[{"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"citation":{"ieee":"A. A. Khostovan <i>et al.</i>, “The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar mass,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 478, no. 3. Oxford University Press, pp. 2999–3015, 2018.","chicago":"Khostovan, A A, D Sobral, B Mobasher, P N Best, I Smail, Jorryt J Matthee, B Darvish, H Nayyeri, S Hemmati, and J P Stott. “The Clustering of H β + [O III] and [O II] Emitters since z ∼ 5: Dependencies with Line Luminosity and Stellar Mass.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2018. <a href=\"https://doi.org/10.1093/mnras/sty925\">https://doi.org/10.1093/mnras/sty925</a>.","apa":"Khostovan, A. A., Sobral, D., Mobasher, B., Best, P. N., Smail, I., Matthee, J. J., … Stott, J. P. (2018). The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar mass. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/sty925\">https://doi.org/10.1093/mnras/sty925</a>","ama":"Khostovan AA, Sobral D, Mobasher B, et al. The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar mass. <i>Monthly Notices of the Royal Astronomical Society</i>. 2018;478(3):2999-3015. doi:<a href=\"https://doi.org/10.1093/mnras/sty925\">10.1093/mnras/sty925</a>","short":"A.A. Khostovan, D. Sobral, B. Mobasher, P.N. Best, I. Smail, J.J. Matthee, B. Darvish, H. Nayyeri, S. Hemmati, J.P. Stott, Monthly Notices of the Royal Astronomical Society 478 (2018) 2999–3015.","ista":"Khostovan AA, Sobral D, Mobasher B, Best PN, Smail I, Matthee JJ, Darvish B, Nayyeri H, Hemmati S, Stott JP. 2018. The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar mass. Monthly Notices of the Royal Astronomical Society. 478(3), 2999–3015.","mla":"Khostovan, A. A., et al. “The Clustering of H β + [O III] and [O II] Emitters since z ∼ 5: Dependencies with Line Luminosity and Stellar Mass.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 478, no. 3, Oxford University Press, 2018, pp. 2999–3015, doi:<a href=\"https://doi.org/10.1093/mnras/sty925\">10.1093/mnras/sty925</a>."},"external_id":{"arxiv":["1705.01101"]},"article_type":"original","issue":"3","status":"public","acknowledgement":"We thank the anonymous referee for their useful comments and suggestions that improved this study. AAK thanks Anahita Alavi and Irene Shivaei for useful discussion in the making of this paper. AAK acknowledges that this work was supported by NASA Headquarters under the NASA Earth and Space Science Fellowship Program – Grant NNX16AO92H. DS acknowledges financial support from the Netherlands Organization for Scientific Research (NWO) through a Veni fellowship and from Lancaster University through an Early Career Internal Grant A100679. PNB is grateful for support from STFC via grant STM001229/1. IRS acknowledges support from STFC (ST/L00075X/1), the ERC Advanced Grant DUSTYGAL (321334), and a Royal Society/Wolfson Merit award. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. BD acknowledges financial support from NASA through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G.","year":"2018","_id":"11549","type":"journal_article","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","page":"2999-3015","volume":478,"extern":"1","abstract":[{"lang":"eng","text":"We investigate the clustering properties of ∼7000 H β + [O III] and [O II] narrowband-selected emitters at z ∼ 0.8–4.7 from the High-z Emission Line Survey. We find clustering lengths, r0, of 1.5–4.0 h−1 Mpc and minimum dark matter halo masses of 1010.7–12.1 M⊙ for our z = 0.8–3.2 H β + [O III] emitters and r0 ∼ 2.0–8.3 h−1 Mpc and halo masses of 1011.5–12.6 M⊙ for our z = 1.5–4.7 [O II] emitters. We find r0 to strongly increase both with increasing line luminosity and redshift. By taking into account the evolution of the characteristic line luminosity, L⋆(z), and using our model predictions of halo mass given r0, we find a strong, redshift-independent increasing trend between L/L⋆(z) and minimum halo mass. The faintest H β + [O III] emitters are found to reside in 109.5 M⊙ haloes and the brightest emitters in 1013.0 M⊙ haloes. For [O II] emitters, the faintest emitters are found in 1010.5 M⊙ haloes and the brightest emitters in 1012.6 M⊙ haloes. A redshift-independent stellar mass dependency is also observed where the halo mass increases from 1011 to 1012.5 M⊙ for stellar masses of 108.5 to 1011.5 M⊙, respectively. We investigate the interdependencies of these trends by repeating our analysis in a Lline−Mstar grid space for our most populated samples (H β + [O III] z = 0.84 and [O II] z = 1.47) and find that the line luminosity dependency is stronger than the stellar mass dependency on halo mass. For L > L⋆ emitters at all epochs, we find a relatively flat trend with halo masses of 1012.5–13 M⊙, which may be due to quenching mechanisms in massive haloes that is consistent with a transitional halo mass predicted by models."}],"arxiv":1,"oa_version":"Published Version","date_created":"2022-07-08T11:48:48Z","publisher":"Oxford University Press","title":"The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar mass","publication":"Monthly Notices of the Royal Astronomical Society","language":[{"iso":"eng"}],"month":"08","day":"01","publication_status":"published","intvolume":"       478","main_file_link":[{"url":"https://arxiv.org/abs/1705.01101"}],"quality_controlled":"1","scopus_import":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: haloes","galaxies: high-redshift","galaxies: star formation","cosmology: observations","large-scale structure of Universe"],"doi":"10.1093/mnras/sty925","date_updated":"2022-08-19T06:53:39Z","article_processing_charge":"No","author":[{"last_name":"Khostovan","first_name":"A A","full_name":"Khostovan, A A"},{"full_name":"Sobral, D","last_name":"Sobral","first_name":"D"},{"full_name":"Mobasher, B","last_name":"Mobasher","first_name":"B"},{"full_name":"Best, P N","first_name":"P N","last_name":"Best"},{"full_name":"Smail, I","last_name":"Smail","first_name":"I"},{"first_name":"Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"full_name":"Darvish, B","first_name":"B","last_name":"Darvish"},{"full_name":"Nayyeri, H","first_name":"H","last_name":"Nayyeri"},{"full_name":"Hemmati, S","first_name":"S","last_name":"Hemmati"},{"full_name":"Stott, J P","first_name":"J P","last_name":"Stott"}],"date_published":"2018-08-01T00:00:00Z"},{"date_updated":"2022-08-19T06:58:06Z","doi":"10.1093/mnras/sty1088","article_processing_charge":"No","author":[{"full_name":"Carniani, S","last_name":"Carniani","first_name":"S"},{"full_name":"Maiolino, R","last_name":"Maiolino","first_name":"R"},{"first_name":"R","last_name":"Amorin","full_name":"Amorin, R"},{"first_name":"L","last_name":"Pentericci","full_name":"Pentericci, L"},{"last_name":"Pallottini","first_name":"A","full_name":"Pallottini, A"},{"full_name":"Ferrara, A","first_name":"A","last_name":"Ferrara"},{"last_name":"Willott","first_name":"C J","full_name":"Willott, C J"},{"full_name":"Smit, R","first_name":"R","last_name":"Smit"},{"orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J"},{"full_name":"Sobral, D","last_name":"Sobral","first_name":"D"},{"first_name":"P","last_name":"Santini","full_name":"Santini, P"},{"full_name":"Castellano, M","first_name":"M","last_name":"Castellano"},{"full_name":"De Barros, S","first_name":"S","last_name":"De Barros"},{"full_name":"Fontana, A","last_name":"Fontana","first_name":"A"},{"full_name":"Grazian, A","last_name":"Grazian","first_name":"A"},{"last_name":"Guaita","first_name":"L","full_name":"Guaita, L"}],"date_published":"2018-07-01T00:00:00Z","quality_controlled":"1","scopus_import":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","galaxies: ISM","galaxies: formation"],"day":"01","language":[{"iso":"eng"}],"month":"07","publication_status":"published","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1712.03985"}],"intvolume":"       478","arxiv":1,"extern":"1","abstract":[{"lang":"eng","text":"We investigate the morphology of the [C II] emission in a sample of ‘normal’ star-forming galaxies at 5 < z < 7.2 in relation to their UV (rest-frame) counterpart. We use new Atacama Large Millimetre/submillimetre Array (ALMA) observations of galaxies at z ∼ 6–7, as well as a careful re-analysis of archival ALMA data. In total 29 galaxies were analysed, 21 of which are detected in [C II]. For several of the latter the [C II] emission breaks into multiple components. Only a fraction of these [C II] components, if any, is associated with the primary UV systems, while the bulk of the [C II] emission is associated either with fainter UV components, or not associated with any UV counterpart at the current limits. By taking into account the presence of all these components, we find that the L[CII]–SFR (star formation rate) relation at early epochs is fully consistent with the local relation, but it has a dispersion of 0.48 ± 0.07 dex, which is about two times larger than observed locally. We also find that the deviation from the local L[CII]–SFR relation has a weak anticorrelation with the EW(Ly α). The morphological analysis also reveals that [C II] emission is generally much more extended than the UV emission. As a consequence, these primordial galaxies are characterized by a [C II] surface brightness generally much lower than expected from the local Σ[CII]−ΣSFR relation. These properties are likely a consequence of a combination of different effects, namely gas metallicity, [C II] emission from obscured star-forming regions, strong variations of the ionization parameter, and circumgalactic gas in accretion or ejected by these primeval galaxies."}],"publisher":"Oxford University Press","title":"Kiloparsec-scale gaseous clumps and star formation at z = 5–7","publication":"Monthly Notices of the Royal Astronomical Society","oa_version":"Preprint","date_created":"2022-07-11T08:05:42Z","external_id":{"arxiv":["1712.03985"]},"article_type":"original","issue":"1","status":"public","oa":1,"acknowledgement":"This paper makes use of the following ALMA data:\r\nADS/JAO.ALMA#2012.1.00719.S, ADS/JAO.ALMA#2012.A.00040.S,\r\nADS/JAO.ALMA#2013.A.00433.S, ADS/JAO.ALMA#2011.0.00115.S,\r\nADS/JAO.ALMA#2012.1.00033.S, ADS/JAO.ALMA#2012.1.00523.S,\r\nADS/JAO.ALMA#2013.1.00815.S, ADS/JAO.ALMA#2015.1.00834.S.,\r\nADS/JAO.ALMA#2015.1.01105.S, AND ADS/JAO.ALMA#2016.1.01240.S\r\nwhich can be retrieved from the ALMA data archive:\r\nhttps://almascience.eso.org/ alma-data/archive. