[{"date_created":"2022-07-06T08:49:03Z","month":"10","date_published":"2021-10-15T00:00:00Z","article_type":"original","scopus_import":"1","publisher":"EDP Sciences","language":[{"iso":"eng"}],"publication":"Astronomy & Astrophysics","day":"15","type":"journal_article","intvolume":"       654","status":"public","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2108.01713"}],"article_number":"A80","doi":"10.1051/0004-6361/202140876","year":"2021","external_id":{"arxiv":["2108.01713"]},"title":"Recovery and analysis of rest-frame UV emission lines in 2052 galaxies observed with MUSE at 1.5 < z < 6.4","arxiv":1,"article_processing_charge":"No","date_updated":"2022-07-19T09:34:36Z","oa":1,"volume":654,"extern":"1","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"_id":"11498","oa_version":"Published Version","quality_controlled":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","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).","citation":{"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>","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.","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>.","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>.","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>","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.","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)."},"publication_status":"published","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."}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","ultraviolet: galaxies / galaxies: high-redshift / galaxies: ISM / ISM: lines and bands / methods: observational / techniques: imaging spectroscopy"],"author":[{"full_name":"Schmidt, K. B.","last_name":"Schmidt","first_name":"K. B."},{"last_name":"Kerutt","full_name":"Kerutt, J.","first_name":"J."},{"first_name":"L.","last_name":"Wisotzki","full_name":"Wisotzki, L."},{"full_name":"Urrutia, T.","last_name":"Urrutia","first_name":"T."},{"first_name":"A.","full_name":"Feltre, A.","last_name":"Feltre"},{"first_name":"M. V.","last_name":"Maseda","full_name":"Maseda, M. V."},{"first_name":"T.","last_name":"Nanayakkara","full_name":"Nanayakkara, T."},{"first_name":"R.","full_name":"Bacon, R.","last_name":"Bacon"},{"last_name":"Boogaard","full_name":"Boogaard, L. A.","first_name":"L. A."},{"last_name":"Conseil","full_name":"Conseil, S.","first_name":"S."},{"last_name":"Contini","full_name":"Contini, T.","first_name":"T."},{"last_name":"Herenz","full_name":"Herenz, E. C.","first_name":"E. C."},{"first_name":"W.","full_name":"Kollatschny, W.","last_name":"Kollatschny"},{"last_name":"Krumpe","full_name":"Krumpe, M.","first_name":"M."},{"first_name":"F.","full_name":"Leclercq, F.","last_name":"Leclercq"},{"first_name":"G.","full_name":"Mahler, G.","last_name":"Mahler"},{"first_name":"Jorryt J","last_name":"Matthee","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"full_name":"Mauerhofer, V.","last_name":"Mauerhofer","first_name":"V."},{"first_name":"J.","last_name":"Richard","full_name":"Richard, J."},{"first_name":"J.","last_name":"Schaye","full_name":"Schaye, J."}]},{"status":"public","intvolume":"       505","type":"journal_article","day":"01","page":"1382-1412","issue":"1","publication":"Monthly Notices of the Royal Astronomical Society","language":[{"iso":"eng"}],"publisher":"Oxford University Press","scopus_import":"1","article_type":"original","date_published":"2021-07-01T00:00:00Z","month":"07","date_created":"2022-07-07T09:33:39Z","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: formation","galaxies: ISM","galaxies: starburst","dark ages","reionization","first stars"],"author":[{"full_name":"Matthee, Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Sobral","full_name":"Sobral, David","first_name":"David"},{"last_name":"Hayes","full_name":"Hayes, Matthew","first_name":"Matthew"},{"first_name":"Gabriele","last_name":"Pezzulli","full_name":"Pezzulli, Gabriele"},{"first_name":"Max","last_name":"Gronke","full_name":"Gronke, Max"},{"full_name":"Schaerer, Daniel","last_name":"Schaerer","first_name":"Daniel"},{"first_name":"Rohan P","last_name":"Naidu","full_name":"Naidu, Rohan P"},{"first_name":"Huub","last_name":"Röttgering","full_name":"Röttgering, Huub"},{"full_name":"Calhau, João","last_name":"Calhau","first_name":"João"},{"last_name":"Paulino-Afonso","full_name":"Paulino-Afonso, Ana","first_name":"Ana"},{"first_name":"Sérgio","last_name":"Santos","full_name":"Santos, Sérgio"},{"last_name":"Amorín","full_name":"Amorín, Ricardo","first_name":"Ricardo"}],"abstract":[{"lang":"eng","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⊙."}],"publication_status":"published","citation":{"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>","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>.","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.","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.","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>","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.","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>."},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","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).","oa_version":"Preprint","quality_controlled":"1","_id":"11523","extern":"1","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"date_updated":"2022-08-18T10:49:00Z","volume":505,"oa":1,"article_processing_charge":"No","arxiv":1,"external_id":{"arxiv":["2102.07779"]},"title":"The X-SHOOTER Lyman α survey at z = 2 (XLS-z2) I: What makes a galaxy a Lyman α emitter?","doi":"10.1093/mnras/stab1304","year":"2021","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2102.07779"}]},{"main_file_link":[{"url":"https://doi.org/10.1093/mnras/staa622","open_access":"1"}],"title":"Elevated ionizing photon production efficiency in faint high-equivalent-width Lyman-α emitters","external_id":{"arxiv":["2002.11117"]},"doi":"10.1093/mnras/staa622","year":"2020","extern":"1","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"_id":"11531","oa_version":"Published Version","quality_controlled":"1","acknowledgement":"We would like to thank the anonymous referee for a thoughtful report and suggestions that have improved this manuscript. We are also grateful to everyone involved in the Spitzer Space Telescope mission and everyone at the Spitzer Science Center: we are truly fortunate to have been able to use data from this facility. J. B. acknowledges support by FCT/MCTES through national funds by this grant UID/FIS/04434/2019 