[{"publication_status":"published","article_processing_charge":"No","date_created":"2022-07-12T10:41:08Z","title":"Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6","intvolume":" 476","_id":"11558","scopus_import":"1","author":[{"full_name":"Sobral, David","first_name":"David","last_name":"Sobral"},{"full_name":"Santos, Sérgio","first_name":"Sérgio","last_name":"Santos"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","last_name":"Matthee"},{"first_name":"Ana","last_name":"Paulino-Afonso","full_name":"Paulino-Afonso, Ana"},{"first_name":"Bruno","last_name":"Ribeiro","full_name":"Ribeiro, Bruno"},{"first_name":"João","last_name":"Calhau","full_name":"Calhau, João"},{"last_name":"Khostovan","first_name":"Ali A","full_name":"Khostovan, Ali A"}],"issue":"4","publisher":"Oxford University Press","article_type":"original","page":"4725-4752","quality_controlled":"1","arxiv":1,"doi":"10.1093/mnras/sty378","day":"01","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."}],"date_updated":"2022-08-19T07:04:45Z","year":"2018","citation":{"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.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2018. https://doi.org/10.1093/mnras/sty378.","ieee":"D. Sobral et al., “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, vol. 476, no. 4. Oxford University Press, pp. 4725–4752, 2018.","ama":"Sobral D, Santos S, Matthee JJ, et al. Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6. Monthly Notices of the Royal Astronomical Society. 2018;476(4):4725-4752. doi:10.1093/mnras/sty378","apa":"Sobral, D., Santos, S., Matthee, J. J., Paulino-Afonso, A., Ribeiro, B., Calhau, J., & 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. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/sty378","ista":"Sobral D, Santos S, Matthee JJ, Paulino-Afonso A, Ribeiro B, Calhau J, Khostovan AA. 2018. Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6. Monthly Notices of the Royal Astronomical Society. 476(4), 4725–4752.","mla":"Sobral, David, et al. “Slicing COSMOS with SC4K: The Evolution of Typical Ly α Emitters and the Ly α Escape Fraction from z ∼ 2 to 6.” Monthly Notices of the Royal Astronomical Society, vol. 476, no. 4, Oxford University Press, 2018, pp. 4725–52, doi:10.1093/mnras/sty378.","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."},"external_id":{"arxiv":["1712.04451"]},"acknowledgement":"We thank the anonymous referee for their constructive comments that helped us improve the manuscript. DS acknowledges the hospitality of the IAC and a Severo Ochoa visiting grant. SS and JC acknowledge studentships from the Lancaster University. JM acknowledges a Huygens PhD fellowship from Leiden University. APA acknowledges financial support from the Science and Technology Foundation (FCT, Portugal) through research grants UID/FIS/04434/2013 and fellowship PD/BD/52706/2014. The authors thank Alyssa Drake, Kimihiko Nakajima, Yuichi Harikane, Max Gronke, Irene Shivaei, Helmut Dannerbauer, Huub Rottgering, ¨ Marius Eide, and Masami Ouchi for many engaging and stimulating discussions. We also thank Sara Perez, Alex Bennett, and Tom Rose for their involvement in the early stages of this project. Based on data products from observations made with European Southern Observatory (ESO) Telescopes at the La Silla Paranal Observatory under ESO programme IDs 294.A-5018, 097.A 0943,\r\n098.A-0819, 099.A-0254, and 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. Based on observations using the WFC on the 2.5 m INT, as part of programmes 2013AN002, 2013BN008, 2014AC88, 2014AN002, 2014BN006, 2014BC118, and 2016AN001. The INT is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. This work is based in part on data products produced at TERAPIX available at the Canadian Astronomy Data Centre as part of the Canada–France– Hawaii Telescope Legacy Survey (CFHTLS), a collaborative project of NRC and CNRS.\r\nWe are grateful to the CFHTLS, COSMOS-UltraVISTA, and COSMOS survey teams. We are also unmeasurably thankful to the pioneering and continuous work from previous Ly α surveys’ teams. Without these previous Ly α and the wider reach legacy surveys, this research would have been impossible. We also thank the VUDS team for making available spectroscopic redshifts from data obtained with VIMOS at the European Southern Observatory Very Large Telescope, Paranal, Chile, under Large Programme 185.A-0791. Finally, the authors acknowledge the unique value of the publicly available programming language PYTHON, including the NUMPY and SCIPY (Van Der Walt, Colbert & Varoquaux 2011; Jones et al. 2001), MATPLOTLIB (Hunter 2007), ASTROPY (Astropy Collaboration et al. 2013), and the TOPCAT analysis program (Taylor 2005). We publicly release a catalogue with all LAEs used in this paper (SC4K), so it can be freely explored by the community (see five example entries in Table A1).","volume":476,"extern":"1","oa_version":"Preprint","month":"06","publication":"Monthly Notices of the Royal Astronomical Society","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: formation","galaxies: high-redshift","galaxies: luminosity function","mass function","galaxies: statistics"],"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"oa":1,"date_published":"2018-06-01T00:00:00Z","type":"journal_article","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1712.04451"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public"},{"extern":"1","volume":479,"acknowledgement":"We thank the anonymous referee for their constructive comments. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. We thank Jarle Brinchmann, Rob Crain and David Sobral for discussions. We acknowledge the use of the TOPCAT software (Taylor 2013) for assisting in rapid exploration of multidimensional data sets and the use of PYTHON and its NUMPY, MATPLOTLIB, and PANDAS packages.","abstract":[{"text":"Observations show that star-forming galaxies reside on a tight 3D plane between mass, gas-phase metallicity, and star formation rate (SFR), which can be explained by the interplay between metal-poor gas inflows, SFR and outflows. However, different metals are released on different time-scales, which may affect the slope of this relation. Here, we use central, star-forming galaxies with Mstar = 109.0–10.5 M⊙ from the EAGLE hydrodynamical simulation to examine 3D relations between mass, SFR, and chemical enrichment using absolute and relative C, N, O, and Fe abundances. We show that the scatter is smaller when gas-phase α-enhancement is used rather than metallicity. A similar plane also exists for stellar α-enhancement, implying that present-day specific SFRs are correlated with long time-scale star formation histories. Between z = 0 and 1, the α-enhancement plane is even more insensitive to redshift than the plane using metallicity. However, it evolves at z > 1 due to lagging iron yields. At fixed mass, galaxies with higher SFRs have star formation histories shifted towards late times, are more α-enhanced, and this α-enhancement increases with redshift as observed. These findings suggest that relations between physical properties inferred from observations may be affected by systematic variations in α-enhancements.","lang":"eng"}],"arxiv":1,"doi":"10.1093/mnrasl/sly093","day":"01","external_id":{"arxiv":["1802.06786"]},"date_updated":"2022-08-19T08:35:45Z","citation":{"ieee":"J. J. Matthee and J. Schaye, “Star-forming galaxies are predicted to lie on a fundamental plane of mass, star formation rate, and α-enhancement,” Monthly Notices of the Royal Astronomical Society: Letters, vol. 479, no. 1. Oxford University Press, pp. L34–L39, 2018.","chicago":"Matthee, Jorryt J, and Joop Schaye. “Star-Forming Galaxies Are Predicted to Lie on a Fundamental Plane of Mass, Star Formation Rate, and α-Enhancement.” Monthly Notices of the Royal Astronomical Society: Letters. Oxford University Press, 2018. https://doi.org/10.1093/mnrasl/sly093.","ama":"Matthee JJ, Schaye J. Star-forming galaxies are predicted to lie on a fundamental plane of mass, star formation rate, and α-enhancement. Monthly Notices of the Royal Astronomical Society: Letters. 2018;479(1):L34-L39. doi:10.1093/mnrasl/sly093","apa":"Matthee, J. J., & Schaye, J. (2018). Star-forming galaxies are predicted to lie on a fundamental plane of mass, star formation rate, and α-enhancement. Monthly Notices of the Royal Astronomical Society: Letters. Oxford University Press. https://doi.org/10.1093/mnrasl/sly093","ista":"Matthee JJ, Schaye J. 2018. Star-forming galaxies are predicted to lie on a fundamental plane of mass, star formation rate, and α-enhancement. Monthly Notices of the Royal Astronomical Society: Letters. 479(1), L34–L39.","mla":"Matthee, Jorryt J., and Joop Schaye. “Star-Forming Galaxies Are Predicted to Lie on a Fundamental Plane of Mass, Star Formation Rate, and α-Enhancement.” Monthly Notices of the Royal Astronomical Society: Letters, vol. 479, no. 1, Oxford University Press, 2018, pp. L34–39, doi:10.1093/mnrasl/sly093.","short":"J.J. Matthee, J. Schaye, Monthly Notices of the Royal Astronomical Society: Letters 479 (2018) L34–L39."},"year":"2018","article_type":"original","publisher":"Oxford University Press","page":"L34 - L39","quality_controlled":"1","title":"Star-forming galaxies are predicted to lie on a fundamental plane of mass, star formation rate, and α-enhancement","intvolume":" 479","publication_status":"published","article_processing_charge":"No","date_created":"2022-07-14T12:49:47Z","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J"},{"full_name":"Schaye, Joop","first_name":"Joop","last_name":"Schaye"}],"issue":"1","_id":"11584","scopus_import":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","main_file_link":[{"url":"https://arxiv.org/abs/1802.06786","open_access":"1"}],"oa":1,"publication_identifier":{"issn":["1745-3925"],"eissn":["1745-3933"]},"date_published":"2018-09-01T00:00:00Z","type":"journal_article","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: abundances","galaxies: evolution","galaxies: formation","galaxies: star formation"],"month":"09","oa_version":"Preprint","publication":"Monthly Notices of the Royal Astronomical Society: Letters"},{"external_id":{"arxiv":["1609.05897"]},"year":"2017","citation":{"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. Monthly Notices of the Royal Astronomical Society. 2017;466(1):1242-1258. doi:10.1093/mnras/stw3090","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. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stw3090","ieee":"D. Sobral et al., “The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23,” Monthly Notices of the Royal Astronomical Society, vol. 466, no. 1. Oxford University Press, pp. 1242–1258, 2017.","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.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2017. https://doi.org/10.1093/mnras/stw3090.","mla":"Sobral, David, et al. “The CALYMHA Survey: Lyα Luminosity Function and Global Escape Fraction of Lyα Photons at z = 2.23.” Monthly Notices of the Royal Astronomical Society, vol. 466, no. 1, Oxford University Press, 2017, pp. 1242–58, doi:10.1093/mnras/stw3090.","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.","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."