[{"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"url":"https://arxiv.org/abs/1605.08782","open_access":"1"}],"oa_version":"Preprint","day":"01","month":"03","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"arxiv":1,"author":[{"orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J"},{"full_name":"Sobral, David","first_name":"David","last_name":"Sobral"},{"last_name":"Best","first_name":"Philip","full_name":"Best, Philip"},{"last_name":"Khostovan","first_name":"Ali Ahmad","full_name":"Khostovan, Ali Ahmad"},{"first_name":"Iván","full_name":"Oteo, Iván","last_name":"Oteo"},{"last_name":"Bouwens","first_name":"Rychard","full_name":"Bouwens, Rychard"},{"last_name":"Röttgering","first_name":"Huub","full_name":"Röttgering, Huub"}],"status":"public","type":"journal_article","intvolume":" 465","scopus_import":"1","title":"The production and escape of Lyman-Continuum radiation from star-forming galaxies at z ∼ 2 and their redshift evolution","article_processing_charge":"No","issue":"3","date_updated":"2022-08-19T07:53:04Z","oa":1,"publication":"Monthly Notices of the Royal Astronomical Society","language":[{"iso":"eng"}],"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"}],"external_id":{"arxiv":["1605.08782"]},"publication_status":"published","volume":465,"quality_controlled":"1","extern":"1","page":"3637-3655","date_published":"2017-03-01T00:00:00Z","publisher":"Oxford University Press","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","cosmology: observations","dark ages","reionization","first stars"],"citation":{"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.","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.","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.","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.","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","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"},"date_created":"2022-07-12T12:12:14Z","year":"2017","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).","doi":"10.1093/mnras/stw2973","article_type":"original","_id":"11564"},{"abstract":[{"lang":"eng","text":"While traditionally associated with active galactic nuclei (AGN), the properties of the C II] (λ = 2326 Å), C III] (λ, λ = 1907, 1909 Å) and C IV (λ, λ = 1549, 1551 Å) emission lines are still uncertain as large, unbiased samples of sources are scarce. We present the first blind, statistical study of C II], C III] and C IV emitters at z ∼ 0.68, 1.05, 1.53, respectively, uniformly selected down to a flux limit of ∼4 × 10−17 erg s−1 cm−1 through a narrow-band survey covering an area of ∼1.4 deg2 over COSMOS and UDS. We detect 16 C II], 35 C III] and 17 C IV emitters, whose nature we investigate using optical colours as well as Hubble Space Telescope (HST), X-ray, radio and far-infrared data. We find that z ∼ 0.7 C II] emitters are consistent with a mixture of blue (UV slope β = −2.0 ± 0.4) star-forming (SF) galaxies with discy HST structure and AGN with Seyfert-like morphologies. Bright C II] emitters have individual X-ray detections as well as high average black hole accretion rates (BHARs) of ∼0.1 M⊙ yr−1. C III] emitters at z ∼ 1.05 trace a general population of SF galaxies, with β = −0.8 ± 1.1, a variety of optical morphologies, including isolated and interacting galaxies and low BHAR (<0.02 M⊙ yr−1). Our C IV emitters at z ∼ 1.5 are consistent with young, blue quasars (β ∼ −1.9) with point-like optical morphologies, bright X-ray counterparts and large BHAR (0.8 M⊙ yr−1). We also find some surprising C II], C III] and C IV emitters with rest-frame equivalent widths (EWs) that could be as large as 50–100 Å. AGN or spatial offsets between the UV continuum stellar disc and the line-emitting regions may explain the large EW. These bright C II], C III] and C IV emitters are ideal candidates for spectroscopic follow-up to fully unveil their nature."}],"external_id":{"arxiv":["1703.10169"]},"publication_status":"published","date_published":"2017-11-01T00:00:00Z","publisher":"Oxford University Press","quality_controlled":"1","volume":471,"page":"2558-2574","extern":"1","year":"2017","acknowledgement":"We would like to thank the anonymous referee for her/his valuable input that helped improve the clarity and interpretation of our results. DS acknowledges financial support from the Netherlands Organisation for Scientific research (NWO), through a Veni fellowship. IO acknowledges support from the European Research Council in the form of the Advanced Investigator Programme, 321302, COSMICISM. CALYMHA data are based on observations made with the Isaac Newton Telescope (proposals 13AN002, I14AN002, 088-INT7/14A, I14BN006, 118-INT13/14B, I15AN008) 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 Astrofísica de Canarias. Also based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme IDs 098.A-0819 and 179.A-2005. We are grateful to E. L. Wright and J. Schombert for their cosmology calculator. We would like to thank the authors of NUMPY (van der Walt et al. 2011), SCIPY (Jones et al. 2001), MATPLOTLIB (Hunter 2007) and ASTROPY (Astropy Collaboration et al. 2013) for making these packages publicly available. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is ","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: active","galaxies: high-redshift","quasars: emission lines","galaxies: star formation","cosmology: observations"],"date_created":"2022-07-12T12:33:16Z","citation":{"mla":"Stroe, Andra, et al. “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, Morphologies and Equivalent Widths .” Monthly Notices of the Royal Astronomical Society, vol. 471, no. 3, Oxford University Press, 2017, pp. 2558–74, doi:10.1093/mnras/stx1712.","ista":"Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. 2017. A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent widths . Monthly Notices of the Royal Astronomical Society. 471(3), 2558–2574.","chicago":"Stroe, Andra, David Sobral, Jorryt J Matthee, João Calhau, and Ivan Oteo. “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, Morphologies and Equivalent Widths .” