[{"article_type":"original","year":"2022","oa_version":"Preprint","scopus_import":"1","external_id":{"arxiv":["2110.11967"]},"date_updated":"2022-08-18T10:42:47Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"arxiv":1,"article_processing_charge":"No","issue":"4","_id":"11521","date_published":"2022-06-01T00:00:00Z","abstract":[{"text":"The cosmic ionizing emissivity from star-forming galaxies has long been anchored to UV luminosity functions. Here, we introduce an emissivity framework based on Lyα emitters (LAEs), which naturally hones in on the subset of galaxies responsible for the ionizing background due to the intimate connection between production and escape of Lyα and LyC photons. Using constraints on the escape fractions of bright LAEs (LLyα > 0.2L*) at z ≈ 2 obtained from resolved Lyα profiles, and arguing for their redshift-invariance, we show that: (i) quasars and LAEs together reproduce the relatively flat emissivity at z ≈ 2–6, which is non-trivial given the strong evolution in both the star formation density and quasar number density at these epochs and (ii) LAEs produce late and rapid reionization between z ≈ 6−9 under plausible assumptions. Within this framework, the >10 × rise in the UV population-averaged fesc between z ≈ 3–7 naturally arises due to the same phenomena that drive the growing LAE fraction with redshift. Generally, a LAE dominated emissivity yields a peak in the distribution of the ionizing budget with UV luminosity as reported in latest simulations. Using our adopted parameters (⁠fesc=50 per cent⁠, ξion = 1025.9 Hz erg−1 for half the bright LAEs), a highly ionizing minority of galaxies with MUV < −17 accounts for the entire ionizing budget from star-forming galaxies. Rapid flashes of LyC from such rare galaxies produce a ‘disco’ ionizing background. We conclude proposing tests to further develop our suggested Lyα-anchored formalism.","lang":"eng"}],"publication_status":"published","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2110.11967"}],"oa":1,"volume":512,"citation":{"apa":"Matthee, J. J., Naidu, R. P., Pezzulli, G., Gronke, M., Sobral, D., Oesch, P. A., … Röttgering, H. (2022). (Re)Solving reionization with Lyα: How bright Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stac801\">https://doi.org/10.1093/mnras/stac801</a>","ama":"Matthee JJ, Naidu RP, Pezzulli G, et al. (Re)Solving reionization with Lyα: How bright Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background. <i>Monthly Notices of the Royal Astronomical Society</i>. 2022;512(4):5960-5977. doi:<a href=\"https://doi.org/10.1093/mnras/stac801\">10.1093/mnras/stac801</a>","short":"J.J. Matthee, R.P. Naidu, G. Pezzulli, M. Gronke, D. Sobral, P.A. Oesch, M. Hayes, D. Erb, D. Schaerer, R. Amorín, S. Tacchella, A.P.-A. Ana Paulino-Afonso, M. Llerena, J. Calhau, H. Röttgering, Monthly Notices of the Royal Astronomical Society 512 (2022) 5960–5977.","mla":"Matthee, Jorryt J., et al. “(Re)Solving Reionization with Lyα: How Bright Lyα Emitters Account for the z ≈ 2 − 8 Cosmic Ionizing Background.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 512, no. 4, Oxford University Press, 2022, pp. 5960–77, doi:<a href=\"https://doi.org/10.1093/mnras/stac801\">10.1093/mnras/stac801</a>.","ista":"Matthee JJ, Naidu RP, Pezzulli G, Gronke M, Sobral D, Oesch PA, Hayes M, Erb D, Schaerer D, Amorín R, Tacchella S, Ana Paulino-Afonso AP-A, Llerena M, Calhau J, Röttgering H. 2022. (Re)Solving reionization with Lyα: How bright Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background. Monthly Notices of the Royal Astronomical Society. 512(4), 5960–5977.","ieee":"J. J. Matthee <i>et al.