},"date_updated":"2022-08-19T07:18:20Z","abstract":[{"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.","lang":"eng"}],"day":"01","doi":"10.1093/mnras/stw3090","arxiv":1,"extern":"1","volume":466,"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.","issue":"1","author":[{"full_name":"Sobral, David","last_name":"Sobral","first_name":"David"},{"first_name":"Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"first_name":"Philip","last_name":"Best","full_name":"Best, Philip"},{"full_name":"Stroe, Andra","first_name":"Andra","last_name":"Stroe"},{"last_name":"Röttgering","first_name":"Huub","full_name":"Röttgering, Huub"},{"last_name":"Oteo","first_name":"Iván","full_name":"Oteo, Iván"},{"full_name":"Smail, Ian","last_name":"Smail","first_name":"Ian"},{"first_name":"Leah","last_name":"Morabito","full_name":"Morabito, Leah"},{"last_name":"Paulino-Afonso","first_name":"Ana","full_name":"Paulino-Afonso, Ana"}],"scopus_import":"1","_id":"11562","intvolume":" 466","title":"The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23","article_processing_charge":"No","date_created":"2022-07-12T12:04:16Z","publication_status":"published","quality_controlled":"1","page":"1242-1258","article_type":"original","publisher":"Oxford University Press","type":"journal_article","date_published":"2017-04-01T00:00:00Z","oa":1,"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1609.05897"}],"publication":"Monthly Notices of the Royal Astronomical Society","month":"04","oa_version":"Preprint","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: haloes","galaxies: high-redshift","galaxies: luminosity function","mass function","galaxies: statistics","cosmology: observations"],"language":[{"iso":"eng"}]},{"extern":"1","acknowledgement":"We thank the referee for the many helpful and constructive comments which have significantly improved this paper. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. DS acknowledges financial support from the Netherlands Organization for Scientific research (NWO) through a Veni fellowship and 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. IO acknowledges support from the European Research Council in the form of the Advanced Investigator Programme, 321302, COSMICISM. The authors thank Andreas Faisst, Michael Rutkowski and Andreas Sandberg for answering questions related to this work and Daniel Schaerer and Mark Dijkstra for discussions. We acknowledge the work that has been done by both the COSMOS team in assembling such large, state-of-the-art multi-wavelength data set, as this has been crucial for the results presented in this paper. We have benefited greatly from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY (Jones et al. 2001; Hunter 2007; Van Der Walt, Colbert & Varoquaux 2011) and ASTROPY (Astropy Collaboration et al. 2013) packages, the astronomical imaging tools SEXTRACTOR and SWARP (Bertin & Arnouts 1996;\r\nBertin 2010) and the TOPCAT analysis program (Taylor 2013).","volume":465,"abstract":[{"text":"We study the production rate of ionizing photons of a sample of 588 Hα emitters (HAEs) and 160 Lyman-α emitters (LAEs) at z = 2.2 in the COSMOS field in order to assess the implied emissivity from galaxies, based on their ultraviolet (UV) luminosity. By exploring the rest-frame Lyman Continuum (LyC) with GALEX/NUV data, we find fesc < 2.8 (6.4) per cent through median (mean) stacking. By combining the Hα luminosity density with intergalactic medium emissivity measurements from absorption studies, we find a globally averaged 〈fesc〉 of 5.9+14.5−4.2 per cent at z = 2.2 if we assume HAEs are the only source of ionizing photons. We find similarly low values of the global 〈fesc〉 at z ≈ 3–5, also ruling out a high 〈fesc〉 at z < 5. These low escape fractions allow us to measure ξion, the number of produced ionizing photons per unit UV luminosity, and investigate how this depends on galaxy properties. We find a typical ξion ≈ 1024.77 ± 0.04 Hz erg−1 for HAEs and ξion ≈ 1025.14 ± 0.09 Hz erg−1 for LAEs. LAEs and low-mass HAEs at z = 2.2 show similar values of ξion as typically assumed in the reionization era, while the typical HAE is three times less ionizing. Due to an increasing ξion with increasing EW(Hα), ξion likely increases with redshift. This evolution alone is fully in line with the observed evolution of ξion between z ≈ 2 and 5, indicating a typical value of ξion ≈ 1025.4 Hz erg−1 in the reionization era.","lang":"eng"}],"arxiv":1,"doi":"10.1093/mnras/stw2973","day":"01","external_id":{"arxiv":["1605.08782"]},"date_updated":"2022-08-19T07:53:04Z","year":"2017","citation":{"chicago":"Matthee, Jorryt J, David Sobral, Philip Best, Ali Ahmad Khostovan, Iván Oteo, Rychard Bouwens, and Huub Röttgering. “The Production and Escape of Lyman-Continuum Radiation from Star-Forming Galaxies at z ∼ 2 and Their Redshift Evolution.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2017. https://doi.org/10.1093/mnras/stw2973.","ieee":"J. J. Matthee et al., “The production and escape of Lyman-Continuum radiation from star-forming galaxies at z ∼ 2 and their redshift evolution,” Monthly Notices of the Royal Astronomical Society, vol. 465, no. 3. Oxford University Press, pp. 3637–3655, 2017.","apa":"Matthee, J. J., Sobral, D., Best, P., Khostovan, A. A., Oteo, I., Bouwens, R., & Röttgering, H. (2017). The production and escape of Lyman-Continuum radiation from star-forming galaxies at z ∼ 2 and their redshift evolution. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stw2973","ama":"Matthee JJ, Sobral D, Best P, et al. The production and escape of Lyman-Continuum radiation from star-forming galaxies at z ∼ 2 and their redshift evolution. Monthly Notices of the Royal Astronomical Society. 2017;465(3):3637-3655. doi:10.1093/mnras/stw2973","ista":"Matthee JJ, Sobral D, Best P, Khostovan AA, Oteo I, Bouwens R, Röttgering H. 2017. The production and escape of Lyman-Continuum radiation from star-forming galaxies at z ∼ 2 and their redshift evolution. Monthly Notices of the Royal Astronomical Society. 465(3), 3637–3655.","mla":"Matthee, Jorryt J., et al. “The Production and Escape of Lyman-Continuum Radiation from Star-Forming Galaxies at z ∼ 2 and Their Redshift Evolution.” Monthly Notices of the Royal Astronomical Society, vol. 465, no. 3, Oxford University Press, 2017, pp. 3637–55, doi:10.1093/mnras/stw2973.","short":"J.J. Matthee, D. Sobral, P. Best, A.A. Khostovan, I. Oteo, R. Bouwens, H. Röttgering, Monthly Notices of the Royal Astronomical Society 465 (2017) 3637–3655."},"article_type":"original","publisher":"Oxford University Press","page":"3637-3655","quality_controlled":"1","title":"The production and escape of Lyman-Continuum radiation from star-forming galaxies at z ∼ 2 and their redshift evolution","intvolume":" 465","publication_status":"published","article_processing_charge":"No","date_created":"2022-07-12T12:12:14Z","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","last_name":"Matthee"},{"full_name":"Sobral, David","first_name":"David","last_name":"Sobral"},{"full_name":"Best, Philip","first_name":"Philip","last_name":"Best"},{"last_name":"Khostovan","first_name":"Ali Ahmad","full_name":"Khostovan, Ali Ahmad"},{"full_name":"Oteo, Iván","first_name":"Iván","last_name":"Oteo"},{"full_name":"Bouwens, Rychard","last_name":"Bouwens","first_name":"Rychard"},{"full_name":"Röttgering, Huub","last_name":"Röttgering","first_name":"Huub"}],"issue":"3","_id":"11564","scopus_import":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1605.08782"}],"oa":1,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"date_published":"2017-03-01T00:00:00Z","type":"journal_article","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","cosmology: observations","dark ages","reionization","first stars"],"month":"03","oa_version":"Preprint","publication":"Monthly Notices of the Royal Astronomical Society"},{"quality_controlled":"1","page":"2381-2396","publisher":"Oxford University Press","article_type":"original","scopus_import":"1","_id":"11565","issue":"2","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J"},{"full_name":"Schaye, Joop","last_name":"Schaye","first_name":"Joop"},{"full_name":"Crain, Robert A.","first_name":"Robert A.","last_name":"Crain"},{"full_name":"Schaller, Matthieu","last_name":"Schaller","first_name":"Matthieu"},{"first_name":"Richard","last_name":"Bower","full_name":"Bower, Richard"},{"first_name":"Tom","last_name":"Theuns","full_name":"Theuns, Tom"}],"date_created":"2022-07-12T12:25:08Z","article_processing_charge":"No","publication_status":"published","intvolume":" 465","title":"The origin of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE simulation","volume":465,"acknowledgement":"We thank the anonymous referee for their comments. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. JM thanks David Sobral for useful discussions and help with fitting routines and Jonas Chavez Montero and Ying Zu for providing data. We thank PRACE for the access to the Curie facility in France. We have used the DiRAC system which is a part of National E-Infrastructure at Durham University, operated by the Institute for Computational Cosmology on behalf of the STFC DiRAC HPC Facility (www.dirac.ac.uk); the equipment was funded by BIS National E-infrastructure capital grant ST/K00042X/1, STFC capital grant ST/H008519/1, STFC DiRAC Operations grant ST/K003267/1 and Durham University. The study was sponsored by the Dutch National Computing Facilities Foundation (NCF) for the use of supercomputer facilities, with financial support from the Netherlands Organisation for Scientific Research (NWO), through VICI grant 639.043.409, and the European Research Council under the European Union’s Seventh Framework Programme (FP7/2007-2013)/ERC Grant agreement 278594- GasAroundGalaxies, and from the Belgian Science Policy Office ([AP P7/08 CHARM]). We have benefited greatly from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY, H5PY and RPY2 packages, and the TOPCAT analysis program (Taylor 2005).","extern":"1","citation":{"apa":"Matthee, J. J., Schaye, J., Crain, R. A., Schaller, M., Bower, R., & Theuns, T. (2017). The origin of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE simulation. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stw2884","ama":"Matthee JJ, Schaye J, Crain RA, Schaller M, Bower R, Theuns T. The origin of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE simulation. Monthly Notices of the Royal Astronomical Society. 2017;465(2):2381-2396. doi:10.1093/mnras/stw2884","ieee":"J. J. Matthee, J. Schaye, R. A. Crain, M. Schaller, R. Bower, and T. Theuns, “The origin of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE simulation,” Monthly Notices of the Royal Astronomical Society, vol. 465, no. 2. Oxford University Press, pp. 2381–2396, 2017.","chicago":"Matthee, Jorryt J, Joop Schaye, Robert A. Crain, Matthieu Schaller, Richard Bower, and Tom Theuns. “The Origin of Scatter in the Stellar Mass–Halo Mass Relation of Central Galaxies in the EAGLE Simulation.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2017. https://doi.org/10.1093/mnras/stw2884.","short":"J.J. Matthee, J. Schaye, R.A. Crain, M. Schaller, R. Bower, T. Theuns, Monthly Notices of the Royal Astronomical Society 465 (2017) 2381–2396.","mla":"Matthee, Jorryt J., et al. “The Origin of Scatter in the Stellar Mass–Halo Mass Relation of Central Galaxies in the EAGLE Simulation.” Monthly Notices of the Royal Astronomical Society, vol. 465, no. 2, Oxford University Press, 2017, pp. 2381–96, doi:10.1093/mnras/stw2884.","ista":"Matthee JJ, Schaye J, Crain RA, Schaller M, Bower R, Theuns T. 2017. The origin of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE simulation. Monthly Notices of the Royal Astronomical Society. 465(2), 2381–2396."