and through the Investigador FCT contract no. IF/01654/2014/CP1215/CT0003. S. C. gratefully acknowledges support from Swiss National Science Foundation grant PP00P2 163824. We would also like to thank Mauro Stefanon for his assistance with de-blending the IRAC photometry, Pieter van Dokkum for a number of useful suggestions, and Daniel Schaerer for information regarding the stellar population models. This study is based on observations made with ESO telescopes at the La Silla Paranal Observatory under programs IDs 094.A-2089(B), 095.A0010(A), 096.A-0045(A), and 096.A-0045(B).","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","arxiv":1,"article_processing_charge":"No","date_updated":"2022-08-18T11:23:27Z","oa":1,"volume":493,"abstract":[{"lang":"eng","text":"While low-luminosity galaxies dominate number counts at all redshifts, their contribution to cosmic reionization is poorly understood due to a lack of knowledge of their physical properties. We isolate a sample of 35 z ≈ 4–5 continuum-faint Lyman-α emitters from deep VLT/MUSE spectroscopy and directly measure their H α emission using stacked Spitzer/IRAC Ch. 1 photometry. Based on Hubble Space Telescope imaging, we determine that the average UV continuum magnitude is fainter than −16 (≈ 0.01 L⋆), implying a median Lyman-α equivalent width of 259 Å. By combining the H α measurement with the UV magnitude, we determine the ionizing photon production efficiency, ξion, a first for such faint galaxies. The measurement of log10 (ξion [Hz erg−1]) = 26.28 (⁠+0.28−0.40⁠) is in excess of literature measurements of both continuum- and emission line-selected samples, implying a more efficient production of ionizing photons in these lower luminosity, Lyman-α-selected systems. We conclude that this elevated efficiency can be explained by stellar populations with metallicities between 4 × 10−4 and 0.008, with light-weighted ages less than 3 Myr."}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","Galaxies: evolution","Galaxies: high-redshift","Galaxies: ISM"],"author":[{"full_name":"Maseda, Michael V","last_name":"Maseda","first_name":"Michael V"},{"first_name":"Roland","full_name":"Bacon, Roland","last_name":"Bacon"},{"full_name":"Lam, Daniel","last_name":"Lam","first_name":"Daniel"},{"orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","last_name":"Matthee","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"first_name":"Jarle","last_name":"Brinchmann","full_name":"Brinchmann, Jarle"},{"last_name":"Schaye","full_name":"Schaye, Joop","first_name":"Joop"},{"first_name":"Ivo","last_name":"Labbe","full_name":"Labbe, Ivo"},{"first_name":"Kasper B","full_name":"Schmidt, Kasper B","last_name":"Schmidt"},{"last_name":"Boogaard","full_name":"Boogaard, Leindert","first_name":"Leindert"},{"first_name":"Rychard","full_name":"Bouwens, Rychard","last_name":"Bouwens"},{"last_name":"Cantalupo","full_name":"Cantalupo, Sebastiano","first_name":"Sebastiano"},{"first_name":"Marijn","last_name":"Franx","full_name":"Franx, Marijn"},{"full_name":"Hashimoto, Takuya","last_name":"Hashimoto","first_name":"Takuya"},{"full_name":"Inami, Hanae","last_name":"Inami","first_name":"Hanae"},{"full_name":"Kusakabe, Haruka","last_name":"Kusakabe","first_name":"Haruka"},{"full_name":"Mahler, Guillaume","last_name":"Mahler","first_name":"Guillaume"},{"first_name":"Themiya","full_name":"Nanayakkara, Themiya","last_name":"Nanayakkara"},{"last_name":"Richard","full_name":"Richard, Johan","first_name":"Johan"},{"full_name":"Wisotzki, Lutz","last_name":"Wisotzki","first_name":"Lutz"}],"citation":{"ista":"Maseda MV, Bacon R, Lam D, Matthee JJ, Brinchmann J, Schaye J, Labbe I, Schmidt KB, Boogaard L, Bouwens R, Cantalupo S, Franx M, Hashimoto T, Inami H, Kusakabe H, Mahler G, Nanayakkara T, Richard J, Wisotzki L. 2020. Elevated ionizing photon production efficiency in faint high-equivalent-width Lyman-α emitters. Monthly Notices of the Royal Astronomical Society. 493(4), 5120–5130.","short":"M.V. Maseda, R. Bacon, D. Lam, J.J. Matthee, J. Brinchmann, J. Schaye, I. Labbe, K.B. Schmidt, L. Boogaard, R. Bouwens, S. Cantalupo, M. Franx, T. Hashimoto, H. Inami, H. Kusakabe, G. Mahler, T. Nanayakkara, J. Richard, L. Wisotzki, Monthly Notices of the Royal Astronomical Society 493 (2020) 5120–5130.","mla":"Maseda, Michael V., et al. “Elevated Ionizing Photon Production Efficiency in Faint High-Equivalent-Width Lyman-α Emitters.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 493, no. 4, Oxford University Press, 2020, pp. 5120–30, doi:<a href=\"https://doi.org/10.1093/mnras/staa622\">10.1093/mnras/staa622</a>.","ama":"Maseda MV, Bacon R, Lam D, et al. Elevated ionizing photon production efficiency in faint high-equivalent-width Lyman-α emitters. <i>Monthly Notices of the Royal Astronomical Society</i>. 2020;493(4):5120-5130. doi:<a href=\"https://doi.org/10.1093/mnras/staa622\">10.1093/mnras/staa622</a>","chicago":"Maseda, Michael V, Roland Bacon, Daniel Lam, Jorryt J Matthee, Jarle Brinchmann, Joop Schaye, Ivo Labbe, et al. “Elevated Ionizing Photon Production Efficiency in Faint High-Equivalent-Width Lyman-α Emitters.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2020. <a href=\"https://doi.org/10.1093/mnras/staa622\">https://doi.org/10.1093/mnras/staa622</a>.","apa":"Maseda, M. V., Bacon, R., Lam, D., Matthee, J. J., Brinchmann, J., Schaye, J., … Wisotzki, L. (2020). Elevated ionizing photon production efficiency in faint high-equivalent-width Lyman-α emitters. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staa622\">https://doi.org/10.1093/mnras/staa622</a>","ieee":"M. V. Maseda <i>et al.</i>, “Elevated ionizing photon production efficiency in faint high-equivalent-width Lyman-α emitters,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 493, no. 4. Oxford University Press, pp. 5120–5130, 2020."