[{"publication":"Astronomy & Astrophysics","oa_version":"Published Version","month":"04","article_number":"A44","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift / galaxies: formation / galaxies: evolution / cosmology: observations"],"date_published":"2022-04-07T00:00:00Z","type":"journal_article","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"oa":1,"main_file_link":[{"url":"https://arxiv.org/abs/2201.07257","open_access":"1"}],"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","_id":"11488","scopus_import":"1","author":[{"full_name":"Kusakabe, Haruka","first_name":"Haruka","last_name":"Kusakabe"},{"full_name":"Verhamme, Anne","first_name":"Anne","last_name":"Verhamme"},{"full_name":"Blaizot, Jérémy","first_name":"Jérémy","last_name":"Blaizot"},{"first_name":"Thibault","last_name":"Garel","full_name":"Garel, Thibault"},{"full_name":"Wisotzki, Lutz","last_name":"Wisotzki","first_name":"Lutz"},{"full_name":"Leclercq, Floriane","last_name":"Leclercq","first_name":"Floriane"},{"last_name":"Bacon","first_name":"Roland","full_name":"Bacon, Roland"},{"last_name":"Schaye","first_name":"Joop","full_name":"Schaye, Joop"},{"last_name":"Gallego","first_name":"Sofia G.","full_name":"Gallego, Sofia G."},{"full_name":"Kerutt, Josephine","first_name":"Josephine","last_name":"Kerutt"},{"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":"Maseda, Michael","last_name":"Maseda","first_name":"Michael"},{"full_name":"Nanayakkara, Themiya","first_name":"Themiya","last_name":"Nanayakkara"},{"full_name":"Pelló, Roser","last_name":"Pelló","first_name":"Roser"},{"last_name":"Richard","first_name":"Johan","full_name":"Richard, Johan"},{"last_name":"Tresse","first_name":"Laurence","full_name":"Tresse, Laurence"},{"full_name":"Urrutia, Tanya","first_name":"Tanya","last_name":"Urrutia"},{"full_name":"Vitte, Eloïse","first_name":"Eloïse","last_name":"Vitte"}],"publication_status":"published","article_processing_charge":"No","date_created":"2022-07-05T14:27:26Z","title":"The MUSE eXtremely Deep Field: Individual detections of Ly<i>α</i> haloes around rest-frame UV-selected galaxies at <i>z</i> ≃ 2.9–4.4","intvolume":"       660","quality_controlled":"1","publisher":"EDP Sciences","article_type":"original","date_updated":"2022-07-19T09:33:24Z","citation":{"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 &#38; Astrophysics 660 (2022).","mla":"Kusakabe, Haruka, et al. “The MUSE EXtremely Deep Field: Individual Detections of Ly<i>α</i> Haloes around Rest-Frame UV-Selected Galaxies at <i>z</i> ≃ 2.9–4.4.” <i>Astronomy &#38; Astrophysics</i>, vol. 660, A44, EDP Sciences, 2022, doi:<a href=\"https://doi.org/10.1051/0004-6361/202142302\">10.1051/0004-6361/202142302</a>.","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 Ly<i>α</i> haloes around rest-frame UV-selected galaxies at <i>z</i> ≃ 2.9–4.4. Astronomy &#38; Astrophysics. 660, A44.","ama":"Kusakabe H, Verhamme A, Blaizot J, et al. The MUSE eXtremely Deep Field: Individual detections of Ly<i>α</i> haloes around rest-frame UV-selected galaxies at <i>z</i> ≃ 2.9–4.4. <i>Astronomy &#38; Astrophysics</i>. 2022;660. doi:<a href=\"https://doi.org/10.1051/0004-6361/202142302\">10.1051/0004-6361/202142302</a>","apa":"Kusakabe, H., Verhamme, A., Blaizot, J., Garel, T., Wisotzki, L., Leclercq, F., … Vitte, E. (2022). The MUSE eXtremely Deep Field: Individual detections of Ly<i>α</i> haloes around rest-frame UV-selected galaxies at <i>z</i> ≃ 2.9–4.4. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202142302\">https://doi.org/10.1051/0004-6361/202142302</a>","ieee":"H. Kusakabe <i>et al.</i>, “The MUSE eXtremely Deep Field: Individual detections of Ly<i>α</i> haloes around rest-frame UV-selected galaxies at <i>z</i> ≃ 2.9–4.4,” <i>Astronomy &#38; Astrophysics</i>, vol. 660. EDP Sciences, 2022.","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 Ly<i>α</i> Haloes around Rest-Frame UV-Selected Galaxies at <i>z</i> ≃ 2.9–4.4.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2022. <a href=\"https://doi.org/10.1051/0004-6361/202142302\">https://doi.org/10.1051/0004-6361/202142302</a>."},"year":"2022","external_id":{"arxiv":["2201.07257"]},"doi":"10.1051/0004-6361/202142302","arxiv":1,"day":"07","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"}],"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).","volume":660,"extern":"1"},{"date_published":"2022-03-30T00:00:00Z","type":"journal_article","oa":1,"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"url":"https://arxiv.org/abs/2111.14855","open_access":"1"}],"publication":"Astronomy & Astrophysics","month":"03","article_number":"A10","oa_version":"Published Version","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift / techniques: spectroscopic / galaxies: stellar content / galaxies: formation"],"external_id":{"arxiv":["2111.14855"]},"date_updated":"2022-07-19T09:33:46Z","year":"2022","citation":{"ista":"Matthee JJ, Feltre A, Maseda M, Nanayakkara T, Boogaard L, Bacon R, Verhamme A, Leclercq F, Kusakabe H, Urrutia T, Wisotzki L. 2022. Deciphering stellar metallicities in the early universe: Case study of a young galaxy at z = 4.77 in the MUSE eXtremely Deep Field. Astronomy &#38; Astrophysics. 660, A10.","short":"J.J. Matthee, A. Feltre, M. Maseda, T. Nanayakkara, L. Boogaard, R. Bacon, A. Verhamme, F. Leclercq, H. Kusakabe, T. Urrutia, L. Wisotzki, Astronomy &#38; Astrophysics 660 (2022).","mla":"Matthee, Jorryt J., et al. “Deciphering Stellar Metallicities in the Early Universe: Case Study of a Young Galaxy at z = 4.77 in the MUSE EXtremely Deep Field.” <i>Astronomy &#38; Astrophysics</i>, vol. 660, A10, EDP Sciences, 2022, doi:<a href=\"https://doi.org/10.1051/0004-6361/202142187\">10.1051/0004-6361/202142187</a>.","chicago":"Matthee, Jorryt J, Anna Feltre, Michael Maseda, Themiya Nanayakkara, Leindert Boogaard, Roland Bacon, Anne Verhamme, et al. “Deciphering Stellar Metallicities in the Early Universe: Case Study of a Young Galaxy at z = 4.77 in the MUSE EXtremely Deep Field.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2022. <a href=\"https://doi.org/10.1051/0004-6361/202142187\">https://doi.org/10.1051/0004-6361/202142187</a>.","ieee":"J. J. Matthee <i>et al.</i>, “Deciphering stellar metallicities in the early universe: Case study of a young galaxy at z = 4.77 in the MUSE eXtremely Deep Field,” <i>Astronomy &#38; Astrophysics</i>, vol. 660. EDP Sciences, 2022.","apa":"Matthee, J. J., Feltre, A., Maseda, M., Nanayakkara, T., Boogaard, L., Bacon, R., … Wisotzki, L. (2022). Deciphering stellar metallicities in the early universe: Case study of a young galaxy at z = 4.77 in the MUSE eXtremely Deep Field. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202142187\">https://doi.org/10.1051/0004-6361/202142187</a>","ama":"Matthee JJ, Feltre A, Maseda M, et al. Deciphering stellar metallicities in the early universe: Case study of a young galaxy at z = 4.77 in the MUSE eXtremely Deep Field. <i>Astronomy &#38; Astrophysics</i>. 2022;660. doi:<a href=\"https://doi.org/10.1051/0004-6361/202142187\">10.1051/0004-6361/202142187</a>"},"abstract":[{"lang":"eng","text":"Directly characterising the first generations of stars in distant galaxies is a key quest of observational cosmology. We present a case study of ID53 at z = 4.77, the UV-brightest (but L⋆) star-forming galaxy at z > 3 in the MUSE eXtremely Deep Field with a mass of ≈109 M⊙. In addition to very strong Lyman-α (Lyα) emission, we clearly detect the (stellar) continuum and an N V P Cygni feature, interstellar absorption, fine-structure emission and nebular C IV emission lines in the 140 h spectrum. Continuum emission from two spatially resolved components in Hubble Space Telescope data are blended in the MUSE data, but we show that the nebular C IV emission originates from a subcomponent of the galaxy. The UV spectrum can be fit with recent BPASS stellar population models combined with single-burst or continuous star formation histories (SFHs), a standard initial mass function, and an attenuation law. Models with a young age and low metallicity (log10(age/yr) = 6.5–7.6 and [Z/H] = −2.15 to −1.15) are preferred, but the details depend on the assumed SFH. The intrinsic Hα luminosity of the best-fit models is an order of magnitude higher than the Hα luminosity inferred from Spitzer/IRAC data, which either suggests a high escape fraction of ionising photons, a high relative attenuation of nebular to stellar dust, or a complex SFH. The metallicity appears lower than the metallicity in more massive galaxies at z = 3 − 5, consistent with the scenario according to which younger galaxies have lower metallicities. This chemical immaturity likely facilitates Lyα escape, explaining why the Lyα equivalent width is anti-correlated with stellar metallicity. Finally, we stress that uncertainties in SFHs impose a challenge for future inferences of the stellar metallicity of young galaxies. This highlights the need for joint (spatially resolved) analyses of stellar spectra and photo-ionisation models."}],"doi":"10.1051/0004-6361/202142187","arxiv":1,"day":"30","extern":"1","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.","volume":660,"author":[{"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":"Feltre, Anna","first_name":"Anna","last_name":"Feltre"},{"full_name":"Maseda, Michael","last_name":"Maseda","first_name":"Michael"},{"full_name":"Nanayakkara, Themiya","first_name":"Themiya","last_name":"Nanayakkara"},{"full_name":"Boogaard, Leindert","first_name":"Leindert","last_name":"Boogaard"},{"first_name":"Roland","last_name":"Bacon","full_name":"Bacon, Roland"},{"full_name":"Verhamme, Anne","first_name":"Anne","last_name":"Verhamme"},{"first_name":"Floriane","last_name":"Leclercq","full_name":"Leclercq, Floriane"},{"full_name":"Kusakabe, Haruka","last_name":"Kusakabe","first_name":"Haruka"},{"last_name":"Urrutia","first_name":"Tanya","full_name":"Urrutia, Tanya"},{"last_name":"Wisotzki","first_name":"Lutz","full_name":"Wisotzki, Lutz"}],"_id":"11490","scopus_import":"1","title":"Deciphering stellar metallicities in the early universe: Case study of a young galaxy at z = 4.77 in the MUSE eXtremely Deep Field","intvolume":"       660","publication_status":"published","article_processing_charge":"No","date_created":"2022-07-05T15:25:35Z","quality_controlled":"1","article_type":"original","publisher":"EDP Sciences"},{"day":"25","doi":"10.1051/0004-6361/202141900","arxiv":1,"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."}],"year":"2022","citation":{"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.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2022. <a href=\"https://doi.org/10.1051/0004-6361/202141900\">https://doi.org/10.1051/0004-6361/202141900</a>.","ieee":"J. Kerutt <i>et al.</i>, “Equivalent widths of Lyman α emitters in MUSE-Wide and MUSE-Deep,” <i>Astronomy &#38; Astrophysics</i>, vol. 659. EDP Sciences, 2022.","ama":"Kerutt J, Wisotzki L, Verhamme A, et al. Equivalent widths of Lyman α emitters in MUSE-Wide and MUSE-Deep. <i>Astronomy &#38; Astrophysics</i>. 2022;659. doi:<a href=\"https://doi.org/10.1051/0004-6361/202141900\">10.1051/0004-6361/202141900</a>","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. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202141900\">https://doi.org/10.1051/0004-6361/202141900</a>","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 &#38; Astrophysics. 659, 183.","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 &#38; Astrophysics 659 (2022).","mla":"Kerutt, J., et al. “Equivalent Widths of Lyman α Emitters in MUSE-Wide and MUSE-Deep.” <i>Astronomy &#38; Astrophysics</i>, vol. 659, 183, EDP Sciences, 2022, doi:<a href=\"https://doi.org/10.1051/0004-6361/202141900\">10.1051/0004-6361/202141900</a>."},"date_updated":"2022-07-19T09:47:16Z","external_id":{"arxiv":["2202.06642"]},"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.","extern":"1","article_processing_charge":"No","date_created":"2022-07-06T08:17:27Z","publication_status":"published","intvolume":"       659","title":"Equivalent widths of Lyman α emitters in MUSE-Wide and MUSE-Deep","scopus_import":"1","_id":"11497","author":[{"first_name":"J.","last_name":"Kerutt","full_name":"Kerutt, J."