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. We are grateful to G. Jones to for providing his [C II] flux maps. RM and SC acknowledge support by the Science and Technology Facilities Council (STFC). RM acknowledges ERC Advanced Grant 695671 ‘QUENCH’. AF acknowledges support from the ERC Advanced Grant INTERSTELLAR H2020/740120.","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"citation":{"ieee":"S. Carniani <i>et al.</i>, “Kiloparsec-scale gaseous clumps and star formation at z = 5–7,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 478, no. 1. Oxford University Press, pp. 1170–1184, 2018.","chicago":"Carniani, S, R Maiolino, R Amorin, L Pentericci, A Pallottini, A Ferrara, C J Willott, et al. “Kiloparsec-Scale Gaseous Clumps and Star Formation at z = 5–7.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2018. <a href=\"https://doi.org/10.1093/mnras/sty1088\">https://doi.org/10.1093/mnras/sty1088</a>.","apa":"Carniani, S., Maiolino, R., Amorin, R., Pentericci, L., Pallottini, A., Ferrara, A., … Guaita, L. (2018). Kiloparsec-scale gaseous clumps and star formation at z = 5–7. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/sty1088\">https://doi.org/10.1093/mnras/sty1088</a>","ama":"Carniani S, Maiolino R, Amorin R, et al. Kiloparsec-scale gaseous clumps and star formation at z = 5–7. <i>Monthly Notices of the Royal Astronomical Society</i>. 2018;478(1):1170-1184. doi:<a href=\"https://doi.org/10.1093/mnras/sty1088\">10.1093/mnras/sty1088</a>","mla":"Carniani, S., et al. “Kiloparsec-Scale Gaseous Clumps and Star Formation at z = 5–7.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 478, no. 1, Oxford University Press, 2018, pp. 1170–84, doi:<a href=\"https://doi.org/10.1093/mnras/sty1088\">10.1093/mnras/sty1088</a>.","ista":"Carniani S, Maiolino R, Amorin R, Pentericci L, Pallottini A, Ferrara A, Willott CJ, Smit R, Matthee JJ, Sobral D, Santini P, Castellano M, De Barros S, Fontana A, Grazian A, Guaita L. 2018. Kiloparsec-scale gaseous clumps and star formation at z = 5–7. Monthly Notices of the Royal Astronomical Society. 478(1), 1170–1184.","short":"S. Carniani, R. Maiolino, R. Amorin, L. Pentericci, A. Pallottini, A. Ferrara, C.J. Willott, R. Smit, J.J. Matthee, D. Sobral, P. Santini, M. Castellano, S. De Barros, A. Fontana, A. Grazian, L. Guaita, Monthly Notices of the Royal Astronomical Society 478 (2018) 1170–1184."},"type":"journal_article","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","page":"1170-1184","volume":478,"year":"2018","_id":"11555"},{"intvolume":"       477","main_file_link":[{"url":"https://arxiv.org/abs/1802.10102","open_access":"1"}],"publication_status":"published","month":"06","language":[{"iso":"eng"}],"day":"01","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: active","galaxies: evolution","galaxies: high-redshift","galaxies: ISM","galaxies: starburst","cosmology: observations"],"scopus_import":"1","quality_controlled":"1","author":[{"full_name":"Sobral, David","first_name":"David","last_name":"Sobral"},{"orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J"},{"last_name":"Darvish","first_name":"Behnam","full_name":"Darvish, Behnam"},{"full_name":"Smail, Ian","last_name":"Smail","first_name":"Ian"},{"full_name":"Best, Philip N","last_name":"Best","first_name":"Philip N"},{"first_name":"Lara","last_name":"Alegre","full_name":"Alegre, Lara"},{"last_name":"Röttgering","first_name":"Huub","full_name":"Röttgering, Huub"},{"full_name":"Mobasher, Bahram","first_name":"Bahram","last_name":"Mobasher"},{"last_name":"Paulino-Afonso","first_name":"Ana","full_name":"Paulino-Afonso, Ana"},{"full_name":"Stroe, Andra","last_name":"Stroe","first_name":"Andra"},{"full_name":"Oteo, Iván","first_name":"Iván","last_name":"Oteo"}],"date_published":"2018-06-01T00:00:00Z","article_processing_charge":"No","date_updated":"2022-08-19T07:01:08Z","doi":"10.1093/mnras/sty782","_id":"11557","year":"2018","volume":477,"page":"2817-2840","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","type":"journal_article","citation":{"ama":"Sobral D, Matthee JJ, Darvish B, et al. The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN. <i>Monthly Notices of the Royal Astronomical Society</i>. 2018;477(2):2817-2840. doi:<a href=\"https://doi.org/10.1093/mnras/sty782\">10.1093/mnras/sty782</a>","mla":"Sobral, David, et al. “The Nature of Luminous Ly α Emitters at z ∼ 2–3: Maximal Dust-Poor Starbursts and Highly Ionizing AGN.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 477, no. 2, Oxford University Press, 2018, pp. 2817–40, doi:<a href=\"https://doi.org/10.1093/mnras/sty782\">10.1093/mnras/sty782</a>.","short":"D. Sobral, J.J. Matthee, B. Darvish, I. Smail, P.N. Best, L. Alegre, H. Röttgering, B. Mobasher, A. Paulino-Afonso, A. Stroe, I. Oteo, Monthly Notices of the Royal Astronomical Society 477 (2018) 2817–2840.","ista":"Sobral D, Matthee JJ, Darvish B, Smail I, Best PN, Alegre L, Röttgering H, Mobasher B, Paulino-Afonso A, Stroe A, Oteo I. 2018. The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN. Monthly Notices of the Royal Astronomical Society. 477(2), 2817–2840.","ieee":"D. Sobral <i>et al.</i>, “The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 477, no. 2. Oxford University Press, pp. 2817–2840, 2018.","chicago":"Sobral, David, Jorryt J Matthee, Behnam Darvish, Ian Smail, Philip N Best, Lara Alegre, Huub Röttgering, et al. “The Nature of Luminous Ly α Emitters at z ∼ 2–3: Maximal Dust-Poor Starbursts and Highly Ionizing AGN.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2018. <a href=\"https://doi.org/10.1093/mnras/sty782\">https://doi.org/10.1093/mnras/sty782</a>.","apa":"Sobral, D., Matthee, J. J., Darvish, B., Smail, I., Best, P. N., Alegre, L., … Oteo, I. (2018). The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/sty782\">https://doi.org/10.1093/mnras/sty782</a>"},"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"oa":1,"status":"public","acknowledgement":"We thank the anonymous reviewer for their timely and constructive comments that greatly helped us to improve the manuscript. DS acknowledges financial support from the Netherlands Organization for Scientific research (NWO) through a Veni fellowship and from Lancaster University through an Early Career Internal Grant A100679. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. BD acknowledges financial support from NASA through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G, and the National Science Foundation, grant number 1716907. IRS acknowledges support from the ERC Advanced Grant DUSTYGAL (321334), STFC (ST/P000541/1), and a Royal Society/Wolfson Merit Award. PNB is grateful for support from STFC via grant ST/M001229/1. We thank Anne Verhamme, Kimihiko Nakajima, Ryan Trainor, Sangeeta Malhotra, Max Gronke, James Rhoads, Fang Xia An, Matthew Hayes, Takashi Kojima, Mark Dijkstra, and Anne Jaskot for many helpful and engaging discussions, particularly during the SnowCLAW Ly α workshop. We thank Bruno Ribeiro, Stephane Charlot, and Joseph Caruana for comments on the manuscript. The authors would also like to thank Ingrid Tengs, Meg Singleton, Ali Khostovan, and Sara Perez for participating in part of the observations. We also thank Joao Calhau, Leah Morabito, Sergio Santos, and Aayush Saxena for their assistance with the narrow-band observations which allowed to select some of the sour ces. Based on observations obtained with the William Herschel Telescope, program: W16AN004; the Very Large Telescope, programs: 098.A-0819 & 099.A-0254; and the Keck II telescope, program: C267D. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme IDs 294.A-5018, 294.A-5039, 092.A-0786, 093.A-0561, 097.A-0943, 098.A-0819, 099.A-0254 and 179.A-2005. The authors acknowledge the award of service time (SW2014b20) on the 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. The authors would also like to thank all the extremely helpful observatory staff that have greatly contributed towards our observations, particularly Fiona Riddick, Lilian Dominguez, Florencia Jimenez, and Ian Skillen. We have benefited greatly from the publicly available programming language PYTHON, including the NUMPY & SCIPY (Van Der Walt, Colbert & Varoquaux 2011; Jones et al. 2001), MATPLOTLIB (Hunter 2007), ASTROPY (Astropy Collaboration et al. 2013), and the TOPCAT analysis program (Taylor 2013). This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France.","issue":"2","external_id":{"arxiv":["1802.10102"]},"article_type":"original","date_created":"2022-07-12T07:18:02Z","oa_version":"Preprint","publication":"Monthly Notices of the Royal Astronomical Society","title":"The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN","publisher":"Oxford University Press","abstract":[{"lang":"eng","text":"Deep narrow-band surveys have revealed a large population of faint Ly α emitters (LAEs) in the distant Universe, but relatively little is known about the most luminous sources (⁠LLyα≳1042.7 erg s−1; LLyα≳L∗Lyα⁠). Here we present the spectroscopic follow-up of 21 luminous LAEs at z ∼ 2–3 found with panoramic narrow-band surveys over five independent extragalactic fields (≈4 × 106 Mpc3 surveyed at z ∼ 2.2 and z ∼ 3.1). We use WHT/ISIS, Keck/DEIMOS, and VLT/X-SHOOTER to study these sources using high ionization UV lines. Luminous LAEs at z ∼ 2–3 have blue UV slopes (⁠β=−2.0+0.3−0.1⁠) and high Ly α escape fractions (⁠50+20−15 per cent) and span five orders of magnitude in UV luminosity (MUV ≈ −19 to −24). Many (70 per cent) show at least one high ionization rest-frame UV line such as C IV, N V, C III], He II or O III], typically blue-shifted by ≈100–200 km s−1 relative to Ly α. Their Ly α profiles reveal a wide variety of shapes, including significant blue-shifted components and widths from 200 to 4000 km s−1. Overall, 60 ± 11  per cent appear to be active galactic nucleus (AGN) dominated, and at LLyα > 1043.3 erg s−1 and/or MUV < −21.5 virtually all LAEs are AGNs with high ionization parameters (log U = 0.6 ± 0.5) and with metallicities of ≈0.5 − 1 Z⊙. Those lacking signatures of AGNs (40 ± 11  per cent) have lower ionization parameters (⁠logU=−3.0+1.6−0.9 and log ξion = 25.4 ± 0.2) and are apparently metal-poor sources likely powered by young, dust-poor ‘maximal’ starbursts. Our results show that luminous LAEs at z ∼ 2–3 are a diverse population and that 2×L∗Lyα and 2×M∗UV mark a sharp transition in the nature of LAEs, from star formation dominated to AGN dominated."