[{"publication":"Monthly Notices of the Royal Astronomical Society","month":"12","oa_version":"Preprint","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift","galaxies: luminosity function","mass function","cosmology: observations","dark ages","reionization","first stars"],"language":[{"iso":"eng"}],"type":"journal_article","date_published":"2016-12-01T00:00:00Z","oa":1,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1606.07435"}],"issue":"2","author":[{"first_name":"Sérgio","last_name":"Santos","full_name":"Santos, Sérgio"},{"first_name":"David","last_name":"Sobral","full_name":"Sobral, David"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X"}],"scopus_import":"1","_id":"11574","intvolume":"       463","title":"The Lyα luminosity function at z= 5.7–6.6 and the steep drop of the faint end: Implications for reionization","date_created":"2022-07-13T10:08:20Z","article_processing_charge":"No","publication_status":"published","quality_controlled":"1","page":"1678-1691","article_type":"original","publisher":"Oxford University Press","external_id":{"arxiv":["1606.07435"]},"year":"2016","citation":{"apa":"Santos, S., Sobral, D., &#38; 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. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stw2076\">https://doi.org/10.1093/mnras/stw2076</a>","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. <i>Monthly Notices of the Royal Astronomical Society</i>. 2016;463(2):1678-1691. doi:<a href=\"https://doi.org/10.1093/mnras/stw2076\">10.1093/mnras/stw2076</a>","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,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 463, no. 2. Oxford University Press, pp. 1678–1691, 2016.","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.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2016. <a href=\"https://doi.org/10.1093/mnras/stw2076\">https://doi.org/10.1093/mnras/stw2076</a>.","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.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 463, no. 2, Oxford University Press, 2016, pp. 1678–91, doi:<a href=\"https://doi.org/10.1093/mnras/stw2076\">10.1093/mnras/stw2076</a>.","short":"S. Santos, D. Sobral, J.J. Matthee, Monthly Notices of the Royal Astronomical Society 463 (2016) 1678–1691.","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."},"date_updated":"2022-08-19T08:09:54Z","abstract":[{"lang":"eng","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."}],"day":"01","arxiv":1,"doi":"10.1093/mnras/stw2076","extern":"1","volume":463,"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."},{"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"oa":1,"type":"journal_article","date_published":"2016-07-01T00:00:00Z","main_file_link":[{"url":"https://arxiv.org/abs/1510.08067","open_access":"1"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","oa_version":"Preprint","month":"07","publication":"Monthly Notices of the Royal Astronomical Society","keyword":["Space and Planetary Science","Astronomy and Astrophysics  stars: formation","ISM: evolution","galaxies: evolution","galaxies: formation","galaxies: ISM"],"language":[{"iso":"eng"}],"day":"01","arxiv":1,"doi":"10.1093/mnras/stw717","abstract":[{"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.","lang":"eng"}],"year":"2016","citation":{"chicago":"Lagos, Claudia del P., Tom Theuns, Joop Schaye, Michelle Furlong, Richard G. Bower, Matthieu Schaller, Robert A. Crain, James W. Trayford, and Jorryt J Matthee. “The Fundamental Plane of Star Formation in Galaxies Revealed by the EAGLE Hydrodynamical Simulations.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2016. <a href=\"https://doi.org/10.1093/mnras/stw717\">https://doi.org/10.1093/mnras/stw717</a>.","ieee":"C. del P. Lagos <i>et al.</i>, “The Fundamental Plane of star formation in galaxies revealed by the EAGLE hydrodynamical simulations,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 459, no. 3. Oxford University Press, pp. 2632–2650, 2016.","apa":"Lagos, C. del P., Theuns, T., Schaye, J., Furlong, M., Bower, R. G., Schaller, M., … Matthee, J. J. (2016). The Fundamental Plane of star formation in galaxies revealed by the EAGLE hydrodynamical simulations. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stw717\">https://doi.org/10.1093/mnras/stw717</a>","ama":"Lagos C del P, Theuns T, Schaye J, et al. The Fundamental Plane of star formation in galaxies revealed by the EAGLE hydrodynamical simulations. <i>Monthly Notices of the Royal Astronomical Society</i>. 2016;459(3):2632-2650. doi:<a href=\"https://doi.org/10.1093/mnras/stw717\">10.1093/mnras/stw717</a>","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.","mla":"Lagos, Claudia del P., et al. “The Fundamental Plane of Star Formation in Galaxies Revealed by the EAGLE Hydrodynamical Simulations.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 459, no. 3, Oxford University Press, 2016, pp. 2632–50, doi:<a href=\"https://doi.org/10.1093/mnras/stw717\">10.1093/mnras/stw717</a>.","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."},"date_updated":"2022-08-19T08:12:07Z","external_id":{"arxiv":["1510.08067"]},"volume":459,"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.","extern":"1","date_created":"2022-07-13T10:21:24Z","article_processing_charge":"No","publication_status":"published","intvolume":"       459","title":"The Fundamental Plane of star formation in galaxies revealed by the EAGLE hydrodynamical simulations","scopus_import":"1","_id":"11575","issue":"3","author":[{"last_name":"Lagos","first_name":"Claudia del P.","full_name":"Lagos, Claudia del P."},{"last_name":"Theuns","first_name":"Tom","full_name":"Theuns, Tom"},{"full_name":"Schaye, Joop","last_name":"Schaye","first_name":"Joop"},{"first_name":"Michelle","last_name":"Furlong","full_name":"Furlong, Michelle"},{"first_name":"Richard G.","last_name":"Bower","full_name":"Bower, Richard G."},{"full_name":"Schaller, Matthieu","first_name":"Matthieu","last_name":"Schaller"},{"full_name":"Crain, Robert A.","last_name":"Crain","first_name":"Robert A."},{"last_name":"Trayford","first_name":"James W.","full_name":"Trayford, James W."},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","last_name":"Matthee"}],"publisher":"Oxford University Press","article_type":"original","quality_controlled":"1","page":"2632-2650"},{"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","cosmology: observations"],"language":[{"iso":"eng"}],"publication":"Monthly Notices of the Royal Astronomical Society","oa_version":"Preprint","month":"04","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1601.02266"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","type":"journal_article","date_published":"2016-04-01T00:00:00Z","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"oa":1,"quality_controlled":"1","page":"1739-1752","publisher":"Oxford University Press","article_type":"original","scopus_import":"1","_id":"11576","issue":"2","author":[{"last_name":"Sobral","first_name":"David","full_name":"Sobral, David"},{"full_name":"Kohn, Saul A.","first_name":"Saul A.","last_name":"Kohn"},{"full_name":"Best, Philip N.","last_name":"Best","first_name":"Philip N."},{"full_name":"Smail, Ian","last_name":"Smail","first_name":"Ian"},{"full_name":"Harrison, Chris M.","first_name":"Chris M.","last_name":"Harrison"},{"last_name":"Stott","first_name":"John","full_name":"Stott, John"},{"last_name":"Calhau","first_name":"João","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"}],"date_created":"2022-07-13T12:50:36Z","article_processing_charge":"No","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","volume":457,"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.","extern":"1","citation":{"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.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2016. <a href=\"https://doi.org/10.1093/mnras/stw022\">https://doi.org/10.1093/mnras/stw022</a>.","ieee":"D. Sobral <i>et al.</i>, “The most luminous H α emitters at z ∼ 0.8–2.23 from HiZELS: Evolution of AGN and star-forming galaxies,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 457, no. 2. Oxford University Press, pp. 1739–1752, 2016.","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. <i>Monthly Notices of the Royal Astronomical Society</i>. 2016;457(2):1739-1752. doi:<a href=\"https://doi.org/10.1093/mnras/stw022\">10.1093/mnras/stw022</a>","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. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stw022\">https://doi.org/10.1093/mnras/stw022</a>","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.","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.