},{"full_name":"Wisotzki, L.","last_name":"Wisotzki","first_name":"L."},{"last_name":"Verhamme","first_name":"A.","full_name":"Verhamme, A."},{"full_name":"Schmidt, K. B.","last_name":"Schmidt","first_name":"K. B."},{"first_name":"F.","last_name":"Leclercq","full_name":"Leclercq, F."},{"first_name":"E. C.","last_name":"Herenz","full_name":"Herenz, E. C."},{"full_name":"Urrutia, T.","first_name":"T.","last_name":"Urrutia"},{"full_name":"Garel, T.","first_name":"T.","last_name":"Garel"},{"last_name":"Hashimoto","first_name":"T.","full_name":"Hashimoto, T."},{"last_name":"Maseda","first_name":"M.","full_name":"Maseda, M."},{"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":"Kusakabe, H.","last_name":"Kusakabe","first_name":"H."},{"full_name":"Schaye, J.","first_name":"J.","last_name":"Schaye"},{"full_name":"Richard, J.","first_name":"J.","last_name":"Richard"},{"full_name":"Guiderdoni, B.","last_name":"Guiderdoni","first_name":"B."},{"first_name":"V.","last_name":"Mauerhofer","full_name":"Mauerhofer, V."},{"full_name":"Nanayakkara, T.","last_name":"Nanayakkara","first_name":"T."},{"last_name":"Vitte","first_name":"E.","full_name":"Vitte, E."}],"publisher":"EDP Sciences","article_type":"original","quality_controlled":"1","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"oa":1,"type":"journal_article","date_published":"2022-03-25T00:00:00Z","main_file_link":[{"url":"https://arxiv.org/abs/2202.06642","open_access":"1"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","oa_version":"Published Version","article_number":"183","month":"03","publication":"Astronomy & Astrophysics","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift / galaxies: formation / galaxies: evolution / cosmology: observations"],"language":[{"iso":"eng"}]},{"language":[{"iso":"eng"}],"keyword":["dark ages","reionization","first stars","intergalactic medium","galaxies: formation"],"publication":"Monthly Notices of the Royal Astronomical Society","oa_version":"Preprint","month":"12","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2004.14496"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","date_published":"2021-12-01T00:00:00Z","type":"journal_article","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"oa":1,"page":"3697-3709","quality_controlled":"1","publisher":"Oxford University Press","article_type":"original","_id":"11522","scopus_import":"1","author":[{"first_name":"Max","last_name":"Gronke","full_name":"Gronke, Max"},{"first_name":"Pierre","last_name":"Ocvirk","full_name":"Ocvirk, Pierre"},{"full_name":"Mason, Charlotte","first_name":"Charlotte","last_name":"Mason"},{"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":"Bosman","first_name":"Sarah E I","full_name":"Bosman, Sarah E I"},{"first_name":"Jenny G","last_name":"Sorce","full_name":"Sorce, Jenny G"},{"first_name":"Joseph","last_name":"Lewis","full_name":"Lewis, Joseph"},{"last_name":"Ahn","first_name":"Kyungjin","full_name":"Ahn, Kyungjin"},{"first_name":"Dominique","last_name":"Aubert","full_name":"Aubert, Dominique"},{"full_name":"Dawoodbhoy, Taha","first_name":"Taha","last_name":"Dawoodbhoy"},{"full_name":"Iliev, Ilian T","last_name":"Iliev","first_name":"Ilian T"},{"last_name":"Shapiro","first_name":"Paul R","full_name":"Shapiro, Paul R"},{"full_name":"Yepes, Gustavo","last_name":"Yepes","first_name":"Gustavo"}],"issue":"3","publication_status":"published","date_created":"2022-07-07T09:30:21Z","article_processing_charge":"No","title":"Lyman-α transmission properties of the intergalactic medium in the CoDaII simulation","intvolume":"       508","acknowledgement":"The authors thank the referee for constructive feedback that improved the outcome of this study. We are grateful to Antoinette Songaila Cowie for sharing the ‘NEPLA4’ spectrum with us. This research has made use of NASA’s Astrophysics Data System, and many open source projects such as trident (Hummels et al. 2017), IPython (Pérez & Granger 2007), SciPy (Virtanen et al. 2019), NumPy (Walt et al. 2011), matplotlib (Hunter 2007), pandas (McKinney 2010), and the yt-project (Turk et al. 2011). MG was supported by NASA through the NASA Hubble Fellowship grant HST-HF2-51409 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. MG acknowledges support from NASA grants HST-GO-15643.017, and HST-AR15797.001 as well as XSEDE grant TG-AST180036. CAM acknowledges support by NASA Headquarters through the NASA Hubble Fellowship grant HST-HF2-51413.001-A. PRS was supported in part by U.S. NSF grant AST-1009799, NASA grant NNX11AE09G, and supercomputer resources from NSF XSEDE grant TG AST090005 and the Texas Advanced Computing Center (TACC) at The University of Texas at Austin. JM acknowledges a Zwicky Prize Fellowship from ETH Zurich. GY acknowledges financial support by MICIU/FEDER under project grant PGC2018-094975-C21. SEIB acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 669253). ITI was supported by the Science and Technology Facilities Council [grants ST/I000976/1, ST/F002858/1, ST/P000525/1, and ST/T000473/1]; and The Southeast Physics Network (SEPNet). KA was supported by NRF2016R1D1A1B04935414 and NRF-2016R1A5A1013277. KA also appreciates APCTP for its hospitality during completion of this work. PO acknowledges support from the French ANR funded project ORAGE (ANR-14-CE33-0016). ND and DA acknowledge funding from the French ANR for project ANR-12-JS05- 0001 (EMMA). The CoDa II simulation was performed at Oak Ridge National Laboratory/Oak Ridge Leadership Computing Facility on the Titan supercomputer (INCITE 2016 award AST031). Processing was performed on the Eos and Rhea clusters. Resolution study simulations were performed on Piz Daint at the Swiss National Supercomputing Center (PRACE Tier 0 award, project id pr37). The authors would like to acknowledge the High Performance Computing center of the University of Strasbourg for supporting this work by providing scientific support and access to computing resources. Part of the computing resources were funded by the Equipex EquipMeso project (Programme Investissements d’Avenir) and the CPER Alsacalcul/Big Data.","volume":508,"extern":"1","date_updated":"2022-08-18T10:45:56Z","citation":{"ama":"Gronke M, Ocvirk P, Mason C, et al. Lyman-α transmission properties of the intergalactic medium in the CoDaII simulation. <i>Monthly Notices of the Royal Astronomical Society</i>. 2021;508(3):3697-3709. doi:<a href=\"https://doi.org/10.1093/mnras/stab2762\">10.1093/mnras/stab2762</a>","apa":"Gronke, M., Ocvirk, P., Mason, C., Matthee, J. J., Bosman, S. E. I., Sorce, J. G., … Yepes, G. (2021). Lyman-α transmission properties of the intergalactic medium in the CoDaII simulation. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stab2762\">https://doi.org/10.1093/mnras/stab2762</a>","chicago":"Gronke, Max, Pierre Ocvirk, Charlotte Mason, Jorryt J Matthee, Sarah E I Bosman, Jenny G Sorce, Joseph Lewis, et al. “Lyman-α Transmission Properties of the Intergalactic Medium in the CoDaII Simulation.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2021. <a href=\"https://doi.org/10.1093/mnras/stab2762\">https://doi.org/10.1093/mnras/stab2762</a>.","ieee":"M. Gronke <i>et al.</i>, “Lyman-α transmission properties of the intergalactic medium in the CoDaII simulation,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 508, no. 3. Oxford University Press, pp. 3697–3709, 2021.","short":"M. Gronke, P. Ocvirk, C. Mason, J.J. Matthee, S.E.I. Bosman, J.G. Sorce, J. Lewis, K. Ahn, D. Aubert, T. Dawoodbhoy, I.T. Iliev, P.R. Shapiro, G. Yepes, Monthly Notices of the Royal Astronomical Society 508 (2021) 3697–3709.","mla":"Gronke, Max, et al. “Lyman-α Transmission Properties of the Intergalactic Medium in the CoDaII Simulation.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 508, no. 3, Oxford University Press, 2021, pp. 3697–709, doi:<a href=\"https://doi.org/10.1093/mnras/stab2762\">10.1093/mnras/stab2762</a>.","ista":"Gronke M, Ocvirk P, Mason C, Matthee JJ, Bosman SEI, Sorce JG, Lewis J, Ahn K, Aubert D, Dawoodbhoy T, Iliev IT, Shapiro PR, Yepes G. 2021. Lyman-α transmission properties of the intergalactic medium in the CoDaII simulation. Monthly Notices of the Royal Astronomical Society. 508(3), 3697–3709."},"year":"2021","external_id":{"arxiv":["2004.14496"]},"arxiv":1,"doi":"10.1093/mnras/stab2762","day":"01","abstract":[{"lang":"eng","text":"The decline in abundance of Lyman-α (Lyα) emitting galaxies at z ≳ 6 is a powerful and commonly used probe to constrain the progress of cosmic reionization. We use the CODAII simulation, which is a radiation hydrodynamic simulation featuring a box of ∼94 comoving Mpc side length, to compute the Lyα transmission properties of the intergalactic medium (IGM) at z ∼ 5.8 to 7. Our results mainly confirm previous studies, i.e. we find a declining Lyα transmission with redshift and a large sightline-to-sightline variation. However, motivated by the recent discovery of blue Lyα peaks at high redshift, we also analyse the IGM transmission on the blue side, which shows a rapid decline at z ≳ 6 of the blue transmission. This low transmission can be attributed not only to the presence of neutral regions but also to the residual neutral hydrogen within ionized regions, for which a density even as low as nHI∼10−9cm−3 (sometimes combined with kinematic effects) leads to a significantly reduced visibility. Still, we find that ∼1 per cent of sightlines towards M1600AB ∼ −21 galaxies at z ∼ 7 are transparent enough to allow a transmission of a blue Lyα peak. We discuss our results in the context of the interpretation of observations."}]},{"language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: formation","galaxies: ISM","galaxies: starburst","dark ages","reionization","first stars"],"month":"07","oa_version":"Preprint","publication":"Monthly Notices of the Royal Astronomical Society","status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2102.07779"}],"oa":1,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"date_published":"2021-07-01T00:00:00Z","type":"journal_article","article_type":"original","publisher":"Oxford University Press","page":"1382-1412","quality_controlled":"1","title":"The X-SHOOTER Lyman α survey at z = 2 (XLS-z2) I: What makes a galaxy a Lyman α emitter?","intvolume":"       505","publication_status":"published","article_processing_charge":"No","date_created":"2022-07-07T09:33:39Z","author":[{"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":"Sobral, David","last_name":"Sobral","first_name":"David"},{"first_name":"Matthew","last_name":"Hayes","full_name":"Hayes, Matthew"},{"first_name":"Gabriele","last_name":"Pezzulli","full_name":"Pezzulli, Gabriele"},{"first_name":"Max","last_name":"Gronke","full_name":"Gronke, Max"},{"first_name":"Daniel","last_name":"Schaerer","full_name":"Schaerer, Daniel"},{"full_name":"Naidu, Rohan P","last_name":"Naidu","first_name":"Rohan P"},{"last_name":"Röttgering","first_name":"Huub","full_name":"Röttgering, Huub"},{"full_name":"Calhau, João","first_name":"João","last_name":"Calhau"},{"first_name":"Ana","last_name":"Paulino-Afonso","full_name":"Paulino-Afonso, Ana"},{"first_name":"Sérgio","last_name":"Santos","full_name":"Santos, Sérgio"},{"last_name":"Amorín","first_name":"Ricardo","full_name":"Amorín, Ricardo"}],"issue":"1","_id":"11523","scopus_import":"1","extern":"1","acknowledgement":"We thank the referee for constructive comments and suggestions. We thank Dawn Erb, Ruari Mackenzie, Ivan Oteo, Ryan Sanders, and Johannes Zabl for useful discussions and suggestions. It is a pleasure to thank the ESO User Support, in particular Giacomo Beccari, Carlo Manara, John Pritchard, Marina Rejkuba, and Lowell Tacconi-Garman for assistance in the preparation and execution of the observations. Based on observations obtained with the VLT, programs 084.A-0303, 088.A-0672, 091.A-0413, 091.A-0546, 092.A0774, 097.A-0153, 098.A-0819, 099.A-0758, 099.A-0254, 101.B0779, and 102.A-0652. 