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2017. https://doi.org/10.1093/mnras/stx1712.","short":"A. Stroe, D. Sobral, J.J. Matthee, J. Calhau, I. Oteo, Monthly Notices of the Royal Astronomical Society 471 (2017) 2558–2574.","ieee":"A. Stroe, D. Sobral, J. J. Matthee, J. Calhau, and I. Oteo, “A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent widths ,” Monthly Notices of the Royal Astronomical Society, vol. 471, no. 3. Oxford University Press, pp. 2558–2574, 2017.","ama":"Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent widths . Monthly Notices of the Royal Astronomical Society. 2017;471(3):2558-2574. doi:10.1093/mnras/stx1712","apa":"Stroe, A., Sobral, D., Matthee, J. J., Calhau, J., & Oteo, I. (2017). A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent widths . Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stx1712"},"doi":"10.1093/mnras/stx1712","article_type":"original","_id":"11566","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"month":"11","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","day":"01","oa_version":"Preprint","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1703.10169"}],"arxiv":1,"author":[{"full_name":"Stroe, Andra","first_name":"Andra","last_name":"Stroe"},{"full_name":"Sobral, David","first_name":"David","last_name":"Sobral"},{"last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","first_name":"Jorryt J","full_name":"Matthee, Jorryt J"},{"full_name":"Calhau, João","first_name":"João","last_name":"Calhau"},{"first_name":"Ivan","full_name":"Oteo, Ivan","last_name":"Oteo"}],"status":"public","type":"journal_article","intvolume":" 471","scopus_import":"1","issue":"3","article_processing_charge":"No","oa":1,"date_updated":"2022-08-19T07:59:57Z","title":"A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent widths ","publication":"Monthly Notices of the Royal Astronomical Society","language":[{"iso":"eng"}]},{"month":"11","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa_version":"Preprint","day":"01","main_file_link":[{"url":"https://arxiv.org/abs/1703.10169","open_access":"1"}],"arxiv":1,"author":[{"full_name":"Stroe, Andra","first_name":"Andra","last_name":"Stroe"},{"last_name":"Sobral","first_name":"David","full_name":"Sobral, David"},{"first_name":"Jorryt J","full_name":"Matthee, Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X"},{"full_name":"Calhau, João","first_name":"João","last_name":"Calhau"},{"last_name":"Oteo","first_name":"Ivan","full_name":"Oteo, Ivan"}],"status":"public","type":"journal_article","scopus_import":"1","intvolume":" 471","article_processing_charge":"No","issue":"3","date_updated":"2022-08-19T08:02:04Z","oa":1,"title":"A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average line ratios","publication":"Monthly Notices of the Royal Astronomical Society","language":[{"iso":"eng"}],"abstract":[{"text":"Recently, the C III] and C IV emission lines have been observed in galaxies in the early Universe (z > 5), providing new ways to measure their redshift and study their stellar populations and active galactic nuclei (AGN). We explore the first blind C II], C III] and C IV survey (z ∼ 0.68, 1.05, 1.53, respectively) presented in Stroe et al. (2017). We derive luminosity functions (LF) and study properties of C II], C III] and C IV line emitters through comparisons to the LFs of H α and Ly α emitters, UV selected star-forming (SF) galaxies and quasars at similar redshifts. The C II] LF at z ∼ 0.68 is equally well described by a Schechter or a power-law LF, characteristic of a mixture of SF and AGN activity. The C III] LF (z ∼ 1.05) is consistent to a scaled down version of the Schechter H α and Ly α LF at their redshift, indicating a SF origin. In stark contrast, the C IV LF at z ∼ 1.53 is well fit by a power-law, quasar-like LF. We find that the brightest UV sources (MUV < −22) will universally have C III] and C IV emission. However, on average, C III] and C IV are not as abundant as H α or Ly α emitters at the same redshift, with cosmic average ratios of ∼0.02–0.06 to H α and ∼0.01–0.1 to intrinsic Ly α. We predict that the C III] and C IV lines can only be truly competitive in confirming high-redshift candidates when the hosts are intrinsically bright and the effective Ly α escape fraction is below 1 per cent. While C III] and C IV were proposed as good tracers of young, relatively low-metallicity galaxies typical of the early Universe, we find that, at least at z ∼ 1.5, C IV is exclusively hosted by AGN/quasars, especially at large line equivalent widths.","lang":"eng"}],"external_id":{"arxiv":["1703.10169"]},"publication_status":"published","date_published":"2017-11-01T00:00:00Z","publisher":"Oxford University Press","quality_controlled":"1","volume":471,"page":"2575-2586","extern":"1","year":"2017","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: active","galaxies: high redshift","galaxies: luminosity function","mass function","quasars: emission lines","star formation","cosmology: observations"],"citation":{"ieee":"A. Stroe, D. Sobral, J. J. Matthee, J. Calhau, and I. Oteo, “A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average line ratios,” Monthly Notices of the Royal Astronomical Society, vol. 471, no. 3. Oxford University Press, pp. 2575–2586, 2017.","ama":"Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average line ratios. Monthly Notices of the Royal Astronomical Society. 2017;471(3):2575-2586. doi:10.1093/mnras/stx1713","short":"A. Stroe, D. Sobral, J.J. Matthee, J. Calhau, I. Oteo, Monthly Notices of the Royal Astronomical Society 471 (2017) 2575–2586.","ista":"Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. 2017. A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average line ratios. Monthly Notices of the Royal Astronomical Society. 471(3), 2575–2586.","mla":"Stroe, Andra, et al. “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity Functions and Cosmic Average Line Ratios.” Monthly Notices of the Royal Astronomical Society, vol. 471, no. 3, Oxford University Press, 2017, pp. 2575–86, doi:10.1093/mnras/stx1713.","chicago":"Stroe, Andra, David Sobral, Jorryt J Matthee, João Calhau, and Ivan Oteo. “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity Functions and Cosmic Average Line Ratios.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2017. https://doi.org/10.1093/mnras/stx1713.","apa":"Stroe, A., Sobral, D., Matthee, J. J., Calhau, J., & Oteo, I. (2017). A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average line ratios. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stx1713"},"date_created":"2022-07-12T12:54:57Z","doi":"10.1093/mnras/stx1713","_id":"11567","article_type":"original"},{"intvolume":" 472","scopus_import":"1","title":"Spectroscopic properties of luminous Ly α emitters at z ≈ 6–7 and comparison to the Lyman-break population","oa":1,"date_updated":"2022-08-19T08:05:37Z","issue":"1","article_processing_charge":"No","publication":"Monthly Notices of the Royal Astronomical Society","language":[{"iso":"eng"}],"oa_version":"Preprint","day":"01","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1706.06591"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","month":"11","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"author":[{"first_name":"Jorryt J","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X"},{"first_name":"David","full_name":"Sobral, David","last_name":"Sobral"},{"last_name":"Darvish","full_name":"Darvish, Behnam","first_name":"Behnam"},{"last_name":"Santos","first_name":"Sérgio","full_name":"Santos, Sérgio"},{"full_name":"Mobasher, Bahram","first_name":"Bahram","last_name":"Mobasher"},{"full_name":"Paulino-Afonso, Ana","first_name":"Ana","last_name":"Paulino-Afonso"},{"full_name":"Röttgering, Huub","first_name":"Huub","last_name":"Röttgering"},{"first_name":"Lara","full_name":"Alegre, Lara","last_name":"Alegre"}],"arxiv":1,"status":"public","type":"journal_article","citation":{"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.","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","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.","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.","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"},"date_created":"2022-07-13T09:47:39Z","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution – galaxies: high-redshift","dark ages","reionization","first stars","cosmology: observations"],"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).","year":"2017","doi":"10.1093/mnras/stx2061","article_type":"original","_id":"11572","external_id":{"arxiv":["1706.06591"]},"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."}],"publication_status":"published","page":"772-787","extern":"1","volume":472,"quality_controlled":"1","publisher":"Oxford University Press","date_published":"2017-11-01T00:00:00Z"},{"volume":471,"quality_controlled":"1","extern":"1","page":"1280-1320","date_published":"2017-10-01T00:00:00Z","publisher":"Oxford University Press","publication_status":"published","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"}],"external_id":{"arxiv":["1704.06263"]},"_id":"11573","article_type":"original","doi":"10.1093/mnras/stx1366","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","galaxies: kinematics and dynamics"],"citation":{"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","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.","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.","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.","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","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.","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."},"date_created":"2022-07-13T10:03:01Z","year":"2017","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).","type":"journal_article","status":"public","arxiv":1,"author":[{"last_name":"Turner","first_name":"O. J.","full_name":"Turner, O. J."},{"full_name":"Cirasuolo, M.","first_name":"M.","last_name":"Cirasuolo"},{"full_name":"Harrison, C. M.","first_name":"C. M.","last_name":"Harrison"},{"last_name":"McLure","first_name":"R. J.","full_name":"McLure, R. J."},{"full_name":"Dunlop, J. S.","first_name":"J. S.","last_name":"Dunlop"},{"last_name":"Swinbank","full_name":"Swinbank, A. M.","first_name":"A. M."},{"first_name":"H. L.","full_name":"Johnson, H. L.","last_name":"Johnson"},{"last_name":"Sobral","full_name":"Sobral, D.","first_name":"D."},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X","first_name":"Jorryt J","full_name":"Matthee, Jorryt J"},{"last_name":"Sharples","first_name":"R. M.","full_name":"Sharples, R. M."}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","day":"01","main_file_link":[{"url":"https://arxiv.org/abs/1704.06263","open_access":"1"}],"oa_version":"Preprint","month":"10","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"language":[{"iso":"eng"}],"publication":"Monthly Notices of the Royal Astronomical Society","title":"The KMOS Deep Survey (KDS) – I. Dynamical measurements of typical star-forming galaxies at z ≃ 3.5","article_processing_charge":"No","issue":"2","oa":1,"date_updated":"2022-08-19T08:07:31Z","scopus_import":"1","intvolume":" 471"},{"date_created":"2022-07-13T10:08:20Z","citation":{"apa":"Santos, S., Sobral, D., & Matthee, J. J. (2016). The Lyα luminosity function at z= 5.7–6.6 and the steep drop of the faint end: Implications for reionization. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stw2076","ama":"Santos S, Sobral D, Matthee JJ. The Lyα luminosity function at z= 5.7–6.6 and the steep drop of the faint end: Implications for reionization. Monthly Notices of the Royal Astronomical Society. 2016;463(2):1678-1691. doi:10.1093/mnras/stw2076","ieee":"S. Santos, D. Sobral, and J. J. Matthee, “The Lyα luminosity function at z= 5.7–6.6 and the steep drop of the faint end: Implications for reionization,” Monthly Notices of the Royal Astronomical Society, vol. 463, no. 2. Oxford University Press, pp. 1678–1691, 2016.","short":"S. Santos, D. Sobral, J.J. Matthee, Monthly Notices of the Royal Astronomical Society 463 (2016) 1678–1691.","mla":"Santos, Sérgio, et al. “The Lyα Luminosity Function at Z= 5.7–6.6 and the Steep Drop of the Faint End: Implications for Reionization.” Monthly Notices of the Royal Astronomical Society, vol. 463, no. 2, Oxford University Press, 2016, pp. 1678–91, doi:10.1093/mnras/stw2076.","ista":"Santos S, Sobral D, Matthee JJ. 2016. The Lyα luminosity function at z= 5.7–6.6 and the steep drop of the faint end: Implications for reionization. Monthly Notices of the Royal Astronomical Society. 