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 457, no. 2, Oxford University Press, 2016, pp. 1739–52, doi:<a href=\"https://doi.org/10.1093/mnras/stw022\">10.1093/mnras/stw022</a>.","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."},"year":"2016","date_updated":"2022-08-19T08:15:21Z","external_id":{"arxiv":["1601.02266"]},"day":"01","arxiv":1,"doi":"10.1093/mnras/stw022","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."}]},{"quality_controlled":"1","page":"449-467","publisher":"Oxford University Press","article_type":"original","scopus_import":"1","_id":"11578","issue":"1","author":[{"first_name":"Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"full_name":"Sobral, David","last_name":"Sobral","first_name":"David"},{"first_name":"Iván","last_name":"Oteo","full_name":"Oteo, Iván"},{"first_name":"Philip","last_name":"Best","full_name":"Best, Philip"},{"full_name":"Smail, Ian","last_name":"Smail","first_name":"Ian"},{"first_name":"Huub","last_name":"Röttgering","full_name":"Röttgering, Huub"},{"full_name":"Paulino-Afonso, Ana","last_name":"Paulino-Afonso","first_name":"Ana"}],"article_processing_charge":"No","date_created":"2022-07-14T08:51:37Z","publication_status":"published","intvolume":"       458","title":"The CALYMHA survey: Lyα escape fraction and its dependence on galaxy properties at z = 2.23","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","year":"2016","citation":{"apa":"Matthee, J. J., Sobral, D., Oteo, I., Best, P., Smail, I., Röttgering, H., &#38; Paulino-Afonso, A. (2016). The CALYMHA survey: Lyα escape fraction and its dependence on galaxy properties at z = 2.23. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stw322\">https://doi.org/10.1093/mnras/stw322</a>","ama":"Matthee JJ, Sobral D, Oteo I, et al. The CALYMHA survey: Lyα escape fraction and its dependence on galaxy properties at z = 2.23. <i>Monthly Notices of the Royal Astronomical Society</i>. 2016;458(1):449-467. doi:<a href=\"https://doi.org/10.1093/mnras/stw322\">10.1093/mnras/stw322</a>","chicago":"Matthee, Jorryt J, David Sobral, Iván Oteo, Philip Best, Ian Smail, Huub Röttgering, and Ana Paulino-Afonso. “The CALYMHA Survey: Lyα Escape Fraction and Its Dependence on Galaxy Properties at z = 2.23.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2016. <a href=\"https://doi.org/10.1093/mnras/stw322\">https://doi.org/10.1093/mnras/stw322</a>.","ieee":"J. J. Matthee <i>et al.</i>, “The CALYMHA survey: Lyα escape fraction and its dependence on galaxy properties at z = 2.23,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 458, no. 1. Oxford University Press, pp. 449–467, 2016.","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.","mla":"Matthee, Jorryt J., et al. “The CALYMHA Survey: Lyα Escape Fraction and Its Dependence on Galaxy Properties at z = 2.23.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 458, no. 1, Oxford University Press, 2016, pp. 449–67, doi:<a href=\"https://doi.org/10.1093/mnras/stw322\">10.1093/mnras/stw322</a>.","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."},"date_updated":"2022-08-19T08:17:19Z","external_id":{"arxiv":["1602.02756"]},"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."}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","galaxies: ISM"],"language":[{"iso":"eng"}],"publication":"Monthly Notices of the Royal Astronomical Society","oa_version":"Preprint","month":"05","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1602.02756"}],"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","type":"journal_article","date_published":"2016-05-01T00:00:00Z","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"oa":1},{"date_published":"2016-08-18T00:00:00Z","type":"journal_article","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"oa":1,"main_file_link":[{"open_access":"1","url":"https://doi.org/10.1051/0004-6361/201526309"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","publication":"Astronomy & Astrophysics","oa_version":"Published Version","month":"08","article_number":"A147","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"date_updated":"2023-08-09T11:09:50Z","citation":{"apa":"Götberg, Y. L. L., Davies, M. B., Mustill, A. J., Johansen, A., &#38; Church, R. P. (2016). Long-term stability of the HR 8799 planetary system without resonant lock. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201526309\">https://doi.org/10.1051/0004-6361/201526309</a>","ama":"Götberg YLL, Davies MB, Mustill AJ, Johansen A, Church RP. Long-term stability of the HR 8799 planetary system without resonant lock. <i>Astronomy &#38; Astrophysics</i>. 2016;592. doi:<a href=\"https://doi.org/10.1051/0004-6361/201526309\">10.1051/0004-6361/201526309</a>","chicago":"Götberg, Ylva Louise Linsdotter, Melvyn B. Davies, Alexander J. Mustill, Anders Johansen, and Ross P. Church. “Long-Term Stability of the HR 8799 Planetary System without Resonant Lock.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2016. <a href=\"https://doi.org/10.1051/0004-6361/201526309\">https://doi.org/10.1051/0004-6361/201526309</a>.","ieee":"Y. L. L. Götberg, M. B. Davies, A. J. Mustill, A. Johansen, and R. P. Church, “Long-term stability of the HR 8799 planetary system without resonant lock,” <i>Astronomy &#38; Astrophysics</i>, vol. 592. EDP Sciences, 2016.","mla":"Götberg, Ylva Louise Linsdotter, et al. “Long-Term Stability of the HR 8799 Planetary System without Resonant Lock.” <i>Astronomy &#38; Astrophysics</i>, vol. 592, A147, EDP Sciences, 2016, doi:<a href=\"https://doi.org/10.1051/0004-6361/201526309\">10.1051/0004-6361/201526309</a>.","short":"Y.L.L. Götberg, M.B. Davies, A.J. Mustill, A. Johansen, R.P. Church, Astronomy &#38; Astrophysics 592 (2016).","ista":"Götberg YLL, Davies MB, Mustill AJ, Johansen A, Church RP. 2016. Long-term stability of the HR 8799 planetary system without resonant lock. Astronomy &#38; Astrophysics. 592, A147."},"year":"2016","external_id":{"arxiv":["1606.07819"]},"doi":"10.1051/0004-6361/201526309","arxiv":1,"day":"18","abstract":[{"lang":"eng","text":"HR 8799 is a star accompanied by four massive planets on wide orbits. The observed planetary configuration has been shown to be unstable on a timescale much shorter than the estimated age of the system (~30 Myr) unless the planets are locked into mean motion resonances. This condition is characterised by small-amplitude libration of one or more resonant angles that stabilise the system by preventing close encounters. We simulate planetary systems similar to the HR 8799 planetary system, exploring the parameter space in separation between the orbits, planetary masses and distance from the Sun to the star. We find systems that look like HR 8799 and remain stable for longer than the estimated age of HR 8799. None of our systems are forced into resonances. We find, with nominal masses (Mb = 5 MJup and Mc,d,e = 7 MJup) and in a narrow range of orbit separations, that 5 of 100 systems match the observations and lifetime. Considering a broad range of orbit separations, we find 12 of 900 similar systems. The systems survive significantly longer because of their slightly increased initial orbit separations compared to assuming circular orbits from the observed positions. A small increase in separation leads to a significant increase in survival time. The low eccentricity the orbits develop from gravitational interaction is enough for the planets to match the observations. With lower masses, but still comfortably within the estimated planet mass uncertainty, we find 18 of 100 matching and long-lived systems in a narrow orbital separation range. In the broad separation range, we find 82 of 900 matching systems. Our results imply that the planets in the HR 8799 system do not have to be in strong mean motion resonances. We also investigate the future of wide-orbit planetary systems using our HR 8799 analogues. We find that 80% of the systems have two planets left after strong planet-planet scattering and these are on eccentric orbits with semi-major axes of a1 ~ 10 AU and a2 ~ 30−1000 AU. We speculate that other wide-orbit planetary systems, such as AB Pic and HD 106906, are the remnants of HR 8799 analogues that underwent close encounters and dynamical instability."