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. Based on observations made with the NASA/ESA HST through programs 9133, 9367, 11694, and 12471, and obtained from the Hubble Legacy Archive, which is a collaboration between the Space Telescope Science Institute (STScI/NASA), the Space Telescope European Coordinating Facility (ST-ECF/ESA), and the Canadian Astronomy Data Centre (CADC/NRC/CSA). This work is based on observations taken by the CANDELS Multi-Cycle Treasury Program with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. MG was supported by NASA through the NASA Hubble Fellowship grant HST-HF2-51409 and acknowledges support from HST grants\r\nHST-GO-15643.017-A, HST-AR-15039.003-A, and XSEDE grant TG-AST180036. GP acknowledges support from the Netherlands Research School for Astronomy (NOVA). RA acknowledges the support of ANID FONDECYT Regular Grant 1202007. We gratefully acknowledge the PYTHON programming language, its NUMPY, MATPLOTLIB, SCIPY, LMFIT (Jones et al. 2001; Hunter 2007; van der Walt, Colbert & Varoquaux 2011), PANDAS (McKinney 2010), and ASTROPY (Astropy Collaboration 2013) packages, and the TOPCAT analysis tool (Taylor 2013). Dedicated to the memory of A. C. J.Matthee (1953–2020).","volume":505,"abstract":[{"text":"We present the first results from the X-SHOOTER Lyman α survey at z = 2 (XLS-z2). XLS-z2 is a deep spectroscopic survey of 35 Lyman α emitters (LAEs) utilizing ≈90 h of exposure time with Very Large Telescope/X-SHOOTER and covers rest-frame Ly α to H α emission with R ≈ 4000. We present the sample selection, the observations, and the data reduction. Systemic redshifts are measured from rest-frame optical lines for 33/35 sources. In the stacked spectrum, our LAEs are characterized by an interstellar medium with little dust, a low metallicity, and a high ionization state. The ionizing sources are young hot stars that power strong emission lines in the optical and high-ionization lines in the ultraviolet (UV). The LAEs exhibit clumpy UV morphologies and have outflowing kinematics with blueshifted Si II absorption, a broad [O III] component, and a red-skewed Ly α line. Typically, 30 per cent of the Ly α photons escape, of which one quarter on the blue side of the systemic velocity. A fraction of Ly α photons escape directly at the systemic suggesting clear channels enabling an ≈10 per cent escape of ionizing photons, consistent with an inference based on Mg II. A combination of a low effective H I column density, a low dust content, and young starburst determines whether a star-forming galaxy is observed as an LAE. The first is possibly related to outflows and/or a fortunate viewing angle, while we find that the latter two in LAEs are typical for their stellar mass of 109 M⊙.","lang":"eng"}],"arxiv":1,"doi":"10.1093/mnras/stab1304","day":"01","external_id":{"arxiv":["2102.07779"]},"date_updated":"2022-08-18T10:49:00Z","year":"2021","citation":{"apa":"Matthee, J. J., Sobral, D., Hayes, M., Pezzulli, G., Gronke, M., Schaerer, D., … Amorín, R. (2021). The X-SHOOTER Lyman α survey at z = 2 (XLS-z2) I: What makes a galaxy a Lyman α emitter? <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stab1304\">https://doi.org/10.1093/mnras/stab1304</a>","ama":"Matthee JJ, Sobral D, Hayes M, et al. The X-SHOOTER Lyman α survey at z = 2 (XLS-z2) I: What makes a galaxy a Lyman α emitter? <i>Monthly Notices of the Royal Astronomical Society</i>. 2021;505(1):1382-1412. doi:<a href=\"https://doi.org/10.1093/mnras/stab1304\">10.1093/mnras/stab1304</a>","chicago":"Matthee, Jorryt J, David Sobral, Matthew Hayes, Gabriele Pezzulli, Max Gronke, Daniel Schaerer, Rohan P Naidu, et al. “The X-SHOOTER Lyman α Survey at z = 2 (XLS-Z2) I: What Makes a Galaxy a Lyman α Emitter?” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2021. <a href=\"https://doi.org/10.1093/mnras/stab1304\">https://doi.org/10.1093/mnras/stab1304</a>.","ieee":"J. J. Matthee <i>et al.</i>, “The X-SHOOTER Lyman α survey at z = 2 (XLS-z2) I: What makes a galaxy a Lyman α emitter?,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 505, no. 1. Oxford University Press, pp. 1382–1412, 2021.","short":"J.J. Matthee, D. Sobral, M. Hayes, G. Pezzulli, M. Gronke, D. Schaerer, R.P. Naidu, H. Röttgering, J. Calhau, A. Paulino-Afonso, S. Santos, R. Amorín, Monthly Notices of the Royal Astronomical Society 505 (2021) 1382–1412.","mla":"Matthee, Jorryt J., et al. “The X-SHOOTER Lyman α Survey at z = 2 (XLS-Z2) I: What Makes a Galaxy a Lyman α Emitter?” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 505, no. 1, Oxford University Press, 2021, pp. 1382–412, doi:<a href=\"https://doi.org/10.1093/mnras/stab1304\">10.1093/mnras/stab1304</a>.","ista":"Matthee JJ, Sobral D, Hayes M, Pezzulli G, Gronke M, Schaerer D, Naidu RP, Röttgering H, Calhau J, Paulino-Afonso A, Santos S, Amorín R. 2021. The X-SHOOTER Lyman α survey at z = 2 (XLS-z2) I: What makes a galaxy a Lyman α emitter? Monthly Notices of the Royal Astronomical Society. 505(1), 1382–1412."}},{"scopus_import":"1","_id":"11504","author":[{"last_name":"Leclercq","first_name":"Floriane","full_name":"Leclercq, Floriane"},{"last_name":"Bacon","first_name":"Roland","full_name":"Bacon, Roland"},{"full_name":"Verhamme, Anne","first_name":"Anne","last_name":"Verhamme"},{"last_name":"Garel","first_name":"Thibault","full_name":"Garel, Thibault"},{"full_name":"Blaizot, Jérémy","last_name":"Blaizot","first_name":"Jérémy"},{"first_name":"Jarle","last_name":"Brinchmann","full_name":"Brinchmann, Jarle"},{"last_name":"Cantalupo","first_name":"Sebastiano","full_name":"Cantalupo, Sebastiano"},{"full_name":"Claeyssens, Adélaïde","last_name":"Claeyssens","first_name":"Adélaïde"},{"last_name":"Conseil","first_name":"Simon","full_name":"Conseil, Simon"},{"full_name":"Contini, Thierry","first_name":"Thierry","last_name":"Contini"},{"last_name":"Hashimoto","first_name":"Takuya","full_name":"Hashimoto, Takuya"},{"last_name":"Herenz","first_name":"Edmund Christian","full_name":"Herenz, Edmund Christian"},{"last_name":"Kusakabe","first_name":"Haruka","full_name":"Kusakabe, Haruka"},{"last_name":"Marino","first_name":"Raffaella Anna","full_name":"Marino, Raffaella Anna"},{"full_name":"Maseda, Michael","first_name":"Michael","last_name":"Maseda"},{"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":"Mitchell","first_name":"Peter","full_name":"Mitchell, Peter"},{"last_name":"Pezzulli","first_name":"Gabriele","full_name":"Pezzulli, Gabriele"},{"full_name":"Richard, Johan","first_name":"Johan","last_name":"Richard"},{"full_name":"Schmidt, Kasper Borello","last_name":"Schmidt","first_name":"Kasper Borello"},{"last_name":"Wisotzki","first_name":"Lutz","full_name":"Wisotzki, Lutz"}],"date_created":"2022-07-06T09:56:20Z","article_processing_charge":"No","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","quality_controlled":"1","publisher":"EDP Sciences","article_type":"original","year":"2020","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 &#62; 3.” <i>Astronomy &#38; Astrophysics</i>, vol. 635, A82, EDP Sciences, 2020, doi:<a href=\"https://doi.org/10.1051/0004-6361/201937339\">10.1051/0004-6361/201937339</a>.","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 &#38; 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 &#62; 3. Astronomy &#38; 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 &#62; 3. <i>Astronomy &#38; Astrophysics</i>. 2020;635. doi:<a href=\"https://doi.org/10.1051/0004-6361/201937339\">10.1051/0004-6361/201937339</a>","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 &#62; 3. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201937339\">https://doi.org/10.1051/0004-6361/201937339</a>","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 &#62; 3.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2020. <a href=\"https://doi.org/10.1051/0004-6361/201937339\">https://doi.org/10.1051/0004-6361/201937339</a>.","ieee":"F. Leclercq <i>et al.</i>, “The MUSE Hubble Ultra Deep field survey: XIII. Spatially resolved spectral properties of Lyman α haloes around star-forming galaxies at z &#62; 3,” <i>Astronomy &#38; Astrophysics</i>, vol. 635. EDP Sciences, 2020."},"date_updated":"2022-07-19T09:36:58Z","external_id":{"arxiv":["2002.05731"]},"day":"11","arxiv":1,"doi":"10.1051/0004-6361/201937339","abstract":[{"lang":"eng","text":"We present spatially resolved maps of six individually-detected Lyman α haloes (LAHs) as well as a first statistical analysis of the Lyman α (Lyα) spectral signature in the circum-galactic medium of high-redshift star-forming galaxies (−17.5 >  MUV >  −21.5) using the Multi-Unit Spectroscopic Explorer. Our resolved spectroscopic analysis of the LAHs reveals significant intrahalo variations of the Lyα line profile. Using a three-dimensional two-component model for the Lyα emission, we measured the full width at half maximum (FWHM), the peak velocity shift, and the asymmetry of the Lyα line in the core and in the halo of 19 galaxies. We find that the Lyα line shape is statistically different in the halo compared to the core (in terms of width, peak wavelength, and asymmetry) for ≈40% of our galaxies. Similarly to object-by-object based studies and a recent resolved study using lensing, we find a correlation between the peak velocity shift and the width of the Lyα line both at the interstellar and circum-galactic scales. This trend has been predicted by radiative transfer simulations of galactic winds as a result of resonant scattering in outflows. While there is a lack of correlation between the spectral properties and the spatial scale lengths of our LAHs, we find a correlation between the width of the line in the LAH and the halo flux fraction. Interestingly, UV bright galaxies (MUV <  −20) show broader, more redshifted, and less asymmetric Lyα lines in their haloes. The most significant correlation found is for the FWHM of the line and the UV continuum slope of the galaxy, suggesting that the redder galaxies have broader Lyα lines. The generally broad and red line shapes found in the halo component suggest that the Lyα haloes are powered either by scattering processes through an outflowing medium, fluorescent emission from outflowing cold clumps of gas, or a mix of both. Considering the large diversity of the Lyα line profiles observed in our sample and the lack of strong correlation, the interpretation of our results is still broadly open and underlines the need for realistic spatially resolved models of the LAHs."}],"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","publication":"Astronomy & Astrophysics","oa_version":"Published Version","article_number":"A82","month":"03","keyword":["Space and Planetary Science","Astronomy and Astrophysics galaxies: high-redshift / galaxies: formation / galaxies: evolution / cosmology: observations"],"language":[{"iso":"eng"}],"type":"journal_article","date_published":"2020-03-11T00:00:00Z","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"oa":1,"main_file_link":[{"url":"https://arxiv.org/abs/2002.05731","open_access":"1"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public"},{"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1910.02959"}],"date_published":"2020-03-01T00:00:00Z","type":"journal_article","oa":1,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: formation","galaxies: high-redshift","galaxies: star formation"],"publication":"Monthly Notices of the Royal Astronomical Society","month":"03","oa_version":"Preprint","extern":"1","volume":493,"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.","external_id":{"arxiv":["1910.02959"]},"date_updated":"2022-08-18T11:27:43Z","citation":{"short":"S. Santos, D. Sobral, J.J. Matthee, J. Calhau, E. da Cunha, B. Ribeiro, A. Paulino-Afonso, P. Arrabal Haro, J. Butterworth, Monthly Notices of the Royal Astronomical Society 493 (2020) 141–160.","mla":"Santos, S., et al. “The Evolution of Rest-Frame UV Properties, Ly α EWs, and the SFR–Stellar Mass Relation at z ∼ 2–6 for SC4K LAEs.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 493, no. 1, Oxford University Press, 2020, pp. 141–60, doi:<a href=\"https://doi.org/10.1093/mnras/staa093\">10.1093/mnras/staa093</a>.","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.","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. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staa093\">https://doi.org/10.1093/mnras/staa093</a>","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. <i>Monthly Notices of the Royal Astronomical Society</i>. 2020;493(1):141-160. doi:<a href=\"https://doi.org/10.1093/mnras/staa093\">10.1093/mnras/staa093</a>","ieee":"S. Santos <i>et al.</i>, “The evolution of rest-frame UV properties, Ly α EWs, and the SFR–stellar mass relation at z ∼ 2–6 for SC4K LAEs,” <i>Monthly Notices of the Royal Astronomical Society</i>, 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.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2020. <a href=\"https://doi.org/10.1093/mnras/staa093\">https://doi.org/10.1093/mnras/staa093</a>."},"year":"2020","abstract":[{"text":"We explore deep rest-frame UV to FIR data in the COSMOS field to measure the individual spectral energy distributions (SED) of the ∼4000 SC4K (Sobral et al.) Lyman α (Ly α) emitters (LAEs) at z ∼ 2–6. We find typical stellar masses of 109.3 ± 0.6 M⊙ and star formation rates (SFR) of SFRSED=4.4+10.5−2.4 M⊙ yr−1 and SFRLyα=5.9+6.3−2.6 M⊙ yr−1, combined with very blue UV slopes of β=−2.1+0.5−0.4⁠, but with significant variations within the population. MUV and β are correlated in a similar way to UV-selected sources, but LAEs are consistently bluer. This suggests that LAEs are the youngest and/or most dust-poor subset of the UV-selected population. We also study the Ly α rest-frame equivalent width (EW0) and find 45 ‘extreme’ LAEs with EW0 > 240 Å (3σ), implying a low number density of (7 ± 1) × 10−7 Mpc−3. Overall, we measure little to no evolution of the Ly α EW0 and scale length parameter (w0), which are consistently high (EW0=140+280−70 Å, w0=129+11−11 Å) from z ∼ 6 to z ∼ 2 and below. However, w0 is anticorrelated with MUV and stellar mass. Our results imply that sources selected as LAEs have a high Ly α escape fraction (fesc,Ly α) irrespective of cosmic time, but fesc,Ly α is still higher for UV-fainter and lower mass LAEs. The least massive LAEs (<109.5 M⊙) are typically located above the star formation ‘main sequence’ (MS), but the offset from the MS decreases towards z ∼ 6 and towards 1010 M⊙. Our results imply a lack of evolution in the properties of LAEs across time and reveals the increasing overlap in properties of LAEs and UV-continuum selected galaxies as typical star-forming galaxies at high redshift effectively become LAEs.","lang":"eng"}],"doi":"10.1093/mnras/staa093","arxiv":1,"day":"01","page":"141-160","quality_controlled":"1","article_type":"original","publisher":"Oxford University Press","author":[{"first_name":"S","last_name":"Santos","full_name":"Santos, S"},{"full_name":"Sobral, D","last_name":"Sobral","first_name":"D"},{"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":"Calhau","first_name":"J","full_name":"Calhau, J"},{"last_name":"da Cunha","first_name":"E","full_name":"da Cunha, E"},{"first_name":"B","last_name":"Ribeiro","full_name":"Ribeiro, B"},{"first_name":"A","last_name":"Paulino-Afonso","full_name":"Paulino-Afonso, A"},{"full_name":"Arrabal Haro, P","first_name":"P","last_name":"Arrabal Haro"},{"first_name":"J","last_name":"Butterworth","full_name":"Butterworth, J"}],"issue":"1","_id":"11533","scopus_import":"1","title":"The evolution of rest-frame UV properties, Ly α EWs, and the SFR–stellar mass relation at z ∼ 2–6 for SC4K LAEs","intvolume":"       493","publication_status":"published","date_created":"2022-07-07T12:05:23Z","article_processing_charge":"No"},{"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1911.04774"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","type":"conference","date_published":"2020-06-04T00:00:00Z","publication_identifier":{"issn":["1743-9213"],"eissn":["1743-9221"]},"oa":1,"keyword":["Astronomy and Astrophysics","Space and Planetary Science","galaxies: formation","galaxies: evolution","galaxies: high-redshift"],"language":[{"iso":"eng"}],"publication":"Proceedings of the International Astronomical Union","oa_version":"Preprint","month":"06","volume":15,"extern":"1","citation":{"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.” <i>Proceedings of the International Astronomical Union</i>, vol. 15, no. S352, Cambridge University Press, 2020, pp. 21–25, doi:<a href=\"https://doi.org/10.1017/s1743921319009451\">10.1017/s1743921319009451</a>.","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.","apa":"Matthee, J. J., &#38; Sobral, D. (2020). Unveiling the most luminous Lyman-α emitters in the epoch of reionisation. In <i>Proceedings of the International Astronomical Union</i> (Vol. 15, pp. 21–25). Cambridge University Press. <a href=\"https://doi.org/10.1017/s1743921319009451\">https://doi.org/10.1017/s1743921319009451</a>","ama":"Matthee JJ, Sobral D. Unveiling the most luminous Lyman-α emitters in the epoch of reionisation. In: <i>Proceedings of the International Astronomical Union</i>. Vol 15. Cambridge University Press; 2020:21-25. doi:<a href=\"https://doi.org/10.1017/s1743921319009451\">10.1017/s1743921319009451</a>","ieee":"J. J. Matthee and D. Sobral, “Unveiling the most luminous Lyman-α emitters in the epoch of reionisation,” in <i>Proceedings of the International Astronomical Union</i>, 2020, vol. 15, no. S352, pp. 21–25.","chicago":"Matthee, Jorryt J, and David Sobral. “Unveiling the Most Luminous Lyman-α Emitters in the Epoch of Reionisation.” In <i>Proceedings of the International Astronomical Union</i>, 15:21–25. Cambridge University Press, 2020. <a href=\"https://doi.org/10.1017/s1743921319009451\">https://doi.org/10.1017/s1743921319009451</a>."},"year":"2020","date_updated":"2022-08-19T08:41:12Z","external_id":{"arxiv":["1911.04774"]},"day":"04","doi":"10.1017/s1743921319009451","arxiv":1,"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."}],"quality_controlled":"1","page":"21-25","publisher":"Cambridge University Press","scopus_import":"1","_id":"11586","issue":"S352","author":[{"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":"David","last_name":"Sobral","full_name":"Sobral, David"}],"date_created":"2022-07-14T14:08:41Z","article_processing_charge":"No","publication_status":"published","intvolume":"        15","title":"Unveiling the most luminous Lyman-α emitters in the epoch of reionisation"},{"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1803.08923"}],"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"oa":1,"type":"journal_article","date_published":"2019-03-26T00:00:00Z","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift / galaxies: star formation / galaxies: statistics / galaxies: evolution / galaxies: formation / galaxies: ISM"],"language":[{"iso":"eng"}],"oa_version":"Published Version","article_number":"A157","month":"03","publication":"Astronomy & Astrophysics","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.","volume":623,"extern":"1","day":"26","doi":"10.1051/0004-6361/201833075","arxiv":1,"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"}],"citation":{"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 &#38; Astrophysics. 623, A157.","short":"D. Sobral, J.J. Matthee, Astronomy &#38; Astrophysics 623 (2019).","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.” <i>Astronomy &#38; Astrophysics</i>, vol. 623, A157, EDP Sciences, 2019, doi:<a href=\"https://doi.org/10.1051/0004-6361/201833075\">10.1051/0004-6361/201833075</a>.","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,” <i>Astronomy &#38; Astrophysics</i>, vol. 623. EDP Sciences, 2019.","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.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2019. <a href=\"https://doi.org/10.1051/0004-6361/201833075\">https://doi.org/10.1051/0004-6361/201833075</a>.","ama":"Sobral D, Matthee JJ. Predicting Lyα escape fractions with a simple observable: Lyα in emission as an empirically calibrated star formation rate indicator. <i>Astronomy &#38; Astrophysics</i>. 2019;623. doi:<a href=\"https://doi.org/10.1051/0004-6361/201833075\">10.1051/0004-6361/201833075</a>","apa":"Sobral, D., &#38; Matthee, J. J. (2019). Predicting Lyα escape fractions with a simple observable: Lyα in emission as an empirically calibrated star formation rate indicator. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201833075\">https://doi.org/10.1051/0004-6361/201833075</a>"},"year":"2019","date_updated":"2022-07-19T09:37:20Z","external_id":{"arxiv":["1803.08923"]},"publisher":"EDP Sciences","article_type":"original","quality_controlled":"1","article_processing_charge":"No","date_created":"2022-07-06T11:08:16Z","publication_status":"published","intvolume":"       623","title":"Predicting Lyα escape fractions with a simple observable: Lyα in emission as an empirically calibrated star formation rate indicator","scopus_import":"1","_id":"11507","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"}]},{"arxiv":1,"doi":"10.1093/mnras/stz030","day":"01","abstract":[{"lang":"eng","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."}],"date_updated":"2022-08-19T06:42:43Z","year":"2019","citation":{"ama":"Matthee JJ, Schaye J. The origin of scatter in the star formation rate–stellar mass relation. <i>Monthly Notices of the Royal Astronomical Society</i>. 2019;484(1):915-932. doi:<a href=\"https://doi.org/10.1093/mnras/stz030\">10.1093/mnras/stz030</a>","apa":"Matthee, J. J., &#38; Schaye, J. (2019). The origin of scatter in the star formation rate–stellar mass relation. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stz030\">https://doi.org/10.1093/mnras/stz030</a>","ieee":"J. J. Matthee and J. Schaye, “The origin of scatter in the star formation rate–stellar mass relation,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 484, no. 1. Oxford University Press, pp. 915–932, 2019.","chicago":"Matthee, Jorryt J, and Joop Schaye. “The Origin of Scatter in the Star Formation Rate–Stellar Mass Relation.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2019. <a href=\"https://doi.org/10.1093/mnras/stz030\">https://doi.org/10.1093/mnras/stz030</a>.","mla":"Matthee, Jorryt J., and Joop Schaye. “The Origin of Scatter in the Star Formation Rate–Stellar Mass Relation.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 484, no. 1, Oxford University Press, 2019, pp. 915–32, doi:<a href=\"https://doi.org/10.1093/mnras/stz030\">10.1093/mnras/stz030</a>.","short":"J.J. Matthee, J. Schaye, Monthly Notices of the Royal Astronomical Society 484 (2019) 915–932.","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."