463(2), 1678–1691.","chicago":"Santos, Sérgio, David Sobral, and Jorryt J Matthee. “The Lyα Luminosity Function at Z= 5.7–6.6 and the Steep Drop of the Faint End: Implications for Reionization.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2016. https://doi.org/10.1093/mnras/stw2076."},"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift","galaxies: luminosity function","mass function","cosmology: observations","dark ages","reionization","first stars"],"acknowledgement":"We thank the anonymous referee for useful and constructive comments and suggestions which greatly improved the quality and clarity of our work. The authors acknowledge financial support from the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship. SS and DS acknowledge funding from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010). SS also acknowledges support from FCT through the research grants UID/FIS/04434/2013 and PTDC/FIS-AST/2194/2012. JM acknowledges a Huygens PhD fellowship from Leiden University. Based on observations with the Subaru Telescope (Program IDs: S05B-027, S06A-025, S06B-010, S07A-013, S07B-008, S08B-008, S09A-017, S14A-086). Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 294.A-5018. 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. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. We are grateful to the CFHTLS, COSMOS-UltraVISTA, UKIDSS, SXDF and COSMOS survey teams. Without these legacy surveys, this research would have been impossible. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct and explore observations from this mountain. Finally, the authors acknowledge the unique value of the publicly available programming language PYTHON, including the NUMPY, PYFITS, MATPLOTLIB, SCIPY and ASTROPY (Astropy Collaboration et al.","year":"2016","_id":"11574","article_type":"original","doi":"10.1093/mnras/stw2076","publication_status":"published","external_id":{"arxiv":["1606.07435"]},"abstract":[{"text":"We present new results from the widest narrow-band survey search for Lyα emitters at z = 5.7, just after reionization. We survey a total of 7 deg2 spread over the COSMOS, UDS and SA22 fields. We find over 11 000 line emitters, out of which 514 are robust Lyα candidates at z = 5.7 within a volume of 6.3 × 106 Mpc3. Our Lyα emitters span a wide range in Lyα luminosities, from faint to bright (LLyα ∼ 1042.5–44 erg s−1) and rest-frame equivalent widths (EW0 ∼ 25–1000 Å) in a single, homogeneous data set. By combining all our fields, we find that the faint end slope of the z = 5.7 Lyα luminosity function is very steep, with α=−2.3+0.4−0.3. We also present an updated z = 6.6 Lyα luminosity function, based on comparable volumes and obtained with the same methods, which we directly compare with that at z = 5.7. We find a significant decline of the number density of faint Lyα emitters from z = 5.7 to 6.6 (by 0.5 ± 0.1 dex), but no evolution at the bright end/no evolution in L*. Faint Lyα emitters at z = 6.6 show much more extended haloes than those at z = 5.7, suggesting that neutral Hydrogen plays an important role, increasing the scattering and leading to observations missing faint Lyα emission within the epoch of reionization. Altogether, our results suggest that we are observing patchy reionization which happens first around the brightest Lyα emitters, allowing the number densities of those sources to remain unaffected by the increase of neutral Hydrogen fraction from z ∼ 5 to 7.","lang":"eng"}],"page":"1678-1691","extern":"1","volume":463,"quality_controlled":"1","publisher":"Oxford University Press","date_published":"2016-12-01T00:00:00Z","title":"The Lyα luminosity function at z= 5.7–6.6 and the steep drop of the faint end: Implications for reionization","oa":1,"date_updated":"2022-08-19T08:09:54Z","article_processing_charge":"No","issue":"2","intvolume":" 463","scopus_import":"1","language":[{"iso":"eng"}],"publication":"Monthly Notices of the Royal Astronomical Society","author":[{"last_name":"Santos","first_name":"Sérgio","full_name":"Santos, Sérgio"},{"first_name":"David","full_name":"Sobral, David","last_name":"Sobral"},{"first_name":"Jorryt J","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee"}],"arxiv":1,"day":"01","main_file_link":[{"url":"https://arxiv.org/abs/1606.07435","open_access":"1"}],"oa_version":"Preprint","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"month":"12","type":"journal_article","status":"public"},{"abstract":[{"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.","lang":"eng"}],"external_id":{"arxiv":["1601.02266"]},"publication_status":"published","quality_controlled":"1","volume":457,"extern":"1","page":"1739-1752","date_published":"2016-04-01T00:00:00Z","publisher":"Oxford University Press","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","cosmology: observations"],"citation":{"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.","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.","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.","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","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.","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"},"date_created":"2022-07-13T12:50:36Z","year":"2016","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.","doi":"10.1093/mnras/stw022","_id":"11576","article_type":"original","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","day":"01","oa_version":"Preprint","main_file_link":[{"url":"https://arxiv.org/abs/1601.02266","open_access":"1"}],"month":"04","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"arxiv":1,"author":[{"full_name":"Sobral, David","first_name":"David","last_name":"Sobral"},{"full_name":"Kohn, Saul A.","first_name":"Saul A.","last_name":"Kohn"},{"first_name":"Philip N.","full_name":"Best, Philip N.","last_name":"Best"},{"last_name":"Smail","first_name":"Ian","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"},{"last_name":"Calhau","first_name":"João","full_name":"Calhau, João"},{"orcid":"0000-0003-2871-127X","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","first_name":"Jorryt J"}],"type":"journal_article","status":"public","scopus_import":"1","intvolume":" 457","title":"The most luminous H α emitters at z ∼ 0.8–2.23 from HiZELS: Evolution of AGN and star-forming