[{"quality_controlled":"1","article_type":"original","publisher":"EDP Sciences","author":[{"last_name":"Kusakabe","first_name":"Haruka","full_name":"Kusakabe, Haruka"},{"full_name":"Verhamme, Anne","last_name":"Verhamme","first_name":"Anne"},{"last_name":"Blaizot","first_name":"Jérémy","full_name":"Blaizot, Jérémy"},{"full_name":"Garel, Thibault","first_name":"Thibault","last_name":"Garel"},{"full_name":"Wisotzki, Lutz","first_name":"Lutz","last_name":"Wisotzki"},{"full_name":"Leclercq, Floriane","last_name":"Leclercq","first_name":"Floriane"},{"full_name":"Bacon, Roland","last_name":"Bacon","first_name":"Roland"},{"full_name":"Schaye, Joop","first_name":"Joop","last_name":"Schaye"},{"full_name":"Gallego, Sofia G.","last_name":"Gallego","first_name":"Sofia G."},{"full_name":"Kerutt, Josephine","last_name":"Kerutt","first_name":"Josephine"},{"first_name":"Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Maseda","first_name":"Michael","full_name":"Maseda, Michael"},{"full_name":"Nanayakkara, Themiya","last_name":"Nanayakkara","first_name":"Themiya"},{"full_name":"Pelló, Roser","first_name":"Roser","last_name":"Pelló"},{"first_name":"Johan","last_name":"Richard","full_name":"Richard, Johan"},{"first_name":"Laurence","last_name":"Tresse","full_name":"Tresse, Laurence"},{"full_name":"Urrutia, Tanya","last_name":"Urrutia","first_name":"Tanya"},{"full_name":"Vitte, Eloïse","last_name":"Vitte","first_name":"Eloïse"}],"scopus_import":"1","_id":"11488","intvolume":"       660","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","date_created":"2022-07-05T14:27:26Z","article_processing_charge":"No","publication_status":"published","extern":"1","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,"external_id":{"arxiv":["2201.07257"]},"citation":{"apa":"Kusakabe, H., Verhamme, A., Blaizot, J., Garel, T., Wisotzki, L., Leclercq, F., … Vitte, E. (2022). The MUSE eXtremely Deep Field: Individual detections of 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>","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>","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>.","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.","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>.","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).","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."},"year":"2022","date_updated":"2022-07-19T09:33:24Z","abstract":[{"lang":"eng","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."}],"day":"07","doi":"10.1051/0004-6361/202142302","arxiv":1,"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift / galaxies: formation / galaxies: evolution / cosmology: observations"],"language":[{"iso":"eng"}],"publication":"Astronomy & Astrophysics","article_number":"A44","month":"04","oa_version":"Published Version","status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"url":"https://arxiv.org/abs/2201.07257","open_access":"1"}],"type":"journal_article","date_published":"2022-04-07T00:00:00Z","oa":1,"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]}},{"month":"03","article_number":"183","oa_version":"Published Version","publication":"Astronomy & Astrophysics","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift / galaxies: formation / galaxies: evolution / cosmology: observations"],"oa":1,"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"date_published":"2022-03-25T00:00:00Z","type":"journal_article","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2202.06642"}],"title":"Equivalent widths of Lyman α emitters in MUSE-Wide and MUSE-Deep","intvolume":"       659","publication_status":"published","date_created":"2022-07-06T08:17:27Z","article_processing_charge":"No","author":[{"first_name":"J.","last_name":"Kerutt","full_name":"Kerutt, J."},{"full_name":"Wisotzki, L.","first_name":"L.","last_name":"Wisotzki"},{"last_name":"Verhamme","first_name":"A.","full_name":"Verhamme, A."},{"first_name":"K. B.","last_name":"Schmidt","full_name":"Schmidt, K. B."},{"first_name":"F.","last_name":"Leclercq","full_name":"Leclercq, F."},{"last_name":"Herenz","first_name":"E. C.","full_name":"Herenz, E. C."},{"last_name":"Urrutia","first_name":"T.","full_name":"Urrutia, T."},{"last_name":"Garel","first_name":"T.","full_name":"Garel, T."},{"last_name":"Hashimoto","first_name":"T.","full_name":"Hashimoto, T."},{"first_name":"M.","last_name":"Maseda","full_name":"Maseda, M."},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J"},{"full_name":"Kusakabe, H.","first_name":"H.","last_name":"Kusakabe"},{"full_name":"Schaye, J.","last_name":"Schaye","first_name":"J."},{"full_name":"Richard, J.","last_name":"Richard","first_name":"J."},{"full_name":"Guiderdoni, B.","last_name":"Guiderdoni","first_name":"B."},{"full_name":"Mauerhofer, V.","first_name":"V.","last_name":"Mauerhofer"},{"full_name":"Nanayakkara, T.","first_name":"T.","last_name":"Nanayakkara"},{"last_name":"Vitte","first_name":"E.","full_name":"Vitte, E."