},"year":"2017","date_updated":"2022-08-19T07:56:07Z","external_id":{"arxiv":["1608.08218"]},"day":"01","doi":"10.1093/mnras/stw2884","arxiv":1,"abstract":[{"lang":"eng","text":"We use the hydrodynamical EAGLE simulation to study the magnitude and origin of the scatter in the stellar mass–halo mass relation for central galaxies. We separate cause and effect by correlating stellar masses in the baryonic simulation with halo properties in a matched dark matter only (DMO) simulation. The scatter in stellar mass increases with redshift and decreases with halo mass. At z = 0.1, it declines from 0.25 dex at M200, DMO ≈ 1011 M⊙ to 0.12 dex at M200, DMO ≈ 1013 M⊙, but the trend is weak above 1012 M⊙. For M200, DMO < 1012.5 M⊙ up to 0.04 dex of the scatter is due to scatter in the halo concentration. At fixed halo mass, a larger stellar mass corresponds to a more concentrated halo. This is likely because higher concentrations imply earlier formation times and hence more time for accretion and star formation, and/or because feedback is less efficient in haloes with higher binding energies. The maximum circular velocity, Vmax, DMO, and binding energy are therefore more fundamental properties than halo mass, meaning that they are more accurate predictors of stellar mass, and we provide fitting formulae for their relations with stellar mass. However, concentration alone cannot explain the total scatter in the Mstar−M200,DMO relation, and it does not explain the scatter in Mstar–Vmax, DMO. Halo spin, sphericity, triaxiality, substructure and environment are also not responsible for the remaining scatter, which thus could be due to more complex halo properties or non-linear/stochastic baryonic effects."}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: formation","galaxies: haloes","cosmology: theory"],"language":[{"iso":"eng"}],"publication":"Monthly Notices of the Royal Astronomical Society","oa_version":"Preprint","month":"02","main_file_link":[{"url":"https://arxiv.org/abs/1608.08218","open_access":"1"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","type":"journal_article","date_published":"2017-02-01T00:00:00Z","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"oa":1},{"publication_status":"published","date_created":"2022-07-13T09:47:39Z","article_processing_charge":"No","title":"Spectroscopic properties of luminous Ly α emitters at z ≈ 6–7 and comparison to the Lyman-break population","intvolume":" 472","_id":"11572","scopus_import":"1","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"},{"last_name":"Darvish","first_name":"Behnam","full_name":"Darvish, Behnam"},{"full_name":"Santos, Sérgio","first_name":"Sérgio","last_name":"Santos"},{"first_name":"Bahram","last_name":"Mobasher","full_name":"Mobasher, Bahram"},{"full_name":"Paulino-Afonso, Ana","last_name":"Paulino-Afonso","first_name":"Ana"},{"last_name":"Röttgering","first_name":"Huub","full_name":"Röttgering, Huub"},{"full_name":"Alegre, Lara","last_name":"Alegre","first_name":"Lara"}],"issue":"1","publisher":"Oxford University Press","article_type":"original","page":"772-787","quality_controlled":"1","arxiv":1,"doi":"10.1093/mnras/stx2061","day":"01","abstract":[{"lang":"eng","text":"We present spectroscopic follow-up of candidate luminous Ly α emitters (LAEs) at z = 5.7–6.6 in the SA22 field with VLT/X-SHOOTER. We confirm two new luminous LAEs at z = 5.676 (SR6) and z = 6.532 (VR7), and also present HST follow-up of both sources. These sources have luminosities LLy α ≈ 3 × 1043 erg s−1, very high rest-frame equivalent widths of EW0 ≳ 200 Å and narrow Ly α lines (200–340 km s−1). VR7 is the most UV-luminous LAE at z > 6.5, with M1500 = −22.5, even brighter in the UV than CR7. Besides Ly α, we do not detect any other rest-frame UV lines in the spectra of SR6 and VR7, and argue that rest-frame UV lines are easier to observe in bright galaxies with low Ly α equivalent widths. We confirm that Ly α line widths increase with Ly α luminosity at z = 5.7, while there are indications that Ly α lines of faint LAEs become broader at z = 6.6, potentially due to reionization. We find a large spread of up to 3 dex in UV luminosity for >L⋆ LAEs, but find that the Ly α luminosity of the brightest LAEs is strongly related to UV luminosity at z = 6.6. Under basic assumptions, we find that several LAEs at z ≈ 6–7 have Ly α escape fractions ≳ 100 per cent, indicating bursty star formation histories, alternative Ly α production mechanisms, or dust attenuating Ly α emission differently than UV emission. Finally, we present a method to compute ξion, the production efficiency of ionizing photons, and find that LAEs at z ≈ 6–7 have high values of log10(ξion/Hz erg−1) ≈ 25.51 ± 0.09 that may alleviate the need for high Lyman-Continuum escape fractions required for reionization."}],"date_updated":"2022-08-19T08:05:37Z","year":"2017","citation":{"ista":"Matthee JJ, Sobral D, Darvish B, Santos S, Mobasher B, Paulino-Afonso A, Röttgering H, Alegre L. 2017. Spectroscopic properties of luminous Ly α emitters at z ≈ 6–7 and comparison to the Lyman-break population. Monthly Notices of the Royal Astronomical Society. 472(1), 772–787.","mla":"Matthee, Jorryt J., et al. “Spectroscopic Properties of Luminous Ly α Emitters at z ≈ 6–7 and Comparison to the Lyman-Break Population.” Monthly Notices of the Royal Astronomical Society, vol. 472, no. 1, Oxford University Press, 2017, pp. 772–87, doi:10.1093/mnras/stx2061.","short":"J.J. Matthee, D. Sobral, B. Darvish, S. Santos, B. Mobasher, A. Paulino-Afonso, H. Röttgering, L. Alegre, Monthly Notices of the Royal Astronomical Society 472 (2017) 772–787.","ieee":"J. J. Matthee et al., “Spectroscopic properties of luminous Ly α emitters at z ≈ 6–7 and comparison to the Lyman-break population,” Monthly Notices of the Royal Astronomical Society, vol. 472, no. 1. Oxford University Press, pp. 772–787, 2017.","chicago":"Matthee, Jorryt J, David Sobral, Behnam Darvish, Sérgio Santos, Bahram Mobasher, Ana Paulino-Afonso, Huub Röttgering, and Lara Alegre. “Spectroscopic Properties of Luminous Ly α Emitters at z ≈ 6–7 and Comparison to the Lyman-Break Population.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2017. https://doi.org/10.1093/mnras/stx2061.","apa":"Matthee, J. J., Sobral, D., Darvish, B., Santos, S., Mobasher, B., Paulino-Afonso, A., … Alegre, L. (2017). Spectroscopic properties of luminous Ly α emitters at z ≈ 6–7 and comparison to the Lyman-break population. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stx2061","ama":"Matthee JJ, Sobral D, Darvish B, et al. Spectroscopic properties of luminous Ly α emitters at z ≈ 6–7 and comparison to the Lyman-break population. Monthly Notices of the Royal Astronomical Society. 2017;472(1):772-787. doi:10.1093/mnras/stx2061"},"external_id":{"arxiv":["1706.06591"]},"acknowledgement":"We thank the referee for a constructive report that has improved the quality and clarity of this work. The authors thank Grecco Oyarzún for discussions. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. DS 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. BD acknowledges financial support from NASA through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G. We thank Kasper Schmidt for providing measurements. Based on observations with the W.M. Keck Observatory through programme C267D. The W.M. Keck Observatory is operated as a scientific partnership amongst the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 097.A-0943, 294.A 5018 and 098.A-0819 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 observing time (W16AN004) and 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. Based on observations made with the NASA/ESA HST, obtained (from the Data Archive) 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 programme #14699. We are grateful for the excellent data sets from the COSMOS, UltraVISTA, SXDS, UDS and CFHTLS survey teams; without these legacy surveys, this research would have been impossible. We have benefited from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY and ASTROPY packages, the astronomical imaging tools SEXTRACTOR, SWARP and SCAMP and the TOPCAT analysis tool (Taylor 2013).","volume":472,"extern":"1","oa_version":"Preprint","month":"11","publication":"Monthly Notices of the Royal Astronomical Society","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution – galaxies: high-redshift","dark ages","reionization","first stars","cosmology: observations"],"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"oa":1,"date_published":"2017-11-01T00:00:00Z","type":"journal_article","main_file_link":[{"url":"https://arxiv.org/abs/1706.06591","open_access":"1"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public"},{"extern":"1","acknowledgement":"We wish to thank the anonymous referee for their comments, which have improved the quality and clarity of this work. OJT acknowledges the financial support of the Science and Technology Facilities Council through a studentship award. MC and OJT acknowledge the KMOS team and all the personnel of the European Southern Observatory Very Large Telescope for outstanding support during the KMOS GTO observations. CMH, AMS and RMS acknowledge the Science and Technology Facilities Council through grant code ST/L00075X/1. RJM acknowledges the support of the European Research Council via the award of a Consolidator Grant (PI: McLure). JSD acknowledges the support of the European Research Council via the award of an Advanced Grant (PI J. Dunlop), and the contribution of the EC FP7 SPACE project ASTRODEEP (Ref.No: 312725). AMS acknowledges the Leverhulme Foundation. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. DS acknowledges financial support from the Netherlands Organization for Scientific research (NWO) through a Veni fellowship and from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010). This work is based on observations taken by the CANDELS Multi-Cycle Treasury Program with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. This work is based on observations taken by the 3D HST Treasury Program (GO 12177 and 12328) with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Based on data obtained with the European Southern Observatory Very Large Telescope, Paranal, Chile, under Large Program 185.A-0791, and made available by the VUDS team at the CESAM data centre, Laboratoire d’Astrophysique de Marseille, France. Based on observations obtained at the Very Large Telescope of the European Southern Observatory. Programme IDs: 092.A 0399(A), 093.A-0122(A,B), 094.A-0214(A,B),095.A0680(A,B),096.A-0315(A,B,C).","volume":471,"external_id":{"arxiv":["1704.06263"]},"year":"2017","citation":{"ista":"Turner OJ, Cirasuolo M, Harrison CM, McLure RJ, Dunlop JS, Swinbank AM, Johnson HL, Sobral D, Matthee JJ, Sharples RM. 2017. The KMOS Deep Survey (KDS) – I. Dynamical measurements of typical star-forming galaxies at z ≃ 3.5. Monthly Notices of the Royal Astronomical Society. 471(2), 1280–1320.","mla":"Turner, O. J., et al. “The KMOS Deep Survey (KDS) – I. Dynamical Measurements of Typical Star-Forming Galaxies at z ≃ 3.5.” Monthly Notices of the Royal Astronomical Society, vol. 471, no. 2, Oxford University Press, 2017, pp. 1280–320, doi:10.1093/mnras/stx1366.","short":"O.J. Turner, M. Cirasuolo, C.M. Harrison, R.J. McLure, J.S. Dunlop, A.M. Swinbank, H.L. Johnson, D. Sobral, J.J. Matthee, R.M. Sharples, Monthly Notices of the Royal Astronomical Society 471 (2017) 1280–1320.","chicago":"Turner, O. J., M. Cirasuolo, C. M. Harrison, R. J. McLure, J. S. Dunlop, A. M. Swinbank, H. L. Johnson, D. Sobral, Jorryt J Matthee, and R. M. Sharples. “The KMOS Deep Survey (KDS) – I. Dynamical Measurements of Typical Star-Forming Galaxies at z ≃ 3.5.