galaxies","issue":"2","article_processing_charge":"No","date_updated":"2022-08-19T08:15:21Z","oa":1,"publication":"Monthly Notices of the Royal Astronomical Society","language":[{"iso":"eng"}]},{"publication":"Monthly Notices of the Royal Astronomical Society","language":[{"iso":"eng"}],"scopus_import":"1","intvolume":" 458","article_processing_charge":"No","issue":"1","date_updated":"2022-08-19T08:17:19Z","oa":1,"title":"The CALYMHA survey: Lyα escape fraction and its dependence on galaxy properties at z = 2.23","status":"public","type":"journal_article","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"month":"05","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1602.02756"}],"day":"01","oa_version":"Preprint","arxiv":1,"author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X","first_name":"Jorryt J","full_name":"Matthee, Jorryt J"},{"last_name":"Sobral","full_name":"Sobral, David","first_name":"David"},{"last_name":"Oteo","first_name":"Iván","full_name":"Oteo, Iván"},{"last_name":"Best","full_name":"Best, Philip","first_name":"Philip"},{"last_name":"Smail","full_name":"Smail, Ian","first_name":"Ian"},{"last_name":"Röttgering","full_name":"Röttgering, Huub","first_name":"Huub"},{"last_name":"Paulino-Afonso","first_name":"Ana","full_name":"Paulino-Afonso, Ana"}],"doi":"10.1093/mnras/stw322","_id":"11578","article_type":"original","year":"2016","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).","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","galaxies: ISM"],"citation":{"chicago":"Matthee, Jorryt J, David Sobral, Iván Oteo, Philip Best, Ian Smail, Huub Röttgering, and Ana Paulino-Afonso. “The CALYMHA Survey: Lyα Escape Fraction and Its Dependence on Galaxy Properties at z = 2.23.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2016. https://doi.org/10.1093/mnras/stw322.","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.","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","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.","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.","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"},"date_created":"2022-07-14T08:51:37Z","date_published":"2016-05-01T00:00:00Z","publisher":"Oxford University Press","volume":458,"quality_controlled":"1","page":"449-467","extern":"1","abstract":[{"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.","lang":"eng"}],"external_id":{"arxiv":["1602.02756"]},"publication_status":"published"},{"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","day":"01","oa_version":"Preprint","main_file_link":[{"url":"https://arxiv.org/abs/1506.07173","open_access":"1"}],"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"month":"11","arxiv":1,"author":[{"first_name":"A.","full_name":"Pallottini, A.","last_name":"Pallottini"},{"full_name":"Ferrara, A.","first_name":"A.","last_name":"Ferrara"},{"last_name":"Pacucci","full_name":"Pacucci, F.","first_name":"F."},{"last_name":"Gallerani","first_name":"S.","full_name":"Gallerani, S."},{"last_name":"Salvadori","full_name":"Salvadori, S.","first_name":"S."},{"last_name":"Schneider","full_name":"Schneider, R.","first_name":"R."},{"last_name":"Schaerer","full_name":"Schaerer, D.","first_name":"D."},{"last_name":"Sobral","first_name":"D.","full_name":"Sobral, D."},{"full_name":"Matthee, Jorryt J","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X"}],"status":"public","type":"journal_article","scopus_import":"1","intvolume":" 453","title":"The brightest Lyα emitter: Pop III or black hole?","article_processing_charge":"No","issue":"3","date_updated":"2022-08-19T08:19:23Z","oa":1,"publication":"Monthly Notices of the Royal Astronomical Society","language":[{"iso":"eng"}],"abstract":[{"lang":"eng","text":"CR7 is the brightest z = 6.6 Ly α emitter (LAE) known to date, and spectroscopic follow-up by Sobral et al. suggests that CR7 might host Population (Pop) III stars. We examine this interpretation using cosmological hydrodynamical simulations. Several simulated galaxies show the same ‘Pop III wave’ pattern observed in CR7. However, to reproduce the extreme CR7 Ly α/He II1640 line luminosities (Lα/HeII) a top-heavy initial mass function and a massive ( ≳ 107 M⊙) Pop III burst with age ≲ 2 Myr are required. Assuming that the observed properties of Ly α and He II emission are typical for Pop III, we predict that in the COSMOS/UDS/SA22 fields, 14 out of the 30 LAEs at z = 6.6 with Lα > 1043.3 erg s−1 should also host Pop III stars producing an observable LHeII≳1042.7ergs−1. As an alternate explanation, we explore the possibility that CR7 is instead powered by accretion on to a direct collapse black hole. Our model predicts Lα, LHeII, and X-ray luminosities that are in agreement with the observations. In any case, the observed properties of CR7 indicate that this galaxy is most likely powered by sources formed from pristine gas. We propose that further X-ray observations can distinguish between the two above scenarios."}],"external_id":{"arxiv":["1506.07173"]},"publication_status":"published","quality_controlled":"1","volume":453,"extern":"1","page":"2465-2470","date_published":"2015-11-01T00:00:00Z","publisher":"Oxford University Press","keyword":["Space and Planetary Science","Astronomy and Astrophysics","black hole physics","stars: Population III","galaxies: high-redshift"],"date_created":"2022-07-14T08:58:36Z","citation":{"apa":"Pallottini, A., Ferrara, A., Pacucci, F., Gallerani, S., Salvadori, S., Schneider, R., … Matthee, J. J. (2015). The brightest Lyα emitter: Pop III or black hole? Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stv1795","chicago":"Pallottini, A., A. Ferrara, F. Pacucci, S. Gallerani, S. Salvadori, R. Schneider, D. Schaerer, D. Sobral, and Jorryt J Matthee. “The Brightest Lyα Emitter: Pop III or Black Hole?” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2015. https://doi.org/10.1093/mnras/stv1795.","mla":"Pallottini, A., et al. “The Brightest Lyα Emitter: Pop III or Black Hole?” Monthly Notices of the Royal Astronomical Society, vol. 453, no. 3, Oxford University Press, 2015, pp. 2465–70, doi:10.1093/mnras/stv1795.","ista":"Pallottini A, Ferrara A, Pacucci F, Gallerani S, Salvadori S, Schneider R, Schaerer D, Sobral D, Matthee JJ. 2015. The brightest Lyα emitter: Pop III or black hole? Monthly Notices of the Royal Astronomical Society. 