVλλ1548,1551 doublet either in emission or P-Cygni. We compared the observed spectral properties of the different mean spectra and find the emission lines to vary with the observational and physical properties of the LAEs. In particular, the mean spectra of LAEs with larger Lyα equivalent widths, fainter UV magnitudes, bluer UV spectral slopes, and lower stellar masses show the strongest nebular emission. The line ratios of these lines are similar to those measured in the spectra of local metal-poor galaxies, while their equivalent widths are weaker compared to the handful of extreme values detected in individual spectra of z > 2 galaxies. This suggests that weak UV features are likely ubiquitous in high z, low-mass, and faint LAEs. We publicly released the stacked spectra, as they can serve as empirical templates for the design of future observations, such as those with the James Webb Space Telescope and the Extremely Large Telescope.","lang":"eng"}],"acknowledgement":"We thank Margherita Talia, Stéphane Charlot, Adele Plat and Alba Vidal-García for helpful discussions. This work is supported by the ERC advanced grant 339659-MUSICOS (R. Bacon). AF acknowledges the support from grant PRIN MIUR 2017 20173ML3WW. MVM and JP would like to thank the Leiden/ESA Astrophysics Program for Summer Students (LEAPS) for funding at the outset of this project. FL, HK, and AV acknowledge support from the ERC starting grant ERC-757258-TRIPLE. TH was supported by Leading Initiative for Excellent Young Researchers, MEXT, Japan. JB acknowledges support by FCT/MCTES through national funds by the grant UID/FIS/04434/2019, UIDB/04434/2020 and UIDP/04434/2020 and through the Investigador FCT Contract No. IF/01654/2014/CP1215/CT0003. HI acknowledges support from JSPS KAKENHI Grant Number JP19K23462. We would also like to thank the organizers and participants of the Leiden Lorentz Center workshop: Revolutionary Spectroscopy of Today as a Springboard to Webb. This work made use of several open source python packages: NUMPY (van der Walt et al. 2011), MATPLOTLIB (Hunter 2007), ASTROPY (Astropy Collaboration 2013) and MPDAF (MUSE Python Data Analysis Framework, Piqueras et al. 2019).","volume":641,"extern":"1","publication":"Astronomy & Astrophysics","oa_version":"Published Version","article_number":"A118","month":"09","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution / galaxies: high-redshift / ISM: lines and bands / ultraviolet: ISM / ultraviolet: galaxies"],"language":[{"iso":"eng"}],"type":"journal_article","date_published":"2020-09-18T00:00:00Z","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"oa":1,"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2007.01878"}],"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87"},{"volume":638,"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.","extern":"1","citation":{"apa":"Kusakabe, H., Blaizot, J., Garel, T., Verhamme, A., Bacon, R., Richard, J., … Mahler, G. (2020). The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201937340","ama":"Kusakabe H, Blaizot J, Garel T, et al. The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6. Astronomy & Astrophysics. 2020;638. doi:10.1051/0004-6361/201937340","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.","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.","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.","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).","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."},"year":"2020","date_updated":"2022-07-19T09:35:20Z","external_id":{"arxiv":["2003.12083"]},"day":"03","doi":"10.1051/0004-6361/201937340","arxiv":1,"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"}],"quality_controlled":"1","publisher":"EDP Sciences","article_type":"original","scopus_import":"1","_id":"11503","author":[{"full_name":"Kusakabe, Haruka","first_name":"Haruka","last_name":"Kusakabe"},{"full_name":"Blaizot, Jérémy","first_name":"Jérémy","last_name":"Blaizot"},{"full_name":"Garel, Thibault","first_name":"Thibault","last_name":"Garel"},{"first_name":"Anne","last_name":"Verhamme","full_name":"Verhamme, Anne"},{"first_name":"Roland","last_name":"Bacon","full_name":"Bacon, Roland"},{"full_name":"Richard, Johan","last_name":"Richard","first_name":"Johan"},{"full_name":"Hashimoto, Takuya","last_name":"Hashimoto","first_name":"Takuya"},{"full_name":"Inami, Hanae","last_name":"Inami","first_name":"Hanae"},{"last_name":"Conseil","first_name":"Simon","full_name":"Conseil, Simon"},{"first_name":"Bruno","last_name":"Guiderdoni","full_name":"Guiderdoni, Bruno"},{"last_name":"Drake","first_name":"Alyssa B.","full_name":"Drake, Alyssa B."},{"first_name":"Edmund","last_name":"Christian Herenz","full_name":"Christian Herenz, Edmund"},{"full_name":"Schaye, Joop","first_name":"Joop","last_name":"Schaye"},{"full_name":"Oesch, Pascal","first_name":"Pascal","last_name":"Oesch"},{"last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"full_name":"Anna Marino, Raffaella","last_name":"Anna Marino","first_name":"Raffaella"},{"full_name":"Borello Schmidt, Kasper","first_name":"Kasper","last_name":"Borello Schmidt"},{"first_name":"Roser","last_name":"Pelló","full_name":"Pelló, Roser"},{"full_name":"Maseda, Michael","first_name":"Michael","last_name":"Maseda"},{"full_name":"Leclercq, Floriane","first_name":"Floriane","last_name":"Leclercq"},{"first_name":"Josephine","last_name":"Kerutt","full_name":"Kerutt, Josephine"},{"first_name":"Guillaume","last_name":"Mahler","full_name":"Mahler, Guillaume"}],"date_created":"2022-07-06T09:50:48Z","article_processing_charge":"No","publication_status":"published","intvolume":" 638","title":"The MUSE Hubble Ultra Deep Field Survey: XIV. Evolution of the Lyα emitter fraction from z = 3 to z = 6","main_file_link":[{"url":"https://arxiv.org/abs/2003.12083","open_access":"1"}],"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","type":"journal_article","date_published":"2020-06-03T00:00:00Z","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"oa":1,"keyword":["Space and Planetary Science","Astronomy and Astrophysics","dark ages / reionization / first stars / early Universe / cosmology: observations / galaxies: evolution / galaxies: high-redshift / intergalactic medium"],"language":[{"iso":"eng"}],"publication":"Astronomy & Astrophysics","oa_version":"Published Version","article_number":"A12","month":"06"},{"keyword":["Space and Planetary Science","Astronomy and Astrophysics galaxies: high-redshift / galaxies: formation / galaxies: evolution / cosmology: observations"],"language":[{"iso":"eng"}],"publication":"Astronomy & Astrophysics","oa_version":"Published Version","article_number":"A82","month":"03","main_file_link":[{"url":"https://arxiv.org/abs/2002.05731","open_access":"1"}],"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","type":"journal_article","date_published":"2020-03-11T00:00:00Z","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"oa":1,"quality_controlled":"1","publisher":"EDP Sciences","article_type":"original","scopus_import":"1","_id":"11504","author":[{"full_name":"Leclercq, Floriane","last_name":"Leclercq","first_name":"Floriane"},{"full_name":"Bacon, Roland","last_name":"Bacon","first_name":"Roland"},{"full_name":"Verhamme, Anne","first_name":"Anne","last_name":"Verhamme"},{"full_name":"Garel, Thibault","first_name":"Thibault","last_name":"Garel"},{"full_name":"Blaizot, Jérémy","last_name":"Blaizot","first_name":"Jérémy"},{"full_name":"Brinchmann, Jarle","first_name":"Jarle","last_name":"Brinchmann"},{"last_name":"Cantalupo","first_name":"Sebastiano","full_name":"Cantalupo, Sebastiano"},{"full_name":"Claeyssens, Adélaïde","last_name":"Claeyssens","first_name":"Adélaïde"},{"first_name":"Simon","last_name":"Conseil","full_name":"Conseil, Simon"},{"full_name":"Contini, Thierry","first_name":"Thierry","last_name":"Contini"},{"full_name":"Hashimoto, Takuya","first_name":"Takuya","last_name":"Hashimoto"},{"full_name":"Herenz, Edmund Christian","first_name":"Edmund Christian","last_name":"Herenz"},{"full_name":"Kusakabe, Haruka","last_name":"Kusakabe","first_name":"Haruka"},{"first_name":"Raffaella Anna","last_name":"Marino","full_name":"Marino, Raffaella Anna"},{"full_name":"Maseda, Michael","last_name":"Maseda","first_name":"Michael"},{"first_name":"Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"first_name":"Peter","last_name":"Mitchell","full_name":"Mitchell, Peter"},{"full_name":"Pezzulli, Gabriele","first_name":"Gabriele","last_name":"Pezzulli"},{"last_name":"Richard","first_name":"Johan","full_name":"Richard, Johan"},{"first_name":"Kasper