}],"_id":"11497","scopus_import":"1","article_type":"original","publisher":"EDP Sciences","quality_controlled":"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."}],"doi":"10.1051/0004-6361/202141900","arxiv":1,"day":"25","external_id":{"arxiv":["2202.06642"]},"date_updated":"2022-07-19T09:47:16Z","year":"2022","citation":{"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.","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>.","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).","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.","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>.","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>","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>"},"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":659},{"extern":"1","volume":654,"acknowledgement":"We would like to thank Charlotte Mason for useful discussions and for providing the data for the curves shown in Fig. 13 and Dawn Erb for providing the observational data for the comparison sample studied by Steidel et al. (2014), also shown in Fig. 13. This work has been supported by the BMBF grant 05A14BAC and we acknowledge support by the Competitive Fund of the Leibniz Association through grant SAW-2015-AIP-2. AF acknowledges the support from grant PRIN MIUR2017-20173ML3WW_001. JS acknowledges the support from Vici grant 639.043.409 from the Dutch Research Council (NWO). GM received funding from the European Union’s Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant agreement No MARACAS – DLV-896778. This paper is based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programmes 094.A-0289(B), 095.A-0010(A), 096.A-0045(A), 096.A-0045(B), 094.A-0205, 095.A-0240, 096.A-0090, 097.A-0160, and 098.A-0017. This paper also makes use of observations made with the NASA/ESA Hubble Space Telescope obtained at STScI. This research made use of the following programs and open-source packages for Python and we are thankful to their developers: DS9 (Joye & Mandel 2003), Astropy (Astropy Collaboration 2013, 2018), APLpy (Robitaille & Bressert 2012), iPython (Pérez & Granger 2007), numpy (van der Walt et al. 2011), matplotlib (Hunter 2007), and SciPy (Jones et al. 2001).","abstract":[{"lang":"eng","text":"Rest-frame ultraviolet (UV) emission lines probe electron densities, gas-phase abundances, metallicities, and ionization parameters of the emitting star-forming galaxies and their environments. The strongest main UV emission line, Lyα, has been instrumental in advancing the general knowledge of galaxy formation in the early universe. However, observing Lyα emission becomes increasingly challenging at z ≳ 6 when the neutral hydrogen fraction of the circumgalactic and intergalactic media increases. Secondary weaker UV emission lines provide important alternative methods for studying galaxy properties at high redshift. We present a large sample of rest-frame UV emission line sources at intermediate redshift for calibrating and exploring the connection between secondary UV lines and the emitting galaxies’ physical properties and their Lyα emission. The sample of 2052 emission line sources with 1.5 < z < 6.4 was collected from integral field data from the MUSE-Wide and MUSE-Deep surveys taken as part of Guaranteed Time Observations. The objects were selected through untargeted source detection (i.e., no preselection of sources as in dedicated spectroscopic campaigns) in the three-dimensional MUSE data cubes. We searched optimally extracted one-dimensional spectra of the full sample for UV emission features via emission line template matching, resulting in a sample of more than 100 rest-frame UV emission line detections. We show that the detection efficiency of (non-Lyα) UV emission lines increases with survey depth, and that the emission line strength of He IIλ1640 Å, [O III] λ1661 + O III] λ1666, and [Si III] λ1883 + Si III] λ1892 correlate with the strength of [C III] λ1907 + C III] λ1909. The rest-frame equivalent width (EW0) of [C III] λ1907 + C III] λ1909 is found to be roughly 0.22 ± 0.18 of EW0(Lyα). We measured the velocity offsets of resonant emission lines with respect to systemic tracers. For C IVλ1548 + C IVλ1551 we find that ΔvC IV ≲ 250 km s−1, whereas ΔvLyα falls in the range of 250−500 km s−1 which is in agreement with previous results from the literature. The electron density ne measured from [Si III] λ1883 + Si III] λ1892 and [C III] λ1907 + C III] λ1909 line flux ratios is generally < 105 cm−3 and the gas-phase abundance is below solar at 12 + log10(O/H)≈8. Lastly, we used “PhotoIonization Model Probability Density Functions” to infer physical parameters of the full sample and individual systems based on photoionization model parameter grids and observational constraints from our UV emission line searches. This reveals that the UV line emitters generally have ionization parameter log10(U) ≈ −2.5 and metal mass fractions that scatter around Z ≈ 10−2, that is Z ≈ 0.66 Z⊙. Value-added catalogs of the full sample of MUSE objects studied in this work and a collection of UV line emitters from the literature are provided with this paper."