},"publication_status":"published","date_created":"2022-07-07T10:46:41Z","scopus_import":"1","publisher":"Oxford University Press","language":[{"iso":"eng"}],"month":"04","article_type":"original","date_published":"2020-04-01T00:00:00Z","publication":"Monthly Notices of the Royal Astronomical Society","issue":"4","page":"5120-5130","intvolume":"       493","status":"public","day":"01","type":"journal_article"},{"publication":"Astronomy & Astrophysics","day":"16","type":"journal_article","intvolume":"       648","status":"public","date_created":"2022-07-06T09:07:06Z","month":"04","date_published":"2019-04-16T00:00:00Z","article_type":"original","scopus_import":"1","publisher":"EDP Sciences","language":[{"iso":"eng"}],"arxiv":1,"article_processing_charge":"No","volume":648,"oa":1,"date_updated":"2022-07-19T09:36:08Z","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"extern":"1","_id":"11499","oa_version":"Published Version","quality_controlled":"1","acknowledgement":"The authors wish to thank the referee for constructive comments that improved the paper substantially. We thank the BPASS team for making the stellar population models available. We thank Elizabeth Stanway, Claus Leitherer, Daniel Schaerer, Jorick Vink, and Nell Byler for insightful discussions. We thank the Lorentz Centre and the scientific organizers of the Characterizing galaxies with spectroscopy with a view for JWST workshop held at the Lorentz Centre in 2017 October, which promoted useful discussions in the wider community. TN, JB, and RB acknowledges the Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO) top grant TOP1.16.057. AF acknowledges support from the ERC via an Advanced Grant under grant agreement no. 339659-MUSICOS. JB acknowledges support by Fundação para a Ciência e a Tecnologia (FCT) through national funds (UID/FIS/04434/2013) and Investigador FCT contract IF/01654/2014/CP1215/CT0003, and by FEDER through COMPETE2020 (POCI-01-0145-FEDER-007672). JR acknowledges support from the ERC Starting grant 336736 (CALENDS). This research made use of astropy (http://www.astropy.org) a community-developed core Python package for Astronomy (Astropy Collaboration 2013, 2018) and pandas (McKinney 2010). Figures were generated using matplotlib (Hunter 2007) and seaborn (https://seaborn.pydata.org). Facilities: VLT (MUSE).","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"short":"T. Nanayakkara, J. Brinchmann, L. Boogaard, R. Bouwens, S. Cantalupo, A. Feltre, W. Kollatschny, R.A. Marino, M. Maseda, J.J. Matthee, M. Paalvast, J. Richard, A. Verhamme, Astronomy &#38; Astrophysics 648 (2019).","ista":"Nanayakkara T, Brinchmann J, Boogaard L, Bouwens R, Cantalupo S, Feltre A, Kollatschny W, Marino RA, Maseda M, Matthee JJ, Paalvast M, Richard J, Verhamme A. 2019. Exploring He II λ1640 emission line properties at z ∼2−4. Astronomy &#38; Astrophysics. 648, A89.","ama":"Nanayakkara T, Brinchmann J, Boogaard L, et al. Exploring He II λ1640 emission line properties at z ∼2−4. <i>Astronomy &#38; Astrophysics</i>. 2019;648. doi:<a href=\"https://doi.org/10.1051/0004-6361/201834565\">10.1051/0004-6361/201834565</a>","mla":"Nanayakkara, Themiya, et al. “Exploring He II Λ1640 Emission Line Properties at z ∼2−4.” <i>Astronomy &#38; Astrophysics</i>, vol. 648, A89, EDP Sciences, 2019, doi:<a href=\"https://doi.org/10.1051/0004-6361/201834565\">10.1051/0004-6361/201834565</a>.","chicago":"Nanayakkara, Themiya, Jarle Brinchmann, Leindert Boogaard, Rychard Bouwens, Sebastiano Cantalupo, Anna Feltre, Wolfram Kollatschny, et al. “Exploring He II Λ1640 Emission Line Properties at z ∼2−4.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2019. <a href=\"https://doi.org/10.1051/0004-6361/201834565\">https://doi.org/10.1051/0004-6361/201834565</a>.","ieee":"T. Nanayakkara <i>et al.</i>, “Exploring He II λ1640 emission line properties at z ∼2−4,” <i>Astronomy &#38; Astrophysics</i>, vol. 648. EDP Sciences, 2019.","apa":"Nanayakkara, T., Brinchmann, J., Boogaard, L., Bouwens, R., Cantalupo, S., Feltre, A., … Verhamme, A. (2019). Exploring He II λ1640 emission line properties at z ∼2−4. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201834565\">https://doi.org/10.1051/0004-6361/201834565</a>"},"publication_status":"published","abstract":[{"lang":"eng","text":"Deep optical spectroscopic surveys of galaxies provide a unique opportunity to investigate rest-frame ultra-violet (UV) emission line properties of galaxies at z ∼ 2 − 4.5. Here we combine VLT/MUSE Guaranteed Time Observations of the Hubble Deep Field South, Ultra Deep Field, COSMOS, and several quasar fields with other publicly available data from VLT/VIMOS and VLT/FORS2 to construct a catalogue of He II λ1640 emitters at z ≳ 2. The deepest areas of our MUSE pointings reach a 3σ line flux limit of 3.1 × 10−19 erg s−1 cm−2. After discarding broad-line active galactic nuclei, we find 13 He II λ1640 detections from MUSE with a median MUV = −20.1 and 21 tentative He II λ1640 detections from other public surveys. Excluding Lyα, all except two galaxies in our sample show at least one other rest-UV emission line, with C III] λ1907, λ1909 being the most prominent. We use multi-wavelength data available in the Hubble legacy fields to derive basic galaxy properties of our sample through spectral energy distribution fitting techniques. Taking advantage of the high-quality spectra obtained by MUSE (∼10 − 30 h of exposure time per pointing), we use photo-ionisation models to study the rest-UV emission line diagnostics of the He II λ1640 emitters. Line ratios of our sample can be reproduced by moderately sub-solar photo-ionisation models, however, we find that including effects of binary stars lead to degeneracies in most free parameters. Even after considering extra ionising photons produced by extreme sub-solar metallicity binary stellar models, photo-ionisation models are unable to reproduce rest-frame He II λ1640 equivalent widths (∼0.2 − 10 Å), thus additional mechanisms are necessary in models to match the observed He II λ1640 properties."}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: ISM / galaxies: star formation / galaxies: evolution / galaxies: high-redshift"],"author":[{"first_name":"Themiya","last_name":"Nanayakkara","full_name":"Nanayakkara, Themiya"},{"first_name":"Jarle","last_name":"Brinchmann","full_name":"Brinchmann, Jarle"},{"last_name":"Boogaard","full_name":"Boogaard, Leindert","first_name":"Leindert"},{"first_name":"Rychard","full_name":"Bouwens, Rychard","last_name":"Bouwens"},{"first_name":"Sebastiano","full_name":"Cantalupo, Sebastiano","last_name":"Cantalupo"},{"first_name":"Anna","last_name":"Feltre","full_name":"Feltre, Anna"},{"first_name":"Wolfram","full_name":"Kollatschny, Wolfram","last_name":"Kollatschny"},{"first_name":"Raffaella Anna","full_name":"Marino, Raffaella Anna","last_name":"Marino"},{"first_name":"Michael","full_name":"Maseda, Michael","last_name":"Maseda"},{"first_name":"Jorryt