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2017. https://doi.org/10.1093/mnras/stx1366.","ieee":"O. J. Turner et al., “The KMOS Deep Survey (KDS) – I. Dynamical measurements of typical star-forming galaxies at z ≃ 3.5,” Monthly Notices of the Royal Astronomical Society, vol. 471, no. 2. Oxford University Press, pp. 1280–1320, 2017.","apa":"Turner, O. J., Cirasuolo, M., Harrison, C. M., McLure, R. J., Dunlop, J. S., Swinbank, A. M., … Sharples, R. M. (2017). The KMOS Deep Survey (KDS) – I. Dynamical measurements of typical star-forming galaxies at z ≃ 3.5. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stx1366","ama":"Turner OJ, Cirasuolo M, Harrison CM, et al. The KMOS Deep Survey (KDS) – I. Dynamical measurements of typical star-forming galaxies at z ≃ 3.5. Monthly Notices of the Royal Astronomical Society. 2017;471(2):1280-1320. doi:10.1093/mnras/stx1366"},"date_updated":"2022-08-19T08:07:31Z","abstract":[{"text":"We present dynamical measurements from the KMOS (K-band multi-object spectrograph) Deep Survey (KDS), which comprises 77 typical star-forming galaxies at z ≃ 3.5 in the mass range 9.0 < log (M⋆/M⊙) < 10.5. These measurements constrain the internal dynamics, the intrinsic velocity dispersions (σint) and rotation velocities (VC) of galaxies in the high-redshift Universe. The mean velocity dispersion of the galaxies in our sample is σint=70.8+3.3−3.1kms−1, revealing that the increasing average σint with increasing redshift, reported for z ≲ 2, continues out to z ≃ 3.5. Only 36 ± 8 per cent of our galaxies are rotation-dominated (VC/σint > 1), with the sample average VC/σint value much smaller than at lower redshift. After carefully selecting comparable star-forming samples at multiple epochs, we find that the rotation-dominated fraction evolves with redshift with a z−0.2 dependence. The rotation-dominated KDS galaxies show no clear offset from the local rotation velocity–stellar mass (i.e. VC–M⋆) relation, although a smaller fraction of the galaxies are on the relation due to the increase in the dispersion-dominated fraction. These observations are consistent with a simple equilibrium model picture, in which random motions are boosted in high-redshift galaxies by a combination of the increasing gas fractions, accretion efficiency, specific star formation rate and stellar feedback and which may provide significant pressure support against gravity on the galactic disc scale.","lang":"eng"}],"day":"01","doi":"10.1093/mnras/stx1366","arxiv":1,"quality_controlled":"1","page":"1280-1320","article_type":"original","publisher":"Oxford University Press","issue":"2","author":[{"full_name":"Turner, O. J.","last_name":"Turner","first_name":"O. J."},{"full_name":"Cirasuolo, M.","first_name":"M.","last_name":"Cirasuolo"},{"first_name":"C. M.","last_name":"Harrison","full_name":"Harrison, C. M."},{"full_name":"McLure, R. J.","first_name":"R. J.","last_name":"McLure"},{"last_name":"Dunlop","first_name":"J. S.","full_name":"Dunlop, J. S."},{"last_name":"Swinbank","first_name":"A. M.","full_name":"Swinbank, A. M."},{"full_name":"Johnson, H. L.","last_name":"Johnson","first_name":"H. L."},{"full_name":"Sobral, D.","last_name":"Sobral","first_name":"D."},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J"},{"full_name":"Sharples, R. M.","last_name":"Sharples","first_name":"R. M."}],"scopus_import":"1","_id":"11573","intvolume":" 471","title":"The KMOS Deep Survey (KDS) – I. Dynamical measurements of typical star-forming galaxies at z ≃ 3.5","date_created":"2022-07-13T10:03:01Z","article_processing_charge":"No","publication_status":"published","status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"url":"https://arxiv.org/abs/1704.06263","open_access":"1"}],"type":"journal_article","date_published":"2017-10-01T00:00:00Z","oa":1,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","galaxies: kinematics and dynamics"],"language":[{"iso":"eng"}],"publication":"Monthly Notices of the Royal Astronomical Society","month":"10","oa_version":"Preprint"},{"title":"The Fundamental Plane of star formation in galaxies revealed by the EAGLE hydrodynamical simulations","intvolume":" 459","publication_status":"published","article_processing_charge":"No","date_created":"2022-07-13T10:21:24Z","author":[{"full_name":"Lagos, Claudia del P.","last_name":"Lagos","first_name":"Claudia del P."},{"full_name":"Theuns, Tom","last_name":"Theuns","first_name":"Tom"},{"full_name":"Schaye, Joop","last_name":"Schaye","first_name":"Joop"},{"full_name":"Furlong, Michelle","last_name":"Furlong","first_name":"Michelle"},{"full_name":"Bower, Richard G.","first_name":"Richard G.","last_name":"Bower"},{"full_name":"Schaller, Matthieu","last_name":"Schaller","first_name":"Matthieu"},{"full_name":"Crain, Robert A.","first_name":"Robert A.","last_name":"Crain"},{"first_name":"James W.","last_name":"Trayford","full_name":"Trayford, James W."},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J"}],"issue":"3","_id":"11575","scopus_import":"1","article_type":"original","publisher":"Oxford University Press","page":"2632-2650","quality_controlled":"1","abstract":[{"lang":"eng","text":"We investigate correlations between different physical properties of star-forming galaxies in the ‘Evolution and Assembly of GaLaxies and their Environments’ (EAGLE) cosmological hydrodynamical simulation suite over the redshift range 0 ≤ z ≤ 4.5. A principal component analysis reveals that neutral gas fraction (fgas,neutral), stellar mass (Mstellar) and star formation rate (SFR) account for most of the variance seen in the population, with galaxies tracing a two-dimensional, nearly flat, surface in the three-dimensional space of fgas, neutral–Mstellar–SFR with little scatter. The location of this plane varies little with redshift, whereas galaxies themselves move along the plane as their fgas, neutral and SFR drop with redshift. The positions of galaxies along the plane are highly correlated with gas metallicity. The metallicity can therefore be robustly predicted from fgas, neutral, or from the Mstellar and SFR. We argue that the appearance of this ‘Fundamental Plane of star formation’ is a consequence of self-regulation, with the plane's curvature set by the dependence of the SFR on gas density and metallicity. We analyse a large compilation of observations spanning the redshift range 0 ≲ z ≲ 3, and find that such a plane is also present in the data. The properties of the observed Fundamental Plane of star formation are in good agreement with EAGLE's predictions."}],"doi":"10.1093/mnras/stw717","arxiv":1,"day":"01","external_id":{"arxiv":["1510.08067"]},"date_updated":"2022-08-19T08:12:07Z","year":"2016","citation":{"mla":"Lagos, Claudia del P., et al. “The Fundamental Plane of Star Formation in Galaxies Revealed by the EAGLE Hydrodynamical Simulations.” Monthly Notices of the Royal Astronomical Society, vol. 459, no. 3, Oxford University Press, 2016, pp. 2632–50, doi:10.1093/mnras/stw717.","short":"C. del P. Lagos, T. Theuns, J. Schaye, M. Furlong, R.G. Bower, M. Schaller, R.A. Crain, J.W. Trayford, J.J. Matthee, Monthly Notices of the Royal Astronomical Society 459 (2016) 2632–2650.","ista":"Lagos C del P, Theuns T, Schaye J, Furlong M, Bower RG, Schaller M, Crain RA, Trayford JW, Matthee JJ. 2016. The Fundamental Plane of star formation in galaxies revealed by the EAGLE hydrodynamical simulations. Monthly Notices of the Royal Astronomical Society. 459(3), 2632–2650.","ama":"Lagos C del P, Theuns T, Schaye J, et al. The Fundamental Plane of star formation in galaxies revealed by the EAGLE hydrodynamical simulations. Monthly Notices of the Royal Astronomical Society. 2016;459(3):2632-2650. doi:10.1093/mnras/stw717","apa":"Lagos, C. del P., Theuns, T., Schaye, J., Furlong, M., Bower, R. G., Schaller, M., … Matthee, J. J. (2016). The Fundamental Plane of star formation in galaxies revealed by the EAGLE hydrodynamical simulations. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stw717","chicago":"Lagos, Claudia del P., Tom Theuns, Joop Schaye, Michelle Furlong, Richard G. Bower, Matthieu Schaller, Robert A. Crain, James W. Trayford, and Jorryt J Matthee. “The Fundamental Plane of Star Formation in Galaxies Revealed by the EAGLE Hydrodynamical Simulations.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2016. https://doi.org/10.1093/mnras/stw717.","ieee":"C. del P. Lagos et al., “The Fundamental Plane of star formation in galaxies revealed by the EAGLE hydrodynamical simulations,” Monthly Notices of the Royal Astronomical Society, vol. 459, no. 3. Oxford University Press, pp. 2632–2650, 2016."},"extern":"1","acknowledgement":"We thank Luca Cortese, Matt Bothwell, Paola Santini and Tim Davis for providing observational data sets, and Aaron Robotham, Luca Cortese and Barbara Catinella for useful discussions. CdPL is funded by a Discovery Early Career Researcher Award (DE150100618). CdPL also thanks the MERAC Foundation for a Postdoctoral Research Award. This work used the DiRAC Data Centric system at Durham University, operated by the Institute for Computational Cosmology on behalf of the STFC DiRAC HPC Facility (www.dirac.ac.uk). This equipment was funded by BIS National E-infrastructure capital grant ST/K00042X/1, STFC capital grant ST/H008519/1, and STFC DiRAC Operations grant ST/K003267/1 and Durham University. DiRAC is part of the National E-Infrastructure. Support was also received via the Interuniversity Attraction Poles Programme initiated by the Belgian Science Policy Office ([AP P7/08 CHARM]), the National Science Foundation under grant no. NSF PHY11-25915, and the UK Science and Technology Facilities Council (grant numbers ST/F001166/1 and ST/I000976/1) via rolling and consolidating grants awarded to the ICC. The research was supported in part by the European Research Council under the European Union‘s Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement 278594-GasAroundGalaxies.","volume":459,"month":"07","oa_version":"Preprint","publication":"Monthly Notices of the Royal Astronomical Society","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics stars: formation","ISM: evolution","galaxies: evolution","galaxies: formation","galaxies: ISM"],"oa":1,"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"date_published":"2016-07-01T00:00:00Z","type":"journal_article","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1510.08067"}]},{"article_processing_charge":"No","date_created":"2022-07-13T12:50:36Z","publication_status":"published","intvolume":" 457","title":"The most luminous H α emitters at z ∼ 0.8–2.23 from HiZELS: Evolution of AGN and star-forming galaxies","scopus_import":"1","_id":"11576","issue":"2","author":[{"full_name":"Sobral, David","last_name":"Sobral","first_name":"David"},{"full_name":"Kohn, Saul A.","last_name":"Kohn","first_name":"Saul A."},{"last_name":"Best","first_name":"Philip N.","full_name":"Best, Philip N."},{"first_name":"Ian","last_name":"Smail","full_name":"Smail, Ian"},{"last_name":"Harrison","first_name":"Chris M.","full_name":"Harrison, Chris M."