}],"day":"15","arxiv":1,"doi":"10.1051/0004-6361/202140876","external_id":{"arxiv":["2108.01713"]},"year":"2021","citation":{"mla":"Schmidt, K. B., et al. “Recovery and Analysis of Rest-Frame UV Emission Lines in 2052 Galaxies Observed with MUSE at 1.5 &#60; z &#60; 6.4.” <i>Astronomy &#38; Astrophysics</i>, vol. 654, A80, EDP Sciences, 2021, doi:<a href=\"https://doi.org/10.1051/0004-6361/202140876\">10.1051/0004-6361/202140876</a>.","short":"K.B. Schmidt, J. Kerutt, L. Wisotzki, T. Urrutia, A. Feltre, M.V. Maseda, T. Nanayakkara, R. Bacon, L.A. Boogaard, S. Conseil, T. Contini, E.C. Herenz, W. Kollatschny, M. Krumpe, F. Leclercq, G. Mahler, J.J. Matthee, V. Mauerhofer, J. Richard, J. Schaye, Astronomy &#38; Astrophysics 654 (2021).","ista":"Schmidt KB, Kerutt J, Wisotzki L, Urrutia T, Feltre A, Maseda MV, Nanayakkara T, Bacon R, Boogaard LA, Conseil S, Contini T, Herenz EC, Kollatschny W, Krumpe M, Leclercq F, Mahler G, Matthee JJ, Mauerhofer V, Richard J, Schaye J. 2021. Recovery and analysis of rest-frame UV emission lines in 2052 galaxies observed with MUSE at 1.5 &#60; z &#60; 6.4. Astronomy &#38; Astrophysics. 654, A80.","ama":"Schmidt KB, Kerutt J, Wisotzki L, et al. Recovery and analysis of rest-frame UV emission lines in 2052 galaxies observed with MUSE at 1.5 &#60; z &#60; 6.4. <i>Astronomy &#38; Astrophysics</i>. 2021;654. doi:<a href=\"https://doi.org/10.1051/0004-6361/202140876\">10.1051/0004-6361/202140876</a>","apa":"Schmidt, K. B., Kerutt, J., Wisotzki, L., Urrutia, T., Feltre, A., Maseda, M. V., … Schaye, J. (2021). Recovery and analysis of rest-frame UV emission lines in 2052 galaxies observed with MUSE at 1.5 &#60; z &#60; 6.4. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202140876\">https://doi.org/10.1051/0004-6361/202140876</a>","chicago":"Schmidt, K. B., J. Kerutt, L. Wisotzki, T. Urrutia, A. Feltre, M. V. Maseda, T. Nanayakkara, et al. “Recovery and Analysis of Rest-Frame UV Emission Lines in 2052 Galaxies Observed with MUSE at 1.5 &#60; z &#60; 6.4.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2021. <a href=\"https://doi.org/10.1051/0004-6361/202140876\">https://doi.org/10.1051/0004-6361/202140876</a>.","ieee":"K. B. Schmidt <i>et al.</i>, “Recovery and analysis of rest-frame UV emission lines in 2052 galaxies observed with MUSE at 1.5 &#60; z &#60; 6.4,” <i>Astronomy &#38; Astrophysics</i>, vol. 654. EDP Sciences, 2021."},"date_updated":"2022-07-19T09:34:36Z","article_type":"original","publisher":"EDP Sciences","quality_controlled":"1","intvolume":"       654","title":"Recovery and analysis of rest-frame UV emission lines in 2052 galaxies observed with MUSE at 1.5 < z < 6.4","article_processing_charge":"No","date_created":"2022-07-06T08:49:03Z","publication_status":"published","author":[{"last_name":"Schmidt","first_name":"K. B.","full_name":"Schmidt, K. B."},{"full_name":"Kerutt, J.","last_name":"Kerutt","first_name":"J."},{"first_name":"L.","last_name":"Wisotzki","full_name":"Wisotzki, L."},{"first_name":"T.","last_name":"Urrutia","full_name":"Urrutia, T."},{"first_name":"A.","last_name":"Feltre","full_name":"Feltre, A."},{"last_name":"Maseda","first_name":"M. V.","full_name":"Maseda, M. V."},{"first_name":"T.","last_name":"Nanayakkara","full_name":"Nanayakkara, T."},{"full_name":"Bacon, R.","first_name":"R.","last_name":"Bacon"},{"last_name":"Boogaard","first_name":"L. A.","full_name":"Boogaard, L. A."},{"first_name":"S.","last_name":"Conseil","full_name":"Conseil, S."},{"full_name":"Contini, T.","first_name":"T.","last_name":"Contini"},{"first_name":"E. C.","last_name":"Herenz","full_name":"Herenz, E. C."},{"first_name":"W.","last_name":"Kollatschny","full_name":"Kollatschny, W."},{"last_name":"Krumpe","first_name":"M.","full_name":"Krumpe, M."},{"last_name":"Leclercq","first_name":"F.","full_name":"Leclercq, F."},{"full_name":"Mahler, G.","first_name":"G.","last_name":"Mahler"},{"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":"Mauerhofer, V.","last_name":"Mauerhofer","first_name":"V."},{"full_name":"Richard, J.","first_name":"J.","last_name":"Richard"},{"full_name":"Schaye, J.","first_name":"J.","last_name":"Schaye"}],"scopus_import":"1","_id":"11498","status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2108.01713"}],"oa":1,"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"type":"journal_article","date_published":"2021-10-15T00:00:00Z","keyword":["Space and Planetary Science","Astronomy and Astrophysics","ultraviolet: galaxies / galaxies: high-redshift / galaxies: ISM / ISM: lines and bands / methods: observational / techniques: imaging spectroscopy"],"language":[{"iso":"eng"}],"article_number":"A80","month":"10","oa_version":"Published Version","publication":"Astronomy & Astrophysics"},{"abstract":[{"lang":"eng","text":"We report the discovery of diffuse extended Lyα emission from redshift 3.1 to 4.5, tracing cosmic web filaments on scales of 2.5−4 cMpc. These structures have been