J","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"full_name":"Paalvast, Mieke","last_name":"Paalvast","first_name":"Mieke"},{"first_name":"Johan","full_name":"Richard, Johan","last_name":"Richard"},{"first_name":"Anne","last_name":"Verhamme","full_name":"Verhamme, Anne"}],"article_number":"A89","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1902.05960"}],"related_material":{"link":[{"relation":"erratum","url":"https://doi.org/10.1051/0004-6361/201834565e"}]},"doi":"10.1051/0004-6361/201834565","year":"2019","title":"Exploring He II λ1640 emission line properties at z ∼2−4","external_id":{"arxiv":["1902.05960"]}},{"doi":"10.1051/0004-6361/201833075","year":"2019","title":"Predicting Lyα escape fractions with a simple observable: Lyα in emission as an empirically calibrated star formation rate indicator","external_id":{"arxiv":["1803.08923"]},"article_number":"A157","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1803.08923"}],"publication_status":"published","citation":{"chicago":"Sobral, David, and Jorryt J Matthee. “Predicting Lyα Escape Fractions with a Simple Observable: Lyα in Emission as an Empirically Calibrated Star Formation Rate Indicator.” <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>.","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.","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.","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>.","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>"},"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"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift / galaxies: star formation / galaxies: statistics / galaxies: evolution / galaxies: formation / galaxies: ISM"],"author":[{"first_name":"David","last_name":"Sobral","full_name":"Sobral, David"},{"first_name":"Jorryt J","full_name":"Matthee, Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720"}],"arxiv":1,"date_updated":"2022-07-19T09:37:20Z","volume":623,"oa":1,"article_processing_charge":"No","_id":"11507","extern":"1","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"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.","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa_version":"Published Version","quality_controlled":"1","month":"03","date_published":"2019-03-26T00:00:00Z","article_type":"original","publisher":"EDP Sciences","scopus_import":"1","language":[{"iso":"eng"}],"date_created":"2022-07-06T11:08:16Z","day":"26","type":"journal_article","intvolume":"       623","status":"public","publication":"Astronomy & Astrophysics"},{"publication_status":"published","citation":{"chicago":"Sobral, David, Jorryt J Matthee, Gabriel Brammer, Andrea Ferrara, Lara Alegre, Huub Röttgering, Daniel Schaerer, Bahram Mobasher, and Behnam Darvish. “On the Nature and Physical Conditions of the Luminous Ly α Emitter CR7 and Its Rest-Frame UV Components.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2019. <a href=\"https://doi.org/10.1093/mnras/sty2779\">https://doi.org/10.1093/mnras/sty2779</a>.","ieee":"D. Sobral <i>et al.</i>, “On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 482, no. 2. Oxford University Press, pp. 2422–2441, 2019.","apa":"Sobral, D., Matthee, J. J., Brammer, G., Ferrara, A., Alegre, L., Röttgering, H., … Darvish, B. (2019). On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/sty2779\">https://doi.org/10.1093/mnras/sty2779</a>","ista":"Sobral D, Matthee JJ, Brammer G, Ferrara A, Alegre L, Röttgering H, Schaerer D, Mobasher B, Darvish B. 2019. On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components. Monthly Notices of the Royal Astronomical Society. 482(2), 2422–2441.","short":"D. Sobral, J.J. Matthee, G. Brammer, A. Ferrara, L. Alegre, H. Röttgering, D. Schaerer, B. Mobasher, B. Darvish, Monthly Notices of the Royal Astronomical Society 482 (2019) 2422–2441.","ama":"Sobral D, Matthee JJ, Brammer G, et al. On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components. <i>Monthly Notices of the Royal Astronomical Society</i>. 2019;482(2):2422-2441. doi:<a href=\"https://doi.org/10.1093/mnras/sty2779\">10.1093/mnras/sty2779</a>","mla":"Sobral, David, et al. “On the Nature and Physical Conditions of the Luminous Ly α Emitter CR7 and Its Rest-Frame UV Components.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 482, no. 2, Oxford University Press, 2019, pp. 2422–41, doi:<a href=\"https://doi.org/10.1093/mnras/sty2779\">10.1093/mnras/sty2779</a>."},"abstract":[{"lang":"eng","text":"We present new Hubble Space Telescope (HST)/WFC3 observations and re-analyse VLT data to unveil the continuum, variability, and rest-frame ultraviolet (UV) lines of the multiple UV clumps of the most luminous Lyα emitter at z = 6.6, CR7 (COSMOS Redshift 7). Our re-reduced, flux-calibrated X-SHOOTER spectra of CR7 reveal an He II emission line in observations obtained along the major axis of Lyα emission with the best seeing conditions. He II is spatially offset by ≈+0.8 arcsec from the peak of Lyα emission, and it is found towards clump B. Our WFC3 grism spectra detects the UV continuum of CR7’s clump A, yielding a power law with β=−2.5+0.6−0.7 and MUV=−21.87+0.25−0.20⁠. No significant variability is found for any of the UV clumps on their own, but there is tentative (≈2.2 σ) brightening of CR7 in F110W as a whole from 2012 to 2017. HST grism data fail to robustly detect rest-frame UV lines in any of the clumps, implying fluxes ≲2×10−17 erg s−1 cm−2 (3σ). We perform CLOUDY modelling to constrain the metallicity and the ionizing nature of CR7. CR7 seems to be actively forming stars without any clear active galactic nucleus activity in clump A, consistent with a metallicity of ∼0.05–0.2 Z⊙. Component C or an interclump component between B and C may host a high ionization source. Our results highlight the need for spatially resolved information to study the formation and assembly of early galaxies."}],"author":[{"full_name":"Sobral, David","last_name":"Sobral","first_name":"David"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X"},{"full_name":"Brammer, Gabriel","last_name":"Brammer","first_name":"Gabriel"},{"full_name":"Ferrara, Andrea","last_name":"Ferrara","first_name":"Andrea"},{"first_name":"Lara","last_name":"Alegre","full_name":"Alegre, Lara"},{"full_name":"Röttgering, Huub","last_name":"Röttgering","first_name":"Huub"},{"first_name":"Daniel","full_name":"Schaerer, Daniel","last_name":"Schaerer"},{"last_name":"Mobasher","full_name":"Mobasher, Bahram","first_name":"Bahram"},{"full_name":"Darvish, Behnam","last_name":"Darvish","first_name":"Behnam"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","galaxies: ISM","cosmology: observations","dark ages","reionization","first stars","early Universe"],"arxiv":1,"oa":1,"volume":482,"date_updated":"2022-08-19T06:49:36Z","article_processing_charge":"No","_id":"11541","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"extern":"1","acknowledgement":"We thank the anonymous reviewer for the numerous detailed comments that led us to greatly improve the quality, extent, and statistical robustness of this work. DS acknowledges financial support from the Netherlands Organisation for Scientific research through a Veni fellowship. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. AF acknowledges support from the ERC Advanced Grant INTERSTELLAR H2020/740120. BD acknowledges financial support from NASA through the Astrophysics Data Analysis Program, grant number NNX12AE20G and the National Science Foundation, grant number 1716907. We are thankful for several discussions and constructive comments from Johannes Zabl, Eros Vanzella, Bo Milvang-Jensen, Henry McCracken, Max Gronke, Mark Dijkstra, Richard Ellis, and Nicolas Laporte. We also thank Umar Burhanudin and Izzy Garland for taking part in the XGAL internship in Lancaster and for exploring the HST grism data independently. Based on observations obtained with HST/WFC3 programs 12578, 14495, and 14596. Based on observations of the National Japanese Observatory with the Suprime-Cam on the Subaru telescope (S14A-086) on the big island of Hawaii. This work is based in part on data products produced at TERAPIX available at the Canadian Astronomy Data Centre as part of the Canada–France–Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme IDs 294.A-5018, 294.A-5039, 092.A 0786, 093.A-0561, 097.A0043, 097.A-0943, 098.A-0819, 298.A-5012, and 179.A-2005, and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. The authors acknowledge the award of service time (SW2014b20) on the William Herschel Telescope (WHT). WHT and its service programme are operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. This research was supported by the Munich Institute for Astro- and Particle Physics of the DFG cluster of excellence ‘Origin and Structure of the Universe’. We have benefitted immensely from the public available programming language PYTHON, including NUMPY and SCIPY (Jones et al. 2001; Van Der Walt, Colbert & Varoquaux 2011), MATPLOTLIB (Hunter 2007), ASTROPY (Astropy Collaboration et al. 2013), and the TOPCAT analysis program (Taylor 2013). This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France. All data used for this paper are publicly available, and we make all reduced data available with the refereed paper.","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","quality_controlled":"1","oa_version":"Preprint","year":"2019","doi":"10.1093/mnras/sty2779","title":"On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components","external_id":{"arxiv":["1710.08422"]},"main_file_link":[{"url":"https://arxiv.org/abs/1710.08422","open_access":"1"}],"day":"01","type":"journal_article","intvolume":"       482","status":"public","issue":"2","publication":"Monthly Notices of the Royal Astronomical Society","page":"2422-2441","month":"01","date_published":"2019-01-01T00:00:00Z","article_type":"original","publisher":"Oxford University Press","scopus_import":"1","language":[{"iso":"eng"}],"date_created":"2022-07-08T10:40:05Z"},{"page":"1170-1184","publication":"Monthly Notices of the Royal Astronomical Society","issue":"1","type":"journal_article","day":"01","status":"public","intvolume":"       478","date_created":"2022-07-11T08:05:42Z","article_type":"original","date_published":"2018-07-01T00:00:00Z","month":"07","language":[{"iso":"eng"}],"scopus_import":"1","publisher":"Oxford University Press","article_processing_charge":"No","date_updated":"2022-08-19T06:58:06Z","volume":478,"oa":1,"arxiv":1,"quality_controlled":"1","oa_version":"Preprint","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","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_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"_id":"11555","citation":{"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>","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>.","short":"S. Carniani, R. Maiolino, R. Amorin, L. Pentericci, A. Pallottini, A. Ferrara, C.J. Willott, R. Smit, J.J. Matthee, D. Sobral, P. Santini, M. Castellano, S. De Barros, A. Fontana, A. Grazian, L. Guaita, Monthly Notices of the Royal Astronomical Society 478 (2018) 1170–1184.","ista":"Carniani S, Maiolino R, Amorin R, Pentericci L, Pallottini A, Ferrara A, Willott CJ, Smit R, Matthee JJ, Sobral D, Santini P, Castellano M, De Barros S, Fontana A, Grazian A, Guaita L. 2018. Kiloparsec-scale gaseous clumps and star formation at z = 5–7. Monthly Notices of the Royal Astronomical Society. 478(1), 1170–1184.","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>","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>."},"publication_status":"published","author":[{"first_name":"S","full_name":"Carniani, S","last_name":"Carniani"},{"first_name":"R","full_name":"Maiolino, R","last_name":"Maiolino"},{"first_name":"R","last_name":"Amorin","full_name":"Amorin, R"},{"first_name":"L","full_name":"Pentericci, L","last_name":"Pentericci"},{"full_name":"Pallottini, A","last_name":"Pallottini","first_name":"A"},{"full_name":"Ferrara, A","last_name":"Ferrara","first_name":"A"},{"last_name":"Willott","full_name":"Willott, C J","first_name":"C J"},{"first_name":"R","full_name":"Smit, R","last_name":"Smit"},{"first_name":"Jorryt J","last_name":"Matthee","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"first_name":"D","full_name":"Sobral, D","last_name":"Sobral"},{"full_name":"Santini, P","last_name":"Santini","first_name":"P"},{"full_name":"Castellano, M","last_name":"Castellano","first_name":"M"},{"first_name":"S","last_name":"De Barros","full_name":"De Barros, S"},{"last_name":"Fontana","full_name":"Fontana, A","first_name":"A"},{"first_name":"A","last_name":"Grazian","full_name":"Grazian, A"},{"last_name":"Guaita","full_name":"Guaita, L","first_name":"L"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","galaxies: ISM","galaxies: formation"],"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"}],"main_file_link":[{"url":"https://arxiv.org/abs/1712.03985","open_access":"1"}],"doi":"10.1093/mnras/sty1088","year":"2018","external_id":{"arxiv":["1712.03985"]},"title":"Kiloparsec-scale gaseous clumps and star formation at z = 5–7"},{"scopus_import":"1","publisher":"Oxford University