Borello","last_name":"Schmidt","full_name":"Schmidt, Kasper Borello"},{"full_name":"Wisotzki, Lutz","last_name":"Wisotzki","first_name":"Lutz"}],"article_processing_charge":"No","date_created":"2022-07-06T09:56:20Z","publication_status":"published","intvolume":" 635","title":"The MUSE Hubble Ultra Deep field survey: XIII. Spatially resolved spectral properties of Lyman α haloes around star-forming galaxies at z > 3","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.","volume":635,"extern":"1","citation":{"mla":"Leclercq, Floriane, et al. “The MUSE Hubble Ultra Deep Field Survey: XIII. Spatially Resolved Spectral Properties of Lyman α Haloes around Star-Forming Galaxies at z > 3.” Astronomy & Astrophysics, vol. 635, A82, EDP Sciences, 2020, doi:10.1051/0004-6361/201937339.","short":"F. Leclercq, R. Bacon, A. Verhamme, T. Garel, J. Blaizot, J. Brinchmann, S. Cantalupo, A. Claeyssens, S. Conseil, T. Contini, T. Hashimoto, E.C. Herenz, H. Kusakabe, R.A. Marino, M. Maseda, J.J. Matthee, P. Mitchell, G. Pezzulli, J. Richard, K.B. Schmidt, L. Wisotzki, Astronomy & Astrophysics 635 (2020).","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.","ama":"Leclercq F, Bacon R, Verhamme A, et al. The MUSE Hubble Ultra Deep field survey: XIII. Spatially resolved spectral properties of Lyman α haloes around star-forming galaxies at z > 3. Astronomy & Astrophysics. 2020;635. doi:10.1051/0004-6361/201937339","apa":"Leclercq, F., Bacon, R., Verhamme, A., Garel, T., Blaizot, J., Brinchmann, J., … Wisotzki, L. (2020). The MUSE Hubble Ultra Deep field survey: XIII. Spatially resolved spectral properties of Lyman α haloes around star-forming galaxies at z > 3. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201937339","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.","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."},"year":"2020","date_updated":"2022-07-19T09:36:58Z","external_id":{"arxiv":["2002.05731"]},"day":"11","doi":"10.1051/0004-6361/201937339","arxiv":1,"abstract":[{"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.","lang":"eng"}]},{"month":"10","oa_version":"Preprint","publication":"Monthly Notices of the Royal Astronomical Society","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","dark ages","reionization","first stars","cosmology: observations"],"oa":1,"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"date_published":"2020-10-01T00:00:00Z","type":"journal_article","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2008.01731"}],"title":"The nature of CR7 revealed with MUSE: A young starburst powering extended Ly α emission at z = 6.6","intvolume":" 498","publication_status":"published","article_processing_charge":"No","date_created":"2022-07-07T10:36:01Z","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J"},{"last_name":"Pezzulli","first_name":"Gabriele","full_name":"Pezzulli, Gabriele"},{"last_name":"Mackenzie","first_name":"Ruari","full_name":"Mackenzie, Ruari"},{"first_name":"Sebastiano","last_name":"Cantalupo","full_name":"Cantalupo, Sebastiano"},{"full_name":"Kusakabe, Haruka","first_name":"Haruka","last_name":"Kusakabe"},{"first_name":"Floriane","last_name":"Leclercq","full_name":"Leclercq, Floriane"},{"first_name":"David","last_name":"Sobral","full_name":"Sobral, David"},{"first_name":"Johan","last_name":"Richard","full_name":"Richard, Johan"},{"last_name":"Wisotzki","first_name":"Lutz","full_name":"Wisotzki, Lutz"},{"full_name":"Lilly, Simon","last_name":"Lilly","first_name":"Simon"},{"full_name":"Boogaard, Leindert","last_name":"Boogaard","first_name":"Leindert"},{"last_name":"Marino","first_name":"Raffaella","full_name":"Marino, Raffaella"},{"last_name":"Maseda","first_name":"Michael","full_name":"Maseda, Michael"},{"full_name":"Nanayakkara, Themiya","first_name":"Themiya","last_name":"Nanayakkara"}],"issue":"2","_id":"11529","scopus_import":"1","article_type":"original","publisher":"Oxford University Press","page":"3043-3059","quality_controlled":"1","abstract":[{"text":"CR7 is among the most luminous Ly α emitters (LAEs) known at z = 6.6 and consists of at least three UV components that are surrounded by Ly α emission. Previous studies have suggested that it may host an extreme ionizing source. Here, we present deep integral field spectroscopy of CR7 with VLT/Multi Unit Spectroscopic Explorer (MUSE). We measure extended emission with a similar halo scale length as typical LAEs at z ≈ 5. CR7’s Ly α halo is clearly elongated along the direction connecting the multiple components, likely tracing the underlying gas distribution. The Ly α emission originates almost exclusively from the brightest UV component, but we also identify a faint kinematically distinct Ly α emitting region nearby a fainter component. Combined with new near-infrared data, the MUSE data show that the rest-frame Ly α equivalent width (EW) is ≈100 Å. This is a factor 4 higher than the EW measured in low-redshift analogues with carefully matched Ly α profiles (and thus arguably H I column density), but this EW can plausibly be explained by star formation. Alternative scenarios requiring active galactic nucleus (AGN) powering are also disfavoured by the narrower and steeper Ly α spectrum and much smaller IR to UV ratio compared to obscured AGN in other Ly α blobs. CR7’s Ly α emission, while extremely luminous, resembles the emission in more common LAEs at lower redshifts very well and is likely powered by a young metal-poor starburst.","lang":"eng"}],"arxiv":1,"doi":"10.1093/mnras/staa2550","day":"01","external_id":{"arxiv":["2008.01731"]},"date_updated":"2022-08-18T11:04:05Z","year":"2020","citation":{"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.","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.","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.","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.","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.","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","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"},"extern":"1","volume":498},{"keyword":["Space and Planetary Science","Astronomy and Astrophysics","Galaxies: evolution","Galaxies: high-redshift","Galaxies: ISM"],"language":[{"iso":"eng"}],"month":"04","oa_version":"Published Version","publication":"Monthly Notices of the Royal Astronomical Society","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/staa622"}],"oa":1,"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"type":"journal_article","date_published":"2020-04-01T00:00:00Z","article_type":"original","publisher":"Oxford University Press","quality_controlled":"1","page":"5120-5130","intvolume":" 493","title":"Elevated ionizing photon production efficiency in faint high-equivalent-width Lyman-α emitters","article_processing_charge":"No","date_created":"2022-07-07T10:46:41Z","publication_status":"published","issue":"4","author":[{"first_name":"Michael V","last_name":"Maseda","full_name":"Maseda, Michael V"},{"full_name":"Bacon, Roland","last_name":"Bacon","first_name":"Roland"},{"full_name":"Lam, Daniel","last_name":"Lam","first_name":"Daniel"},{"first_name":"Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Brinchmann","first_name":"Jarle","full_name":"Brinchmann, Jarle"},{"full_name":"Schaye, Joop","first_name":"Joop","last_name":"Schaye"},{"first_name":"Ivo","last_name":"Labbe","full_name":"Labbe, Ivo"},{"full_name":"Schmidt, Kasper B","last_name":"Schmidt","first_name":"Kasper B"},{"full_name":"Boogaard, Leindert","last_name":"Boogaard","first_name":"Leindert"},{"full_name":"Bouwens, Rychard","first_name":"Rychard","last_name":"Bouwens"},{"first_name":"Sebastiano","last_name":"Cantalupo","full_name":"Cantalupo, Sebastiano"},{"first_name":"Marijn","last_name":"Franx","full_name":"Franx, Marijn"},{"first_name":"Takuya","last_name":"Hashimoto","full_name":"Hashimoto, Takuya"},{"last_name":"Inami","first_name":"Hanae","full_name":"Inami, Hanae"},{"last_name":"Kusakabe","first_name":"Haruka","full_name":"Kusakabe, Haruka"},{"full_name":"Mahler, Guillaume","first_name":"Guillaume","last_name":"Mahler"},{"full_name":"Nanayakkara, Themiya","last_name":"Nanayakkara","first_name":"Themiya"},{"full_name":"Richard, Johan","first_name":"Johan","last_name":"Richard"},{"last_name":"Wisotzki","first_name":"Lutz","full_name":"Wisotzki, Lutz"}],"scopus_import":"1","_id":"11531","extern":"1","volume":493,"acknowledgement":"We would like to thank the anonymous referee for a