observed in overdensities of Lyα emitters in the MUSE Extremely Deep Field, a 140 h deep MUSE observation located in the Hubble Ultra-Deep Field. Among the 22 overdense regions identified, five are likely to harbor very extended Lyα emission at high significance with an average surface brightness of 5 × 10−20 erg s−1 cm−2 arcsec−2. Remarkably, 70% of the total Lyα luminosity from these filaments comes from beyond the circumgalactic medium of any identified Lyα emitter. Fluorescent Lyα emission powered by the cosmic UV background can only account for less than 34% of this emission at z ≈ 3 and for not more than 10% at higher redshift. We find that the bulk of this diffuse emission can be reproduced by the unresolved Lyα emission of a large population of ultra low-luminosity Lyα emitters (< 1040 erg s−1), provided that the faint end of the Lyα luminosity function is steep (α ⪅ −1.8), it extends down to luminosities lower than 1038 − 1037 erg s−1, and the clustering of these Lyα emitters is significant (filling factor < 1/6). If these Lyα emitters are powered by star formation, then this implies their luminosity function needs to extend down to star formation rates < 10−4 M⊙ yr−1. These observations provide the first detection of the cosmic web in Lyα emission in typical filamentary environments and the first observational clue indicating the existence of a large population of ultra low-luminosity Lyα emitters at high redshift."}],"day":"18","doi":"10.1051/0004-6361/202039887","arxiv":1,"external_id":{"arxiv":["2102.05516"]},"citation":{"ista":"Bacon R, Mary D, Garel T, Blaizot J, Maseda M, Schaye J, Wisotzki L, Conseil S, Brinchmann J, Leclercq F, Abril-Melgarejo V, Boogaard L, Bouché NF, Contini T, Feltre A, Guiderdoni B, Herenz C, Kollatschny W, Kusakabe H, Matthee JJ, Michel-Dansac L, Nanayakkara T, Richard J, Roth M, Schmidt KB, Steinmetz M, Tresse L, Urrutia T, Verhamme A, Weilbacher PM, Zabl J, Zoutendijk SL. 2021. The MUSE Extremely Deep Field: The cosmic web in emission at high redshift. Astronomy &#38; Astrophysics. 647, A107.","mla":"Bacon, R., et al. “The MUSE Extremely Deep Field: The Cosmic Web in Emission at High Redshift.” <i>Astronomy &#38; Astrophysics</i>, vol. 647, A107, EDP Sciences, 2021, doi:<a href=\"https://doi.org/10.1051/0004-6361/202039887\">10.1051/0004-6361/202039887</a>.","short":"R. Bacon, D. Mary, T. Garel, J. Blaizot, M. Maseda, J. Schaye, L. Wisotzki, S. Conseil, J. Brinchmann, F. Leclercq, V. Abril-Melgarejo, L. Boogaard, N.F. Bouché, T. Contini, A. Feltre, B. Guiderdoni, C. Herenz, W. Kollatschny, H. Kusakabe, J.J. Matthee, L. Michel-Dansac, T. Nanayakkara, J. Richard, M. Roth, K.B. Schmidt, M. Steinmetz, L. Tresse, T. Urrutia, A. Verhamme, P.M. Weilbacher, J. Zabl, S.L. Zoutendijk, Astronomy &#38; Astrophysics 647 (2021).","chicago":"Bacon, R., D. Mary, T. Garel, J. Blaizot, M. Maseda, J. Schaye, L. Wisotzki, et al. “The MUSE Extremely Deep Field: The Cosmic Web in Emission at High Redshift.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2021. <a href=\"https://doi.org/10.1051/0004-6361/202039887\">https://doi.org/10.1051/0004-6361/202039887</a>.","ieee":"R. Bacon <i>et al.</i>, “The MUSE Extremely Deep Field: The cosmic web in emission at high redshift,” <i>Astronomy &#38; Astrophysics</i>, vol. 647. EDP Sciences, 2021.","apa":"Bacon, R., Mary, D., Garel, T., Blaizot, J., Maseda, M., Schaye, J., … Zoutendijk, S. L. (2021). The MUSE Extremely Deep Field: The cosmic web in emission at high redshift. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202039887\">https://doi.org/10.1051/0004-6361/202039887</a>","ama":"Bacon R, Mary D, Garel T, et al. The MUSE Extremely Deep Field: The cosmic web in emission at high redshift. <i>Astronomy &#38; Astrophysics</i>. 2021;647. doi:<a href=\"https://doi.org/10.1051/0004-6361/202039887\">10.1051/0004-6361/202039887</a>"},"year":"2021","date_updated":"2022-07-19T09:34:57Z","extern":"1","acknowledgement":"We warmly thank ESO Paranal staff for their great professional support during all MXDF GTO observing runs. We thank the anonymous referee for a careful reading of the manuscript and helpful comments. We also thank Matthew Lehnert for fruitful discussions. RB, AF, SC acknowledge support from the ERC advanced grant 339659-MUSICOS. JB acknowledges support by Fundação para a Ciência e a Tecnologia (FCT) through the research grants UID/FIS/04434/2019, UIDB/04434/2020, UIDP/04434/2020 and through the Investigador FCT Contract No. IF/01654/2014/CP1215/CT0003. TG, AV acknowledges support from the European Research Council under grant agreement ERC-stg-757258 (TRIPLE). DM acknowledges A. Dabbech for useful interactions about IUWT and support from the GDR ISIS through the Projets exploratoires program (project TASTY). AF acknowledges the support from grant PRIN MIUR2017-20173ML3WW_001. SLZ acknowledges support by The Netherlands Organisation for Scientific Research (NWO) through a TOP Grant Module 1 under project number 614.001.652. This research made use of the following open-source software and we are thankful to the developers of these: GNU Octave (Eaton et al. 2018) and its statistics, signal and image packages, the Python packages Matplotlib (Hunter 2007), Numpy (van der Walt et al. 2010), MPDAF (Piqueras et al. 2017), Astropy (Astropy Collaboration 2018), PyWavelets (Lee et al. 2019).","volume":647,"intvolume":"       647","title":"The MUSE Extremely Deep Field: The cosmic web in emission at high redshift","date_created":"2022-07-06T09:31:50Z","article_processing_charge":"No","publication_status":"published","author":[{"last_name":"Bacon","first_name":"R.","full_name":"Bacon, R."