453(3), 2465–2470.","short":"A. Pallottini, A. Ferrara, F. Pacucci, S. Gallerani, S. Salvadori, R. Schneider, D. Schaerer, D. Sobral, J.J. Matthee, Monthly Notices of the Royal Astronomical Society 453 (2015) 2465–2470.","ama":"Pallottini A, Ferrara A, Pacucci F, et al. The brightest Lyα emitter: Pop III or black hole? Monthly Notices of the Royal Astronomical Society. 2015;453(3):2465-2470. doi:10.1093/mnras/stv1795","ieee":"A. Pallottini et al., “The brightest Lyα emitter: Pop III or black hole?,” Monthly Notices of the Royal Astronomical Society, vol. 453, no. 3. Oxford University Press, pp. 2465–2470, 2015."},"year":"2015","acknowledgement":"SS acknowledges support from the Netherlands Organization for Scientific research (NWO), VENI grant 639.041.233. RS acknowledges support from the European Research Council under the European Union (FP/2007-2013)/ERC grant agreement no. 306476. DS acknowledges (i) financial support from the NWO through a Veni fellowship and (ii) funding from FCT through a FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010) and from FCT grant PEstOE/FIS/UI2751/2014.","doi":"10.1093/mnras/stv1795","_id":"11579","article_type":"original"},{"publication":"Monthly Notices of the Royal Astronomical Society","language":[{"iso":"eng"}],"intvolume":" 440","scopus_import":"1","oa":1,"date_updated":"2022-08-19T08:30:30Z","issue":"3","article_processing_charge":"No","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","type":"journal_article","status":"public","month":"05","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1402.6697"}],"day":"21","oa_version":"Preprint","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","author":[{"first_name":"Jorryt J","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee"},{"first_name":"David","full_name":"Sobral, David","last_name":"Sobral"},{"last_name":"Swinbank","first_name":"A. M.","full_name":"Swinbank, A. M."},{"first_name":"Ian","full_name":"Smail, Ian","last_name":"Smail"},{"first_name":"P. N.","full_name":"Best, P. N.","last_name":"Best"},{"last_name":"Kim","full_name":"Kim, Jae-Woo","first_name":"Jae-Woo"},{"full_name":"Franx, Marijn","first_name":"Marijn","last_name":"Franx"},{"last_name":"Milvang-Jensen","full_name":"Milvang-Jensen, Bo","first_name":"Bo"},{"first_name":"Johan","full_name":"Fynbo, Johan","last_name":"Fynbo"}],"arxiv":1,"doi":"10.1093/mnras/stu392","article_type":"original","_id":"11583","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.","year":"2014","citation":{"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","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.","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.","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.","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.","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"},"date_created":"2022-07-14T12:33:24Z","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","cosmology: observations","dark ages","reionization","first stars"],"publisher":"Oxford University Press","date_published":"2014-05-21T00:00:00Z","extern":"1","page":"2375-2387","volume":440,"quality_controlled":"1","external_id":{"arxiv":["1402.6697"]},"abstract":[{"lang":"eng","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."}],"publication_status":"published"},{"author":[{"last_name":"Sobral","full_name":"Sobral, D.","first_name":"D."},{"last_name":"Swinbank","full_name":"Swinbank, A. M.","first_name":"A. M."},{"last_name":"Stott","first_name":"J. P.","full_name":"Stott, J. P."},{"first_name":"Jorryt J","full_name":"Matthee, Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X"},{"first_name":"R. G.","full_name":"Bower, R. G.","last_name":"Bower"},{"last_name":"Smail","first_name":"Ian","full_name":"Smail, Ian"},{"first_name":"P.","full_name":"Best, P.","last_name":"Best"},{"first_name":"J. E.","full_name":"Geach, J. E.","last_name":"Geach"},{"last_name":"Sharples","full_name":"Sharples, R. M.","first_name":"R. M."}],"arxiv":1,"publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"month":"12","main_file_link":[{"url":"https://arxiv.org/abs/1310.3822","open_access":"1"}],"day":"03","oa_version":"Preprint","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","type":"journal_article","oa":1,"date_updated":"2022-08-18T10:43:07Z","issue":"2","article_processing_charge":"No","title":"The dynamics of z=0.8 H-alpha-selected star-forming galaxies from KMOS/CF-HiZELS","intvolume":" 779","scopus_import":"1","language":[{"iso":"eng"}],"publication":"The Astrophysical Journal","publication_status":"published","external_id":{"arxiv":["1310.3822"]},"abstract":[{"lang":"eng","text":"We present the spatially resolved Hα dynamics of 16 star-forming galaxies at z ∼ 0.81 using the new KMOS multi-object integral field spectrograph on the ESO Very Large Telescope. These galaxies, selected using 1.18 μm narrowband imaging from the 10 deg2 CFHT-HiZELS survey of the SA 22 hr field, are found in a ∼4 Mpc overdensity of Hα emitters and likely reside in a group/intermediate environment, but not a cluster. We confirm and identify a rich group of star-forming galaxies at z = 0.813 ± 0.003, with 13 galaxies within 1000 km s−1 of each other, and seven within a diameter of 3 Mpc. All of our galaxies are “typical” star-forming galaxies at their redshift, 0.8 ± 0.4 SFR$^*_{z = 0.8}$, spanning a range of specific star formation rates (sSFRs) of 0.2–1.1 Gyr−1 and have a median metallicity very close to solar of 12 + log(O/H) = 8.62 ± 0.06. We measure the spatially resolved Hα dynamics of the galaxies in our sample and show that 13 out of 16 galaxies can be described by rotating disks and use the data to derive inclination corrected rotation speeds of 50–275 km s−1. The fraction of disks within our sample is 75% ± 8%, consistent with previous results based on Hubble Space Telescope morphologies of Hα-selected galaxies at z ∼ 1 and confirming that disks dominate the SFR density at z ∼ 1. Our Hα galaxies are well fitted by the z ∼ 1–2 Tully–Fisher (TF) relation, confirming the evolution seen in the zero point. Apart from having, on average, higher stellar masses and lower sSFRs, our group galaxies at z = 0.81 present the same mass–metallicity and TF relation as z ∼ 1 field galaxies and are all disk galaxies."