thoughtful report and suggestions that have improved this manuscript. We are also grateful to everyone involved in the Spitzer Space Telescope mission and everyone at the Spitzer Science Center: we are truly fortunate to have been able to use data from this facility. J. B. acknowledges support by FCT/MCTES through national funds by this grant UID/FIS/04434/2019 and through the Investigador FCT contract no. IF/01654/2014/CP1215/CT0003. S. C. gratefully acknowledges support from Swiss National Science Foundation grant PP00P2 163824. We would also like to thank Mauro Stefanon for his assistance with de-blending the IRAC photometry, Pieter van Dokkum for a number of useful suggestions, and Daniel Schaerer for information regarding the stellar population models. This study is based on observations made with ESO telescopes at the La Silla Paranal Observatory under programs IDs 094.A-2089(B), 095.A0010(A), 096.A-0045(A), and 096.A-0045(B).","abstract":[{"text":"While low-luminosity galaxies dominate number counts at all redshifts, their contribution to cosmic reionization is poorly understood due to a lack of knowledge of their physical properties. We isolate a sample of 35 z ≈ 4–5 continuum-faint Lyman-α emitters from deep VLT/MUSE spectroscopy and directly measure their H α emission using stacked Spitzer/IRAC Ch. 1 photometry. Based on Hubble Space Telescope imaging, we determine that the average UV continuum magnitude is fainter than −16 (≈ 0.01 L⋆), implying a median Lyman-α equivalent width of 259 Å. By combining the H α measurement with the UV magnitude, we determine the ionizing photon production efficiency, ξion, a first for such faint galaxies. The measurement of log10 (ξion [Hz erg−1]) = 26.28 (+0.28−0.40) is in excess of literature measurements of both continuum- and emission line-selected samples, implying a more efficient production of ionizing photons in these lower luminosity, Lyman-α-selected systems. We conclude that this elevated efficiency can be explained by stellar populations with metallicities between 4 × 10−4 and 0.008, with light-weighted ages less than 3 Myr.","lang":"eng"}],"day":"01","doi":"10.1093/mnras/staa622","arxiv":1,"external_id":{"arxiv":["2002.11117"]},"citation":{"ista":"Maseda MV, Bacon R, Lam D, Matthee JJ, Brinchmann J, Schaye J, Labbe I, Schmidt KB, Boogaard L, Bouwens R, Cantalupo S, Franx M, Hashimoto T, Inami H, Kusakabe H, Mahler G, Nanayakkara T, Richard J, Wisotzki L. 2020. Elevated ionizing photon production efficiency in faint high-equivalent-width Lyman-α emitters. Monthly Notices of the Royal Astronomical Society. 493(4), 5120–5130.","short":"M.V. Maseda, R. Bacon, D. Lam, J.J. Matthee, J. Brinchmann, J. Schaye, I. Labbe, K.B. Schmidt, L. Boogaard, R. Bouwens, S. Cantalupo, M. Franx, T. Hashimoto, H. Inami, H. Kusakabe, G. Mahler, T. Nanayakkara, J. Richard, L. Wisotzki, Monthly Notices of the Royal Astronomical Society 493 (2020) 5120–5130.","mla":"Maseda, Michael V., et al. “Elevated Ionizing Photon Production Efficiency in Faint High-Equivalent-Width Lyman-α Emitters.” Monthly Notices of the Royal Astronomical Society, vol. 493, no. 4, Oxford University Press, 2020, pp. 5120–30, doi:10.1093/mnras/staa622.","chicago":"Maseda, Michael V, Roland Bacon, Daniel Lam, Jorryt J Matthee, Jarle Brinchmann, Joop Schaye, Ivo Labbe, et al. “Elevated Ionizing Photon Production Efficiency in Faint High-Equivalent-Width Lyman-α Emitters.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2020. https://doi.org/10.1093/mnras/staa622.","ieee":"M. V. Maseda et al., “Elevated ionizing photon production efficiency in faint high-equivalent-width Lyman-α emitters,” Monthly Notices of the Royal Astronomical Society, vol. 493, no. 4. Oxford University Press, pp. 5120–5130, 2020.","ama":"Maseda MV, Bacon R, Lam D, et al. Elevated ionizing photon production efficiency in faint high-equivalent-width Lyman-α emitters. Monthly Notices of the Royal Astronomical Society. 2020;493(4):5120-5130. doi:10.1093/mnras/staa622","apa":"Maseda, M. V., Bacon, R., Lam, D., Matthee, J. J., Brinchmann, J., Schaye, J., … Wisotzki, L. (2020). Elevated ionizing photon production efficiency in faint high-equivalent-width Lyman-α emitters. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staa622"},"year":"2020","date_updated":"2022-08-18T11:23:27Z"},{"day":"01","doi":"10.1093/mnras/staa093","arxiv":1,"abstract":[{"lang":"eng","text":"We explore deep rest-frame UV to FIR data in the COSMOS field to measure the individual spectral energy distributions (SED) of the ∼4000 SC4K (Sobral et al.) Lyman α (Ly α) emitters (LAEs) at z ∼ 2–6. We find typical stellar masses of 109.3 ± 0.6 M⊙ and star formation rates (SFR) of SFRSED=4.4+10.5−2.4 M⊙ yr−1 and SFRLyα=5.9+6.3−2.6 M⊙ yr−1, combined with very blue UV slopes of β=−2.1+0.5−0.4, but with significant variations within the population. MUV and β are correlated in a similar way to UV-selected sources, but LAEs are consistently bluer. This suggests that LAEs are the youngest and/or most dust-poor subset of the UV-selected population. We also study the Ly α rest-frame equivalent width (EW0) and find 45 ‘extreme’ LAEs with EW0 > 240 Å (3σ), implying a low number density of (7 ± 1) × 10−7 Mpc−3. Overall, we measure little to no evolution of the Ly α EW0 and scale length parameter (w0), which are consistently high (EW0=140+280−70 Å, w0=129+11−11 Å) from z ∼ 6 to z ∼ 2 and below. However, w0 is anticorrelated with MUV and stellar mass. Our results imply that sources selected as LAEs have a high Ly α escape fraction (fesc,Ly α) irrespective of cosmic time, but fesc,Ly α is still higher for UV-fainter and lower mass LAEs. The least massive LAEs (<109.5 M⊙) are typically located above the star formation ‘main sequence’ (MS), but the offset from the MS decreases towards z ∼ 6 and towards 1010 M⊙. Our results imply a lack of evolution in the properties of LAEs across time and reveals the increasing overlap in properties of LAEs and UV-continuum selected galaxies as typical star-forming galaxies at high redshift effectively become LAEs."}],"year":"2020","citation":{"mla":"Santos, S., et al. “The Evolution of Rest-Frame UV Properties, Ly α EWs, and the SFR–Stellar Mass Relation at z ∼ 2–6 for SC4K LAEs.” Monthly Notices of the Royal Astronomical Society, vol. 493, no. 1, Oxford University Press, 2020, pp. 141–60, doi:10.1093/mnras/staa093.","short":"S. Santos, D. Sobral, J.J. Matthee, J. Calhau, E. da Cunha, B. Ribeiro, A. Paulino-Afonso, P. Arrabal Haro, J. Butterworth, Monthly Notices of the Royal Astronomical Society 493 (2020) 141–160.","ista":"Santos S, Sobral D, Matthee JJ, Calhau J, da Cunha E, Ribeiro B, Paulino-Afonso A, Arrabal Haro P, Butterworth J. 2020. The evolution of rest-frame UV properties, Ly α EWs, and the SFR–stellar mass relation at z ∼ 2–6 for SC4K LAEs. Monthly Notices of the Royal Astronomical Society. 493(1), 141–160.","ama":"Santos S, Sobral D, Matthee JJ, et al. The evolution of rest-frame UV properties, Ly α EWs, and the SFR–stellar mass relation at z ∼ 2–6 for SC4K LAEs. Monthly Notices of the Royal Astronomical Society. 2020;493(1):141-160. doi:10.1093/mnras/staa093","apa":"Santos, S., Sobral, D., Matthee, J. J., Calhau, J., da Cunha, E., Ribeiro, B., … Butterworth, J. (2020). The evolution of rest-frame UV properties, Ly α EWs, and the SFR–stellar mass relation at z ∼ 2–6 for SC4K LAEs. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staa093","ieee":"S. Santos et al., “The evolution of rest-frame UV properties, Ly α EWs, and the SFR–stellar mass relation at z ∼ 2–6 for SC4K LAEs,” Monthly Notices of the Royal Astronomical Society, vol. 493, no. 1. Oxford University Press, pp. 141–160, 2020.","chicago":"Santos, S, D Sobral, Jorryt J Matthee, J Calhau, E da Cunha, B Ribeiro, A Paulino-Afonso, P Arrabal Haro, and J Butterworth. “The Evolution of Rest-Frame UV Properties, Ly α EWs, and the SFR–Stellar Mass Relation at z ∼ 2–6 for SC4K LAEs.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2020. https://doi.org/10.1093/mnras/staa093."},"date_updated":"2022-08-18T11:27:43Z","external_id":{"arxiv":["1910.02959"]},"acknowledgement":"We thank the anonymous referee for the valuable feedback that significantly improved the quality and clarity of this paper. SS and JC acknowledge studentships from Lancaster University. APA acknowledges support from Fundação para a Ciência e a Tecnologia through the project PTDC/FISAST/31546/2017. The authors would like to thank Ali Khostovan, Sara Perez Sanchez, Alex Bennett and Tom Rose for contributions and discussions in the early stages of this work. