[{"acknowledgement":"We thank the referee for their constructive comments, which have helped improve the quality and clarity of this work. We thank Raffaella Schneider for comments on an earlier version of this paper. We thank Leindert Boogaard, Steven Bos, Rychard Bouwens, and Renske Smit for discussions. J.M. acknowledges the support of a Huygens PhD fellowship from Leiden University. D.S. acknowledges financial support from the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship and from Lancaster University through an Early Career Internal Grant A100679. A.F. acknowledges support from the ERC Advanced Grant INTERSTELLAR H2020/740120. B.D. acknowledges financial support from NASA through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 294.A-5018. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2015.1.00122.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ.","doi":"10.3847/1538-4357/aa9931","language":[{"iso":"eng"}],"day":"21","date_updated":"2022-08-18T10:23:35Z","type":"journal_article","oa_version":"Preprint","article_processing_charge":"No","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","arxiv":1,"publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"scopus_import":"1","date_published":"2017-12-21T00:00:00Z","external_id":{"arxiv":["1709.06569"]},"keyword":["Space and Planetary Science","Astronomy and Astrophysics","dark ages","reionization","first stars – galaxies: formation – galaxies: high-redshift – galaxies: ISM – galaxies: kinematics and dynamics"],"publication_status":"published","abstract":[{"lang":"eng","text":"We present spectroscopic follow-up observations of CR7 with ALMA, targeted at constraining the infrared (IR) continuum and [C II]158 mm line-emission at high spatial resolution matched to the HST/WFC3 imaging. CR7 is a luminous Lyα emitting galaxy at z = 6.6 that consists of three separated UV-continuum components. Our observations reveal several well-separated components of [C II] emission. The two most luminous components in [C II] coincide with the brightest UV components (A and B), blueshifted by »150 km s−1 with respect to the\r\npeak of Lyα emission. Other [C II] components are observed close to UV clumps B and C and are blueshifted by »300 and ≈80 km s−1 with respect to the systemic redshift. We do not detect FIR continuum emission due to dust with a 3σ limiting luminosity LIR T L d 35 K 3.1 10 = <´ 10 ( ) . This allows us to mitigate uncertainties in the dust-corrected SFR and derive SFRs for the three UV clumps A, B, and C of 28, 5, and 7 M yr−1. All clumps have [C II] luminosities consistent within the scatter observed in the local relation between SFR and L[ ] C II , implying that strong Lyα emission does not necessarily anti-correlate with [C II] luminosity. Combining\r\nour measurements with the literature, we show that galaxies with blue UV slopes have weaker [C II] emission at fixed SFR, potentially due to their lower metallicities and/or higher photoionization. Comparison with hydrodynamical simulations suggests that CR7ʼs clumps have metallicities of 0.1 Z Z 0.2 < < . The observed ISM structure of CR7 indicates that we are likely witnessing the build up of a central galaxy in the early universe through complex accretion of satellites."}],"oa":1,"_id":"11518","title":"ALMA reveals metals yet no dust within multiple components in CR7","publication":"The Astrophysical Journal","year":"2017","extern":"1","author":[{"first_name":"Jorryt J","last_name":"Matthee","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"full_name":"Sobral, D.","last_name":"Sobral","first_name":"D."},{"full_name":"Boone, F.","first_name":"F.","last_name":"Boone"},{"last_name":"Röttgering","first_name":"H.","full_name":"Röttgering, H."},{"last_name":"Schaerer","first_name":"D.","full_name":"Schaerer, D."},{"full_name":"Girard, M.","first_name":"M.","last_name":"Girard"},{"full_name":"Pallottini, A.","last_name":"Pallottini","first_name":"A."},{"full_name":"Vallini, L.","last_name":"Vallini","first_name":"L."},{"last_name":"Ferrara","first_name":"A.","full_name":"Ferrara, A."},{"full_name":"Darvish, B.","last_name":"Darvish","first_name":"B."},{"full_name":"Mobasher, B.","last_name":"Mobasher","first_name":"B."}],"quality_controlled":"1","citation":{"mla":"Matthee, Jorryt J., et al. “ALMA Reveals Metals yet No Dust within Multiple Components in CR7.” <i>The Astrophysical Journal</i>, vol. 851, no. 2, 145, IOP Publishing, 2017, doi:<a href=\"https://doi.org/10.3847/1538-4357/aa9931\">10.3847/1538-4357/aa9931</a>.","apa":"Matthee, J. J., Sobral, D., Boone, F., Röttgering, H., Schaerer, D., Girard, M., … Mobasher, B. (2017). ALMA reveals metals yet no dust within multiple components in CR7. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/aa9931\">https://doi.org/10.3847/1538-4357/aa9931</a>","chicago":"Matthee, Jorryt J, D. Sobral, F. Boone, H. Röttgering, D. Schaerer, M. Girard, A. Pallottini, et al. “ALMA Reveals Metals yet No Dust within Multiple Components in CR7.” <i>The Astrophysical Journal</i>. IOP Publishing, 2017. <a href=\"https://doi.org/10.3847/1538-4357/aa9931\">https://doi.org/10.3847/1538-4357/aa9931</a>.","short":"J.J. Matthee, D. Sobral, F. Boone, H. Röttgering, D. Schaerer, M. Girard, A. Pallottini, L. Vallini, A. Ferrara, B. Darvish, B. Mobasher, The Astrophysical Journal 851 (2017).","ista":"Matthee JJ, Sobral D, Boone F, Röttgering H, Schaerer D, Girard M, Pallottini A, Vallini L, Ferrara A, Darvish B, Mobasher B. 2017. ALMA reveals metals yet no dust within multiple components in CR7. The Astrophysical Journal. 