}],"publisher":"IOP Publishing","date_published":"2013-12-03T00:00:00Z","extern":"1","volume":779,"quality_controlled":"1","acknowledgement":"We thank the referee for many helpful comments and suggestions which greatly improved the clarity and quality of this work. D.S. acknowledges financial support from the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship and also funding from the European Community Seventh Framework Programme (FP7/2007-2013) under grant agreement number RG226604 (OPTICON) which allowed access to CFHT time (proposals: 11BO29 & 12AO19). A.M.S. gratefully acknowledges an STFC Advanced Fellowship through grant number ST/H005234/1. I.R.S., J.P.S., and R.G.B. acknowledge support from the UK Science and Technology Facilities Council (STFC) under ST/I001573/1. I.R.S. acknowledges STFC (ST/J001422/1), the ERC Advanced Investigator program DUSTYGAL and a Royal Society/Wolfson Merit Award. P.N.B. acknowledges support from STFC. R.M.S. acknowledges support from the grant ST/1001573/1. The data presented here are based on observations with the KMOS spectrograph on the ESO/VLT under program 60.A-9460 and can be accessed through the ESO data archive. The authors also wish to acknowledge the help from Michael Hilker in preparing the KMOS observations.","year":"2013","date_created":"2022-07-07T09:14:48Z","citation":{"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).","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.","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","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.","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.","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"},"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution – galaxies","high-redshift – galaxies","starburst"],"article_number":"139","_id":"11520","article_type":"original","doi":"10.1088/0004-637x/779/2/139"},{"publisher":"Elsevier","date_published":"2011-06-01T00:00:00Z","status":"public","type":"journal_article","extern":"1","page":"246-259","quality_controlled":"1","volume":210,"month":"06","publication_identifier":{"issn":["1090-7807"]},"day":"01","oa_version":"None","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","abstract":[{"lang":"eng","text":"The accurate experimental determination of dipolar-coupling constants for one-bond heteronuclear dipolar couplings in solids is a key for the quantification of the amplitudes of motional processes. Averaging of the dipolar coupling reports on motions on time scales up to the inverse of the coupling constant, in our case tens of microseconds. Combining dipolar-coupling derived order parameters that characterize the amplitudes of the motion with relaxation data leads to a more precise characterization of the dynamical parameters and helps to disentangle the amplitudes and the time scales of the motional processes, which impact relaxation rates in a highly correlated way. Here. we describe and characterize an improved experimental protocol – based on REDOR – to measure these couplings in perdeuterated proteins with a reduced sensitivity to experimental missettings. Because such effects are presently the dominant source of systematic errors in experimental dipolar-coupling measurements, these compensated experiments should help to significantly improve the precision of such data. A detailed comparison with other commonly used pulse sequences (T-MREV, phase-inverted CP,R18 5/2, and R18 7/1) is provided."}],"publication_status":"published","author":[{"orcid":"0000-0002-9350-7606","last_name":"Schanda","id":"7B541462-FAF6-11E9-A490-E8DFE5697425","first_name":"Paul","full_name":"Schanda, Paul"},{"last_name":"Meier","first_name":"Beat H.","full_name":"Meier, Beat H."},{"full_name":"Ernst, Matthias","first_name":"Matthias","last_name":"Ernst"}],"publication":"Journal of Magnetic Resonance","doi":"10.1016/j.jmr.2011.03.015","_id":"8469","language":[{"iso":"eng"}],"article_type":"original","intvolume":" 210","date_updated":"2021-01-12T08:19:29Z","article_processing_charge":"No","issue":"2","year":"2011","title":"Accurate measurement of one-bond H–X heteronuclear dipolar couplings in MAS solid-state NMR","date_created":"2020-09-18T10:10:50Z","citation":{"apa":"Schanda, P., Meier, B. H., & Ernst, M. (2011). Accurate measurement of one-bond H–X heteronuclear dipolar couplings in MAS solid-state NMR. Journal of Magnetic Resonance. Elsevier. https://doi.org/10.1016/j.jmr.2011.03.015","chicago":"Schanda, Paul, Beat H. Meier, and Matthias Ernst. “Accurate Measurement of One-Bond H–X Heteronuclear Dipolar Couplings in MAS Solid-State NMR.” Journal of Magnetic Resonance. Elsevier, 2011. https://doi.org/10.1016/j.jmr.2011.03.015.","ista":"Schanda P, Meier BH, Ernst M. 2011. Accurate measurement of one-bond H–X heteronuclear dipolar couplings in MAS solid-state NMR. Journal of Magnetic Resonance. 210(2), 246–259.","mla":"Schanda, Paul, et al. “Accurate Measurement of One-Bond H–X Heteronuclear Dipolar Couplings in MAS Solid-State NMR.” Journal of Magnetic Resonance, vol. 210, no. 2, Elsevier, 2011, pp. 246–59, doi:10.1016/j.jmr.2011.03.015.","ieee":"P. Schanda, B. H. Meier, and M. Ernst, “Accurate measurement of one-bond H–X heteronuclear dipolar couplings in MAS solid-state NMR,” Journal of Magnetic Resonance, vol. 210, no. 2. Elsevier, pp. 246–259, 2011.","ama":"Schanda P, Meier BH, Ernst M. Accurate measurement of one-bond H–X heteronuclear dipolar couplings in MAS solid-state NMR. Journal of Magnetic Resonance. 2011;210(2):246-259. doi:10.1016/j.jmr.2011.03.015","short":"P. Schanda, B.H. Meier, M. Ernst, Journal of Magnetic Resonance 210 (2011) 246–259."