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by CALET and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. Finally, the authors acknowledge the unique value of the publicly available analysis software TOPCAT (Taylor 2005) and publicly available programming language Python, including the numpy, pyfits, matplotlib, scipy and astropy (Astropy Collaboration et al. 2013) packages. This work is based on the public SC4K sample of LAEs (Sobral et al. 2018a) and we release the full catalogue with all the photometry and properties derived in this paper, in electronic format, along with the relevant tables.","volume":493,"extern":"1","date_created":"2022-07-07T12:05:23Z","article_processing_charge":"No","publication_status":"published","intvolume":" 493","title":"The evolution of rest-frame UV properties, Ly α EWs, and the SFR–stellar mass relation at z ∼ 2–6 for SC4K LAEs","scopus_import":"1","_id":"11533","issue":"1","author":[{"full_name":"Santos, S","first_name":"S","last_name":"Santos"},{"full_name":"Sobral, D","last_name":"Sobral","first_name":"D"},{"first_name":"Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"first_name":"J","last_name":"Calhau","full_name":"Calhau, J"},{"first_name":"E","last_name":"da Cunha","full_name":"da Cunha, E"},{"last_name":"Ribeiro","first_name":"B","full_name":"Ribeiro, B"},{"last_name":"Paulino-Afonso","first_name":"A","full_name":"Paulino-Afonso, A"},{"first_name":"P","last_name":"Arrabal Haro","full_name":"Arrabal Haro, P"},{"first_name":"J","last_name":"Butterworth","full_name":"Butterworth, J"}],"publisher":"Oxford University Press","article_type":"original","quality_controlled":"1","page":"141-160","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"oa":1,"type":"journal_article","date_published":"2020-03-01T00:00:00Z","main_file_link":[{"url":"https://arxiv.org/abs/1910.02959","open_access":"1"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","oa_version":"Preprint","month":"03","publication":"Monthly Notices of the Royal Astronomical Society","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: formation","galaxies: high-redshift","galaxies: star formation"],"language":[{"iso":"eng"}]},{"type":"journal_article","date_published":"2020-02-01T00:00:00Z","oa":1,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"url":"https://arxiv.org/abs/1909.06376","open_access":"1"}],"publication":"Monthly Notices of the Royal Astronomical Society","month":"02","oa_version":"Preprint","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","dark ages","reionization","first stars","cosmology: observations"],"language":[{"iso":"eng"}],"external_id":{"arxiv":["1909.06376"]},"year":"2020","citation":{"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","chicago":"Matthee, Jorryt J, David Sobral, Max Gronke, Gabriele Pezzulli, Sebastiano Cantalupo, Huub Röttgering, Behnam Darvish, and Sérgio Santos. “Resolved Lyman-α Properties of a Luminous Lyman-Break Galaxy in a Large Ionized Bubble at z = 6.53 .” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2020. https://doi.org/10.1093/mnras/stz3554.","ieee":"J. J. Matthee et al., “Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 ,” Monthly Notices of the Royal Astronomical Society, vol. 492, no. 2. Oxford University Press, pp. 1778–1790, 2020.","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.","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.","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."},"date_updated":"2022-08-18T11:29:53Z","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"}],"day":"01","doi":"10.1093/mnras/stz3554","arxiv":1,"extern":"1","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).","volume":492,"issue":"2","author":[{"last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"full_name":"Sobral, David","last_name":"Sobral","first_name":"David"},{"last_name":"Gronke","first_name":"Max","full_name":"Gronke, Max"},{"full_name":"Pezzulli, Gabriele","last_name":"Pezzulli","first_name":"Gabriele"},{"first_name":"Sebastiano","last_name":"Cantalupo","full_name":"Cantalupo, Sebastiano"},{"full_name":"Röttgering, Huub","last_name":"Röttgering","first_name":"Huub"},{"last_name":"Darvish","first_name":"Behnam","full_name":"Darvish, Behnam"},{"last_name":"Santos","first_name":"Sérgio","full_name":"Santos, Sérgio"}],"scopus_import":"1","_id":"11534","intvolume":" 492","title":"Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 ","date_created":"2022-07-07T12:21:36Z","article_processing_charge":"No","publication_status":"published","quality_controlled":"1","page":"1778-1790","article_type":"original","publisher":"Oxford University Press"},{"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"url":"https://arxiv.org/abs/1909.11672","open_access":"1"}],"oa":1,"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"date_published":"2020-04-01T00:00:00Z","type":"journal_article","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: active","galaxies: evolution","galaxies: high-redshift","quasars: supermassive black holes","galaxies: star formation","cosmology: observations","X-rays: galaxies"],"month":"04","oa_version":"Preprint","publication":"Monthly Notices of the Royal Astronomical Society","extern":"1","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).","volume":493,"abstract":[{"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.","lang":"eng"}],"arxiv":1,"doi":"10.1093/mnras/staa476","day":"01","external_id":{"arxiv":["1909.11672"]},"date_updated":"2022-08-18T11:25:31Z","citation":{"ama":"Calhau J, Sobral D, Santos S, et al. The X-ray and radio activity of typical and luminous Ly α emitters from z ∼ 2 to z ∼ 6: Evidence for a diverse, evolving population. Monthly Notices of the Royal Astronomical Society. 2020;493(3):3341-3362. doi:10.1093/mnras/staa476","apa":"Calhau, J., Sobral, D., Santos, S., Matthee, J. J., Paulino-Afonso, A., Stroe, A., … Adams, B. (2020). The X-ray and radio activity of typical and luminous Ly α emitters from z ∼ 2 to z ∼ 6: Evidence for a diverse, evolving population. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staa476","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.","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.","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.","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.","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."},"year":"2020","article_type":"original","publisher":"Oxford University Press","page":"3341-3362","quality_controlled":"1","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","intvolume":" 493","publication_status":"published","article_processing_charge":"No","date_created":"2022-07-08T07:34:10Z","author":[{"first_name":"João","last_name":"Calhau","full_name":"Calhau, João"},{"full_name":"Sobral, David","first_name":"David","last_name":"Sobral"},{"last_name":"Santos","first_name":"Sérgio","full_name":"Santos, Sérgio"},{"first_name":"Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"full_name":"Paulino-Afonso, Ana","first_name":"Ana","last_name":"Paulino-Afonso"},{"full_name":"Stroe, Andra","last_name":"Stroe","first_name":"Andra"},{"first_name":"Brooke","last_name":"Simmons","full_name":"Simmons, Brooke"},{"full_name":"Barlow-Hall, Cassandra","last_name":"Barlow-Hall","first_name":"Cassandra"},{"first_name":"Benjamin","last_name":"Adams","full_name":"Adams, Benjamin"}],"issue":"3","_id":"11539","scopus_import":"1"},{"publisher":"Cambridge University Press","page":"21-25","quality_controlled":"1","title":"Unveiling the most luminous Lyman-α emitters in the epoch of reionisation","intvolume":" 15","publication_status":"published","article_processing_charge":"No","date_created":"2022-07-14T14:08:41Z","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J"},{"last_name":"Sobral","first_name":"David","full_name":"Sobral, David"}],"issue":"S352","_id":"11586","scopus_import":"1","extern":"1","volume":15,"abstract":[{"lang":"eng","text":"Distant luminous Lyman-α emitters are excellent targets for detailed observations of galaxies in the epoch of reionisation. Spatially resolved observations of these galaxies allow us to simultaneously probe the emission from young stars, partially ionised gas in the interstellar medium and to constrain the properties of the surrounding hydrogen in the circumgalactic medium. We review recent results from (spectroscopic) follow-up studies of the rest-frame UV, Lyman-α and [CII] emission in luminous galaxies observed ∼500 Myr after the Big Bang with ALMA, HST/WFC3 and VLT/X-SHOOTER. These galaxies likely reside in early ionised bubbles and are complex systems, consisting of multiple well separated and resolved components where traces of metals are already present."