}],"volume":592,"extern":"1","_id":"13478","scopus_import":"1","author":[{"first_name":"Ylva Louise Linsdotter","last_name":"Götberg","orcid":"0000-0002-6960-6911","full_name":"Götberg, Ylva Louise Linsdotter","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d"},{"full_name":"Davies, Melvyn B.","first_name":"Melvyn B.","last_name":"Davies"},{"full_name":"Mustill, Alexander J.","first_name":"Alexander J.","last_name":"Mustill"},{"full_name":"Johansen, Anders","first_name":"Anders","last_name":"Johansen"},{"last_name":"Church","first_name":"Ross P.","full_name":"Church, Ross P."}],"publication_status":"published","article_processing_charge":"No","date_created":"2023-08-03T10:15:28Z","title":"Long-term stability of the HR 8799 planetary system without resonant lock","intvolume":"       592","quality_controlled":"1","publisher":"EDP Sciences","article_type":"original"},{"publication":"The Astrophysical Journal","oa_version":"Preprint","month":"07","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","dark ages","reionization","first stars – early universe – galaxies: evolution"],"date_published":"2015-07-28T00:00:00Z","type":"journal_article","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"oa":1,"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1504.01734"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","_id":"11519","scopus_import":"1","author":[{"full_name":"Sobral, David","last_name":"Sobral","first_name":"David"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X"},{"first_name":"Behnam","last_name":"Darvish","full_name":"Darvish, Behnam"},{"first_name":"Daniel","last_name":"Schaerer","full_name":"Schaerer, Daniel"},{"first_name":"Bahram","last_name":"Mobasher","full_name":"Mobasher, Bahram"},{"last_name":"Röttgering","first_name":"Huub","full_name":"Röttgering, Huub"},{"first_name":"Sérgio","last_name":"Santos","full_name":"Santos, Sérgio"},{"last_name":"Hemmati","first_name":"Shoubaneh","full_name":"Hemmati, Shoubaneh"}],"issue":"2","publication_status":"published","date_created":"2022-07-07T09:00:58Z","article_processing_charge":"No","title":"Evidence for PopIII-like stellar populations in the most luminous Lyα emitters at the epoch of reionisation: Spectroscopic confirmation","intvolume":"       808","page":"139","quality_controlled":"1","publisher":"IOP Publishing","article_type":"original","date_updated":"2022-08-18T10:30:13Z","citation":{"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.","mla":"Sobral, David, et al. “Evidence for PopIII-like Stellar Populations in the Most Luminous Lyα Emitters at the Epoch of Reionisation: Spectroscopic Confirmation.” <i>The Astrophysical Journal</i>, vol. 808, no. 2, IOP Publishing, 2015, p. 139, doi:<a href=\"https://doi.org/10.1088/0004-637X/808/2/139\">10.1088/0004-637X/808/2/139</a>.","short":"D. Sobral, J.J. Matthee, B. Darvish, D. Schaerer, B. Mobasher, H. Röttgering, S. Santos, S. Hemmati, The Astrophysical Journal 808 (2015) 139.","ieee":"D. Sobral <i>et al.</i>, “Evidence for PopIII-like stellar populations in the most luminous Lyα emitters at the epoch of reionisation: Spectroscopic confirmation,” <i>The Astrophysical Journal</i>, 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.” <i>The Astrophysical Journal</i>. IOP Publishing, 2015. <a href=\"https://doi.org/10.1088/0004-637X/808/2/139\">https://doi.org/10.1088/0004-637X/808/2/139</a>.","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. <i>The Astrophysical Journal</i>. 2015;808(2):139. doi:<a href=\"https://doi.org/10.1088/0004-637X/808/2/139\">10.1088/0004-637X/808/2/139</a>","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. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.1088/0004-637X/808/2/139\">https://doi.org/10.1088/0004-637X/808/2/139</a>"},"year":"2015","external_id":{"arxiv":["1504.01734"]},"arxiv":1,"doi":"10.1088/0004-637X/808/2/139","day":"28","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"}],"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,"extern":"1"},{"main_file_link":[{"url":"https://arxiv.org/abs/1506.07173","open_access":"1"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","type":"journal_article","date_published":"2015-11-01T00:00:00Z","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"oa":1,"keyword":["Space and Planetary Science","Astronomy and Astrophysics","black hole physics","stars: Population III","galaxies: high-redshift"],"language":[{"iso":"eng"}],"publication":"Monthly Notices of the Royal Astronomical Society","oa_version":"Preprint","month":"11","volume":453,"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.","extern":"1","citation":{"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.","mla":"Pallottini, A., et al. “The Brightest Lyα Emitter: Pop III or Black Hole?” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 453, no. 3, Oxford University Press, 2015, pp. 2465–70, doi:<a href=\"https://doi.org/10.1093/mnras/stv1795\">10.1093/mnras/stv1795</a>.","ieee":"A. Pallottini <i>et al.</i>, “The brightest Lyα emitter: Pop III or black hole?,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 453, no. 3. Oxford University Press, pp. 2465–2470, 2015.","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?” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2015. <a href=\"https://doi.org/10.1093/mnras/stv1795\">https://doi.org/10.1093/mnras/stv1795</a>.","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? <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stv1795\">https://doi.org/10.1093/mnras/stv1795</a>","ama":"Pallottini A, Ferrara A, Pacucci F, et al. The brightest Lyα emitter: Pop III or black hole? <i>Monthly Notices of the Royal Astronomical Society</i>. 2015;453(3):2465-2470. doi:<a href=\"https://doi.org/10.1093/mnras/stv1795\">10.1093/mnras/stv1795</a>"},"year":"2015","date_updated":"2022-08-19T08:19:23Z","external_id":{"arxiv":["1506.07173"]},"day":"01","doi":"10.1093/mnras/stv1795","arxiv":1,"abstract":[{"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.","lang":"eng"}],"quality_controlled":"1","page":"2465-2470","publisher":"Oxford University Press","article_type":"original","scopus_import":"1","_id":"11579","issue":"3","author":[{"full_name":"Pallottini, A.","last_name":"Pallottini","first_name":"A."},{"first_name":"A.","last_name":"Ferrara","full_name":"Ferrara, A."},{"full_name":"Pacucci, F.","first_name":"F.","last_name":"Pacucci"},{"first_name":"S.","last_name":"Gallerani","full_name":"Gallerani, S."},{"first_name":"S.","last_name":"Salvadori","full_name":"Salvadori, S."},{"full_name":"Schneider, R.","first_name":"R.","last_name":"Schneider"},{"first_name":"D.","last_name":"Schaerer","full_name":"Schaerer, D."},{"first_name":"D.","last_name":"Sobral","full_name":"Sobral, D."},{"first_name":"Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"}],"article_processing_charge":"No","date_created":"2022-07-14T08:58:36Z","publication_status":"published","intvolume":"       453","title":"The brightest Lyα emitter: Pop III or black hole?"},{"main_file_link":[{"url":"https://arxiv.org/abs/1502.06602","open_access":"1"}],"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"oa":1,"type":"journal_article","date_published":"2015-08-11T00:00:00Z","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"}],"oa_version":"Preprint","month":"08","publication":"Monthly Notices of the Royal Astronomical Society","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).","volume":451,"extern":"1","day":"11","arxiv":1,"doi":"10.1093/mnras/stv1076","abstract":[{"lang":"eng","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."}],"year":"2015","citation":{"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 .” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2015. <a href=\"https://doi.org/10.1093/mnras/stv1076\">https://doi.org/10.1093/mnras/stv1076</a>.","ieee":"D. Sobral <i>et al.</i>, “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 ,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 451, no. 3. Oxford University Press, pp. 2303–2323, 2015.","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 . <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stv1076\">https://doi.org/10.1093/mnras/stv1076</a>","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 . <i>Monthly Notices of the Royal Astronomical Society</i>. 2015;451(3):2303-2323. doi:<a href=\"https://doi.org/10.1093/mnras/stv1076\">10.1093/mnras/stv1076</a>","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 .” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 451, no. 3, Oxford University Press, 2015, pp. 2303–23, doi:<a href=\"https://doi.org/10.1093/mnras/stv1076\">10.1093/mnras/stv1076</a>.","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"]},"publisher":"Oxford University Press","article_type":"original","quality_controlled":"1","page":"2303-2323","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":[{"full_name":"Sobral, D.","first_name":"D.","last_name":"Sobral"},{"orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"full_name":"Best, P. N.","first_name":"P. N.","last_name":"Best"},{"full_name":"Smail, I.","last_name":"Smail","first_name":"I."