Press","language":[{"iso":"eng"}],"month":"06","article_type":"original","date_published":"2018-06-01T00:00:00Z","date_created":"2022-07-12T07:18:02Z","intvolume":"       477","status":"public","day":"01","type":"journal_article","publication":"Monthly Notices of the Royal Astronomical Society","issue":"2","page":"2817-2840","title":"The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN","external_id":{"arxiv":["1802.10102"]},"year":"2018","doi":"10.1093/mnras/sty782","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1802.10102"}],"abstract":[{"text":"Deep narrow-band surveys have revealed a large population of faint Ly α emitters (LAEs) in the distant Universe, but relatively little is known about the most luminous sources (⁠LLyα≳1042.7 erg s−1; LLyα≳L∗Lyα⁠). Here we present the spectroscopic follow-up of 21 luminous LAEs at z ∼ 2–3 found with panoramic narrow-band surveys over five independent extragalactic fields (≈4 × 106 Mpc3 surveyed at z ∼ 2.2 and z ∼ 3.1). We use WHT/ISIS, Keck/DEIMOS, and VLT/X-SHOOTER to study these sources using high ionization UV lines. Luminous LAEs at z ∼ 2–3 have blue UV slopes (⁠β=−2.0+0.3−0.1⁠) and high Ly α escape fractions (⁠50+20−15 per cent) and span five orders of magnitude in UV luminosity (MUV ≈ −19 to −24). Many (70 per cent) show at least one high ionization rest-frame UV line such as C IV, N V, C III], He II or O III], typically blue-shifted by ≈100–200 km s−1 relative to Ly α. Their Ly α profiles reveal a wide variety of shapes, including significant blue-shifted components and widths from 200 to 4000 km s−1. Overall, 60 ± 11  per cent appear to be active galactic nucleus (AGN) dominated, and at LLyα > 1043.3 erg s−1 and/or MUV < −21.5 virtually all LAEs are AGNs with high ionization parameters (log U = 0.6 ± 0.5) and with metallicities of ≈0.5 − 1 Z⊙. Those lacking signatures of AGNs (40 ± 11  per cent) have lower ionization parameters (⁠logU=−3.0+1.6−0.9 and log ξion = 25.4 ± 0.2) and are apparently metal-poor sources likely powered by young, dust-poor ‘maximal’ starbursts. Our results show that luminous LAEs at z ∼ 2–3 are a diverse population and that 2×L∗Lyα and 2×M∗UV mark a sharp transition in the nature of LAEs, from star formation dominated to AGN dominated.","lang":"eng"}],"author":[{"full_name":"Sobral, David","last_name":"Sobral","first_name":"David"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J"},{"last_name":"Darvish","full_name":"Darvish, Behnam","first_name":"Behnam"},{"first_name":"Ian","last_name":"Smail","full_name":"Smail, Ian"},{"full_name":"Best, Philip N","last_name":"Best","first_name":"Philip N"},{"last_name":"Alegre","full_name":"Alegre, Lara","first_name":"Lara"},{"first_name":"Huub","full_name":"Röttgering, Huub","last_name":"Röttgering"},{"first_name":"Bahram","last_name":"Mobasher","full_name":"Mobasher, Bahram"},{"first_name":"Ana","full_name":"Paulino-Afonso, Ana","last_name":"Paulino-Afonso"},{"first_name":"Andra","last_name":"Stroe","full_name":"Stroe, Andra"},{"full_name":"Oteo, Iván","last_name":"Oteo","first_name":"Iván"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: active","galaxies: evolution","galaxies: high-redshift","galaxies: ISM","galaxies: starburst","cosmology: observations"],"citation":{"short":"D. Sobral, J.J. Matthee, B. Darvish, I. Smail, P.N. Best, L. Alegre, H. Röttgering, B. Mobasher, A. Paulino-Afonso, A. Stroe, I. Oteo, Monthly Notices of the Royal Astronomical Society 477 (2018) 2817–2840.","ista":"Sobral D, Matthee JJ, Darvish B, Smail I, Best PN, Alegre L, Röttgering H, Mobasher B, Paulino-Afonso A, Stroe A, Oteo I. 2018. The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN. Monthly Notices of the Royal Astronomical Society. 477(2), 2817–2840.","mla":"Sobral, David, et al. “The Nature of Luminous Ly α Emitters at z ∼ 2–3: Maximal Dust-Poor Starbursts and Highly Ionizing AGN.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 477, no. 2, Oxford University Press, 2018, pp. 2817–40, doi:<a href=\"https://doi.org/10.1093/mnras/sty782\">10.1093/mnras/sty782</a>.","ama":"Sobral D, Matthee JJ, Darvish B, et al. The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN. <i>Monthly Notices of the Royal Astronomical Society</i>. 2018;477(2):2817-2840. doi:<a href=\"https://doi.org/10.1093/mnras/sty782\">10.1093/mnras/sty782</a>","chicago":"Sobral, David, Jorryt J Matthee, Behnam Darvish, Ian Smail, Philip N Best, Lara Alegre, Huub Röttgering, et al. “The Nature of Luminous Ly α Emitters at z ∼ 2–3: Maximal Dust-Poor Starbursts and Highly Ionizing AGN.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2018. <a href=\"https://doi.org/10.1093/mnras/sty782\">https://doi.org/10.1093/mnras/sty782</a>.","apa":"Sobral, D., Matthee, J. J., Darvish, B., Smail, I., Best, P. N., Alegre, L., … Oteo, I. (2018). The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/sty782\">https://doi.org/10.1093/mnras/sty782</a>","ieee":"D. Sobral <i>et al.</i>, “The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 477, no. 2. Oxford University Press, pp. 2817–2840, 2018."},"publication_status":"published","extern":"1","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"_id":"11557","quality_controlled":"1","oa_version":"Preprint","acknowledgement":"We thank the anonymous reviewer for their timely and constructive comments that greatly helped us to improve the manuscript. DS acknowledges financial support from the Netherlands Organization for Scientific research (NWO) through a Veni fellowship and from Lancaster University through an Early Career Internal Grant A100679. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. BD acknowledges financial support from NASA through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G, and the National Science Foundation, grant number 1716907. IRS acknowledges support from the ERC Advanced Grant DUSTYGAL (321334), STFC (ST/P000541/1), and a Royal Society/Wolfson Merit Award. PNB is grateful for support from STFC via grant ST/M001229/1. We thank Anne Verhamme, Kimihiko Nakajima, Ryan Trainor, Sangeeta Malhotra, Max Gronke, James Rhoads, Fang Xia An, Matthew Hayes, Takashi Kojima, Mark Dijkstra, and Anne Jaskot for many helpful and engaging discussions, particularly during the SnowCLAW Ly α workshop. We thank Bruno Ribeiro, Stephane Charlot, and Joseph Caruana for comments on the manuscript. The authors would also like to thank Ingrid Tengs, Meg Singleton, Ali Khostovan, and Sara Perez for participating in part of the observations. We also thank Joao Calhau, Leah Morabito, Sergio Santos, and Aayush Saxena for their assistance with the narrow-band observations which allowed to select some of the sour ces. Based on observations obtained with the William Herschel Telescope, program: W16AN004; the Very Large Telescope, programs: 098.A-0819 & 099.A-0254; and the Keck II telescope, program: C267D. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme IDs 294.A-5018, 294.A-5039, 092.A-0786, 093.A-0561, 097.A-0943, 098.A-0819, 099.A-0254 and 179.A-2005. The authors acknowledge the award of service time (SW2014b20) on the WHT. WHT and its service programme are operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. The authors would also like to thank all the extremely helpful observatory staff that have greatly contributed towards our observations, particularly Fiona Riddick, Lilian Dominguez, Florencia Jimenez, and Ian Skillen. We have benefited greatly from the publicly available programming language PYTHON, including the NUMPY & SCIPY (Van Der Walt, Colbert & Varoquaux 2011; Jones et al. 2001), MATPLOTLIB (Hunter 2007), ASTROPY (Astropy Collaboration et al. 2013), and the TOPCAT analysis program (Taylor 2013). This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France.","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","arxiv":1,"article_processing_charge":"No","oa":1,"volume":477,"date_updated":"2022-08-19T07:01:08Z"},{"doi":"10.3847/1538-4357/aa9931","year":"2017","external_id":{"arxiv":["1709.06569"]},"title":"ALMA reveals metals yet no dust within multiple components in CR7","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1709.06569"}],"article_number":"145","citation":{"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>.","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>","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).","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.","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>.","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>"},"publication_status":"published","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"}],"author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","first_name":"Jorryt J"},{"full_name":"Sobral, D.","last_name":"Sobral","first_name":"D."},{"full_name":"Boone, F.","last_name":"Boone","first_name":"F."},{"first_name":"H.","full_name":"Röttgering, H.","last_name":"Röttgering"},{"first_name":"D.","full_name":"Schaerer, D.","last_name":"Schaerer"},{"last_name":"Girard","full_name":"Girard, M.","first_name":"M."},{"last_name":"Pallottini","full_name":"Pallottini, A.","first_name":"A."},{"first_name":"L.","full_name":"Vallini, L.","last_name":"Vallini"},{"last_name":"Ferrara","full_name":"Ferrara, A.","first_name":"A."},{"first_name":"B.","full_name":"Darvish, B.","last_name":"Darvish"},{"first_name":"B.","last_name":"Mobasher","full_name":"Mobasher, B."}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","dark ages","reionization","first stars – galaxies: formation – galaxies: high-redshift – galaxies: ISM – galaxies: kinematics and dynamics"],"arxiv":1,"article_processing_charge":"No","oa":1,"date_updated":"2022-08-18T10:23:35Z","volume":851,"extern":"1","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"_id":"11518","oa_version":"Preprint","quality_controlled":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","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.","month":"12","date_published":"2017-12-21T00:00:00Z","article_type":"original","scopus_import":"1","publisher":"IOP Publishing","language":[{"iso":"eng"}],"date_created":"2022-07-07T08:48:04Z","day":"21","type":"journal_article","intvolume":"       851","status":"public","publication":"The Astrophysical Journal","issue":"2"},{"_id":"11575","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"extern":"1","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.","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa_version":"Preprint","quality_controlled":"1","arxiv":1,"oa":1,"volume":459,"date_updated":"2022-08-19T08:12:07Z","article_processing_charge":"No","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."}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics  stars: formation","ISM: evolution","galaxies: evolution","galaxies: formation","galaxies: ISM"],"author":[{"last_name":"Lagos","full_name":"Lagos, Claudia del P.","first_name":"Claudia del P."},{"first_name":"Tom","last_name":"Theuns","full_name":"Theuns, Tom"},{"full_name":"Schaye, Joop","last_name":"Schaye","first_name":"Joop"},{"first_name":"Michelle","full_name":"Furlong, Michelle","last_name":"Furlong"},{"full_name":"Bower, Richard G.","last_name":"Bower","first_name":"Richard G."},{"first_name":"Matthieu","full_name":"Schaller, Matthieu","last_name":"Schaller"},{"last_name":"Crain","full_name":"Crain, Robert A.","first_name":"Robert A."},{"first_name":"James W.","last_name":"Trayford","full_name":"Trayford, James W."},{"orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"}],"publication_status":"published","citation":{"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>.","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>","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.","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>","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>."},"main_file_link":[{"url":"https://arxiv.org/abs/1510.08067","open_access":"1"}],"external_id":{"arxiv":["1510.08067"]},"title":"The Fundamental Plane of star formation in galaxies revealed by the EAGLE hydrodynamical simulations","year":"2016","doi":"10.1093/mnras/stw717","issue":"3","publication":"Monthly Notices of the Royal Astronomical Society","page":"2632-2650","intvolume":"       459","status":"public","day":"01","type":"journal_article","date_created":"2022-07-13T10:21:24Z","publisher":"Oxford University Press","scopus_import":"1","language":[{"iso":"eng"}],"month":"07","article_type":"original","date_published":"2016-07-01T00:00:00Z"},{"doi":"10.1093/mnras/stw322","year":"2016","external_id":{"arxiv":["1602.02756"]},"title":"The CALYMHA survey: Lyα escape fraction and its dependence on galaxy properties at z = 2.23","main_file_link":[{"url":"https://arxiv.org/abs/1602.02756","open_access":"1"}],"publication_status":"published","citation":{"chicago":"Matthee, Jorryt J, David Sobral, Iván Oteo, Philip Best, Ian Smail, Huub Röttgering, and Ana Paulino-Afonso. “The CALYMHA Survey: Lyα Escape Fraction and Its Dependence on Galaxy Properties at z = 2.23.