},"keyword":["Nuclear and High Energy Physics","Biophysics","Biochemistry","Condensed Matter Physics"]},{"publication_status":"published","author":[{"last_name":"Kern","full_name":"Kern, Thomas","first_name":"Thomas"},{"last_name":"Schanda","id":"7B541462-FAF6-11E9-A490-E8DFE5697425","orcid":"0000-0002-9350-7606","full_name":"Schanda, Paul","first_name":"Paul"},{"first_name":"Bernhard","full_name":"Brutscher, Bernhard","last_name":"Brutscher"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","abstract":[{"text":"The SOFAST-HMQC experiment [P. Schanda, B. Brutscher, Very fast two-dimensional NMR spectroscopy for real-time investigation of dynamic events in proteins on the time scale of seconds, J. Am. Chem. Soc. 127 (2005) 8014–8015] allows recording two-dimensional correlation spectra of macromolecules such as proteins in only a few seconds acquisition time. To achieve the highest possible sensitivity, SOFAST-HMQC experiments are preferably performed on high-field NMR spectrometers equipped with cryogenically cooled probes. The duty cycle of over 80% in fast-pulsing SOFAST-HMQC experiments, however, may cause problems when using a cryogenic probe. Here we introduce SE-IPAP-SOFAST-HMQC, a new pulse sequence that provides comparable sensitivity to standard SOFAST-HMQC, while avoiding heteronuclear decoupling during 1H detection, and thus significantly reducing the radiofrequency load of the probe during the experiment. The experiment is also attractive for fast and sensitive measurement of heteronuclear one-bond spin coupling constants.","lang":"eng"}],"day":"01","oa_version":"None","publication_identifier":{"issn":["1090-7807"]},"month":"02","volume":190,"quality_controlled":"1","extern":"1","page":"333-338","status":"public","date_published":"2008-02-01T00:00:00Z","type":"journal_article","publisher":"Elsevier","keyword":["Nuclear and High Energy Physics","Biophysics","Biochemistry","Condensed Matter Physics"],"title":"Sensitivity-enhanced IPAP-SOFAST-HMQC for fast-pulsing 2D NMR with reduced radiofrequency load","citation":{"ama":"Kern T, Schanda P, Brutscher B. Sensitivity-enhanced IPAP-SOFAST-HMQC for fast-pulsing 2D NMR with reduced radiofrequency load. Journal of Magnetic Resonance. 2008;190(2):333-338. doi:10.1016/j.jmr.2007.11.015","ieee":"T. Kern, P. Schanda, and B. Brutscher, “Sensitivity-enhanced IPAP-SOFAST-HMQC for fast-pulsing 2D NMR with reduced radiofrequency load,” Journal of Magnetic Resonance, vol. 190, no. 2. Elsevier, pp. 333–338, 2008.","short":"T. Kern, P. Schanda, B. Brutscher, Journal of Magnetic Resonance 190 (2008) 333–338.","mla":"Kern, Thomas, et al. “Sensitivity-Enhanced IPAP-SOFAST-HMQC for Fast-Pulsing 2D NMR with Reduced Radiofrequency Load.” Journal of Magnetic Resonance, vol. 190, no. 2, Elsevier, 2008, pp. 333–38, doi:10.1016/j.jmr.2007.11.015.","ista":"Kern T, Schanda P, Brutscher B. 2008. Sensitivity-enhanced IPAP-SOFAST-HMQC for fast-pulsing 2D NMR with reduced radiofrequency load. Journal of Magnetic Resonance. 190(2), 333–338.","chicago":"Kern, Thomas, Paul Schanda, and Bernhard Brutscher. “Sensitivity-Enhanced IPAP-SOFAST-HMQC for Fast-Pulsing 2D NMR with Reduced Radiofrequency Load.” Journal of Magnetic Resonance. Elsevier, 2008. https://doi.org/10.1016/j.jmr.2007.11.015.","apa":"Kern, T., Schanda, P., & Brutscher, B. (2008). Sensitivity-enhanced IPAP-SOFAST-HMQC for fast-pulsing 2D NMR with reduced radiofrequency load. Journal of Magnetic Resonance. Elsevier. https://doi.org/10.1016/j.jmr.2007.11.015"},"date_created":"2020-09-18T10:12:46Z","article_processing_charge":"No","year":"2008","issue":"2","date_updated":"2021-01-12T08:19:35Z","intvolume":" 190","_id":"8482","article_type":"letter_note","language":[{"iso":"eng"}],"doi":"10.1016/j.jmr.2007.11.015","publication":"Journal of Magnetic Resonance"},{"publication":"Journal of Magnetic Resonance","doi":"10.1016/j.jmr.2005.10.007","_id":"8490","language":[{"iso":"eng"}],"article_type":"original","intvolume":" 178","year":"2006","issue":"2","article_processing_charge":"No","date_updated":"2021-01-12T08:19:38Z","keyword":["Nuclear and High Energy Physics","Biophysics","Biochemistry","Condensed Matter Physics"],"date_created":"2020-09-18T10:13:51Z","citation":{"apa":"Schanda, P., & Brutscher, B. (2006). Hadamard frequency-encoded SOFAST-HMQC for ultrafast two-dimensional protein NMR. Journal of Magnetic Resonance. Elsevier. https://doi.org/10.1016/j.jmr.2005.10.007","short":"P. Schanda, B. Brutscher, Journal of Magnetic Resonance 178 (2006) 334–339.","ieee":"P. Schanda and B. Brutscher, “Hadamard frequency-encoded SOFAST-HMQC for ultrafast two-dimensional protein NMR,” Journal of Magnetic Resonance, vol. 178, no. 2. Elsevier, pp. 334–339, 2006.","ama":"Schanda P, Brutscher B. Hadamard frequency-encoded SOFAST-HMQC for ultrafast two-dimensional protein NMR. Journal of Magnetic Resonance. 2006;178(2):334-339. doi:10.1016/j.jmr.2005.10.007","mla":"Schanda, Paul, and Bernhard Brutscher. “Hadamard Frequency-Encoded SOFAST-HMQC for Ultrafast Two-Dimensional Protein NMR.” Journal of Magnetic Resonance, vol. 178, no. 2, Elsevier, 2006, pp. 334–39, doi:10.1016/j.jmr.2005.10.007.","chicago":"Schanda, Paul, and Bernhard Brutscher. “Hadamard Frequency-Encoded SOFAST-HMQC for Ultrafast Two-Dimensional Protein NMR.” Journal of Magnetic Resonance. Elsevier, 2006. https://doi.org/10.1016/j.jmr.2005.10.007.","ista":"Schanda P, Brutscher B. 2006. Hadamard frequency-encoded SOFAST-HMQC for ultrafast two-dimensional protein NMR. Journal of Magnetic Resonance. 178(2), 334–339."},"title":"Hadamard frequency-encoded SOFAST-HMQC for ultrafast two-dimensional protein NMR","date_published":"2006-02-01T00:00:00Z","status":"public","type":"journal_article","publisher":"Elsevier","volume":178,"extern":"1","page":"334-339","month":"02","publication_identifier":{"issn":["1090-7807"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","abstract":[{"lang":"eng","text":"We demonstrate the feasibility of recording 1H–15N correlation spectra of proteins in only one second of acquisition time. The experiment combines recently proposed SOFAST-HMQC with Hadamard-type 15N frequency encoding. This allows site-resolved real-time NMR studies of kinetic processes in proteins with an increased time resolution. The sensitivity of the experiment is sufficient to be applicable to a wide range of molecular systems available at millimolar concentration on a high magnetic field spectrometer."}],"day":"01","oa_version":"None","publication_status":"published","author":[{"full_name":"Schanda, Paul","first_name":"Paul","orcid":"0000-0002-9350-7606","last_name":"Schanda","id":"7B541462-FAF6-11E9-A490-E8DFE5697425"},{"last_name":"Brutscher","first_name":"Bernhard","full_name":"Brutscher, Bernhard"}]}]