[{"status":"public","month":"08","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"],"extern":"1","language":[{"iso":"eng"}],"external_id":{"arxiv":["1502.06602"]},"date_published":"2015-08-11T00:00:00Z","type":"journal_article","publisher":"Oxford University Press","issue":"3","quality_controlled":"1","day":"11","page":"2303-2323","publication":"Monthly Notices of the Royal Astronomical Society","date_updated":"2022-08-19T08:23:18Z","intvolume":"       451","arxiv":1,"oa":1,"volume":451,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","author":[{"first_name":"D.","last_name":"Sobral","full_name":"Sobral, D."},{"first_name":"Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J"},{"last_name":"Best","first_name":"P. N.","full_name":"Best, P. N."},{"full_name":"Smail, I.","last_name":"Smail","first_name":"I."},{"full_name":"Khostovan, A. A.","first_name":"A. A.","last_name":"Khostovan"},{"last_name":"Milvang-Jensen","first_name":"B.","full_name":"Milvang-Jensen, B."},{"first_name":"J.-W.","last_name":"Kim","full_name":"Kim, J.-W."},{"last_name":"Stott","first_name":"J.","full_name":"Stott, J."},{"full_name":"Calhau, J.","last_name":"Calhau","first_name":"J."},{"full_name":"Nayyeri, H.","last_name":"Nayyeri","first_name":"H."},{"full_name":"Mobasher, B.","last_name":"Mobasher","first_name":"B."}],"_id":"11580","date_created":"2022-07-14T09:02:22Z","abstract":[{"text":"We present results from the largest contiguous narrow-band survey in the near-infrared. We have used the wide-field infrared camera/Canada–France–Hawaii Telescope and the lowOH2 filter (1.187 ± 0.005 μm) to survey ≈10 deg2 of contiguous extragalactic sky in the SA22 field. A total of ∼6000 candidate emission-line galaxies are found. We use deep ugrizJK data to obtain robust photometric redshifts. We combine our data with the High-redshift(Z) Emission Line Survey (HiZELS), explore spectroscopic surveys (VVDS, VIPERS) and obtain our own spectroscopic follow-up with KMOS, FMOS and MOSFIRE to derive large samples of high-redshift emission-line selected galaxies: 3471 Hα emitters at z = 0.8, 1343 [O III] + Hβ emitters at z = 1.4 and 572 [O II] emitters at z = 2.2. We probe comoving volumes of >106 Mpc3 and find significant overdensities, including an 8.5σ (spectroscopically confirmed) overdensity of Hα emitters at z = 0.81. We derive Hα, [O III] + Hβ and [O II] luminosity functions at z = 0.8, 1.4, 2.2, respectively, and present implications for future surveys such as Euclid. Our uniquely large volumes/areas allow us to subdivide the samples in thousands of randomized combinations of areas and provide a robust empirical measurement of sample/cosmic variance. We show that surveys for star-forming/emission-line galaxies at a depth similar to ours can only overcome cosmic-variance (errors <10 per cent) if they are based on volumes >5 × 105 Mpc3; errors on L* and ϕ* due to sample (cosmic) variance on surveys probing ∼104 and ∼105 Mpc3 are typically very high: ∼300 and ∼40–60 per cent, respectively.","lang":"eng"}],"year":"2015","citation":{"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>.","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>.","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.","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>","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.","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."},"article_processing_charge":"No","oa_version":"Preprint","publication_status":"published","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 ","article_type":"original","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).","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"doi":"10.1093/mnras/stv1076","main_file_link":[{"url":"https://arxiv.org/abs/1502.06602","open_access":"1"}],"scopus_import":"1"},{"page":"400-417","day":"21","quality_controlled":"1","issue":"1","publisher":"Oxford University Press","type":"journal_article","external_id":{"arxiv":["1502.07355"]},"date_published":"2015-07-21T00:00:00Z","language":[{"iso":"eng"}],"extern":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"month":"07","status":"public","scopus_import":"1","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1502.07355"}],"doi":"10.1093/mnras/stv947","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"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)","article_type":"original","publication_status":"published","title":"Identification of the brightest Lyα emitters at z = 6.6: implications for the evolution of the luminosity function in the reionization era","article_processing_charge":"No","oa_version":"Preprint","citation":{"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>","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.","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.","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>.","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.","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>","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>."},"year":"2015","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"}],"date_created":"2022-07-14T11:57:03Z","_id":"11581","author":[{"last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X"},{"first_name":"David","last_name":"Sobral","full_name":"Sobral, David"},{"last_name":"Santos","first_name":"Sérgio","full_name":"Santos, Sérgio"},{"full_name":"Röttgering, Huub","first_name":"Huub","last_name":"Röttgering"},{"first_name":"Behnam","last_name":"Darvish","full_name":"Darvish, Behnam"},{"last_name":"Mobasher","first_name":"Bahram","full_name":"Mobasher, Bahram"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","volume":451,"oa":1,"arxiv":1,"intvolume":"       451","date_updated":"2022-08-19T08:25:25Z","publication":"Monthly Notices of the Royal Astronomical Society"},{"quality_controlled":"1","page":"2695-2704","day":"21","issue":"3","external_id":{"arxiv":["1407.1047"]},"date_published":"2014-09-21T00:00:00Z","type":"journal_article","publisher":"Oxford