}],"arxiv":1,"doi":"10.1017/s1743921319009451","day":"04","external_id":{"arxiv":["1911.04774"]},"date_updated":"2022-08-19T08:41:12Z","year":"2020","citation":{"apa":"Matthee, J. J., & Sobral, D. (2020). Unveiling the most luminous Lyman-α emitters in the epoch of reionisation. In Proceedings of the International Astronomical Union (Vol. 15, pp. 21–25). Cambridge University Press. https://doi.org/10.1017/s1743921319009451","ama":"Matthee JJ, Sobral D. Unveiling the most luminous Lyman-α emitters in the epoch of reionisation. In: Proceedings of the International Astronomical Union. Vol 15. Cambridge University Press; 2020:21-25. doi:10.1017/s1743921319009451","chicago":"Matthee, Jorryt J, and David Sobral. “Unveiling the Most Luminous Lyman-α Emitters in the Epoch of Reionisation.” In Proceedings of the International Astronomical Union, 15:21–25. Cambridge University Press, 2020. https://doi.org/10.1017/s1743921319009451.","ieee":"J. J. Matthee and D. Sobral, “Unveiling the most luminous Lyman-α emitters in the epoch of reionisation,” in Proceedings of the International Astronomical Union, 2020, vol. 15, no. S352, pp. 21–25.","short":"J.J. Matthee, D. Sobral, in:, Proceedings of the International Astronomical Union, Cambridge University Press, 2020, pp. 21–25.","mla":"Matthee, Jorryt J., and David Sobral. “Unveiling the Most Luminous Lyman-α Emitters in the Epoch of Reionisation.” Proceedings of the International Astronomical Union, vol. 15, no. S352, Cambridge University Press, 2020, pp. 21–25, doi:10.1017/s1743921319009451.","ista":"Matthee JJ, Sobral D. 2020. Unveiling the most luminous Lyman-α emitters in the epoch of reionisation. Proceedings of the International Astronomical Union. vol. 15, 21–25."},"language":[{"iso":"eng"}],"keyword":["Astronomy and Astrophysics","Space and Planetary Science","galaxies: formation","galaxies: evolution","galaxies: high-redshift"],"month":"06","oa_version":"Preprint","publication":"Proceedings of the International Astronomical Union","status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1911.04774"}],"oa":1,"publication_identifier":{"issn":["1743-9213"],"eissn":["1743-9221"]},"date_published":"2020-06-04T00:00:00Z","type":"conference"},{"date_published":"2019-04-16T00:00:00Z","type":"journal_article","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"oa":1,"main_file_link":[{"url":"https://arxiv.org/abs/1902.05960","open_access":"1"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","related_material":{"link":[{"relation":"erratum","url":"https://doi.org/10.1051/0004-6361/201834565e"}]},"publication":"Astronomy & Astrophysics","oa_version":"Published Version","month":"04","article_number":"A89","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: ISM / galaxies: star formation / galaxies: evolution / galaxies: high-redshift"],"date_updated":"2022-07-19T09:36:08Z","year":"2019","citation":{"apa":"Nanayakkara, T., Brinchmann, J., Boogaard, L., Bouwens, R., Cantalupo, S., Feltre, A., … Verhamme, A. (2019). Exploring He II λ1640 emission line properties at z ∼2−4. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201834565","ama":"Nanayakkara T, Brinchmann J, Boogaard L, et al. Exploring He II λ1640 emission line properties at z ∼2−4. Astronomy & Astrophysics. 2019;648. doi:10.1051/0004-6361/201834565","chicago":"Nanayakkara, Themiya, Jarle Brinchmann, Leindert Boogaard, Rychard Bouwens, Sebastiano Cantalupo, Anna Feltre, Wolfram Kollatschny, et al. “Exploring He II Λ1640 Emission Line Properties at z ∼2−4.” Astronomy & Astrophysics. EDP Sciences, 2019. https://doi.org/10.1051/0004-6361/201834565.","ieee":"T. Nanayakkara et al., “Exploring He II λ1640 emission line properties at z ∼2−4,” Astronomy & Astrophysics, vol. 648. EDP Sciences, 2019.","mla":"Nanayakkara, Themiya, et al. “Exploring He II Λ1640 Emission Line Properties at z ∼2−4.” Astronomy & Astrophysics, vol. 648, A89, EDP Sciences, 2019, doi:10.1051/0004-6361/201834565.","short":"T. Nanayakkara, J. Brinchmann, L. Boogaard, R. Bouwens, S. Cantalupo, A. Feltre, W. Kollatschny, R.A. Marino, M. Maseda, J.J. Matthee, M. Paalvast, J. Richard, A. Verhamme, Astronomy & Astrophysics 648 (2019).","ista":"Nanayakkara T, Brinchmann J, Boogaard L, Bouwens R, Cantalupo S, Feltre A, Kollatschny W, Marino RA, Maseda M, Matthee JJ, Paalvast M, Richard J, Verhamme A. 2019. Exploring He II λ1640 emission line properties at z ∼2−4. Astronomy & Astrophysics. 648, A89."},"external_id":{"arxiv":["1902.05960"]},"doi":"10.1051/0004-6361/201834565","arxiv":1,"day":"16","abstract":[{"text":"Deep optical spectroscopic surveys of galaxies provide a unique opportunity to investigate rest-frame ultra-violet (UV) emission line properties of galaxies at z ∼ 2 − 4.5. Here we combine VLT/MUSE Guaranteed Time Observations of the Hubble Deep Field South, Ultra Deep Field, COSMOS, and several quasar fields with other publicly available data from VLT/VIMOS and VLT/FORS2 to construct a catalogue of He II λ1640 emitters at z ≳ 2. The deepest areas of our MUSE pointings reach a 3σ line flux limit of 3.1 × 10−19 erg s−1 cm−2. After discarding broad-line active galactic nuclei, we find 13 He II λ1640 detections from MUSE with a median MUV = −20.1 and 21 tentative He II λ1640 detections from other public surveys. Excluding Lyα, all except two galaxies in our sample show at least one other rest-UV emission line, with C III] λ1907, λ1909 being the most prominent. We use multi-wavelength data available in the Hubble legacy fields to derive basic galaxy properties of our sample through spectral energy distribution fitting techniques. Taking advantage of the high-quality spectra obtained by MUSE (∼10 − 30 h of exposure time per pointing), we use photo-ionisation models to study the rest-UV emission line diagnostics of the He II λ1640 emitters. Line ratios of our sample can be reproduced by moderately sub-solar photo-ionisation models, however, we find that including effects of binary stars lead to degeneracies in most free parameters. Even after considering extra ionising photons produced by extreme sub-solar metallicity binary stellar models, photo-ionisation models are unable to reproduce rest-frame He II λ1640 equivalent widths (∼0.2 − 10 Å), thus additional mechanisms are necessary in models to match the observed He II λ1640 properties.","lang":"eng"}],"volume":648,"acknowledgement":"The authors wish to thank the referee for constructive comments that improved the paper substantially. We thank the BPASS team for making the stellar population models available. We thank Elizabeth Stanway, Claus Leitherer, Daniel Schaerer, Jorick Vink, and Nell Byler for insightful discussions. We thank the Lorentz Centre and the scientific organizers of the Characterizing galaxies with spectroscopy with a view for JWST workshop held at the Lorentz Centre in 2017 October, which promoted useful discussions in the wider community. TN, JB, and RB acknowledges the Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO) top grant TOP1.16.057. AF acknowledges support from the ERC via an Advanced Grant under grant agreement no. 339659-MUSICOS. JB acknowledges support by Fundação para a Ciência e a Tecnologia (FCT) through national funds (UID/FIS/04434/2013) and Investigador FCT contract IF/01654/2014/CP1215/CT0003, and by FEDER through COMPETE2020 (POCI-01-0145-FEDER-007672). JR acknowledges support from the ERC Starting grant 336736 (CALENDS). This research made use of astropy (http://www.astropy.org) a community-developed core Python package for Astronomy (Astropy Collaboration 2013, 2018) and pandas (McKinney 2010). Figures were generated using matplotlib (Hunter 2007) and seaborn (https://seaborn.pydata.org). Facilities: VLT (MUSE).","extern":"1","_id":"11499","scopus_import":"1","author":[{"last_name":"Nanayakkara","first_name":"Themiya","full_name":"Nanayakkara, Themiya"},{"full_name":"Brinchmann, Jarle","first_name":"Jarle","last_name":"Brinchmann"},{"last_name":"Boogaard","first_name":"Leindert","full_name":"Boogaard, Leindert"},{"first_name":"Rychard","last_name":"Bouwens","full_name":"Bouwens, Rychard"},{"full_name":"Cantalupo, Sebastiano","last_name":"Cantalupo","first_name":"Sebastiano"},{"full_name":"Feltre, Anna","last_name":"Feltre","first_name":"Anna"},{"first_name":"Wolfram","last_name":"Kollatschny","full_name":"Kollatschny, Wolfram"},{"first_name":"Raffaella Anna","last_name":"Marino","full_name":"Marino, Raffaella Anna"},{"full_name":"Maseda, Michael","last_name":"Maseda","first_name":"Michael"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J"},{"full_name":"Paalvast, Mieke","last_name":"Paalvast","first_name":"Mieke"},{"first_name":"Johan","last_name":"Richard","full_name":"Richard, Johan"},{"full_name":"Verhamme, Anne","last_name":"Verhamme","first_name":"Anne"}],"publication_status":"published","article_processing_charge":"No","date_created":"2022-07-06T09:07:06Z","title":"Exploring He II λ1640 emission line properties at z ∼2−4","intvolume":" 648","quality_controlled":"1","publisher":"EDP Sciences","article_type":"original"},{"volume":623,"acknowledgement":"We thank the anonymous referees for multiple comments and suggestions which have improved the manuscript. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. We have benefited greatly from the publicly available programming language PYTHON, including the NUMPY & SCIPY (Van Der Walt et al. 2011; Jones et al. 2001), MATPLOTLIB (Hunter 2007) and ASTROPY (Astropy Collaboration 2013) packages, and the TOPCAT analysis program (Taylor 2013). The results and samples of LAEs used for this paper are publicly available (see e.g. Sobral et al. 2017, 2018a) and we also provide the toy model used as a PYTHON script.","extern":"1","doi":"10.1051/0004-6361/201833075","arxiv":1,"day":"26","abstract":[{"text":"Lyman-α (Lyα) is intrinsically the brightest line emitted from active galaxies. While it originates from many physical processes, for star-forming galaxies the intrinsic Lyα luminosity is a direct tracer of the Lyman-continuum (LyC) radiation produced by the most massive O- and early-type B-stars (M⋆ ≳ 10 M⊙) with lifetimes of a few Myrs. As such, Lyα luminosity should be an excellent instantaneous star formation rate (SFR) indicator. However, its resonant nature and susceptibility to dust as a rest-frame UV photon makes Lyα very hard to interpret due to the uncertain Lyα escape fraction, fesc, Lyα. Here we explore results from the CAlibrating LYMan-α with Hα (CALYMHA) survey at z = 2.2, follow-up of Lyα emitters (LAEs) at z = 2.2 − 2.6 and a z ∼ 0−0.3 compilation of LAEs to directly measure fesc, Lyα with Hα. We derive a simple empirical relation that robustly retrieves fesc, Lyα as a function of Lyα rest-frame EW (EW0): fesc,Lyα = 0.0048 EW0[Å] ± 0.05 and we show that it constrains a well-defined anti-correlation between ionisation efficiency (ξion) and dust extinction in LAEs. Observed Lyα luminosities and EW0 are easy measurable quantities at high redshift, thus making our relation a practical tool to estimate intrinsic Lyα and LyC luminosities under well controlled and simple assumptions. Our results allow observed Lyα luminosities to be used to compute SFRs for LAEs at z ∼ 0−2.6 within ±0.2 dex of the Hα dust corrected SFRs. We apply our empirical SFR(Lyα,EW0) calibration to several sources at z ≥ 2.6 to find that star-forming LAEs have SFRs typically ranging from 0.1 to 20 M⊙ yr−1 and that our calibration might be even applicable for the most luminous LAEs within the epoch of re-ionisation. Our results imply high ionisation efficiencies (log10[ξion/Hz erg−1] = 25.4−25.6) and low dust content in LAEs across cosmic time, and will be easily tested with future observations with JWST which can obtain Hα and Hβ measurements for high-redshift LAEs.","lang":"eng"}],"date_updated":"2022-07-19T09:37:20Z","year":"2019","citation":{"chicago":"Sobral, David, and Jorryt J Matthee. “Predicting Lyα Escape Fractions with a Simple Observable: Lyα in Emission as an Empirically Calibrated Star Formation Rate Indicator.” Astronomy & Astrophysics. EDP Sciences, 2019. https://doi.org/10.1051/0004-6361/201833075.","ieee":"D. Sobral and J. J. Matthee, “Predicting Lyα escape fractions with a simple observable: Lyα in emission as an empirically calibrated star formation rate indicator,” Astronomy & Astrophysics, vol. 623. EDP Sciences, 2019.","apa":"Sobral, D., & Matthee, J. J. (2019). Predicting Lyα escape fractions with a simple observable: Lyα in emission as an empirically calibrated star formation rate indicator. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201833075","ama":"Sobral D, Matthee JJ. Predicting Lyα escape fractions with a simple observable: Lyα in emission as an empirically calibrated star formation rate indicator. Astronomy & Astrophysics. 2019;623. doi:10.1051/0004-6361/201833075","ista":"Sobral D, Matthee JJ. 2019. Predicting Lyα escape fractions with a simple observable: Lyα in emission as an empirically calibrated star formation rate indicator. Astronomy & Astrophysics. 623, A157.","mla":"Sobral, David, and Jorryt J. Matthee. “Predicting Lyα Escape Fractions with a Simple Observable: Lyα in Emission as an Empirically Calibrated Star Formation Rate Indicator.” Astronomy & Astrophysics, vol. 623, A157, EDP Sciences, 2019, doi:10.1051/0004-6361/201833075.","short":"D. Sobral, J.J. Matthee, Astronomy & Astrophysics 623 (2019)."},"external_id":{"arxiv":["1803.08923"]},"publisher":"EDP Sciences","article_type":"original","quality_controlled":"1","publication_status":"published","date_created":"2022-07-06T11:08:16Z","article_processing_charge":"No","title":"Predicting Lyα escape fractions with a simple observable: Lyα in emission as an empirically calibrated star formation rate indicator","intvolume":" 623","_id":"11507","scopus_import":"1","author":[{"full_name":"Sobral, David","last_name":"Sobral","first_name":"David"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J"}],"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1803.08923"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"oa":1,"date_published":"2019-03-26T00:00:00Z","type":"journal_article","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift / galaxies: star formation / galaxies: statistics / galaxies: evolution / galaxies: formation / galaxies: ISM"],"oa_version":"Published Version","month":"03","article_number":"A157","publication":"Astronomy & Astrophysics"},{"type":"journal_article","date_published":"2019-10-01T00:00:00Z","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"oa":1,"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1811.00556"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","publication":"Monthly Notices of the Royal Astronomical Society","oa_version":"Preprint","month":"10","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"],"language":[{"iso":"eng"}],"year":"2019","citation":{"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.","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.","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.","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","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","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.","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."},"date_updated":"2022-08-19T06:38:42Z","external_id":{"arxiv":["1811.00556"]},"day":"01","doi":"10.1093/mnras/stz2149","arxiv":1,"abstract":[{"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.","lang":"eng"}],"volume":489,"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).","extern":"1","scopus_import":"1","_id":"11535","issue":"1","author":[{"last_name":"Khostovan","first_name":"A A","full_name":"Khostovan, A A"},{"full_name":"Sobral, D","first_name":"D","last_name":"Sobral"},{"full_name":"Mobasher, B","first_name":"B","last_name":"Mobasher"},{"last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"first_name":"R K","last_name":"Cochrane","full_name":"Cochrane, R K"},{"full_name":"Chartab, N","first_name":"N","last_name":"Chartab"},{"full_name":"Jafariyazani, M","first_name":"M","last_name":"Jafariyazani"},{"first_name":"A","last_name":"Paulino-Afonso","full_name":"Paulino-Afonso, A"},{"last_name":"Santos","first_name":"S","full_name":"Santos, S"},{"full_name":"Calhau, J","first_name":"J","last_name":"Calhau"}],"article_processing_charge":"No","date_created":"2022-07-07T13:01:03Z","publication_status":"published","intvolume":" 489","title":"The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities","quality_controlled":"1","page":"555-573","publisher":"Oxford University Press","article_type":"original"},{"oa_version":"Preprint","month":"03","publication":"Monthly Notices of the Royal Astronomical