851(2), 145.","ieee":"J. J. Matthee <i>et al.</i>, “ALMA reveals metals yet no dust within multiple components in CR7,” <i>The Astrophysical Journal</i>, vol. 851, no. 2. IOP Publishing, 2017.","ama":"Matthee JJ, Sobral D, Boone F, et al. ALMA reveals metals yet no dust within multiple components in CR7. <i>The Astrophysical Journal</i>. 2017;851(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/aa9931\">10.3847/1538-4357/aa9931</a>"},"main_file_link":[{"url":"https://arxiv.org/abs/1709.06569","open_access":"1"}],"status":"public","article_number":"145","date_created":"2022-07-07T08:48:04Z","month":"12","intvolume":"       851","article_type":"original","publisher":"IOP Publishing","issue":"2","volume":851},{"title":"Evidence for PopIII-like stellar populations in the most luminous Lyα emitters at the epoch of reionisation: Spectroscopic confirmation","publication":"The Astrophysical Journal","_id":"11519","oa":1,"abstract":[{"lang":"eng","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."}],"publication_status":"published","citation":{"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.","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>","short":"D. Sobral, J.J. Matthee, B. Darvish, D. Schaerer, B. Mobasher, H. Röttgering, S. Santos, S. Hemmati, The Astrophysical Journal 808 (2015) 139.","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>.","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>.","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>"},"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1504.01734"}],"author":[{"last_name":"Sobral","first_name":"David","full_name":"Sobral, David"},{"last_name":"Matthee","first_name":"Jorryt J","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"full_name":"Darvish, Behnam","last_name":"Darvish","first_name":"Behnam"},{"full_name":"Schaerer, Daniel","last_name":"Schaerer","first_name":"Daniel"},{"last_name":"Mobasher","first_name":"Bahram","full_name":"Mobasher, Bahram"},{"first_name":"Huub","last_name":"Röttgering","full_name":"Röttgering, Huub"},{"full_name":"Santos, Sérgio","first_name":"Sérgio","last_name":"Santos"},{"full_name":"Hemmati, Shoubaneh","first_name":"Shoubaneh","last_name":"Hemmati"}],"extern":"1","quality_controlled":"1","year":"2015","intvolume":"       808","month":"07","date_created":"2022-07-07T09:00:58Z","status":"public","issue":"2","volume":808,"publisher":"IOP Publishing","article_type":"original","doi":"10.1088/0004-637X/808/2/139","language":[{"iso":"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.","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","article_processing_charge":"No","oa_version":"Preprint","date_updated":"2022-08-18T10:30:13Z","type":"journal_article","day":"28","scopus_import":"1","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"arxiv":1,"keyword":["Space and Planetary Science","Astronomy and Astrophysics","dark ages","reionization","first stars – early universe – galaxies: evolution"],"external_id":{"arxiv":["1504.01734"]},"date_published":"2015-07-28T00:00:00Z","page":"139"},{"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.","doi":"10.1088/0004-637x/779/2/139","language":[{"iso":"eng"}],"date_updated":"2022-08-18T10:43:07Z","type":"journal_article","oa_version":"Preprint","day":"03","article_processing_charge":"No","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","arxiv":1,"publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"scopus_import":"1","date_published":"2013-12-03T00:00:00Z","external_id":{"arxiv":["1310.3822"]},"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution – galaxies","high-redshift – galaxies","starburst"],"publication_status":"published","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."}],"title":"The dynamics of z=0.8 H-alpha-selected star-forming galaxies from KMOS/CF-HiZELS","publication":"The Astrophysical Journal","oa":1,"_id":"11520","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.","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>.","short":"D. Sobral, A.M. Swinbank, J.P. Stott, J.J. Matthee, R.G. Bower, I. Smail, P. Best, J.E. Geach, R.M. Sharples, The Astrophysical Journal 779 (2013).","ieee":"D. Sobral <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>","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>."},"main_file_link":[{"url":"https://arxiv.org/abs/1310.3822","open_access":"1"}],"author":[{"full_name":"Sobral, D.","first_name":"D.","last_name":"Sobral"},{"first_name":"A. M.","last_name":"Swinbank","full_name":"Swinbank, A. M."},{"full_name":"Stott, J. P.","last_name":"Stott","first_name":"J. P."},{"orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","first_name":"Jorryt J"},{"full_name":"Bower, R. G.","last_name":"Bower","first_name":"R. G."},{"full_name":"Smail, Ian","last_name":"Smail","first_name":"Ian"},{"full_name":"Best, P.","first_name":"P.","last_name":"Best"},{"first_name":"J. E.","last_name":"Geach","full_name":"Geach, J. E."},{"last_name":"Sharples","first_name":"R. M.","full_name":"Sharples, R. M."}],"quality_controlled":"1","extern":"1","date_created":"2022-07-07T09:14:48Z","month":"12","status":"public","article_number":"139","intvolume":"       779","publisher":"IOP Publishing","article_type":"original","volume":779,"issue":"2"}]