},{"last_name":"Mary","first_name":"D.","full_name":"Mary, D."},{"full_name":"Garel, T.","last_name":"Garel","first_name":"T."},{"last_name":"Blaizot","first_name":"J.","full_name":"Blaizot, J."},{"full_name":"Maseda, M.","last_name":"Maseda","first_name":"M."},{"last_name":"Schaye","first_name":"J.","full_name":"Schaye, J."},{"first_name":"L.","last_name":"Wisotzki","full_name":"Wisotzki, L."},{"full_name":"Conseil, S.","last_name":"Conseil","first_name":"S."},{"first_name":"J.","last_name":"Brinchmann","full_name":"Brinchmann, J."},{"full_name":"Leclercq, F.","first_name":"F.","last_name":"Leclercq"},{"full_name":"Abril-Melgarejo, V.","first_name":"V.","last_name":"Abril-Melgarejo"},{"first_name":"L.","last_name":"Boogaard","full_name":"Boogaard, L."},{"first_name":"N. F.","last_name":"Bouché","full_name":"Bouché, N. F."},{"full_name":"Contini, T.","last_name":"Contini","first_name":"T."},{"full_name":"Feltre, A.","last_name":"Feltre","first_name":"A."},{"last_name":"Guiderdoni","first_name":"B.","full_name":"Guiderdoni, B."},{"first_name":"C.","last_name":"Herenz","full_name":"Herenz, C."},{"last_name":"Kollatschny","first_name":"W.","full_name":"Kollatschny, W."},{"first_name":"H.","last_name":"Kusakabe","full_name":"Kusakabe, H."},{"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":"Michel-Dansac, L.","last_name":"Michel-Dansac","first_name":"L."},{"full_name":"Nanayakkara, T.","last_name":"Nanayakkara","first_name":"T."},{"last_name":"Richard","first_name":"J.","full_name":"Richard, J."},{"last_name":"Roth","first_name":"M.","full_name":"Roth, M."},{"full_name":"Schmidt, K. B.","last_name":"Schmidt","first_name":"K. B."},{"full_name":"Steinmetz, M.","last_name":"Steinmetz","first_name":"M."},{"full_name":"Tresse, L.","last_name":"Tresse","first_name":"L."},{"full_name":"Urrutia, T.","last_name":"Urrutia","first_name":"T."},{"full_name":"Verhamme, A.","last_name":"Verhamme","first_name":"A."},{"full_name":"Weilbacher, P. M.","first_name":"P. M.","last_name":"Weilbacher"},{"first_name":"J.","last_name":"Zabl","full_name":"Zabl, J."},{"full_name":"Zoutendijk, S. L.","first_name":"S. L.","last_name":"Zoutendijk"}],"scopus_import":"1","_id":"11500","article_type":"original","publisher":"EDP Sciences","quality_controlled":"1","oa":1,"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"type":"journal_article","date_published":"2021-03-18T00:00:00Z","status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"url":"https://arxiv.org/abs/2102.05516","open_access":"1"}],"article_number":"A107","month":"03","oa_version":"Published Version","publication":"Astronomy & Astrophysics","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift / galaxies: groups: general / cosmology: observations"],"language":[{"iso":"eng"}]},{"volume":635,"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.","extern":"1","day":"11","doi":"10.1051/0004-6361/201937339","arxiv":1,"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."}],"year":"2020","citation":{"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.","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>.","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>","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.","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).","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>."},"date_updated":"2022-07-19T09:36:58Z","external_id":{"arxiv":["2002.05731"]},"publisher":"EDP Sciences","article_type":"original","quality_controlled":"1","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","scopus_import":"1","_id":"11504","author":[{"first_name":"Floriane","last_name":"Leclercq","full_name":"Leclercq, Floriane"},{"first_name":"Roland","last_name":"Bacon","full_name":"Bacon, Roland"},{"first_name":"Anne","last_name":"Verhamme","full_name":"Verhamme, Anne"},{"full_name":"Garel, Thibault","last_name":"Garel","first_name":"Thibault"},{"full_name":"Blaizot, Jérémy","first_name":"Jérémy","last_name":"Blaizot"},{"full_name":"Brinchmann, Jarle","last_name":"Brinchmann","first_name":"Jarle"},{"full_name":"Cantalupo, Sebastiano","last_name":"Cantalupo","first_name":"Sebastiano"},{"full_name":"Claeyssens, Adélaïde","first_name":"Adélaïde","last_name":"Claeyssens"},{"last_name":"Conseil","first_name":"Simon","full_name":"Conseil, Simon"},{"first_name":"Thierry","last_name":"Contini","full_name":"Contini, Thierry"},{"last_name":"Hashimoto","first_name":"Takuya","full_name":"Hashimoto, Takuya"},{"full_name":"Herenz, Edmund