},"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_status":"published","article_processing_charge":"No","date_created":"2022-07-08T07:48:31Z","title":"The origin of scatter in the star formation rate–stellar mass relation","intvolume":"       484","_id":"11540","scopus_import":"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"},{"first_name":"Joop","last_name":"Schaye","full_name":"Schaye, Joop"}],"issue":"1","publisher":"Oxford University Press","article_type":"original","page":"915-932","quality_controlled":"1","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"oa":1,"date_published":"2019-03-01T00:00:00Z","type":"journal_article","main_file_link":[{"url":"https://arxiv.org/abs/1805.05956","open_access":"1"}],"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa_version":"Preprint","month":"03","publication":"Monthly Notices of the Royal Astronomical Society","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics : galaxies: evolution","galaxies: formation","galaxies: star formation","cosmology: theory"]},{"oa":1,"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"type":"journal_article","date_published":"2018-11-19T00:00:00Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","main_file_link":[{"url":"https://arxiv.org/abs/1805.11621","open_access":"1"}],"article_number":"A136","month":"11","oa_version":"Published Version","publication":"Astronomy & Astrophysics","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift / galaxies: formation / dark ages / reionization / first stars / techniques: spectroscopic / intergalactic medium"],"language":[{"iso":"eng"}],"abstract":[{"text":"Distant luminous Lyman-α emitters (LAEs) are excellent targets for spectroscopic observations of galaxies in the epoch of reionisation (EoR). We present deep high-resolution (R = 5000) VLT/X-shooter observations, along with an extensive collection of photometric data of COLA1, a proposed double peaked LAE at z = 6.6. We rule out the possibility that COLA1’s emission line is an [OII] doublet at z = 1.475 on the basis of i) the asymmetric red line-profile and flux ratio of the peaks (blue/red=0.31 ± 0.03) and ii) an unphysical [OII]/Hα ratio ([OII]/Hα >  22). We show that COLA1’s observed B-band flux is explained by a faint extended foreground LAE, for which we detect Lyα and [OIII] at z = 2.142. We thus conclude that COLA1 is a real double-peaked LAE at z = 6.593, the first discovered at z >  6. COLA1 is UV luminous (M1500 = −21.6 ± 0.3), has a high equivalent width (EW0,Lyα = 120−40+50 Å) and very compact Lyα emission (r50,Lyα = 0.33−0.04+0.07 kpc). Relatively weak inferred Hβ+[OIII] line-emission from Spitzer/IRAC indicates an extremely low metallicity of Z <  1/20 Z⊙ or reduced strength of nebular lines due to high escape of ionising photons. The small Lyα peak separation of 220 ± 20 km s−1 implies a low HI column density and an ionising photon escape fraction of ≈15 − 30%, providing the first direct evidence that such galaxies contribute actively to the reionisation of the Universe at z >  6. Based on simple estimates, we find that COLA1 could have provided just enough photons to reionise its own ≈0.3 pMpc (2.3 cMpc) bubble, allowing the blue Lyα line to be observed. However, we also discuss alternative scenarios explaining the detected double peaked nature of COLA1. Our results show that future high-resolution observations of statistical samples of double peaked LAEs at z >  5 are a promising probe of the occurrence of ionised regions around galaxies in the EoR.","lang":"eng"}],"day":"19","arxiv":1,"doi":"10.1051/0004-6361/201833528","external_id":{"arxiv":["1805.11621"]},"year":"2018","citation":{"ista":"Matthee JJ, Sobral D, Gronke M, Paulino-Afonso A, Stefanon M, Röttgering H. 2018. Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly contributing to the reionisation of the universe. Astronomy &#38; Astrophysics. 619, A136.","short":"J.J. Matthee, D. Sobral, M. Gronke, A. Paulino-Afonso, M. Stefanon, H. Röttgering, Astronomy &#38; Astrophysics 619 (2018).","mla":"Matthee, Jorryt J., et al. “Confirmation of Double Peaked Lyα Emission at z = 6.593: Witnessing a Galaxy Directly Contributing to the Reionisation of the Universe.” <i>Astronomy &#38; Astrophysics</i>, vol. 619, A136, EDP Sciences, 2018, doi:<a href=\"https://doi.org/10.1051/0004-6361/201833528\">10.1051/0004-6361/201833528</a>.","ieee":"J. J. Matthee, D. Sobral, M. Gronke, A. Paulino-Afonso, M. Stefanon, and H. Röttgering, “Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly contributing to the reionisation of the universe,” <i>Astronomy &#38; Astrophysics</i>, vol. 619. EDP Sciences, 2018.","chicago":"Matthee, Jorryt J, David Sobral, Max Gronke, Ana Paulino-Afonso, Mauro Stefanon, and Huub Röttgering. “Confirmation of Double Peaked Lyα Emission at z = 6.593: Witnessing a Galaxy Directly Contributing to the Reionisation of the Universe.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2018. <a href=\"https://doi.org/10.1051/0004-6361/201833528\">https://doi.org/10.1051/0004-6361/201833528</a>.","ama":"Matthee JJ, Sobral D, Gronke M, Paulino-Afonso A, Stefanon M, Röttgering H. Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly contributing to the reionisation of the universe. <i>Astronomy &#38; Astrophysics</i>. 2018;619. doi:<a href=\"https://doi.org/10.1051/0004-6361/201833528\">10.1051/0004-6361/201833528</a>","apa":"Matthee, J. J., Sobral, D., Gronke, M., Paulino-Afonso, A., Stefanon, M., &#38; Röttgering, H. (2018). Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly contributing to the reionisation of the universe. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201833528\">https://doi.org/10.1051/0004-6361/201833528</a>"},"date_updated":"2022-07-19T09:32:08Z","extern":"1","volume":619,"acknowledgement":"JM acknowledges the award of a Huygens PhD fellowship from Leiden University. MG acknowledges support from NASA grant NNX17AK58G. APA, PhD::SPACE fellow, acknowledges support from the FCT through the fellowship PD/BD/52706/2014. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 294.A-5018, 098.A-0819, 099.A-0254 and 0100.A-0213. We are grateful for the excellent data-sets from the COSMOS and UltraVISTA survey teams. This research was supported by the Munich Institute for Astro- and Particle Physics (MIAPP) of the DFG cluster of excellence “Origin and Structure of the Universe”. We thank the referee for their comments that improved the paper. We also thank Christoph Behrens, Len Cowie, Koki Kakiichi, Peter Laursen, Charlotte Mason, Eros Vanzella, Lewis Weinberger and Johannes Zabl for discussions. We have benefited from the public available programming language Python, including the numpy, matplotlib, scipy and astropy packages (Hunter 2007; Astropy Collaboration 2013), the astronomical imaging tools Swarp (Bertin 2010) and ds9 and the Topcat analysis tool (Taylor 2013).","intvolume":"       619","title":"Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly contributing to the reionisation of the universe","date_created":"2022-07-06T11:14:23Z","article_processing_charge":"No","publication_status":"published","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X"},{"first_name":"David","last_name":"Sobral","full_name":"Sobral, David"},{"full_name":"Gronke, Max","last_name":"Gronke","first_name":"Max"},{"first_name":"Ana","last_name":"Paulino-Afonso","full_name":"Paulino-Afonso, Ana"},{"full_name":"Stefanon, Mauro","last_name":"Stefanon","first_name":"Mauro"},{"first_name":"Huub","last_name":"Röttgering","full_name":"Röttgering, Huub"}],"scopus_import":"1","_id":"11508","article_type":"original","publisher":"EDP Sciences","quality_controlled":"1"},{"doi":"10.1093/mnras/sty1088","arxiv":1,"day":"01","abstract":[{"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.","lang":"eng"}],"date_updated":"2022-08-19T06:58:06Z","year":"2018","citation":{"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.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2018. <a href=\"https://doi.org/10.1093/mnras/sty1088\">https://doi.org/10.1093/mnras/sty1088</a>.","ieee":"S. Carniani <i>et al.</i>, “Kiloparsec-scale gaseous clumps and star formation at z = 5–7,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 478, no. 1. Oxford University Press, pp. 1170–1184, 2018.","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. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/sty1088\">https://doi.org/10.1093/mnras/sty1088</a>","ama":"Carniani S, Maiolino R, Amorin R, et al. Kiloparsec-scale gaseous clumps and star formation at z = 5–7. <i>Monthly Notices of the Royal Astronomical Society</i>. 2018;478(1):1170-1184. doi:<a href=\"https://doi.org/10.1093/mnras/sty1088\">10.1093/mnras/sty1088</a>","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.","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.","mla":"Carniani, S., et al. “Kiloparsec-Scale Gaseous Clumps and Star Formation at z = 5–7.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 478, no. 1, Oxford University Press, 2018, pp. 1170–84, doi:<a href=\"https://doi.org/10.1093/mnras/sty1088\">10.1093/mnras/sty1088</a>."},"external_id":{"arxiv":["1712.03985"]},"volume":478,"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.","extern":"1","publication_status":"published","date_created":"2022-07-11T08:05:42Z","article_processing_charge":"No","title":"Kiloparsec-scale gaseous clumps and star formation at z = 5–7","intvolume":"       478","_id":"11555","scopus_import":"1","author":[{"last_name":"Carniani","first_name":"S","full_name":"Carniani, S"},{"full_name":"Maiolino, R","first_name":"R","last_name":"Maiolino"},{"last_name":"Amorin","first_name":"R","full_name":"Amorin, R"},{"first_name":"L","last_name":"Pentericci","full_name":"Pentericci, L"},{"full_name":"Pallottini, A","first_name":"A","last_name":"Pallottini"},{"full_name":"Ferrara, A","first_name":"A","last_name":"Ferrara"},{"full_name":"Willott, C J","first_name":"C J","last_name":"Willott"},{"full_name":"Smit, R","last_name":"Smit","first_name":"R"},{"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":"Sobral","first_name":"D","full_name":"Sobral, D"},{"first_name":"P","last_name":"Santini","full_name":"Santini, P"},{"last_name":"Castellano","first_name":"M","full_name":"Castellano, M"},{"full_name":"De Barros, S","last_name":"De Barros","first_name":"S"},{"full_name":"Fontana, A","first_name":"A","last_name":"Fontana"},{"full_name":"Grazian, A","first_name":"A","last_name":"Grazian"},{"first_name":"L","last_name":"Guaita","full_name":"Guaita, L"}],"issue":"1","publisher":"Oxford University Press","article_type":"original","page":"1170-1184","quality_controlled":"1","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"oa":1,"date_published":"2018-07-01T00:00:00Z","type":"journal_article","main_file_link":[{"url":"https://arxiv.org/abs/1712.03985","open_access":"1"}],"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa_version":"Preprint","month":"07","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"]},{"type":"journal_article","date_published":"2018-06-01T00:00:00Z","oa":1,"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1712.04451"}],"publication":"Monthly Notices of the Royal Astronomical Society","month":"06","oa_version":"Preprint","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: formation","galaxies: high-redshift","galaxies: luminosity function","mass function","galaxies: statistics"],"language":[{"iso":"eng"}],"external_id":{"arxiv":["1712.04451"]},"citation":{"ista":"Sobral D, Santos S, Matthee JJ, Paulino-Afonso A, Ribeiro B, Calhau J, Khostovan AA. 2018. Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6. Monthly Notices of the Royal Astronomical Society. 476(4), 4725–4752.","mla":"Sobral, David, et al. “Slicing COSMOS with SC4K: The Evolution of Typical Ly α Emitters and the Ly α Escape Fraction from z ∼ 2 to 6.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 476, no. 4, Oxford University Press, 2018, pp. 4725–52, doi:<a href=\"https://doi.org/10.1093/mnras/sty378\">10.1093/mnras/sty378</a>.","short":"D. Sobral, S. Santos, J.J. Matthee, A. Paulino-Afonso, B. Ribeiro, J. Calhau, A.A. Khostovan, Monthly Notices of the Royal Astronomical Society 476 (2018) 4725–4752.","chicago":"Sobral, David, Sérgio Santos, Jorryt J Matthee, Ana Paulino-Afonso, Bruno Ribeiro, João Calhau, and Ali A Khostovan. “Slicing COSMOS with SC4K: The Evolution of Typical Ly α Emitters and the Ly α Escape Fraction from z ∼ 2 to 6.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2018. <a href=\"https://doi.org/10.1093/mnras/sty378\">https://doi.org/10.1093/mnras/sty378</a>.","ieee":"D. Sobral <i>et al.</i>, “Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 476, no. 4. Oxford University Press, pp. 4725–4752, 2018.","ama":"Sobral D, Santos S, Matthee JJ, et al. Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6. <i>Monthly Notices of the Royal Astronomical Society</i>. 2018;476(4):4725-4752. doi:<a href=\"https://doi.org/10.1093/mnras/sty378\">10.1093/mnras/sty378</a>","apa":"Sobral, D., Santos, S., Matthee, J. J., Paulino-Afonso, A., Ribeiro, B., Calhau, J., &#38; Khostovan, A. A. (2018). Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/sty378\">https://doi.org/10.1093/mnras/sty378</a>"},"year":"2018","date_updated":"2022-08-19T07:04:45Z","abstract":[{"text":"We present and explore deep narrow- and medium-band data obtained with the Subaru and the Isaac Newton Telescopes in the ∼2 deg2 COSMOS field. We use these data as an extremely wide, low-resolution (R ∼ 20–80) Integral Field Unit survey to slice through the COSMOS field and obtain a large sample of ∼4000 Ly α emitters (LAEs) from z ∼ 2 to 6 in 16 redshift slices (SC4K). We present new Ly α luminosity functions (LFs) covering a comoving volume of ∼108 Mpc3. SC4K extensively complements ultradeep surveys, jointly covering over 4 dex in Ly α luminosity and revealing a global (2.5 < z < 6) synergy LF with α=−1.93+0.12−0.12⁠, log10Φ∗Lyα=−3.45+0.22−0.29 Mpc−3, and log10L∗Lyα=42.93+0.15−0.11 erg s−1. The Schechter component of the Ly α LF reveals a factor ∼5 rise in L∗Lyα and a ∼7 × decline in Φ∗Lyα from z ∼ 2 to 6. The data reveal an extra power-law (or Schechter) component above LLy α ≈ 1043.3 erg s−1 at z ∼ 2.2–3.5 and we show that it is partially driven by X-ray and radio active galactic nucleus (AGN), as their Ly α LF resembles the excess. The power-law component vanishes and/or is below our detection limits above z > 3.5, likely linked with the evolution of the AGN population. The Ly α luminosity density rises by a factor ∼2 from z ∼ 2 to 3 but is then found to be roughly constant (⁠1.1+0.2−0.2×1040 erg s−1 Mpc−3) to z ∼ 6, despite the ∼0.7 dex drop in ultraviolet (UV) luminosity density. The Ly α/UV luminosity density ratio rises from 4 ± 1 per cent to 30 ± 6 per cent from z ∼ 2.2 to 6. Our results imply a rise of a factor of ≈2 in the global ionization efficiency (ξion) and a factor ≈4 ± 1 in the Ly α escape fraction from z ∼ 2 to 6, hinting for evolution in both the typical burstiness/stellar populations and even more so in the typical interstellar medium conditions allowing Ly α photons to escape.","lang":"eng"}],"day":"01","arxiv":1,"doi":"10.1093/mnras/sty378","extern":"1","acknowledgement":"We thank the anonymous referee for their constructive comments that helped us improve the manuscript. DS acknowledges the hospitality of the IAC and a Severo Ochoa visiting grant. SS and JC acknowledge studentships from the Lancaster University. JM acknowledges a Huygens PhD fellowship from Leiden University. APA acknowledges financial support from the Science and Technology Foundation (FCT, Portugal) through research grants UID/FIS/04434/2013 and fellowship PD/BD/52706/2014. The authors thank Alyssa Drake, Kimihiko Nakajima, Yuichi Harikane, Max Gronke, Irene Shivaei, Helmut Dannerbauer, Huub Rottgering, ¨ Marius Eide, and Masami Ouchi for many engaging and stimulating discussions. We also thank Sara Perez, Alex Bennett, and Tom Rose for their involvement in the early stages of this project. Based on data products from observations made with European Southern Observatory (ESO) Telescopes at the La Silla Paranal Observatory under ESO programme IDs 294.A-5018, 097.A 0943,\r\n098.A-0819, 099.A-0254, and 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. Based on observations using the WFC on the 2.5 m INT, as part of programmes 2013AN002, 2013BN008, 2014AC88, 2014AN002, 2014BN006, 2014BC118, and 2016AN001. The INT is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. 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 (CFHTLS), a collaborative project of NRC and CNRS.\r\nWe are grateful to the CFHTLS, COSMOS-UltraVISTA, and COSMOS survey teams. We are also unmeasurably thankful to the pioneering and continuous work from previous Ly α surveys’ teams. Without these previous Ly α and the wider reach legacy surveys, this research would have been impossible. We also thank the VUDS team for making available spectroscopic redshifts from data obtained with VIMOS at the European Southern Observatory Very Large Telescope, Paranal, Chile, under Large Programme 185.A-0791. Finally, the authors acknowledge the unique value of the publicly available programming language PYTHON, including the NUMPY and 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 2005). We publicly release a catalogue with all LAEs used in this paper (SC4K), so it can be freely explored by the community (see five example entries in Table A1).","volume":476,"issue":"4","author":[{"first_name":"David","last_name":"Sobral","full_name":"Sobral, David"},{"full_name":"Santos, Sérgio","first_name":"Sérgio","last_name":"Santos"},{"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":"Paulino-Afonso, Ana","last_name":"Paulino-Afonso","first_name":"Ana"},{"full_name":"Ribeiro, Bruno","last_name":"Ribeiro","first_name":"Bruno"},{"full_name":"Calhau, João","first_name":"João","last_name":"Calhau"},{"full_name":"Khostovan, Ali A","first_name":"Ali A","last_name":"Khostovan"}],"scopus_import":"1","_id":"11558","intvolume":"       476","title":"Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6","article_processing_charge":"No","date_created":"2022-07-12T10:41:08Z","publication_status":"published","quality_controlled":"1","page":"4725-4752","article_type":"original","publisher":"Oxford University Press"},{"publication":"Monthly Notices of the Royal Astronomical Society: Letters","month":"09","oa_version":"Preprint","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: abundances","galaxies: evolution","galaxies: formation","galaxies: star formation"],"language":[{"iso":"eng"}],"type":"journal_article","date_published":"2018-09-01T00:00:00Z","oa":1,"publication_identifier":{"issn":["1745-3925"],"eissn":["1745-3933"]},"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1802.06786"}],"issue":"1","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":"Schaye, Joop","last_name":"Schaye","first_name":"Joop"}],"scopus_import":"1","_id":"11584","intvolume":"       479","title":"Star-forming galaxies are predicted to lie on a fundamental plane of mass, star formation rate, and α-enhancement","date_created":"2022-07-14T12:49:47Z","article_processing_charge":"No","publication_status":"published","quality_controlled":"1","page":"L34 - L39","article_type":"original","publisher":"Oxford University Press","external_id":{"arxiv":["1802.06786"]},"year":"2018","citation":{"ista":"Matthee JJ, Schaye J. 2018. Star-forming galaxies are predicted to lie on a fundamental plane of mass, star formation rate, and α-enhancement. Monthly Notices of the Royal Astronomical Society: Letters. 479(1), L34–L39.","mla":"Matthee, Jorryt J., and Joop Schaye. “Star-Forming Galaxies Are Predicted to Lie on a Fundamental Plane of Mass, Star Formation Rate, and α-Enhancement.” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>, vol. 479, no. 1, Oxford University Press, 2018, pp. L34–39, doi:<a href=\"https://doi.org/10.1093/mnrasl/sly093\">10.1093/mnrasl/sly093</a>.","short":"J.J. Matthee, J. Schaye, Monthly Notices of the Royal Astronomical Society: Letters 479 (2018) L34–L39.","ieee":"J. J. Matthee and J. Schaye, “Star-forming galaxies are predicted to lie on a fundamental plane of mass, star formation rate, and α-enhancement,” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>, vol. 479, no. 1. Oxford University Press, pp. L34–L39, 2018.","chicago":"Matthee, Jorryt J, and Joop Schaye. “Star-Forming Galaxies Are Predicted to Lie on a Fundamental Plane of Mass, Star Formation Rate, and α-Enhancement.” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. Oxford University Press, 2018. <a href=\"https://doi.org/10.1093/mnrasl/sly093\">https://doi.org/10.1093/mnrasl/sly093</a>.","ama":"Matthee JJ, Schaye J. Star-forming galaxies are predicted to lie on a fundamental plane of mass, star formation rate, and α-enhancement. <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. 2018;479(1):L34-L39. doi:<a href=\"https://doi.org/10.1093/mnrasl/sly093\">10.1093/mnrasl/sly093</a>","apa":"Matthee, J. J., &#38; Schaye, J. (2018). Star-forming galaxies are predicted to lie on a fundamental plane of mass, star formation rate, and α-enhancement. <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnrasl/sly093\">https://doi.org/10.1093/mnrasl/sly093</a>"},"date_updated":"2022-08-19T08:35:45Z","abstract":[{"lang":"eng","text":"Observations show that star-forming galaxies reside on a tight 3D plane between mass, gas-phase metallicity, and star formation rate (SFR), which can be explained by the interplay between metal-poor gas inflows, SFR and outflows. However, different metals are released on different time-scales, which may affect the slope of this relation. Here, we use central, star-forming galaxies with Mstar = 109.0–10.5 M⊙ from the EAGLE hydrodynamical simulation to examine 3D relations between mass, SFR, and chemical enrichment using absolute and relative C, N, O, and Fe abundances. We show that the scatter is smaller when gas-phase α-enhancement is used rather than metallicity. A similar plane also exists for stellar α-enhancement, implying that present-day specific SFRs are correlated with long time-scale star formation histories. Between z = 0 and 1, the α-enhancement plane is even more insensitive to redshift than the plane using metallicity. However, it evolves at z > 1 due to lagging iron yields. At fixed mass, galaxies with higher SFRs have star formation histories shifted towards late times, are more α-enhanced, and this α-enhancement increases with redshift as observed. These findings suggest that relations between physical properties inferred from observations may be affected by systematic variations in α-enhancements."}],"day":"01","doi":"10.1093/mnrasl/sly093","arxiv":1,"extern":"1","volume":479,"acknowledgement":"We thank the anonymous referee for their constructive comments. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. We thank Jarle Brinchmann, Rob Crain and David Sobral for discussions. We acknowledge the use of the TOPCAT software (Taylor 2013) for assisting in rapid exploration of multidimensional data sets and the use of PYTHON and its NUMPY, MATPLOTLIB, and PANDAS packages."},{"article_number":"145","month":"12","oa_version":"Preprint","publication":"The Astrophysical Journal","keyword":["Space and Planetary Science","Astronomy and Astrophysics","dark ages","reionization","first stars – galaxies: formation – galaxies: high-redshift – galaxies: ISM – galaxies: kinematics and dynamics"],"language":[{"iso":"eng"}],"oa":1,"publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"type":"journal_article","date_published":"2017-12-21T00:00:00Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","main_file_link":[{"url":"https://arxiv.org/abs/1709.06569","open_access":"1"}],"intvolume":"       851","title":"ALMA reveals metals yet no dust within multiple components in CR7","date_created":"2022-07-07T08:48:04Z","article_processing_charge":"No","publication_status":"published","issue":"2","author":[{"full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"first_name":"D.","last_name":"Sobral","full_name":"Sobral, D."},{"full_name":"Boone, F.","last_name":"Boone","first_name":"F."},{"full_name":"Röttgering, H.","last_name":"Röttgering","first_name":"H."},{"full_name":"Schaerer, D.","last_name":"Schaerer","first_name":"D."},{"last_name":"Girard","first_name":"M.","full_name":"Girard, M."},{"full_name":"Pallottini, A.","first_name":"A.","last_name":"Pallottini"},{"full_name":"Vallini, L.","last_name":"Vallini","first_name":"L."},{"last_name":"Ferrara","first_name":"A.","full_name":"Ferrara, A."},{"full_name":"Darvish, B.","last_name":"Darvish","first_name":"B."},{"last_name":"Mobasher","first_name":"B.","full_name":"Mobasher, B."}],"scopus_import":"1","_id":"11518","article_type":"original","publisher":"IOP Publishing","quality_controlled":"1","abstract":[{"text":"We present spectroscopic follow-up observations of CR7 with ALMA, targeted at constraining the infrared (IR) continuum and [C II]158 mm line-emission at high spatial resolution matched to the HST/WFC3 imaging. CR7 is a luminous Lyα emitting galaxy at z = 6.6 that consists of three separated UV-continuum components. Our observations reveal several well-separated components of [C II] emission. The two most luminous components in [C II] coincide with the brightest UV components (A and B), blueshifted by »150 km s−1 with respect to the\r\npeak of Lyα emission. Other [C II] components are observed close to UV clumps B and C and are blueshifted by »300 and ≈80 km s−1 with respect to the systemic redshift. We do not detect FIR continuum emission due to dust with a 3σ limiting luminosity LIR T L d 35 K 3.1 10 = <´ 10 ( ) . This allows us to mitigate uncertainties in the dust-corrected SFR and derive SFRs for the three UV clumps A, B, and C of 28, 5, and 7 M yr−1. All clumps have [C II] luminosities consistent within the scatter observed in the local relation between SFR and L[ ] C II , implying that strong Lyα emission does not necessarily anti-correlate with [C II] luminosity. Combining\r\nour measurements with the literature, we show that galaxies with blue UV slopes have weaker [C II] emission at fixed SFR, potentially due to their lower metallicities and/or higher photoionization. Comparison with hydrodynamical simulations suggests that CR7ʼs clumps have metallicities of 0.1 Z Z 0.2 < < . The observed ISM structure of CR7 indicates that we are likely witnessing the build up of a central galaxy in the early universe through complex accretion of satellites.","lang":"eng"}],"day":"21","arxiv":1,"doi":"10.3847/1538-4357/aa9931","external_id":{"arxiv":["1709.06569"]},"year":"2017","citation":{"ama":"Matthee JJ, Sobral D, Boone F, et al. ALMA reveals metals yet no dust within multiple components in CR7. <i>The Astrophysical Journal</i>. 