}],"extern":"1","arxiv":1},{"publication":"Monthly Notices of the Royal Astronomical Society","title":"Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6","publisher":"Oxford University Press","date_created":"2022-07-12T10:41:08Z","oa_version":"Preprint","arxiv":1,"abstract":[{"lang":"eng","text":"We present and explore deep narrow- and medium-band data obtained with the Subaru and the Isaac Newton Telescopes in the ∼2 deg2 COSMOS field. We use these data as an extremely wide, low-resolution (R ∼ 20–80) Integral Field Unit survey to slice through the COSMOS field and obtain a large sample of ∼4000 Ly α emitters (LAEs) from z ∼ 2 to 6 in 16 redshift slices (SC4K). We present new Ly α luminosity functions (LFs) covering a comoving volume of ∼108 Mpc3. SC4K extensively complements ultradeep surveys, jointly covering over 4 dex in Ly α luminosity and revealing a global (2.5 < z < 6) synergy LF with α=−1.93+0.12−0.12⁠, log10Φ∗Lyα=−3.45+0.22−0.29 Mpc−3, and log10L∗Lyα=42.93+0.15−0.11 erg s−1. The Schechter component of the Ly α LF reveals a factor ∼5 rise in L∗Lyα and a ∼7 × decline in Φ∗Lyα from z ∼ 2 to 6. The data reveal an extra power-law (or Schechter) component above LLy α ≈ 1043.3 erg s−1 at z ∼ 2.2–3.5 and we show that it is partially driven by X-ray and radio active galactic nucleus (AGN), as their Ly α LF resembles the excess. The power-law component vanishes and/or is below our detection limits above z > 3.5, likely linked with the evolution of the AGN population. The Ly α luminosity density rises by a factor ∼2 from z ∼ 2 to 3 but is then found to be roughly constant (⁠1.1+0.2−0.2×1040 erg s−1 Mpc−3) to z ∼ 6, despite the ∼0.7 dex drop in ultraviolet (UV) luminosity density. The Ly α/UV luminosity density ratio rises from 4 ± 1 per cent to 30 ± 6 per cent from z ∼ 2.2 to 6. Our results imply a rise of a factor of ≈2 in the global ionization efficiency (ξion) and a factor ≈4 ± 1 in the Ly α escape fraction from z ∼ 2 to 6, hinting for evolution in both the typical burstiness/stellar populations and even more so in the typical interstellar medium conditions allowing Ly α photons to escape."}],"extern":"1","volume":476,"page":"4725-4752","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","type":"journal_article","_id":"11558","year":"2018","acknowledgement":"We thank the anonymous referee for their constructive comments that helped us improve the manuscript. DS acknowledges the hospitality of the IAC and a Severo Ochoa visiting grant. SS and JC acknowledge studentships from the Lancaster University. JM acknowledges a Huygens PhD fellowship from Leiden University. APA acknowledges financial support from the Science and Technology Foundation (FCT, Portugal) through research grants UID/FIS/04434/2013 and fellowship PD/BD/52706/2014. The authors thank Alyssa Drake, Kimihiko Nakajima, Yuichi Harikane, Max Gronke, Irene Shivaei, Helmut Dannerbauer, Huub Rottgering, ¨ Marius Eide, and Masami Ouchi for many engaging and stimulating discussions. We also thank Sara Perez, Alex Bennett, and Tom Rose for their involvement in the early stages of this project. Based on data products from observations made with European Southern Observatory (ESO) Telescopes at the La Silla Paranal Observatory under ESO programme IDs 294.A-5018, 097.A 0943,\r\n098.A-0819, 099.A-0254, and 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. Based on observations using the WFC on the 2.5 m INT, as part of programmes 2013AN002, 2013BN008, 2014AC88, 2014AN002, 2014BN006, 2014BC118, and 2016AN001. The 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. 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 (CFHTLS), a collaborative project of NRC and CNRS.\r\nWe are grateful to the CFHTLS, COSMOS-UltraVISTA, and COSMOS survey teams. We are also unmeasurably thankful to the pioneering and continuous work from previous Ly α surveys’ teams. Without these previous Ly α and the wider reach legacy surveys, this research would have been impossible. We also thank the VUDS team for making available spectroscopic redshifts from data obtained with VIMOS at the European Southern Observatory Very Large Telescope, Paranal, Chile, under Large Programme 185.A-0791. Finally, the authors acknowledge the unique value of the publicly available programming language PYTHON, including the NUMPY and SCIPY (Van Der Walt, Colbert & Varoquaux 2011; Jones et al. 2001), MATPLOTLIB (Hunter 2007), ASTROPY (Astropy Collaboration et al. 2013), and the TOPCAT analysis program (Taylor 2005). We publicly release a catalogue with all LAEs used in this paper (SC4K), so it can be freely explored by the community (see five example entries in Table A1).","oa":1,"status":"public","issue":"4","external_id":{"arxiv":["1712.04451"]},"article_type":"original","citation":{"ieee":"D. Sobral <i>et al.</i>, “Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 476, no. 4. Oxford University Press, pp. 4725–4752, 2018.","chicago":"Sobral, David, Sérgio Santos, Jorryt J Matthee, Ana Paulino-Afonso, Bruno Ribeiro, João Calhau, and Ali A Khostovan. “Slicing COSMOS with SC4K: The Evolution of Typical Ly α Emitters and the Ly α Escape Fraction from z ∼ 2 to 6.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2018. <a href=\"https://doi.org/10.1093/mnras/sty378\">https://doi.org/10.1093/mnras/sty378</a>.","apa":"Sobral, D., Santos, S., Matthee, J. J., Paulino-Afonso, A., Ribeiro, B., Calhau, J., &#38; Khostovan, A. A. (2018). Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/sty378\">https://doi.org/10.1093/mnras/sty378</a>","ama":"Sobral D, Santos S, Matthee JJ, et al. Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6. <i>Monthly Notices of the Royal Astronomical Society</i>. 2018;476(4):4725-4752. doi:<a href=\"https://doi.org/10.1093/mnras/sty378\">10.1093/mnras/sty378</a>","short":"D. Sobral, S. Santos, J.J. Matthee, A. Paulino-Afonso, B. Ribeiro, J. Calhau, A.A. Khostovan, Monthly Notices of the Royal Astronomical Society 476 (2018) 4725–4752.","mla":"Sobral, David, et al. “Slicing COSMOS with SC4K: The Evolution of Typical Ly α Emitters and the Ly α Escape Fraction from z ∼ 2 to 6.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 476, no. 4, Oxford University Press, 2018, pp. 4725–52, doi:<a href=\"https://doi.org/10.1093/mnras/sty378\">10.1093/mnras/sty378</a>.","ista":"Sobral D, Santos S, Matthee JJ, Paulino-Afonso A, Ribeiro B, Calhau J, Khostovan AA. 2018. Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6. Monthly Notices of the Royal Astronomical Society. 476(4), 4725–4752."},"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"date_published":"2018-06-01T00:00:00Z","author":[{"full_name":"Sobral, David","first_name":"David","last_name":"Sobral"},{"full_name":"Santos, Sérgio","first_name":"Sérgio","last_name":"Santos"},{"full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee"},{"full_name":"Paulino-Afonso, Ana","last_name":"Paulino-Afonso","first_name":"Ana"},{"last_name":"Ribeiro","first_name":"Bruno","full_name":"Ribeiro, Bruno"},{"first_name":"João","last_name":"Calhau","full_name":"Calhau, João"},{"full_name":"Khostovan, Ali A","first_name":"Ali A","last_name":"Khostovan"}],"article_processing_charge":"No","date_updated":"2022-08-19T07:04:45Z","doi":"10.1093/mnras/sty378","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: formation","galaxies: high-redshift","galaxies: luminosity function","mass function","galaxies: statistics"],"scopus_import":"1","quality_controlled":"1","intvolume":"       476","main_file_link":[{"url":"https://arxiv.org/abs/1712.04451","open_access":"1"}],"publication_status":"published","day":"01","month":"06","language":[{"iso":"eng"}]},{"day":"01","language":[{"iso":"eng"}],"month":"09","publication_status":"published","intvolume":"       479","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1802.06786"}],"date_updated":"2022-08-19T08:35:45Z","doi":"10.1093/mnrasl/sly093","article_processing_charge":"No","date_published":"2018-09-01T00:00:00Z","author":[{"full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee"},{"full_name":"Schaye, Joop","first_name":"Joop","last_name":"Schaye"}],"quality_controlled":"1","scopus_import":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: abundances","galaxies: evolution","galaxies: formation","galaxies: star formation"],"external_id":{"arxiv":["1802.06786"]},"article_type":"original","issue":"1","oa":1,"acknowledgement":"We thank the anonymous referee for their constructive comments. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. We thank Jarle Brinchmann, Rob Crain and David Sobral for discussions. We acknowledge the use of the TOPCAT software (Taylor 2013) for assisting in rapid exploration of multidimensional data sets and the use of PYTHON and its NUMPY, MATPLOTLIB, and PANDAS packages.","status":"public","publication_identifier":{"issn":["1745-3925"],"eissn":["1745-3933"]},"citation":{"apa":"Matthee, J. J., &#38; Schaye, J. (2018). Star-forming galaxies are predicted to lie on a fundamental plane of mass, star formation rate, and α-enhancement. <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnrasl/sly093\">https://doi.org/10.1093/mnrasl/sly093</a>","ieee":"J. J. Matthee and J. Schaye, “Star-forming galaxies are predicted to lie on a fundamental plane of mass, star formation rate, and α-enhancement,” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>, vol. 479, no. 1. Oxford University Press, pp. L34–L39, 2018.","chicago":"Matthee, Jorryt J, and Joop Schaye. “Star-Forming Galaxies Are Predicted to Lie on a Fundamental Plane of Mass, Star Formation Rate, and α-Enhancement.” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. Oxford University Press, 2018. <a href=\"https://doi.org/10.1093/mnrasl/sly093\">https://doi.org/10.1093/mnrasl/sly093</a>.","ista":"Matthee JJ, Schaye J. 2018. Star-forming galaxies are predicted to lie on a fundamental plane of mass, star formation rate, and α-enhancement. Monthly Notices of the Royal Astronomical Society: Letters. 479(1), L34–L39.","short":"J.J. Matthee, J. Schaye, Monthly Notices of the Royal Astronomical Society: Letters 479 (2018) L34–L39.","mla":"Matthee, Jorryt J., and Joop Schaye. “Star-Forming Galaxies Are Predicted to Lie on a Fundamental Plane of Mass, Star Formation Rate, and α-Enhancement.” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>, vol. 479, no. 1, Oxford University Press, 2018, pp. L34–39, doi:<a href=\"https://doi.org/10.1093/mnrasl/sly093\">10.1093/mnrasl/sly093</a>.","ama":"Matthee JJ, Schaye J. Star-forming galaxies are predicted to lie on a fundamental plane of mass, star formation rate, and α-enhancement. <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. 