},{"full_name":"Khostovan, A. A.","last_name":"Khostovan","first_name":"A. A."},{"full_name":"Milvang-Jensen, B.","last_name":"Milvang-Jensen","first_name":"B."},{"full_name":"Kim, J.-W.","last_name":"Kim","first_name":"J.-W."},{"full_name":"Stott, J.","first_name":"J.","last_name":"Stott"},{"full_name":"Calhau, J.","first_name":"J.","last_name":"Calhau"},{"full_name":"Nayyeri, H.","last_name":"Nayyeri","first_name":"H."},{"first_name":"B.","last_name":"Mobasher","full_name":"Mobasher, B."}]},{"oa_version":"Preprint","month":"07","publication":"Monthly Notices of the Royal Astronomical Society","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"language":[{"iso":"eng"}],"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"oa":1,"type":"journal_article","date_published":"2015-07-21T00:00:00Z","main_file_link":[{"url":"https://arxiv.org/abs/1502.07355","open_access":"1"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","article_processing_charge":"No","date_created":"2022-07-14T11:57:03Z","publication_status":"published","intvolume":"       451","title":"Identification of the brightest Lyα emitters at z = 6.6: implications for the evolution of the luminosity function in the reionization era","scopus_import":"1","_id":"11581","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"},{"full_name":"Sobral, David","first_name":"David","last_name":"Sobral"},{"full_name":"Santos, Sérgio","first_name":"Sérgio","last_name":"Santos"},{"full_name":"Röttgering, Huub","first_name":"Huub","last_name":"Röttgering"},{"last_name":"Darvish","first_name":"Behnam","full_name":"Darvish, Behnam"},{"last_name":"Mobasher","first_name":"Bahram","full_name":"Mobasher, Bahram"}],"publisher":"Oxford University Press","article_type":"original","quality_controlled":"1","page":"400-417","day":"21","doi":"10.1093/mnras/stv947","arxiv":1,"abstract":[{"text":"Using wide-field narrow-band surveys, we provide a new measurement of the z = 6.6 Lymanα emitter (LAE) luminosity function (LF), which constraints the bright end for the first time. We use a combination of archival narrow-band NB921 data in UDS and new NB921 measurements in SA22 and COSMOS/UltraVISTA, all observed with the Subaru telescope, with a total area of ∼5 deg2. We exclude lower redshift interlopers by using broad-band optical and near-infrared photometry and also exclude three supernovae with data split over multiple epochs. Combining the UDS and COSMOS samples, we find no evolution of the bright end of the Lyα LF between z = 5.7 and 6.6, which is supported by spectroscopic follow-up, and conclude that sources with Himiko-like luminosity are not as rare as previously thought, with number densities of ∼1.5 × 10−5 Mpc−3. Combined with our wide-field SA22 measurements, our results indicate a non-Schechter-like bright end of the LF at z = 6.6 and a different evolution of observed faint and bright LAEs, overcoming cosmic variance. This differential evolution is also seen in the spectroscopic follow-up of UV-selected galaxies and is now also confirmed for LAEs, and we argue that it may be an effect of reionization. Using a toy model, we show that such differential evolution of the LF is expected, since brighter sources are able to ionize their surroundings earlier, such that Lyα photons are able to escape. Our targets are excellent candidates for detailed follow-up studies and provide the possibility to give a unique view on the earliest stages in the formation of galaxies and reionization process.","lang":"eng"}],"year":"2015","citation":{"ista":"Matthee JJ, Sobral D, Santos S, Röttgering H, Darvish B, Mobasher B. 2015. Identification of the brightest Lyα emitters at z = 6.6: implications for the evolution of the luminosity function in the reionization era. Monthly Notices of the Royal Astronomical Society. 451(1), 400–417.","mla":"Matthee, Jorryt J., et al. “Identification of the Brightest Lyα Emitters at z = 6.6: Implications for the Evolution of the Luminosity Function in the Reionization Era.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 451, no. 1, Oxford University Press, 2015, pp. 400–17, doi:<a href=\"https://doi.org/10.1093/mnras/stv947\">10.1093/mnras/stv947</a>.","short":"J.J. Matthee, D. Sobral, S. Santos, H. Röttgering, B. Darvish, B. Mobasher, Monthly Notices of the Royal Astronomical Society 451 (2015) 400–417.","chicago":"Matthee, Jorryt J, David Sobral, Sérgio Santos, Huub Röttgering, Behnam Darvish, and Bahram Mobasher. “Identification of the Brightest Lyα Emitters at z = 6.6: Implications for the Evolution of the Luminosity Function in the Reionization Era.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2015. <a href=\"https://doi.org/10.1093/mnras/stv947\">https://doi.org/10.1093/mnras/stv947</a>.","ieee":"J. J. Matthee, D. Sobral, S. Santos, H. Röttgering, B. Darvish, and B. Mobasher, “Identification of the brightest Lyα emitters at z = 6.6: implications for the evolution of the luminosity function in the reionization era,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 451, no. 1. Oxford University Press, pp. 400–417, 2015.","apa":"Matthee, J. J., Sobral, D., Santos, S., Röttgering, H., Darvish, B., &#38; Mobasher, B. (2015). Identification of the brightest Lyα emitters at z = 6.6: implications for the evolution of the luminosity function in the reionization era. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stv947\">https://doi.org/10.1093/mnras/stv947</a>","ama":"Matthee JJ, Sobral D, Santos S, Röttgering H, Darvish B, Mobasher B. Identification of the brightest Lyα emitters at z = 6.6: implications for the evolution of the luminosity function in the reionization era. <i>Monthly Notices of the Royal Astronomical Society</i>. 2015;451(1):400-417. doi:<a href=\"https://doi.org/10.1093/mnras/stv947\">10.1093/mnras/stv947</a>"},"date_updated":"2022-08-19T08:25:25Z","external_id":{"arxiv":["1502.07355"]},"acknowledgement":"We thank the anonymous referee for the comments and suggestions which have improved the quality of this work. We thank Masami Ouchi for his useful comments on an earlier version of this paper. JM acknowledges the support of a Huygens PhD fellowship from Leiden University and is thankful for the hospitality of the Center for Astronomy and Astrophysics of the University of Lisbon where part of this research has been done. DS acknowledges financial support from the Netherlands Organization 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) and from FCT grant PEstOE/FIS/UI2751/2014. HR acknowledges support from the ERC Advanced Investigator programme NewClusters 321271. We acknowledge the award of ESO DDT time (294.A-5018) for providing the possibility of a timely publication of this work.\r\nBased on observations with the Subaru Telescope (Programme IDs: our observations: S14A-086; archival: S05B-027, S06A-025, S06B-010, S07A-013, S07B-008, S08B-008 and S09A-017) and the W.M. Keck Observatory. The Subaru telescope is operated by the National Astronomical Observatory of Japan. The W.M. Keck Observatory is operated as a scientific partnership among 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 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 CFHT 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.\r\nIn addition to the CFHT-LS and COSMOS-UltraVISTA surveys, we are grateful for the excellent data sets from the UKIRT-DXS, SXDF and S-COSMOS survey teams, without these legacy surveys, this research would have been impossible. We have benefited greatly 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 indispensable TOPCAT analysis tool (Taylor 2013)","volume":451,"extern":"1"},{"volume":120,"extern":"1","doi":"10.1002/2015jd023137","day":"18","abstract":[{"lang":"eng","text":"Air temperature is one of the most relevant input variables for snow and ice melt calculations. However, local meteorological conditions, complex topography, and logistical concerns in glacierized regions make the measuring and modeling of air temperature a difficult task. In this study, we investigate the spatial distribution of 2 m air temperature over mountain glaciers and propose a modification to an existing model to improve its representation. Spatially distributed meteorological data from Haut Glacier d'Arolla (Switzerland), Place (Canada), and Juncal Norte (Chile) Glaciers are used to examine approximate flow line temperatures during their respective ablation seasons. During warm conditions (off-glacier temperatures well above 0°C), observed air temperatures in the upper reaches of Place Glacier and Haut Glacier d'Arolla decrease down glacier along the approximate flow line. At Juncal Norte and Haut Glacier d'Arolla, an increase in air temperature is observed over the glacier tongue. While the temperature behavior over the upper part can be explained by the cooling effect of the glacier surface, the temperature increase over the glacier tongue may be caused by several processes induced by the surrounding warm atmosphere. In order to capture the latter effect, we add an additional term to the Greuell and Böhm (GB) thermodynamic glacier wind model. For high off-glacier temperatures, the modified GB model reduces root-mean-square error up to 32% and provides a new approach for distributing air temperature over mountain glaciers as a function of off-glacier temperatures and approximate glacier flow lines."