Society","keyword":["Space and Planetary Science","Astronomy and Astrophysics : galaxies: evolution","galaxies: formation","galaxies: star formation","cosmology: theory"],"language":[{"iso":"eng"}],"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"oa":1,"type":"journal_article","date_published":"2019-03-01T00:00:00Z","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1805.05956"}],"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","article_processing_charge":"No","date_created":"2022-07-08T07:48:31Z","publication_status":"published","intvolume":" 484","title":"The origin of scatter in the star formation rate–stellar mass relation","scopus_import":"1","_id":"11540","issue":"1","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X"},{"last_name":"Schaye","first_name":"Joop","full_name":"Schaye, Joop"}],"publisher":"Oxford University Press","article_type":"original","quality_controlled":"1","page":"915-932","day":"01","arxiv":1,"doi":"10.1093/mnras/stz030","abstract":[{"text":"Observations have revealed that the star formation rate (SFR) and stellar mass (Mstar) of star-forming galaxies follow a tight relation known as the galaxy main sequence. However, what physical information is encoded in this relation is under debate. Here, we use the EAGLE cosmological hydrodynamical simulation to study the mass dependence, evolution, and origin of scatter in the SFR–Mstar relation. At z = 0, we find that the scatter decreases slightly with stellar mass from 0.35 dex at Mstar ≈ 109 M⊙ to 0.30 dex at Mstar ≳ 1010.5 M⊙. The scatter decreases from z = 0 to z = 5 by 0.05 dex at Mstar ≳ 1010 M⊙ and by 0.15 dex for lower masses. We show that the scatter at z = 0.1 originates from a combination of fluctuations on short time-scales (ranging from 0.2–2 Gyr) that are presumably associated with self-regulation from cooling, star formation, and outflows, but is dominated by long time-scale (∼10 Gyr) variations related to differences in halo formation times. Shorter time-scale fluctuations are relatively more important for lower mass galaxies. At high masses, differences in black hole formation efficiency cause additional scatter, but also diminish the scatter caused by different halo formation times. While individual galaxies cross the main sequence multiple times during their evolution, they fluctuate around tracks associated with their halo properties, i.e. galaxies above/below the main sequence at z = 0.1 tend to have been above/below the main sequence for ≫1 Gyr.","lang":"eng"}],"year":"2019","citation":{"apa":"Matthee, J. J., & Schaye, J. (2019). The origin of scatter in the star formation rate–stellar mass relation. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stz030","ama":"Matthee JJ, Schaye J. The origin of scatter in the star formation rate–stellar mass relation. Monthly Notices of the Royal Astronomical Society. 2019;484(1):915-932. doi:10.1093/mnras/stz030","chicago":"Matthee, Jorryt J, and Joop Schaye. “The Origin of Scatter in the Star Formation Rate–Stellar Mass Relation.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2019. https://doi.org/10.1093/mnras/stz030.","ieee":"J. J. Matthee and J. Schaye, “The origin of scatter in the star formation rate–stellar mass relation,” Monthly Notices of the Royal Astronomical Society, vol. 484, no. 1. Oxford University Press, pp. 915–932, 2019.","short":"J.J. Matthee, J. Schaye, Monthly Notices of the Royal Astronomical Society 484 (2019) 915–932.","mla":"Matthee, Jorryt J., and Joop Schaye. “The Origin of Scatter in the Star Formation Rate–Stellar Mass Relation.” Monthly Notices of the Royal Astronomical Society, vol. 484, no. 1, Oxford University Press, 2019, pp. 915–32, doi:10.1093/mnras/stz030.","ista":"Matthee JJ, Schaye J. 2019. The origin of scatter in the star formation rate–stellar mass relation. Monthly Notices of the Royal Astronomical Society. 484(1), 915–932."},"date_updated":"2022-08-19T06:42:43Z","external_id":{"arxiv":["1805.05956"]},"volume":484,"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).","extern":"1"},{"publication":"Monthly Notices of the Royal Astronomical Society","oa_version":"Preprint","month":"01","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","galaxies: ISM","cosmology: observations","dark ages","reionization","first stars","early Universe"],"date_published":"2019-01-01T00:00:00Z","type":"journal_article","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"oa":1,"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1710.08422"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","_id":"11541","scopus_import":"1","author":[{"full_name":"Sobral, David","first_name":"David","last_name":"Sobral"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X"},{"last_name":"Brammer","first_name":"Gabriel","full_name":"Brammer, Gabriel"},{"full_name":"Ferrara, Andrea","first_name":"Andrea","last_name":"Ferrara"},{"first_name":"Lara","last_name":"Alegre","full_name":"Alegre, Lara"},{"first_name":"Huub","last_name":"Röttgering","full_name":"Röttgering, Huub"},{"full_name":"Schaerer, Daniel","last_name":"Schaerer","first_name":"Daniel"},{"full_name":"Mobasher, Bahram","first_name":"Bahram","last_name":"Mobasher"},{"last_name":"Darvish","first_name":"Behnam","full_name":"Darvish, Behnam"}],"issue":"2","publication_status":"published","article_processing_charge":"No","date_created":"2022-07-08T10:40:05Z","title":"On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components","intvolume":" 482","page":"2422-2441","quality_controlled":"1","publisher":"Oxford University Press","article_type":"original","date_updated":"2022-08-19T06:49:36Z","citation":{"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.","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.","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","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","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.","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.","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."},"year":"2019","external_id":{"arxiv":["1710.08422"]},"arxiv":1,"doi":"10.1093/mnras/sty2779","day":"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."}],"volume":482,"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.","extern":"1"},{"article_type":"original","publisher":"Oxford University Press","page":"2999-3015","quality_controlled":"1","title":"The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar mass","intvolume":" 478","publication_status":"published","date_created":"2022-07-08T11:48:48Z","article_processing_charge":"No","author":[{"first_name":"A A","last_name":"Khostovan","full_name":"Khostovan, A A"},{"full_name":"Sobral, D","last_name":"Sobral","first_name":"D"},{"full_name":"Mobasher, B","first_name":"B","last_name":"Mobasher"},{"full_name":"Best, P N","first_name":"P N","last_name":"Best"},{"full_name":"Smail, I","first_name":"I","last_name":"Smail"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X"},{"full_name":"Darvish, B","last_name":"Darvish","first_name":"B"},{"full_name":"Nayyeri, H","last_name":"Nayyeri","first_name":"H"},{"last_name":"Hemmati","first_name":"S","full_name":"Hemmati, S"},{"last_name":"Stott","first_name":"J P","full_name":"Stott, J P"}],"issue":"3","_id":"11549","scopus_import":"1","extern":"1","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.","volume":478,"abstract":[{"lang":"eng","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."}],"doi":"10.1093/mnras/sty925","arxiv":1,"day":"01","external_id":{"arxiv":["1705.01101"]},"date_updated":"2022-08-19T06:53:39Z","citation":{"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.","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.","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.","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","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.","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."