2018;479(1):L34-L39. doi:<a href=\"https://doi.org/10.1093/mnrasl/sly093\">10.1093/mnrasl/sly093</a>"},"type":"journal_article","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","page":"L34 - L39","volume":479,"year":"2018","_id":"11584","arxiv":1,"extern":"1","abstract":[{"lang":"eng","text":"Observations show that star-forming galaxies reside on a tight 3D plane between mass, gas-phase metallicity, and star formation rate (SFR), which can be explained by the interplay between metal-poor gas inflows, SFR and outflows. However, different metals are released on different time-scales, which may affect the slope of this relation. Here, we use central, star-forming galaxies with Mstar = 109.0–10.5 M⊙ from the EAGLE hydrodynamical simulation to examine 3D relations between mass, SFR, and chemical enrichment using absolute and relative C, N, O, and Fe abundances. We show that the scatter is smaller when gas-phase α-enhancement is used rather than metallicity. A similar plane also exists for stellar α-enhancement, implying that present-day specific SFRs are correlated with long time-scale star formation histories. Between z = 0 and 1, the α-enhancement plane is even more insensitive to redshift than the plane using metallicity. However, it evolves at z > 1 due to lagging iron yields. At fixed mass, galaxies with higher SFRs have star formation histories shifted towards late times, are more α-enhanced, and this α-enhancement increases with redshift as observed. These findings suggest that relations between physical properties inferred from observations may be affected by systematic variations in α-enhancements."}],"publisher":"Oxford University Press","title":"Star-forming galaxies are predicted to lie on a fundamental plane of mass, star formation rate, and α-enhancement","publication":"Monthly Notices of the Royal Astronomical Society: Letters","oa_version":"Preprint","date_created":"2022-07-14T12:49:47Z"},{"volume":620,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","type":"journal_article","_id":"11618","year":"2018","status":"public","oa":1,"acknowledgement":"We thank the anonymous referee for the very useful comments. We would also like to thank M. Benbakoura for his help in analyzing the light curves of several binary systems included in our set of stars. L.B. and R.A.G. acknowledge the support from PLATO and GOLF CNES grants. S.M. acknowledges support from the National Aeronautics and Space Administration under Grant NNX15AF13G, the National Science Foundation grant AST-1411685, and the Ramon y Cajal fellowship no. RYC-2015-17697. E.C. is funded by the European Union’s Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement no. 664931. O.J.H and B.M.R. acknowledge the support of the UK Science and Technology Facilities Council (STFC). Funding for the Stellar Astrophysics Centre is provided by the Danish National Research Foundation (Grant DNRF106). This research has made use of NASA’s Astrophysics Data System. Data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555.","external_id":{"arxiv":["1809.05105"]},"article_type":"original","citation":{"apa":"Bugnet, L. A., García, R. A., Davies, G. R., Mathur, S., Corsaro, E., Hall, O. J., &#38; Rendle, B. M. (2018). FliPer: A global measure of power density to estimate surface gravities of main-sequence solar-like stars and red giants. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201833106\">https://doi.org/10.1051/0004-6361/201833106</a>","chicago":"Bugnet, Lisa Annabelle, R. A. García, G. R. Davies, S. Mathur, E. Corsaro, O. J. Hall, and B. M. Rendle. “FliPer: A Global Measure of Power Density to Estimate Surface Gravities of Main-Sequence Solar-like Stars and Red Giants.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2018. <a href=\"https://doi.org/10.1051/0004-6361/201833106\">https://doi.org/10.1051/0004-6361/201833106</a>.","ieee":"L. A. Bugnet <i>et al.</i>, “FliPer: A global measure of power density to estimate surface gravities of main-sequence solar-like stars and red giants,” <i>Astronomy &#38; Astrophysics</i>, vol. 620. EDP Sciences, 2018.","mla":"Bugnet, Lisa Annabelle, et al. “FliPer: A Global Measure of Power Density to Estimate Surface Gravities of Main-Sequence Solar-like Stars and Red Giants.” <i>Astronomy &#38; Astrophysics</i>, vol. 620, A38, EDP Sciences, 2018, doi:<a href=\"https://doi.org/10.1051/0004-6361/201833106\">10.1051/0004-6361/201833106</a>.","ista":"Bugnet LA, García RA, Davies GR, Mathur S, Corsaro E, Hall OJ, Rendle BM. 2018. FliPer: A global measure of power density to estimate surface gravities of main-sequence solar-like stars and red giants. Astronomy &#38; Astrophysics. 620, A38.","short":"L.A. Bugnet, R.A. García, G.R. Davies, S. Mathur, E. Corsaro, O.J. Hall, B.M. Rendle, Astronomy &#38; Astrophysics 620 (2018).","ama":"Bugnet LA, García RA, Davies GR, et al. FliPer: A global measure of power density to estimate surface gravities of main-sequence solar-like stars and red giants. <i>Astronomy &#38; Astrophysics</i>. 2018;620. doi:<a href=\"https://doi.org/10.1051/0004-6361/201833106\">10.1051/0004-6361/201833106</a>"},"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"publication":"Astronomy & Astrophysics","title":"FliPer: A global measure of power density to estimate surface gravities of main-sequence solar-like stars and red giants","publisher":"EDP Sciences","date_created":"2022-07-18T14:37:39Z","oa_version":"Preprint","arxiv":1,"abstract":[{"lang":"eng","text":"Asteroseismology provides global stellar parameters such as masses, radii, or surface gravities using mean global seismic parameters and effective temperature for thousands of low-mass stars (0.8 M⊙ < M < 3 M⊙). This methodology has been successfully applied to stars in which acoustic modes excited by turbulent convection are measured. Other methods such as the Flicker technique can also be used to determine stellar surface gravities, but only works for log g above 2.5 dex. In this work, we present a new metric called FliPer (Flicker in spectral power density, in opposition to the standard Flicker measurement which is computed in the time domain); it is able to extend the range for which reliable surface gravities can be obtained (0.1 < log g < 4.6 dex) without performing any seismic analysis for stars brighter than Kp < 14. FliPer takes into account the average variability of a star measured in the power density spectrum in a given range of frequencies. However, FliPer values calculated on several ranges of frequency are required to better characterize a star. Using a large set of asteroseismic targets it is possible to calibrate the behavior of surface gravity with FliPer through machine learning. This calibration made with a random forest regressor covers a wide range of surface gravities from main-sequence stars to subgiants and red giants, with very small uncertainties from 0.04 to 0.1 dex. FliPer values can be inserted in automatic global seismic pipelines to either give an estimation of the stellar surface gravity or to assess the quality of the seismic results by detecting any outliers in the obtained νmax values. FliPer also constrains the surface gravities of main-sequence dwarfs using only long-cadence data for which the Nyquist frequency is too low to measure the acoustic-mode properties."}],"extern":"1","intvolume":"       620","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1809.05105"}],"publication_status":"published","day":"01","month":"12","language":[{"iso":"eng"}],"article_number":"A38","author":[{"id":"d9edb345-f866-11ec-9b37-d119b5234501","full_name":"Bugnet, Lisa Annabelle","orcid":"0000-0003-0142-4000","last_name":"Bugnet","first_name":"Lisa Annabelle"},{"last_name":"García","first_name":"R. A.","full_name":"García, R. A."},{"full_name":"Davies, G. R.","last_name":"Davies","first_name":"G. R."},{"first_name":"S.","last_name":"Mathur","full_name":"Mathur, S."},{"last_name":"Corsaro","first_name":"E.","full_name":"Corsaro, E."},{"full_name":"Hall, O. J.","first_name":"O. J.","last_name":"Hall"},{"last_name":"Rendle","first_name":"B. M.","full_name":"Rendle, B. M."}],"date_published":"2018-12-01T00:00:00Z","article_processing_charge":"No","doi":"10.1051/0004-6361/201833106","date_updated":"2022-08-22T07:41:07Z","keyword":["Space and Planetary Science","Astronomy and Astrophysics","asteroseismology / methods","data analysis / stars","oscillations"],"scopus_import":"1","quality_controlled":"1"},{"language":[{"iso":"eng"}],"month":"11","day":"22","publication_status":"published","intvolume":"       619","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1809.07573"}],"quality_controlled":"1","scopus_import":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics","planetary systems / planets and satellites","detection / planets and satellites","fundamental parameters / planets and satellites","terrestrial planets / stars","fundamental parameters"],"date_updated":"2022-08-22T07:43:29Z","doi":"10.1051/0004-6361/201834289","article_processing_charge":"No","author":[{"full_name":"Gandolfi, D.","last_name":"Gandolfi","first_name":"D."},{"full_name":"Barragán, O.","first_name":"O.","last_name":"Barragán"},{"last_name":"Livingston","first_name":"J. H.","full_name":"Livingston, J. H."},{"last_name":"Fridlund","first_name":"M.","full_name":"Fridlund, M."},{"first_name":"A. B.","last_name":"Justesen","full_name":"Justesen, A. B."},{"full_name":"Redfield, S.","last_name":"Redfield","first_name":"S."},{"full_name":"Fossati, L.","first_name":"L.","last_name":"Fossati"},{"first_name":"S.","last_name":"Mathur","full_name":"Mathur, S."},{"last_name":"Grziwa","first_name":"S.","full_name":"Grziwa, S."},{"full_name":"Cabrera, J.","first_name":"J.","last_name":"Cabrera"},{"full_name":"García, R. A.","last_name":"García","first_name":"R. A."},{"full_name":"Persson, C. M.","last_name":"Persson","first_name":"C. M."},{"full_name":"Van Eylen, V.","first_name":"V.","last_name":"Van Eylen"},{"last_name":"Hatzes","first_name":"A. P.","full_name":"Hatzes, A. P."},{"first_name":"D.","last_name":"Hidalgo","full_name":"Hidalgo, D."},{"full_name":"Albrecht, S.","first_name":"S.","last_name":"Albrecht"},{"first_name":"Lisa Annabelle","last_name":"Bugnet","orcid":"0000-0003-0142-4000","full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501"},{"first_name":"W. D.","last_name":"Cochran","full_name":"Cochran, W. D."},{"full_name":"Csizmadia, Sz.","last_name":"Csizmadia","first_name":"Sz."},{"first_name":"H.","last_name":"Deeg","full_name":"Deeg, H."