}],"date_updated":"2023-02-24T09:16:26Z","citation":{"ama":"Ayala A, Pellicciotti F, Shea JM. Modeling 2 m air temperatures over mountain glaciers: Exploring the influence of katabatic cooling and external warming. <i>Journal of Geophysical Research: Atmospheres</i>. 2015;120(8):3139-3157. doi:<a href=\"https://doi.org/10.1002/2015jd023137\">10.1002/2015jd023137</a>","apa":"Ayala, A., Pellicciotti, F., &#38; Shea, J. M. (2015). Modeling 2 m air temperatures over mountain glaciers: Exploring the influence of katabatic cooling and external warming. <i>Journal of Geophysical Research: Atmospheres</i>. American Geophysical Union. <a href=\"https://doi.org/10.1002/2015jd023137\">https://doi.org/10.1002/2015jd023137</a>","ieee":"A. Ayala, F. Pellicciotti, and J. M. Shea, “Modeling 2 m air temperatures over mountain glaciers: Exploring the influence of katabatic cooling and external warming,” <i>Journal of Geophysical Research: Atmospheres</i>, vol. 120, no. 8. American Geophysical Union, pp. 3139–3157, 2015.","chicago":"Ayala, A., Francesca Pellicciotti, and J. M. Shea. “Modeling 2 m Air Temperatures over Mountain Glaciers: Exploring the Influence of Katabatic Cooling and External Warming.” <i>Journal of Geophysical Research: Atmospheres</i>. American Geophysical Union, 2015. <a href=\"https://doi.org/10.1002/2015jd023137\">https://doi.org/10.1002/2015jd023137</a>.","mla":"Ayala, A., et al. “Modeling 2 m Air Temperatures over Mountain Glaciers: Exploring the Influence of Katabatic Cooling and External Warming.” <i>Journal of Geophysical Research: Atmospheres</i>, vol. 120, no. 8, American Geophysical Union, 2015, pp. 3139–57, doi:<a href=\"https://doi.org/10.1002/2015jd023137\">10.1002/2015jd023137</a>.","short":"A. Ayala, F. Pellicciotti, J.M. Shea, Journal of Geophysical Research: Atmospheres 120 (2015) 3139–3157.","ista":"Ayala A, Pellicciotti F, Shea JM. 2015. Modeling 2 m air temperatures over mountain glaciers: Exploring the influence of katabatic cooling and external warming. Journal of Geophysical Research: Atmospheres. 120(8), 3139–3157."},"year":"2015","publisher":"American Geophysical Union","article_type":"original","page":"3139-3157","quality_controlled":"1","publication_status":"published","article_processing_charge":"No","date_created":"2023-02-20T08:16:28Z","title":"Modeling 2 m air temperatures over mountain glaciers: Exploring the influence of katabatic cooling and external warming","intvolume":"       120","_id":"12631","scopus_import":"1","author":[{"last_name":"Ayala","first_name":"A.","full_name":"Ayala, A."},{"full_name":"Pellicciotti, Francesca","first_name":"Francesca","last_name":"Pellicciotti","id":"b28f055a-81ea-11ed-b70c-a9fe7f7b0e70"},{"full_name":"Shea, J. M.","first_name":"J. M.","last_name":"Shea"}],"issue":"8","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","publication_identifier":{"issn":["2169-897X"],"eissn":["2169-8996"]},"date_published":"2015-04-18T00:00:00Z","type":"journal_article","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Earth and Planetary Sciences (miscellaneous)","Atmospheric Science","Geophysics"],"oa_version":"Published Version","month":"04","publication":"Journal of Geophysical Research: Atmospheres"},{"publication":"Monthly Notices of the Royal Astronomical Society","month":"09","oa_version":"Preprint","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: abundances","galaxies: evolution","galaxies: kinematics and dynamics"],"language":[{"iso":"eng"}],"type":"journal_article","date_published":"2014-09-21T00:00:00Z","oa":1,"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1407.1047"}],"issue":"3","author":[{"first_name":"John P.","last_name":"Stott","full_name":"Stott, John P."},{"full_name":"Sobral, David","first_name":"David","last_name":"Sobral"},{"full_name":"Swinbank, A. M.","last_name":"Swinbank","first_name":"A. M."},{"last_name":"Smail","first_name":"Ian","full_name":"Smail, Ian"},{"last_name":"Bower","first_name":"Richard","full_name":"Bower, Richard"},{"full_name":"Best, Philip N.","first_name":"Philip N.","last_name":"Best"},{"last_name":"Sharples","first_name":"Ray M.","full_name":"Sharples, Ray M."},{"first_name":"James E.","last_name":"Geach","full_name":"Geach, James E."},{"first_name":"Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"}],"scopus_import":"1","_id":"11582","intvolume":"       443","title":"A relationship between specific star formation rate and metallicity gradient within z ∼ 1 galaxies from KMOS-HiZELS","article_processing_charge":"No","date_created":"2022-07-14T12:16:10Z","publication_status":"published","quality_controlled":"1","page":"2695-2704","article_type":"original","publisher":"Oxford University Press","external_id":{"arxiv":["1407.1047"]},"citation":{"ieee":"J. P. Stott <i>et al.</i>, “A relationship between specific star formation rate and metallicity gradient within z ∼ 1 galaxies from KMOS-HiZELS,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 443, no. 3. Oxford University Press, pp. 2695–2704, 2014.","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.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2014. <a href=\"https://doi.org/10.1093/mnras/stu1343\">https://doi.org/10.1093/mnras/stu1343</a>.","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. <i>Monthly Notices of the Royal Astronomical Society</i>. 2014;443(3):2695-2704. doi:<a href=\"https://doi.org/10.1093/mnras/stu1343\">10.1093/mnras/stu1343</a>","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. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stu1343\">https://doi.org/10.1093/mnras/stu1343</a>","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.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 443, no. 3, Oxford University Press, 2014, pp. 2695–704, doi:<a href=\"https://doi.org/10.1093/mnras/stu1343\">10.1093/mnras/stu1343</a>.","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","date_updated":"2022-08-19T08:27:25Z","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"}],"day":"21","arxiv":1,"doi":"10.1093/mnras/stu1343","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."},{"type":"journal_article","date_published":"2014-05-21T00:00:00Z","oa":1,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1402.6697"}],"publication":"Monthly Notices of the Royal Astronomical Society","month":"05","oa_version":"Preprint","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","cosmology: observations","dark ages","reionization","first stars"],"language":[{"iso":"eng"}],"external_id":{"arxiv":["1402.6697"]},"citation":{"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. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stu392\">https://doi.org/10.1093/mnras/stu392</a>","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. <i>Monthly Notices of the Royal Astronomical Society</i>. 2014;440(3):2375-2387. doi:<a href=\"https://doi.org/10.1093/mnras/stu392\">10.1093/mnras/stu392</a>","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.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2014. <a href=\"https://doi.org/10.1093/mnras/stu392\">https://doi.org/10.1093/mnras/stu392</a>.","ieee":"J. J. Matthee <i>et al.</i>, “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,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 440, no. 3. Oxford University Press, pp. 2375–2387, 2014.","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.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 440, no. 3, Oxford University Press, 2014, pp. 2375–87, doi:<a href=\"https://doi.org/10.1093/mnras/stu392\">10.1093/mnras/stu392</a>.","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.","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."