</i>, “(Re)Solving reionization with Lyα: How bright Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 512, no. 4. Oxford University Press, pp. 5960–5977, 2022.","chicago":"Matthee, Jorryt J, Rohan P. Naidu, Gabriele Pezzulli, Max Gronke, David Sobral, Pascal A. Oesch, Matthew Hayes, et al. “(Re)Solving Reionization with Lyα: How Bright Lyα Emitters Account for the z ≈ 2 − 8 Cosmic Ionizing Background.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2022. <a href=\"https://doi.org/10.1093/mnras/stac801\">https://doi.org/10.1093/mnras/stac801</a>."},"title":"(Re)Solving reionization with Lyα: How bright Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background","day":"01","author":[{"last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"first_name":"Rohan P.","full_name":"Naidu, Rohan P.","last_name":"Naidu"},{"first_name":"Gabriele","full_name":"Pezzulli, Gabriele","last_name":"Pezzulli"},{"first_name":"Max","full_name":"Gronke, Max","last_name":"Gronke"},{"last_name":"Sobral","first_name":"David","full_name":"Sobral, David"},{"first_name":"Pascal A.","full_name":"Oesch, Pascal A.","last_name":"Oesch"},{"last_name":"Hayes","first_name":"Matthew","full_name":"Hayes, Matthew"},{"first_name":"Dawn","full_name":"Erb, Dawn","last_name":"Erb"},{"last_name":"Schaerer","full_name":"Schaerer, Daniel","first_name":"Daniel"},{"last_name":"Amorín","first_name":"Ricardo","full_name":"Amorín, Ricardo"},{"last_name":"Tacchella","full_name":"Tacchella, Sandro","first_name":"Sandro"},{"last_name":"Ana Paulino-Afonso","full_name":"Ana Paulino-Afonso, Ana Paulino-Afonso","first_name":"Ana Paulino-Afonso"},{"first_name":"Mario","full_name":"Llerena, Mario","last_name":"Llerena"},{"first_name":"João","full_name":"Calhau, João","last_name":"Calhau"},{"full_name":"Röttgering, Huub","first_name":"Huub","last_name":"Röttgering"}],"type":"journal_article","acknowledgement":"We thank an anonymous referee for an encouraging and constructive report that helped improving the quality of this work. We acknowledge illuminating conversations with Xiaohan Wu, Chris Cain, Anna-Christina Eilers, Simon Lilly and Ruari Mackenzie. RPN gratefully acknowledges an Ashford Fellowship granted by Harvard University. MG was supported by NASA through the NASA Hubble Fellowship grant HST-HF2-51409. PO acknowledges support from the Swiss National Science Foundation through the SNSF Professorship grant 190079. GP acknowledges support from the Netherlands Research School for Astronomy (NOVA). MH is fellow of the Knut and Alice Wallenberg Foundation. DE is supported by the US National Science Foundation (NSF) through Astronomy & Astrophysics grant AST-1909198. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant No. 140. RA acknowledges support from Fondecyt Regular Grant 1202007. ST is supported by the 2021 Research Fund 1.210134.01 of UNIST (Ulsan National Institute of Science & Technology). MLl acknowledges support from the ANID/Scholarship Program/Doctorado Nacional/2019-21191036. JC acknowledges support from the Spanish Ministry of Science and Innovation, project PID2019-107408GB-C43 (ESTALLIDOS) and from Gobierno de Canarias through EU FEDER funding, project PID2020010050.","keyword":["galaxies: high-redshift","intergalactic medium","cosmology: observations","dark ages","reionization","first stars","ultraviolet: galaxies"],"language":[{"iso":"eng"}],"doi":"10.1093/mnras/stac801","page":"5960-5977","month":"06","extern":"1","date_created":"2022-07-07T09:21:30Z","publisher":"Oxford University Press","publication":"Monthly Notices of the Royal Astronomical Society","quality_controlled":"1","intvolume":"       512","status":"public"},{"publisher":"EDP Sciences","quality_controlled":"1","publication":"Astronomy & Astrophysics","intvolume":"       654","status":"public","extern":"1","month":"10","date_created":"2022-07-06T08:49:03Z","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).","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","ultraviolet: galaxies / galaxies: high-redshift / galaxies: ISM / ISM: lines and bands / methods: observational / techniques: imaging spectroscopy"],"doi":"10.1051/0004-6361/202140876","citation":{"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>","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).","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>.","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>.","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.","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."},"title":"Recovery and analysis of rest-frame UV emission lines in 2052 galaxies observed with MUSE at 1.5 < z < 6.4","day":"15","author":[{"last_name":"Schmidt","first_name":"K. B.","full_name":"Schmidt, K. B."},{"last_name":"Kerutt","first_name":"J.","full_name":"Kerutt, J."},{"full_name":"Wisotzki, L.","first_name":"L.","last_name":"Wisotzki"},{"first_name":"T.","full_name":"Urrutia, T.","last_name":"Urrutia"},{"last_name":"Feltre","first_name":"A.","full_name":"Feltre, A."},{"first_name":"M. V.","full_name":"Maseda, M. V.","last_name":"Maseda"},{"first_name":"T.","full_name":"Nanayakkara, T.","last_name":"Nanayakkara"},{"full_name":"Bacon, R.","first_name":"R.","last_name":"Bacon"},{"first_name":"L. A.","full_name":"Boogaard, L. A.","last_name":"Boogaard"},{"last_name":"Conseil","first_name":"S.","full_name":"Conseil, S."},{"first_name":"T.","full_name":"Contini, T.","last_name":"Contini"},{"full_name":"Herenz, E. C.","first_name":"E. C.","last_name":"Herenz"},{"full_name":"Kollatschny, W.","first_name":"W.","last_name":"Kollatschny"},{"last_name":"Krumpe","full_name":"Krumpe, M.","first_name":"M."},{"full_name":"Leclercq, F.","first_name":"F.","last_name":"Leclercq"},{"first_name":"G.","full_name":"Mahler, G.","last_name":"Mahler"},{"full_name":"Matthee, Jorryt J","first_name":"Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Mauerhofer","first_name":"V.","full_name":"Mauerhofer, V."},{"first_name":"J.","full_name":"Richard, J.","last_name":"Richard"},{"full_name":"Schaye, J.","first_name":"J.","last_name":"Schaye"}],"type":"journal_article","publication_status":"published","oa":1,"main_file_link":[{"url":"https://arxiv.org/abs/2108.01713","open_access":"1"}],"volume":654,"arxiv":1,"article_processing_charge":"No","article_number":"A80","_id":"11498","date_published":"2021-10-15T00:00:00Z","abstract":[{"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.","lang":"eng"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2022-07-19T09:34:36Z","external_id":{"arxiv":["2108.01713"]},"scopus_import":"1","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"article_type":"original","year":"2021","oa_version":"Published Version"},{"day":"18","type":"journal_article","author":[{"last_name":"Feltre","full_name":"Feltre, Anna","first_name":"Anna"},{"full_name":"Maseda, Michael V.","first_name":"Michael V.","last_name":"Maseda"},{"first_name":"Roland","full_name":"Bacon, Roland","last_name":"Bacon"},{"last_name":"Pradeep","full_name":"Pradeep, Jayadev","first_name":"Jayadev"},{"first_name":"Floriane","full_name":"Leclercq, Floriane","last_name":"Leclercq"},{"last_name":"Kusakabe","full_name":"Kusakabe, Haruka","first_name":"Haruka"},{"last_name":"Wisotzki","first_name":"Lutz","full_name":"Wisotzki, Lutz"},{"last_name":"Hashimoto","full_name":"Hashimoto, Takuya","first_name":"Takuya"},{"last_name":"Schmidt","first_name":"Kasper B.","full_name":"Schmidt, Kasper B."