},{"first_name":"Ph.","last_name":"Eigmüller","full_name":"Eigmüller, Ph."},{"first_name":"M.","last_name":"Endl","full_name":"Endl, M."},{"last_name":"Erikson","first_name":"A.","full_name":"Erikson, A."},{"full_name":"Esposito, M.","first_name":"M.","last_name":"Esposito"},{"full_name":"Guenther, E.","last_name":"Guenther","first_name":"E."},{"full_name":"Korth, J.","first_name":"J.","last_name":"Korth"},{"full_name":"Luque, R.","last_name":"Luque","first_name":"R."},{"last_name":"Montañes Rodríguez","first_name":"P.","full_name":"Montañes Rodríguez, P."},{"last_name":"Nespral","first_name":"D.","full_name":"Nespral, D."},{"first_name":"G.","last_name":"Nowak","full_name":"Nowak, G."},{"full_name":"Pätzold, M.","last_name":"Pätzold","first_name":"M."},{"first_name":"J.","last_name":"Prieto-Arranz","full_name":"Prieto-Arranz, J."}],"date_published":"2018-11-22T00:00:00Z","article_number":"L10","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"citation":{"short":"D. Gandolfi, O. Barragán, J.H. Livingston, M. Fridlund, A.B. Justesen, S. Redfield, L. Fossati, S. Mathur, S. Grziwa, J. Cabrera, R.A. García, C.M. Persson, V. Van Eylen, A.P. Hatzes, D. Hidalgo, S. Albrecht, L.A. Bugnet, W.D. Cochran, S. Csizmadia, H. Deeg, P. Eigmüller, M. Endl, A. Erikson, M. Esposito, E. Guenther, J. Korth, R. Luque, P. Montañes Rodríguez, D. Nespral, G. Nowak, M. Pätzold, J. Prieto-Arranz, Astronomy &#38; Astrophysics 619 (2018).","ista":"Gandolfi D, Barragán O, Livingston JH, Fridlund M, Justesen AB, Redfield S, Fossati L, Mathur S, Grziwa S, Cabrera J, García RA, Persson CM, Van Eylen V, Hatzes AP, Hidalgo D, Albrecht S, Bugnet LA, Cochran WD, Csizmadia S, Deeg H, Eigmüller P, Endl M, Erikson A, Esposito M, Guenther E, Korth J, Luque R, Montañes Rodríguez P, Nespral D, Nowak G, Pätzold M, Prieto-Arranz J. 2018. TESS’s first planet: A super-Earth transiting the naked-eye star π Mensae. Astronomy &#38; Astrophysics. 619, L10.","mla":"Gandolfi, D., et al. “TESS’s First Planet: A Super-Earth Transiting the Naked-Eye Star π Mensae.” <i>Astronomy &#38; Astrophysics</i>, vol. 619, L10, EDP Sciences, 2018, doi:<a href=\"https://doi.org/10.1051/0004-6361/201834289\">10.1051/0004-6361/201834289</a>.","ama":"Gandolfi D, Barragán O, Livingston JH, et al. TESS’s first planet: A super-Earth transiting the naked-eye star π Mensae. <i>Astronomy &#38; Astrophysics</i>. 2018;619. doi:<a href=\"https://doi.org/10.1051/0004-6361/201834289\">10.1051/0004-6361/201834289</a>","apa":"Gandolfi, D., Barragán, O., Livingston, J. H., Fridlund, M., Justesen, A. B., Redfield, S., … Prieto-Arranz, J. (2018). TESS’s first planet: A super-Earth transiting the naked-eye star π Mensae. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201834289\">https://doi.org/10.1051/0004-6361/201834289</a>","ieee":"D. Gandolfi <i>et al.</i>, “TESS’s first planet: A super-Earth transiting the naked-eye star π Mensae,” <i>Astronomy &#38; Astrophysics</i>, vol. 619. EDP Sciences, 2018.","chicago":"Gandolfi, D., O. Barragán, J. H. Livingston, M. Fridlund, A. B. Justesen, S. Redfield, L. Fossati, et al. “TESS’s First Planet: A Super-Earth Transiting the Naked-Eye Star π Mensae.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2018. <a href=\"https://doi.org/10.1051/0004-6361/201834289\">https://doi.org/10.1051/0004-6361/201834289</a>."},"external_id":{"arxiv":["1809.07573"]},"article_type":"letter_note","oa":1,"status":"public","year":"2018","_id":"11619","type":"journal_article","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","volume":619,"extern":"1","abstract":[{"lang":"eng","text":"We report on the confirmation and mass determination of π Men c, the first transiting planet discovered by NASA’s TESS space mission. π Men is a naked-eye (V = 5.65 mag), quiet G0 V star that was previously known to host a sub-stellar companion (π Men b) on a longperiod (Porb = 2091 days), eccentric (e = 0.64) orbit. Using TESS time-series photometry, combined with Gaia data, published UCLES at AAT Doppler measurements, and archival HARPS at ESO-3.6m radial velocities, we found that π Men c is a close-in planet with an orbital period of Porb = 6.27 days, a mass of Mc = 4.52 ± 0.81 M⊕, and a radius of Rc = 2.06 ± 0.03 R⊕. Based on the planet’s orbital period and size, π Men c is a super-Earth located at, or close to, the radius gap, while its mass and bulk density suggest it may have held on to a significant atmosphere. Because of the brightness of the host star, this system is highly suitable for a wide range of further studies to characterize the planetary atmosphere and dynamical properties. We also performed an asteroseismic analysis of the TESS data and detected a hint of power excess consistent with the seismic values expected for this star, although this result depends on the photometric aperture used to extract the light curve. This marginal detection is expected from pre-launch simulations hinting at the asteroseismic potential of the TESS mission for longer, multi-sector observations and/or for more evolved bright stars."}],"arxiv":1,"oa_version":"Preprint","date_created":"2022-07-18T14:41:16Z","publisher":"EDP Sciences","title":"TESS’s first planet: A super-Earth transiting the naked-eye star π Mensae","publication":"Astronomy & Astrophysics"},{"oa_version":"Preprint","date_created":"2022-07-18T14:43:17Z","title":"HD 89345: A bright oscillating star hosting a transiting warm Saturn-sized planet observed by K2","publication":"Monthly Notices of the Royal Astronomical Society","publisher":"Oxford University Press","abstract":[{"text":"We report the discovery and characterization of HD 89345b (K2-234b; EPIC 248777106b), a Saturn-sized planet orbiting a slightly evolved star. HD 89345 is a bright star (V = 9.3 mag) observed by the K2 mission with 1 min time sampling. It exhibits solar-like oscillations. We conducted asteroseismology to determine the parameters of the star, finding the mass and radius to be 1.12+0.04−0.01M⊙ and 1.657+0.020−0.004R⊙⁠, respectively. The star appears to have recently left the main sequence, based on the inferred age, 9.4+0.4−1.3Gyr⁠, and the non-detection of mixed modes. The star hosts a ‘warm Saturn’ (P = 11.8 d, Rp = 6.86 ± 0.14 R⊕). Radial-velocity follow-up observations performed with the FIbre-fed Echelle Spectrograph, HARPS, and HARPS-N spectrographs show that the planet has a mass of 35.7 ± 3.3 M⊕. The data also show that the planet’s orbit is eccentric (e ≈ 0.2). An investigation of the rotational splitting of the oscillation frequencies of the star yields no conclusive evidence on the stellar inclination angle. We further obtained Rossiter–McLaughlin observations, which result in a broad posterior of the stellar obliquity. The planet seems to confirm to the same patterns that have been observed for other sub-Saturns regarding planet mass and multiplicity, orbital eccentricity, and stellar metallicity.","lang":"eng"}],"extern":"1","arxiv":1,"_id":"11620","year":"2018","page":"4866-4880","volume":478,"type":"journal_article","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"short":"V. Van Eylen, F. Dai, S. Mathur, D. Gandolfi, S. Albrecht, M. Fridlund, R.A. García, E. Guenther, M. Hjorth, A.B. Justesen, J. Livingston, M.N. Lund, F. Pérez Hernández, J. Prieto-Arranz, C. Regulo, L.A. Bugnet, M.E. Everett, T. Hirano, D. Nespral, G. Nowak, E. Palle, V. Silva Aguirre, T. Trifonov, J.N. Winn, O. Barragán, P.G. Beck, W.J. Chaplin, W.D. Cochran, S. Csizmadia, H. Deeg, M. Endl, P. Heeren, S. Grziwa, A.P. Hatzes, D. Hidalgo, J. Korth, S. Mathis, P. Montañes Rodriguez, N. Narita, M. Patzold, C.M. Persson, F. Rodler, A.M.S. Smith, Monthly Notices of the Royal Astronomical Society 478 (2018) 4866–4880.","mla":"Van Eylen, V., et al. “HD 89345: A Bright Oscillating Star Hosting a Transiting Warm Saturn-Sized Planet Observed by K2.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 478, no. 4, Oxford University Press, 2018, pp. 4866–80, doi:<a href=\"https://doi.org/10.1093/mnras/sty1390\">10.1093/mnras/sty1390</a>.","ista":"Van Eylen V, Dai F, Mathur S, Gandolfi D, Albrecht S, Fridlund M, García RA, Guenther E, Hjorth M, Justesen AB, Livingston J, Lund MN, Pérez Hernández F, Prieto-Arranz J, Regulo C, Bugnet LA, Everett ME, Hirano T, Nespral D, Nowak G, Palle E, Silva Aguirre V, Trifonov T, Winn JN, Barragán O, Beck PG, Chaplin WJ, Cochran WD, Csizmadia S, Deeg H, Endl M, Heeren P, Grziwa S, Hatzes AP, Hidalgo D, Korth J, Mathis S, Montañes Rodriguez P, Narita N, Patzold M, Persson CM, Rodler F, Smith AMS. 2018. HD 89345: A bright oscillating star hosting a transiting warm Saturn-sized planet observed by K2. Monthly Notices of the Royal Astronomical Society. 478(4), 4866–4880.","ama":"Van Eylen V, Dai F, Mathur S, et al. HD 89345: A bright oscillating star hosting a transiting warm Saturn-sized planet observed by K2. <i>Monthly Notices of the Royal Astronomical Society</i>. 2018;478(4):4866-4880. doi:<a href=\"https://doi.org/10.1093/mnras/sty1390\">10.1093/mnras/sty1390</a>","apa":"Van Eylen, V., Dai, F., Mathur, S., Gandolfi, D., Albrecht, S., Fridlund, M., … Smith, A. M. S. (2018). HD 89345: A bright oscillating star hosting a transiting warm Saturn-sized planet observed by K2. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/sty1390\">https://doi.org/10.1093/mnras/sty1390</a>","chicago":"Van Eylen, V, F Dai, S Mathur, D Gandolfi, S Albrecht, M Fridlund, R A García, et al. “HD 89345: A Bright Oscillating Star Hosting a Transiting Warm Saturn-Sized Planet Observed by K2.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2018. <a href=\"https://doi.org/10.1093/mnras/sty1390\">https://doi.org/10.1093/mnras/sty1390</a>.","ieee":"V. Van Eylen <i>et al.</i>, “HD 89345: A bright oscillating star hosting a transiting warm Saturn-sized planet observed by K2,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 478, no. 4. Oxford University Press, pp. 4866–4880, 2018."