[{"publication_status":"published","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1702.04721"}],"oa":1,"volume":471,"arxiv":1,"issue":"1","article_processing_charge":"No","abstract":[{"lang":"eng","text":"We present a sample of ∼1000 emission-line galaxies at z = 0.4–4.7 from the ∼0.7deg2 High-z Emission-Line Survey in the Boötes field identified with a suite of six narrow-band filters at ≈0.4–2.1 μm. These galaxies have been selected on their Ly α (73), [O II] (285), H β/[O III] (387) or H α (362) emission line, and have been classified with optical to near-infrared colours. A subsample of 98 sources have reliable redshifts from multiple narrow-band (e.g. [O II]–H α) detections and/or spectroscopy. In this survey paper, we present the observations, selection and catalogues of emitters. We measure number densities of Ly α, [O II], H β/[O III] and H α and confirm strong luminosity evolution in star-forming galaxies from z ∼ 0.4 to ∼5, in agreement with previous results. To demonstrate the usefulness of dual-line emitters, we use the sample of dual [O II]–H α emitters to measure the observed [O II]/H α ratio at z = 1.47. The observed [O II]/H α ratio increases significantly from 0.40 ± 0.01 at z = 0.1 to 0.52 ± 0.05 at z = 1.47, which we attribute to either decreasing dust attenuation with redshift, or due to a bias in the (typically) fibre measurements in the local Universe that only measure the central kpc regions. At the bright end, we find that both the H α and Ly α number densities at z ≈ 2.2 deviate significantly from a Schechter form, following a power law. We show that this is driven entirely by an increasing X-ray/active galactic nucleus fraction with line luminosity, which reaches ≈100 per cent at line luminosities L ≳ 3 × 1044 erg s−1."}],"_id":"11561","date_published":"2017-10-01T00:00:00Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2022-08-19T07:15:14Z","scopus_import":"1","external_id":{"arxiv":["1702.04721"]},"publication_identifier":{"issn":["0035-8711","1365-2966"]},"article_type":"original","year":"2017","oa_version":"Preprint","publisher":"Oxford University Press","quality_controlled":"1","publication":"Monthly Notices of the Royal Astronomical Society","intvolume":"       471","status":"public","page":"629-649","extern":"1","month":"10","date_created":"2022-07-12T11:01:35Z","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics galaxies","active","galaxies","evolution","galaxies","high-redshift","galaxies","luminosity function","mass function","galaxies: star formation"],"doi":"10.1093/mnras/stx1569","citation":{"mla":"Matthee, Jorryt J., et al. “Boötes-HiZELS: An Optical to near-Infrared Survey of Emission-Line Galaxies at z = 0.4–4.7.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 471, no. 1, Oxford University Press, 2017, pp. 629–49, doi:<a href=\"https://doi.org/10.1093/mnras/stx1569\">10.1093/mnras/stx1569</a>.","chicago":"Matthee, Jorryt J, David Sobral, Philip Best, Ian Smail, Fuyan Bian, Behnam Darvish, Huub Röttgering, and Xiaohui Fan. “Boötes-HiZELS: An Optical to near-Infrared Survey of Emission-Line Galaxies at z = 0.4–4.7.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stx1569\">https://doi.org/10.1093/mnras/stx1569</a>.","ista":"Matthee JJ, Sobral D, Best P, Smail I, Bian F, Darvish B, Röttgering H, Fan X. 2017. Boötes-HiZELS: An optical to near-infrared survey of emission-line galaxies at z = 0.4–4.7. Monthly Notices of the Royal Astronomical Society. 471(1), 629–649.","ieee":"J. J. Matthee <i>et al.</i>, “Boötes-HiZELS: An optical to near-infrared survey of emission-line galaxies at z = 0.4–4.7,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 471, no. 1. Oxford University Press, pp. 629–649, 2017.","ama":"Matthee JJ, Sobral D, Best P, et al. Boötes-HiZELS: An optical to near-infrared survey of emission-line galaxies at z = 0.4–4.7. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;471(1):629-649. doi:<a href=\"https://doi.org/10.1093/mnras/stx1569\">10.1093/mnras/stx1569</a>","apa":"Matthee, J. J., Sobral, D., Best, P., Smail, I., Bian, F., Darvish, B., … Fan, X. (2017). Boötes-HiZELS: An optical to near-infrared survey of emission-line galaxies at z = 0.4–4.7. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stx1569\">https://doi.org/10.1093/mnras/stx1569</a>","short":"J.J. Matthee, D. Sobral, P. Best, I. Smail, F. Bian, B. Darvish, H. Röttgering, X. Fan, Monthly Notices of the Royal Astronomical Society 471 (2017) 629–649."},"title":"Boötes-HiZELS: An optical to near-infrared survey of emission-line galaxies at z = 0.4–4.7","day":"01","author":[{"last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"full_name":"Sobral, David","first_name":"David","last_name":"Sobral"},{"first_name":"Philip","full_name":"Best, Philip","last_name":"Best"},{"full_name":"Smail, Ian","first_name":"Ian","last_name":"Smail"},{"last_name":"Bian","full_name":"Bian, Fuyan","first_name":"Fuyan"},{"last_name":"Darvish","full_name":"Darvish, Behnam","first_name":"Behnam"},{"last_name":"Röttgering","full_name":"Röttgering, Huub","first_name":"Huub"},{"last_name":"Fan","first_name":"Xiaohui","full_name":"Fan, Xiaohui"}],"type":"journal_article"},{"abstract":[{"lang":"eng","text":"We present the CAlibrating LYMan-α with Hα (CALYMHA) pilot survey and new results on Lyman α (Lyα) selected galaxies at z ∼ 2. We use a custom-built Lyα narrow-band filter at the Isaac Newton Telescope, designed to provide a matched volume coverage to the z = 2.23 Hα HiZELS survey. Here, we present the first results for the COSMOS and UDS fields. Our survey currently reaches a 3σ line flux limit of ∼4 × 10−17 erg s−1 cm−2, and a Lyα luminosity limit of ∼1042.3 erg s−1. We find 188 Lyα emitters over 7.3 × 105 Mpc3, but also find significant numbers of other line-emitting sources corresponding to He II, C III] and C IV emission lines. These sources are important contaminants, and we carefully remove them, unlike most previous studies. We find that the Lyα luminosity function at z = 2.23 is very well described by a Schechter function up to LLy α ≈ 1043 erg s−1 with L∗=1042.59+0.16−0.08 erg s−1, ϕ∗=10−3.09+0.14−0.34 Mpc−3 and α = −1.75 ± 0.25. Above LLy α ≈ 1043 erg s−1, the Lyα luminosity function becomes power-law like, driven by X-ray AGN. We find that Lyα-selected emitters have a high escape fraction of 37 ± 7 per cent, anticorrelated with Lyα luminosity and correlated with Lyα equivalent width. Lyα emitters have ubiquitous large (≈40 kpc) Lyα haloes, ∼2 times larger than their Hα extents. By directly comparing our Lyα and Hα luminosity functions, we find that the global/overall escape fraction of Lyα photons (within a 13 kpc radius) from the full population of star-forming galaxies is 5.1 ± 0.2 per cent at the peak of the star formation history. An extra 3.3 ± 0.3 per cent of Lyα photons likely still escape, but at larger radii."}],"_id":"11562","date_published":"2017-04-01T00:00:00Z","article_processing_charge":"No","issue":"1","arxiv":1,"volume":466,"main_file_link":[{"url":"https://arxiv.org/abs/1609.05897","open_access":"1"}],"oa":1,"publication_status":"published","year":"2017","oa_version":"Preprint","article_type":"original","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"scopus_import":"1","external_id":{"arxiv":["1609.05897"]},"date_updated":"2022-08-19T07:18:20Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_created":"2022-07-12T12:04:16Z","month":"04","extern":"1","page":"1242-1258","status":"public","intvolume":"       466","publication":"Monthly Notices of the Royal Astronomical Society","quality_controlled":"1","publisher":"Oxford University Press","type":"journal_article","author":[{"last_name":"Sobral","first_name":"David","full_name":"Sobral, David"},{"orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","last_name":"Matthee"},{"last_name":"Best","first_name":"Philip","full_name":"Best, Philip"},{"last_name":"Stroe","first_name":"Andra","full_name":"Stroe, Andra"},{"last_name":"Röttgering","full_name":"Röttgering, Huub","first_name":"Huub"},{"last_name":"Oteo","full_name":"Oteo, Iván","first_name":"Iván"},{"full_name":"Smail, Ian","first_name":"Ian","last_name":"Smail"},{"full_name":"Morabito, Leah","first_name":"Leah","last_name":"Morabito"},{"first_name":"Ana","full_name":"Paulino-Afonso, Ana","last_name":"Paulino-Afonso"}],"day":"01","title":"The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23","citation":{"mla":"Sobral, David, et al. “The CALYMHA Survey: Lyα Luminosity Function and Global Escape Fraction of Lyα Photons at z = 2.23.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 466, no. 1, Oxford University Press, 2017, pp. 1242–58, doi:<a href=\"https://doi.org/10.1093/mnras/stw3090\">10.1093/mnras/stw3090</a>.","chicago":"Sobral, David, Jorryt J Matthee, Philip Best, Andra Stroe, Huub Röttgering, Iván Oteo, Ian Smail, Leah Morabito, and Ana Paulino-Afonso. “The CALYMHA Survey: Lyα Luminosity Function and Global Escape Fraction of Lyα Photons at z = 2.23.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stw3090\">https://doi.org/10.1093/mnras/stw3090</a>.","ieee":"D. Sobral <i>et al.</i>, “The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 466, no. 1. Oxford University Press, pp. 1242–1258, 2017.","ista":"Sobral D, Matthee JJ, Best P, Stroe A, Röttgering H, Oteo I, Smail I, Morabito L, Paulino-Afonso A. 2017. The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23. Monthly Notices of the Royal Astronomical Society. 466(1), 1242–1258.","ama":"Sobral D, Matthee JJ, Best P, et al. The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;466(1):1242-1258. doi:<a href=\"https://doi.org/10.1093/mnras/stw3090\">10.1093/mnras/stw3090</a>","apa":"Sobral, D., Matthee, J. J., Best, P., Stroe, A., Röttgering, H., Oteo, I., … Paulino-Afonso, A. (2017). The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stw3090\">https://doi.org/10.1093/mnras/stw3090</a>","short":"D. Sobral, J.J. Matthee, P. Best, A. Stroe, H. Röttgering, I. Oteo, I. Smail, L. Morabito, A. Paulino-Afonso, Monthly Notices of the Royal Astronomical Society 466 (2017) 1242–1258."},"doi":"10.1093/mnras/stw3090","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: haloes","galaxies: high-redshift","galaxies: luminosity function","mass function","galaxies: statistics","cosmology: observations"],"language":[{"iso":"eng"}],"acknowledgement":"We thank the reviewer for his/her helpful comments and suggestions that have greatly improved this work. DS and JM acknowledge financial support from the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship. DS also acknowledges funding from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010). PNB is grateful for support from the UK STFC via grant ST/M001229/1. IRS acknowledges support from STFC (ST/L00075X/1), the ERC Advanced Investigator programme DUSTYGAL 321334 and a Royal Society/Wolfson merit award. We thank Matthew Hayes, Ryan Trainor, Kimihiko Nakajima and Anne Verhamme for many helpful discussions and Ana Sobral, Carolina Duarte and Miguel Domingos for taking part in observations with the NB392 filter. We also thank Sergio Santos for helpful comments. This research is based on observations obtained on the Isaac Newton Telescope (INT), programs: I13AN002, I14AN002, 088-INT7/14A, I14BN006, 118-INT13/14B & I15AN008. The authors acknowledge the award of time from programmes: I13AN002, I14AN002, 088-INT7/14A, I14BN006, 118-INT13/14B, I15AN008 on the INT. INT is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 098.A 0819. We have benefited greatly from the publicly available programming language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY and ASTROPY packages, the astronomical imaging tools SEXTRACTOR, SWARP (Bertin & Arnouts 1996; Bertin 2010), SCAMP (Bertin 2006) and TOPCAT (Taylor 2005). Dedicated to the memory of M. L. Nicolau and M. C. Serrano."},{"title":"The production and escape of Lyman-Continuum radiation from star-forming galaxies at z ∼ 2 and their redshift evolution","citation":{"ama":"Matthee JJ, Sobral D, Best P, et al. The production and escape of Lyman-Continuum radiation from star-forming galaxies at z ∼ 2 and their redshift evolution. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;465(3):3637-3655. doi:<a href=\"https://doi.org/10.1093/mnras/stw2973\">10.1093/mnras/stw2973</a>","apa":"Matthee, J. J., Sobral, D., Best, P., Khostovan, A. A., Oteo, I., Bouwens, R., &#38; Röttgering, H. (2017). The production and escape of Lyman-Continuum radiation from star-forming galaxies at z ∼ 2 and their redshift evolution. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stw2973\">https://doi.org/10.1093/mnras/stw2973</a>","short":"J.J. Matthee, D. Sobral, P. Best, A.A. Khostovan, I. Oteo, R. Bouwens, H. Röttgering, Monthly Notices of the Royal Astronomical Society 465 (2017) 3637–3655.","mla":"Matthee, Jorryt J., et al. “The Production and Escape of Lyman-Continuum Radiation from Star-Forming Galaxies at z ∼ 2 and Their Redshift Evolution.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 465, no. 3, Oxford University Press, 2017, pp. 3637–55, doi:<a href=\"https://doi.org/10.1093/mnras/stw2973\">10.1093/mnras/stw2973</a>.","chicago":"Matthee, Jorryt J, David Sobral, Philip Best, Ali Ahmad Khostovan, Iván Oteo, Rychard Bouwens, and Huub Röttgering. “The Production and Escape of Lyman-Continuum Radiation from Star-Forming Galaxies at z ∼ 2 and Their Redshift Evolution.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stw2973\">https://doi.org/10.1093/mnras/stw2973</a>.","ieee":"J. J. Matthee <i>et al.</i>, “The production and escape of Lyman-Continuum radiation from star-forming galaxies at z ∼ 2 and their redshift evolution,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 465, no. 3. Oxford University Press, pp. 3637–3655, 2017.","ista":"Matthee JJ, Sobral D, Best P, Khostovan AA, Oteo I, Bouwens R, Röttgering H. 2017. The production and escape of Lyman-Continuum radiation from star-forming galaxies at z ∼ 2 and their redshift evolution. Monthly Notices of the Royal Astronomical Society. 465(3), 3637–3655."},"type":"journal_article","author":[{"orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","full_name":"Matthee, Jorryt J","first_name":"Jorryt J"},{"first_name":"David","full_name":"Sobral, David","last_name":"Sobral"},{"first_name":"Philip","full_name":"Best, Philip","last_name":"Best"},{"last_name":"Khostovan","first_name":"Ali Ahmad","full_name":"Khostovan, Ali Ahmad"},{"last_name":"Oteo","full_name":"Oteo, Iván","first_name":"Iván"},{"first_name":"Rychard","full_name":"Bouwens, Rychard","last_name":"Bouwens"},{"last_name":"Röttgering","full_name":"Röttgering, Huub","first_name":"Huub"}],"day":"01","acknowledgement":"We thank the referee for the many helpful and constructive comments which have significantly improved this paper. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. DS acknowledges financial support from the Netherlands Organization for Scientific research (NWO) through a Veni fellowship and from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010). PNB is grateful for support from the UK STFC via grant ST/M001229/1. IO acknowledges support from the European Research Council in the form of the Advanced Investigator Programme, 321302, COSMICISM. The authors thank Andreas Faisst, Michael Rutkowski and Andreas Sandberg for answering questions related to this work and Daniel Schaerer and Mark Dijkstra for discussions. We acknowledge the work that has been done by both the COSMOS team in assembling such large, state-of-the-art multi-wavelength data set, as this has been crucial for the results presented in this paper. We have benefited greatly from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY (Jones et al. 2001; Hunter 2007; Van Der Walt, Colbert & Varoquaux 2011) and ASTROPY (Astropy Collaboration et al. 2013) packages, the astronomical imaging tools SEXTRACTOR and SWARP (Bertin & Arnouts 1996;\r\nBertin 2010) and the TOPCAT analysis program (Taylor 2013).","doi":"10.1093/mnras/stw2973","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","cosmology: observations","dark ages","reionization","first stars"],"page":"3637-3655","date_created":"2022-07-12T12:12:14Z","extern":"1","month":"03","publisher":"Oxford University Press","intvolume":"       465","status":"public","quality_controlled":"1","publication":"Monthly Notices of the Royal Astronomical Society","year":"2017","oa_version":"Preprint","article_type":"original","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"date_updated":"2022-08-19T07:53:04Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","scopus_import":"1","external_id":{"arxiv":["1605.08782"]},"issue":"3","article_processing_charge":"No","arxiv":1,"date_published":"2017-03-01T00:00:00Z","_id":"11564","abstract":[{"lang":"eng","text":"We study the production rate of ionizing photons of a sample of 588 Hα emitters (HAEs) and 160 Lyman-α emitters (LAEs) at z = 2.2 in the COSMOS field in order to assess the implied emissivity from galaxies, based on their ultraviolet (UV) luminosity. By exploring the rest-frame Lyman Continuum (LyC) with GALEX/NUV data, we find fesc < 2.8 (6.4) per cent through median (mean) stacking. By combining the Hα luminosity density with intergalactic medium emissivity measurements from absorption studies, we find a globally averaged 〈fesc〉 of 5.9+14.5−4.2 per cent at z = 2.2 if we assume HAEs are the only source of ionizing photons. We find similarly low values of the global 〈fesc〉 at z ≈ 3–5, also ruling out a high 〈fesc〉 at z < 5. These low escape fractions allow us to measure ξion, the number of produced ionizing photons per unit UV luminosity, and investigate how this depends on galaxy properties. We find a typical ξion ≈ 1024.77 ± 0.04 Hz erg−1 for HAEs and ξion ≈ 1025.14 ± 0.09 Hz erg−1 for LAEs. LAEs and low-mass HAEs at z = 2.2 show similar values of ξion as typically assumed in the reionization era, while the typical HAE is three times less ionizing. Due to an increasing ξion with increasing EW(Hα), ξion likely increases with redshift. This evolution alone is fully in line with the observed evolution of ξion between z ≈ 2 and 5, indicating a typical value of ξion ≈ 1025.4 Hz erg−1 in the reionization era."}],"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1605.08782"}],"oa":1,"publication_status":"published","volume":465},{"article_type":"original","oa_version":"Preprint","year":"2017","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2022-08-19T07:56:07Z","external_id":{"arxiv":["1608.08218"]},"scopus_import":"1","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"arxiv":1,"issue":"2","article_processing_charge":"No","abstract":[{"lang":"eng","text":"We use the hydrodynamical EAGLE simulation to study the magnitude and origin of the scatter in the stellar mass–halo mass relation for central galaxies. We separate cause and effect by correlating stellar masses in the baryonic simulation with halo properties in a matched dark matter only (DMO) simulation. The scatter in stellar mass increases with redshift and decreases with halo mass. At z = 0.1, it declines from 0.25 dex at M200, DMO ≈ 1011 M⊙ to 0.12 dex at M200, DMO ≈ 1013 M⊙, but the trend is weak above 1012 M⊙. For M200, DMO < 1012.5 M⊙ up to 0.04 dex of the scatter is due to scatter in the halo concentration. At fixed halo mass, a larger stellar mass corresponds to a more concentrated halo. This is likely because higher concentrations imply earlier formation times and hence more time for accretion and star formation, and/or because feedback is less efficient in haloes with higher binding energies. The maximum circular velocity, Vmax, DMO, and binding energy are therefore more fundamental properties than halo mass, meaning that they are more accurate predictors of stellar mass, and we provide fitting formulae for their relations with stellar mass. However, concentration alone cannot explain the total scatter in the Mstar−M200,DMO relation, and it does not explain the scatter in Mstar–Vmax, DMO. Halo spin, sphericity, triaxiality, substructure and environment are also not responsible for the remaining scatter, which thus could be due to more complex halo properties or non-linear/stochastic baryonic effects."}],"_id":"11565","date_published":"2017-02-01T00:00:00Z","publication_status":"published","main_file_link":[{"url":"https://arxiv.org/abs/1608.08218","open_access":"1"}],"oa":1,"volume":465,"citation":{"ieee":"J. J. Matthee, J. Schaye, R. A. Crain, M. Schaller, R. Bower, and T. Theuns, “The origin of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE simulation,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 465, no. 2. Oxford University Press, pp. 2381–2396, 2017.","ista":"Matthee JJ, Schaye J, Crain RA, Schaller M, Bower R, Theuns T. 2017. The origin of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE simulation. Monthly Notices of the Royal Astronomical Society. 465(2), 2381–2396.","chicago":"Matthee, Jorryt J, Joop Schaye, Robert A. Crain, Matthieu Schaller, Richard Bower, and Tom Theuns. “The Origin of Scatter in the Stellar Mass–Halo Mass Relation of Central Galaxies in the EAGLE Simulation.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stw2884\">https://doi.org/10.1093/mnras/stw2884</a>.","mla":"Matthee, Jorryt J., et al. “The Origin of Scatter in the Stellar Mass–Halo Mass Relation of Central Galaxies in the EAGLE Simulation.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 465, no. 2, Oxford University Press, 2017, pp. 2381–96, doi:<a href=\"https://doi.org/10.1093/mnras/stw2884\">10.1093/mnras/stw2884</a>.","short":"J.J. Matthee, J. Schaye, R.A. Crain, M. Schaller, R. Bower, T. Theuns, Monthly Notices of the Royal Astronomical Society 465 (2017) 2381–2396.","apa":"Matthee, J. J., Schaye, J., Crain, R. A., Schaller, M., Bower, R., &#38; Theuns, T. (2017). The origin of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE simulation. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stw2884\">https://doi.org/10.1093/mnras/stw2884</a>","ama":"Matthee JJ, Schaye J, Crain RA, Schaller M, Bower R, Theuns T. The origin of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE simulation. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;465(2):2381-2396. doi:<a href=\"https://doi.org/10.1093/mnras/stw2884\">10.1093/mnras/stw2884</a>"},"title":"The origin of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE simulation","day":"01","type":"journal_article","author":[{"orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","full_name":"Matthee, Jorryt J","first_name":"Jorryt J"},{"last_name":"Schaye","full_name":"Schaye, Joop","first_name":"Joop"},{"full_name":"Crain, Robert A.","first_name":"Robert A.","last_name":"Crain"},{"full_name":"Schaller, Matthieu","first_name":"Matthieu","last_name":"Schaller"},{"last_name":"Bower","first_name":"Richard","full_name":"Bower, Richard"},{"last_name":"Theuns","first_name":"Tom","full_name":"Theuns, Tom"}],"acknowledgement":"We thank the anonymous referee for their comments. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. JM thanks David Sobral for useful discussions and help with fitting routines and Jonas Chavez Montero and Ying Zu for providing data. We thank PRACE for the access to the Curie facility in France. We have used the DiRAC system which is a part of National E-Infrastructure at Durham University, operated by the Institute for Computational Cosmology on behalf of the STFC DiRAC HPC Facility (www.dirac.ac.uk); the equipment was funded by BIS National E-infrastructure capital grant ST/K00042X/1, STFC capital grant ST/H008519/1, STFC DiRAC Operations grant ST/K003267/1 and Durham University. The study was sponsored by the Dutch National Computing Facilities Foundation (NCF) for the use of supercomputer facilities, with financial support from the Netherlands Organisation for Scientific Research (NWO), through VICI grant 639.043.409, and the European Research Council under the European Union’s Seventh Framework Programme (FP7/2007-2013)/ERC Grant agreement 278594- GasAroundGalaxies, and from the Belgian Science Policy Office ([AP P7/08 CHARM]). We have benefited greatly from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY, H5PY and RPY2 packages, and the TOPCAT analysis program (Taylor 2005).","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: formation","galaxies: haloes","cosmology: theory"],"doi":"10.1093/mnras/stw2884","page":"2381-2396","extern":"1","month":"02","date_created":"2022-07-12T12:25:08Z","publisher":"Oxford University Press","quality_controlled":"1","publication":"Monthly Notices of the Royal Astronomical Society","status":"public","intvolume":"       465"},{"oa_version":"Preprint","year":"2017","article_type":"original","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"external_id":{"arxiv":["1703.10169"]},"scopus_import":"1","date_updated":"2022-08-19T07:59:57Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","abstract":[{"text":"While traditionally associated with active galactic nuclei (AGN), the properties of the C II] (λ = 2326 Å), C III] (λ, λ = 1907, 1909 Å) and C IV (λ, λ = 1549, 1551 Å) emission lines are still uncertain as large, unbiased samples of sources are scarce. We present the first blind, statistical study of C II], C III] and C IV emitters at z ∼ 0.68, 1.05, 1.53, respectively, uniformly selected down to a flux limit of ∼4 × 10−17 erg s−1 cm−1 through a narrow-band survey covering an area of ∼1.4 deg2 over COSMOS and UDS. We detect 16 C II], 35 C III] and 17 C IV emitters, whose nature we investigate using optical colours as well as Hubble Space Telescope (HST), X-ray, radio and far-infrared data. We find that z ∼ 0.7 C II] emitters are consistent with a mixture of blue (UV slope β = −2.0 ± 0.4) star-forming (SF) galaxies with discy HST structure and AGN with Seyfert-like morphologies. Bright C II] emitters have individual X-ray detections as well as high average black hole accretion rates (BHARs) of ∼0.1 M⊙ yr−1. C III] emitters at z ∼ 1.05 trace a general population of SF galaxies, with β = −0.8 ± 1.1, a variety of optical morphologies, including isolated and interacting galaxies and low BHAR (<0.02 M⊙ yr−1). Our C IV emitters at z ∼ 1.5 are consistent with young, blue quasars (β ∼ −1.9) with point-like optical morphologies, bright X-ray counterparts and large BHAR (0.8  M⊙ yr−1). We also find some surprising C II], C III] and C IV emitters with rest-frame equivalent widths (EWs) that could be as large as 50–100 Å. AGN or spatial offsets between the UV continuum stellar disc and the line-emitting regions may explain the large EW. These bright C II], C III] and C IV emitters are ideal candidates for spectroscopic follow-up to fully unveil their nature.","lang":"eng"}],"_id":"11566","date_published":"2017-11-01T00:00:00Z","article_processing_charge":"No","issue":"3","arxiv":1,"volume":471,"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1703.10169"}],"oa":1,"publication_status":"published","author":[{"last_name":"Stroe","full_name":"Stroe, Andra","first_name":"Andra"},{"first_name":"David","full_name":"Sobral, David","last_name":"Sobral"},{"last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"first_name":"João","full_name":"Calhau, João","last_name":"Calhau"},{"first_name":"Ivan","full_name":"Oteo, Ivan","last_name":"Oteo"}],"type":"journal_article","day":"01","title":"A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent widths ","citation":{"short":"A. Stroe, D. Sobral, J.J. Matthee, J. Calhau, I. Oteo, Monthly Notices of the Royal Astronomical Society 471 (2017) 2558–2574.","ama":"Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent widths . <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;471(3):2558-2574. doi:<a href=\"https://doi.org/10.1093/mnras/stx1712\">10.1093/mnras/stx1712</a>","apa":"Stroe, A., Sobral, D., Matthee, J. J., Calhau, J., &#38; Oteo, I. (2017). A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent widths . <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stx1712\">https://doi.org/10.1093/mnras/stx1712</a>","chicago":"Stroe, Andra, David Sobral, Jorryt J Matthee, João Calhau, and Ivan Oteo. “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, Morphologies and Equivalent Widths .” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stx1712\">https://doi.org/10.1093/mnras/stx1712</a>.","ieee":"A. Stroe, D. Sobral, J. J. Matthee, J. Calhau, and I. Oteo, “A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent widths ,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 471, no. 3. Oxford University Press, pp. 2558–2574, 2017.","ista":"Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. 2017. A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent widths . Monthly Notices of the Royal Astronomical Society. 471(3), 2558–2574.","mla":"Stroe, Andra, et al. “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, Morphologies and Equivalent Widths .” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 471, no. 3, Oxford University Press, 2017, pp. 2558–74, doi:<a href=\"https://doi.org/10.1093/mnras/stx1712\">10.1093/mnras/stx1712</a>."},"doi":"10.1093/mnras/stx1712","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: active","galaxies: high-redshift","quasars: emission lines","galaxies: star formation","cosmology: observations"],"language":[{"iso":"eng"}],"acknowledgement":"We would like to thank the anonymous referee for her/his valuable input that helped improve the clarity and interpretation of our results. DS acknowledges financial support from the Netherlands Organisation for Scientific research (NWO), through a Veni fellowship. IO acknowledges support from the European Research Council in the form of the Advanced Investigator Programme, 321302, COSMICISM. CALYMHA data are based on observations made with the Isaac Newton Telescope (proposals 13AN002, I14AN002, 088-INT7/14A, I14BN006, 118-INT13/14B, I15AN008) operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias. Also based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme IDs 098.A-0819 and 179.A-2005. We are grateful to E. L. Wright and J. Schombert for their cosmology calculator. We would like to thank the authors of NUMPY (van der Walt et al. 2011), SCIPY (Jones et al. 2001), MATPLOTLIB (Hunter 2007) and ASTROPY (Astropy Collaboration et al. 2013) for making these packages publicly available. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is ","date_created":"2022-07-12T12:33:16Z","month":"11","extern":"1","page":"2558-2574","intvolume":"       471","status":"public","publication":"Monthly Notices of the Royal Astronomical Society","quality_controlled":"1","publisher":"Oxford University Press"},{"oa_version":"Preprint","year":"2017","article_type":"original","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"external_id":{"arxiv":["1703.10169"]},"scopus_import":"1","date_updated":"2022-08-19T08:02:04Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","_id":"11567","date_published":"2017-11-01T00:00:00Z","abstract":[{"lang":"eng","text":"Recently, the C III] and C IV emission lines have been observed in galaxies in the early Universe (z > 5), providing new ways to measure their redshift and study their stellar populations and active galactic nuclei (AGN). We explore the first blind C II], C III] and C IV survey (z ∼ 0.68, 1.05, 1.53, respectively) presented in Stroe et al. (2017). We derive luminosity functions (LF) and study properties of C II], C III] and C IV line emitters through comparisons to the LFs of H α and Ly α emitters, UV selected star-forming (SF) galaxies and quasars at similar redshifts. The C II] LF at z ∼ 0.68 is equally well described by a Schechter or a power-law LF, characteristic of a mixture of SF and AGN activity. The C III] LF (z ∼ 1.05) is consistent to a scaled down version of the Schechter H α and Ly α LF at their redshift, indicating a SF origin. In stark contrast, the C IV LF at z ∼ 1.53 is well fit by a power-law, quasar-like LF. We find that the brightest UV sources (MUV < −22) will universally have C III] and C IV emission. However, on average, C III] and C IV are not as abundant as H α or Ly α emitters at the same redshift, with cosmic average ratios of ∼0.02–0.06 to H α and ∼0.01–0.1 to intrinsic Ly α. We predict that the C III] and C IV lines can only be truly competitive in confirming high-redshift candidates when the hosts are intrinsically bright and the effective Ly α escape fraction is below 1 per cent. While C III] and C IV were proposed as good tracers of young, relatively low-metallicity galaxies typical of the early Universe, we find that, at least at z ∼ 1.5, C IV is exclusively hosted by AGN/quasars, especially at large line equivalent widths."}],"article_processing_charge":"No","issue":"3","arxiv":1,"volume":471,"oa":1,"main_file_link":[{"url":"https://arxiv.org/abs/1703.10169","open_access":"1"}],"publication_status":"published","author":[{"full_name":"Stroe, Andra","first_name":"Andra","last_name":"Stroe"},{"first_name":"David","full_name":"Sobral, David","last_name":"Sobral"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J"},{"first_name":"João","full_name":"Calhau, João","last_name":"Calhau"},{"first_name":"Ivan","full_name":"Oteo, Ivan","last_name":"Oteo"}],"type":"journal_article","day":"01","title":"A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average line ratios","citation":{"apa":"Stroe, A., Sobral, D., Matthee, J. J., Calhau, J., &#38; Oteo, I. (2017). A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average line ratios. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stx1713\">https://doi.org/10.1093/mnras/stx1713</a>","ama":"Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average line ratios. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;471(3):2575-2586. doi:<a href=\"https://doi.org/10.1093/mnras/stx1713\">10.1093/mnras/stx1713</a>","short":"A. Stroe, D. Sobral, J.J. Matthee, J. Calhau, I. Oteo, Monthly Notices of the Royal Astronomical Society 471 (2017) 2575–2586.","mla":"Stroe, Andra, et al. “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity Functions and Cosmic Average Line Ratios.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 471, no. 3, Oxford University Press, 2017, pp. 2575–86, doi:<a href=\"https://doi.org/10.1093/mnras/stx1713\">10.1093/mnras/stx1713</a>.","ista":"Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. 2017. A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average line ratios. Monthly Notices of the Royal Astronomical Society. 471(3), 2575–2586.","ieee":"A. Stroe, D. Sobral, J. J. Matthee, J. Calhau, and I. Oteo, “A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average line ratios,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 471, no. 3. Oxford University Press, pp. 2575–2586, 2017.","chicago":"Stroe, Andra, David Sobral, Jorryt J Matthee, João Calhau, and Ivan Oteo. “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity Functions and Cosmic Average Line Ratios.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stx1713\">https://doi.org/10.1093/mnras/stx1713</a>."},"doi":"10.1093/mnras/stx1713","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: active","galaxies: high redshift","galaxies: luminosity function","mass function","quasars: emission lines","star formation","cosmology: observations"],"language":[{"iso":"eng"}],"date_created":"2022-07-12T12:54:57Z","month":"11","extern":"1","page":"2575-2586","intvolume":"       471","status":"public","publication":"Monthly Notices of the Royal Astronomical Society","quality_controlled":"1","publisher":"Oxford University Press"},{"publication_status":"published","oa":1,"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1706.06591"}],"volume":472,"arxiv":1,"article_processing_charge":"No","issue":"1","_id":"11572","abstract":[{"text":"We present spectroscopic follow-up of candidate luminous Ly α emitters (LAEs) at z = 5.7–6.6 in the SA22 field with VLT/X-SHOOTER. We confirm two new luminous LAEs at z = 5.676 (SR6) and z = 6.532 (VR7), and also present HST follow-up of both sources. These sources have luminosities LLy α ≈ 3 × 1043 erg s−1, very high rest-frame equivalent widths of EW0 ≳ 200 Å and narrow Ly α lines (200–340 km s−1). VR7 is the most UV-luminous LAE at z > 6.5, with M1500 = −22.5, even brighter in the UV than CR7. Besides Ly α, we do not detect any other rest-frame UV lines in the spectra of SR6 and VR7, and argue that rest-frame UV lines are easier to observe in bright galaxies with low Ly α equivalent widths. We confirm that Ly α line widths increase with Ly α luminosity at z = 5.7, while there are indications that Ly α lines of faint LAEs become broader at z = 6.6, potentially due to reionization. We find a large spread of up to 3 dex in UV luminosity for >L⋆ LAEs, but find that the Ly α luminosity of the brightest LAEs is strongly related to UV luminosity at z = 6.6. Under basic assumptions, we find that several LAEs at z ≈ 6–7 have Ly α escape fractions ≳ 100  per cent, indicating bursty star formation histories, alternative Ly α production mechanisms, or dust attenuating Ly α emission differently than UV emission. Finally, we present a method to compute ξion, the production efficiency of ionizing photons, and find that LAEs at z ≈ 6–7 have high values of log10(ξion/Hz erg−1) ≈ 25.51 ± 0.09 that may alleviate the need for high Lyman-Continuum escape fractions required for reionization.","lang":"eng"}],"date_published":"2017-11-01T00:00:00Z","scopus_import":"1","external_id":{"arxiv":["1706.06591"]},"date_updated":"2022-08-19T08:05:37Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"article_type":"original","oa_version":"Preprint","year":"2017","publisher":"Oxford University Press","publication":"Monthly Notices of the Royal Astronomical Society","quality_controlled":"1","intvolume":"       472","status":"public","page":"772-787","month":"11","extern":"1","date_created":"2022-07-13T09:47:39Z","acknowledgement":"We thank the referee for a constructive report that has improved the quality and clarity of this work. The authors thank Grecco Oyarzún for discussions. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. DS acknowledges financial support from the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship and from Lancaster University through an Early Career Internal Grant A100679. BD acknowledges financial support from NASA through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G. We thank Kasper Schmidt for providing measurements. Based on observations with the W.M. Keck Observatory through programme C267D. The W.M. Keck Observatory is operated as a scientific partnership amongst the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 097.A-0943, 294.A 5018 and 098.A-0819 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. The authors acknowledge the award of observing time (W16AN004) and of service time (SW2014b20) on the William Herschel Telescope (WHT). WHT and its service programme are operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. Based on observations made with the NASA/ESA HST, obtained (from the Data Archive) at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with programme #14699. We are grateful for the excellent data sets from the COSMOS, UltraVISTA, SXDS, UDS and CFHTLS survey teams; without these legacy surveys, this research would have been impossible. We have benefited from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY and ASTROPY packages, the astronomical imaging tools SEXTRACTOR, SWARP and SCAMP and the TOPCAT analysis tool (Taylor 2013).","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution – galaxies: high-redshift","dark ages","reionization","first stars","cosmology: observations"],"language":[{"iso":"eng"}],"doi":"10.1093/mnras/stx2061","citation":{"short":"J.J. Matthee, D. Sobral, B. Darvish, S. Santos, B. Mobasher, A. Paulino-Afonso, H. Röttgering, L. Alegre, Monthly Notices of the Royal Astronomical Society 472 (2017) 772–787.","apa":"Matthee, J. J., Sobral, D., Darvish, B., Santos, S., Mobasher, B., Paulino-Afonso, A., … Alegre, L. (2017). Spectroscopic properties of luminous Ly α emitters at z ≈ 6–7 and comparison to the Lyman-break population. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stx2061\">https://doi.org/10.1093/mnras/stx2061</a>","ama":"Matthee JJ, Sobral D, Darvish B, et al. Spectroscopic properties of luminous Ly α emitters at z ≈ 6–7 and comparison to the Lyman-break population. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;472(1):772-787. doi:<a href=\"https://doi.org/10.1093/mnras/stx2061\">10.1093/mnras/stx2061</a>","ista":"Matthee JJ, Sobral D, Darvish B, Santos S, Mobasher B, Paulino-Afonso A, Röttgering H, Alegre L. 2017. Spectroscopic properties of luminous Ly α emitters at z ≈ 6–7 and comparison to the Lyman-break population. Monthly Notices of the Royal Astronomical Society. 472(1), 772–787.","ieee":"J. J. Matthee <i>et al.</i>, “Spectroscopic properties of luminous Ly α emitters at z ≈ 6–7 and comparison to the Lyman-break population,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 472, no. 1. Oxford University Press, pp. 772–787, 2017.","chicago":"Matthee, Jorryt J, David Sobral, Behnam Darvish, Sérgio Santos, Bahram Mobasher, Ana Paulino-Afonso, Huub Röttgering, and Lara Alegre. “Spectroscopic Properties of Luminous Ly α Emitters at z ≈ 6–7 and Comparison to the Lyman-Break Population.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stx2061\">https://doi.org/10.1093/mnras/stx2061</a>.","mla":"Matthee, Jorryt J., et al. “Spectroscopic Properties of Luminous Ly α Emitters at z ≈ 6–7 and Comparison to the Lyman-Break Population.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 472, no. 1, Oxford University Press, 2017, pp. 772–87, doi:<a href=\"https://doi.org/10.1093/mnras/stx2061\">10.1093/mnras/stx2061</a>."},"title":"Spectroscopic properties of luminous Ly α emitters at z ≈ 6–7 and comparison to the Lyman-break population","day":"01","type":"journal_article","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J"},{"full_name":"Sobral, David","first_name":"David","last_name":"Sobral"},{"first_name":"Behnam","full_name":"Darvish, Behnam","last_name":"Darvish"},{"last_name":"Santos","full_name":"Santos, Sérgio","first_name":"Sérgio"},{"last_name":"Mobasher","first_name":"Bahram","full_name":"Mobasher, Bahram"},{"first_name":"Ana","full_name":"Paulino-Afonso, Ana","last_name":"Paulino-Afonso"},{"last_name":"Röttgering","full_name":"Röttgering, Huub","first_name":"Huub"},{"full_name":"Alegre, Lara","first_name":"Lara","last_name":"Alegre"}]},{"month":"10","extern":"1","date_created":"2022-07-13T10:03:01Z","page":"1280-1320","publication":"Monthly Notices of the Royal Astronomical Society","quality_controlled":"1","intvolume":"       471","status":"public","publisher":"Oxford University Press","day":"01","author":[{"first_name":"O. J.","full_name":"Turner, O. J.","last_name":"Turner"},{"full_name":"Cirasuolo, M.","first_name":"M.","last_name":"Cirasuolo"},{"last_name":"Harrison","full_name":"Harrison, C. M.","first_name":"C. M."},{"last_name":"McLure","full_name":"McLure, R. J.","first_name":"R. J."},{"full_name":"Dunlop, J. S.","first_name":"J. S.","last_name":"Dunlop"},{"first_name":"A. M.","full_name":"Swinbank, A. M.","last_name":"Swinbank"},{"last_name":"Johnson","full_name":"Johnson, H. L.","first_name":"H. L."},{"last_name":"Sobral","first_name":"D.","full_name":"Sobral, D."},{"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":"Sharples","first_name":"R. M.","full_name":"Sharples, R. M."}],"type":"journal_article","citation":{"mla":"Turner, O. J., et al. “The KMOS Deep Survey (KDS) – I. Dynamical Measurements of Typical Star-Forming Galaxies at z ≃ 3.5.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 471, no. 2, Oxford University Press, 2017, pp. 1280–320, doi:<a href=\"https://doi.org/10.1093/mnras/stx1366\">10.1093/mnras/stx1366</a>.","ista":"Turner OJ, Cirasuolo M, Harrison CM, McLure RJ, Dunlop JS, Swinbank AM, Johnson HL, Sobral D, Matthee JJ, Sharples RM. 2017. The KMOS Deep Survey (KDS) – I. Dynamical measurements of typical star-forming galaxies at z ≃ 3.5. Monthly Notices of the Royal Astronomical Society. 471(2), 1280–1320.","ieee":"O. J. Turner <i>et al.</i>, “The KMOS Deep Survey (KDS) – I. Dynamical measurements of typical star-forming galaxies at z ≃ 3.5,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 471, no. 2. Oxford University Press, pp. 1280–1320, 2017.","chicago":"Turner, O. J., M. Cirasuolo, C. M. Harrison, R. J. McLure, J. S. Dunlop, A. M. Swinbank, H. L. Johnson, D. Sobral, Jorryt J Matthee, and R. M. Sharples. “The KMOS Deep Survey (KDS) – I. Dynamical Measurements of Typical Star-Forming Galaxies at z ≃ 3.5.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stx1366\">https://doi.org/10.1093/mnras/stx1366</a>.","apa":"Turner, O. J., Cirasuolo, M., Harrison, C. M., McLure, R. J., Dunlop, J. S., Swinbank, A. M., … Sharples, R. M. (2017). The KMOS Deep Survey (KDS) – I. Dynamical measurements of typical star-forming galaxies at z ≃ 3.5. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stx1366\">https://doi.org/10.1093/mnras/stx1366</a>","ama":"Turner OJ, Cirasuolo M, Harrison CM, et al. The KMOS Deep Survey (KDS) – I. Dynamical measurements of typical star-forming galaxies at z ≃ 3.5. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;471(2):1280-1320. doi:<a href=\"https://doi.org/10.1093/mnras/stx1366\">10.1093/mnras/stx1366</a>","short":"O.J. Turner, M. Cirasuolo, C.M. Harrison, R.J. McLure, J.S. Dunlop, A.M. Swinbank, H.L. Johnson, D. Sobral, J.J. Matthee, R.M. Sharples, Monthly Notices of the Royal Astronomical Society 471 (2017) 1280–1320."},"title":"The KMOS Deep Survey (KDS) – I. Dynamical measurements of typical star-forming galaxies at z ≃ 3.5","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","galaxies: kinematics and dynamics"],"language":[{"iso":"eng"}],"doi":"10.1093/mnras/stx1366","acknowledgement":"We wish to thank the anonymous referee for their comments, which have improved the quality and clarity of this work. OJT acknowledges the financial support of the Science and Technology Facilities Council through a studentship award. MC and OJT acknowledge the KMOS team and all the personnel of the European Southern Observatory Very Large Telescope for outstanding support during the KMOS GTO observations. CMH, AMS and RMS acknowledge the Science and Technology Facilities Council through grant code ST/L00075X/1. RJM acknowledges the support of the European Research Council via the award of a Consolidator Grant (PI: McLure). JSD acknowledges the support of the European Research Council via the award of an Advanced Grant (PI J. Dunlop), and the contribution of the EC FP7 SPACE project ASTRODEEP (Ref.No: 312725). AMS acknowledges the Leverhulme Foundation. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. DS acknowledges financial support from the Netherlands Organization for Scientific research (NWO) through a Veni fellowship and from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010). This work is based on observations taken by the CANDELS Multi-Cycle Treasury Program with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. This work is based on observations taken by the 3D HST Treasury Program (GO 12177 and 12328) with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Based on data obtained with the European Southern Observatory Very Large Telescope, Paranal, Chile, under Large Program 185.A-0791, and made available by the VUDS team at the CESAM data centre, Laboratoire d’Astrophysique de Marseille, France. Based on observations obtained at the Very Large Telescope of the European Southern Observatory. Programme IDs: 092.A 0399(A), 093.A-0122(A,B), 094.A-0214(A,B),095.A0680(A,B),096.A-0315(A,B,C).","date_published":"2017-10-01T00:00:00Z","_id":"11573","abstract":[{"text":"We present dynamical measurements from the KMOS (K-band multi-object spectrograph) Deep Survey (KDS), which comprises 77 typical star-forming galaxies at z ≃ 3.5 in the mass range 9.0 < log (M⋆/M⊙) < 10.5. These measurements constrain the internal dynamics, the intrinsic velocity dispersions (σint) and rotation velocities (VC) of galaxies in the high-redshift Universe. The mean velocity dispersion of the galaxies in our sample is σint=70.8+3.3−3.1kms−1⁠, revealing that the increasing average σint with increasing redshift, reported for z ≲ 2, continues out to z ≃ 3.5. Only 36 ± 8 per cent of our galaxies are rotation-dominated (VC/σint > 1), with the sample average VC/σint value much smaller than at lower redshift. After carefully selecting comparable star-forming samples at multiple epochs, we find that the rotation-dominated fraction evolves with redshift with a z−0.2 dependence. The rotation-dominated KDS galaxies show no clear offset from the local rotation velocity–stellar mass (i.e. VC–M⋆) relation, although a smaller fraction of the galaxies are on the relation due to the increase in the dispersion-dominated fraction. These observations are consistent with a simple equilibrium model picture, in which random motions are boosted in high-redshift galaxies by a combination of the increasing gas fractions, accretion efficiency, specific star formation rate and stellar feedback and which may provide significant pressure support against gravity on the galactic disc scale.","lang":"eng"}],"arxiv":1,"article_processing_charge":"No","issue":"2","volume":471,"publication_status":"published","oa":1,"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1704.06263"}],"article_type":"original","year":"2017","oa_version":"Preprint","external_id":{"arxiv":["1704.06263"]},"scopus_import":"1","date_updated":"2022-08-19T08:07:31Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]}},{"date_created":"2023-08-03T10:15:09Z","month":"12","extern":"1","publisher":"EDP Sciences","status":"public","intvolume":"       608","publication":"Astronomy & Astrophysics","quality_controlled":"1","title":"Ionizing spectra of stars that lose their envelope through interaction with a binary companion: Role of metallicity","citation":{"apa":"Götberg, Y. L. L., de Mink, S. E., &#38; Groh, J. H. (2017). Ionizing spectra of stars that lose their envelope through interaction with a binary companion: Role of metallicity. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201730472\">https://doi.org/10.1051/0004-6361/201730472</a>","ama":"Götberg YLL, de Mink SE, Groh JH. Ionizing spectra of stars that lose their envelope through interaction with a binary companion: Role of metallicity. <i>Astronomy &#38; Astrophysics</i>. 2017;608. doi:<a href=\"https://doi.org/10.1051/0004-6361/201730472\">10.1051/0004-6361/201730472</a>","short":"Y.L.L. Götberg, S.E. de Mink, J.H. Groh, Astronomy &#38; Astrophysics 608 (2017).","mla":"Götberg, Ylva Louise Linsdotter, et al. “Ionizing Spectra of Stars That Lose Their Envelope through Interaction with a Binary Companion: Role of Metallicity.” <i>Astronomy &#38; Astrophysics</i>, vol. 608, A11, EDP Sciences, 2017, doi:<a href=\"https://doi.org/10.1051/0004-6361/201730472\">10.1051/0004-6361/201730472</a>.","ista":"Götberg YLL, de Mink SE, Groh JH. 2017. Ionizing spectra of stars that lose their envelope through interaction with a binary companion: Role of metallicity. Astronomy &#38; Astrophysics. 608, A11.","ieee":"Y. L. L. Götberg, S. E. de Mink, and J. H. Groh, “Ionizing spectra of stars that lose their envelope through interaction with a binary companion: Role of metallicity,” <i>Astronomy &#38; Astrophysics</i>, vol. 608. EDP Sciences, 2017.","chicago":"Götberg, Ylva Louise Linsdotter, S. E. de Mink, and J. H. Groh. “Ionizing Spectra of Stars That Lose Their Envelope through Interaction with a Binary Companion: Role of Metallicity.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2017. <a href=\"https://doi.org/10.1051/0004-6361/201730472\">https://doi.org/10.1051/0004-6361/201730472</a>."},"type":"journal_article","author":[{"id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","orcid":"0000-0002-6960-6911","last_name":"Götberg","full_name":"Götberg, Ylva Louise Linsdotter","first_name":"Ylva Louise Linsdotter"},{"last_name":"de Mink","first_name":"S. E.","full_name":"de Mink, S. E."},{"full_name":"Groh, J. H.","first_name":"J. H.","last_name":"Groh"}],"day":"01","doi":"10.1051/0004-6361/201730472","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"language":[{"iso":"eng"}],"article_processing_charge":"No","arxiv":1,"_id":"13476","abstract":[{"text":"Understanding ionizing fluxes of stellar populations is crucial for various astrophysical problems including the epoch of reionization. Short-lived massive stars are generally considered as the main stellar sources. We examine the potential role of less massive stars that lose their envelope through interaction with a binary companion. Here, we focus on the role of metallicity (Z). For this purpose we used the evolutionary code MESA and created tailored atmosphere models with the radiative transfer code CMFGEN. We show that typical progenitors, with initial masses of 12 M⊙, produce hot and compact stars (~ 4 M⊙, 60–80 kK, ~1 R⊙). These stripped stars copiously produce ionizing photons, emitting 60–85% and 30–60% of their energy as HI and HeI ionizing radiation, for Z = 0.0001–0.02, respectively. Their output is comparable to what massive stars emit during their Wolf-Rayet phase, if we account for their longer lifetimes and the favorable slope of the initial mass function. Their relative importance for reionization may be further favored since they emit their photons with a time delay (~ 20 Myr after birth in our fiducial model). This allows time for the dispersal of the birth clouds, allowing the ionizing photons to escape into the intergalactic medium. At low Z, we find that Roche stripping fails to fully remove the H-rich envelope, because of the reduced opacity in the subsurface layers. This is in sharp contrast with the assumption of complete stripping that is made in rapid population synthesis simulations, which are widely used to simulate the binary progenitors of supernovae and gravitational waves. Finally, we discuss the urgency to increase the observed sample of stripped stars to test these models and we discuss how our predictions can help to design efficient observational campaigns.","lang":"eng"}],"date_published":"2017-12-01T00:00:00Z","article_number":"A11","main_file_link":[{"url":"https://doi.org/10.1051/0004-6361/201730472","open_access":"1"}],"oa":1,"publication_status":"published","volume":608,"year":"2017","oa_version":"Published Version","article_type":"original","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"scopus_import":"1","external_id":{"arxiv":["1701.07439"]},"date_updated":"2023-08-09T11:27:06Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87"},{"day":"01","author":[{"full_name":"Zapartas, E.","first_name":"E.","last_name":"Zapartas"},{"first_name":"S. E.","full_name":"de Mink, S. E.","last_name":"de Mink"},{"last_name":"Izzard","first_name":"R. G.","full_name":"Izzard, R. G."},{"last_name":"Yoon","full_name":"Yoon, S.-C.","first_name":"S.-C."},{"first_name":"C.","full_name":"Badenes, C.","last_name":"Badenes"},{"last_name":"Götberg","full_name":"Götberg, Ylva Louise Linsdotter","first_name":"Ylva Louise Linsdotter","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","orcid":"0000-0002-6960-6911"},{"last_name":"de Koter","first_name":"A.","full_name":"de Koter, A."},{"full_name":"Neijssel, C. J.","first_name":"C. J.","last_name":"Neijssel"},{"last_name":"Renzo","first_name":"M.","full_name":"Renzo, M."},{"last_name":"Schootemeijer","first_name":"A.","full_name":"Schootemeijer, A."},{"first_name":"T. S.","full_name":"Shrotriya, T. S.","last_name":"Shrotriya"}],"type":"journal_article","citation":{"chicago":"Zapartas, E., S. E. de Mink, R. G. Izzard, S.-C. Yoon, C. Badenes, Ylva Louise Linsdotter Götberg, A. de Koter, et al. “Delay-Time Distribution of Core-Collapse Supernovae with Late Events Resulting from Binary Interaction.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2017. <a href=\"https://doi.org/10.1051/0004-6361/201629685\">https://doi.org/10.1051/0004-6361/201629685</a>.","ieee":"E. Zapartas <i>et al.</i>, “Delay-time distribution of core-collapse supernovae with late events resulting from binary interaction,” <i>Astronomy &#38; Astrophysics</i>, vol. 601, no. A&#38;A. EDP Sciences, 2017.","ista":"Zapartas E, de Mink SE, Izzard RG, Yoon S-C, Badenes C, Götberg YLL, de Koter A, Neijssel CJ, Renzo M, Schootemeijer A, Shrotriya TS. 2017. Delay-time distribution of core-collapse supernovae with late events resulting from binary interaction. Astronomy &#38; Astrophysics. 601(A&#38;A), A29.","mla":"Zapartas, E., et al. “Delay-Time Distribution of Core-Collapse Supernovae with Late Events Resulting from Binary Interaction.” <i>Astronomy &#38; Astrophysics</i>, vol. 601, no. A&#38;A, A29, EDP Sciences, 2017, doi:<a href=\"https://doi.org/10.1051/0004-6361/201629685\">10.1051/0004-6361/201629685</a>.","short":"E. Zapartas, S.E. de Mink, R.G. Izzard, S.-C. Yoon, C. Badenes, Y.L.L. Götberg, A. de Koter, C.J. Neijssel, M. Renzo, A. Schootemeijer, T.S. Shrotriya, Astronomy &#38; Astrophysics 601 (2017).","ama":"Zapartas E, de Mink SE, Izzard RG, et al. Delay-time distribution of core-collapse supernovae with late events resulting from binary interaction. <i>Astronomy &#38; Astrophysics</i>. 2017;601(A&#38;A). doi:<a href=\"https://doi.org/10.1051/0004-6361/201629685\">10.1051/0004-6361/201629685</a>","apa":"Zapartas, E., de Mink, S. E., Izzard, R. G., Yoon, S.-C., Badenes, C., Götberg, Y. L. L., … Shrotriya, T. S. (2017). Delay-time distribution of core-collapse supernovae with late events resulting from binary interaction. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201629685\">https://doi.org/10.1051/0004-6361/201629685</a>"},"title":"Delay-time distribution of core-collapse supernovae with late events resulting from binary interaction","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"language":[{"iso":"eng"}],"doi":"10.1051/0004-6361/201629685","month":"05","extern":"1","date_created":"2023-08-03T10:15:18Z","publication":"Astronomy & Astrophysics","quality_controlled":"1","status":"public","intvolume":"       601","publisher":"EDP Sciences","article_type":"original","oa_version":"Published Version","year":"2017","scopus_import":"1","external_id":{"arxiv":["1701.07032"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2023-08-09T11:15:49Z","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"article_number":"A29","date_published":"2017-05-01T00:00:00Z","_id":"13477","abstract":[{"text":"Most massive stars, the progenitors of core-collapse supernovae, are in close binary systems and may interact with their companion through mass transfer or merging. We undertake a population synthesis study to compute the delay-time distribution of core-collapse supernovae, that is, the supernova rate versus time following a starburst, taking into account binary interactions. We test the systematic robustness of our results by running various simulations to account for the uncertainties in our standard assumptions. We find that a significant fraction, 15+9-8%, of core-collapse supernovae are “late”, that is, they occur 50–200 Myr after birth, when all massive single stars have already exploded. These late events originate predominantly from binary systems with at least one, or, in most cases, with both stars initially being of intermediate mass (4–8 M⊙). The main evolutionary channels that contribute often involve either the merging of the initially more massive primary star with its companion or the engulfment of the remaining core of the primary by the expanding secondary that has accreted mass at an earlier evolutionary stage. Also, the total number of core-collapse supernovae increases by 14+15-14% because of binarity for the same initial stellar mass. The high rate implies that we should have already observed such late core-collapse supernovae, but have not recognized them as such. We argue that φ Persei is a likely progenitor and that eccentric neutron star – white dwarf systems are likely descendants. Late events can help explain the discrepancy in the delay-time distributions derived from supernova remnants in the Magellanic Clouds and extragalactic type Ia events, lowering the contribution of prompt Ia events. We discuss ways to test these predictions and speculate on the implications for supernova feedback in simulations of galaxy evolution.","lang":"eng"}],"arxiv":1,"article_processing_charge":"No","issue":"A&A","volume":601,"publication_status":"published","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1051/0004-6361/201629685"}],"oa":1},{"publisher":"American Physical Society","status":"public","intvolume":"       119","quality_controlled":"1","publication":"Physical Review Letters","date_created":"2023-08-10T06:35:51Z","extern":"1","month":"11","doi":"10.1103/physrevlett.119.203201","language":[{"iso":"eng"}],"keyword":["General Physics and Astronomy"],"title":"Signatures of electronic structure in bicircular high-harmonic spectroscopy","citation":{"ieee":"D. R. Baykusheva, S. Brennecke, M. Lein, and H. J. Wörner, “Signatures of electronic structure in bicircular high-harmonic spectroscopy,” <i>Physical Review Letters</i>, vol. 119, no. 20. American Physical Society, 2017.","ista":"Baykusheva DR, Brennecke S, Lein M, Wörner HJ. 2017. Signatures of electronic structure in bicircular high-harmonic spectroscopy. Physical Review Letters. 