},"year":"2014","date_updated":"2022-08-19T08:30:30Z","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"}],"day":"21","arxiv":1,"doi":"10.1093/mnras/stu392","extern":"1","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.","issue":"3","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X"},{"first_name":"David","last_name":"Sobral","full_name":"Sobral, David"},{"last_name":"Swinbank","first_name":"A. M.","full_name":"Swinbank, A. M."},{"full_name":"Smail, Ian","last_name":"Smail","first_name":"Ian"},{"full_name":"Best, P. N.","last_name":"Best","first_name":"P. N."},{"first_name":"Jae-Woo","last_name":"Kim","full_name":"Kim, Jae-Woo"},{"first_name":"Marijn","last_name":"Franx","full_name":"Franx, Marijn"},{"first_name":"Bo","last_name":"Milvang-Jensen","full_name":"Milvang-Jensen, Bo"},{"full_name":"Fynbo, Johan","last_name":"Fynbo","first_name":"Johan"}],"scopus_import":"1","_id":"11583","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","article_processing_charge":"No","date_created":"2022-07-14T12:33:24Z","publication_status":"published","quality_controlled":"1","page":"2375-2387","article_type":"original","publisher":"Oxford University Press"},{"main_file_link":[{"url":"https://arxiv.org/abs/1310.3822","open_access":"1"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"oa":1,"date_published":"2013-12-03T00:00:00Z","type":"journal_article","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution – galaxies","high-redshift – galaxies","starburst"],"oa_version":"Preprint","month":"12","article_number":"139","publication":"The Astrophysical Journal","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.","volume":779,"extern":"1","doi":"10.1088/0004-637x/779/2/139","arxiv":1,"day":"03","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."}],"date_updated":"2022-08-18T10:43:07Z","year":"2013","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.” <i>The Astrophysical Journal</i>, vol. 779, no. 2, 139, IOP Publishing, 2013, doi:<a href=\"https://doi.org/10.1088/0004-637x/779/2/139\">10.1088/0004-637x/779/2/139</a>.","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.” <i>The Astrophysical Journal</i>. IOP Publishing, 2013. <a href=\"https://doi.org/10.1088/0004-637x/779/2/139\">https://doi.org/10.1088/0004-637x/779/2/139</a>.","ieee":"D. Sobral <i>et al.</i>, “The dynamics of z=0.8 H-alpha-selected star-forming galaxies from KMOS/CF-HiZELS,” <i>The Astrophysical Journal</i>, 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. <i>The Astrophysical Journal</i>. 2013;779(2). doi:<a href=\"https://doi.org/10.1088/0004-637x/779/2/139\">10.1088/0004-637x/779/2/139</a>","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. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.1088/0004-637x/779/2/139\">https://doi.org/10.1088/0004-637x/779/2/139</a>"},"external_id":{"arxiv":["1310.3822"]},"publisher":"IOP Publishing","article_type":"original","quality_controlled":"1","publication_status":"published","article_processing_charge":"No","date_created":"2022-07-07T09:14:48Z","title":"The dynamics of z=0.8 H-alpha-selected star-forming galaxies from KMOS/CF-HiZELS","intvolume":"       779","_id":"11520","scopus_import":"1","author":[{"full_name":"Sobral, D.","first_name":"D.","last_name":"Sobral"},{"first_name":"A. M.","last_name":"Swinbank","full_name":"Swinbank, A. M."},{"last_name":"Stott","first_name":"J. P.","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"},{"last_name":"Bower","first_name":"R. G.","full_name":"Bower, R. G."},{"full_name":"Smail, Ian","last_name":"Smail","first_name":"Ian"},{"first_name":"P.","last_name":"Best","full_name":"Best, P."},{"full_name":"Geach, J. E.","first_name":"J. E.","last_name":"Geach"},{"first_name":"R. M.","last_name":"Sharples","full_name":"Sharples, R. M."}],"issue":"2"},{"type":"journal_article","date_published":"2013-04-27T00:00:00Z","publication_identifier":{"issn":["2169-897X"]},"oa":1,"main_file_link":[{"url":"https://doi.org/10.1002/jgrd.50277","open_access":"1"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","publication":"Journal of Geophysical Research: Atmospheres","oa_version":"Published Version","month":"04","keyword":["Space and Planetary Science","Earth and Planetary Sciences (miscellaneous)","Atmospheric Science","Geophysics"],"language":[{"iso":"eng"}],"citation":{"ama":"Juszak I, Pellicciotti F. A comparison of parameterizations of incoming longwave radiation over melting glaciers: Model robustness and seasonal variability. <i>Journal of Geophysical Research: Atmospheres</i>. 2013;118(8):3066-3084. doi:<a href=\"https://doi.org/10.1002/jgrd.50277\">10.1002/jgrd.50277</a>","apa":"Juszak, I., &#38; Pellicciotti, F. (2013). A comparison of parameterizations of incoming longwave radiation over melting glaciers: Model robustness and seasonal variability. <i>Journal of Geophysical Research: Atmospheres</i>. American Geophysical Union. <a href=\"https://doi.org/10.1002/jgrd.50277\">https://doi.org/10.1002/jgrd.50277</a>","ieee":"I. Juszak and F. Pellicciotti, “A comparison of parameterizations of incoming longwave radiation over melting glaciers: Model robustness and seasonal variability,” <i>Journal of Geophysical Research: Atmospheres</i>, vol. 118, no. 8. American Geophysical Union, pp. 3066–3084, 2013.","chicago":"Juszak, I., and Francesca Pellicciotti. “A Comparison of Parameterizations of Incoming Longwave Radiation over Melting Glaciers: Model Robustness and Seasonal Variability.” <i>Journal of Geophysical Research: Atmospheres</i>. American Geophysical Union, 2013. <a href=\"https://doi.org/10.1002/jgrd.50277\">https://doi.org/10.1002/jgrd.50277</a>.","mla":"Juszak, I., and Francesca Pellicciotti. “A Comparison of Parameterizations of Incoming Longwave Radiation over Melting Glaciers: Model Robustness and Seasonal Variability.” <i>Journal of Geophysical Research: Atmospheres</i>, vol. 118, no. 8, American Geophysical Union, 2013, pp. 3066–84, doi:<a href=\"https://doi.org/10.1002/jgrd.50277\">10.1002/jgrd.50277</a>.","short":"I. Juszak, F. Pellicciotti, Journal of Geophysical Research: Atmospheres 118 (2013) 3066–3084.","ista":"Juszak I, Pellicciotti F. 2013. A comparison of parameterizations of incoming longwave radiation over melting glaciers: Model robustness and seasonal variability. Journal of Geophysical Research: Atmospheres. 118(8), 3066–3084."},"year":"2013","date_updated":"2023-02-21T10:10:46Z","day":"27","doi":"10.1002/jgrd.50277","abstract":[{"text":"Parameterizations of incoming longwave radiation are increasingly receiving attention for both low and high elevation glacierized sites. In this paper, we test 13 clear-sky parameterizations combined with seven cloud corrections for all-sky atmospheric emissivity at one location on Haut Glacier d'Arolla. We also analyze the four seasons separately and conduct a cross-validation to test the parameters’ robustness. The best parameterization is the one by Dilley and O'Brien, B for clear-sky conditions combined with Unsworth and Monteith cloud correction. This model is also the most robust when tested in cross-validation. When validated at different sites in the southern Alps of Switzerland and north-western Italian Alps, all parameterizations show a substantial decrease in performance, except for one site, thus suggesting that it is important to recalibrate parameterizations of incoming longwave radiation for different locations. We argue that this is due to differences in the structure of the atmosphere at the sites. We also quantify the effect that the incoming longwave radiation parameterizations have on energy-balance melt modeling, and show that recalibration of model parameters is needed. Using parameters from other sites leads to a significant underestimation of melt and to an error that is larger than that associated with using different parameterizations. Once recalibrated, however, the parameters of most models seem to be stable over seasons and years at the location on Haut Glacier d'Arolla.","lang":"eng"}],"volume":118,"extern":"1","scopus_import":"1","_id":"12643","issue":"8","author":[{"last_name":"Juszak","first_name":"I.","full_name":"Juszak, I."