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2016. <a href=\"https://doi.org/10.1093/mnras/stw322\">https://doi.org/10.1093/mnras/stw322</a>.","ieee":"J. J. Matthee <i>et al.</i>, “The CALYMHA survey: Lyα escape fraction and its dependence on galaxy properties at z = 2.23,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 458, no. 1. Oxford University Press, pp. 449–467, 2016.","apa":"Matthee, J. J., Sobral, D., Oteo, I., Best, P., Smail, I., Röttgering, H., &#38; Paulino-Afonso, A. (2016). The CALYMHA survey: Lyα escape fraction and its dependence on galaxy properties at z = 2.23. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stw322\">https://doi.org/10.1093/mnras/stw322</a>","short":"J.J. Matthee, D. Sobral, I. Oteo, P. Best, I. Smail, H. Röttgering, A. Paulino-Afonso, Monthly Notices of the Royal Astronomical Society 458 (2016) 449–467.","ista":"Matthee JJ, Sobral D, Oteo I, Best P, Smail I, Röttgering H, Paulino-Afonso A. 2016. The CALYMHA survey: Lyα escape fraction and its dependence on galaxy properties at z = 2.23. Monthly Notices of the Royal Astronomical Society. 458(1), 449–467.","ama":"Matthee JJ, Sobral D, Oteo I, et al. The CALYMHA survey: Lyα escape fraction and its dependence on galaxy properties at z = 2.23. <i>Monthly Notices of the Royal Astronomical Society</i>. 2016;458(1):449-467. doi:<a href=\"https://doi.org/10.1093/mnras/stw322\">10.1093/mnras/stw322</a>","mla":"Matthee, Jorryt J., et al. “The CALYMHA Survey: Lyα Escape Fraction and Its Dependence on Galaxy Properties at z = 2.23.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 458, no. 1, Oxford University Press, 2016, pp. 449–67, doi:<a href=\"https://doi.org/10.1093/mnras/stw322\">10.1093/mnras/stw322</a>."},"author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","first_name":"Jorryt J"},{"last_name":"Sobral","full_name":"Sobral, David","first_name":"David"},{"first_name":"Iván","last_name":"Oteo","full_name":"Oteo, Iván"},{"first_name":"Philip","full_name":"Best, Philip","last_name":"Best"},{"first_name":"Ian","last_name":"Smail","full_name":"Smail, Ian"},{"first_name":"Huub","last_name":"Röttgering","full_name":"Röttgering, Huub"},{"full_name":"Paulino-Afonso, Ana","last_name":"Paulino-Afonso","first_name":"Ana"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","galaxies: ISM"],"abstract":[{"lang":"eng","text":"We present the first results from our CAlibrating LYMan α with Hα (CALYMHA) pilot survey at the Isaac Newton Telescope. We measure Lyα emission for 488 Hα selected galaxies at z = 2.23 from High-z Emission Line Survey in the COSMOS and UDS fields with a specially designed narrow-band filter (λc = 3918 Å, Δλ = 52 Å). We find 17 dual Hα-Lyα emitters [fLyα > 5 × 10−17 erg s−1 cm−2, of which five are X-ray active galactic nuclei (AGN)]. For star-forming galaxies, we find a range of Lyα escape fractions (fesc, measured with 3 arcsec apertures) from 2 to 30 per cent. These galaxies have masses from 3 × 108 M⊙ to 1011 M⊙ and dust attenuations E(B − V) = 0–0.5. Using stacking, we measure a median escape fraction of 1.6 ± 0.5 per cent (4.0 ± 1.0 per cent without correcting Hα for dust), but show that this depends on galaxy properties. The stacked fesc tends to decrease with increasing star formation rate and dust attenuation. However, at the highest masses and dust attenuations, we detect individual galaxies with fesc much higher than the typical values from stacking, indicating significant scatter in the values of fesc. Relations between fesc and UV slope are bimodal, with high fesc for either the bluest or reddest galaxies. We speculate that this bimodality and large scatter in the values of fesc is due to additional physical mechanisms such as outflows facilitating fesc for dusty/massive systems. Lyα is significantly more extended than Hα and the UV. fesc continues to increase up to at least 20 kpc (3σ, 40 kpc [2σ]) for typical star-forming galaxies and thus the aperture is the most important predictor of fesc."}],"volume":458,"oa":1,"date_updated":"2022-08-19T08:17:19Z","article_processing_charge":"No","arxiv":1,"acknowledgement":"We thank the anonymous referee for constructive comments and suggestions which have improved the quality of this work. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. DS and JM acknowledge financial support from the Netherlands Organization for Scientific research (NWO) through a Veni fellowship, and DS from FCT through a FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010) and from FCT grant PEst-OE/FIS/UI2751/2014. IO acknowledges support from the European Research Council (ERC) in the form of Advanced Investigator Programme, COSMICISM, 321302. HR acknowledges support from the ERC Advanced Investigator programme NewClusters 321271. IRS acknowledges support from STFC (ST/L00075X/1), the ERC Advanced Investigator programme DUSTYGAL 321334 and a Royal Society/Wolfson Merit Award. APA acknowledges support from the Fundac¸ao para a Ciencia e para a Tecnologia (FCT) through the Fellowship SFRH/BD/52706/2014.\r\nBased on observations made with the Isaac Newton Telescope (proposals 2013AN002, 2013BN008, 2014AC88, 2014AN002, 2014BN006, 2014BC118) 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 Astrof´ısica de Canarias. We acknowledge the tremendous work that has been done by both COSMOS and UKIDSS UDS/SXDF teams in assembling such large, state-ofthe-art multi-wavelength data sets over such wide areas, as those have been crucial for the results presented in this paper. The sample of HAEs is publicly available from Sobral et al. (2013).\r\nWe have benefited greatly from the publically available programming language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY (Jones et al. 2001; Hunter 2007; Van Der Walt, Colbert & Varoquaux 2011) and ASTROPY (Astropy Collaboration et al. 2013) packages, the imaging tools SEXTRACTOR, SWARP and SCAMP (Bertin & Arnouts 1996; Bertin 2006, 2010) and the TOPCAT analysis program (Taylor 2005).","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","quality_controlled":"1","oa_version":"Preprint","_id":"11578","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"extern":"1","date_published":"2016-05-01T00:00:00Z","article_type":"original","month":"05","language":[{"iso":"eng"}],"publisher":"Oxford University Press","scopus_import":"1","date_created":"2022-07-14T08:51:37Z","type":"journal_article","day":"01","status":"public","intvolume":"       458","page":"449-467","issue":"1","publication":"Monthly Notices of the Royal Astronomical Society"}]