119(20), 203201.","chicago":"Baykusheva, Denitsa Rangelova, Simon Brennecke, Manfred Lein, and Hans Jakob Wörner. “Signatures of Electronic Structure in Bicircular High-Harmonic Spectroscopy.” <i>Physical Review Letters</i>. American Physical Society, 2017. <a href=\"https://doi.org/10.1103/physrevlett.119.203201\">https://doi.org/10.1103/physrevlett.119.203201</a>.","mla":"Baykusheva, Denitsa Rangelova, et al. “Signatures of Electronic Structure in Bicircular High-Harmonic Spectroscopy.” <i>Physical Review Letters</i>, vol. 119, no. 20, 203201, American Physical Society, 2017, doi:<a href=\"https://doi.org/10.1103/physrevlett.119.203201\">10.1103/physrevlett.119.203201</a>.","short":"D.R. Baykusheva, S. Brennecke, M. Lein, H.J. Wörner, Physical Review Letters 119 (2017).","apa":"Baykusheva, D. R., Brennecke, S., Lein, M., &#38; Wörner, H. J. (2017). Signatures of electronic structure in bicircular high-harmonic spectroscopy. <i>Physical Review Letters</i>. American Physical Society. <a href=\"https://doi.org/10.1103/physrevlett.119.203201\">https://doi.org/10.1103/physrevlett.119.203201</a>","ama":"Baykusheva DR, Brennecke S, Lein M, Wörner HJ. Signatures of electronic structure in bicircular high-harmonic spectroscopy. <i>Physical Review Letters</i>. 2017;119(20). doi:<a href=\"https://doi.org/10.1103/physrevlett.119.203201\">10.1103/physrevlett.119.203201</a>"},"author":[{"full_name":"Baykusheva, Denitsa Rangelova","first_name":"Denitsa Rangelova","last_name":"Baykusheva","id":"71b4d059-2a03-11ee-914d-dfa3beed6530"},{"first_name":"Simon","full_name":"Brennecke, Simon","last_name":"Brennecke"},{"first_name":"Manfred","full_name":"Lein, Manfred","last_name":"Lein"},{"first_name":"Hans Jakob","full_name":"Wörner, Hans Jakob","last_name":"Wörner"}],"type":"journal_article","day":"17","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1710.04474"}],"oa":1,"publication_status":"published","volume":119,"issue":"20","article_processing_charge":"No","arxiv":1,"_id":"14004","date_published":"2017-11-17T00:00:00Z","abstract":[{"text":"High-harmonic spectroscopy driven by circularly polarized laser pulses and their counterrotating second harmonic is a new branch of attosecond science which currently lacks quantitative interpretations. We extend this technique to the midinfrared regime and record detailed high-harmonic spectra of several rare-gas atoms. These results are compared with the solution of the Schrödinger equation in three dimensions and calculations based on the strong-field approximation that incorporate accurate scattering-wave recombination matrix elements. A quantum-orbit analysis of these results provides a transparent interpretation of the measured intensity ratios of symmetry-allowed neighboring harmonics in terms of (i) a set of propensity rules related to the angular momentum of the atomic orbitals, (ii) atom-specific matrix elements related to their electronic structure, and (iii) the interference of the emissions associated with electrons in orbitals corotating or counterrotating with the laser fields. These results provide the foundation for a quantitative understanding of bicircular high-harmonic spectroscopy.","lang":"eng"}],"article_number":"203201","publication_identifier":{"issn":["0031-9007"],"eissn":["1079-7114"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2023-08-22T08:21:10Z","scopus_import":"1","external_id":{"arxiv":["1710.04474"]},"oa_version":"Preprint","year":"2017","article_type":"original"},{"language":[{"iso":"eng"}],"keyword":["General Physics and Astronomy","General Biochemistry","Genetics and Molecular Biology","General Chemistry","Multidisciplinary"],"doi":"10.1038/ncomms15651","pmid":1,"day":"15","type":"journal_article","author":[{"last_name":"Walt","first_name":"Samuel G.","full_name":"Walt, Samuel G."},{"last_name":"Bhargava Ram","first_name":"Niraghatam","full_name":"Bhargava Ram, Niraghatam"},{"last_name":"Atala","first_name":"Marcos","full_name":"Atala, Marcos"},{"last_name":"Shvetsov-Shilovski","full_name":"Shvetsov-Shilovski, Nikolay I","first_name":"Nikolay I"},{"full_name":"von Conta, Aaron","first_name":"Aaron","last_name":"von Conta"},{"id":"71b4d059-2a03-11ee-914d-dfa3beed6530","first_name":"Denitsa Rangelova","full_name":"Baykusheva, Denitsa Rangelova","last_name":"Baykusheva"},{"first_name":"Manfred","full_name":"Lein, Manfred","last_name":"Lein"},{"first_name":"Hans Jakob","full_name":"Wörner, Hans Jakob","last_name":"Wörner"}],"citation":{"mla":"Walt, Samuel G., et al. “Dynamics of Valence-Shell Electrons and Nuclei Probed by Strong-Field Holography and Rescattering.” <i>Nature Communications</i>, vol. 8, 15651, Springer Nature, 2017, doi:<a href=\"https://doi.org/10.1038/ncomms15651\">10.1038/ncomms15651</a>.","chicago":"Walt, Samuel G., Niraghatam Bhargava Ram, Marcos Atala, Nikolay I Shvetsov-Shilovski, Aaron von Conta, Denitsa Rangelova Baykusheva, Manfred Lein, and Hans Jakob Wörner. “Dynamics of Valence-Shell Electrons and Nuclei Probed by Strong-Field Holography and Rescattering.” <i>Nature Communications</i>. Springer Nature, 2017. <a href=\"https://doi.org/10.1038/ncomms15651\">https://doi.org/10.1038/ncomms15651</a>.","ieee":"S. G. Walt <i>et al.</i>, “Dynamics of valence-shell electrons and nuclei probed by strong-field holography and rescattering,” <i>Nature Communications</i>, vol. 8. Springer Nature, 2017.","ista":"Walt SG, Bhargava Ram N, Atala M, Shvetsov-Shilovski NI, von Conta A, Baykusheva DR, Lein M, Wörner HJ. 2017. Dynamics of valence-shell electrons and nuclei probed by strong-field holography and rescattering. Nature Communications. 8, 15651.","ama":"Walt SG, Bhargava Ram N, Atala M, et al. Dynamics of valence-shell electrons and nuclei probed by strong-field holography and rescattering. <i>Nature Communications</i>. 2017;8. doi:<a href=\"https://doi.org/10.1038/ncomms15651\">10.1038/ncomms15651</a>","apa":"Walt, S. G., Bhargava Ram, N., Atala, M., Shvetsov-Shilovski, N. I., von Conta, A., Baykusheva, D. R., … Wörner, H. J. (2017). Dynamics of valence-shell electrons and nuclei probed by strong-field holography and rescattering. <i>Nature Communications</i>. Springer Nature. <a href=\"https://doi.org/10.1038/ncomms15651\">https://doi.org/10.1038/ncomms15651</a>","short":"S.G. Walt, N. Bhargava Ram, M. Atala, N.I. Shvetsov-Shilovski, A. von Conta, D.R. Baykusheva, M. Lein, H.J. Wörner, Nature Communications 8 (2017)."},"title":"Dynamics of valence-shell electrons and nuclei probed by strong-field holography and rescattering","quality_controlled":"1","publication":"Nature Communications","intvolume":"         8","status":"public","publisher":"Springer Nature","extern":"1","month":"06","date_created":"2023-08-10T06:36:09Z","date_updated":"2023-08-22T08:26:06Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","scopus_import":"1","external_id":{"pmid":["28643771"]},"publication_identifier":{"eissn":["2041-1723"]},"article_type":"original","oa_version":"Published Version","year":"2017","volume":8,"publication_status":"published","oa":1,"main_file_link":[{"url":"https://doi.org/10.1038/ncomms15651","open_access":"1"}],"article_number":"15651","_id":"14005","date_published":"2017-06-15T00:00:00Z","abstract":[{"lang":"eng","text":"Strong-field photoelectron holography and laser-induced electron diffraction (LIED) are two powerful emerging methods for probing the ultrafast dynamics of molecules. However, both of them have remained restricted to static systems and to nuclear dynamics induced by strong-field ionization. Here we extend these promising methods to image purely electronic valence-shell dynamics in molecules using photoelectron holography. In the same experiment, we use LIED and photoelectron holography simultaneously, to observe coupled electronic-rotational dynamics taking place on similar timescales. These results offer perspectives for imaging ultrafast dynamics of molecules on femtosecond to attosecond timescales."}],"article_processing_charge":"No"},{"article_type":"original","year":"2017","oa_version":"None","date_updated":"2023-08-22T08:30:59Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","external_id":{"pmid":["28388142"]},"scopus_import":"1","publication_identifier":{"issn":["0021-9606"],"eissn":["1089-7690"]},"issue":"12","article_processing_charge":"No","article_number":"124306","date_published":"2017-03-28T00:00:00Z","_id":"14006","abstract":[{"lang":"eng","text":"We present a theoretical formalism for the calculation of attosecond delays in molecular photoionization. It is shown how delays relevant to one-photon-ionization, also known as Eisenbud-Wigner-Smith delays, can be obtained from the complex dipole matrix elements provided by molecular quantum scattering theory. These results are used to derive formulae for the delays measured by two-photon attosecond interferometry based on an attosecond pulse train and a dressing femtosecond infrared pulse. These effective delays are first expressed in the molecular frame where maximal information about the molecular photoionization dynamics is available. The effects of averaging over the emission direction of the electron and the molecular orientation are introduced analytically. We illustrate this general formalism for the case of two polyatomic molecules. N2O serves as an example of a polar linear molecule characterized by complex photoionization dynamics resulting from the presence of molecular shape resonances. H2O illustrates the case of a non-linear molecule with comparably simple photoionization dynamics resulting from a flat continuum. Our theory establishes the foundation for interpreting measurements of the photoionization dynamics of all molecules by attosecond metrology."}],"publication_status":"published","volume":146,"citation":{"ama":"Baykusheva DR, Wörner HJ. Theory of attosecond delays in molecular photoionization. <i>The Journal of Chemical Physics</i>. 2017;146(12). doi:<a href=\"https://doi.org/10.1063/1.4977933\">10.1063/1.4977933</a>","apa":"Baykusheva, D. R., &#38; Wörner, H. J. (2017). Theory of attosecond delays in molecular photoionization. <i>The Journal of Chemical Physics</i>. AIP Publishing. <a href=\"https://doi.org/10.1063/1.4977933\">https://doi.org/10.1063/1.4977933</a>","short":"D.R. Baykusheva, H.J. Wörner, The Journal of Chemical Physics 146 (2017).","mla":"Baykusheva, Denitsa Rangelova, and Hans Jakob Wörner. “Theory of Attosecond Delays in Molecular Photoionization.” <i>The Journal of Chemical Physics</i>, vol. 146, no. 12, 124306, AIP Publishing, 2017, doi:<a href=\"https://doi.org/10.1063/1.4977933\">10.1063/1.4977933</a>.","chicago":"Baykusheva, Denitsa Rangelova, and Hans Jakob Wörner. “Theory of Attosecond Delays in Molecular Photoionization.” <i>The Journal of Chemical Physics</i>. AIP Publishing, 2017. <a href=\"https://doi.org/10.1063/1.4977933\">https://doi.org/10.1063/1.4977933</a>.","ista":"Baykusheva DR, Wörner HJ. 2017. Theory of attosecond delays in molecular photoionization. The Journal of Chemical Physics. 146(12), 124306.","ieee":"D. R. Baykusheva and H. J. Wörner, “Theory of attosecond delays in molecular photoionization,” <i>The Journal of Chemical Physics</i>, vol. 146, no. 12. AIP Publishing, 2017."