[{"quality_controlled":"1","status":"public","language":[{"iso":"eng"}],"publication_status":"published","abstract":[{"text":"We explore deep rest-frame UV to FIR data in the COSMOS field to measure the individual spectral energy distributions (SED) of the ∼4000 SC4K (Sobral et al.) Lyman α (Ly α) emitters (LAEs) at z ∼ 2–6. We find typical stellar masses of 109.3 ± 0.6 M⊙ and star formation rates (SFR) of SFRSED=4.4+10.5−2.4 M⊙ yr−1 and SFRLyα=5.9+6.3−2.6 M⊙ yr−1, combined with very blue UV slopes of β=−2.1+0.5−0.4⁠, but with significant variations within the population. MUV and β are correlated in a similar way to UV-selected sources, but LAEs are consistently bluer. This suggests that LAEs are the youngest and/or most dust-poor subset of the UV-selected population. We also study the Ly α rest-frame equivalent width (EW0) and find 45 ‘extreme’ LAEs with EW0 > 240 Å (3σ), implying a low number density of (7 ± 1) × 10−7 Mpc−3. Overall, we measure little to no evolution of the Ly α EW0 and scale length parameter (w0), which are consistently high (EW0=140+280−70 Å, w0=129+11−11 Å) from z ∼ 6 to z ∼ 2 and below. However, w0 is anticorrelated with MUV and stellar mass. Our results imply that sources selected as LAEs have a high Ly α escape fraction (fesc,Ly α) irrespective of cosmic time, but fesc,Ly α is still higher for UV-fainter and lower mass LAEs. The least massive LAEs (<109.5 M⊙) are typically located above the star formation ‘main sequence’ (MS), but the offset from the MS decreases towards z ∼ 6 and towards 1010 M⊙. Our results imply a lack of evolution in the properties of LAEs across time and reveals the increasing overlap in properties of LAEs and UV-continuum selected galaxies as typical star-forming galaxies at high redshift effectively become LAEs.","lang":"eng"}],"article_type":"original","citation":{"ieee":"S. Santos <i>et al.</i>, “The evolution of rest-frame UV properties, Ly α EWs, and the SFR–stellar mass relation at z ∼ 2–6 for SC4K LAEs,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 493, no. 1. Oxford University Press, pp. 141–160, 2020.","short":"S. Santos, D. Sobral, J.J. Matthee, J. Calhau, E. da Cunha, B. Ribeiro, A. Paulino-Afonso, P. Arrabal Haro, J. Butterworth, Monthly Notices of the Royal Astronomical Society 493 (2020) 141–160.","apa":"Santos, S., Sobral, D., Matthee, J. J., Calhau, J., da Cunha, E., Ribeiro, B., … Butterworth, J. (2020). The evolution of rest-frame UV properties, Ly α EWs, and the SFR–stellar mass relation at z ∼ 2–6 for SC4K LAEs. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staa093\">https://doi.org/10.1093/mnras/staa093</a>","ista":"Santos S, Sobral D, Matthee JJ, Calhau J, da Cunha E, Ribeiro B, Paulino-Afonso A, Arrabal Haro P, Butterworth J. 2020. The evolution of rest-frame UV properties, Ly α EWs, and the SFR–stellar mass relation at z ∼ 2–6 for SC4K LAEs. Monthly Notices of the Royal Astronomical Society. 493(1), 141–160.","mla":"Santos, S., et al. “The Evolution of Rest-Frame UV Properties, Ly α EWs, and the SFR–Stellar Mass Relation at z ∼ 2–6 for SC4K LAEs.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 493, no. 1, Oxford University Press, 2020, pp. 141–60, doi:<a href=\"https://doi.org/10.1093/mnras/staa093\">10.1093/mnras/staa093</a>.","chicago":"Santos, S, D Sobral, Jorryt J Matthee, J Calhau, E da Cunha, B Ribeiro, A Paulino-Afonso, P Arrabal Haro, and J Butterworth. “The Evolution of Rest-Frame UV Properties, Ly α EWs, and the SFR–Stellar Mass Relation at z ∼ 2–6 for SC4K LAEs.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2020. <a href=\"https://doi.org/10.1093/mnras/staa093\">https://doi.org/10.1093/mnras/staa093</a>.","ama":"Santos S, Sobral D, Matthee JJ, et al. The evolution of rest-frame UV properties, Ly α EWs, and the SFR–stellar mass relation at z ∼ 2–6 for SC4K LAEs. <i>Monthly Notices of the Royal Astronomical Society</i>. 2020;493(1):141-160. doi:<a href=\"https://doi.org/10.1093/mnras/staa093\">10.1093/mnras/staa093</a>"},"type":"journal_article","year":"2020","author":[{"first_name":"S","full_name":"Santos, S","last_name":"Santos"},{"full_name":"Sobral, D","last_name":"Sobral","first_name":"D"},{"first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J"},{"last_name":"Calhau","full_name":"Calhau, J","first_name":"J"},{"full_name":"da Cunha, E","last_name":"da Cunha","first_name":"E"},{"full_name":"Ribeiro, B","last_name":"Ribeiro","first_name":"B"},{"full_name":"Paulino-Afonso, A","last_name":"Paulino-Afonso","first_name":"A"},{"last_name":"Arrabal Haro","full_name":"Arrabal Haro, P","first_name":"P"},{"last_name":"Butterworth","full_name":"Butterworth, J","first_name":"J"}],"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"day":"01","publisher":"Oxford University Press","oa_version":"Preprint","arxiv":1,"doi":"10.1093/mnras/staa093","oa":1,"intvolume":"       493","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","acknowledgement":"We thank the anonymous referee for the valuable feedback that significantly improved the quality and clarity of this paper. SS and JC acknowledge studentships from Lancaster University. APA acknowledges support from Fundação para a Ciência e a Tecnologia through the project PTDC/FISAST/31546/2017. The authors would like to thank Ali Khostovan, Sara Perez Sanchez, Alex Bennett and Tom Rose for contributions and discussions in the early stages of this work. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by CALET and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. Finally, the authors acknowledge the unique value of the publicly available analysis software TOPCAT (Taylor 2005) and publicly available programming language Python, including the numpy, pyfits, matplotlib, scipy and astropy (Astropy Collaboration et al. 2013) packages. This work is based on the public SC4K sample of LAEs (Sobral et al. 2018a) and we release the full catalogue with all the photometry and properties derived in this paper, in electronic format, along with the relevant tables.","issue":"1","main_file_link":[{"url":"https://arxiv.org/abs/1910.02959","open_access":"1"}],"volume":493,"extern":"1","scopus_import":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: formation","galaxies: high-redshift","galaxies: star formation"],"article_processing_charge":"No","date_published":"2020-03-01T00:00:00Z","month":"03","title":"The evolution of rest-frame UV properties, Ly α EWs, and the SFR–stellar mass relation at z ∼ 2–6 for SC4K LAEs","date_updated":"2022-08-18T11:27:43Z","external_id":{"arxiv":["1910.02959"]},"date_created":"2022-07-07T12:05:23Z","_id":"11533","page":"141-160","publication":"Monthly Notices of the Royal Astronomical Society"},{"publisher":"Oxford University Press","day":"01","doi":"10.1093/mnras/stz3554","arxiv":1,"oa_version":"Preprint","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","last_name":"Matthee"},{"first_name":"David","full_name":"Sobral, David","last_name":"Sobral"},{"full_name":"Gronke, Max","last_name":"Gronke","first_name":"Max"},{"first_name":"Gabriele","last_name":"Pezzulli","full_name":"Pezzulli, Gabriele"},{"last_name":"Cantalupo","full_name":"Cantalupo, Sebastiano","first_name":"Sebastiano"},{"last_name":"Röttgering","full_name":"Röttgering, Huub","first_name":"Huub"},{"first_name":"Behnam","last_name":"Darvish","full_name":"Darvish, Behnam"},{"first_name":"Sérgio","last_name":"Santos","full_name":"Santos, Sérgio"}],"year":"2020","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"article_type":"original","citation":{"ieee":"J. J. Matthee <i>et al.</i>, “Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 ,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 492, no. 2. Oxford University Press, pp. 1778–1790, 2020.","apa":"Matthee, J. J., Sobral, D., Gronke, M., Pezzulli, G., Cantalupo, S., Röttgering, H., … Santos, S. (2020). Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 . <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stz3554\">https://doi.org/10.1093/mnras/stz3554</a>","short":"J.J. Matthee, D. Sobral, M. Gronke, G. Pezzulli, S. Cantalupo, H. Röttgering, B. Darvish, S. Santos, Monthly Notices of the Royal Astronomical Society 492 (2020) 1778–1790.","mla":"Matthee, Jorryt J., et al. “Resolved Lyman-α Properties of a Luminous Lyman-Break Galaxy in a Large Ionized Bubble at z = 6.53 .” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 492, no. 2, Oxford University Press, 2020, pp. 1778–90, doi:<a href=\"https://doi.org/10.1093/mnras/stz3554\">10.1093/mnras/stz3554</a>.","ista":"Matthee JJ, Sobral D, Gronke M, Pezzulli G, Cantalupo S, Röttgering H, Darvish B, Santos S. 2020. Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 . Monthly Notices of the Royal Astronomical Society. 492(2), 1778–1790.","ama":"Matthee JJ, Sobral D, Gronke M, et al. Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 . <i>Monthly Notices of the Royal Astronomical Society</i>. 2020;492(2):1778-1790. doi:<a href=\"https://doi.org/10.1093/mnras/stz3554\">10.1093/mnras/stz3554</a>","chicago":"Matthee, Jorryt J, David Sobral, Max Gronke, Gabriele Pezzulli, Sebastiano Cantalupo, Huub Röttgering, Behnam Darvish, and Sérgio Santos. “Resolved Lyman-α Properties of a Luminous Lyman-Break Galaxy in a Large Ionized Bubble at z = 6.53 .” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2020. <a href=\"https://doi.org/10.1093/mnras/stz3554\">https://doi.org/10.1093/mnras/stz3554</a>."},"type":"journal_article","quality_controlled":"1","publication_status":"published","abstract":[{"text":"The observed properties of the Lyman-α (Ly α) emission line are a powerful probe of neutral gas in and around galaxies. We present spatially resolved Ly α spectroscopy with VLT/MUSE targeting VR7, a UV-luminous galaxy at z = 6.532 with moderate Ly α equivalent width (EW0 ≈ 38 Å). These data are combined with deep resolved [CII]158μm spectroscopy obtained with ALMA and UV imaging from HST and we also detect UV continuum with MUSE. Ly α emission is clearly detected with S/N ≈ 40 and FWHM of 374 km s−1. Ly α and [C II] are similarly extended beyond the UV, with effective radius reff = 2.1 ± 0.2 kpc for a single exponential model or reff,Lyα,halo=3.45+1.08−0.87 kpc when measured jointly with the UV continuum. The Ly α profile is broader and redshifted with respect to the [C II] line (by 213 km s−1), but there are spatial variations that are qualitatively similar in both lines and coincide with resolved UV components. This suggests that the emission originates from two components with plausibly different H I column densities. We place VR7 in the context of other galaxies at similar and lower redshift. The Ly α halo scale length is similar at different redshifts and velocity shifts with respect to the systemic are typically smaller. Overall, we find little indications of a more neutral vicinity at higher redshift. This means that the local (∼10 kpc) neutral gas conditions that determine the observed Ly α properties in VR7 resemble the conditions in post-reionization galaxies.","lang":"eng"}],"language":[{"iso":"eng"}],"status":"public","_id":"11534","date_created":"2022-07-07T12:21:36Z","external_id":{"arxiv":["1909.06376"]},"publication":"Monthly Notices of the Royal Astronomical Society","page":"1778-1790","date_published":"2020-02-01T00:00:00Z","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","dark ages","reionization","first stars","cosmology: observations"],"article_processing_charge":"No","date_updated":"2022-08-18T11:29:53Z","title":"Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 ","month":"02","scopus_import":"1","extern":"1","acknowledgement":"We thank the referee for their suggestions and constructive comments that helped to improve the presentation of our results. Based on observations obtained with the Very Large Telescope, program 99.A-0462. Based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program #14699. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2017.1.01451.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan) and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. MG acknowledges support from NASA grant NNX17AK58G. GP and SC gratefully acknowledge support from Swiss National Science Foundation grant PP00P2 163824. BD acknowledges financial support from the National Science Foundation, grant number 1716907. We have benefited greatly from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, SCIPY (Jones et al. 2001; Hunter 2007; van der Walt, Colbert & Varoquaux 2011) and ASTROPY (Astropy Collaboration 2013) packages, the astronomical imaging tools SEXTRACTOR, SWARP, and SCAMP (Bertin & Arnouts 1996; Bertin 2006, 2010) and the TOPCAT analysis tool (Taylor 2013).","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","issue":"2","oa":1,"intvolume":"       492","volume":492,"main_file_link":[{"url":"https://arxiv.org/abs/1909.06376","open_access":"1"}]},{"citation":{"chicago":"Calhau, João, David Sobral, Sérgio Santos, Jorryt J Matthee, Ana Paulino-Afonso, Andra Stroe, Brooke Simmons, Cassandra Barlow-Hall, and Benjamin Adams. “The X-Ray and Radio Activity of Typical and Luminous Ly α Emitters from z ∼ 2 to z ∼ 6: Evidence for a Diverse, Evolving Population.