},{"last_name":"Stott","first_name":"John","full_name":"Stott, John"},{"first_name":"João","last_name":"Calhau","full_name":"Calhau, João"},{"last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720"}],"publisher":"Oxford University Press","article_type":"original","quality_controlled":"1","page":"1739-1752","day":"01","doi":"10.1093/mnras/stw022","arxiv":1,"abstract":[{"lang":"eng","text":"We use new near-infrared spectroscopic observations to investigate the nature and evolution of the most luminous Hα emitters at z ∼ 0.8–2.23, which evolve strongly in number density over this period, and compare them to more typical Hα emitters. We study 59 luminous Hα emitters with LHα > L∗Hα, roughly equally split per redshift slice at z ∼ 0.8, 1.47 and 2.23 from the HiZELS and CF-HiZELS surveys. We find that, overall, 30 ± 8 per cent are active galactic nuclei [AGNs; 80 ± 30 per cent of these AGNs are broad-line AGNs, BL-AGNs], and we find little to no evolution in the AGN fraction with redshift, within the errors. However, the AGN fraction increases strongly with Hα luminosity and correlates best with LHα/L∗Hα(z). While LHα ≤ L∗Hα(z) Hα emitters are largely dominated by star-forming galaxies (>80 per cent), the most luminous Hα emitters (LHα>10L∗Hα(z)) at any cosmic time are essentially all BL-AGN. Using our AGN-decontaminated sample of luminous star-forming galaxies, and integrating down to a fixed Hα luminosity, we find a factor of ∼1300 evolution in the star formation rate density from z = 0 to 2.23. This is much stronger than the evolution from typical Hα star-forming galaxies and in line with the evolution seen for constant luminosity cuts used to select ‘ultraluminous’ infrared galaxies and/or sub-millimetre galaxies. By taking into account the evolution in the typical Hα luminosity, we show that the most strongly star-forming Hα-selected galaxies at any epoch (LHα>L∗Hα(z)) contribute the same fractional amount of ≈15 per cent to the total star formation rate density, at least up to z = 2.23."}],"year":"2016","citation":{"ista":"Sobral D, Kohn SA, Best PN, Smail I, Harrison CM, Stott J, Calhau J, Matthee JJ. 2016. The most luminous H α emitters at z ∼ 0.8–2.23 from HiZELS: Evolution of AGN and star-forming galaxies. Monthly Notices of the Royal Astronomical Society. 457(2), 1739–1752.","short":"D. Sobral, S.A. Kohn, P.N. Best, I. Smail, C.M. Harrison, J. Stott, J. Calhau, J.J. Matthee, Monthly Notices of the Royal Astronomical Society 457 (2016) 1739–1752.","mla":"Sobral, David, et al. “The Most Luminous H α Emitters at z ∼ 0.8–2.23 from HiZELS: Evolution of AGN and Star-Forming Galaxies.” Monthly Notices of the Royal Astronomical Society, vol. 457, no. 2, Oxford University Press, 2016, pp. 1739–52, doi:10.1093/mnras/stw022.","ieee":"D. Sobral et al., “The most luminous H α emitters at z ∼ 0.8–2.23 from HiZELS: Evolution of AGN and star-forming galaxies,” Monthly Notices of the Royal Astronomical Society, vol. 457, no. 2. Oxford University Press, pp. 1739–1752, 2016.","chicago":"Sobral, David, Saul A. Kohn, Philip N. Best, Ian Smail, Chris M. Harrison, John Stott, João Calhau, and Jorryt J Matthee. “The Most Luminous H α Emitters at z ∼ 0.8–2.23 from HiZELS: Evolution of AGN and Star-Forming Galaxies.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2016. https://doi.org/10.1093/mnras/stw022.","apa":"Sobral, D., Kohn, S. A., Best, P. N., Smail, I., Harrison, C. M., Stott, J., … Matthee, J. J. (2016). The most luminous H α emitters at z ∼ 0.8–2.23 from HiZELS: Evolution of AGN and star-forming galaxies. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stw022","ama":"Sobral D, Kohn SA, Best PN, et al. The most luminous H α emitters at z ∼ 0.8–2.23 from HiZELS: Evolution of AGN and star-forming galaxies. Monthly Notices of the Royal Astronomical Society. 2016;457(2):1739-1752. doi:10.1093/mnras/stw022"},"date_updated":"2022-08-19T08:15:21Z","external_id":{"arxiv":["1601.02266"]},"acknowledgement":"The authors would like to thank the anonymous reviewer for the many helpful comments and suggestions which greatly improved the clarity and quality of this work. DS and SAK 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) and from FCT grant PEst-OE/FIS/UI2751/2014. Part of this project was undertaken during the inaugural Leiden/ESA Astrophysics Program for Summer Students (LEAPS). IRS acknowledges support from STFC (ST/L00075X/1), the ERC Advanced Investigator programme DUSTYGAL 321334 and a Royal Society/Wolfson merit award. CH acknowledges support from STFC. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 087.A-0337 and ID 089.A-0965. Also based on data from the Telescopio Nazionale Galileo, with time awarded through OPTICON programmes 2011A/026 and 2012A020 and the William Herschel Telescope under programme W12BN007. The William Herschel Telescope is operated on the island of La Palma by the Isaac Newton Group in the Spanish\r\nObservatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. The authors wish to thank all the help given by the telescope staff from all the observatories used in this study: ESO staff in La Silla, and the TNG and WHT staff in La Palma. This publication makes use of data products from the Two Micron All-Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation.","volume":457,"extern":"1","oa_version":"Preprint","month":"04","publication":"Monthly Notices of the Royal Astronomical Society","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","cosmology: observations"],"language":[{"iso":"eng"}],"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"oa":1,"type":"journal_article","date_published":"2016-04-01T00:00:00Z","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1601.02266"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public"},{"day":"01","arxiv":1,"doi":"10.1093/mnras/stw322","abstract":[{"lang":"eng","text":"We present the first results from our CAlibrating LYMan α with Hα (CALYMHA) pilot survey at the Isaac Newton Telescope. We measure Lyα emission for 488 Hα selected galaxies at z = 2.23 from High-z Emission Line Survey in the COSMOS and UDS fields with a specially designed narrow-band filter (λc = 3918 Å, Δλ = 52 Å). We find 17 dual Hα-Lyα emitters [fLyα > 5 × 10−17 erg s−1 cm−2, of which five are X-ray active galactic nuclei (AGN)]. For star-forming galaxies, we find a range of Lyα escape fractions (fesc, measured with 3 arcsec apertures) from 2 to 30 per cent. These galaxies have masses from 3 × 108 M⊙ to 1011 M⊙ and dust attenuations E(B − V) = 0–0.5. Using stacking, we measure a median escape fraction of 1.6 ± 0.5 per cent (4.0 ± 1.0 per cent without correcting Hα for dust), but show that this depends on galaxy properties. The stacked fesc tends to decrease with increasing star formation rate and dust attenuation. However, at the highest masses and dust attenuations, we detect individual galaxies with fesc much higher than the typical values from stacking, indicating significant scatter in the values of fesc. Relations between fesc and UV slope are bimodal, with high fesc for either the bluest or reddest galaxies. We speculate that this bimodality and large scatter in the values of fesc is due to additional physical mechanisms such as outflows facilitating fesc for dusty/massive systems. Lyα is significantly more extended than Hα and the UV. fesc continues to increase up to at least 20 kpc (3σ, 40 kpc [2σ]) for typical star-forming galaxies and thus the aperture is the most important predictor of fesc."}],"citation":{"mla":"Matthee, Jorryt J., et al. “The CALYMHA Survey: Lyα Escape Fraction and Its Dependence on Galaxy Properties at z = 2.23.” Monthly Notices of the Royal Astronomical Society, vol. 458, no. 1, Oxford University Press, 2016, pp. 449–67, doi:10.1093/mnras/stw322.","short":"J.J. Matthee, D. Sobral, I. Oteo, P. Best, I. Smail, H. Röttgering, A. Paulino-Afonso, Monthly Notices of the Royal Astronomical Society 458 (2016) 449–467.","ista":"Matthee JJ, Sobral D, Oteo I, Best P, Smail I, Röttgering H, Paulino-Afonso A. 2016. The CALYMHA survey: Lyα escape fraction and its dependence on galaxy properties at z = 2.23. Monthly Notices of the Royal Astronomical Society. 458(1), 449–467.","ama":"Matthee JJ, Sobral D, Oteo I, et al. The CALYMHA survey: Lyα escape fraction and its dependence on galaxy properties at z = 2.23. Monthly Notices of the Royal Astronomical Society. 2016;458(1):449-467. doi:10.1093/mnras/stw322","apa":"Matthee, J. J., Sobral, D., Oteo, I., Best, P., Smail, I., Röttgering, H., & Paulino-Afonso, A. (2016). The CALYMHA survey: Lyα escape fraction and its dependence on galaxy properties at z = 2.23. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stw322","ieee":"J. J. Matthee et al., “The CALYMHA survey: Lyα escape fraction and its dependence on galaxy properties at z = 2.23,” Monthly Notices of the Royal Astronomical Society, vol. 458, no. 1. Oxford University Press, pp. 449–467, 2016.","chicago":"Matthee, Jorryt J, David Sobral, Iván Oteo, Philip Best, Ian Smail, Huub Röttgering, and Ana Paulino-Afonso. “The CALYMHA Survey: Lyα Escape Fraction and Its Dependence on Galaxy Properties at z = 2.23.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2016. https://doi.org/10.1093/mnras/stw322."},"year":"2016","date_updated":"2022-08-19T08:17:19Z","external_id":{"arxiv":["1602.02756"]},"volume":458,"acknowledgement":"We thank the anonymous referee for constructive comments and suggestions which have improved the quality of this work. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. DS and JM acknowledge financial support from the Netherlands Organization for Scientific research (NWO) through a Veni fellowship, and DS from FCT through a FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010) and from FCT grant PEst-OE/FIS/UI2751/2014. IO acknowledges support from the European Research Council (ERC) in the form of Advanced Investigator Programme, COSMICISM, 321302. HR acknowledges support from the ERC Advanced Investigator programme NewClusters 321271. IRS acknowledges support from STFC (ST/L00075X/1), the ERC Advanced Investigator programme DUSTYGAL 321334 and a Royal Society/Wolfson Merit Award. APA acknowledges support from the Fundac¸ao para a Ciencia e para a Tecnologia (FCT) through the Fellowship SFRH/BD/52706/2014.\r\nBased on observations made with the Isaac Newton Telescope (proposals 2013AN002, 2013BN008, 2014AC88, 2014AN002, 2014BN006, 2014BC118) operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrof´ısica de Canarias. We acknowledge the tremendous work that has been done by both COSMOS and UKIDSS UDS/SXDF teams in assembling such large, state-ofthe-art multi-wavelength data sets over such wide areas, as those have been crucial for the results presented in this paper. The sample of HAEs is publicly available from Sobral et al. (2013).