Christian","first_name":"Edmund Christian","last_name":"Herenz"},{"full_name":"Kusakabe, Haruka","first_name":"Haruka","last_name":"Kusakabe"},{"full_name":"Marino, Raffaella Anna","first_name":"Raffaella Anna","last_name":"Marino"},{"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"},{"first_name":"Gabriele","last_name":"Pezzulli","full_name":"Pezzulli, Gabriele"},{"last_name":"Richard","first_name":"Johan","full_name":"Richard, Johan"},{"full_name":"Schmidt, Kasper Borello","first_name":"Kasper Borello","last_name":"Schmidt"},{"last_name":"Wisotzki","first_name":"Lutz","full_name":"Wisotzki, Lutz"}],"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2002.05731"}],"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"oa":1,"type":"journal_article","date_published":"2020-03-11T00:00:00Z","keyword":["Space and Planetary Science","Astronomy and Astrophysics galaxies: high-redshift / galaxies: formation / galaxies: evolution / cosmology: observations"],"language":[{"iso":"eng"}],"oa_version":"Published Version","article_number":"A82","month":"03","publication":"Astronomy & Astrophysics"},{"author":[{"last_name":"Sobral","first_name":"David","full_name":"Sobral, David"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X"}],"scopus_import":"1","_id":"11507","intvolume":"       623","title":"Predicting Lyα escape fractions with a simple observable: Lyα in emission as an empirically calibrated star formation rate indicator","date_created":"2022-07-06T11:08:16Z","article_processing_charge":"No","publication_status":"published","quality_controlled":"1","article_type":"original","publisher":"EDP Sciences","external_id":{"arxiv":["1803.08923"]},"citation":{"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>","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>.","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>.","short":"D. Sobral, J.J. Matthee, Astronomy &#38; Astrophysics 623 (2019).","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."},"year":"2019","date_updated":"2022-07-19T09:37:20Z","abstract":[{"lang":"eng","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."}],"day":"26","arxiv":1,"doi":"10.1051/0004-6361/201833075","extern":"1","volume":623,"acknowledgement":"We thank the anonymous referees for multiple comments and suggestions which have improved the manuscript. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. We have benefited greatly from the publicly available programming language PYTHON, including the NUMPY & SCIPY (Van Der Walt et al. 2011; Jones et al. 2001), MATPLOTLIB (Hunter 2007) and ASTROPY (Astropy Collaboration 2013) packages, and the TOPCAT analysis program (Taylor 2013). The results and samples of LAEs used for this paper are publicly available (see e.g. Sobral et al. 2017, 2018a) and we also provide the toy model used as a PYTHON script.","publication":"Astronomy & Astrophysics","article_number":"A157","month":"03","oa_version":"Published Version","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"}],"type":"journal_article","date_published":"2019-03-26T00:00:00Z","oa":1,"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"url":"https://arxiv.org/abs/1803.08923","open_access":"1"}]},{"type":"journal_article","date_published":"2018-11-19T00:00:00Z","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"oa":1,"main_file_link":[{"url":"https://arxiv.org/abs/1805.11621","open_access":"1"}],"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication":"Astronomy & Astrophysics","oa_version":"Published Version","article_number":"A136","month":"11","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"}],"citation":{"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>.","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.","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>","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>","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.","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>.","short":"J.J. Matthee, D. Sobral, M. Gronke, A. Paulino-Afonso, M. Stefanon, H. Röttgering, Astronomy &#38; Astrophysics 619 (2018)."},"year":"2018","date_updated":"2022-07-19T09:32:08Z","external_id":{"arxiv":["1805.11621"]},"day":"19","doi":"10.1051/0004-6361/201833528","arxiv":1,"abstract":[{"lang":"eng","text":"Distant luminous Lyman-α emitters (LAEs) are excellent targets for spectroscopic observations of galaxies in the epoch of reionisation (EoR). We present deep high-resolution (R = 5000) VLT/X-shooter observations, along with an extensive collection of photometric data of COLA1, a proposed double peaked LAE at z = 6.6. We rule out the possibility that COLA1’s emission line is an [OII] doublet at z = 1.475 on the basis of i) the asymmetric red line-profile and flux ratio of the peaks (blue/red=0.31 ± 0.03) and ii) an unphysical [OII]/Hα ratio ([OII]/Hα >  22). We show that COLA1’s observed