University Press","month":"09","status":"public","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: abundances","galaxies: evolution","galaxies: kinematics and dynamics"],"extern":"1","title":"A relationship between specific star formation rate and metallicity gradient within z ∼ 1 galaxies from KMOS-HiZELS","publication_status":"published","oa_version":"Preprint","article_processing_charge":"No","doi":"10.1093/mnras/stu1343","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1407.1047"}],"scopus_import":"1","article_type":"original","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"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.","_id":"11582","date_created":"2022-07-14T12:16:10Z","year":"2014","citation":{"chicago":"Stott, John P., David Sobral, A. M. Swinbank, Ian Smail, Richard Bower, Philip N. Best, Ray M. Sharples, James E. Geach, and Jorryt J Matthee. “A Relationship between Specific Star Formation Rate and Metallicity Gradient within z ∼ 1 Galaxies from KMOS-HiZELS.” <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>.","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>","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.","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>.","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>","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.","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."},"abstract":[{"lang":"eng","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."}],"oa":1,"volume":443,"author":[{"first_name":"John P.","last_name":"Stott","full_name":"Stott, John P."},{"full_name":"Sobral, David","last_name":"Sobral","first_name":"David"},{"full_name":"Swinbank, A. M.","first_name":"A. M.","last_name":"Swinbank"},{"full_name":"Smail, Ian","last_name":"Smail","first_name":"Ian"},{"full_name":"Bower, Richard","last_name":"Bower","first_name":"Richard"},{"last_name":"Best","first_name":"Philip N.","full_name":"Best, Philip N."},{"last_name":"Sharples","first_name":"Ray M.","full_name":"Sharples, Ray M."},{"full_name":"Geach, James E.","last_name":"Geach","first_name":"James E."},{"first_name":"Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication":"Monthly Notices of the Royal Astronomical Society","date_updated":"2022-08-19T08:27:25Z","arxiv":1,"intvolume":"       443"},{"intvolume":"       440","arxiv":1,"publication":"Monthly Notices of the Royal Astronomical Society","date_updated":"2022-08-19T08:30:30Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","author":[{"full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J"},{"full_name":"Sobral, David","first_name":"David","last_name":"Sobral"},{"last_name":"Swinbank","first_name":"A. M.","full_name":"Swinbank, A. M."},{"first_name":"Ian","last_name":"Smail","full_name":"Smail, Ian"},{"first_name":"P. N.","last_name":"Best","full_name":"Best, P. N."},{"last_name":"Kim","first_name":"Jae-Woo","full_name":"Kim, Jae-Woo"},{"first_name":"Marijn","last_name":"Franx","full_name":"Franx, Marijn"},{"last_name":"Milvang-Jensen","first_name":"Bo","full_name":"Milvang-Jensen, Bo"},{"last_name":"Fynbo","first_name":"Johan","full_name":"Fynbo, Johan"}],"oa":1,"volume":440,"abstract":[{"lang":"eng","text":"Candidate galaxies at redshifts of z ∼ 10 are now being found in extremely deep surveys, probing very small areas. As a consequence, candidates are very faint, making spectroscopic confirmation practically impossible. In order to overcome such limitations, we have undertaken the CF-HiZELS survey, which is a large-area, medium-depth near-infrared narrow-band survey targeted at z = 8.8 Lyman α (Lyα) emitters (LAEs) and covering 10 deg2 in part of the SSA22 field with the Canada–France–Hawaii Telescope (CFHT). We surveyed a comoving volume of 4.7 × 106 Mpc3 to a Lyα luminosity limit of 6.3 × 1043舁erg舁s−1. We look for Lyα candidates by applying the following criteria: (i) clear emission-line source, (ii) no optical detections (ugriz from CFHTLS), (iii) no visible detection in the optical stack (ugriz > 27), (iv) visually checked reliable NBJ and J detections and (v) J − K ≤ 0. We compute photometric redshifts and remove a significant amount of dusty lower redshift line-emitters at z ∼ 1.4 or 2.2. A total of 13 Lyα candidates were found, of which two are marked as strong candidates, but the majority have very weak constraints on their spectral energy distributions. Using follow-up observations with SINFONI/VLT, we are able to exclude the most robust candidates as LAEs. We put a strong constraint on the Lyα luminosity function at z ∼ 9 and make realistic predictions for ongoing and future surveys. Our results show that surveys for the highest redshift LAEs are susceptible of multiple contaminations and that spectroscopic follow-up is absolutely necessary."}],"year":"2014","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>","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.","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>.","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>.","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>","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.","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."},"_id":"11583","date_created":"2022-07-14T12:33:24Z","article_type":"original","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.","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1402.6697"}],"doi":"10.1093/mnras/stu392","scopus_import":"1","article_processing_charge":"No","oa_version":"Preprint","publication_status":"published","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","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","cosmology: observations","dark ages","reionization","first stars"],"extern":"1","language":[{"iso":"eng"}],"status":"public","month":"05","publisher":"Oxford University Press","external_id":{"arxiv":["1402.6697"]},"date_published":"2014-05-21T00:00:00Z","type":"journal_article","issue":"3","day":"21","page":"2375-2387","quality_controlled":"1"}]