},{"last_name":"Pellicciotti","first_name":"Francesca","full_name":"Pellicciotti, Francesca","id":"b28f055a-81ea-11ed-b70c-a9fe7f7b0e70"}],"date_created":"2023-02-20T08:17:34Z","article_processing_charge":"No","publication_status":"published","intvolume":"       118","title":"A comparison of parameterizations of incoming longwave radiation over melting glaciers: Model robustness and seasonal variability","quality_controlled":"1","page":"3066-3084","publisher":"American Geophysical Union","article_type":"original"},{"article_processing_charge":"No","date_created":"2023-02-20T08:17:57Z","publication_status":"published","intvolume":"       117","title":"Including debris cover effects in a distributed model of glacier ablation","scopus_import":"1","_id":"12648","issue":"D18","author":[{"full_name":"Reid, T. D.","first_name":"T. D.","last_name":"Reid"},{"last_name":"Carenzo","first_name":"M.","full_name":"Carenzo, M."},{"full_name":"Pellicciotti, Francesca","last_name":"Pellicciotti","first_name":"Francesca","id":"b28f055a-81ea-11ed-b70c-a9fe7f7b0e70"},{"first_name":"B. W.","last_name":"Brock","full_name":"Brock, B. W."}],"publisher":"American Geophysical Union","article_type":"original","quality_controlled":"1","day":"27","doi":"10.1029/2012jd017795","abstract":[{"lang":"eng","text":"Distributed glacier melt models generally assume that the glacier surface consists of bare exposed ice and snow. In reality, many glaciers are wholly or partially covered in layers of debris that tend to suppress ablation rates. In this paper, an existing physically based point model for the ablation of debris-covered ice is incorporated in a distributed melt model and applied to Haut Glacier d'Arolla, Switzerland, which has three large patches of debris cover on its surface. The model is based on a 10 m resolution digital elevation model (DEM) of the area; each glacier pixel in the DEM is defined as either bare or debris-covered ice, and may be covered in snow that must be melted off before ice ablation is assumed to occur. Each debris-covered pixel is assigned a debris thickness value using probability distributions based on over 1000 manual thickness measurements. Locally observed meteorological data are used to run energy balance calculations in every pixel, using an approach suitable for snow, bare ice or debris-covered ice as appropriate. The use of the debris model significantly reduces the total ablation in the debris-covered areas, however the precise reduction is sensitive to the temperature extrapolation used in the model distribution because air near the debris surface tends to be slightly warmer than over bare ice. Overall results suggest that the debris patches, which cover 10% of the glacierized area, reduce total runoff from the glacierized part of the basin by up to 7%."}],"year":"2012","citation":{"ista":"Reid TD, Carenzo M, Pellicciotti F, Brock BW. 2012. Including debris cover effects in a distributed model of glacier ablation. Journal of Geophysical Research: Atmospheres. 117(D18), D18105.","mla":"Reid, T. D., et al. “Including Debris Cover Effects in a Distributed Model of Glacier Ablation.” <i>Journal of Geophysical Research: Atmospheres</i>, vol. 117, no. D18, D18105, American Geophysical Union, 2012, doi:<a href=\"https://doi.org/10.1029/2012jd017795\">10.1029/2012jd017795</a>.","short":"T.D. Reid, M. Carenzo, F. Pellicciotti, B.W. Brock, Journal of Geophysical Research: Atmospheres 117 (2012).","ieee":"T. D. Reid, M. Carenzo, F. Pellicciotti, and B. W. Brock, “Including debris cover effects in a distributed model of glacier ablation,” <i>Journal of Geophysical Research: Atmospheres</i>, vol. 117, no. D18. American Geophysical Union, 2012.","chicago":"Reid, T. D., M. Carenzo, Francesca Pellicciotti, and B. W. Brock. “Including Debris Cover Effects in a Distributed Model of Glacier Ablation.” <i>Journal of Geophysical Research: Atmospheres</i>. American Geophysical Union, 2012. <a href=\"https://doi.org/10.1029/2012jd017795\">https://doi.org/10.1029/2012jd017795</a>.","apa":"Reid, T. D., Carenzo, M., Pellicciotti, F., &#38; Brock, B. W. (2012). Including debris cover effects in a distributed model of glacier ablation. <i>Journal of Geophysical Research: Atmospheres</i>. American Geophysical Union. <a href=\"https://doi.org/10.1029/2012jd017795\">https://doi.org/10.1029/2012jd017795</a>","ama":"Reid TD, Carenzo M, Pellicciotti F, Brock BW. Including debris cover effects in a distributed model of glacier ablation. <i>Journal of Geophysical Research: Atmospheres</i>. 2012;117(D18). doi:<a href=\"https://doi.org/10.1029/2012jd017795\">10.1029/2012jd017795</a>"},"date_updated":"2023-02-20T10:57:31Z","volume":117,"extern":"1","oa_version":"Published Version","article_number":"D18105","month":"09","publication":"Journal of Geophysical Research: Atmospheres","keyword":["Paleontology","Space and Planetary Science","Earth and Planetary Sciences (miscellaneous)","Atmospheric Science","Earth-Surface Processes","Geochemistry and Petrology","Soil Science","Water Science and Technology","Ecology","Aquatic Science","Forestry","Oceanography","Geophysics"],"language":[{"iso":"eng"}],"publication_identifier":{"issn":["0148-0227"]},"oa":1,"type":"journal_article","date_published":"2012-09-27T00:00:00Z","main_file_link":[{"url":"https://doi.org/10.1029/2012JD017795","open_access":"1"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public"},{"date_published":"2011-12-16T00:00:00Z","type":"journal_article","oa":1,"publication_identifier":{"issn":["0148-0227"]},"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1029/2011JD01584"}],"publication":"Journal of Geophysical Research: Atmospheres","month":"12","article_number":"D23109","oa_version":"Published Version","language":[{"iso":"eng"}],"keyword":["Paleontology","Space and Planetary Science","Earth and Planetary Sciences (miscellaneous)","Atmospheric Science","Earth-Surface Processes","Geochemistry and Petrology","Soil Science","Water Science and Technology","Ecology","Aquatic Science","Forestry","Oceanography","Geophysics"],"date_updated":"2023-02-20T10:29:44Z","year":"2011","citation":{"ama":"Petersen L, Pellicciotti F. Spatial and temporal variability of air temperature on a melting glacier: Atmospheric controls, extrapolation methods and their effect on melt modeling, Juncal Norte Glacier, Chile. <i>Journal of Geophysical Research: Atmospheres</i>. 2011;116(D23). doi:<a href=\"https://doi.org/10.1029/2011jd015842\">10.1029/2011jd015842</a>","apa":"Petersen, L., &#38; Pellicciotti, F. (2011). Spatial and temporal variability of air temperature on a melting glacier: Atmospheric controls, extrapolation methods and their effect on melt modeling, Juncal Norte Glacier, Chile. <i>Journal of Geophysical Research: Atmospheres</i>. American Geophysical Union. <a href=\"https://doi.org/10.1029/2011jd015842\">https://doi.org/10.1029/2011jd015842</a>","chicago":"Petersen, L., and Francesca Pellicciotti. “Spatial and Temporal Variability of Air Temperature on a Melting Glacier: Atmospheric Controls, Extrapolation Methods and Their Effect on Melt Modeling, Juncal Norte Glacier, Chile.” <i>Journal of Geophysical Research: Atmospheres</i>. American Geophysical Union, 2011. <a href=\"https://doi.org/10.1029/2011jd015842\">https://doi.org/10.1029/2011jd015842</a>.","ieee":"L. Petersen and F. Pellicciotti, “Spatial and temporal variability of air temperature on a melting glacier: Atmospheric controls, extrapolation methods and their effect on melt modeling, Juncal Norte Glacier, Chile,” <i>Journal of Geophysical Research: Atmospheres</i>, vol. 116, no. D23. American Geophysical Union, 2011.","short":"L. Petersen, F. Pellicciotti, Journal of Geophysical Research: Atmospheres 116 (2011).","mla":"Petersen, L., and Francesca Pellicciotti. “Spatial and Temporal Variability of Air Temperature on a Melting Glacier: Atmospheric Controls, Extrapolation Methods and Their Effect on Melt Modeling, Juncal Norte Glacier, Chile.” <i>Journal of Geophysical Research: Atmospheres</i>, vol. 116, no. D23, D23109, American Geophysical Union, 2011, doi:<a href=\"https://doi.org/10.1029/2011jd015842\">10.1029/2011jd015842</a>.","ista":"Petersen L, Pellicciotti F. 2011. Spatial and temporal variability of air temperature on a melting glacier: Atmospheric controls, extrapolation methods and their effect on melt modeling, Juncal Norte Glacier, Chile. Journal of Geophysical Research: Atmospheres. 116(D23), D23109."