},"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"acknowledgement":"We gratefully acknowledge many helpful suggestions by the anonymous referee. Based on observations made with a) the Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos; b) the ESO-3.6m telescope at La Silla Observatory under programme ID 0100.C-0808; c) the Italian Telescopio Nazionale Galileo operated on the island of La Palma by the Fundación Galileo Galilei of the Istituto Nazionale di Astrofisica. NESSI was funded by the NASA Exoplanet Exploration Program and the NASA Ames Research Center. NESSI was built at the Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. This project has received funding from the European Union’s Horizon 2020 research and innovation programme under grant agreement No 730890. This material reflects only the authors views and the Commission is not liable for any use that may be made of the information contained therein. DG gratefully acknowledges the financial support of the Programma Giovani Ricercatori – Rita Levi Montalcini – Rientro dei Cervelli (2012) awarded by the Italian Ministry of Education, Universities and Research (MIUR). SaM would like to acknowledge support from the Ramon y Cajal fellowship number RYC-2015-17697. AJ, MH, and SA acknowledge support by the Danish Council for Independent Research, through a DFF Sapere Aude Starting Grant nr. 4181-00487B. SzCs, APH, MP, and HR acknowledge the support of the DFG priority program SPP 1992Exploring the Diversity of Extrasolar Planets (grants HA 3279/12-1, PA 525/18-1, PA5 25/19-1 and PA525/20-1, RA 714/14-1) HD, CR, and FPH acknowledge the financial support from MINECO under grants ESP2015-65712-C5-4-R and AYA2016-76378-P. This paper has made use of the IAC Supercomputing facility HTCondor (http://research.cs.wisc.edu/htcondor/), partly financed by the Ministry of Economy and Competitiveness with FEDER funds, code IACA13-3E-2493. MF and CMP gratefully acknowledge the support of the Swedish National Space Board. RAG and StM thanks the support of the CNES PLATO grant. PGB is a postdoctoral fellow in the MINECO-programme ’Juan de la Cierva Incorporacion’ (IJCI-2015-26034). StM acknowledges support from ERC through SPIRE grant (647383) and from ISSI through the ENCELADE 2.0 team. VSA acknowledges support from VILLUM FONDEN (research grant 10118). MNL acknowledges support from the ESA-PRODEX programme. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (Grant agreement no.: DNRF106) This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This research was made with the use of NASA’s Astrophysics Data System and the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program.","status":"public","oa":1,"article_type":"original","external_id":{"arxiv":["1805.01860"]},"issue":"4","scopus_import":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics","asteroseismology","planets and satellites: composition","planets and satellites: formation","planets and satellites: fundamental parameters"],"quality_controlled":"1","author":[{"last_name":"Van Eylen","first_name":"V","full_name":"Van Eylen, V"},{"full_name":"Dai, F","first_name":"F","last_name":"Dai"},{"first_name":"S","last_name":"Mathur","full_name":"Mathur, S"},{"full_name":"Gandolfi, D","first_name":"D","last_name":"Gandolfi"},{"full_name":"Albrecht, S","first_name":"S","last_name":"Albrecht"},{"full_name":"Fridlund, M","last_name":"Fridlund","first_name":"M"},{"full_name":"García, R A","last_name":"García","first_name":"R A"},{"full_name":"Guenther, E","first_name":"E","last_name":"Guenther"},{"first_name":"M","last_name":"Hjorth","full_name":"Hjorth, M"},{"full_name":"Justesen, A B","last_name":"Justesen","first_name":"A B"},{"last_name":"Livingston","first_name":"J","full_name":"Livingston, J"},{"first_name":"M N","last_name":"Lund","full_name":"Lund, M N"},{"full_name":"Pérez Hernández, F","first_name":"F","last_name":"Pérez Hernández"},{"full_name":"Prieto-Arranz, J","last_name":"Prieto-Arranz","first_name":"J"},{"last_name":"Regulo","first_name":"C","full_name":"Regulo, C"},{"first_name":"Lisa Annabelle","orcid":"0000-0003-0142-4000","last_name":"Bugnet","full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501"},{"full_name":"Everett, M E","last_name":"Everett","first_name":"M E"},{"full_name":"Hirano, T","first_name":"T","last_name":"Hirano"},{"first_name":"D","last_name":"Nespral","full_name":"Nespral, D"},{"full_name":"Nowak, G","last_name":"Nowak","first_name":"G"},{"full_name":"Palle, E","first_name":"E","last_name":"Palle"},{"full_name":"Silva Aguirre, V","first_name":"V","last_name":"Silva Aguirre"},{"full_name":"Trifonov, T","last_name":"Trifonov","first_name":"T"},{"last_name":"Winn","first_name":"J N","full_name":"Winn, J N"},{"last_name":"Barragán","first_name":"O","full_name":"Barragán, O"},{"full_name":"Beck, P G","first_name":"P G","last_name":"Beck"},{"full_name":"Chaplin, W J","first_name":"W J","last_name":"Chaplin"},{"full_name":"Cochran, W D","first_name":"W D","last_name":"Cochran"},{"last_name":"Csizmadia","first_name":"S","full_name":"Csizmadia, S"},{"last_name":"Deeg","first_name":"H","full_name":"Deeg, H"},{"full_name":"Endl, M","last_name":"Endl","first_name":"M"},{"first_name":"P","last_name":"Heeren","full_name":"Heeren, P"},{"full_name":"Grziwa, S","last_name":"Grziwa","first_name":"S"},{"full_name":"Hatzes, A P","first_name":"A P","last_name":"Hatzes"},{"last_name":"Hidalgo","first_name":"D","full_name":"Hidalgo, D"},{"full_name":"Korth, J","last_name":"Korth","first_name":"J"},{"last_name":"Mathis","first_name":"S","full_name":"Mathis, S"},{"first_name":"P","last_name":"Montañes Rodriguez","full_name":"Montañes Rodriguez, P"},{"last_name":"Narita","first_name":"N","full_name":"Narita, N"},{"last_name":"Patzold","first_name":"M","full_name":"Patzold, M"},{"full_name":"Persson, C M","last_name":"Persson","first_name":"C M"},{"last_name":"Rodler","first_name":"F","full_name":"Rodler, F"},{"full_name":"Smith, A M S","last_name":"Smith","first_name":"A M S"}],"date_published":"2018-08-01T00:00:00Z","doi":"10.1093/mnras/sty1390","date_updated":"2022-08-22T07:45:38Z","article_processing_charge":"No","intvolume":"       478","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1805.01860"}],"publication_status":"published","language":[{"iso":"eng"}],"month":"08","day":"01"},{"_id":"8419","intvolume":"       376","year":"2018","publication_status":"published","volume":376,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","type":"journal_article","citation":{"chicago":"Kaloshin, Vadim, and Alfonso Sorrentino. “On the Integrability of Birkhoff Billiards.” <i>Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences</i>. The Royal Society, 2018. <a href=\"https://doi.org/10.1098/rsta.2017.0419\">https://doi.org/10.1098/rsta.2017.0419</a>.","ieee":"V. Kaloshin and A. Sorrentino, “On the integrability of Birkhoff billiards,” <i>Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences</i>, vol. 376, no. 2131. The Royal Society, 2018.","apa":"Kaloshin, V., &#38; Sorrentino, A. (2018). On the integrability of Birkhoff billiards. <i>Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences</i>. The Royal Society. <a href=\"https://doi.org/10.1098/rsta.2017.0419\">https://doi.org/10.1098/rsta.2017.0419</a>","ama":"Kaloshin V, Sorrentino A. On the integrability of Birkhoff billiards. <i>Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences</i>. 2018;376(2131). doi:<a href=\"https://doi.org/10.1098/rsta.2017.0419\">10.1098/rsta.2017.0419</a>","short":"V. Kaloshin, A. Sorrentino, Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 376 (2018).","ista":"Kaloshin V, Sorrentino A. 2018. On the integrability of Birkhoff billiards. Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences. 376(2131), 20170419.","mla":"Kaloshin, Vadim, and Alfonso Sorrentino. “On the Integrability of Birkhoff Billiards.” <i>Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences</i>, vol. 376, no. 2131, 20170419, The Royal Society, 2018, doi:<a href=\"https://doi.org/10.1098/rsta.2017.0419\">10.1098/rsta.2017.0419</a>."},"month":"10","language":[{"iso":"eng"}],"publication_identifier":{"issn":["1364-503X","1471-2962"]},"status":"public","issue":"2131","article_type":"original","day":"28","date_created":"2020-09-17T10:42:01Z","oa_version":"None","publication":"Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences","title":"On the integrability of Birkhoff billiards","article_number":"20170419","publisher":"The Royal Society","keyword":["General Engineering","General Physics and Astronomy","General Mathematics"],"abstract":[{"text":"In this survey, we provide a concise introduction to convex billiards and describe some recent results, obtained by the authors and collaborators, on the classification of integrable billiards, namely the so-called Birkhoff conjecture.\r\n\r\nThis article is part of the theme issue ‘Finite dimensional integrable systems: new trends and methods’.","lang":"eng"}],"extern":"1","quality_controlled":"1","author":[{"full_name":"Kaloshin, Vadim","id":"FE553552-CDE8-11E9-B324-C0EBE5697425","first_name":"Vadim","orcid":"0000-0002-6051-2628","last_name":"Kaloshin"},{"first_name":"Alfonso","last_name":"Sorrentino","full_name":"Sorrentino, Alfonso"}],"date_published":"2018-10-28T00:00:00Z","article_processing_charge":"No","date_updated":"2021-01-12T08:19:09Z","doi":"10.1098/rsta.2017.0419"},{"arxiv":1,"extern":"1","abstract":[{"lang":"eng","text":"We show that in the space of all convex billiard boundaries, the set of boundaries with rational caustics is dense. More precisely, the set of billiard boundaries with caustics of rotation number 1/q is polynomially sense in the smooth case, and exponentially dense in the analytic case."}],"publisher":"IOP Publishing","title":"Density of convex billiards with rational caustics","publication":"Nonlinearity","oa_version":"Preprint","date_created":"2020-09-17T10:42:09Z","external_id":{"arxiv":["1706.07968"]},"article_type":"original","issue":"11","oa":1,"status":"public","publication_identifier":{"issn":["0951-7715","1361-6544"]},"citation":{"chicago":"Kaloshin, Vadim, and Ke Zhang. “Density of Convex Billiards with Rational Caustics.” <i>Nonlinearity</i>. IOP Publishing, 2018. <a href=\"https://doi.org/10.1088/1361-6544/aadc12\">https://doi.org/10.1088/1361-6544/aadc12</a>.","ieee":"V. Kaloshin and K. Zhang, “Density of convex billiards with rational caustics,” <i>Nonlinearity</i>, vol. 31, no. 11. IOP Publishing, pp. 5214–5234, 2018.","apa":"Kaloshin, V., &#38; Zhang, K. (2018). Density of convex billiards with rational caustics. <i>Nonlinearity</i>. IOP Publishing. <a href=\"https://doi.org/10.1088/1361-6544/aadc12\">https://doi.org/10.1088/1361-6544/aadc12</a>","ama":"Kaloshin V, Zhang K. Density of convex billiards with rational caustics. <i>Nonlinearity</i>. 2018;31(11):5214-5234. doi:<a href=\"https://doi.org/10.1088/1361-6544/aadc12\">10.1088/1361-6544/aadc12</a>","ista":"Kaloshin V, Zhang K. 2018. Density of convex billiards with rational caustics. Nonlinearity. 