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2020. <a href=\"https://doi.org/10.1093/mnras/staa476\">https://doi.org/10.1093/mnras/staa476</a>.","ama":"Calhau J, Sobral D, Santos S, et al. The X-ray and radio activity of typical and luminous Ly α emitters from z ∼ 2 to z ∼ 6: Evidence for a diverse, evolving population. <i>Monthly Notices of the Royal Astronomical Society</i>. 2020;493(3):3341-3362. doi:<a href=\"https://doi.org/10.1093/mnras/staa476\">10.1093/mnras/staa476</a>","mla":"Calhau, João, et al. “The X-Ray and Radio Activity of Typical and Luminous Ly α Emitters from z ∼ 2 to z ∼ 6: Evidence for a Diverse, Evolving Population.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 493, no. 3, Oxford University Press, 2020, pp. 3341–62, doi:<a href=\"https://doi.org/10.1093/mnras/staa476\">10.1093/mnras/staa476</a>.","ista":"Calhau J, Sobral D, Santos S, Matthee JJ, Paulino-Afonso A, Stroe A, Simmons B, Barlow-Hall C, Adams B. 2020. The X-ray and radio activity of typical and luminous Ly α emitters from z ∼ 2 to z ∼ 6: Evidence for a diverse, evolving population. Monthly Notices of the Royal Astronomical Society. 493(3), 3341–3362.","short":"J. Calhau, D. Sobral, S. Santos, J.J. Matthee, A. Paulino-Afonso, A. Stroe, B. Simmons, C. Barlow-Hall, B. Adams, Monthly Notices of the Royal Astronomical Society 493 (2020) 3341–3362.","apa":"Calhau, J., Sobral, D., Santos, S., Matthee, J. J., Paulino-Afonso, A., Stroe, A., … Adams, B. (2020). The X-ray and radio activity of typical and luminous Ly α emitters from z ∼ 2 to z ∼ 6: Evidence for a diverse, evolving population. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staa476\">https://doi.org/10.1093/mnras/staa476</a>","ieee":"J. Calhau <i>et al.</i>, “The X-ray and radio activity of typical and luminous Ly α emitters from z ∼ 2 to z ∼ 6: Evidence for a diverse, evolving population,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 493, no. 3. Oxford University Press, pp. 3341–3362, 2020."},"type":"journal_article","article_type":"original","abstract":[{"text":"Despite recent progress in understanding Ly α emitters (LAEs), relatively little is known regarding their typical black hole activity across cosmic time. Here, we study the X-ray and radio properties of ∼4000 LAEs at 2.2 < z < 6 from the SC4K survey in the COSMOS field. We detect 254 (⁠6.8per cent±0.4per cent⁠) LAEs individually in the X-rays (S/N > 3) with an average luminosity of 1044.31±0.01ergs−1 and average black hole accretion rate (BHAR) of 0.72±0.01 M⊙ yr−1, consistent with moderate to high accreting active galactic neuclei (AGNs). We detect 120 sources in deep radio data (radio AGN fraction of 3.2per cent±0.3per cent⁠). The global AGN fraction (⁠8.6per cent±0.4per cent⁠) rises with Ly α luminosity and declines with increasing redshift. For X-ray-detected LAEs, Ly α luminosities correlate with the BHARs, suggesting that Ly α luminosity becomes a BHAR indicator. Most LAEs (⁠93.1per cent±0.6per cent⁠) at 2 < z < 6 have no detectable X-ray emission (BHARs < 0.017 M⊙ yr−1). The median star formation rate (SFR) of star-forming LAEs from Ly α and radio luminosities is 7.6+6.6−2.8 M⊙ yr−1. The black hole to galaxy growth ratio (BHAR/SFR) for LAEs is <0.0022, consistent with typical star-forming galaxies and the local BHAR/SFR relation. We conclude that LAEs at 2 < z < 6 include two different populations: an AGN population, where Ly α luminosity traces BHAR, and another with low SFRs which remain undetected in even the deepest X-ray stacks but is detected in the radio stacks.","lang":"eng"}],"publication_status":"published","language":[{"iso":"eng"}],"status":"public","quality_controlled":"1","doi":"10.1093/mnras/staa476","oa_version":"Preprint","arxiv":1,"publisher":"Oxford University Press","day":"01","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"author":[{"full_name":"Calhau, João","last_name":"Calhau","first_name":"João"},{"first_name":"David","last_name":"Sobral","full_name":"Sobral, David"},{"full_name":"Santos, Sérgio","last_name":"Santos","first_name":"Sérgio"},{"orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J"},{"first_name":"Ana","last_name":"Paulino-Afonso","full_name":"Paulino-Afonso, Ana"},{"last_name":"Stroe","full_name":"Stroe, Andra","first_name":"Andra"},{"first_name":"Brooke","last_name":"Simmons","full_name":"Simmons, Brooke"},{"first_name":"Cassandra","last_name":"Barlow-Hall","full_name":"Barlow-Hall, Cassandra"},{"last_name":"Adams","full_name":"Adams, Benjamin","first_name":"Benjamin"}],"year":"2020","scopus_import":"1","extern":"1","volume":493,"main_file_link":[{"url":"https://arxiv.org/abs/1909.11672","open_access":"1"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","issue":"3","acknowledgement":"JM acknowledges the support of a Huygens PhD fellowship from Leiden University. We thank Camila Correa for help analysing snipshot merger trees. We thank the anonymous referee for constructive comments. We also thank Jarle Brinchmann, Rob Crain, Antonios Katsianis, Paola Popesso, and David Sobral for discussions and suggestions. We also thank the participants of the Lorentz Center workshop ‘A Decade of the Star-Forming Main Sequence’ held on 2017 September 4–8, for discussions and ideas. We have benefited from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, and SCIPY (Hunter 2007) packages and the TOPCAT analysis tool (Taylor 2013).","oa":1,"intvolume":"       493","publication":"Monthly Notices of the Royal Astronomical Society","page":"3341-3362","_id":"11539","date_created":"2022-07-08T07:34:10Z","external_id":{"arxiv":["1909.11672"]},"title":"The X-ray and radio activity of typical and luminous Ly α emitters from z ∼ 2 to z ∼ 6: Evidence for a diverse, evolving population","date_updated":"2022-08-18T11:25:31Z","month":"04","date_published":"2020-04-01T00:00:00Z","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: active","galaxies: evolution","galaxies: high-redshift","quasars: supermassive black holes","galaxies: star formation","cosmology: observations","X-rays: galaxies"],"article_processing_charge":"No"},{"publication_status":"published","abstract":[{"lang":"eng","text":"Distant luminous Lyman-α emitters are excellent targets for detailed observations of galaxies in the epoch of reionisation. Spatially resolved observations of these galaxies allow us to simultaneously probe the emission from young stars, partially ionised gas in the interstellar medium and to constrain the properties of the surrounding hydrogen in the circumgalactic medium. We review recent results from (spectroscopic) follow-up studies of the rest-frame UV, Lyman-α and [CII] emission in luminous galaxies observed ∼500 Myr after the Big Bang with ALMA, HST/WFC3 and VLT/X-SHOOTER. These galaxies likely reside in early ionised bubbles and are complex systems, consisting of multiple well separated and resolved components where traces of metals are already present."}],"language":[{"iso":"eng"}],"status":"public","quality_controlled":"1","citation":{"chicago":"Matthee, Jorryt J, and David Sobral. “Unveiling the Most Luminous Lyman-α Emitters in the Epoch of Reionisation.” In <i>Proceedings of the International Astronomical Union</i>, 15:21–25. Cambridge University Press, 2020. <a href=\"https://doi.org/10.1017/s1743921319009451\">https://doi.org/10.1017/s1743921319009451</a>.","ama":"Matthee JJ, Sobral D. Unveiling the most luminous Lyman-α emitters in the epoch of reionisation. In: <i>Proceedings of the International Astronomical Union</i>. Vol 15. Cambridge University Press; 2020:21-25. doi:<a href=\"https://doi.org/10.1017/s1743921319009451\">10.1017/s1743921319009451</a>","ista":"Matthee JJ, Sobral D. 2020. Unveiling the most luminous Lyman-α emitters in the epoch of reionisation. Proceedings of the International Astronomical Union. vol. 15, 21–25.","mla":"Matthee, Jorryt J., and David Sobral. “Unveiling the Most Luminous Lyman-α Emitters in the Epoch of Reionisation.” <i>Proceedings of the International Astronomical Union</i>, vol. 15, no. S352, Cambridge University Press, 2020, pp. 21–25, doi:<a href=\"https://doi.org/10.1017/s1743921319009451\">10.1017/s1743921319009451</a>.","apa":"Matthee, J. J., &#38; Sobral, D. (2020). Unveiling the most luminous Lyman-α emitters in the epoch of reionisation. In <i>Proceedings of the International Astronomical Union</i> (Vol. 15, pp. 21–25). Cambridge University Press. <a href=\"https://doi.org/10.1017/s1743921319009451\">https://doi.org/10.1017/s1743921319009451</a>","short":"J.J. Matthee, D. Sobral, in:, Proceedings of the International Astronomical Union, Cambridge University Press, 2020, pp. 21–25.","ieee":"J. J. Matthee and D. Sobral, “Unveiling the most luminous Lyman-α emitters in the epoch of reionisation,” in <i>Proceedings of the International Astronomical Union</i>, 2020, vol. 15, no. S352, pp. 21–25."},"type":"conference","publication_identifier":{"eissn":["1743-9221"],"issn":["1743-9213"]},"author":[{"full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"full_name":"Sobral, David","last_name":"Sobral","first_name":"David"}],"year":"2020","doi":"10.1017/s1743921319009451","oa_version":"Preprint","arxiv":1,"publisher":"Cambridge University Press","day":"04","volume":15,"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1911.04774"}],"issue":"S352","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","intvolume":"        15","oa":1,"scopus_import":"1","extern":"1","title":"Unveiling the most luminous Lyman-α emitters in the epoch of reionisation","date_updated":"2022-08-19T08:41:12Z","month":"06","date_published":"2020-06-04T00:00:00Z","article_processing_charge":"No","keyword":["Astronomy and Astrophysics","Space and Planetary Science","galaxies: formation","galaxies: evolution","galaxies: high-redshift"],"publication":"Proceedings of the International Astronomical Union","page":"21-25","_id":"11586","date_created":"2022-07-14T14:08:41Z","external_id":{"arxiv":["1911.04774"]}},{"publication_identifier":{"issn":["1090-7807"]},"title":"Relaxing with liquids and solids – A perspective on biomolecular dynamics","date_updated":"2021-01-12T08:19:04Z","month":"09","year":"2019","article_processing_charge":"No","keyword":["Nuclear and High Energy Physics","Biophysics","Biochemistry","Condensed Matter Physics"],"date_published":"2019-09-01T00:00:00Z","author":[{"id":"7B541462-FAF6-11E9-A490-E8DFE5697425","first_name":"Paul","full_name":"Schanda, Paul","orcid":"0000-0002-9350-7606","last_name":"Schanda"}],"publication":"Journal of Magnetic Resonance","doi":"10.1016/j.jmr.2019.07.025","oa_version":"Submitted Version","page":"180-186","_id":"8407","publisher":"Elsevier","day":"01","external_id":{"pmid":["31350165"]},"date_created":"2020-09-17T10:28:47Z","publication_status":"published","volume":306,"status":"public","pmid":1,"language":[{"iso":"eng"}],"quality_controlled":"1","intvolume":"       306","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","extern":"1","citation":{"short":"P. Schanda, Journal of Magnetic Resonance 306 (2019) 180–186.","apa":"Schanda, P. (2019). Relaxing with liquids and solids – A perspective on biomolecular dynamics. <i>Journal of Magnetic Resonance</i>. Elsevier. <a href=\"https://doi.org/10.1016/j.jmr.2019.07.025\">https://doi.org/10.1016/j.jmr.2019.07.025</a>","ieee":"P. Schanda, “Relaxing with liquids and solids – A perspective on biomolecular dynamics,” <i>Journal of Magnetic Resonance</i>, vol. 306. Elsevier, pp. 180–186, 2019.","chicago":"Schanda, Paul. “Relaxing with Liquids and Solids – A Perspective on Biomolecular Dynamics.” <i>Journal of Magnetic Resonance</i>. Elsevier, 2019. <a href=\"https://doi.org/10.1016/j.jmr.2019.07.025\">https://doi.org/10.1016/j.jmr.2019.07.025</a>.","ama":"Schanda P. Relaxing with liquids and solids – A perspective on biomolecular dynamics. <i>Journal of Magnetic Resonance</i>. 2019;306:180-186. doi:<a href=\"https://doi.org/10.1016/j.jmr.2019.07.025\">10.1016/j.jmr.2019.07.025</a>","ista":"Schanda P. 2019. Relaxing with liquids and solids – A perspective on biomolecular dynamics. Journal of Magnetic Resonance. 306, 180–186.","mla":"Schanda, Paul. “Relaxing with Liquids and Solids – A Perspective on Biomolecular Dynamics.” <i>Journal of Magnetic Resonance</i>, vol. 306, Elsevier, 2019, pp. 180–86, doi:<a href=\"https://doi.org/10.1016/j.jmr.2019.07.025\">10.1016/j.jmr.2019.07.025</a>."},"type":"journal_article","article_type":"original"},{"article_type":"original","citation":{"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>.","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>","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.","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>.","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).","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>","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."