2017;851(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/aa9931\">10.3847/1538-4357/aa9931</a>","apa":"Matthee, J. J., Sobral, D., Boone, F., Röttgering, H., Schaerer, D., Girard, M., … Mobasher, B. (2017). ALMA reveals metals yet no dust within multiple components in CR7. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/aa9931\">https://doi.org/10.3847/1538-4357/aa9931</a>","chicago":"Matthee, Jorryt J, D. Sobral, F. Boone, H. Röttgering, D. Schaerer, M. Girard, A. Pallottini, et al. “ALMA Reveals Metals yet No Dust within Multiple Components in CR7.” <i>The Astrophysical Journal</i>. IOP Publishing, 2017. <a href=\"https://doi.org/10.3847/1538-4357/aa9931\">https://doi.org/10.3847/1538-4357/aa9931</a>.","ieee":"J. J. Matthee <i>et al.</i>, “ALMA reveals metals yet no dust within multiple components in CR7,” <i>The Astrophysical Journal</i>, vol. 851, no. 2. IOP Publishing, 2017.","short":"J.J. Matthee, D. Sobral, F. Boone, H. Röttgering, D. Schaerer, M. Girard, A. Pallottini, L. Vallini, A. Ferrara, B. Darvish, B. Mobasher, The Astrophysical Journal 851 (2017).","mla":"Matthee, Jorryt J., et al. “ALMA Reveals Metals yet No Dust within Multiple Components in CR7.” <i>The Astrophysical Journal</i>, vol. 851, no. 2, 145, IOP Publishing, 2017, doi:<a href=\"https://doi.org/10.3847/1538-4357/aa9931\">10.3847/1538-4357/aa9931</a>.","ista":"Matthee JJ, Sobral D, Boone F, Röttgering H, Schaerer D, Girard M, Pallottini A, Vallini L, Ferrara A, Darvish B, Mobasher B. 2017. ALMA reveals metals yet no dust within multiple components in CR7. The Astrophysical Journal. 851(2), 145."},"date_updated":"2022-08-18T10:23:35Z","extern":"1","volume":851,"acknowledgement":"We thank the referee for their constructive comments, which have helped improve the quality and clarity of this work. We thank Raffaella Schneider for comments on an earlier version of this paper. We thank Leindert Boogaard, Steven Bos, Rychard Bouwens, and Renske Smit for discussions. J.M. acknowledges the support of a Huygens PhD fellowship from Leiden University. D.S. acknowledges financial support from the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship and from Lancaster University through an Early Career Internal Grant A100679. A.F. acknowledges support from the ERC Advanced Grant INTERSTELLAR H2020/740120. B.D. acknowledges financial support from NASA through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 294.A-5018. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2015.1.00122.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ."},{"issue":"2","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J"},{"full_name":"Schaye, Joop","first_name":"Joop","last_name":"Schaye"},{"last_name":"Crain","first_name":"Robert A.","full_name":"Crain, Robert A."},{"full_name":"Schaller, Matthieu","first_name":"Matthieu","last_name":"Schaller"},{"full_name":"Bower, Richard","last_name":"Bower","first_name":"Richard"},{"full_name":"Theuns, Tom","last_name":"Theuns","first_name":"Tom"}],"scopus_import":"1","_id":"11565","intvolume":"       465","title":"The origin of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE simulation","article_processing_charge":"No","date_created":"2022-07-12T12:25:08Z","publication_status":"published","quality_controlled":"1","page":"2381-2396","article_type":"original","publisher":"Oxford University Press","external_id":{"arxiv":["1608.08218"]},"year":"2017","citation":{"ista":"Matthee JJ, Schaye J, Crain RA, Schaller M, Bower R, Theuns T. 2017. The origin of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE simulation. Monthly Notices of the Royal Astronomical Society. 465(2), 2381–2396.","mla":"Matthee, Jorryt J., et al. “The Origin of Scatter in the Stellar Mass–Halo Mass Relation of Central Galaxies in the EAGLE Simulation.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 465, no. 2, Oxford University Press, 2017, pp. 2381–96, doi:<a href=\"https://doi.org/10.1093/mnras/stw2884\">10.1093/mnras/stw2884</a>.","short":"J.J. Matthee, J. Schaye, R.A. Crain, M. Schaller, R. Bower, T. Theuns, Monthly Notices of the Royal Astronomical Society 465 (2017) 2381–2396.","ieee":"J. J. Matthee, J. Schaye, R. A. Crain, M. Schaller, R. Bower, and T. Theuns, “The origin of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE simulation,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 465, no. 2. Oxford University Press, pp. 2381–2396, 2017.","chicago":"Matthee, Jorryt J, Joop Schaye, Robert A. Crain, Matthieu Schaller, Richard Bower, and Tom Theuns. “The Origin of Scatter in the Stellar Mass–Halo Mass Relation of Central Galaxies in the EAGLE Simulation.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stw2884\">https://doi.org/10.1093/mnras/stw2884</a>.","ama":"Matthee JJ, Schaye J, Crain RA, Schaller M, Bower R, Theuns T. The origin of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE simulation. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;465(2):2381-2396. doi:<a href=\"https://doi.org/10.1093/mnras/stw2884\">10.1093/mnras/stw2884</a>","apa":"Matthee, J. J., Schaye, J., Crain, R. A., Schaller, M., Bower, R., &#38; Theuns, T. (2017). The origin of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE simulation. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stw2884\">https://doi.org/10.1093/mnras/stw2884</a>"},"date_updated":"2022-08-19T07:56:07Z","abstract":[{"text":"We use the hydrodynamical EAGLE simulation to study the magnitude and origin of the scatter in the stellar mass–halo mass relation for central galaxies. We separate cause and effect by correlating stellar masses in the baryonic simulation with halo properties in a matched dark matter only (DMO) simulation. The scatter in stellar mass increases with redshift and decreases with halo mass. At z = 0.1, it declines from 0.25 dex at M200, DMO ≈ 1011 M⊙ to 0.12 dex at M200, DMO ≈ 1013 M⊙, but the trend is weak above 1012 M⊙. For M200, DMO < 1012.5 M⊙ up to 0.04 dex of the scatter is due to scatter in the halo concentration. At fixed halo mass, a larger stellar mass corresponds to a more concentrated halo. This is likely because higher concentrations imply earlier formation times and hence more time for accretion and star formation, and/or because feedback is less efficient in haloes with higher binding energies. The maximum circular velocity, Vmax, DMO, and binding energy are therefore more fundamental properties than halo mass, meaning that they are more accurate predictors of stellar mass, and we provide fitting formulae for their relations with stellar mass. However, concentration alone cannot explain the total scatter in the Mstar−M200,DMO relation, and it does not explain the scatter in Mstar–Vmax, DMO. Halo spin, sphericity, triaxiality, substructure and environment are also not responsible for the remaining scatter, which thus could be due to more complex halo properties or non-linear/stochastic baryonic effects.","lang":"eng"}],"day":"01","arxiv":1,"doi":"10.1093/mnras/stw2884","extern":"1","volume":465,"acknowledgement":"We thank the anonymous referee for their comments. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. JM thanks David Sobral for useful discussions and help with fitting routines and Jonas Chavez Montero and Ying Zu for providing data. We thank PRACE for the access to the Curie facility in France. We have used the DiRAC system which is a part of National E-Infrastructure at Durham University, operated by the Institute for Computational Cosmology on behalf of the STFC DiRAC HPC Facility (www.dirac.ac.uk); the equipment was funded by BIS National E-infrastructure capital grant ST/K00042X/1, STFC capital grant ST/H008519/1, STFC DiRAC Operations grant ST/K003267/1 and Durham University. The study was sponsored by the Dutch National Computing Facilities Foundation (NCF) for the use of supercomputer facilities, with financial support from the Netherlands Organisation for Scientific Research (NWO), through VICI grant 639.043.409, and the European Research Council under the European Union’s Seventh Framework Programme (FP7/2007-2013)/ERC Grant agreement 278594- GasAroundGalaxies, and from the Belgian Science Policy Office ([AP P7/08 CHARM]). We have benefited greatly from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY, H5PY and RPY2 packages, and the TOPCAT analysis program (Taylor 2005).","publication":"Monthly Notices of the Royal Astronomical Society","month":"02","oa_version":"Preprint","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: formation","galaxies: haloes","cosmology: theory"],"language":[{"iso":"eng"}],"type":"journal_article","date_published":"2017-02-01T00:00:00Z","oa":1,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1608.08218"}]},{"extern":"1","volume":459,"acknowledgement":"We thank Luca Cortese, Matt Bothwell, Paola Santini and Tim Davis for providing observational data sets, and Aaron Robotham, Luca Cortese and Barbara Catinella for useful discussions. CdPL is funded by a Discovery Early Career Researcher Award (DE150100618). CdPL also thanks the MERAC Foundation for a Postdoctoral Research Award. This work used the DiRAC Data Centric system at Durham University, operated by the Institute for Computational Cosmology on behalf of the STFC DiRAC HPC Facility (www.dirac.ac.uk). This equipment was funded by BIS National E-infrastructure capital grant ST/K00042X/1, STFC capital grant ST/H008519/1, and STFC DiRAC Operations grant ST/K003267/1 and Durham University. DiRAC is part of the National E-Infrastructure. Support was also received via the Interuniversity Attraction Poles Programme initiated by the Belgian Science Policy Office ([AP P7/08 CHARM]), the National Science Foundation under grant no. NSF PHY11-25915, and the UK Science and Technology Facilities Council (grant numbers ST/F001166/1 and ST/I000976/1) via rolling and consolidating grants awarded to the ICC. The research was supported in part by the European Research Council under the European Union‘s Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement 278594-GasAroundGalaxies.","abstract":[{"lang":"eng","text":"We investigate correlations between different physical properties of star-forming galaxies in the ‘Evolution and Assembly of GaLaxies and their Environments’ (EAGLE) cosmological hydrodynamical simulation suite over the redshift range 0 ≤ z ≤ 4.5. A principal component analysis reveals that neutral gas fraction (fgas,neutral), stellar mass (Mstellar) and star formation rate (SFR) account for most of the variance seen in the population, with galaxies tracing a two-dimensional, nearly flat, surface in the three-dimensional space of fgas, neutral–Mstellar–SFR with little scatter. The location of this plane varies little with redshift, whereas galaxies themselves move along the plane as their fgas, neutral and SFR drop with redshift. The positions of galaxies along the plane are highly correlated with gas metallicity. The metallicity can therefore be robustly predicted from fgas, neutral, or from the Mstellar and SFR. We argue that the appearance of this ‘Fundamental Plane of star formation’ is a consequence of self-regulation, with the plane's curvature set by the dependence of the SFR on gas density and metallicity. We analyse a large compilation of observations spanning the redshift range 0 ≲ z ≲ 3, and find that such a plane is also present in the data. The properties of the observed Fundamental Plane of star formation are in good agreement with EAGLE's predictions."