31(11), 5214–5234.","short":"V. Kaloshin, K. Zhang, Nonlinearity 31 (2018) 5214–5234.","mla":"Kaloshin, Vadim, and Ke Zhang. “Density of Convex Billiards with Rational Caustics.” <i>Nonlinearity</i>, vol. 31, no. 11, IOP Publishing, 2018, pp. 5214–34, doi:<a href=\"https://doi.org/10.1088/1361-6544/aadc12\">10.1088/1361-6544/aadc12</a>."},"type":"journal_article","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","page":"5214-5234","volume":31,"year":"2018","_id":"8420","date_updated":"2021-01-12T08:19:10Z","doi":"10.1088/1361-6544/aadc12","article_processing_charge":"No","author":[{"first_name":"Vadim","last_name":"Kaloshin","orcid":"0000-0002-6051-2628","full_name":"Kaloshin, Vadim","id":"FE553552-CDE8-11E9-B324-C0EBE5697425"},{"full_name":"Zhang, Ke","first_name":"Ke","last_name":"Zhang"}],"date_published":"2018-10-15T00:00:00Z","quality_controlled":"1","keyword":["Mathematical Physics","General Physics and Astronomy","Applied Mathematics","Statistical and Nonlinear Physics"],"day":"15","language":[{"iso":"eng"}],"month":"10","publication_status":"published","intvolume":"        31","main_file_link":[{"url":"https://arxiv.org/abs/1706.07968","open_access":"1"}]},{"publication_status":"published","main_file_link":[{"url":"https://doi.org/10.1038/s41467-017-02715-6","open_access":"1"}],"intvolume":"         9","language":[{"iso":"eng"}],"month":"02","day":"13","pmid":1,"article_number":"641","quality_controlled":"1","scopus_import":"1","keyword":["General Physics and Astronomy","General Biochemistry","Genetics and Molecular Biology","General Chemistry","Multidisciplinary"],"doi":"10.1038/s41467-017-02715-6","date_updated":"2023-08-07T10:54:05Z","related_material":{"link":[{"url":"https://doi.org/10.1038/s41467-018-03701-2","relation":"erratum"}]},"article_processing_charge":"No","date_published":"2018-02-13T00:00:00Z","author":[{"first_name":"Dipak","last_name":"Samanta","full_name":"Samanta, Dipak"},{"full_name":"Galaktionova, Daria","last_name":"Galaktionova","first_name":"Daria"},{"full_name":"Gemen, Julius","last_name":"Gemen","first_name":"Julius"},{"last_name":"Shimon","first_name":"Linda J. W.","full_name":"Shimon, Linda J. W."},{"first_name":"Yael","last_name":"Diskin-Posner","full_name":"Diskin-Posner, Yael"},{"full_name":"Avram, Liat","last_name":"Avram","first_name":"Liat"},{"last_name":"Král","first_name":"Petr","full_name":"Král, Petr"},{"first_name":"Rafal","last_name":"Klajn","full_name":"Klajn, Rafal","id":"8e84690e-1e48-11ed-a02b-a1e6fb8bb53b"}],"year":"2018","_id":"13374","type":"journal_article","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","volume":9,"publication_identifier":{"eissn":["2041-1723"]},"citation":{"apa":"Samanta, D., Galaktionova, D., Gemen, J., Shimon, L. J. W., Diskin-Posner, Y., Avram, L., … Klajn, R. (2018). Reversible chromism of spiropyran in the cavity of a flexible coordination cage. <i>Nature Communications</i>. Springer Nature. <a href=\"https://doi.org/10.1038/s41467-017-02715-6\">https://doi.org/10.1038/s41467-017-02715-6</a>","ieee":"D. Samanta <i>et al.</i>, “Reversible chromism of spiropyran in the cavity of a flexible coordination cage,” <i>Nature Communications</i>, vol. 9. Springer Nature, 2018.","chicago":"Samanta, Dipak, Daria Galaktionova, Julius Gemen, Linda J. W. Shimon, Yael Diskin-Posner, Liat Avram, Petr Král, and Rafal Klajn. “Reversible Chromism of Spiropyran in the Cavity of a Flexible Coordination Cage.” <i>Nature Communications</i>. Springer Nature, 2018. <a href=\"https://doi.org/10.1038/s41467-017-02715-6\">https://doi.org/10.1038/s41467-017-02715-6</a>.","ista":"Samanta D, Galaktionova D, Gemen J, Shimon LJW, Diskin-Posner Y, Avram L, Král P, Klajn R. 2018. Reversible chromism of spiropyran in the cavity of a flexible coordination cage. Nature Communications. 9, 641.","mla":"Samanta, Dipak, et al. “Reversible Chromism of Spiropyran in the Cavity of a Flexible Coordination Cage.” <i>Nature Communications</i>, vol. 9, 641, Springer Nature, 2018, doi:<a href=\"https://doi.org/10.1038/s41467-017-02715-6\">10.1038/s41467-017-02715-6</a>.","short":"D. Samanta, D. Galaktionova, J. Gemen, L.J.W. Shimon, Y. Diskin-Posner, L. Avram, P. Král, R. Klajn, Nature Communications 9 (2018).","ama":"Samanta D, Galaktionova D, Gemen J, et al. Reversible chromism of spiropyran in the cavity of a flexible coordination cage. <i>Nature Communications</i>. 2018;9. doi:<a href=\"https://doi.org/10.1038/s41467-017-02715-6\">10.1038/s41467-017-02715-6</a>"},"article_type":"original","external_id":{"pmid":["29440687"]},"oa":1,"status":"public","oa_version":"Published Version","date_created":"2023-08-01T09:39:32Z","publisher":"Springer Nature","title":"Reversible chromism of spiropyran in the cavity of a flexible coordination cage","publication":"Nature Communications","extern":"1","abstract":[{"lang":"eng","text":"Confining molecules to volumes only slightly larger than the molecules themselves can profoundly alter their properties. Molecular switches—entities that can be toggled between two or more forms upon exposure to an external stimulus—often require conformational freedom to isomerize. Therefore, placing these switches in confined spaces can render them non-operational. To preserve the switchability of these species under confinement, we work with a water-soluble coordination cage that is flexible enough to adapt its shape to the conformation of the encapsulated guest. We show that owing to its flexibility, the cage is not only capable of accommodating—and solubilizing in water—several light-responsive spiropyran-based molecular switches, but, more importantly, it also provides an environment suitable for the efficient, reversible photoisomerization of the bound guests. Our findings pave the way towards studying various molecular switching processes in confined environments."}]},{"_id":"13473","year":"2018","volume":615,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","type":"journal_article","citation":{"short":"A. Schootemeijer, Y.L.L. Götberg, S.E. de Mink, D. Gies, E. Zapartas, Astronomy &#38; Astrophysics 615 (2018).","ista":"Schootemeijer A, Götberg YLL, de Mink SE, Gies D, Zapartas E. 2018. Clues about the scarcity of stripped-envelope stars from the evolutionary state of the sdO+Be binary system φ Persei. Astronomy &#38; Astrophysics. 615, A30.","mla":"Schootemeijer, A., et al. “Clues about the Scarcity of Stripped-Envelope Stars from the Evolutionary State of the SdO+Be Binary System φ Persei.” <i>Astronomy &#38; Astrophysics</i>, vol. 615, A30, EDP Sciences, 2018, doi:<a href=\"https://doi.org/10.1051/0004-6361/201731194\">10.1051/0004-6361/201731194</a>.","ama":"Schootemeijer A, Götberg YLL, de Mink SE, Gies D, Zapartas E. Clues about the scarcity of stripped-envelope stars from the evolutionary state of the sdO+Be binary system φ Persei. <i>Astronomy &#38; Astrophysics</i>. 2018;615. doi:<a href=\"https://doi.org/10.1051/0004-6361/201731194\">10.1051/0004-6361/201731194</a>","apa":"Schootemeijer, A., Götberg, Y. L. L., de Mink, S. E., Gies, D., &#38; Zapartas, E. (2018). Clues about the scarcity of stripped-envelope stars from the evolutionary state of the sdO+Be binary system φ Persei. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201731194\">https://doi.org/10.1051/0004-6361/201731194</a>","chicago":"Schootemeijer, A., Ylva Louise Linsdotter Götberg, S. E. de Mink, D. Gies, and E. Zapartas. “Clues about the Scarcity of Stripped-Envelope Stars from the Evolutionary State of the SdO+Be Binary System φ Persei.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2018. <a href=\"https://doi.org/10.1051/0004-6361/201731194\">https://doi.org/10.1051/0004-6361/201731194</a>.","ieee":"A. Schootemeijer, Y. L. L. Götberg, S. E. de Mink, D. Gies, and E. Zapartas, “Clues about the scarcity of stripped-envelope stars from the evolutionary state of the sdO+Be binary system φ Persei,” <i>Astronomy &#38; Astrophysics</i>, vol. 615. EDP Sciences, 2018."},"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"status":"public","oa":1,"external_id":{"arxiv":["1803.02379"]},"article_type":"original","date_created":"2023-08-03T10:14:37Z","oa_version":"Published Version","publication":"Astronomy & Astrophysics","title":"Clues about the scarcity of stripped-envelope stars from the evolutionary state of the sdO+Be binary system φ Persei","publisher":"EDP Sciences","abstract":[{"lang":"eng","text":"Stripped-envelope stars form in binary systems after losing mass through Roche-lobe overflow. They bear astrophysical significance as sources of UV and ionizing radiation in older stellar populations and, if sufficiently massive, as stripped supernova progenitors. Binary evolutionary models predict that they are common, but only a handful of subdwarfs with B-type companions are known. The question is whether a large population of such systems has evaded detection as a result of biases, or whether the model predictions are wrong. We reanalyze the well-studied post-interaction binary φ Persei. Recently, new data have improved the orbital solution of the system, which contains an ~1.2M⊙ stripped-envelope star and a rapidly rotating ~9.6M⊙ Be star. We compare with an extensive grid of evolutionary models using a Bayesian approach and constrain the initial masses of the progenitor to 7.2 ± 0.4M⊙ for the stripped star and 3.8 ± 0.4M⊙ for the Be star. The system must have evolved through near-conservative mass transfer. These findings are consistent with earlier studies. The age we obtain, 57 ± 9 Myr, is in excellent agreement with the age of the α Persei cluster. We note that neither star was initially massive enough to produce a core-collapse supernova, but mass exchange pushed the Be star above the mass threshold. We find that the subdwarf is overluminous for its mass by almost an order of magnitude, compared to the expectations for a helium core burning star. We can only reconcile this if the subdwarf resides in a late phase of helium shell burning, which lasts only 2–3% of the total lifetime as a subdwarf. Assuming continuous star formation implies that up to ~50 less evolved, dimmer subdwarfs exist for each system similar to φ Persei, but have evaded detection so far. Our findings can be interpreted as a strong indication that a substantial population of stripped-envelope stars indeed exists, but has so far evaded detection because of observational biases and lack of large-scale systematic searches."