},"type":"journal_article","quality_controlled":"1","publication_status":"published","abstract":[{"text":"Deep optical spectroscopic surveys of galaxies provide a unique opportunity to investigate rest-frame ultra-violet (UV) emission line properties of galaxies at z ∼ 2 − 4.5. Here we combine VLT/MUSE Guaranteed Time Observations of the Hubble Deep Field South, Ultra Deep Field, COSMOS, and several quasar fields with other publicly available data from VLT/VIMOS and VLT/FORS2 to construct a catalogue of He II λ1640 emitters at z ≳ 2. The deepest areas of our MUSE pointings reach a 3σ line flux limit of 3.1 × 10−19 erg s−1 cm−2. After discarding broad-line active galactic nuclei, we find 13 He II λ1640 detections from MUSE with a median MUV = −20.1 and 21 tentative He II λ1640 detections from other public surveys. Excluding Lyα, all except two galaxies in our sample show at least one other rest-UV emission line, with C III] λ1907, λ1909 being the most prominent. We use multi-wavelength data available in the Hubble legacy fields to derive basic galaxy properties of our sample through spectral energy distribution fitting techniques. Taking advantage of the high-quality spectra obtained by MUSE (∼10 − 30 h of exposure time per pointing), we use photo-ionisation models to study the rest-UV emission line diagnostics of the He II λ1640 emitters. Line ratios of our sample can be reproduced by moderately sub-solar photo-ionisation models, however, we find that including effects of binary stars lead to degeneracies in most free parameters. Even after considering extra ionising photons produced by extreme sub-solar metallicity binary stellar models, photo-ionisation models are unable to reproduce rest-frame He II λ1640 equivalent widths (∼0.2 − 10 Å), thus additional mechanisms are necessary in models to match the observed He II λ1640 properties.","lang":"eng"}],"language":[{"iso":"eng"}],"status":"public","publisher":"EDP Sciences","day":"16","doi":"10.1051/0004-6361/201834565","arxiv":1,"oa_version":"Published Version","author":[{"first_name":"Themiya","last_name":"Nanayakkara","full_name":"Nanayakkara, Themiya"},{"last_name":"Brinchmann","full_name":"Brinchmann, Jarle","first_name":"Jarle"},{"full_name":"Boogaard, Leindert","last_name":"Boogaard","first_name":"Leindert"},{"full_name":"Bouwens, Rychard","last_name":"Bouwens","first_name":"Rychard"},{"first_name":"Sebastiano","full_name":"Cantalupo, Sebastiano","last_name":"Cantalupo"},{"last_name":"Feltre","full_name":"Feltre, Anna","first_name":"Anna"},{"last_name":"Kollatschny","full_name":"Kollatschny, Wolfram","first_name":"Wolfram"},{"full_name":"Marino, Raffaella Anna","last_name":"Marino","first_name":"Raffaella Anna"},{"last_name":"Maseda","full_name":"Maseda, Michael","first_name":"Michael"},{"last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J"},{"first_name":"Mieke","last_name":"Paalvast","full_name":"Paalvast, Mieke"},{"last_name":"Richard","full_name":"Richard, Johan","first_name":"Johan"},{"full_name":"Verhamme, Anne","last_name":"Verhamme","first_name":"Anne"}],"year":"2019","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"scopus_import":"1","extern":"1","article_number":"A89","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","intvolume":"       648","oa":1,"volume":648,"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1902.05960"}],"related_material":{"link":[{"url":"https://doi.org/10.1051/0004-6361/201834565e","relation":"erratum"}]},"_id":"11499","date_created":"2022-07-06T09:07:06Z","external_id":{"arxiv":["1902.05960"]},"publication":"Astronomy & Astrophysics","date_published":"2019-04-16T00:00:00Z","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: ISM / galaxies: star formation / galaxies: evolution / galaxies: high-redshift"],"article_processing_charge":"No","date_updated":"2022-07-19T09:36:08Z","title":"Exploring He II λ1640 emission line properties at z ∼2−4","month":"04"},{"article_type":"original","type":"journal_article","citation":{"ieee":"G. de La Vieuville <i>et al.</i>, “Faint end of the z ∼ 3–7 luminosity function of Lyman-alpha emitters behind lensing clusters observed with MUSE,” <i>Astronomy &#38; Astrophysics</i>, vol. 628. EDP Sciences, 2019.","apa":"de La Vieuville, G., Bina, D., Pello, R., Mahler, G., Richard, J., Drake, A. B., … Soucail, G. (2019). Faint end of the z ∼ 3–7 luminosity function of Lyman-alpha emitters behind lensing clusters observed with MUSE. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201834471\">https://doi.org/10.1051/0004-6361/201834471</a>","short":"G. de La Vieuville, D. Bina, R. Pello, G. Mahler, J. Richard, A.B. Drake, E.C. Herenz, F.E. Bauer, B. Clément, D. Lagattuta, N. Laporte, J. Martinez, V. Patrício, L. Wisotzki, J. Zabl, R.J. Bouwens, T. Contini, T. Garel, B. Guiderdoni, R.A. Marino, M.V. Maseda, J.J. Matthee, J. Schaye, G. Soucail, Astronomy &#38; Astrophysics 628 (2019).","mla":"de La Vieuville, G., et al. “Faint End of the z ∼ 3–7 Luminosity Function of Lyman-Alpha Emitters behind Lensing Clusters Observed with MUSE.” <i>Astronomy &#38; Astrophysics</i>, vol. 628, A3, EDP Sciences, 2019, doi:<a href=\"https://doi.org/10.1051/0004-6361/201834471\">10.1051/0004-6361/201834471</a>.","ista":"de La Vieuville G, Bina D, Pello R, Mahler G, Richard J, Drake AB, Herenz EC, Bauer FE, Clément B, Lagattuta D, Laporte N, Martinez J, Patrício V, Wisotzki L, Zabl J, Bouwens RJ, Contini T, Garel T, Guiderdoni B, Marino RA, Maseda MV, Matthee JJ, Schaye J, Soucail G. 2019. Faint end of the z ∼ 3–7 luminosity function of Lyman-alpha emitters behind lensing clusters observed with MUSE. Astronomy &#38; Astrophysics. 628, A3.","chicago":"La Vieuville, G. de, D. Bina, R. Pello, G. Mahler, J. Richard, A. B. Drake, E. C. Herenz, et al. “Faint End of the z ∼ 3–7 Luminosity Function of Lyman-Alpha Emitters behind Lensing Clusters Observed with MUSE.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2019. <a href=\"https://doi.org/10.1051/0004-6361/201834471\">https://doi.org/10.1051/0004-6361/201834471</a>.","ama":"de La Vieuville G, Bina D, Pello R, et al. Faint end of the z ∼ 3–7 luminosity function of Lyman-alpha emitters behind lensing clusters observed with MUSE. <i>Astronomy &#38; Astrophysics</i>. 2019;628. doi:<a href=\"https://doi.org/10.1051/0004-6361/201834471\">10.1051/0004-6361/201834471</a>"},"quality_controlled":"1","publication_status":"published","abstract":[{"text":"Contact. This paper presents the results obtained with the Multi-Unit Spectroscopic Explorer (MUSE) at the ESO Very Large Telescope on the faint end of the Lyman-alpha luminosity function (LF) based on deep observations of four lensing clusters. The goal of our project is to set strong constraints on the relative contribution of the Lyman-alpha emitter (LAE) population to cosmic reionization.\r\n\r\nAims. The precise aim of the present study is to further constrain the abundance of LAEs by taking advantage of the magnification provided by lensing clusters to build a blindly selected sample of galaxies which is less biased than current blank field samples in redshift and luminosity. By construction, this sample of LAEs is complementary to those built from deep blank fields, whether observed by MUSE or by other facilities, and makes it possible to determine the shape of the LF at fainter levels, as well as its evolution with redshift.\r\n\r\nMethods. We selected a sample of 156 LAEs with redshifts between 2.9 ≤ z ≤ 6.7 and magnification-corrected luminosities in the range 39 ≲ log LLyα [erg s−1] ≲43. To properly take into account the individual differences in detection conditions between the LAEs when computing the LF, including lensing configurations, and spatial and spectral morphologies, the non-parametric 1/Vmax method was adopted. The price to pay to benefit from magnification is a reduction of the effective volume of the survey, together with a more complex analysis procedure to properly determine the effective volume Vmax for each galaxy. In this paper we present a complete procedure for the determination of the LF based on IFU detections in lensing clusters. This procedure, including some new methods for masking, effective volume integration and (individual) completeness determinations, has been fully automated when possible, and it can be easily generalized to the analysis of IFU observations in blank fields.\r\n\r\nResults. As a result of this analysis, the Lyman-alpha LF has been obtained in four different redshift bins: 2.9 <  z <  6, 7, 2.9 <  z <  4.0, 4.0 <  z <  5.0, and 5.0 <  z <  6.7 with constraints down to log LLyα = 40.5. From our data only, no significant evolution of LF mean slope can be found. When performing a Schechter analysis also including data from the literature to complete the present sample towards the brightest luminosities, a steep faint end slope was measured varying from α = −1.69−0.08+0.08 to α = −1.87−0.12+0.12 between the lowest and the highest redshift bins.\r\n\r\nConclusions. The contribution of the LAE population to the star formation rate density at z ∼ 6 is ≲50% depending on the luminosity limit considered, which is of the same order as the Lyman-break galaxy (LBG) contribution. The evolution of the LAE contribution with redshift depends on the assumed escape fraction of Lyman-alpha photons, and appears to slightly increase with increasing redshift when this fraction is conservatively set to one. Depending on the intersection between the LAE/LBG populations, the contribution of the observed galaxies to the ionizing flux may suffice to keep the universe ionized at z ∼ 6.","lang":"eng"}],"language":[{"iso":"eng"}],"status":"public","publisher":"EDP Sciences","day":"25","doi":"10.1051/0004-6361/201834471","arxiv":1,"oa_version":"Published Version","author":[{"first_name":"G.","full_name":"de La Vieuville, G.","last_name":"de La Vieuville"},{"last_name":"Bina","full_name":"Bina, D.","first_name":"D."},{"first_name":"R.","last_name":"Pello","full_name":"Pello, R."},{"last_name":"Mahler","full_name":"Mahler, G.","first_name":"G."},{"full_name":"Richard, J.","last_name":"Richard","first_name":"J."},{"first_name":"A. B.","full_name":"Drake, A. B.","last_name":"Drake"},{"last_name":"Herenz","full_name":"Herenz, E. C.","first_name":"E. C."},{"last_name":"Bauer","full_name":"Bauer, F. E.","first_name":"F. E."},{"first_name":"B.","last_name":"Clément","full_name":"Clément, B."},{"first_name":"D.","last_name":"Lagattuta","full_name":"Lagattuta, D."},{"first_name":"N.","full_name":"Laporte, N.","last_name":"Laporte"},{"last_name":"Martinez","full_name":"Martinez, J.","first_name":"J."},{"full_name":"Patrício, V.","last_name":"Patrício","first_name":"V."},{"last_name":"Wisotzki","full_name":"Wisotzki, L.","first_name":"L."},{"last_name":"Zabl","full_name":"Zabl, J.","first_name":"J."},{"full_name":"Bouwens, R. J.","last_name":"Bouwens","first_name":"R. J."},{"last_name":"Contini","full_name":"Contini, T.","first_name":"T."},{"first_name":"T.","full_name":"Garel, T.","last_name":"Garel"},{"first_name":"B.","last_name":"Guiderdoni","full_name":"Guiderdoni, B."},{"last_name":"Marino","full_name":"Marino, R. A.","first_name":"R. A."},{"full_name":"Maseda, M. V.","last_name":"Maseda","first_name":"M. V."},{"first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J"},{"full_name":"Schaye, J.","last_name":"Schaye","first_name":"J."},{"full_name":"Soucail, G.","last_name":"Soucail","first_name":"G."}],"year":"2019","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"scopus_import":"1","extern":"1","article_number":"A3","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","acknowledgement":"We thank the anonymous referee for their critical review and useful suggestions. This work has been carried out thanks to the support of the OCEVU Labex (ANR-11-LABX-0060) and the A*MIDEX project (ANR-11-IDEX-0001-02) funded by the “Investissements d’Avenir” French government programme managed by the ANR. Partially funded by the ERC starting grant CALENDS (JR, VP, BC, JM), the Agence Nationale de la recherche bearing the reference ANR-13-BS05-0010-02 (FOGHAR), and the “Programme National de Cosmologie and Galaxies” (PNCG) of CNRS/INSU, France. GdV, RP, JR, GM, JM, BC, and VP also acknowledge support by the Programa de Cooperacion Cientifica – ECOS SUD Program C16U02. NL acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No 669253), ABD acknowledges support from the ERC advanced grant “Cosmic Gas”. LW acknowledges support by the Competitive Fund of the Leibniz Association through grant SAW-2015-AIP-2, and TG acknowledges support from the European Research Council under grant agreement ERC-stg-757258 (TRIPLE).. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 060.A-9345, 094.A-0115, 095.A-0181, 096.A-0710, 097.A0269, 100.A-0249, and 294.A-5032. Also based on observations obtained with the NASA/ESA Hubble Space Telescope, retrieved from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute (STScI). STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. This research made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration 2013). All plots in this paper were created using Matplotlib (Hunter 2007).","intvolume":"       628","oa":1,"volume":628,"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1905.13696"}],"_id":"11505","date_created":"2022-07-06T10:09:36Z","external_id":{"arxiv":["1905.13696"]},"publication":"Astronomy & Astrophysics","date_published":"2019-07-25T00:00:00Z","keyword":["Space and Planetary Science","Astronomy and Astrophysics","gravitational lensing: strong / galaxies: high-redshift / dark ages","reionization","first stars / galaxies: clusters: general / galaxies: luminosity function","mass function"],"article_processing_charge":"No","date_updated":"2022-07-19T09:36:31Z","title":"Faint end of the z ∼ 3–7 luminosity function of Lyman-alpha emitters behind lensing clusters observed with MUSE","month":"07"},{"publisher":"EDP Sciences","day":"26","doi":"10.1051/0004-6361/201833075","arxiv":1,"oa_version":"Published Version","year":"2019","author":[{"last_name":"Sobral","full_name":"Sobral, David","first_name":"David"},{"last_name":"Matthee","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"}],"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"article_type":"original","type":"journal_article","citation":{"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).","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>","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>","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>."