B-band flux is explained by a faint extended foreground LAE, for which we detect Lyα and [OIII] at z = 2.142. We thus conclude that COLA1 is a real double-peaked LAE at z = 6.593, the first discovered at z >  6. COLA1 is UV luminous (M1500 = −21.6 ± 0.3), has a high equivalent width (EW0,Lyα = 120−40+50 Å) and very compact Lyα emission (r50,Lyα = 0.33−0.04+0.07 kpc). Relatively weak inferred Hβ+[OIII] line-emission from Spitzer/IRAC indicates an extremely low metallicity of Z <  1/20 Z⊙ or reduced strength of nebular lines due to high escape of ionising photons. The small Lyα peak separation of 220 ± 20 km s−1 implies a low HI column density and an ionising photon escape fraction of ≈15 − 30%, providing the first direct evidence that such galaxies contribute actively to the reionisation of the Universe at z >  6. Based on simple estimates, we find that COLA1 could have provided just enough photons to reionise its own ≈0.3 pMpc (2.3 cMpc) bubble, allowing the blue Lyα line to be observed. However, we also discuss alternative scenarios explaining the detected double peaked nature of COLA1. Our results show that future high-resolution observations of statistical samples of double peaked LAEs at z >  5 are a promising probe of the occurrence of ionised regions around galaxies in the EoR."}],"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).","extern":"1","scopus_import":"1","_id":"11508","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J"},{"full_name":"Sobral, David","first_name":"David","last_name":"Sobral"},{"full_name":"Gronke, Max","first_name":"Max","last_name":"Gronke"},{"first_name":"Ana","last_name":"Paulino-Afonso","full_name":"Paulino-Afonso, Ana"},{"full_name":"Stefanon, Mauro","last_name":"Stefanon","first_name":"Mauro"},{"full_name":"Röttgering, Huub","last_name":"Röttgering","first_name":"Huub"}],"date_created":"2022-07-06T11:14:23Z","article_processing_charge":"No","publication_status":"published","intvolume":"       619","title":"Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly contributing to the reionisation of the universe","quality_controlled":"1","publisher":"EDP Sciences","article_type":"original"},{"oa":1,"publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"type":"journal_article","date_published":"2017-12-21T00:00:00Z","status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1709.06569"}],"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"}],"abstract":[{"lang":"eng","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."}],"day":"21","arxiv":1,"doi":"10.3847/1538-4357/aa9931","external_id":{"arxiv":["1709.06569"]},"citation":{"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>","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>","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.","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>.","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."},"year":"2017","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.","intvolume":"       851","title":"ALMA reveals metals yet no dust within multiple components in CR7","article_processing_charge":"No","date_created":"2022-07-07T08:48:04Z","publication_status":"published","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":"Sobral, D.","first_name":"D.","last_name":"Sobral"},{"full_name":"Boone, F.","last_name":"Boone","first_name":"F."},{"full_name":"Röttgering, H.","first_name":"H.","last_name":"Röttgering"},{"full_name":"Schaerer, D.","first_name":"D.","last_name":"Schaerer"},{"last_name":"Girard","first_name":"M.","full_name":"Girard, M."},{"full_name":"Pallottini, A.","first_name":"A.","last_name":"Pallottini"},{"full_name":"Vallini, L.","first_name":"L.","last_name":"Vallini"},{"first_name":"A.","last_name":"Ferrara","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":[{"lang":"eng","text":"We present the spatially resolved Hα dynamics of 16 star-forming galaxies at z ∼ 0.81 using the new KMOS multi-object integral field spectrograph on the ESO Very Large Telescope. These galaxies, selected using 1.18 μm narrowband imaging from the 10 deg2 CFHT-HiZELS survey of the SA 22 hr field, are found in a ∼4 Mpc overdensity of Hα emitters and likely reside in a group/intermediate environment, but not a cluster. We confirm and identify a rich group of star-forming galaxies at z = 0.813 ± 0.003, with 13 galaxies within 1000 km s−1 of each other, and seven within a diameter of 3 Mpc. All of our galaxies are “typical” star-forming galaxies at their redshift, 0.8 ± 0.4 SFR$^*_{z = 0.8}$, spanning a range of specific star formation rates (sSFRs) of 0.2–1.1 Gyr−1 and have a median metallicity very close to solar of 12 + log(O/H) = 8.62 ± 0.06. We measure the spatially resolved Hα dynamics of the galaxies in our sample and show that 13 out of 16 galaxies can be described by rotating disks and use the data to derive inclination corrected rotation speeds of 50–275 km s−1. The fraction of disks within our sample is 75% ± 8%, consistent with previous results based on Hubble Space Telescope morphologies of Hα-selected galaxies at z ∼ 1 and confirming that disks dominate the SFR density at z ∼ 1. Our Hα galaxies are well fitted by the z ∼ 1–2 Tully–Fisher (TF) relation, confirming the evolution seen in the zero point. Apart from having, on average, higher stellar masses and lower sSFRs, our group galaxies at z = 0.81 present the same mass–metallicity and TF relation as z ∼ 1 field galaxies and are all disk galaxies."