}],"arxiv":1,"doi":"10.1093/mnras/stw717","day":"01","external_id":{"arxiv":["1510.08067"]},"date_updated":"2022-08-19T08:12:07Z","citation":{"short":"C. del P. Lagos, T. Theuns, J. Schaye, M. Furlong, R.G. Bower, M. Schaller, R.A. Crain, J.W. Trayford, J.J. Matthee, Monthly Notices of the Royal Astronomical Society 459 (2016) 2632–2650.","mla":"Lagos, Claudia del P., et al. “The Fundamental Plane of Star Formation in Galaxies Revealed by the EAGLE Hydrodynamical Simulations.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 459, no. 3, Oxford University Press, 2016, pp. 2632–50, doi:<a href=\"https://doi.org/10.1093/mnras/stw717\">10.1093/mnras/stw717</a>.","ista":"Lagos C del P, Theuns T, Schaye J, Furlong M, Bower RG, Schaller M, Crain RA, Trayford JW, Matthee JJ. 2016. The Fundamental Plane of star formation in galaxies revealed by the EAGLE hydrodynamical simulations. Monthly Notices of the Royal Astronomical Society. 459(3), 2632–2650.","apa":"Lagos, C. del P., Theuns, T., Schaye, J., Furlong, M., Bower, R. G., Schaller, M., … Matthee, J. J. (2016). The Fundamental Plane of star formation in galaxies revealed by the EAGLE hydrodynamical simulations. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stw717\">https://doi.org/10.1093/mnras/stw717</a>","ama":"Lagos C del P, Theuns T, Schaye J, et al. The Fundamental Plane of star formation in galaxies revealed by the EAGLE hydrodynamical simulations. <i>Monthly Notices of the Royal Astronomical Society</i>. 2016;459(3):2632-2650. doi:<a href=\"https://doi.org/10.1093/mnras/stw717\">10.1093/mnras/stw717</a>","ieee":"C. del P. Lagos <i>et al.</i>, “The Fundamental Plane of star formation in galaxies revealed by the EAGLE hydrodynamical simulations,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 459, no. 3. Oxford University Press, pp. 2632–2650, 2016.","chicago":"Lagos, Claudia del P., Tom Theuns, Joop Schaye, Michelle Furlong, Richard G. Bower, Matthieu Schaller, Robert A. Crain, James W. Trayford, and Jorryt J Matthee. “The Fundamental Plane of Star Formation in Galaxies Revealed by the EAGLE Hydrodynamical Simulations.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2016. <a href=\"https://doi.org/10.1093/mnras/stw717\">https://doi.org/10.1093/mnras/stw717</a>."},"year":"2016","article_type":"original","publisher":"Oxford University Press","page":"2632-2650","quality_controlled":"1","title":"The Fundamental Plane of star formation in galaxies revealed by the EAGLE hydrodynamical simulations","intvolume":"       459","publication_status":"published","article_processing_charge":"No","date_created":"2022-07-13T10:21:24Z","author":[{"last_name":"Lagos","first_name":"Claudia del P.","full_name":"Lagos, Claudia del P."},{"last_name":"Theuns","first_name":"Tom","full_name":"Theuns, Tom"},{"first_name":"Joop","last_name":"Schaye","full_name":"Schaye, Joop"},{"full_name":"Furlong, Michelle","last_name":"Furlong","first_name":"Michelle"},{"full_name":"Bower, Richard G.","first_name":"Richard G.","last_name":"Bower"},{"full_name":"Schaller, Matthieu","first_name":"Matthieu","last_name":"Schaller"},{"full_name":"Crain, Robert A.","first_name":"Robert A.","last_name":"Crain"},{"last_name":"Trayford","first_name":"James W.","full_name":"Trayford, James W."},{"orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720"}],"issue":"3","_id":"11575","scopus_import":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1510.08067"}],"oa":1,"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"date_published":"2016-07-01T00:00:00Z","type":"journal_article","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics  stars: formation","ISM: evolution","galaxies: evolution","galaxies: formation","galaxies: ISM"],"month":"07","oa_version":"Preprint","publication":"Monthly Notices of the Royal Astronomical Society"},{"oa":1,"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"type":"journal_article","date_published":"2015-08-11T00:00:00Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","main_file_link":[{"url":"https://arxiv.org/abs/1502.06602","open_access":"1"}],"month":"08","oa_version":"Preprint","publication":"Monthly Notices of the Royal Astronomical Society","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: formation","galaxies: luminosity function","mass function","cosmology: observations","early Universe","large-scale structure of Universe"],"language":[{"iso":"eng"}],"abstract":[{"text":"We present results from the largest contiguous narrow-band survey in the near-infrared. We have used the wide-field infrared camera/Canada–France–Hawaii Telescope and the lowOH2 filter (1.187 ± 0.005 μm) to survey ≈10 deg2 of contiguous extragalactic sky in the SA22 field. A total of ∼6000 candidate emission-line galaxies are found. We use deep ugrizJK data to obtain robust photometric redshifts. We combine our data with the High-redshift(Z) Emission Line Survey (HiZELS), explore spectroscopic surveys (VVDS, VIPERS) and obtain our own spectroscopic follow-up with KMOS, FMOS and MOSFIRE to derive large samples of high-redshift emission-line selected galaxies: 3471 Hα emitters at z = 0.8, 1343 [O III] + Hβ emitters at z = 1.4 and 572 [O II] emitters at z = 2.2. We probe comoving volumes of >106 Mpc3 and find significant overdensities, including an 8.5σ (spectroscopically confirmed) overdensity of Hα emitters at z = 0.81. We derive Hα, [O III] + Hβ and [O II] luminosity functions at z = 0.8, 1.4, 2.2, respectively, and present implications for future surveys such as Euclid. Our uniquely large volumes/areas allow us to subdivide the samples in thousands of randomized combinations of areas and provide a robust empirical measurement of sample/cosmic variance. We show that surveys for star-forming/emission-line galaxies at a depth similar to ours can only overcome cosmic-variance (errors <10 per cent) if they are based on volumes >5 × 105 Mpc3; errors on L* and ϕ* due to sample (cosmic) variance on surveys probing ∼104 and ∼105 Mpc3 are typically very high: ∼300 and ∼40–60 per cent, respectively.","lang":"eng"}],"day":"11","arxiv":1,"doi":"10.1093/mnras/stv1076","external_id":{"arxiv":["1502.06602"]},"year":"2015","citation":{"chicago":"Sobral, D., Jorryt J Matthee, P. N. Best, I. Smail, A. A. Khostovan, B. Milvang-Jensen, J.-W. Kim, et al. “CF-HiZELS, an ∼10 Deg2 Emission-Line Survey with Spectroscopic Follow-up: Hα, [O III] + Hβ and [O II] Luminosity Functions at z = 0.8, 1.4 and 2.2 .” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2015. <a href=\"https://doi.org/10.1093/mnras/stv1076\">https://doi.org/10.1093/mnras/stv1076</a>.","ieee":"D. Sobral <i>et al.</i>, “CF-HiZELS, an ∼10 deg2 emission-line survey with spectroscopic follow-up: Hα, [O III] + Hβ and [O II] luminosity functions at z = 0.8, 1.4 and 2.2 ,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 451, no. 3. Oxford University Press, pp. 2303–2323, 2015.","apa":"Sobral, D., Matthee, J. J., Best, P. N., Smail, I., Khostovan, A. A., Milvang-Jensen, B., … Mobasher, B. (2015). CF-HiZELS, an ∼10 deg2 emission-line survey with spectroscopic follow-up: Hα, [O III] + Hβ and [O II] luminosity functions at z = 0.8, 1.4 and 2.2 . <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stv1076\">https://doi.org/10.1093/mnras/stv1076</a>","ama":"Sobral D, Matthee JJ, Best PN, et al. CF-HiZELS, an ∼10 deg2 emission-line survey with spectroscopic follow-up: Hα, [O III] + Hβ and [O II] luminosity functions at z = 0.8, 1.4 and 2.2 . <i>Monthly Notices of the Royal Astronomical Society</i>. 2015;451(3):2303-2323. doi:<a href=\"https://doi.org/10.1093/mnras/stv1076\">10.1093/mnras/stv1076</a>","ista":"Sobral D, Matthee JJ, Best PN, Smail I, Khostovan AA, Milvang-Jensen B, Kim J-W, Stott J, Calhau J, Nayyeri H, Mobasher B. 2015. CF-HiZELS, an ∼10 deg2 emission-line survey with spectroscopic follow-up: Hα, [O III] + Hβ and [O II] luminosity functions at z = 0.8, 1.4 and 2.2 . Monthly Notices of the Royal Astronomical Society. 451(3), 2303–2323.","mla":"Sobral, D., et al. “CF-HiZELS, an ∼10 Deg2 Emission-Line Survey with Spectroscopic Follow-up: Hα, [O III] + Hβ and [O II] Luminosity Functions at z = 0.8, 1.4 and 2.2 .” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 451, no. 3, Oxford University Press, 2015, pp. 2303–23, doi:<a href=\"https://doi.org/10.1093/mnras/stv1076\">10.1093/mnras/stv1076</a>.","short":"D. Sobral, J.J. Matthee, P.N. Best, I. Smail, A.A. Khostovan, B. Milvang-Jensen, J.-W. Kim, J. Stott, J. Calhau, H. Nayyeri, B. Mobasher, Monthly Notices of the Royal Astronomical Society 451 (2015) 2303–2323."},"date_updated":"2022-08-19T08:23:18Z","extern":"1","volume":451,"acknowledgement":"The authors wish to thank the anonymous reviewer for many helpful comments and suggestions which greatly improved the clarity and quality of this work. DS acknowledges financial support from the Netherlands Organization for Scientific research (NWO) through a Veni fellowship, from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010), from FCT grant PEst-OE/FIS/UI2751/2014, and from LSF and LKBF. JM acknowledges the award of a Huygens PhD fellowship. PNB is grateful for support from STFC. IRS acknowledges support from STFC, a Leverhulme Fellowship, the ERC Advanced Investigator programme DUSTYGAL and a Royal Society/Wolfson Merit Award. BMJ acknowledges support from the ERC-StG grant EGGS-278202. The Dark Cosmology Centre is funded by the DNRF. The Dark Cosmology Centre is funded by the DNRF. JWK acknowledges support from the National Research Foundation of Korea (NRF) grant, no. 2008-0060544, funded by the Korea government (MSIP). JPS acknowledges support from STFC (ST/I001573/1). JC acknowledges support from the FCT-IF grant IF/01154/2012/CP0189/CT0010. The work was only possible due to OPTICON/FP7 and the invaluable access that it granted to the CFHT telescope. We would also like to acknowledge the excellent work done by CFHT staff in conducting the observations in service mode, and on delivering truly excellent data. We are also tremendously thankful to Kentaro Aoki for the incredible support while observing at Subaru with FMOS, and also to the Keck staff for the help with the observations with MOSFIRE. This work is based on observations obtained with WIRCam on the CFHT, OPTICON programme 2011B/029, 2012A019 and 2012B/016. Based on observations made with ESO telescopes at the La Silla Paranal Observatory under programmes IDs 60.A-9460 (data can be accessed through the ESO data archive), 087.A 0337 and 089.A-0965. Based on observations done with FMOS on Subaru under programme S14A-084, and on MOSFIRE/Keck observations under programme U066M. Part of the data on which this analysis is based are available from Sobral et al. (2013a). Dedicated to the memory of C. M. Sobral (1953-2014).","intvolume":"       451","title":"CF-HiZELS, an ∼10 deg2 emission-line survey with spectroscopic follow-up: Hα, [O III] + Hβ and [O II] luminosity functions at z = 0.8, 1.4 and 2.2 ","date_created":"2022-07-14T09:02:22Z","article_processing_charge":"No","publication_status":"published","issue":"3","author":[{"first_name":"D.","last_name":"Sobral","full_name":"Sobral, D."},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J"},{"full_name":"Best, P. N.","last_name":"Best","first_name":"P. N."},{"last_name":"Smail","first_name":"I.","full_name":"Smail, I."},{"full_name":"Khostovan, A. A.","first_name":"A. A.","last_name":"Khostovan"},{"full_name":"Milvang-Jensen, B.","last_name":"Milvang-Jensen","first_name":"B."},{"first_name":"J.-W.","last_name":"Kim","full_name":"Kim, J.-W."},{"full_name":"Stott, J.","first_name":"J.","last_name":"Stott"},{"last_name":"Calhau","first_name":"J.","full_name":"Calhau, J."},{"first_name":"H.","last_name":"Nayyeri","full_name":"Nayyeri, H."},{"full_name":"Mobasher, B.","last_name":"Mobasher","first_name":"B."}],"scopus_import":"1","_id":"11580","article_type":"original","publisher":"Oxford University Press","quality_controlled":"1","page":"2303-2323"}]