},"quality_controlled":"1","abstract":[{"lang":"eng","text":"Lyman-α (Lyα) is intrinsically the brightest line emitted from active galaxies. While it originates from many physical processes, for star-forming galaxies the intrinsic Lyα luminosity is a direct tracer of the Lyman-continuum (LyC) radiation produced by the most massive O- and early-type B-stars (M⋆ ≳ 10 M⊙) with lifetimes of a few Myrs. As such, Lyα luminosity should be an excellent instantaneous star formation rate (SFR) indicator. However, its resonant nature and susceptibility to dust as a rest-frame UV photon makes Lyα very hard to interpret due to the uncertain Lyα escape fraction, fesc, Lyα. Here we explore results from the CAlibrating LYMan-α with Hα (CALYMHA) survey at z = 2.2, follow-up of Lyα emitters (LAEs) at z = 2.2 − 2.6 and a z ∼ 0−0.3 compilation of LAEs to directly measure fesc, Lyα with Hα. We derive a simple empirical relation that robustly retrieves fesc, Lyα as a function of Lyα rest-frame EW (EW0): fesc,Lyα = 0.0048 EW0[Å] ± 0.05 and we show that it constrains a well-defined anti-correlation between ionisation efficiency (ξion) and dust extinction in LAEs. Observed Lyα luminosities and EW0 are easy measurable quantities at high redshift, thus making our relation a practical tool to estimate intrinsic Lyα and LyC luminosities under well controlled and simple assumptions. Our results allow observed Lyα luminosities to be used to compute SFRs for LAEs at z ∼ 0−2.6 within ±0.2 dex of the Hα dust corrected SFRs. We apply our empirical SFR(Lyα,EW0) calibration to several sources at z ≥ 2.6 to find that star-forming LAEs have SFRs typically ranging from 0.1 to 20 M⊙ yr−1 and that our calibration might be even applicable for the most luminous LAEs within the epoch of re-ionisation. Our results imply high ionisation efficiencies (log10[ξion/Hz erg−1] = 25.4−25.6) and low dust content in LAEs across cosmic time, and will be easily tested with future observations with JWST which can obtain Hα and Hβ measurements for high-redshift LAEs."}],"publication_status":"published","status":"public","language":[{"iso":"eng"}],"_id":"11507","external_id":{"arxiv":["1803.08923"]},"date_created":"2022-07-06T11:08:16Z","publication":"Astronomy & Astrophysics","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift / galaxies: star formation / galaxies: statistics / galaxies: evolution / galaxies: formation / galaxies: ISM"],"article_processing_charge":"No","date_published":"2019-03-26T00:00:00Z","date_updated":"2022-07-19T09:37:20Z","title":"Predicting Lyα escape fractions with a simple observable: Lyα in emission as an empirically calibrated star formation rate indicator","month":"03","extern":"1","scopus_import":"1","article_number":"A157","oa":1,"intvolume":"       623","acknowledgement":"We thank the anonymous referees for multiple comments and suggestions which have improved the manuscript. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. We have benefited greatly from the publicly available programming language PYTHON, including the NUMPY & SCIPY (Van Der Walt et al. 2011; Jones et al. 2001), MATPLOTLIB (Hunter 2007) and ASTROPY (Astropy Collaboration 2013) packages, and the TOPCAT analysis program (Taylor 2013). The results and samples of LAEs used for this paper are publicly available (see e.g. Sobral et al. 2017, 2018a) and we also provide the toy model used as a PYTHON script.","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"url":"https://arxiv.org/abs/1803.08923","open_access":"1"}],"volume":623},{"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1811.00556"}],"volume":489,"intvolume":"       489","oa":1,"issue":"1","acknowledgement":"We thank the anonymous referee for their useful comments and suggestions that helped improve this study. AAK acknowledges that this work was supported by NASA Headquarters under the NASA Earth and Space Science Fellowship Program – Grant NNX16AO92H. JM acknowledges support from the ETH Zwicky fellowship. RKC acknowledges funding from STFC via a studentship. APA acknowledges support from the Fundac¸ao para a Ci ˜ encia e a Tecnologia FCT through the fellowship PD/BD/52706/2014 and the research grant UID/FIS/04434/2013. JC and SS both acknowledge their support from the Lancaster University PhD Fellowship. We have benefited greatly from the publicly available programming language PYTHON, including the NUMPY, SCIPY, MATPLOTLIB, SCIKIT-LEARN, and ASTROPY packages, as well as the TOPCAT analysis program. The SC4K samples used in this paper are all publicly available for use by the community (Sobral et al. 2018a). The catalogue is also available on the COSMOS IPAC website (https://irsa.ipac.caltech.edu/data/COSMOS/overview.html).","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","extern":"1","scopus_import":"1","month":"10","title":"The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities","date_updated":"2022-08-19T06:38:42Z","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: haloes","galaxies: high-redshift","galaxies: star formation","cosmology: observations","large-scale structure of Universe"],"article_processing_charge":"No","date_published":"2019-10-01T00:00:00Z","page":"555-573","publication":"Monthly Notices of the Royal Astronomical Society","external_id":{"arxiv":["1811.00556"]},"date_created":"2022-07-07T13:01:03Z","_id":"11535","status":"public","language":[{"iso":"eng"}],"publication_status":"published","abstract":[{"text":"We investigate the clustering and halo properties of ∼5000 Ly α-selected emission-line galaxies (LAEs) from the Slicing COSMOS 4K (SC4K) and from archival NB497 imaging of SA22 split in 15 discrete redshift slices between z ∼ 2.5 and 6. We measure clustering lengths of r0 ∼ 3–6 h−1 Mpc and typical halo masses of ∼1011 M⊙ for our narrowband-selected LAEs with typical LLy α ∼ 1042–43 erg s−1. The intermediate-band-selected LAEs are observed to have r0 ∼ 3.5–15 h−1 Mpc with typical halo masses of ∼1011–12 M⊙ and typical LLy α ∼ 1043–43.6 erg s−1. We find a strong, redshift-independent correlation between halo mass and Ly α luminosity normalized by the characteristic Ly α luminosity, L⋆(z). The faintest LAEs (L ∼ 0.1 L⋆(z)) typically identified by deep narrowband surveys are found in 1010 M⊙ haloes and the brightest LAEs (L ∼ 7 L⋆(z)) are found in ∼5 × 1012 M⊙ haloes. A dependency on the rest-frame 1500 Å UV luminosity, MUV, is also observed where the halo masses increase from 1011 to 1013 M⊙ for MUV ∼ −19 to −23.5 mag. Halo mass is also observed to increase from 109.8 to 1012 M⊙ for dust-corrected UV star formation rates from ∼0.6 to 10 M⊙ yr−1 and continues to increase up to 1013 M⊙ in halo mass, where the majority of those sources are active galactic nuclei. All the trends we observe are found to be redshift independent. Our results reveal that LAEs are the likely progenitors of a wide range of galaxies depending on their luminosity, from dwarf-like, to Milky Way-type, to bright cluster galaxies. LAEs therefore provide unique insight into the early formation and evolution of the galaxies we observe in the local Universe.","lang":"eng"}],"quality_controlled":"1","citation":{"ama":"Khostovan AA, Sobral D, Mobasher B, et al. The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities. <i>Monthly Notices of the Royal Astronomical Society</i>. 2019;489(1):555-573. doi:<a href=\"https://doi.org/10.1093/mnras/stz2149\">10.1093/mnras/stz2149</a>","chicago":"Khostovan, A A, D Sobral, B Mobasher, Jorryt J Matthee, R K Cochrane, N Chartab, M Jafariyazani, A Paulino-Afonso, S Santos, and J Calhau. “The Clustering of Typical Ly α Emitters from z ∼ 2.5–6: Host Halo Masses Depend on Ly α and UV Luminosities.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2019. <a href=\"https://doi.org/10.1093/mnras/stz2149\">https://doi.org/10.1093/mnras/stz2149</a>.","ista":"Khostovan AA, Sobral D, Mobasher B, Matthee JJ, Cochrane RK, Chartab N, Jafariyazani M, Paulino-Afonso A, Santos S, Calhau J. 2019. The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities. Monthly Notices of the Royal Astronomical Society. 489(1), 555–573.","mla":"Khostovan, A. A., et al. “The Clustering of Typical Ly α Emitters from z ∼ 2.5–6: Host Halo Masses Depend on Ly α and UV Luminosities.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 489, no. 1, Oxford University Press, 2019, pp. 555–73, doi:<a href=\"https://doi.org/10.1093/mnras/stz2149\">10.1093/mnras/stz2149</a>.","apa":"Khostovan, A. A., Sobral, D., Mobasher, B., Matthee, J. J., Cochrane, R. K., Chartab, N., … Calhau, J. (2019). The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stz2149\">https://doi.org/10.1093/mnras/stz2149</a>","short":"A.A. Khostovan, D. Sobral, B. Mobasher, J.J. Matthee, R.K. Cochrane, N. Chartab, M. Jafariyazani, A. Paulino-Afonso, S. Santos, J. Calhau, Monthly Notices of the Royal Astronomical Society 489 (2019) 555–573.","ieee":"A. A. Khostovan <i>et al.</i>, “The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 489, no. 1. Oxford University Press, pp. 555–573, 2019."},"type":"journal_article","article_type":"original","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"year":"2019","author":[{"full_name":"Khostovan, A A","last_name":"Khostovan","first_name":"A A"},{"full_name":"Sobral, D","last_name":"Sobral","first_name":"D"},{"last_name":"Mobasher","full_name":"Mobasher, B","first_name":"B"},{"first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J"},{"last_name":"Cochrane","full_name":"Cochrane, R K","first_name":"R K"},{"full_name":"Chartab, N","last_name":"Chartab","first_name":"N"},{"first_name":"M","last_name":"Jafariyazani","full_name":"Jafariyazani, M"},{"last_name":"Paulino-Afonso","full_name":"Paulino-Afonso, A","first_name":"A"},{"last_name":"Santos","full_name":"Santos, S","first_name":"S"},{"last_name":"Calhau","full_name":"Calhau, J","first_name":"J"}],"oa_version":"Preprint","arxiv":1,"doi":"10.1093/mnras/stz2149","day":"01","publisher":"Oxford University Press"},{"article_processing_charge":"No","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","galaxies: ISM","cosmology: observations","dark ages","reionization","first stars","early Universe"],"date_published":"2019-01-01T00:00:00Z","title":"On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components","date_updated":"2022-08-19T06:49:36Z","month":"01","_id":"11541","external_id":{"arxiv":["1710.08422"]},"date_created":"2022-07-08T10:40:05Z","publication":"Monthly Notices of the Royal Astronomical Society","page":"2422-2441","oa":1,"intvolume":"       482","acknowledgement":"We thank the anonymous reviewer for the numerous detailed comments that led us to greatly improve the quality, extent, and statistical robustness of this work. DS acknowledges financial support from the Netherlands Organisation for Scientific research through a Veni fellowship. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. AF acknowledges support from the ERC Advanced Grant INTERSTELLAR H2020/740120. BD acknowledges financial support from NASA through the Astrophysics Data Analysis Program, grant number NNX12AE20G and the National Science Foundation, grant number 1716907. We are thankful for several discussions and constructive comments from Johannes Zabl, Eros Vanzella, Bo Milvang-Jensen, Henry McCracken, Max Gronke, Mark Dijkstra, Richard Ellis, and Nicolas Laporte. We also thank Umar Burhanudin and Izzy Garland for taking part in the XGAL internship in Lancaster and for exploring the HST grism data independently. Based on observations obtained with HST/WFC3 programs 12578, 14495, and 14596. Based on observations of the National Japanese Observatory with the Suprime-Cam on the Subaru telescope (S14A-086) on the big island of Hawaii. This work is based in part on data products produced at TERAPIX available at the Canadian Astronomy Data Centre as part of the Canada–France–Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme IDs 294.A-5018, 294.A-5039, 092.A 0786, 093.A-0561, 097.A0043, 097.A-0943, 098.A-0819, 298.A-5012, and 179.A-2005, and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. The authors acknowledge the award of service time (SW2014b20) on the William Herschel Telescope (WHT). WHT and its service programme are operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. This research was supported by the Munich Institute for Astro- and Particle Physics of the DFG cluster of excellence ‘Origin and Structure of the Universe’. We have benefitted immensely from the public available programming language PYTHON, including NUMPY and SCIPY (Jones et al. 2001; Van Der Walt, Colbert & Varoquaux 2011), MATPLOTLIB (Hunter 2007), ASTROPY (Astropy Collaboration et al. 2013), and the TOPCAT analysis program (Taylor 2013). This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France. All data used for this paper are publicly available, and we make all reduced data available with the refereed paper.","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","issue":"2","main_file_link":[{"url":"https://arxiv.org/abs/1710.08422","open_access":"1"}],"volume":482,"extern":"1","scopus_import":"1","year":"2019","author":[{"first_name":"David","full_name":"Sobral, David","last_name":"Sobral"},{"orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","last_name":"Matthee","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"full_name":"Brammer, Gabriel","last_name":"Brammer","first_name":"Gabriel"},{"full_name":"Ferrara, Andrea","last_name":"Ferrara","first_name":"Andrea"},{"last_name":"Alegre","full_name":"Alegre, Lara","first_name":"Lara"},{"last_name":"Röttgering","full_name":"Röttgering, Huub","first_name":"Huub"},{"last_name":"Schaerer","full_name":"Schaerer, Daniel","first_name":"Daniel"},{"first_name":"Bahram","full_name":"Mobasher, Bahram","last_name":"Mobasher"},{"full_name":"Darvish, Behnam","last_name":"Darvish","first_name":"Behnam"}],"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"publisher":"Oxford University Press","day":"01","doi":"10.1093/mnras/sty2779","oa_version":"Preprint","arxiv":1,"quality_controlled":"1","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."