},"year":"2018","language":[{"iso":"eng"}],"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"],"month":"08","oa_version":"Published Version","publication":"Monthly Notices of the Royal Astronomical Society","status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"url":"https://arxiv.org/abs/1705.01101"}],"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"date_published":"2018-08-01T00:00:00Z","type":"journal_article"},{"title":"Kiloparsec-scale gaseous clumps and star formation at z = 5–7","intvolume":" 478","publication_status":"published","date_created":"2022-07-11T08:05:42Z","article_processing_charge":"No","author":[{"full_name":"Carniani, S","last_name":"Carniani","first_name":"S"},{"first_name":"R","last_name":"Maiolino","full_name":"Maiolino, R"},{"first_name":"R","last_name":"Amorin","full_name":"Amorin, R"},{"full_name":"Pentericci, L","first_name":"L","last_name":"Pentericci"},{"first_name":"A","last_name":"Pallottini","full_name":"Pallottini, A"},{"last_name":"Ferrara","first_name":"A","full_name":"Ferrara, A"},{"full_name":"Willott, C J","last_name":"Willott","first_name":"C J"},{"first_name":"R","last_name":"Smit","full_name":"Smit, R"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X"},{"full_name":"Sobral, D","last_name":"Sobral","first_name":"D"},{"last_name":"Santini","first_name":"P","full_name":"Santini, P"},{"full_name":"Castellano, M","first_name":"M","last_name":"Castellano"},{"full_name":"De Barros, S","first_name":"S","last_name":"De Barros"},{"last_name":"Fontana","first_name":"A","full_name":"Fontana, A"},{"last_name":"Grazian","first_name":"A","full_name":"Grazian, A"},{"full_name":"Guaita, L","first_name":"L","last_name":"Guaita"}],"issue":"1","_id":"11555","scopus_import":"1","article_type":"original","publisher":"Oxford University Press","page":"1170-1184","quality_controlled":"1","abstract":[{"lang":"eng","text":"We investigate the morphology of the [C II] emission in a sample of ‘normal’ star-forming galaxies at 5 < z < 7.2 in relation to their UV (rest-frame) counterpart. We use new Atacama Large Millimetre/submillimetre Array (ALMA) observations of galaxies at z ∼ 6–7, as well as a careful re-analysis of archival ALMA data. In total 29 galaxies were analysed, 21 of which are detected in [C II]. For several of the latter the [C II] emission breaks into multiple components. Only a fraction of these [C II] components, if any, is associated with the primary UV systems, while the bulk of the [C II] emission is associated either with fainter UV components, or not associated with any UV counterpart at the current limits. By taking into account the presence of all these components, we find that the L[CII]–SFR (star formation rate) relation at early epochs is fully consistent with the local relation, but it has a dispersion of 0.48 ± 0.07 dex, which is about two times larger than observed locally. We also find that the deviation from the local L[CII]–SFR relation has a weak anticorrelation with the EW(Ly α). The morphological analysis also reveals that [C II] emission is generally much more extended than the UV emission. As a consequence, these primordial galaxies are characterized by a [C II] surface brightness generally much lower than expected from the local Σ[CII]−ΣSFR relation. These properties are likely a consequence of a combination of different effects, namely gas metallicity, [C II] emission from obscured star-forming regions, strong variations of the ionization parameter, and circumgalactic gas in accretion or ejected by these primeval galaxies."}],"doi":"10.1093/mnras/sty1088","arxiv":1,"day":"01","external_id":{"arxiv":["1712.03985"]},"date_updated":"2022-08-19T06:58:06Z","year":"2018","citation":{"mla":"Carniani, S., et al. “Kiloparsec-Scale Gaseous Clumps and Star Formation at z = 5–7.” Monthly Notices of the Royal Astronomical Society, vol. 478, no. 1, Oxford University Press, 2018, pp. 1170–84, doi:10.1093/mnras/sty1088.","short":"S. Carniani, R. Maiolino, R. Amorin, L. Pentericci, A. Pallottini, A. Ferrara, C.J. Willott, R. Smit, J.J. Matthee, D. Sobral, P. Santini, M. Castellano, S. De Barros, A. Fontana, A. Grazian, L. Guaita, Monthly Notices of the Royal Astronomical Society 478 (2018) 1170–1184.","ista":"Carniani S, Maiolino R, Amorin R, Pentericci L, Pallottini A, Ferrara A, Willott CJ, Smit R, Matthee JJ, Sobral D, Santini P, Castellano M, De Barros S, Fontana A, Grazian A, Guaita L. 2018. Kiloparsec-scale gaseous clumps and star formation at z = 5–7. Monthly Notices of the Royal Astronomical Society. 478(1), 1170–1184.","ama":"Carniani S, Maiolino R, Amorin R, et al. Kiloparsec-scale gaseous clumps and star formation at z = 5–7. Monthly Notices of the Royal Astronomical Society. 2018;478(1):1170-1184. doi:10.1093/mnras/sty1088","apa":"Carniani, S., Maiolino, R., Amorin, R., Pentericci, L., Pallottini, A., Ferrara, A., … Guaita, L. (2018). Kiloparsec-scale gaseous clumps and star formation at z = 5–7. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/sty1088","ieee":"S. Carniani et al., “Kiloparsec-scale gaseous clumps and star formation at z = 5–7,” Monthly Notices of the Royal Astronomical Society, vol. 478, no. 1. Oxford University Press, pp. 1170–1184, 2018.","chicago":"Carniani, S, R Maiolino, R Amorin, L Pentericci, A Pallottini, A Ferrara, C J Willott, et al. “Kiloparsec-Scale Gaseous Clumps and Star Formation at z = 5–7.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2018. https://doi.org/10.1093/mnras/sty1088."},"extern":"1","acknowledgement":"This paper makes use of the following ALMA data:\r\nADS/JAO.ALMA#2012.1.00719.S, ADS/JAO.ALMA#2012.A.00040.S,\r\nADS/JAO.ALMA#2013.A.00433.S, ADS/JAO.ALMA#2011.0.00115.S,\r\nADS/JAO.ALMA#2012.1.00033.S, ADS/JAO.ALMA#2012.1.00523.S,\r\nADS/JAO.ALMA#2013.1.00815.S, ADS/JAO.ALMA#2015.1.00834.S.,\r\nADS/JAO.ALMA#2015.1.01105.S, AND ADS/JAO.ALMA#2016.1.01240.S\r\nwhich can be retrieved from the ALMA data archive:\r\nhttps://almascience.eso.org/ alma-data/archive. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. We are grateful to G. Jones to for providing his [C II] flux maps. RM and SC acknowledge support by the Science and Technology Facilities Council (STFC). RM acknowledges ERC Advanced Grant 695671 ‘QUENCH’. AF acknowledges support from the ERC Advanced Grant INTERSTELLAR H2020/740120.","volume":478,"month":"07","oa_version":"Preprint","publication":"Monthly Notices of the Royal Astronomical Society","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","galaxies: ISM","galaxies: formation"],"oa":1,"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"date_published":"2018-07-01T00:00:00Z","type":"journal_article","status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"url":"https://arxiv.org/abs/1712.03985","open_access":"1"}]},{"doi":"10.1093/mnras/sty782","arxiv":1,"day":"01","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"}],"date_updated":"2022-08-19T07:01:08Z","citation":{"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","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.","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.","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.","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.","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."},"year":"2018","external_id":{"arxiv":["1802.10102"]},"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.","volume":477,"extern":"1","publication_status":"published","date_created":"2022-07-12T07:18:02Z","article_processing_charge":"No","title":"The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN","intvolume":" 477","_id":"11557","scopus_import":"1","author":[{"first_name":"David","last_name":"Sobral","full_name":"Sobral, David"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J"},{"first_name":"Behnam","last_name":"Darvish","full_name":"Darvish, Behnam"},{"first_name":"Ian","last_name":"Smail","full_name":"Smail, Ian"},{"first_name":"Philip N","last_name":"Best","full_name":"Best, Philip N"},{"last_name":"Alegre","first_name":"Lara","full_name":"Alegre, Lara"},{"last_name":"Röttgering","first_name":"Huub","full_name":"Röttgering, Huub"},{"first_name":"Bahram","last_name":"Mobasher","full_name":"Mobasher, Bahram"},{"last_name":"Paulino-Afonso","first_name":"Ana","full_name":"Paulino-Afonso, Ana"},{"last_name":"Stroe","first_name":"Andra","full_name":"Stroe, Andra"},{"full_name":"Oteo, Iván","last_name":"Oteo","first_name":"Iván"}],"issue":"2","publisher":"Oxford University Press","article_type":"original","page":"2817-2840","quality_controlled":"1","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"oa":1,"date_published":"2018-06-01T00:00:00Z","type":"journal_article","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1802.10102"}],"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa_version":"Preprint","month":"06","publication":"Monthly Notices of the Royal Astronomical Society","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: active","galaxies: evolution","galaxies: high-redshift","galaxies: ISM","galaxies: starburst","cosmology: observations"]}]