},"title":"Theory of attosecond delays in molecular photoionization","day":"28","author":[{"first_name":"Denitsa Rangelova","full_name":"Baykusheva, Denitsa Rangelova","last_name":"Baykusheva","id":"71b4d059-2a03-11ee-914d-dfa3beed6530"},{"full_name":"Wörner, Hans Jakob","first_name":"Hans Jakob","last_name":"Wörner"}],"type":"journal_article","pmid":1,"language":[{"iso":"eng"}],"keyword":["Physical and Theoretical Chemistry","General Physics and Astronomy"],"doi":"10.1063/1.4977933","extern":"1","month":"03","date_created":"2023-08-10T06:36:19Z","publisher":"AIP Publishing","quality_controlled":"1","publication":"The Journal of Chemical Physics","intvolume":"       146","status":"public"},{"date_published":"2017-11-17T00:00:00Z","_id":"14031","abstract":[{"text":"High-harmonic spectroscopy driven by circularly polarized laser pulses and their counterrotating second harmonic is a new branch of attosecond science which currently lacks quantitative interpretations. We extend this technique to the midinfrared regime and record detailed high-harmonic spectra of several rare-gas atoms. These results are compared with the solution of the Schrödinger equation in three dimensions and calculations based on the strong-field approximation that incorporate accurate scattering-wave recombination matrix elements. A quantum-orbit analysis of these results provides a transparent interpretation of the measured intensity ratios of symmetry-allowed neighboring harmonics in terms of (i) a set of propensity rules related to the angular momentum of the atomic orbitals, (ii) atom-specific matrix elements related to their electronic structure, and (iii) the interference of the emissions associated with electrons in orbitals corotating or counterrotating with the laser fields. These results provide the foundation for a quantitative understanding of bicircular high-harmonic spectroscopy.","lang":"eng"}],"article_number":"203201","article_processing_charge":"No","issue":"20","arxiv":1,"volume":119,"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1710.04474"}],"oa":1,"publication_status":"published","oa_version":"Preprint","year":"2017","article_type":"original","publication_identifier":{"eissn":["1079-7114"],"issn":["0031-9007"]},"external_id":{"pmid":["29219334"],"arxiv":["1710.04474"]},"scopus_import":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2023-08-22T06:48:28Z","date_created":"2023-08-10T06:48:12Z","month":"11","extern":"1","status":"public","intvolume":"       119","publication":"Physical Review Letters","quality_controlled":"1","publisher":"American Physical Society","type":"journal_article","author":[{"first_name":"Denitsa Rangelova","full_name":"Baykusheva, Denitsa Rangelova","last_name":"Baykusheva","id":"71b4d059-2a03-11ee-914d-dfa3beed6530"},{"first_name":"Simon","full_name":"Brennecke, Simon","last_name":"Brennecke"},{"last_name":"Lein","full_name":"Lein, Manfred","first_name":"Manfred"},{"last_name":"Wörner","full_name":"Wörner, Hans Jakob","first_name":"Hans Jakob"}],"day":"17","title":"Signatures of electronic structure in bicircular high-harmonic spectroscopy","citation":{"chicago":"Baykusheva, Denitsa Rangelova, Simon Brennecke, Manfred Lein, and Hans Jakob Wörner. “Signatures of Electronic Structure in Bicircular High-Harmonic Spectroscopy.” <i>Physical Review Letters</i>. American Physical Society, 2017. <a href=\"https://doi.org/10.1103/physrevlett.119.203201\">https://doi.org/10.1103/physrevlett.119.203201</a>.","ieee":"D. R. Baykusheva, S. Brennecke, M. Lein, and H. J. Wörner, “Signatures of electronic structure in bicircular high-harmonic spectroscopy,” <i>Physical Review Letters</i>, vol. 119, no. 20. American Physical Society, 2017.","ista":"Baykusheva DR, Brennecke S, Lein M, Wörner HJ. 2017. Signatures of electronic structure in bicircular high-harmonic spectroscopy. Physical Review Letters. 119(20), 203201.","mla":"Baykusheva, Denitsa Rangelova, et al. “Signatures of Electronic Structure in Bicircular High-Harmonic Spectroscopy.” <i>Physical Review Letters</i>, vol. 119, no. 20, 203201, American Physical Society, 2017, doi:<a href=\"https://doi.org/10.1103/physrevlett.119.203201\">10.1103/physrevlett.119.203201</a>.","short":"D.R. Baykusheva, S. Brennecke, M. Lein, H.J. Wörner, Physical Review Letters 119 (2017).","ama":"Baykusheva DR, Brennecke S, Lein M, Wörner HJ. Signatures of electronic structure in bicircular high-harmonic spectroscopy. <i>Physical Review Letters</i>. 2017;119(20). doi:<a href=\"https://doi.org/10.1103/physrevlett.119.203201\">10.1103/physrevlett.119.203201</a>","apa":"Baykusheva, D. R., Brennecke, S., Lein, M., &#38; Wörner, H. J. (2017). Signatures of electronic structure in bicircular high-harmonic spectroscopy. <i>Physical Review Letters</i>. American Physical Society. <a href=\"https://doi.org/10.1103/physrevlett.119.203201\">https://doi.org/10.1103/physrevlett.119.203201</a>"},"doi":"10.1103/physrevlett.119.203201","keyword":["General Physics and Astronomy"],"language":[{"iso":"eng"}],"pmid":1},{"date_created":"2022-04-07T07:48:34Z","extern":"1","month":"12","publisher":"Springer Nature","status":"public","intvolume":"         7","quality_controlled":"1","publication":"Nature Communications","title":"p120-catenin prevents multinucleation through control of MKLP1-dependent RhoA activity during cytokinesis","citation":{"ama":"van de Ven RAH, de Groot JS, Park D, et al. p120-catenin prevents multinucleation through control of MKLP1-dependent RhoA activity during cytokinesis. <i>Nature Communications</i>. 2016;7. doi:<a href=\"https://doi.org/10.1038/ncomms13874\">10.1038/ncomms13874</a>","apa":"van de Ven, R. A. H., de Groot, J. S., Park, D., van Domselaar, R., de Jong, D., Szuhai, K., … Derksen, P. W. B. (2016). p120-catenin prevents multinucleation through control of MKLP1-dependent RhoA activity during cytokinesis. <i>Nature Communications</i>. Springer Nature. <a href=\"https://doi.org/10.1038/ncomms13874\">https://doi.org/10.1038/ncomms13874</a>","short":"R.A.H. van de Ven, J.S. de Groot, D. Park, R. van Domselaar, D. de Jong, K. Szuhai, E. van der Wall, O.M. Rueda, H.R. Ali, C. Caldas, P.J. van Diest, M. Hetzer, E. Sahai, P.W.B. Derksen, Nature Communications 7 (2016).","mla":"van de Ven, Robert A. H., et al. “P120-Catenin Prevents Multinucleation through Control of MKLP1-Dependent RhoA Activity during Cytokinesis.” <i>Nature Communications</i>, vol. 7, 13874, Springer Nature, 2016, doi:<a href=\"https://doi.org/10.1038/ncomms13874\">10.1038/ncomms13874</a>.","chicago":"Ven, Robert A.H. van de, Jolien S. de Groot, Danielle Park, Robert van Domselaar, Danielle de Jong, Karoly Szuhai, Elsken van der Wall, et al. “P120-Catenin Prevents Multinucleation through Control of MKLP1-Dependent RhoA Activity during Cytokinesis.” <i>Nature Communications</i>. Springer Nature, 2016. <a href=\"https://doi.org/10.1038/ncomms13874\">https://doi.org/10.1038/ncomms13874</a>.","ista":"van de Ven RAH, de Groot JS, Park D, van Domselaar R, de Jong D, Szuhai K, van der Wall E, Rueda OM, Ali HR, Caldas C, van Diest PJ, Hetzer M, Sahai E, Derksen PWB. 2016. p120-catenin prevents multinucleation through control of MKLP1-dependent RhoA activity during cytokinesis. Nature Communications. 7, 13874.","ieee":"R. A. H. van de Ven <i>et al.</i>, “p120-catenin prevents multinucleation through control of MKLP1-dependent RhoA activity during cytokinesis,” <i>Nature Communications</i>, vol. 7. Springer Nature, 2016."},"author":[{"last_name":"van de Ven","full_name":"van de Ven, Robert A.H.","first_name":"Robert A.H."},{"last_name":"de Groot","full_name":"de Groot, Jolien S.","first_name":"Jolien S."},{"last_name":"Park","full_name":"Park, Danielle","first_name":"Danielle"},{"last_name":"van Domselaar","first_name":"Robert","full_name":"van Domselaar, Robert"},{"full_name":"de Jong, Danielle","first_name":"Danielle","last_name":"de Jong"},{"first_name":"Karoly","full_name":"Szuhai, Karoly","last_name":"Szuhai"},{"last_name":"van der Wall","full_name":"van der Wall, Elsken","first_name":"Elsken"},{"first_name":"Oscar M.","full_name":"Rueda, Oscar M.","last_name":"Rueda"},{"full_name":"Ali, H. Raza","first_name":"H. Raza","last_name":"Ali"},{"last_name":"Caldas","first_name":"Carlos","full_name":"Caldas, Carlos"},{"last_name":"van Diest","full_name":"van Diest, Paul J.","first_name":"Paul J."},{"orcid":"0000-0002-2111-992X","id":"86c0d31b-b4eb-11ec-ac5a-eae7b2e135ed","full_name":"HETZER, Martin W","first_name":"Martin W","last_name":"HETZER"},{"last_name":"Sahai","full_name":"Sahai, Erik","first_name":"Erik"},{"full_name":"Derksen, Patrick W.B.","first_name":"Patrick W.B.","last_name":"Derksen"}],"type":"journal_article","day":"22","pmid":1,"related_material":{"link":[{"relation":"erratum","url":"https://doi.org/10.1038/ncomms16030"}]},"doi":"10.1038/ncomms13874","language":[{"iso":"eng"}],"keyword":["General Physics and Astronomy","General Biochemistry","Genetics and Molecular Biology","General Chemistry"],"article_processing_charge":"No","_id":"11072","abstract":[{"lang":"eng","text":"Spatiotemporal activation of RhoA and actomyosin contraction underpins cellular adhesion and division. Loss of cell–cell adhesion and chromosomal instability are cardinal events that drive tumour progression. Here, we show that p120-catenin (p120) not only controls cell–cell adhesion, but also acts as a critical regulator of cytokinesis. We find that p120 regulates actomyosin contractility through concomitant binding to RhoA and the centralspindlin component MKLP1, independent of cadherin association. In anaphase, p120 is enriched at the cleavage furrow where it binds MKLP1 to spatially control RhoA GTPase cycling. Binding of p120 to MKLP1 during cytokinesis depends on the N-terminal coiled-coil domain of p120 isoform 1A. Importantly, clinical data show that loss of p120 expression is a common event in breast cancer that strongly correlates with multinucleation and adverse patient survival. In summary, our study identifies p120 loss as a driver event of chromosomal instability in cancer.\r\n"}],"date_published":"2016-12-22T00:00:00Z","article_number":"13874","main_file_link":[{"url":"https://doi.org/10.1038/ncomms13874","open_access":"1"}],"oa":1,"publication_status":"published","volume":7,"year":"2016","oa_version":"Published Version","article_type":"original","publication_identifier":{"issn":["2041-1723"]},"user_id":"72615eeb-f1f3-11ec-aa25-d4573ddc34fd","date_updated":"2022-07-18T08:34:32Z","external_id":{"pmid":["28004812"]},"scopus_import":"1"},{"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2022-08-19T08:09:54Z","scopus_import":"1","external_id":{"arxiv":["1606.07435"]},"oa_version":"Preprint","year":"2016","article_type":"original","volume":463,"main_file_link":[{"url":"https://arxiv.org/abs/1606.07435","open_access":"1"}],"oa":1,"publication_status":"published","_id":"11574","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."}],"date_published":"2016-12-01T00:00:00Z","issue":"2","article_processing_charge":"No","arxiv":1,"doi":"10.1093/mnras/stw2076","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift","galaxies: luminosity function","mass function","cosmology: observations","dark ages","reionization","first stars"],"acknowledgement":"We thank the anonymous referee for useful and constructive comments and suggestions which greatly improved the quality and clarity of our work. The authors acknowledge financial support from the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship. SS and DS acknowledge funding from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010). SS also acknowledges support from FCT through the research grants UID/FIS/04434/2013 and PTDC/FIS-AST/2194/2012. JM acknowledges a Huygens PhD fellowship from Leiden University. Based on observations with the Subaru Telescope (Program IDs: S05B-027, S06A-025, S06B-010, S07A-013, S07B-008, S08B-008, S09A-017, S14A-086). Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 294.A-5018. Based on observations obtained with MegaPrime/Megacam, a joint project of CFHT and CEA/IRFU, at the Canada–France–Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l’Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at TERAPIX available at the Canadian Astronomy Data Centre as part of the Canada–France–Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. We are grateful to the CFHTLS, COSMOS-UltraVISTA, UKIDSS, SXDF and COSMOS survey teams. Without these legacy surveys, this research would have been impossible. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct and explore observations from this mountain. Finally, the authors acknowledge the unique value of the publicly available programming language PYTHON, including the NUMPY, PYFITS, MATPLOTLIB, SCIPY and ASTROPY (Astropy Collaboration et al.","author":[{"full_name":"Santos, Sérgio","first_name":"Sérgio","last_name":"Santos"},{"last_name":"Sobral","first_name":"David","full_name":"Sobral, David"},{"last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720"}],"type":"journal_article","day":"01","title":"The Lyα luminosity function at z= 5.7–6.6 and the steep drop of the faint end: Implications for reionization","citation":{"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>.","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.","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.","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.","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>","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>"},"intvolume":"       463","status":"public","quality_controlled":"1","publication":"Monthly Notices of the Royal Astronomical Society","publisher":"Oxford University Press","date_created":"2022-07-13T10:08:20Z","extern":"1","month":"12","page":"1678-1691"},{"_id":"11575","date_published":"2016-07-01T00:00:00Z","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"}],"issue":"3","article_processing_charge":"No","arxiv":1,"volume":459,"oa":1,"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1510.08067"}],"publication_status":"published","oa_version":"Preprint","year":"2016","article_type":"original","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2022-08-19T08:12:07Z","external_id":{"arxiv":["1510.08067"]},"scopus_import":"1","date_created":"2022-07-13T10:21:24Z","extern":"1","month":"07","page":"2632-2650","intvolume":"       459","status":"public","quality_controlled":"1","publication":"Monthly Notices of the Royal Astronomical Society","publisher":"Oxford University Press","type":"journal_article","author":[{"full_name":"Lagos, Claudia del P.","first_name":"Claudia del P.","last_name":"Lagos"},{"first_name":"Tom","full_name":"Theuns, Tom","last_name":"Theuns"},{"full_name":"Schaye, Joop","first_name":"Joop","last_name":"Schaye"},{"last_name":"Furlong","full_name":"Furlong, Michelle","first_name":"Michelle"},{"first_name":"Richard G.","full_name":"Bower, Richard G.","last_name":"Bower"},{"last_name":"Schaller","full_name":"Schaller, Matthieu","first_name":"Matthieu"},{"last_name":"Crain","first_name":"Robert A.","full_name":"Crain, Robert A."},{"last_name":"Trayford","full_name":"Trayford, James W.","first_name":"James W."},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J"}],"day":"01","title":"The Fundamental Plane of star formation in galaxies revealed by the EAGLE hydrodynamical simulations","citation":{"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>.","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.","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.","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>.","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>","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."},"doi":"10.1093/mnras/stw717","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics  stars: formation","ISM: evolution","galaxies: evolution","galaxies: formation","galaxies: ISM"],"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."},{"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","cosmology: observations"],"language":[{"iso":"eng"}],"doi":"10.1093/mnras/stw022","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.","day":"01","type":"journal_article","author":[{"first_name":"David","full_name":"Sobral, David","last_name":"Sobral"},{"last_name":"Kohn","first_name":"Saul A.","full_name":"Kohn, Saul A."},{"full_name":"Best, Philip N.","first_name":"Philip N.","last_name":"Best"},{"first_name":"Ian","full_name":"Smail, Ian","last_name":"Smail"},{"full_name":"Harrison, Chris M.","first_name":"Chris M.","last_name":"Harrison"},{"first_name":"John","full_name":"Stott, John","last_name":"Stott"},{"full_name":"Calhau, João","first_name":"João","last_name":"Calhau"},{"last_name":"Matthee","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X"}],"citation":{"ista":"Sobral D, Kohn SA, Best PN, Smail I, Harrison CM, Stott J, Calhau J, Matthee JJ. 2016. The most luminous H α emitters at z ∼ 0.8–2.23 from HiZELS: Evolution of AGN and star-forming galaxies. Monthly Notices of the Royal Astronomical Society. 457(2), 1739–1752.","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.","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>.","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.","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>","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>"},"title":"The most luminous H α emitters at z ∼ 0.8–2.23 from HiZELS: Evolution of AGN and star-forming galaxies","publication":"Monthly Notices of the Royal Astronomical Society","quality_controlled":"1","intvolume":"       457","status":"public","publisher":"Oxford University Press","month":"04","extern":"1","date_created":"2022-07-13T12:50:36Z","page":"1739-1752","external_id":{"arxiv":["1601.02266"]},"scopus_import":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2022-08-19T08:15:21Z","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"article_type":"original","oa_version":"Preprint","year":"2016","volume":457,"publication_status":"published","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1601.02266"}],"oa":1,"date_published":"2016-04-01T00:00:00Z","_id":"11576","abstract":[{"text":"We use new near-infrared spectroscopic observations to investigate the nature and evolution of the most luminous Hα emitters at z ∼ 0.8–2.23, which evolve strongly in number density over this period, and compare them to more typical Hα emitters. We study 59 luminous Hα emitters with LHα > L∗Hα⁠, roughly equally split per redshift slice at z ∼ 0.8, 1.47 and 2.23 from the HiZELS and CF-HiZELS surveys. We find that, overall, 30 ± 8 per cent are active galactic nuclei [AGNs; 80 ± 30 per cent of these AGNs are broad-line AGNs, BL-AGNs], and we find little to no evolution in the AGN fraction with redshift, within the errors. However, the AGN fraction increases strongly with Hα luminosity and correlates best with LHα/L∗Hα(z)⁠. While LHα ≤ L∗Hα(z) Hα emitters are largely dominated by star-forming galaxies (>80 per cent), the most luminous Hα emitters (⁠LHα>10L∗Hα(z)⁠) at any cosmic time are essentially all BL-AGN. Using our AGN-decontaminated sample of luminous star-forming galaxies, and integrating down to a fixed Hα luminosity, we find a factor of ∼1300 evolution in the star formation rate density from z = 0 to 2.23. This is much stronger than the evolution from typical Hα star-forming galaxies and in line with the evolution seen for constant luminosity cuts used to select ‘ultraluminous’ infrared galaxies and/or sub-millimetre galaxies. By taking into account the evolution in the typical Hα luminosity, we show that the most strongly star-forming Hα-selected galaxies at any epoch (⁠LHα>L∗Hα(z)⁠) contribute the same fractional amount of ≈15 per cent to the total star formation rate density, at least up to z = 2.23.","lang":"eng"}],"arxiv":1,"article_processing_charge":"No","issue":"2"},{"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"scopus_import":"1","external_id":{"arxiv":["1602.02756"]},"date_updated":"2022-08-19T08:17:19Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","year":"2016","oa_version":"Preprint","article_type":"original","oa":1,"main_file_link":[{"url":"https://arxiv.org/abs/1602.02756","open_access":"1"}],"publication_status":"published","volume":458,"article_processing_charge":"No","issue":"1","arxiv":1,"date_published":"2016-05-01T00:00:00Z","_id":"11578","abstract":[{"text":"We present the first results from our CAlibrating LYMan α with Hα (CALYMHA) pilot survey at the Isaac Newton Telescope. We measure Lyα emission for 488 Hα selected galaxies at z = 2.23 from High-z Emission Line Survey in the COSMOS and UDS fields with a specially designed narrow-band filter (λc = 3918 Å, Δλ = 52 Å). We find 17 dual Hα-Lyα emitters [fLyα > 5 × 10−17 erg s−1 cm−2, of which five are X-ray active galactic nuclei (AGN)]. For star-forming galaxies, we find a range of Lyα escape fractions (fesc, measured with 3 arcsec apertures) from 2 to 30 per cent. These galaxies have masses from 3 × 108 M⊙ to 1011 M⊙ and dust attenuations E(B − V) = 0–0.5. Using stacking, we measure a median escape fraction of 1.6 ± 0.5 per cent (4.0 ± 1.0 per cent without correcting Hα for dust), but show that this depends on galaxy properties. The stacked fesc tends to decrease with increasing star formation rate and dust attenuation. However, at the highest masses and dust attenuations, we detect individual galaxies with fesc much higher than the typical values from stacking, indicating significant scatter in the values of fesc. Relations between fesc and UV slope are bimodal, with high fesc for either the bluest or reddest galaxies. We speculate that this bimodality and large scatter in the values of fesc is due to additional physical mechanisms such as outflows facilitating fesc for dusty/massive systems. Lyα is significantly more extended than Hα and the UV. fesc continues to increase up to at least 20 kpc (3σ, 40 kpc [2σ]) for typical star-forming galaxies and thus the aperture is the most important predictor of fesc.","lang":"eng"}],"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).","doi":"10.1093/mnras/stw322","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","galaxies: ISM"],"language":[{"iso":"eng"}],"title":"The CALYMHA survey: Lyα escape fraction and its dependence on galaxy properties at z = 2.23","citation":{"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.","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.","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>.","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>.","short":"J.J. Matthee, D. Sobral, I. Oteo, P. Best, I. Smail, H. Röttgering, A. Paulino-Afonso, Monthly Notices of the Royal Astronomical Society 458 (2016) 449–467.","apa":"Matthee, J. J., Sobral, D., Oteo, I., Best, P., Smail, I., Röttgering, H., &#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>"},"type":"journal_article","author":[{"last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"full_name":"Sobral, David","first_name":"David","last_name":"Sobral"},{"full_name":"Oteo, Iván","first_name":"Iván","last_name":"Oteo"},{"first_name":"Philip","full_name":"Best, Philip","last_name":"Best"},{"first_name":"Ian","full_name":"Smail, Ian","last_name":"Smail"},{"last_name":"Röttgering","first_name":"Huub","full_name":"Röttgering, Huub"},{"first_name":"Ana","full_name":"Paulino-Afonso, Ana","last_name":"Paulino-Afonso"}],"day":"01","publisher":"Oxford University Press","intvolume":"       458","status":"public","publication":"Monthly Notices of the Royal Astronomical Society","quality_controlled":"1","page":"449-467","date_created":"2022-07-14T08:51:37Z","month":"05","extern":"1"},{"volume":592,"publication_status":"published","oa":1,"main_file_link":[{"url":"https://doi.org/10.1051/0004-6361/201526309","open_access":"1"}],"article_number":"A147","date_published":"2016-08-18T00:00:00Z","_id":"13478","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."}],"arxiv":1,"article_processing_charge":"No","external_id":{"arxiv":["1606.07819"]},"scopus_import":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2023-08-09T11:09:50Z","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"article_type":"original","oa_version":"Published Version","year":"2016","publication":"Astronomy & Astrophysics","quality_controlled":"1","status":"public","intvolume":"       592","publisher":"EDP Sciences","month":"08","extern":"1","date_created":"2023-08-03T10:15:28Z","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"language":[{"iso":"eng"}],"doi":"10.1051/0004-6361/201526309","day":"18","type":"journal_article","author":[{"first_name":"Ylva Louise Linsdotter","full_name":"Götberg, Ylva Louise Linsdotter","last_name":"Götberg","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","orcid":"0000-0002-6960-6911"},{"last_name":"Davies","full_name":"Davies, Melvyn B.","first_name":"Melvyn B."},{"last_name":"Mustill","full_name":"Mustill, Alexander J.","first_name":"Alexander J."},{"full_name":"Johansen, Anders","first_name":"Anders","last_name":"Johansen"},{"last_name":"Church","first_name":"Ross P.","full_name":"Church, Ross P."}],"citation":{"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>.","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.","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).","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>","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>"},"title":"Long-term stability of the HR 8799 planetary system without resonant lock"}]