\r\nWe have benefited greatly from the publically available programming language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY (Jones et al. 2001; Hunter 2007; Van Der Walt, Colbert & Varoquaux 2011) and ASTROPY (Astropy Collaboration et al. 2013) packages, the imaging tools SEXTRACTOR, SWARP and SCAMP (Bertin & Arnouts 1996; Bertin 2006, 2010) and the TOPCAT analysis program (Taylor 2005).","extern":"1","date_created":"2022-07-14T08:51:37Z","article_processing_charge":"No","publication_status":"published","intvolume":" 458","title":"The CALYMHA survey: Lyα escape fraction and its dependence on galaxy properties at z = 2.23","scopus_import":"1","_id":"11578","issue":"1","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J"},{"last_name":"Sobral","first_name":"David","full_name":"Sobral, David"},{"full_name":"Oteo, Iván","last_name":"Oteo","first_name":"Iván"},{"first_name":"Philip","last_name":"Best","full_name":"Best, Philip"},{"last_name":"Smail","first_name":"Ian","full_name":"Smail, Ian"},{"last_name":"Röttgering","first_name":"Huub","full_name":"Röttgering, Huub"},{"full_name":"Paulino-Afonso, Ana","last_name":"Paulino-Afonso","first_name":"Ana"}],"publisher":"Oxford University Press","article_type":"original","quality_controlled":"1","page":"449-467","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"oa":1,"type":"journal_article","date_published":"2016-05-01T00:00:00Z","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1602.02756"}],"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa_version":"Preprint","month":"05","publication":"Monthly Notices of the Royal Astronomical Society","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","galaxies: ISM"],"language":[{"iso":"eng"}]},{"external_id":{"arxiv":["1504.01734"]},"date_updated":"2022-08-18T10:30:13Z","citation":{"mla":"Sobral, David, et al. “Evidence for PopIII-like Stellar Populations in the Most Luminous Lyα Emitters at the Epoch of Reionisation: Spectroscopic Confirmation.” The Astrophysical Journal, vol. 808, no. 2, IOP Publishing, 2015, p. 139, doi:10.1088/0004-637X/808/2/139.","short":"D. Sobral, J.J. Matthee, B. Darvish, D. Schaerer, B. Mobasher, H. Röttgering, S. Santos, S. Hemmati, The Astrophysical Journal 808 (2015) 139.","ista":"Sobral D, Matthee JJ, Darvish B, Schaerer D, Mobasher B, Röttgering H, Santos S, Hemmati S. 2015. Evidence for PopIII-like stellar populations in the most luminous Lyα emitters at the epoch of reionisation: Spectroscopic confirmation. The Astrophysical Journal. 808(2), 139.","apa":"Sobral, D., Matthee, J. J., Darvish, B., Schaerer, D., Mobasher, B., Röttgering, H., … Hemmati, S. (2015). Evidence for PopIII-like stellar populations in the most luminous Lyα emitters at the epoch of reionisation: Spectroscopic confirmation. The Astrophysical Journal. IOP Publishing. https://doi.org/10.1088/0004-637X/808/2/139","ama":"Sobral D, Matthee JJ, Darvish B, et al. Evidence for PopIII-like stellar populations in the most luminous Lyα emitters at the epoch of reionisation: Spectroscopic confirmation. The Astrophysical Journal. 2015;808(2):139. doi:10.1088/0004-637X/808/2/139","ieee":"D. Sobral et al., “Evidence for PopIII-like stellar populations in the most luminous Lyα emitters at the epoch of reionisation: Spectroscopic confirmation,” The Astrophysical Journal, vol. 808, no. 2. IOP Publishing, p. 139, 2015.","chicago":"Sobral, David, Jorryt J Matthee, Behnam Darvish, Daniel Schaerer, Bahram Mobasher, Huub Röttgering, Sérgio Santos, and Shoubaneh Hemmati. “Evidence for PopIII-like Stellar Populations in the Most Luminous Lyα Emitters at the Epoch of Reionisation: Spectroscopic Confirmation.” The Astrophysical Journal. IOP Publishing, 2015. https://doi.org/10.1088/0004-637X/808/2/139."},"year":"2015","abstract":[{"text":"Faint Lyα emitters become increasingly rarer toward the reionization epoch (z ∼ 6–7). However, observations from a very large (∼5 deg2) Lyα narrow-band survey at z = 6.6 show that this is not the case for the most luminous emitters, capable of ionizing their own local bubbles. Here we present follow-up observations of the two most luminous Lyα candidates in the COSMOS field: “MASOSA” and “CR7.” We used X-SHOOTER, SINFONI, and FORS2 on the Very Large Telescope, and DEIMOS on Keck, to confirm both candidates beyond any doubt. We find redshifts of z = 6.541 and z = 6.604 for “MASOSA” and “CR7,” respectively. MASOSA has a strong detection in Lyα with a line width of 386 ± 30 km s−1 (FWHM) and with very high EW0 (>200 Å), but undetected in the continuum, implying very low stellar mass and a likely young, metal-poor stellar population. “CR7,” with an observed Lyα luminosity of 1043.92±0.05 erg s−1 is the most luminous Lyα emitter ever found at z > 6 and is spatially extended (∼16 kpc). “CR7” reveals a narrow Lyα line with 266 ± 15 km s−1 FWHM, being detected in the near-infrared (NIR) (rest-frame UV; β = −2.3 ± 0.1) and in IRAC/Spitzer. We detect a narrow He II 1640 Å emission line (6σ, FWHM = 130 ± 30 km s−1 ) in CR7 which can explain the clear excess seen in the J-band photometry (EW0 ∼ 80 Å). We find no other emission lines from the UV to the NIR in our X-SHOOTER spectra (He II/O III] 1663 Å > 3 and He II/C III] 1908 Å > 2.5). We conclude that CR7 is best explained by a combination of a PopIII-like population, which dominates the rest-frame UV and the nebular emission, and a more normal stellar population, which presumably dominates the mass. Hubble Space Telescope/WFC3 observations show that the light is indeed spatially separated between a very blue component, coincident with Lyα and He II emission, and two red components (∼5 kpc away), which dominate the mass. Our findings are consistent with theoretical predictions of a PopIII wave, with PopIII star formation migrating away from the original sites of star formation.","lang":"eng"}],"arxiv":1,"doi":"10.1088/0004-637X/808/2/139","day":"28","extern":"1","acknowledgement":"We thank the anonymous reviewer for useful and constructive comments and suggestions which greatly improved the quality and clarity of our work. D.S. acknowledges financial support from the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship, from FCT through a FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010), from FCT grant UID/FIS/04434/2013, and from LSF and LKBF. J.M. acknowledges the award of a Huygens PhD fellowship. H.R. acknowledges support from the ERC Advanced Investigator program NewClusters 321271. The authors thank Mark Dijkstra, Bhaskar Agarwal, Jarrett Johnson, Andrea Ferrara, Jarle Brinchmann, Rebecca Bowler, George Becker, Emma Curtis-Lake, Milos Milosavljevic, Raffaella Schneider, Paul Shapiro, and Erik Zackrisson for interesting, stimulating and helpful discussions. The authors are extremely grateful to ESO for the award of ESO DDT time (294.A-5018 and 294.A-5039) which allowed the spectroscopic confirmation of both sources and the detailed investigation of their nature. Observations are also based on data from W.M. Keck Observatory. The W.M. Keck Observatory is operated as a scientific partnership of Caltech, the University of California and the National Aeronautics and Space Administration. Based on observations obtained with MegaPrime/Megacam, a joint project of CFHT and CEA/IRFU, at the Canada–France–Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de lUnivers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University 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, 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.","volume":808,"author":[{"full_name":"Sobral, David","last_name":"Sobral","first_name":"David"},{"orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Darvish","first_name":"Behnam","full_name":"Darvish, Behnam"},{"full_name":"Schaerer, Daniel","first_name":"Daniel","last_name":"Schaerer"},{"last_name":"Mobasher","first_name":"Bahram","full_name":"Mobasher, Bahram"},{"full_name":"Röttgering, Huub","last_name":"Röttgering","first_name":"Huub"},{"full_name":"Santos, Sérgio","first_name":"Sérgio","last_name":"Santos"},{"last_name":"Hemmati","first_name":"Shoubaneh","full_name":"Hemmati, Shoubaneh"}],"issue":"2","_id":"11519","scopus_import":"1","title":"Evidence for PopIII-like stellar populations in the most luminous Lyα emitters at the epoch of reionisation: Spectroscopic confirmation","intvolume":" 808","publication_status":"published","article_processing_charge":"No","date_created":"2022-07-07T09:00:58Z","page":"139","quality_controlled":"1","article_type":"original","publisher":"IOP Publishing","date_published":"2015-07-28T00:00:00Z","type":"journal_article","oa":1,"publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"url":"https://arxiv.org/abs/1504.01734","open_access":"1"}],"publication":"The Astrophysical Journal","month":"07","oa_version":"Preprint","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","dark ages","reionization","first stars – early universe – galaxies: evolution"]},{"day":"11","doi":"10.1093/mnras/stv1076","arxiv":1,"abstract":[{"text":"We present results from the largest contiguous narrow-band survey in the near-infrared. We have used the wide-field infrared camera/Canada–France–Hawaii Telescope and the lowOH2 filter (1.187 ± 0.005 μm) to survey ≈10 deg2 of contiguous extragalactic sky in the SA22 field. A total of ∼6000 candidate emission-line galaxies are found. We use deep ugrizJK data to obtain robust photometric redshifts. We combine our data with the High-redshift(Z) Emission Line Survey (HiZELS), explore spectroscopic surveys (VVDS, VIPERS) and obtain our own spectroscopic follow-up with KMOS, FMOS and MOSFIRE to derive large samples of high-redshift emission-line selected galaxies: 3471 Hα emitters at z = 0.8, 1343 [O III] + Hβ emitters at z = 1.4 and 572 [O II] emitters at z = 2.2. We probe comoving volumes of >106 Mpc3 and find significant overdensities, including an 8.5σ (spectroscopically confirmed) overdensity of Hα emitters at z = 0.81. We derive Hα, [O III] + Hβ and [O II] luminosity functions at z = 0.8, 1.4, 2.2, respectively, and present implications for future surveys such as Euclid. Our uniquely large volumes/areas allow us to subdivide the samples in thousands of randomized combinations of areas and provide a robust empirical measurement of sample/cosmic variance. We show that surveys for star-forming/emission-line galaxies at a depth similar to ours can only overcome cosmic-variance (errors <10 per cent) if they are based on volumes >5 × 105 Mpc3; errors on L* and ϕ* due to sample (cosmic) variance on surveys probing ∼104 and ∼105 Mpc3 are typically very high: ∼300 and ∼40–60 per cent, respectively.","lang":"eng"}],"year":"2015","citation":{"ieee":"D. Sobral et al., “CF-HiZELS, an ∼10 deg2 emission-line survey with spectroscopic follow-up: Hα, [O III] + Hβ and [O II] luminosity functions at z = 0.8, 1.4 and 2.2 ,” Monthly Notices of the Royal Astronomical Society, vol. 451, no. 3. Oxford University Press, pp. 2303–2323, 2015.","chicago":"Sobral, D., Jorryt J Matthee, P. N. Best, I. Smail, A. A. Khostovan, B. Milvang-Jensen, J.-W. Kim, et al. “CF-HiZELS, an ∼10 Deg2 Emission-Line Survey with Spectroscopic Follow-up: Hα, [O III] + Hβ and [O II] Luminosity Functions at z = 0.8, 1.4 and 2.2 .” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2015. https://doi.org/10.1093/mnras/stv1076.","ama":"Sobral D, Matthee JJ, Best PN, et al. CF-HiZELS, an ∼10 deg2 emission-line survey with spectroscopic follow-up: Hα, [O III] + Hβ and [O II] luminosity functions at z = 0.8, 1.4 and 2.2 . Monthly Notices of the Royal Astronomical Society. 2015;451(3):2303-2323. doi:10.1093/mnras/stv1076","apa":"Sobral, D., Matthee, J. J., Best, P. N., Smail, I., Khostovan, A. A., Milvang-Jensen, B., … Mobasher, B. (2015). CF-HiZELS, an ∼10 deg2 emission-line survey with spectroscopic follow-up: Hα, [O III] + Hβ and [O II] luminosity functions at z = 0.8, 1.4 and 2.2 . Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stv1076","ista":"Sobral D, Matthee JJ, Best PN, Smail I, Khostovan AA, Milvang-Jensen B, Kim J-W, Stott J, Calhau J, Nayyeri H, Mobasher B. 2015. CF-HiZELS, an ∼10 deg2 emission-line survey with spectroscopic follow-up: Hα, [O III] + Hβ and [O II] luminosity functions at z = 0.8, 1.4 and 2.2 . Monthly Notices of the Royal Astronomical Society. 451(3), 2303–2323.","mla":"Sobral, D., et al. “CF-HiZELS, an ∼10 Deg2 Emission-Line Survey with Spectroscopic Follow-up: Hα, [O III] + Hβ and [O II] Luminosity Functions at z = 0.8, 1.4 and 2.2 .” Monthly Notices of the Royal Astronomical Society, vol. 451, no. 3, Oxford University Press, 2015, pp. 2303–23, doi:10.1093/mnras/stv1076.","short":"D. Sobral, J.J. Matthee, P.N. Best, I. Smail, A.A. Khostovan, B. Milvang-Jensen, J.