}],"arxiv":1,"doi":"10.1088/0004-637x/779/2/139","day":"03","external_id":{"arxiv":["1310.3822"]},"date_updated":"2022-08-18T10:43:07Z","year":"2013","citation":{"chicago":"Sobral, D., A. M. Swinbank, J. P. Stott, Jorryt J Matthee, R. G. Bower, Ian Smail, P. Best, J. E. Geach, and R. M. Sharples. “The Dynamics of Z=0.8 H-Alpha-Selected Star-Forming Galaxies from KMOS/CF-HiZELS.” <i>The Astrophysical Journal</i>. IOP Publishing, 2013. <a href=\"https://doi.org/10.1088/0004-637x/779/2/139\">https://doi.org/10.1088/0004-637x/779/2/139</a>.","ieee":"D. Sobral <i>et al.</i>, “The dynamics of z=0.8 H-alpha-selected star-forming galaxies from KMOS/CF-HiZELS,” <i>The Astrophysical Journal</i>, vol. 779, no. 2. IOP Publishing, 2013.","apa":"Sobral, D., Swinbank, A. M., Stott, J. P., Matthee, J. J., Bower, R. G., Smail, I., … Sharples, R. M. (2013). The dynamics of z=0.8 H-alpha-selected star-forming galaxies from KMOS/CF-HiZELS. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.1088/0004-637x/779/2/139\">https://doi.org/10.1088/0004-637x/779/2/139</a>","ama":"Sobral D, Swinbank AM, Stott JP, et al. The dynamics of z=0.8 H-alpha-selected star-forming galaxies from KMOS/CF-HiZELS. <i>The Astrophysical Journal</i>. 2013;779(2). doi:<a href=\"https://doi.org/10.1088/0004-637x/779/2/139\">10.1088/0004-637x/779/2/139</a>","ista":"Sobral D, Swinbank AM, Stott JP, Matthee JJ, Bower RG, Smail I, Best P, Geach JE, Sharples RM. 2013. The dynamics of z=0.8 H-alpha-selected star-forming galaxies from KMOS/CF-HiZELS. The Astrophysical Journal. 779(2), 139.","short":"D. Sobral, A.M. Swinbank, J.P. Stott, J.J. Matthee, R.G. Bower, I. Smail, P. Best, J.E. Geach, R.M. Sharples, The Astrophysical Journal 779 (2013).","mla":"Sobral, D., et al. “The Dynamics of Z=0.8 H-Alpha-Selected Star-Forming Galaxies from KMOS/CF-HiZELS.” <i>The Astrophysical Journal</i>, vol. 779, no. 2, 139, IOP Publishing, 2013, doi:<a href=\"https://doi.org/10.1088/0004-637x/779/2/139\">10.1088/0004-637x/779/2/139</a>."},"extern":"1","acknowledgement":"We thank the referee for many helpful comments and suggestions which greatly improved the clarity and quality of this work. D.S. acknowledges financial support from the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship and also funding from the European Community Seventh Framework Programme (FP7/2007-2013) under grant agreement number RG226604 (OPTICON) which allowed access to CFHT time (proposals: 11BO29 & 12AO19). A.M.S. gratefully acknowledges an STFC Advanced Fellowship through grant number ST/H005234/1. I.R.S., J.P.S., and R.G.B. acknowledge support from the UK Science and Technology Facilities Council (STFC) under ST/I001573/1. I.R.S. acknowledges STFC (ST/J001422/1), the ERC Advanced Investigator program DUSTYGAL and a Royal Society/Wolfson Merit Award. P.N.B. acknowledges support from STFC. R.M.S. acknowledges support from the grant ST/1001573/1. The data presented here are based on observations with the KMOS spectrograph on the ESO/VLT under program 60.A-9460 and can be accessed through the ESO data archive. The authors also wish to acknowledge the help from Michael Hilker in preparing the KMOS observations.","volume":779,"title":"The dynamics of z=0.8 H-alpha-selected star-forming galaxies from KMOS/CF-HiZELS","intvolume":"       779","publication_status":"published","article_processing_charge":"No","date_created":"2022-07-07T09:14:48Z","author":[{"first_name":"D.","last_name":"Sobral","full_name":"Sobral, D."},{"last_name":"Swinbank","first_name":"A. M.","full_name":"Swinbank, A. M."},{"full_name":"Stott, J. P.","last_name":"Stott","first_name":"J. P."},{"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":"Bower, R. G.","first_name":"R. G.","last_name":"Bower"},{"first_name":"Ian","last_name":"Smail","full_name":"Smail, Ian"},{"first_name":"P.","last_name":"Best","full_name":"Best, P."},{"full_name":"Geach, J. E.","first_name":"J. E.","last_name":"Geach"},{"full_name":"Sharples, R. M.","first_name":"R. M.","last_name":"Sharples"}],"issue":"2","_id":"11520","scopus_import":"1","article_type":"original","publisher":"IOP Publishing","quality_controlled":"1","oa":1,"publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"date_published":"2013-12-03T00:00:00Z","type":"journal_article","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1310.3822"}],"month":"12","article_number":"139","oa_version":"Preprint","publication":"The Astrophysical Journal","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution – galaxies","high-redshift – galaxies","starburst"]}]