},{"first_name":"Jeremy","full_name":"Blaizot, Jeremy","last_name":"Blaizot"},{"full_name":"Brinchmann, Jarle","first_name":"Jarle","last_name":"Brinchmann"},{"last_name":"Boogaard","full_name":"Boogaard, Leindert","first_name":"Leindert"},{"last_name":"Cantalupo","full_name":"Cantalupo, Sebastiano","first_name":"Sebastiano"},{"full_name":"Carton, David","first_name":"David","last_name":"Carton"},{"full_name":"Inami, Hanae","first_name":"Hanae","last_name":"Inami"},{"last_name":"Kollatschny","full_name":"Kollatschny, Wolfram","first_name":"Wolfram"},{"last_name":"Marino","full_name":"Marino, Raffaella A.","first_name":"Raffaella A."},{"full_name":"Matthee, Jorryt J","first_name":"Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X"},{"full_name":"Nanayakkara, Themiya","first_name":"Themiya","last_name":"Nanayakkara"},{"last_name":"Richard","full_name":"Richard, Johan","first_name":"Johan"},{"full_name":"Schaye, Joop","first_name":"Joop","last_name":"Schaye"},{"first_name":"Laurence","full_name":"Tresse, Laurence","last_name":"Tresse"},{"last_name":"Urrutia","first_name":"Tanya","full_name":"Urrutia, Tanya"},{"last_name":"Verhamme","first_name":"Anne","full_name":"Verhamme, Anne"},{"last_name":"Weilbacher","full_name":"Weilbacher, Peter M.","first_name":"Peter M."}],"citation":{"mla":"Feltre, Anna, et al. “The MUSE Hubble Ultra Deep Field Survey: XV. The Mean Rest-UV Spectra of Lyα Emitters at z &#62; 3.” <i>Astronomy &#38; Astrophysics</i>, vol. 641, A118, EDP Sciences, 2020, doi:<a href=\"https://doi.org/10.1051/0004-6361/202038133\">10.1051/0004-6361/202038133</a>.","ieee":"A. Feltre <i>et al.</i>, “The MUSE Hubble Ultra Deep Field Survey: XV. The mean rest-UV spectra of Lyα emitters at z &#62; 3,” <i>Astronomy &#38; Astrophysics</i>, vol. 641. EDP Sciences, 2020.","ista":"Feltre A, Maseda MV, Bacon R, Pradeep J, Leclercq F, Kusakabe H, Wisotzki L, Hashimoto T, Schmidt KB, Blaizot J, Brinchmann J, Boogaard L, Cantalupo S, Carton D, Inami H, Kollatschny W, Marino RA, Matthee JJ, Nanayakkara T, Richard J, Schaye J, Tresse L, Urrutia T, Verhamme A, Weilbacher PM. 2020. The MUSE Hubble Ultra Deep Field Survey: XV. The mean rest-UV spectra of Lyα emitters at z &#62; 3. Astronomy &#38; Astrophysics. 641, A118.","chicago":"Feltre, Anna, Michael V. Maseda, Roland Bacon, Jayadev Pradeep, Floriane Leclercq, Haruka Kusakabe, Lutz Wisotzki, et al. “The MUSE Hubble Ultra Deep Field Survey: XV. The Mean Rest-UV Spectra of Lyα Emitters at z &#62; 3.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2020. <a href=\"https://doi.org/10.1051/0004-6361/202038133\">https://doi.org/10.1051/0004-6361/202038133</a>.","apa":"Feltre, A., Maseda, M. V., Bacon, R., Pradeep, J., Leclercq, F., Kusakabe, H., … Weilbacher, P. M. (2020). The MUSE Hubble Ultra Deep Field Survey: XV. The mean rest-UV spectra of Lyα emitters at z &#62; 3. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202038133\">https://doi.org/10.1051/0004-6361/202038133</a>","ama":"Feltre A, Maseda MV, Bacon R, et al. The MUSE Hubble Ultra Deep Field Survey: XV. The mean rest-UV spectra of Lyα emitters at z &#62; 3. <i>Astronomy &#38; Astrophysics</i>. 2020;641. doi:<a href=\"https://doi.org/10.1051/0004-6361/202038133\">10.1051/0004-6361/202038133</a>","short":"A. Feltre, M.V. Maseda, R. Bacon, J. Pradeep, F. Leclercq, H. Kusakabe, L. Wisotzki, T. Hashimoto, K.B. Schmidt, J. Blaizot, J. Brinchmann, L. Boogaard, S. Cantalupo, D. Carton, H. Inami, W. Kollatschny, R.A. Marino, J.J. Matthee, T. Nanayakkara, J. Richard, J. Schaye, L. Tresse, T. Urrutia, A. Verhamme, P.M. Weilbacher, Astronomy &#38; Astrophysics 641 (2020)."