}],"publication_status":"published","status":"public","language":[{"iso":"eng"}],"article_type":"original","type":"journal_article","citation":{"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>.","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.","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>.","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>","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.","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.","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>"}},{"oa_version":"Published Version","arxiv":1,"doi":"10.1051/0004-6361/201833528","day":"19","publisher":"EDP Sciences","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"year":"2018","author":[{"orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","last_name":"Matthee","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"full_name":"Sobral, David","last_name":"Sobral","first_name":"David"},{"last_name":"Gronke","full_name":"Gronke, Max","first_name":"Max"},{"last_name":"Paulino-Afonso","full_name":"Paulino-Afonso, Ana","first_name":"Ana"},{"first_name":"Mauro","last_name":"Stefanon","full_name":"Stefanon, Mauro"},{"last_name":"Röttgering","full_name":"Röttgering, Huub","first_name":"Huub"}],"citation":{"apa":"Matthee, J. J., Sobral, D., Gronke, M., Paulino-Afonso, A., Stefanon, M., &#38; Röttgering, H. (2018). Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly contributing to the reionisation of the universe. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201833528\">https://doi.org/10.1051/0004-6361/201833528</a>","short":"J.J. Matthee, D. Sobral, M. Gronke, A. Paulino-Afonso, M. Stefanon, H. Röttgering, Astronomy &#38; Astrophysics 619 (2018).","ieee":"J. J. Matthee, D. Sobral, M. Gronke, A. Paulino-Afonso, M. Stefanon, and H. Röttgering, “Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly contributing to the reionisation of the universe,” <i>Astronomy &#38; Astrophysics</i>, vol. 619. EDP Sciences, 2018.","chicago":"Matthee, Jorryt J, David Sobral, Max Gronke, Ana Paulino-Afonso, Mauro Stefanon, and Huub Röttgering. “Confirmation of Double Peaked Lyα Emission at z = 6.593: Witnessing a Galaxy Directly Contributing to the Reionisation of the Universe.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2018. <a href=\"https://doi.org/10.1051/0004-6361/201833528\">https://doi.org/10.1051/0004-6361/201833528</a>.","ama":"Matthee JJ, Sobral D, Gronke M, Paulino-Afonso A, Stefanon M, Röttgering H. Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly contributing to the reionisation of the universe. <i>Astronomy &#38; Astrophysics</i>. 2018;619. doi:<a href=\"https://doi.org/10.1051/0004-6361/201833528\">10.1051/0004-6361/201833528</a>","ista":"Matthee JJ, Sobral D, Gronke M, Paulino-Afonso A, Stefanon M, Röttgering H. 2018. Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly contributing to the reionisation of the universe. Astronomy &#38; Astrophysics. 619, A136.","mla":"Matthee, Jorryt J., et al. “Confirmation of Double Peaked Lyα Emission at z = 6.593: Witnessing a Galaxy Directly Contributing to the Reionisation of the Universe.” <i>Astronomy &#38; Astrophysics</i>, vol. 619, A136, EDP Sciences, 2018, doi:<a href=\"https://doi.org/10.1051/0004-6361/201833528\">10.1051/0004-6361/201833528</a>."},"type":"journal_article","article_type":"original","status":"public","language":[{"iso":"eng"}],"publication_status":"published","abstract":[{"lang":"eng","text":"Distant luminous Lyman-α emitters (LAEs) are excellent targets for spectroscopic observations of galaxies in the epoch of reionisation (EoR). We present deep high-resolution (R = 5000) VLT/X-shooter observations, along with an extensive collection of photometric data of COLA1, a proposed double peaked LAE at z = 6.6. We rule out the possibility that COLA1’s emission line is an [OII] doublet at z = 1.475 on the basis of i) the asymmetric red line-profile and flux ratio of the peaks (blue/red=0.31 ± 0.03) and ii) an unphysical [OII]/Hα ratio ([OII]/Hα >  22). We show that COLA1’s observed B-band flux is explained by a faint extended foreground LAE, for which we detect Lyα and [OIII] at z = 2.142. We thus conclude that COLA1 is a real double-peaked LAE at z = 6.593, the first discovered at z >  6. COLA1 is UV luminous (M1500 = −21.6 ± 0.3), has a high equivalent width (EW0,Lyα = 120−40+50 Å) and very compact Lyα emission (r50,Lyα = 0.33−0.04+0.07 kpc). Relatively weak inferred Hβ+[OIII] line-emission from Spitzer/IRAC indicates an extremely low metallicity of Z <  1/20 Z⊙ or reduced strength of nebular lines due to high escape of ionising photons. The small Lyα peak separation of 220 ± 20 km s−1 implies a low HI column density and an ionising photon escape fraction of ≈15 − 30%, providing the first direct evidence that such galaxies contribute actively to the reionisation of the Universe at z >  6. Based on simple estimates, we find that COLA1 could have provided just enough photons to reionise its own ≈0.3 pMpc (2.3 cMpc) bubble, allowing the blue Lyα line to be observed. However, we also discuss alternative scenarios explaining the detected double peaked nature of COLA1. Our results show that future high-resolution observations of statistical samples of double peaked LAEs at z >  5 are a promising probe of the occurrence of ionised regions around galaxies in the EoR."}],"quality_controlled":"1","publication":"Astronomy & Astrophysics","external_id":{"arxiv":["1805.11621"]},"date_created":"2022-07-06T11:14:23Z","_id":"11508","month":"11","title":"Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly contributing to the reionisation of the universe","date_updated":"2022-07-19T09:32:08Z","article_processing_charge":"No","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift / galaxies: formation / dark ages / reionization / first stars / techniques: spectroscopic / intergalactic medium"],"date_published":"2018-11-19T00:00:00Z","extern":"1","scopus_import":"1","main_file_link":[{"url":"https://arxiv.org/abs/1805.11621","open_access":"1"}],"volume":619,"oa":1,"intvolume":"       619","acknowledgement":"JM acknowledges the award of a Huygens PhD fellowship from Leiden University. MG acknowledges support from NASA grant NNX17AK58G. APA, PhD::SPACE fellow, acknowledges support from the FCT through the fellowship PD/BD/52706/2014. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 294.A-5018, 098.A-0819, 099.A-0254 and 0100.A-0213. We are grateful for the excellent data-sets from the COSMOS and UltraVISTA survey teams. This research was supported by the Munich Institute for Astro- and Particle Physics (MIAPP) of the DFG cluster of excellence “Origin and Structure of the Universe”. We thank the referee for their comments that improved the paper. We also thank Christoph Behrens, Len Cowie, Koki Kakiichi, Peter Laursen, Charlotte Mason, Eros Vanzella, Lewis Weinberger and Johannes Zabl for discussions. We have benefited from the public available programming language Python, including the numpy, matplotlib, scipy and astropy packages (Hunter 2007; Astropy Collaboration 2013), the astronomical imaging tools Swarp (Bertin 2010) and ds9 and the Topcat analysis tool (Taylor 2013).","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","article_number":"A136"},{"article_type":"original","citation":{"ama":"Khostovan AA, Sobral D, Mobasher B, et al. The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar mass. <i>Monthly Notices of the Royal Astronomical Society</i>. 2018;478(3):2999-3015. doi:<a href=\"https://doi.org/10.1093/mnras/sty925\">10.1093/mnras/sty925</a>","chicago":"Khostovan, A A, D Sobral, B Mobasher, P N Best, I Smail, Jorryt J Matthee, B Darvish, H Nayyeri, S Hemmati, and J P Stott. “The Clustering of H β + [O III] and [O II] Emitters since z ∼ 5: Dependencies with Line Luminosity and Stellar Mass.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2018. <a href=\"https://doi.org/10.1093/mnras/sty925\">https://doi.org/10.1093/mnras/sty925</a>.","mla":"Khostovan, A. A., et al. “The Clustering of H β + [O III] and [O II] Emitters since z ∼ 5: Dependencies with Line Luminosity and Stellar Mass.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 478, no. 3, Oxford University Press, 2018, pp. 2999–3015, doi:<a href=\"https://doi.org/10.1093/mnras/sty925\">10.1093/mnras/sty925</a>.","ista":"Khostovan AA, Sobral D, Mobasher B, Best PN, Smail I, Matthee JJ, Darvish B, Nayyeri H, Hemmati S, Stott JP. 2018. The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar mass. Monthly Notices of the Royal Astronomical Society. 478(3), 2999–3015.","apa":"Khostovan, A. A., Sobral, D., Mobasher, B., Best, P. N., Smail, I., Matthee, J. J., … Stott, J. P. (2018). The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar mass. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/sty925\">https://doi.org/10.1093/mnras/sty925</a>","short":"A.A. Khostovan, D. Sobral, B. Mobasher, P.N. Best, I. Smail, J.J. Matthee, B. Darvish, H. Nayyeri, S. Hemmati, J.P. Stott, Monthly Notices of the Royal Astronomical Society 478 (2018) 2999–3015.","ieee":"A. A. Khostovan <i>et al.</i>, “The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar mass,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 478, no. 3. Oxford University Press, pp. 2999–3015, 2018."},"type":"journal_article","quality_controlled":"1","abstract":[{"text":"We investigate the clustering properties of ∼7000 H β + [O III] and [O II] narrowband-selected emitters at z ∼ 0.8–4.7 from the High-z Emission Line Survey. We find clustering lengths, r0, of 1.5–4.0 h−1 Mpc and minimum dark matter halo masses of 1010.7–12.1 M⊙ for our z = 0.8–3.2 H β + [O III] emitters and r0 ∼ 2.0–8.3 h−1 Mpc and halo masses of 1011.5–12.6 M⊙ for our z = 1.5–4.7 [O II] emitters. We find r0 to strongly increase both with increasing line luminosity and redshift. By taking into account the evolution of the characteristic line luminosity, L⋆(z), and using our model predictions of halo mass given r0, we find a strong, redshift-independent increasing trend between L/L⋆(z) and minimum halo mass. The faintest H β + [O III] emitters are found to reside in 109.5 M⊙ haloes and the brightest emitters in 1013.0 M⊙ haloes. For [O II] emitters, the faintest emitters are found in 1010.5 M⊙ haloes and the brightest emitters in 1012.6 M⊙ haloes. A redshift-independent stellar mass dependency is also observed where the halo mass increases from 1011 to 1012.5 M⊙ for stellar masses of 108.5 to 1011.5 M⊙, respectively. We investigate the interdependencies of these trends by repeating our analysis in a Lline−Mstar grid space for our most populated samples (H β + [O III] z = 0.84 and [O II] z = 1.47) and find that the line luminosity dependency is stronger than the stellar mass dependency on halo mass. For L > L⋆ emitters at all epochs, we find a relatively flat trend with halo masses of 1012.5–13 M⊙, which may be due to quenching mechanisms in massive haloes that is consistent with a transitional halo mass predicted by models.","lang":"eng"}],"publication_status":"published","status":"public","language":[{"iso":"eng"}],"publisher":"Oxford University Press","day":"01","doi":"10.1093/mnras/sty925","oa_version":"Published Version","arxiv":1,"year":"2018","author":[{"full_name":"Khostovan, A A","last_name":"Khostovan","first_name":"A A"},{"last_name":"Sobral","full_name":"Sobral, D","first_name":"D"},{"first_name":"B","full_name":"Mobasher, B","last_name":"Mobasher"},{"first_name":"P N","full_name":"Best, P N","last_name":"Best"},{"full_name":"Smail, I","last_name":"Smail","first_name":"I"},{"first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J"},{"first_name":"B","full_name":"Darvish, B","last_name":"Darvish"},{"last_name":"Nayyeri","full_name":"Nayyeri, H","first_name":"H"},{"first_name":"S","full_name":"Hemmati, S","last_name":"Hemmati"},{"first_name":"J P","last_name":"Stott","full_name":"Stott, J P"}],"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"extern":"1","scopus_import":"1","intvolume":"       478","issue":"3","acknowledgement":"We thank the anonymous referee for their useful comments and suggestions that improved this study. AAK thanks Anahita Alavi and Irene Shivaei for useful discussion in the making of this paper. AAK acknowledges that this work was supported by NASA Headquarters under the NASA Earth and Space Science Fellowship Program – Grant NNX16AO92H. DS acknowledges financial support from the Netherlands Organization for Scientific Research (NWO) through a Veni fellowship and from Lancaster University through an Early Career Internal Grant A100679. PNB is grateful for support from STFC via grant STM001229/1. IRS acknowledges support from STFC (ST/L00075X/1), the ERC Advanced Grant DUSTYGAL (321334), and a Royal Society/Wolfson Merit award. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. BD acknowledges financial support from NASA through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G.","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"url":"https://arxiv.org/abs/1705.01101"}],"volume":478,"_id":"11549","external_id":{"arxiv":["1705.01101"]},"date_created":"2022-07-08T11:48:48Z","publication":"Monthly Notices of the Royal Astronomical Society","page":"2999-3015","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: haloes","galaxies: high-redshift","galaxies: star formation","cosmology: observations","large-scale structure of Universe"],"article_processing_charge":"No","date_published":"2018-08-01T00:00:00Z","date_updated":"2022-08-19T06:53:39Z","title":"The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar mass","month":"08"},{"date_updated":"2022-08-19T06:58:06Z","title":"Kiloparsec-scale gaseous clumps and star formation at z = 5–7","month":"07","date_published":"2018-07-01T00:00:00Z","article_processing_charge":"No","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","galaxies: ISM","galaxies: formation"],"publication":"Monthly Notices of the Royal Astronomical Society","page":"1170-1184","_id":"11555","date_created":"2022-07-11T08:05:42Z","external_id":{"arxiv":["1712.03985"]},"volume":478,"main_file_link":[{"url":"https://arxiv.org/abs/1712.03985","open_access":"1"}],"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.","issue":"1","intvolume":"       478","oa":1,"scopus_import":"1","extern":"1","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"author":[{"full_name":"Carniani, S","last_name":"Carniani","first_name":"S"},{"full_name":"Maiolino, R","last_name":"Maiolino","first_name":"R"},{"full_name":"Amorin, R","last_name":"Amorin","first_name":"R"},{"first_name":"L","last_name":"Pentericci","full_name":"Pentericci, L"},{"first_name":"A","last_name":"Pallottini","full_name":"Pallottini, A"},{"first_name":"A","full_name":"Ferrara, A","last_name":"Ferrara"},{"full_name":"Willott, C J","last_name":"Willott","first_name":"C J"},{"full_name":"Smit, R","last_name":"Smit","first_name":"R"},{"full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"first_name":"D","full_name":"Sobral, D","last_name":"Sobral"},{"first_name":"P","last_name":"Santini","full_name":"Santini, P"},{"last_name":"Castellano","full_name":"Castellano, M","first_name":"M"},{"last_name":"De Barros","full_name":"De Barros, S","first_name":"S"},{"last_name":"Fontana","full_name":"Fontana, A","first_name":"A"},{"first_name":"A","full_name":"Grazian, A","last_name":"Grazian"},{"first_name":"L","last_name":"Guaita","full_name":"Guaita, L"}],"year":"2018","doi":"10.1093/mnras/sty1088","arxiv":1,"oa_version":"Preprint","publisher":"Oxford University Press","day":"01","publication_status":"published","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"}],"language":[{"iso":"eng"}],"status":"public","quality_controlled":"1","citation":{"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>.","ista":"Carniani S, Maiolino R, Amorin R, Pentericci L, Pallottini A, Ferrara A, Willott CJ, Smit R, Matthee JJ, Sobral D, Santini P, Castellano M, De Barros S, Fontana A, Grazian A, Guaita L. 2018. Kiloparsec-scale gaseous clumps and star formation at z = 5–7. Monthly Notices of the Royal Astronomical Society. 478(1), 1170–1184.","ama":"Carniani S, Maiolino R, Amorin R, et al. Kiloparsec-scale gaseous clumps and star formation at z = 5–7. <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>","chicago":"Carniani, S, R Maiolino, R Amorin, L Pentericci, A Pallottini, A Ferrara, C J Willott, et al. “Kiloparsec-Scale Gaseous Clumps and Star Formation at z = 5–7.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2018. <a href=\"https://doi.org/10.1093/mnras/sty1088\">https://doi.org/10.1093/mnras/sty1088</a>.","ieee":"S. Carniani <i>et al.</i>, “Kiloparsec-scale gaseous clumps and star formation at z = 5–7,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 478, no. 1. Oxford University Press, pp. 1170–1184, 2018.","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.","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>"},"type":"journal_article","article_type":"original"},{"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"year":"2018","author":[{"first_name":"David","full_name":"Sobral, David","last_name":"Sobral"},{"full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J"},{"first_name":"Behnam","full_name":"Darvish, Behnam","last_name":"Darvish"},{"last_name":"Smail","full_name":"Smail, Ian","first_name":"Ian"},{"last_name":"Best","full_name":"Best, Philip N","first_name":"Philip N"},{"last_name":"Alegre","full_name":"Alegre, Lara","first_name":"Lara"},{"full_name":"Röttgering, Huub","last_name":"Röttgering","first_name":"Huub"},{"first_name":"Bahram","full_name":"Mobasher, Bahram","last_name":"Mobasher"},{"first_name":"Ana","full_name":"Paulino-Afonso, Ana","last_name":"Paulino-Afonso"},{"first_name":"Andra","full_name":"Stroe, Andra","last_name":"Stroe"},{"full_name":"Oteo, Iván","last_name":"Oteo","first_name":"Iván"}],"doi":"10.1093/mnras/sty782","oa_version":"Preprint","arxiv":1,"publisher":"Oxford University Press","day":"01","abstract":[{"text":"Deep narrow-band surveys have revealed a large population of faint Ly α emitters (LAEs) in the distant Universe, but relatively little is known about the most luminous sources (⁠LLyα≳1042.7 erg s−1; LLyα≳L∗Lyα⁠). Here we present the spectroscopic follow-up of 21 luminous LAEs at z ∼ 2–3 found with panoramic narrow-band surveys over five independent extragalactic fields (≈4 × 106 Mpc3 surveyed at z ∼ 2.2 and z ∼ 3.1). We use WHT/ISIS, Keck/DEIMOS, and VLT/X-SHOOTER to study these sources using high ionization UV lines. Luminous LAEs at z ∼ 2–3 have blue UV slopes (⁠β=−2.0+0.3−0.1⁠) and high Ly α escape fractions (⁠50+20−15 per cent) and span five orders of magnitude in UV luminosity (MUV ≈ −19 to −24). Many (70 per cent) show at least one high ionization rest-frame UV line such as C IV, N V, C III], He II or O III], typically blue-shifted by ≈100–200 km s−1 relative to Ly α. Their Ly α profiles reveal a wide variety of shapes, including significant blue-shifted components and widths from 200 to 4000 km s−1. Overall, 60 ± 11  per cent appear to be active galactic nucleus (AGN) dominated, and at LLyα > 1043.3 erg s−1 and/or MUV < −21.5 virtually all LAEs are AGNs with high ionization parameters (log U = 0.6 ± 0.5) and with metallicities of ≈0.5 − 1 Z⊙. Those lacking signatures of AGNs (40 ± 11  per cent) have lower ionization parameters (⁠logU=−3.0+1.6−0.9 and log ξion = 25.4 ± 0.2) and are apparently metal-poor sources likely powered by young, dust-poor ‘maximal’ starbursts. Our results show that luminous LAEs at z ∼ 2–3 are a diverse population and that 2×L∗Lyα and 2×M∗UV mark a sharp transition in the nature of LAEs, from star formation dominated to AGN dominated.","lang":"eng"}],"publication_status":"published","status":"public","language":[{"iso":"eng"}],"quality_controlled":"1","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.","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.","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>.","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>."},"type":"journal_article","article_type":"original","title":"The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN","date_updated":"2022-08-19T07:01:08Z","month":"06","article_processing_charge":"No","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: active","galaxies: evolution","galaxies: high-redshift","galaxies: ISM","galaxies: starburst","cosmology: observations"],"date_published":"2018-06-01T00:00:00Z","publication":"Monthly Notices of the Royal Astronomical Society","page":"2817-2840","_id":"11557","external_id":{"arxiv":["1802.10102"]},"date_created":"2022-07-12T07:18:02Z","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1802.10102"}],"volume":477,"oa":1,"intvolume":"       477","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","issue":"2","extern":"1","scopus_import":"1"},{"date_published":"2018-06-01T00:00:00Z","article_processing_charge":"No","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: formation","galaxies: high-redshift","galaxies: luminosity function","mass function","galaxies: statistics"],"month":"06","title":"Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6","date_updated":"2022-08-19T07:04:45Z","date_created":"2022-07-12T10:41:08Z","external_id":{"arxiv":["1712.04451"]},"_id":"11558","page":"4725-4752","publication":"Monthly Notices of the Royal Astronomical Society","issue":"4","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","acknowledgement":"We thank the anonymous referee for their constructive comments that helped us improve the manuscript. DS acknowledges the hospitality of the IAC and a Severo Ochoa visiting grant. SS and JC acknowledge studentships from the Lancaster University. JM acknowledges a Huygens PhD fellowship from Leiden University. APA acknowledges financial support from the Science and Technology Foundation (FCT, Portugal) through research grants UID/FIS/04434/2013 and fellowship PD/BD/52706/2014. The authors thank Alyssa Drake, Kimihiko Nakajima, Yuichi Harikane, Max Gronke, Irene Shivaei, Helmut Dannerbauer, Huub Rottgering, ¨ Marius Eide, and Masami Ouchi for many engaging and stimulating discussions. We also thank Sara Perez, Alex Bennett, and Tom Rose for their involvement in the early stages of this project. Based on data products from observations made with European Southern Observatory (ESO) Telescopes at the La Silla Paranal Observatory under ESO programme IDs 294.A-5018, 097.A 0943,\r\n098.A-0819, 099.A-0254, and 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. Based on observations using the WFC on the 2.5 m INT, as part of programmes 2013AN002, 2013BN008, 2014AC88, 2014AN002, 2014BN006, 2014BC118, and 2016AN001. The INT is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. This work is based in part on data products produced at TERAPIX available at the Canadian Astronomy Data Centre as part of the Canada–France– Hawaii Telescope Legacy Survey (CFHTLS), a collaborative project of NRC and CNRS.\r\nWe are grateful to the CFHTLS, COSMOS-UltraVISTA, and COSMOS survey teams. We are also unmeasurably thankful to the pioneering and continuous work from previous Ly α surveys’ teams. Without these previous Ly α and the wider reach legacy surveys, this research would have been impossible. We also thank the VUDS team for making available spectroscopic redshifts from data obtained with VIMOS at the European Southern Observatory Very Large Telescope, Paranal, Chile, under Large Programme 185.A-0791. Finally, the authors acknowledge the unique value of the publicly available programming language PYTHON, including the NUMPY and SCIPY (Van Der Walt, Colbert & Varoquaux 2011; Jones et al. 2001), MATPLOTLIB (Hunter 2007), ASTROPY (Astropy Collaboration et al. 2013), and the TOPCAT analysis program (Taylor 2005). We publicly release a catalogue with all LAEs used in this paper (SC4K), so it can be freely explored by the community (see five example entries in Table A1).","intvolume":"       476","oa":1,"volume":476,"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1712.04451"}],"scopus_import":"1","extern":"1","author":[{"first_name":"David","last_name":"Sobral","full_name":"Sobral, David"},{"first_name":"Sérgio","full_name":"Santos, Sérgio","last_name":"Santos"},{"orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","last_name":"Matthee","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Paulino-Afonso","full_name":"Paulino-Afonso, Ana","first_name":"Ana"},{"last_name":"Ribeiro","full_name":"Ribeiro, Bruno","first_name":"Bruno"},{"last_name":"Calhau","full_name":"Calhau, João","first_name":"João"},{"full_name":"Khostovan, Ali A","last_name":"Khostovan","first_name":"Ali A"}],"year":"2018","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"day":"01","publisher":"Oxford University Press","oa_version":"Preprint","arxiv":1,"doi":"10.1093/mnras/sty378","quality_controlled":"1","language":[{"iso":"eng"}],"status":"public","abstract":[{"lang":"eng","text":"We present and explore deep narrow- and medium-band data obtained with the Subaru and the Isaac Newton Telescopes in the ∼2 deg2 COSMOS field. We use these data as an extremely wide, low-resolution (R ∼ 20–80) Integral Field Unit survey to slice through the COSMOS field and obtain a large sample of ∼4000 Ly α emitters (LAEs) from z ∼ 2 to 6 in 16 redshift slices (SC4K). We present new Ly α luminosity functions (LFs) covering a comoving volume of ∼108 Mpc3. SC4K extensively complements ultradeep surveys, jointly covering over 4 dex in Ly α luminosity and revealing a global (2.5 < z < 6) synergy LF with α=−1.93+0.12−0.12⁠, log10Φ∗Lyα=−3.45+0.22−0.29 Mpc−3, and log10L∗Lyα=42.93+0.15−0.11 erg s−1. The Schechter component of the Ly α LF reveals a factor ∼5 rise in L∗Lyα and a ∼7 × decline in Φ∗Lyα from z ∼ 2 to 6. The data reveal an extra power-law (or Schechter) component above LLy α ≈ 1043.3 erg s−1 at z ∼ 2.2–3.5 and we show that it is partially driven by X-ray and radio active galactic nucleus (AGN), as their Ly α LF resembles the excess. The power-law component vanishes and/or is below our detection limits above z > 3.5, likely linked with the evolution of the AGN population. The Ly α luminosity density rises by a factor ∼2 from z ∼ 2 to 3 but is then found to be roughly constant (⁠1.1+0.2−0.2×1040 erg s−1 Mpc−3) to z ∼ 6, despite the ∼0.7 dex drop in ultraviolet (UV) luminosity density. The Ly α/UV luminosity density ratio rises from 4 ± 1 per cent to 30 ± 6 per cent from z ∼ 2.2 to 6. Our results imply a rise of a factor of ≈2 in the global ionization efficiency (ξion) and a factor ≈4 ± 1 in the Ly α escape fraction from z ∼ 2 to 6, hinting for evolution in both the typical burstiness/stellar populations and even more so in the typical interstellar medium conditions allowing Ly α photons to escape."