-W. Kim, J. Stott, J. Calhau, H. Nayyeri, B. Mobasher, Monthly Notices of the Royal Astronomical Society 451 (2015) 2303–2323."},"date_updated":"2022-08-19T08:23:18Z","external_id":{"arxiv":["1502.06602"]},"volume":451,"acknowledgement":"The authors wish to thank the anonymous reviewer for many helpful comments and suggestions which greatly improved the clarity and quality of this work. DS acknowledges financial support from the Netherlands Organization for Scientific research (NWO) through a Veni fellowship, from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010), from FCT grant PEst-OE/FIS/UI2751/2014, and from LSF and LKBF. JM acknowledges the award of a Huygens PhD fellowship. PNB is grateful for support from STFC. IRS acknowledges support from STFC, a Leverhulme Fellowship, the ERC Advanced Investigator programme DUSTYGAL and a Royal Society/Wolfson Merit Award. BMJ acknowledges support from the ERC-StG grant EGGS-278202. The Dark Cosmology Centre is funded by the DNRF. The Dark Cosmology Centre is funded by the DNRF. JWK acknowledges support from the National Research Foundation of Korea (NRF) grant, no. 2008-0060544, funded by the Korea government (MSIP). JPS acknowledges support from STFC (ST/I001573/1). JC acknowledges support from the FCT-IF grant IF/01154/2012/CP0189/CT0010. The work was only possible due to OPTICON/FP7 and the invaluable access that it granted to the CFHT telescope. We would also like to acknowledge the excellent work done by CFHT staff in conducting the observations in service mode, and on delivering truly excellent data. We are also tremendously thankful to Kentaro Aoki for the incredible support while observing at Subaru with FMOS, and also to the Keck staff for the help with the observations with MOSFIRE. This work is based on observations obtained with WIRCam on the CFHT, OPTICON programme 2011B/029, 2012A019 and 2012B/016. Based on observations made with ESO telescopes at the La Silla Paranal Observatory under programmes IDs 60.A-9460 (data can be accessed through the ESO data archive), 087.A 0337 and 089.A-0965. Based on observations done with FMOS on Subaru under programme S14A-084, and on MOSFIRE/Keck observations under programme U066M. Part of the data on which this analysis is based are available from Sobral et al. (2013a). Dedicated to the memory of C. M. Sobral (1953-2014).","extern":"1","date_created":"2022-07-14T09:02:22Z","article_processing_charge":"No","publication_status":"published","intvolume":" 451","title":"CF-HiZELS, an ∼10 deg2 emission-line survey with spectroscopic follow-up: Hα, [O III] + Hβ and [O II] luminosity functions at z = 0.8, 1.4 and 2.2 ","scopus_import":"1","_id":"11580","issue":"3","author":[{"last_name":"Sobral","first_name":"D.","full_name":"Sobral, D."},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","last_name":"Matthee"},{"full_name":"Best, P. N.","last_name":"Best","first_name":"P. N."},{"full_name":"Smail, I.","last_name":"Smail","first_name":"I."},{"last_name":"Khostovan","first_name":"A. A.","full_name":"Khostovan, A. A."},{"full_name":"Milvang-Jensen, B.","first_name":"B.","last_name":"Milvang-Jensen"},{"first_name":"J.-W.","last_name":"Kim","full_name":"Kim, J.-W."},{"last_name":"Stott","first_name":"J.","full_name":"Stott, J."},{"full_name":"Calhau, J.","first_name":"J.","last_name":"Calhau"},{"first_name":"H.","last_name":"Nayyeri","full_name":"Nayyeri, H."},{"full_name":"Mobasher, B.","first_name":"B.","last_name":"Mobasher"}],"publisher":"Oxford University Press","article_type":"original","quality_controlled":"1","page":"2303-2323","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"oa":1,"type":"journal_article","date_published":"2015-08-11T00:00:00Z","main_file_link":[{"url":"https://arxiv.org/abs/1502.06602","open_access":"1"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","oa_version":"Preprint","month":"08","publication":"Monthly Notices of the Royal Astronomical Society","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: formation","galaxies: luminosity function","mass function","cosmology: observations","early Universe","large-scale structure of Universe"],"language":[{"iso":"eng"}]},{"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1407.1047"}],"date_published":"2014-09-21T00:00:00Z","type":"journal_article","oa":1,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: abundances","galaxies: evolution","galaxies: kinematics and dynamics"],"publication":"Monthly Notices of the Royal Astronomical Society","month":"09","oa_version":"Preprint","extern":"1","volume":443,"acknowledgement":"First, we acknowledge the referee for their comments, which have improved the clarity of this paper. JPS and IRS acknowledge support from STFC (ST/I001573/1). IRS also acknowledges support from the ERC Advanced Investigator programme DUSTYGAL and a Royal Society/Wolfson Merit Award. DS acknowledges financial support from NWO through a Veni fellowship and from FCT through the award of an FCT-IF starting grant. PNB acknowledges STFC for financial support.","external_id":{"arxiv":["1407.1047"]},"date_updated":"2022-08-19T08:27:25Z","citation":{"chicago":"Stott, John P., David Sobral, A. M. Swinbank, Ian Smail, Richard Bower, Philip N. Best, Ray M. Sharples, James E. Geach, and Jorryt J Matthee. “A Relationship between Specific Star Formation Rate and Metallicity Gradient within z ∼ 1 Galaxies from KMOS-HiZELS.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2014. https://doi.org/10.1093/mnras/stu1343.","ieee":"J. P. Stott et al., “A relationship between specific star formation rate and metallicity gradient within z ∼ 1 galaxies from KMOS-HiZELS,” Monthly Notices of the Royal Astronomical Society, vol. 443, no. 3. Oxford University Press, pp. 2695–2704, 2014.","ama":"Stott JP, Sobral D, Swinbank AM, et al. A relationship between specific star formation rate and metallicity gradient within z ∼ 1 galaxies from KMOS-HiZELS. Monthly Notices of the Royal Astronomical Society. 2014;443(3):2695-2704. doi:10.1093/mnras/stu1343","apa":"Stott, J. P., Sobral, D., Swinbank, A. M., Smail, I., Bower, R., Best, P. N., … Matthee, J. J. (2014). A relationship between specific star formation rate and metallicity gradient within z ∼ 1 galaxies from KMOS-HiZELS. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stu1343","ista":"Stott JP, Sobral D, Swinbank AM, Smail I, Bower R, Best PN, Sharples RM, Geach JE, Matthee JJ. 2014. A relationship between specific star formation rate and metallicity gradient within z ∼ 1 galaxies from KMOS-HiZELS. Monthly Notices of the Royal Astronomical Society. 443(3), 2695–2704.","mla":"Stott, John P., et al. “A Relationship between Specific Star Formation Rate and Metallicity Gradient within z ∼ 1 Galaxies from KMOS-HiZELS.” Monthly Notices of the Royal Astronomical Society, vol. 443, no. 3, Oxford University Press, 2014, pp. 2695–704, doi:10.1093/mnras/stu1343.","short":"J.P. Stott, D. Sobral, A.M. Swinbank, I. Smail, R. Bower, P.N. Best, R.M. Sharples, J.E. Geach, J.J. Matthee, Monthly Notices of the Royal Astronomical Society 443 (2014) 2695–2704."},"year":"2014","abstract":[{"text":"We have observed a sample of typical z ∼ 1 star-forming galaxies, selected from the HiZELS survey, with the new K-band Multi-Object Spectrograph (KMOS) near-infrared, multi-integral field unit instrument on the Very Large Telescope (VLT), in order to obtain their dynamics and metallicity gradients. The majority of our galaxies have a metallicity gradient consistent with being flat or negative (i.e. higher metallicity cores than outskirts). Intriguingly, we find a trend between metallicity gradient and specific star formation rate (sSFR), such that galaxies with a high sSFR tend to have relatively metal poor centres, a result which is strengthened when combined with data sets from the literature. This result appears to explain the discrepancies reported between different high-redshift studies and varying claims for evolution. From a galaxy evolution perspective, the trend we see would mean that a galaxy's sSFR is governed by the amount of metal-poor gas that can be funnelled into its core, triggered either by merging or through efficient accretion. In fact, merging may play a significant role as it is the starburst galaxies at all epochs, which have the more positive metallicity gradients. Our results may help to explain the origin of the fundamental metallicity relation, in which galaxies at a fixed mass are observed to have lower metallicities at higher star formation rates, especially if the metallicity is measured in an aperture encompassing only the central regions of the galaxy. Finally, we note that this study demonstrates the power of KMOS as an efficient instrument for large-scale resolved galaxy surveys.","lang":"eng"}],"doi":"10.1093/mnras/stu1343","arxiv":1,"day":"21","page":"2695-2704","quality_controlled":"1","article_type":"original","publisher":"Oxford University Press","author":[{"last_name":"Stott","first_name":"John P.","full_name":"Stott, John P."},{"last_name":"Sobral","first_name":"David","full_name":"Sobral, David"},{"last_name":"Swinbank","first_name":"A. M.","full_name":"Swinbank, A. M."},{"last_name":"Smail","first_name":"Ian","full_name":"Smail, Ian"},{"full_name":"Bower, Richard","first_name":"Richard","last_name":"Bower"},{"first_name":"Philip N.","last_name":"Best","full_name":"Best, Philip N."},{"first_name":"Ray M.","last_name":"Sharples","full_name":"Sharples, Ray M."},{"full_name":"Geach, James E.","first_name":"James E.","last_name":"Geach"},{"full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"}],"issue":"3","_id":"11582","scopus_import":"1","title":"A relationship between specific star formation rate and metallicity gradient within z ∼ 1 galaxies from KMOS-HiZELS","intvolume":" 443","publication_status":"published","date_created":"2022-07-14T12:16:10Z","article_processing_charge":"No"},{"publication":"Monthly Notices of the Royal Astronomical Society","oa_version":"Preprint","month":"05","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","cosmology: observations","dark ages","reionization","first stars"],"language":[{"iso":"eng"}],"type":"journal_article","date_published":"2014-05-21T00:00:00Z","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"oa":1,"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1402.6697"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","scopus_import":"1","_id":"11583","issue":"3","author":[{"orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"first_name":"David","last_name":"Sobral","full_name":"Sobral, David"},{"full_name":"Swinbank, A. M.","first_name":"A. M.","last_name":"Swinbank"},{"first_name":"Ian","last_name":"Smail","full_name":"Smail, Ian"},{"full_name":"Best, P. N.","first_name":"P. N.","last_name":"Best"},{"full_name":"Kim, Jae-Woo","last_name":"Kim","first_name":"Jae-Woo"},{"first_name":"Marijn","last_name":"Franx","full_name":"Franx, Marijn"},{"last_name":"Milvang-Jensen","first_name":"Bo","full_name":"Milvang-Jensen, Bo"},{"full_name":"Fynbo, Johan","first_name":"Johan","last_name":"Fynbo"}],"article_processing_charge":"No","date_created":"2022-07-14T12:33:24Z","publication_status":"published","intvolume":" 440","title":"A 10 deg2 Lyman α survey at z=8.8 with spectroscopic follow-up: Strong constraints on the luminosity function and implications for other surveys","quality_controlled":"1","page":"2375-2387","publisher":"Oxford University Press","article_type":"original","citation":{"ieee":"J. J. Matthee et al., “A 10 deg2 Lyman α survey at z=8.8 with spectroscopic follow-up: Strong constraints on the luminosity function and implications for other surveys,” Monthly Notices of the Royal Astronomical Society, vol. 440, no. 3. Oxford University Press, pp. 2375–2387, 2014.","chicago":"Matthee, Jorryt J, David Sobral, A. M. Swinbank, Ian Smail, P. N. Best, Jae-Woo Kim, Marijn Franx, Bo Milvang-Jensen, and Johan Fynbo. “A 10 Deg2 Lyman α Survey at Z=8.8 with Spectroscopic Follow-up: Strong Constraints on the Luminosity Function and Implications for Other Surveys.