},"abstract":[{"lang":"eng","text":"Temperature data from three Automatic Weather Stations and twelve Temperature Loggers are used to investigate the spatiotemporal variability of temperature over a glacier, its main atmospheric controls, the suitability of extrapolation techniques and their effect on melt modeling. We use data collected on Juncal Norte Glacier, central Chile, during one ablation season. We examine temporal and spatial variability in lapse rates (LRs), together with alternative statistical interpolation methods. The main control over the glacier thermal regime is the development of a katabatic boundary layer (KBL). Katabatic wind occurs at night and in the morning and is eroded in the afternoon. LRs reveal strong diurnal variability, with steeper LRs during the day when the katabatic wind weakens and shallower LRs during the night and morning. We suggest that temporally variable LRs should be used to account for the observed change. They tend to be steeper than equivalent constant LRs, and therefore result in a reduction in simulated melt compared to use of constant LRs when extrapolating from lower to higher elevations. In addition to the temporal variability, the temperature-elevation relationship varies also in space. Differences are evident between local LRs and including such variability in melt modeling affects melt simulations. Extrapolation methods based on the spatial variability of the observations after removal of the elevation trend, such as Inverse Distance Weighting or Kriging, do not seem necessary for simulations of gridded temperature data over a glacier."}],"doi":"10.1029/2011jd015842","day":"16","extern":"1","volume":116,"author":[{"last_name":"Petersen","first_name":"L.","full_name":"Petersen, L."},{"last_name":"Pellicciotti","first_name":"Francesca","full_name":"Pellicciotti, Francesca","id":"b28f055a-81ea-11ed-b70c-a9fe7f7b0e70"}],"issue":"D23","_id":"12651","scopus_import":"1","title":"Spatial and temporal variability of air temperature on a melting glacier: Atmospheric controls, extrapolation methods and their effect on melt modeling, Juncal Norte Glacier, Chile","intvolume":"       116","publication_status":"published","article_processing_charge":"No","date_created":"2023-02-20T08:18:14Z","quality_controlled":"1","article_type":"original","publisher":"American Geophysical Union"},{"doi":"10.1029/2003jd003973","day":"16","abstract":[{"text":"[1] During the ablation period 2001 a glaciometeorological experiment was carried out on Haut Glacier d'Arolla, Switzerland. Five meteorological stations were installed on the glacier, and one permanent automatic weather station in the glacier foreland. The altitudes of the stations ranged between 2500 and 3000 m a.s.l., and they were in operation from end of May to beginning of September 2001. The spatial arrangement of the stations and temporal duration of the measurements generated a unique data set enabling the analysis of the spatial and temporal variability of the meteorological variables across an alpine glacier. All measurements were taken at a nominal height of 2 m, and hourly averages were derived for the analysis. The wind regime was dominated by the glacier wind (mean value 2.8 m s−1) but due to erosion by the synoptic gradient wind, occasionally the wind would blow up the valley. A slight decrease in mean 2 m air temperatures with altitude was found, however the 2 m air temperature gradient varied greatly and frequently changed its sign. Mean relative humidity was 71% and exhibited limited spatial variation. Mean incoming shortwave radiation and albedo both generally increased with elevation. The different components of shortwave radiation are quantified with a parameterization scheme. Resulting spatial variations are mainly due to horizon obstruction and reflections from surrounding slopes, i.e., topography. The effect of clouds accounts for a loss of 30% of the extraterrestrial flux. Albedos derived from a Landsat TM image of 30 July show remarkably constant values, in the range 0.49 to 0.50, across snow covered parts of the glacier, while albedo is highly spatially variable below the zone of continuous snow cover. These results are verified with ground measurements and compared with parameterized albedo. Mean longwave radiative fluxes decreased with elevation due to lower air temperatures and the effect of upper hemisphere slopes. It is shown through parameterization that this effect would even be more pronounced without the effect of clouds. Results are discussed with respect to a similar study which has been carried out on Pasterze Glacier (Austria). The presented algorithms for interpolating, parameterizing and simulating variables and parameters in alpine regions are integrated in the software package AMUNDSEN which is freely available to be adapted and further developed by the community.","lang":"eng"}],"date_updated":"2023-02-20T08:40:21Z","citation":{"short":"U. Strasser, J. Corripio, F. Pellicciotti, P. Burlando, B. Brock, M. Funk, Journal of Geophysical Research: Atmospheres 109 (2004).","mla":"Strasser, Ulrich, et al. “Spatial and Temporal Variability of Meteorological Variables at Haut Glacier d’Arolla (Switzerland) during the Ablation Season 2001: Measurements and Simulations.” <i>Journal of Geophysical Research: Atmospheres</i>, vol. 109, no. D3, D03103, American Geophysical Union, 2004, doi:<a href=\"https://doi.org/10.1029/2003jd003973\">10.1029/2003jd003973</a>.","ista":"Strasser U, Corripio J, Pellicciotti F, Burlando P, Brock B, Funk M. 2004. Spatial and temporal variability of meteorological variables at Haut Glacier d’Arolla (Switzerland) during the ablation season 2001: Measurements and simulations. Journal of Geophysical Research: Atmospheres. 109(D3), D03103.","ama":"Strasser U, Corripio J, Pellicciotti F, Burlando P, Brock B, Funk M. Spatial and temporal variability of meteorological variables at Haut Glacier d’Arolla (Switzerland) during the ablation season 2001: Measurements and simulations. <i>Journal of Geophysical Research: Atmospheres</i>. 2004;109(D3). doi:<a href=\"https://doi.org/10.1029/2003jd003973\">10.1029/2003jd003973</a>","apa":"Strasser, U., Corripio, J., Pellicciotti, F., Burlando, P., Brock, B., &#38; Funk, M. (2004). Spatial and temporal variability of meteorological variables at Haut Glacier d’Arolla (Switzerland) during the ablation season 2001: Measurements and simulations. <i>Journal of Geophysical Research: Atmospheres</i>. American Geophysical Union. <a href=\"https://doi.org/10.1029/2003jd003973\">https://doi.org/10.1029/2003jd003973</a>","ieee":"U. Strasser, J. Corripio, F. Pellicciotti, P. Burlando, B. Brock, and M. Funk, “Spatial and temporal variability of meteorological variables at Haut Glacier d’Arolla (Switzerland) during the ablation season 2001: Measurements and simulations,” <i>Journal of Geophysical Research: Atmospheres</i>, vol. 109, no. D3. American Geophysical Union, 2004.","chicago":"Strasser, Ulrich, Javier Corripio, Francesca Pellicciotti, Paolo Burlando, Ben Brock, and Martin Funk. “Spatial and Temporal Variability of Meteorological Variables at Haut Glacier d’Arolla (Switzerland) during the Ablation Season 2001: Measurements and Simulations.” <i>Journal of Geophysical Research: Atmospheres</i>. American Geophysical Union, 2004. <a href=\"https://doi.org/10.1029/2003jd003973\">https://doi.org/10.1029/2003jd003973</a>."},"year":"2004","volume":109,"extern":"1","publication_status":"published","article_processing_charge":"No","date_created":"2023-02-20T08:18:57Z","title":"Spatial and temporal variability of meteorological variables at Haut Glacier d'Arolla (Switzerland) during the ablation season 2001: Measurements and simulations","intvolume":"       109","_id":"12658","scopus_import":"1","author":[{"full_name":"Strasser, Ulrich","first_name":"Ulrich","last_name":"Strasser"},{"full_name":"Corripio, Javier","last_name":"Corripio","first_name":"Javier"},{"first_name":"Francesca","last_name":"Pellicciotti","full_name":"Pellicciotti, Francesca","id":"b28f055a-81ea-11ed-b70c-a9fe7f7b0e70"},{"full_name":"Burlando, Paolo","first_name":"Paolo","last_name":"Burlando"},{"full_name":"Brock, Ben","last_name":"Brock","first_name":"Ben"},{"first_name":"Martin","last_name":"Funk","full_name":"Funk, Martin"}],"issue":"D3","publisher":"American Geophysical Union","article_type":"original","quality_controlled":"1","publication_identifier":{"issn":["0148-0227"]},"date_published":"2004-02-16T00:00:00Z","type":"journal_article","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","oa_version":"None","month":"02","article_number":"D03103","publication":"Journal of Geophysical Research: Atmospheres","language":[{"iso":"eng"}],"keyword":["Paleontology","Space and Planetary Science","Earth and Planetary Sciences (miscellaneous)","Atmospheric Science","Earth-Surface Processes","Geochemistry and Petrology","Soil Science","Water Science and Technology","Ecology","Aquatic Science","Forestry","Oceanography","Geophysics"]}]