}],"publication_status":"published","article_type":"original","citation":{"short":"D. Sobral, S. Santos, J.J. Matthee, A. Paulino-Afonso, B. Ribeiro, J. Calhau, A.A. Khostovan, Monthly Notices of the Royal Astronomical Society 476 (2018) 4725–4752.","apa":"Sobral, D., Santos, S., Matthee, J. J., Paulino-Afonso, A., Ribeiro, B., Calhau, J., &#38; Khostovan, A. A. (2018). Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/sty378\">https://doi.org/10.1093/mnras/sty378</a>","ieee":"D. Sobral <i>et al.</i>, “Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 476, no. 4. Oxford University Press, pp. 4725–4752, 2018.","chicago":"Sobral, David, Sérgio Santos, Jorryt J Matthee, Ana Paulino-Afonso, Bruno Ribeiro, João Calhau, and Ali A Khostovan. “Slicing COSMOS with SC4K: The Evolution of Typical Ly α Emitters and the Ly α Escape Fraction from z ∼ 2 to 6.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2018. <a href=\"https://doi.org/10.1093/mnras/sty378\">https://doi.org/10.1093/mnras/sty378</a>.","ama":"Sobral D, Santos S, Matthee JJ, et al. Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6. <i>Monthly Notices of the Royal Astronomical Society</i>. 2018;476(4):4725-4752. doi:<a href=\"https://doi.org/10.1093/mnras/sty378\">10.1093/mnras/sty378</a>","mla":"Sobral, David, et al. “Slicing COSMOS with SC4K: The Evolution of Typical Ly α Emitters and the Ly α Escape Fraction from z ∼ 2 to 6.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 476, no. 4, Oxford University Press, 2018, pp. 4725–52, doi:<a href=\"https://doi.org/10.1093/mnras/sty378\">10.1093/mnras/sty378</a>.","ista":"Sobral D, Santos S, Matthee JJ, Paulino-Afonso A, Ribeiro B, Calhau J, Khostovan AA. 2018. Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6. Monthly Notices of the Royal Astronomical Society. 476(4), 4725–4752."},"type":"journal_article"},{"author":[{"first_name":"Diego F.","full_name":"Gauto, Diego F.","last_name":"Gauto"},{"last_name":"Hessel","full_name":"Hessel, Audrey","first_name":"Audrey"},{"full_name":"Rovó, Petra","last_name":"Rovó","first_name":"Petra"},{"full_name":"Kurauskas, Vilius","last_name":"Kurauskas","first_name":"Vilius"},{"first_name":"Rasmus","full_name":"Linser, Rasmus","last_name":"Linser"},{"last_name":"Schanda","full_name":"Schanda, Paul","orcid":"0000-0002-9350-7606","id":"7B541462-FAF6-11E9-A490-E8DFE5697425","first_name":"Paul"}],"date_published":"2017-10-01T00:00:00Z","keyword":["Nuclear and High Energy Physics","Instrumentation","General Chemistry","Radiation"],"year":"2017","article_processing_charge":"No","title":"Protein conformational dynamics studied by 15N and 1HR1ρ relaxation dispersion: Application to wild-type and G53A ubiquitin crystals","date_updated":"2021-01-12T08:19:20Z","publication_identifier":{"issn":["0926-2040"]},"month":"10","_id":"8447","publisher":"Elsevier","date_created":"2020-09-18T10:06:18Z","day":"01","publication":"Solid State Nuclear Magnetic Resonance","doi":"10.1016/j.ssnmr.2017.04.002","oa_version":"None","page":"86-95","quality_controlled":"1","issue":"10","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","intvolume":"        87","volume":87,"publication_status":"published","abstract":[{"lang":"eng","text":"Solid-state NMR spectroscopy can provide site-resolved information about protein dynamics over many time scales. Here we combine protein deuteration, fast magic-angle spinning (~45–60 kHz) and proton detection to study dynamics of ubiquitin in microcrystals, and in particular a mutant in a region that undergoes microsecond motions in a β-turn region in the wild-type protein. We use 15N R1ρ relaxation measurements as a function of the radio-frequency (RF) field strength, i.e. relaxation dispersion, to probe how the G53A mutation alters these dynamics. We report a population-inversion of conformational states: the conformation that in the wild-type protein is populated only sparsely becomes the predominant state. We furthermore explore the potential to use amide-1H R1ρ relaxation to obtain insight into dynamics. We show that while quantitative interpretation of 1H relaxation remains beyond reach under the experimental conditions, due to coherent contributions to decay, one may extract qualitative information about flexibility."}],"language":[{"iso":"eng"}],"status":"public","article_type":"original","citation":{"short":"D.F. Gauto, A. Hessel, P. Rovó, V. Kurauskas, R. Linser, P. Schanda, Solid State Nuclear Magnetic Resonance 87 (2017) 86–95.","apa":"Gauto, D. F., Hessel, A., Rovó, P., Kurauskas, V., Linser, R., &#38; Schanda, P. (2017). Protein conformational dynamics studied by 15N and 1HR1ρ relaxation dispersion: Application to wild-type and G53A ubiquitin crystals. <i>Solid State Nuclear Magnetic Resonance</i>. Elsevier. <a href=\"https://doi.org/10.1016/j.ssnmr.2017.04.002\">https://doi.org/10.1016/j.ssnmr.2017.04.002</a>","ieee":"D. F. Gauto, A. Hessel, P. Rovó, V. Kurauskas, R. Linser, and P. Schanda, “Protein conformational dynamics studied by 15N and 1HR1ρ relaxation dispersion: Application to wild-type and G53A ubiquitin crystals,” <i>Solid State Nuclear Magnetic Resonance</i>, vol. 87, no. 10. Elsevier, pp. 86–95, 2017.","chicago":"Gauto, Diego F., Audrey Hessel, Petra Rovó, Vilius Kurauskas, Rasmus Linser, and Paul Schanda. “Protein Conformational Dynamics Studied by 15N and 1HR1ρ Relaxation Dispersion: Application to Wild-Type and G53A Ubiquitin Crystals.” <i>Solid State Nuclear Magnetic Resonance</i>. Elsevier, 2017. <a href=\"https://doi.org/10.1016/j.ssnmr.2017.04.002\">https://doi.org/10.1016/j.ssnmr.2017.04.002</a>.","ama":"Gauto DF, Hessel A, Rovó P, Kurauskas V, Linser R, Schanda P. Protein conformational dynamics studied by 15N and 1HR1ρ relaxation dispersion: Application to wild-type and G53A ubiquitin crystals. <i>Solid State Nuclear Magnetic Resonance</i>. 2017;87(10):86-95. doi:<a href=\"https://doi.org/10.1016/j.ssnmr.2017.04.002\">10.1016/j.ssnmr.2017.04.002</a>","ista":"Gauto DF, Hessel A, Rovó P, Kurauskas V, Linser R, Schanda P. 2017. Protein conformational dynamics studied by 15N and 1HR1ρ relaxation dispersion: Application to wild-type and G53A ubiquitin crystals. Solid State Nuclear Magnetic Resonance. 87(10), 86–95.","mla":"Gauto, Diego F., et al. “Protein Conformational Dynamics Studied by 15N and 1HR1ρ Relaxation Dispersion: Application to Wild-Type and G53A Ubiquitin Crystals.” <i>Solid State Nuclear Magnetic Resonance</i>, vol. 87, no. 10, Elsevier, 2017, pp. 86–95, doi:<a href=\"https://doi.org/10.1016/j.ssnmr.2017.04.002\">10.1016/j.ssnmr.2017.04.002</a>."},"type":"journal_article","extern":"1"},{"month":"08","publication_identifier":{"issn":["1090-7807"]},"title":"Optimized fast mixing device for real-time NMR applications","date_updated":"2021-01-12T08:19:20Z","article_processing_charge":"No","keyword":["Nuclear and High Energy Physics","Biophysics","Biochemistry","Condensed Matter Physics"],"year":"2017","date_published":"2017-08-01T00:00:00Z","author":[{"last_name":"Franco","full_name":"Franco, Rémi","first_name":"Rémi"},{"last_name":"Favier","full_name":"Favier, Adrien","first_name":"Adrien"},{"id":"7B541462-FAF6-11E9-A490-E8DFE5697425","first_name":"Paul","last_name":"Schanda","full_name":"Schanda, Paul","orcid":"0000-0002-9350-7606"},{"first_name":"Bernhard","full_name":"Brutscher, Bernhard","last_name":"Brutscher"}],"page":"125-129","oa_version":"None","doi":"10.1016/j.jmr.2017.05.016","publication":"Journal of Magnetic Resonance","day":"01","date_created":"2020-09-18T10:06:27Z","publisher":"Elsevier","_id":"8448","status":"public","language":[{"iso":"eng"}],"abstract":[{"text":"We present an improved fast mixing device based on the rapid mixing of two solutions inside the NMR probe, as originally proposed by Hore and coworkers (J. Am. Chem. Soc. 125 (2003) 12484–12492). Such a device is important for off-equilibrium studies of molecular kinetics by multidimensional real-time NMR spectrsocopy. The novelty of this device is that it allows removing the injector from the NMR detection volume after mixing, and thus provides good magnetic field homogeneity independently of the initial sample volume placed in the NMR probe. The apparatus is simple to build, inexpensive, and can be used without any hardware modification on any type of liquid-state NMR spectrometer. We demonstrate the performance of our fast mixing device in terms of improved magnetic field homogeneity, and show an application to the study of protein folding and the structural characterization of transiently populated folding intermediates.","lang":"eng"}],"volume":281,"publication_status":"published","intvolume":"       281","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","issue":"8","quality_controlled":"1","extern":"1","type":"journal_article","citation":{"mla":"Franco, Rémi, et al. “Optimized Fast Mixing Device for Real-Time NMR Applications.” <i>Journal of Magnetic Resonance</i>, vol. 281, no. 8, Elsevier, 2017, pp. 125–29, doi:<a href=\"https://doi.org/10.1016/j.jmr.2017.05.016\">10.1016/j.jmr.2017.05.016</a>.","ista":"Franco R, Favier A, Schanda P, Brutscher B. 2017. Optimized fast mixing device for real-time NMR applications. Journal of Magnetic Resonance. 281(8), 125–129.","ama":"Franco R, Favier A, Schanda P, Brutscher B. Optimized fast mixing device for real-time NMR applications. <i>Journal of Magnetic Resonance</i>. 2017;281(8):125-129. doi:<a href=\"https://doi.org/10.1016/j.jmr.2017.05.016\">10.1016/j.jmr.2017.05.016</a>","chicago":"Franco, Rémi, Adrien Favier, Paul Schanda, and Bernhard Brutscher. “Optimized Fast Mixing Device for Real-Time NMR Applications.” <i>Journal of Magnetic Resonance</i>. Elsevier, 2017. <a href=\"https://doi.org/10.1016/j.jmr.2017.05.016\">https://doi.org/10.1016/j.jmr.2017.05.016</a>.","ieee":"R. Franco, A. Favier, P. Schanda, and B. Brutscher, “Optimized fast mixing device for real-time NMR applications,” <i>Journal of Magnetic Resonance</i>, vol. 281, no. 8. Elsevier, pp. 125–129, 2017.","apa":"Franco, R., Favier, A., Schanda, P., &#38; Brutscher, B. (2017). Optimized fast mixing device for real-time NMR applications. <i>Journal of Magnetic Resonance</i>. Elsevier. <a href=\"https://doi.org/10.1016/j.jmr.2017.05.016\">https://doi.org/10.1016/j.jmr.2017.05.016</a>","short":"R. Franco, A. Favier, P. Schanda, B. Brutscher, Journal of Magnetic Resonance 281 (2017) 125–129."},"article_type":"original"},{"oa_version":"Preprint","arxiv":1,"doi":"10.3847/1538-4357/aa9931","day":"21","publisher":"IOP Publishing","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"author":[{"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":"D.","last_name":"Sobral","full_name":"Sobral, D."},{"last_name":"Boone","full_name":"Boone, F.","first_name":"F."},{"first_name":"H.","full_name":"Röttgering, H.","last_name":"Röttgering"},{"first_name":"D.","last_name":"Schaerer","full_name":"Schaerer, D."},{"first_name":"M.","last_name":"Girard","full_name":"Girard, M."},{"first_name":"A.","last_name":"Pallottini","full_name":"Pallottini, A."},{"first_name":"L.","last_name":"Vallini","full_name":"Vallini, L."},{"first_name":"A.","full_name":"Ferrara, A.","last_name":"Ferrara"},{"first_name":"B.","full_name":"Darvish, B.","last_name":"Darvish"},{"last_name":"Mobasher","full_name":"Mobasher, B.","first_name":"B."}],"year":"2017","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>.","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>","mla":"Matthee, Jorryt J., et al. “ALMA Reveals Metals yet No Dust within Multiple Components in CR7.” <i>The Astrophysical Journal</i>, vol. 851, no. 2, 145, IOP Publishing, 2017, doi:<a href=\"https://doi.org/10.3847/1538-4357/aa9931\">10.3847/1538-4357/aa9931</a>.","ista":"Matthee JJ, Sobral D, Boone F, Röttgering H, Schaerer D, Girard M, Pallottini A, Vallini L, Ferrara A, Darvish B, Mobasher B. 2017. ALMA reveals metals yet no dust within multiple components in CR7. The Astrophysical Journal. 