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2014. https://doi.org/10.1093/mnras/stu392.","ama":"Matthee JJ, Sobral D, Swinbank AM, et al. A 10 deg2 Lyman α survey at z=8.8 with spectroscopic follow-up: Strong constraints on the luminosity function and implications for other surveys. Monthly Notices of the Royal Astronomical Society. 2014;440(3):2375-2387. doi:10.1093/mnras/stu392","apa":"Matthee, J. J., Sobral, D., Swinbank, A. M., Smail, I., Best, P. N., Kim, J.-W., … Fynbo, J. (2014). A 10 deg2 Lyman α survey at z=8.8 with spectroscopic follow-up: Strong constraints on the luminosity function and implications for other surveys. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stu392","ista":"Matthee JJ, Sobral D, Swinbank AM, Smail I, Best PN, Kim J-W, Franx M, Milvang-Jensen B, Fynbo J. 2014. A 10 deg2 Lyman α survey at z=8.8 with spectroscopic follow-up: Strong constraints on the luminosity function and implications for other surveys. Monthly Notices of the Royal Astronomical Society. 440(3), 2375–2387.","short":"J.J. Matthee, D. Sobral, A.M. Swinbank, I. Smail, P.N. Best, J.-W. Kim, M. Franx, B. Milvang-Jensen, J. Fynbo, Monthly Notices of the Royal Astronomical Society 440 (2014) 2375–2387.","mla":"Matthee, Jorryt J., et al. “A 10 Deg2 Lyman α Survey at Z=8.8 with Spectroscopic Follow-up: Strong Constraints on the Luminosity Function and Implications for Other Surveys.” Monthly Notices of the Royal Astronomical Society, vol. 440, no. 3, Oxford University Press, 2014, pp. 2375–87, doi:10.1093/mnras/stu392."},"year":"2014","date_updated":"2022-08-19T08:30:30Z","external_id":{"arxiv":["1402.6697"]},"day":"21","arxiv":1,"doi":"10.1093/mnras/stu392","abstract":[{"text":"Candidate galaxies at redshifts of z ∼ 10 are now being found in extremely deep surveys, probing very small areas. As a consequence, candidates are very faint, making spectroscopic confirmation practically impossible. In order to overcome such limitations, we have undertaken the CF-HiZELS survey, which is a large-area, medium-depth near-infrared narrow-band survey targeted at z = 8.8 Lyman α (Lyα) emitters (LAEs) and covering 10 deg2 in part of the SSA22 field with the Canada–France–Hawaii Telescope (CFHT). We surveyed a comoving volume of 4.7 × 106 Mpc3 to a Lyα luminosity limit of 6.3 × 1043舁erg舁s−1. We look for Lyα candidates by applying the following criteria: (i) clear emission-line source, (ii) no optical detections (ugriz from CFHTLS), (iii) no visible detection in the optical stack (ugriz > 27), (iv) visually checked reliable NBJ and J detections and (v) J − K ≤ 0. We compute photometric redshifts and remove a significant amount of dusty lower redshift line-emitters at z ∼ 1.4 or 2.2. A total of 13 Lyα candidates were found, of which two are marked as strong candidates, but the majority have very weak constraints on their spectral energy distributions. Using follow-up observations with SINFONI/VLT, we are able to exclude the most robust candidates as LAEs. We put a strong constraint on the Lyα luminosity function at z ∼ 9 and make realistic predictions for ongoing and future surveys. Our results show that surveys for the highest redshift LAEs are susceptible of multiple contaminations and that spectroscopic follow-up is absolutely necessary.","lang":"eng"}],"volume":440,"acknowledgement":"We thank the anonymous referee for the comments and suggestions which improved both the quality and clarity of this work. DS acknowledges financial support from the Netherlands Organisation for Scientific Research (NWO) through a Veni fellowship. IRS acknowledges support from STFC (ST/I001573/1), a Leverhulme Fellowship, the ERC Advanced Investigator programme DUSTYGAL 321334 and a Royal Society/Wolfson Merit Award. PNB acknowledges support from the Leverhulme Trust. JWK acknowledges the support from the Creative Research Initiative Program, no. 2008- 0060544, of the National Research Foundation of Korea (NRF) funded by the Korean government (MSIP). JPUF and BMJ acknowledge support from the ERC-StG grant EGGS-278202. The Dark Cosmology Centre is funded by the Danish National Research Foundation. This work is based in part on data obtained as part of the UKIRT Infrared Deep Sky Survey. Based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/IRFU, at the Canada–France–Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l’Univers of the Centre National de la Recherche Scientifique (CNRS) of France and the University 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. This work was only possible due to OPTICON/FP7 and the access that it granted to the CFHT telescope. The authors also wish to acknowledge the CFHTLS and UKIDSS surveys for their excellent legacy and complementary value – without such high-quality data sets, this research would not have been possible.","extern":"1"},{"date_published":"2013-12-03T00:00:00Z","type":"journal_article","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"oa":1,"main_file_link":[{"url":"https://arxiv.org/abs/1310.3822","open_access":"1"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","publication":"The Astrophysical Journal","oa_version":"Preprint","month":"12","article_number":"139","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution – galaxies","high-redshift – galaxies","starburst"],"date_updated":"2022-08-18T10:43:07Z","citation":{"ista":"Sobral D, Swinbank AM, Stott JP, Matthee JJ, Bower RG, Smail I, Best P, Geach JE, Sharples RM. 2013. The dynamics of z=0.8 H-alpha-selected star-forming galaxies from KMOS/CF-HiZELS. The Astrophysical Journal. 779(2), 139.","short":"D. Sobral, A.M. Swinbank, J.P. Stott, J.J. Matthee, R.G. Bower, I. Smail, P. Best, J.E. Geach, R.M. Sharples, The Astrophysical Journal 779 (2013).","mla":"Sobral, D., et al. “The Dynamics of Z=0.8 H-Alpha-Selected Star-Forming Galaxies from KMOS/CF-HiZELS.” The Astrophysical Journal, vol. 779, no. 2, 139, IOP Publishing, 2013, doi:10.1088/0004-637x/779/2/139.","chicago":"Sobral, D., A. M. Swinbank, J. P. Stott, Jorryt J Matthee, R. G. Bower, Ian Smail, P. Best, J. E. Geach, and R. M. Sharples. “The Dynamics of Z=0.8 H-Alpha-Selected Star-Forming Galaxies from KMOS/CF-HiZELS.” The Astrophysical Journal. IOP Publishing, 2013. https://doi.org/10.1088/0004-637x/779/2/139.","ieee":"D. Sobral et al., “The dynamics of z=0.8 H-alpha-selected star-forming galaxies from KMOS/CF-HiZELS,” The Astrophysical Journal, vol. 779, no. 2. IOP Publishing, 2013.","apa":"Sobral, D., Swinbank, A. M., Stott, J. P., Matthee, J. J., Bower, R. G., Smail, I., … Sharples, R. M. (2013). The dynamics of z=0.8 H-alpha-selected star-forming galaxies from KMOS/CF-HiZELS. The Astrophysical Journal. IOP Publishing. https://doi.org/10.1088/0004-637x/779/2/139","ama":"Sobral D, Swinbank AM, Stott JP, et al. The dynamics of z=0.8 H-alpha-selected star-forming galaxies from KMOS/CF-HiZELS. The Astrophysical Journal. 2013;779(2). doi:10.1088/0004-637x/779/2/139"},"year":"2013","external_id":{"arxiv":["1310.3822"]},"arxiv":1,"doi":"10.1088/0004-637x/779/2/139","day":"03","abstract":[{"text":"We present the spatially resolved Hα dynamics of 16 star-forming galaxies at z ∼ 0.81 using the new KMOS multi-object integral field spectrograph on the ESO Very Large Telescope. These galaxies, selected using 1.18 μm narrowband imaging from the 10 deg2 CFHT-HiZELS survey of the SA 22 hr field, are found in a ∼4 Mpc overdensity of Hα emitters and likely reside in a group/intermediate environment, but not a cluster. We confirm and identify a rich group of star-forming galaxies at z = 0.813 ± 0.003, with 13 galaxies within 1000 km s−1 of each other, and seven within a diameter of 3 Mpc. All of our galaxies are “typical” star-forming galaxies at their redshift, 0.8 ± 0.4 SFR$^*_{z = 0.8}$, spanning a range of specific star formation rates (sSFRs) of 0.2–1.1 Gyr−1 and have a median metallicity very close to solar of 12 + log(O/H) = 8.62 ± 0.06. We measure the spatially resolved Hα dynamics of the galaxies in our sample and show that 13 out of 16 galaxies can be described by rotating disks and use the data to derive inclination corrected rotation speeds of 50–275 km s−1. The fraction of disks within our sample is 75% ± 8%, consistent with previous results based on Hubble Space Telescope morphologies of Hα-selected galaxies at z ∼ 1 and confirming that disks dominate the SFR density at z ∼ 1. Our Hα galaxies are well fitted by the z ∼ 1–2 Tully–Fisher (TF) relation, confirming the evolution seen in the zero point. Apart from having, on average, higher stellar masses and lower sSFRs, our group galaxies at z = 0.81 present the same mass–metallicity and TF relation as z ∼ 1 field galaxies and are all disk galaxies.","lang":"eng"}],"volume":779,"acknowledgement":"We thank the referee for many helpful comments and suggestions which greatly improved the clarity and quality of this work. D.S. acknowledges financial support from the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship and also funding from the European Community Seventh Framework Programme (FP7/2007-2013) under grant agreement number RG226604 (OPTICON) which allowed access to CFHT time (proposals: 11BO29 & 12AO19). A.M.S. gratefully acknowledges an STFC Advanced Fellowship through grant number ST/H005234/1. I.R.S., J.P.S., and R.G.B. acknowledge support from the UK Science and Technology Facilities Council (STFC) under ST/I001573/1. I.R.S. acknowledges STFC (ST/J001422/1), the ERC Advanced Investigator program DUSTYGAL and a Royal Society/Wolfson Merit Award. P.N.B. acknowledges support from STFC. R.M.S. acknowledges support from the grant ST/1001573/1. The data presented here are based on observations with the KMOS spectrograph on the ESO/VLT under program 60.A-9460 and can be accessed through the ESO data archive. The authors also wish to acknowledge the help from Michael Hilker in preparing the KMOS observations.","extern":"1","_id":"11520","scopus_import":"1","author":[{"full_name":"Sobral, D.","last_name":"Sobral","first_name":"D."},{"full_name":"Swinbank, A. M.","last_name":"Swinbank","first_name":"A. M."},{"first_name":"J. P.","last_name":"Stott","full_name":"Stott, J. P."},{"last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"full_name":"Bower, R. G.","last_name":"Bower","first_name":"R. G."},{"last_name":"Smail","first_name":"Ian","full_name":"Smail, Ian"},{"full_name":"Best, P.","first_name":"P.","last_name":"Best"},{"full_name":"Geach, J. E.","first_name":"J. E.","last_name":"Geach"},{"last_name":"Sharples","first_name":"R. M.","full_name":"Sharples, R. M."}],"issue":"2","publication_status":"published","date_created":"2022-07-07T09:14:48Z","article_processing_charge":"No","title":"The dynamics of z=0.8 H-alpha-selected star-forming galaxies from KMOS/CF-HiZELS","intvolume":" 779","quality_controlled":"1","publisher":"IOP Publishing","article_type":"original"}]