},"title":"The MUSE Hubble Ultra Deep Field Survey: XV. The mean rest-UV spectra of Lyα emitters at z > 3","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution / galaxies: high-redshift / ISM: lines and bands / ultraviolet: ISM / ultraviolet: galaxies"],"doi":"10.1051/0004-6361/202038133","acknowledgement":"We thank Margherita Talia, Stéphane Charlot, Adele Plat and Alba Vidal-García for helpful discussions. This work is supported by the ERC advanced grant 339659-MUSICOS (R. Bacon). AF acknowledges the support from grant PRIN MIUR 2017 20173ML3WW. MVM and JP would like to thank the Leiden/ESA Astrophysics Program for Summer Students (LEAPS) for funding at the outset of this project. FL, HK, and AV acknowledge support from the ERC starting grant ERC-757258-TRIPLE. TH was supported by Leading Initiative for Excellent Young Researchers, MEXT, Japan. JB acknowledges support by FCT/MCTES through national funds by the grant UID/FIS/04434/2019, UIDB/04434/2020 and UIDP/04434/2020 and through the Investigador FCT Contract No. IF/01654/2014/CP1215/CT0003. HI acknowledges support from JSPS KAKENHI Grant Number JP19K23462. We would also like to thank the organizers and participants of the Leiden Lorentz Center workshop: Revolutionary Spectroscopy of Today as a Springboard to Webb. This work made use of several open source python packages: NUMPY (van der Walt et al. 2011), MATPLOTLIB (Hunter 2007), ASTROPY (Astropy Collaboration 2013) and MPDAF (MUSE Python Data Analysis Framework, Piqueras et al. 2019).","extern":"1","month":"09","date_created":"2022-07-06T09:38:16Z","quality_controlled":"1","publication":"Astronomy & Astrophysics","status":"public","intvolume":"       641","publisher":"EDP Sciences","article_type":"original","year":"2020","oa_version":"Published Version","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2022-07-19T09:35:43Z","external_id":{"arxiv":["2007.01878"]},"scopus_import":"1","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"article_number":"A118","abstract":[{"text":"We investigated the ultraviolet (UV) spectral properties of faint Lyman-α emitters (LAEs) in the redshift range 2.9 ≤ z ≤ 4.6, and we provide material to prepare future observations of the faint Universe. We used data from the MUSE Hubble Ultra Deep Survey to construct mean rest-frame spectra of continuum-faint (median MUV of −18 and down to MUV of −16), low stellar mass (median value of 108.4 M⊙ and down to 107 M⊙) LAEs at redshift z ≳ 3. We computed various averaged spectra of LAEs, subsampled on the basis of their observational (e.g., Lyα strength, UV magnitude and spectral slope) and physical (e.g., stellar mass and star-formation rate) properties. We searched for UV spectral features other than Lyα, such as higher ionization nebular emission lines and absorption features. We successfully observed the O III]λ1666 and [C III]λ1907+C III]λ1909 collisionally excited emission lines and the He IIλ1640 recombination feature, as well as the resonant C IVλλ1548,1551 doublet either in emission or P-Cygni. We compared the observed spectral properties of the different mean spectra and find the emission lines to vary with the observational and physical properties of the LAEs. In particular, the mean spectra of LAEs with larger Lyα equivalent widths, fainter UV magnitudes, bluer UV spectral slopes, and lower stellar masses show the strongest nebular emission. The line ratios of these lines are similar to those measured in the spectra of local metal-poor galaxies, while their equivalent widths are weaker compared to the handful of extreme values detected in individual spectra of z >  2 galaxies. This suggests that weak UV features are likely ubiquitous in high z, low-mass, and faint LAEs. We publicly released the stacked spectra, as they can serve as empirical templates for the design of future observations, such as those with the James Webb Space Telescope and the Extremely Large Telescope.","lang":"eng"}],"_id":"11501","date_published":"2020-09-18T00:00:00Z","arxiv":1,"article_processing_charge":"No","volume":641,"publication_status":"published","main_file_link":[{"url":"https://arxiv.org/abs/2007.01878","open_access":"1"}],"oa":1}]