851(2), 145.","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>","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).","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."},"type":"journal_article","article_type":"original","language":[{"iso":"eng"}],"status":"public","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"}],"publication_status":"published","quality_controlled":"1","publication":"The Astrophysical Journal","date_created":"2022-07-07T08:48:04Z","external_id":{"arxiv":["1709.06569"]},"_id":"11518","month":"12","date_updated":"2022-08-18T10:23:35Z","title":"ALMA reveals metals yet no dust within multiple components in CR7","date_published":"2017-12-21T00:00:00Z","keyword":["Space and Planetary Science","Astronomy and Astrophysics","dark ages","reionization","first stars – galaxies: formation – galaxies: high-redshift – galaxies: ISM – galaxies: kinematics and dynamics"],"article_processing_charge":"No","scopus_import":"1","extern":"1","volume":851,"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1709.06569"}],"issue":"2","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.","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa":1,"intvolume":"       851","article_number":"145"},{"_id":"11561","date_created":"2022-07-12T11:01:35Z","external_id":{"arxiv":["1702.04721"]},"publication":"Monthly Notices of the Royal Astronomical Society","page":"629-649","date_published":"2017-10-01T00:00:00Z","article_processing_charge":"No","keyword":["Space and Planetary Science","Astronomy and Astrophysics galaxies","active","galaxies","evolution","galaxies","high-redshift","galaxies","luminosity function","mass function","galaxies: star formation"],"title":"Boötes-HiZELS: An optical to near-infrared survey of emission-line galaxies at z = 0.4–4.7","date_updated":"2022-08-19T07:15:14Z","month":"10","scopus_import":"1","extern":"1","issue":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa":1,"intvolume":"       471","volume":471,"main_file_link":[{"url":"https://arxiv.org/abs/1702.04721","open_access":"1"}],"publisher":"Oxford University Press","day":"01","doi":"10.1093/mnras/stx1569","oa_version":"Preprint","arxiv":1,"author":[{"first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J"},{"first_name":"David","full_name":"Sobral, David","last_name":"Sobral"},{"first_name":"Philip","full_name":"Best, Philip","last_name":"Best"},{"full_name":"Smail, Ian","last_name":"Smail","first_name":"Ian"},{"last_name":"Bian","full_name":"Bian, Fuyan","first_name":"Fuyan"},{"full_name":"Darvish, Behnam","last_name":"Darvish","first_name":"Behnam"},{"full_name":"Röttgering, Huub","last_name":"Röttgering","first_name":"Huub"},{"first_name":"Xiaohui","full_name":"Fan, Xiaohui","last_name":"Fan"}],"year":"2017","publication_identifier":{"issn":["0035-8711","1365-2966"]},"article_type":"original","citation":{"short":"J.J. Matthee, D. Sobral, P. Best, I. Smail, F. Bian, B. Darvish, H. Röttgering, X. Fan, Monthly Notices of the Royal Astronomical Society 471 (2017) 629–649.","apa":"Matthee, J. J., Sobral, D., Best, P., Smail, I., Bian, F., Darvish, B., … Fan, X. (2017). Boötes-HiZELS: An optical to near-infrared survey of emission-line galaxies at z = 0.4–4.7. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stx1569\">https://doi.org/10.1093/mnras/stx1569</a>","ieee":"J. J. Matthee <i>et al.</i>, “Boötes-HiZELS: An optical to near-infrared survey of emission-line galaxies at z = 0.4–4.7,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 471, no. 1. Oxford University Press, pp. 629–649, 2017.","chicago":"Matthee, Jorryt J, David Sobral, Philip Best, Ian Smail, Fuyan Bian, Behnam Darvish, Huub Röttgering, and Xiaohui Fan. “Boötes-HiZELS: An Optical to near-Infrared Survey of Emission-Line Galaxies at z = 0.4–4.7.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stx1569\">https://doi.org/10.1093/mnras/stx1569</a>.","ama":"Matthee JJ, Sobral D, Best P, et al. Boötes-HiZELS: An optical to near-infrared survey of emission-line galaxies at z = 0.4–4.7. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;471(1):629-649. doi:<a href=\"https://doi.org/10.1093/mnras/stx1569\">10.1093/mnras/stx1569</a>","ista":"Matthee JJ, Sobral D, Best P, Smail I, Bian F, Darvish B, Röttgering H, Fan X. 2017. Boötes-HiZELS: An optical to near-infrared survey of emission-line galaxies at z = 0.4–4.7. Monthly Notices of the Royal Astronomical Society. 471(1), 629–649.","mla":"Matthee, Jorryt J., et al. “Boötes-HiZELS: An Optical to near-Infrared Survey of Emission-Line Galaxies at z = 0.4–4.7.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 471, no. 1, Oxford University Press, 2017, pp. 629–49, doi:<a href=\"https://doi.org/10.1093/mnras/stx1569\">10.1093/mnras/stx1569</a>."},"type":"journal_article","quality_controlled":"1","publication_status":"published","abstract":[{"lang":"eng","text":"We present a sample of ∼1000 emission-line galaxies at z = 0.4–4.7 from the ∼0.7deg2 High-z Emission-Line Survey in the Boötes field identified with a suite of six narrow-band filters at ≈0.4–2.1 μm. These galaxies have been selected on their Ly α (73), [O II] (285), H β/[O III] (387) or H α (362) emission line, and have been classified with optical to near-infrared colours. A subsample of 98 sources have reliable redshifts from multiple narrow-band (e.g. [O II]–H α) detections and/or spectroscopy. In this survey paper, we present the observations, selection and catalogues of emitters. We measure number densities of Ly α, [O II], H β/[O III] and H α and confirm strong luminosity evolution in star-forming galaxies from z ∼ 0.4 to ∼5, in agreement with previous results. To demonstrate the usefulness of dual-line emitters, we use the sample of dual [O II]–H α emitters to measure the observed [O II]/H α ratio at z = 1.47. The observed [O II]/H α ratio increases significantly from 0.40 ± 0.01 at z = 0.1 to 0.52 ± 0.05 at z = 1.47, which we attribute to either decreasing dust attenuation with redshift, or due to a bias in the (typically) fibre measurements in the local Universe that only measure the central kpc regions. At the bright end, we find that both the H α and Ly α number densities at z ≈ 2.2 deviate significantly from a Schechter form, following a power law. We show that this is driven entirely by an increasing X-ray/active galactic nucleus fraction with line luminosity, which reaches ≈100 per cent at line luminosities L ≳ 3 × 1044 erg s−1."}],"language":[{"iso":"eng"}],"status":"public"},{"extern":"1","scopus_import":"1","main_file_link":[{"url":"https://arxiv.org/abs/1609.05897","open_access":"1"}],"volume":466,"intvolume":"       466","oa":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","issue":"1","acknowledgement":"We thank the reviewer for his/her helpful comments and suggestions that have greatly improved this work. DS and JM acknowledge financial support from the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship. DS also acknowledges funding from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010). PNB is grateful for support from the UK STFC via grant ST/M001229/1. IRS acknowledges support from STFC (ST/L00075X/1), the ERC Advanced Investigator programme DUSTYGAL 321334 and a Royal Society/Wolfson merit award. We thank Matthew Hayes, Ryan Trainor, Kimihiko Nakajima and Anne Verhamme for many helpful discussions and Ana Sobral, Carolina Duarte and Miguel Domingos for taking part in observations with the NB392 filter. We also thank Sergio Santos for helpful comments. This research is based on observations obtained on the Isaac Newton Telescope (INT), programs: I13AN002, I14AN002, 088-INT7/14A, I14BN006, 118-INT13/14B & I15AN008. The authors acknowledge the award of time from programmes: I13AN002, I14AN002, 088-INT7/14A, I14BN006, 118-INT13/14B, I15AN008 on the INT. INT is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 098.A 0819. We have benefited greatly from the publicly available programming language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY and ASTROPY packages, the astronomical imaging tools SEXTRACTOR, SWARP (Bertin & Arnouts 1996; Bertin 2010), SCAMP (Bertin 2006) and TOPCAT (Taylor 2005). Dedicated to the memory of M. L. Nicolau and M. C. Serrano.","page":"1242-1258","publication":"Monthly Notices of the Royal Astronomical Society","external_id":{"arxiv":["1609.05897"]},"date_created":"2022-07-12T12:04:16Z","_id":"11562","month":"04","date_updated":"2022-08-19T07:18:20Z","title":"The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23","article_processing_charge":"No","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: haloes","galaxies: high-redshift","galaxies: luminosity function","mass function","galaxies: statistics","cosmology: observations"],"date_published":"2017-04-01T00:00:00Z","citation":{"ieee":"D. Sobral <i>et al.</i>, “The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 466, no. 1. Oxford University Press, pp. 1242–1258, 2017.","short":"D. Sobral, J.J. Matthee, P. Best, A. Stroe, H. Röttgering, I. Oteo, I. Smail, L. Morabito, A. Paulino-Afonso, Monthly Notices of the Royal Astronomical Society 466 (2017) 1242–1258.","apa":"Sobral, D., Matthee, J. J., Best, P., Stroe, A., Röttgering, H., Oteo, I., … Paulino-Afonso, A. (2017). The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stw3090\">https://doi.org/10.1093/mnras/stw3090</a>","ista":"Sobral D, Matthee JJ, Best P, Stroe A, Röttgering H, Oteo I, Smail I, Morabito L, Paulino-Afonso A. 2017. The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23. Monthly Notices of the Royal Astronomical Society. 466(1), 1242–1258.","mla":"Sobral, David, et al. “The CALYMHA Survey: Lyα Luminosity Function and Global Escape Fraction of Lyα Photons at z = 2.23.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 466, no. 1, Oxford University Press, 2017, pp. 1242–58, doi:<a href=\"https://doi.org/10.1093/mnras/stw3090\">10.1093/mnras/stw3090</a>.","chicago":"Sobral, David, Jorryt J Matthee, Philip Best, Andra Stroe, Huub Röttgering, Iván Oteo, Ian Smail, Leah Morabito, and Ana Paulino-Afonso. “The CALYMHA Survey: Lyα Luminosity Function and Global Escape Fraction of Lyα Photons at z = 2.23.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stw3090\">https://doi.org/10.1093/mnras/stw3090</a>.","ama":"Sobral D, Matthee JJ, Best P, et al. The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;466(1):1242-1258. doi:<a href=\"https://doi.org/10.1093/mnras/stw3090\">10.1093/mnras/stw3090</a>"},"type":"journal_article","article_type":"original","status":"public","language":[{"iso":"eng"}],"abstract":[{"lang":"eng","text":"We present the CAlibrating LYMan-α with Hα (CALYMHA) pilot survey and new results on Lyman α (Lyα) selected galaxies at z ∼ 2. We use a custom-built Lyα narrow-band filter at the Isaac Newton Telescope, designed to provide a matched volume coverage to the z = 2.23 Hα HiZELS survey. Here, we present the first results for the COSMOS and UDS fields. Our survey currently reaches a 3σ line flux limit of ∼4 × 10−17 erg s−1 cm−2, and a Lyα luminosity limit of ∼1042.3 erg s−1. We find 188 Lyα emitters over 7.3 × 105 Mpc3, but also find significant numbers of other line-emitting sources corresponding to He II, C III] and C IV emission lines. These sources are important contaminants, and we carefully remove them, unlike most previous studies. We find that the Lyα luminosity function at z = 2.23 is very well described by a Schechter function up to LLy α ≈ 1043 erg s−1 with L∗=1042.59+0.16−0.08 erg s−1, ϕ∗=10−3.09+0.14−0.34 Mpc−3 and α = −1.75 ± 0.25. Above LLy α ≈ 1043 erg s−1, the Lyα luminosity function becomes power-law like, driven by X-ray AGN. We find that Lyα-selected emitters have a high escape fraction of 37 ± 7 per cent, anticorrelated with Lyα luminosity and correlated with Lyα equivalent width. Lyα emitters have ubiquitous large (≈40 kpc) Lyα haloes, ∼2 times larger than their Hα extents. By directly comparing our Lyα and Hα luminosity functions, we find that the global/overall escape fraction of Lyα photons (within a 13 kpc radius) from the full population of star-forming galaxies is 5.1 ± 0.2 per cent at the peak of the star formation history. An extra 3.3 ± 0.3 per cent of Lyα photons likely still escape, but at larger radii."}],"publication_status":"published","quality_controlled":"1","oa_version":"Preprint","arxiv":1,"doi":"10.1093/mnras/stw3090","day":"01","publisher":"Oxford University Press","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"year":"2017","author":[{"first_name":"David","last_name":"Sobral","full_name":"Sobral, David"},{"full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"full_name":"Best, Philip","last_name":"Best","first_name":"Philip"},{"last_name":"Stroe","full_name":"Stroe, Andra","first_name":"Andra"},{"first_name":"Huub","last_name":"Röttgering","full_name":"Röttgering, Huub"},{"full_name":"Oteo, Iván","last_name":"Oteo","first_name":"Iván"},{"first_name":"Ian","last_name":"Smail","full_name":"Smail, Ian"},{"first_name":"Leah","full_name":"Morabito, Leah","last_name":"Morabito"},{"last_name":"Paulino-Afonso","full_name":"Paulino-Afonso, Ana","first_name":"Ana"}]}]