}],"extern":"1","arxiv":1,"main_file_link":[{"url":"https://doi.org/10.1051/0004-6361/201731194","open_access":"1"}],"intvolume":"       615","publication_status":"published","month":"07","language":[{"iso":"eng"}],"day":"06","article_number":"A30","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"scopus_import":"1","quality_controlled":"1","author":[{"last_name":"Schootemeijer","first_name":"A.","full_name":"Schootemeijer, A."},{"first_name":"Ylva Louise Linsdotter","last_name":"Götberg","orcid":"0000-0002-6960-6911","full_name":"Götberg, Ylva Louise Linsdotter","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d"},{"last_name":"de Mink","first_name":"S. E.","full_name":"de Mink, S. E."},{"last_name":"Gies","first_name":"D.","full_name":"Gies, D."},{"full_name":"Zapartas, E.","first_name":"E.","last_name":"Zapartas"}],"date_published":"2018-07-06T00:00:00Z","article_processing_charge":"No","doi":"10.1051/0004-6361/201731194","date_updated":"2023-08-09T12:22:52Z"},{"publication_status":"published","intvolume":"       475","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/stx3181"}],"month":"03","language":[{"iso":"eng"}],"day":"01","quality_controlled":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"scopus_import":"1","article_processing_charge":"No","date_updated":"2023-08-09T12:17:34Z","doi":"10.1093/mnras/stx3181","author":[{"full_name":"Smith, Nathan","last_name":"Smith","first_name":"Nathan"},{"full_name":"Götberg, Ylva Louise Linsdotter","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","first_name":"Ylva Louise Linsdotter","last_name":"Götberg","orcid":"0000-0002-6960-6911"},{"full_name":"de Mink, Selma E","first_name":"Selma E","last_name":"de Mink"}],"date_published":"2018-03-01T00:00:00Z","year":"2018","_id":"13474","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","type":"journal_article","volume":475,"page":"772-782","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"citation":{"chicago":"Smith, Nathan, Ylva Louise Linsdotter Götberg, and Selma E de Mink. “Extreme Isolation of WN3/O3 Stars and Implications for Their Evolutionary Origin as the Elusive Stripped Binaries.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2018. <a href=\"https://doi.org/10.1093/mnras/stx3181\">https://doi.org/10.1093/mnras/stx3181</a>.","ieee":"N. Smith, Y. L. L. Götberg, and S. E. de Mink, “Extreme isolation of WN3/O3 stars and implications for their evolutionary origin as the elusive stripped binaries,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 475, no. 1. Oxford University Press, pp. 772–782, 2018.","apa":"Smith, N., Götberg, Y. L. L., &#38; de Mink, S. E. (2018). Extreme isolation of WN3/O3 stars and implications for their evolutionary origin as the elusive stripped binaries. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stx3181\">https://doi.org/10.1093/mnras/stx3181</a>","ama":"Smith N, Götberg YLL, de Mink SE. Extreme isolation of WN3/O3 stars and implications for their evolutionary origin as the elusive stripped binaries. <i>Monthly Notices of the Royal Astronomical Society</i>. 2018;475(1):772-782. doi:<a href=\"https://doi.org/10.1093/mnras/stx3181\">10.1093/mnras/stx3181</a>","ista":"Smith N, Götberg YLL, de Mink SE. 2018. Extreme isolation of WN3/O3 stars and implications for their evolutionary origin as the elusive stripped binaries. Monthly Notices of the Royal Astronomical Society. 475(1), 772–782.","mla":"Smith, Nathan, et al. “Extreme Isolation of WN3/O3 Stars and Implications for Their Evolutionary Origin as the Elusive Stripped Binaries.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 475, no. 1, Oxford University Press, 2018, pp. 772–82, doi:<a href=\"https://doi.org/10.1093/mnras/stx3181\">10.1093/mnras/stx3181</a>.","short":"N. Smith, Y.L.L. Götberg, S.E. de Mink, Monthly Notices of the Royal Astronomical Society 475 (2018) 772–782."},"issue":"1","external_id":{"arxiv":["1704.03516"]},"article_type":"original","status":"public","oa":1,"date_created":"2023-08-03T10:14:47Z","oa_version":"Published Version","publisher":"Oxford University Press","publication":"Monthly Notices of the Royal Astronomical Society","title":"Extreme isolation of WN3/O3 stars and implications for their evolutionary origin as the elusive stripped binaries","extern":"1","abstract":[{"text":"Recent surveys of the Magellanic Clouds have revealed a subtype of Wolf–Rayet (WR) star with peculiar properties. WN3/O3 spectra exhibit both WR-like emission and O3 V-like absorption – but at lower luminosity than O3 V or WN stars. We examine the projected spatial distribution of WN3/O3 stars in the Large Magellanic Cloud as compared to O-type stars. Surprisingly, WN3/O3 stars are among the most isolated of all classes of massive stars; they have a distribution similar to red supergiants dominated by initial masses of 10–15 M⊙, and are far more dispersed than classical WR stars or luminous blue variables. Their lack of association with clusters of O-type stars suggests strongly that WN3/O3 stars are not the descendants of single massive stars (30 M⊙ or above). Instead, they are likely products of interacting binaries at lower initial mass (10–18 M⊙). Comparison with binary models suggests a probable origin with primaries in this mass range that were stripped of their H envelopes through non-conservative mass transfer by a low-mass secondary. We show that model spectra and positions on the Hertzsprung–Russell diagram for binary-stripped stars are consistent with WN3/O3 stars. Monitoring radial velocities with high-resolution spectra can test for low-mass companions or runaway velocities. With lower initial mass and environments that avoid very massive stars, the WN3/O3 stars fit expectations for progenitors of Type Ib and possibly Type Ibn supernovae.","lang":"eng"}],"arxiv":1},{"volume":615,"type":"journal_article","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","_id":"13475","year":"2018","status":"public","oa":1,"external_id":{"arxiv":["1802.03018"]},"article_type":"original","citation":{"ama":"Götberg YLL, de Mink SE, Groh JH, et al. Spectral models for binary products: Unifying subdwarfs and Wolf-Rayet stars as a sequence of stripped-envelope stars. <i>Astronomy &#38;amp; Astrophysics</i>. 2018;615. doi:<a href=\"https://doi.org/10.1051/0004-6361/201732274\">10.1051/0004-6361/201732274</a>","ista":"Götberg YLL, de Mink SE, Groh JH, Kupfer T, Crowther PA, Zapartas E, Renzo M. 2018. Spectral models for binary products: Unifying subdwarfs and Wolf-Rayet stars as a sequence of stripped-envelope stars. Astronomy &#38;amp; Astrophysics. 615, A78.","mla":"Götberg, Ylva Louise Linsdotter, et al. “Spectral Models for Binary Products: Unifying Subdwarfs and Wolf-Rayet Stars as a Sequence of Stripped-Envelope Stars.” <i>Astronomy &#38;amp; Astrophysics</i>, vol. 615, A78, EDP Sciences, 2018, doi:<a href=\"https://doi.org/10.1051/0004-6361/201732274\">10.1051/0004-6361/201732274</a>.","short":"Y.L.L. Götberg, S.E. de Mink, J.H. Groh, T. Kupfer, P.A. Crowther, E. Zapartas, M. Renzo, Astronomy &#38;amp; Astrophysics 615 (2018).","ieee":"Y. L. L. Götberg <i>et al.</i>, “Spectral models for binary products: Unifying subdwarfs and Wolf-Rayet stars as a sequence of stripped-envelope stars,” <i>Astronomy &#38;amp; Astrophysics</i>, vol. 615. EDP Sciences, 2018.","chicago":"Götberg, Ylva Louise Linsdotter, S. E. de Mink, J. H. Groh, T. Kupfer, P. A. Crowther, E. Zapartas, and M. Renzo. “Spectral Models for Binary Products: Unifying Subdwarfs and Wolf-Rayet Stars as a Sequence of Stripped-Envelope Stars.” <i>Astronomy &#38;amp; Astrophysics</i>. EDP Sciences, 2018. <a href=\"https://doi.org/10.1051/0004-6361/201732274\">https://doi.org/10.1051/0004-6361/201732274</a>.","apa":"Götberg, Y. L. L., de Mink, S. E., Groh, J. H., Kupfer, T., Crowther, P. A., Zapartas, E., &#38; Renzo, M. (2018). Spectral models for binary products: Unifying subdwarfs and Wolf-Rayet stars as a sequence of stripped-envelope stars. <i>Astronomy &#38;amp; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/201732274\">https://doi.org/10.1051/0004-6361/201732274</a>"},"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"title":"Spectral models for binary products: Unifying subdwarfs and Wolf-Rayet stars as a sequence of stripped-envelope stars","publication":"Astronomy &amp; Astrophysics","publisher":"EDP Sciences","oa_version":"Published Version","date_created":"2023-08-03T10:15:00Z","arxiv":1,"abstract":[{"text":"Stars stripped of their hydrogen-rich envelope through interaction with a binary companion are generally not considered when accounting for ionizing radiation from stellar populations, despite the expectation that stripped stars emit hard ionizing radiation, form frequently, and live 10–100 times longer than single massive stars. We compute the first grid of evolutionary and spectral models specially made for stars stripped in binaries for a range of progenitor masses (2–20 M⊙) and metallicities ranging from solar to values representative for pop II stars. For stripped stars with masses in the range 0.3–7 M⊙, we find consistently high effective temperatures (20 000–100 000 K, increasing with mass), small radii (0.2–1 R⊙), and high bolometric luminosities, comparable to that of their progenitor before stripping. The spectra show a continuous sequence that naturally bridges subdwarf-type stars at the low-mass end and Wolf-Rayet-like spectra at the high-mass end. For intermediate masses we find hybrid spectral classes showing a mixture of absorption and emission lines. These appear for stars with mass-loss rates of 10−8−10−6 M⊙ yr−1, which have semi-transparent atmospheres. At low metallicity, substantial hydrogen-rich layers are left at the surface and we predict spectra that resemble O-type stars instead. We obtain spectra undistinguishable from subdwarfs for stripped stars with masses up to 1.7 M⊙, which questions whether the widely adopted canonical value of 0.47 M⊙ is uniformly valid. Only a handful of stripped stars of intermediate mass have currently been identified observationally. Increasing this sample will provide necessary tests for the physics of interaction, internal mixing, and stellar winds. We use our model spectra to investigate the feasibility to detect stripped stars next to an optically bright companion and recommend systematic searches for their UV excess and possible emission lines, most notably HeII λ4686 in the optical and HeII λ1640 in the UV. Our models are publicly available for further investigations or inclusion in spectral synthesis simulations.","lang":"eng"}],"extern":"1","main_file_link":[{"url":"https://doi.org/10.1051/0004-6361/201732274","open_access":"1"}],"intvolume":"       615","publication_status":"published","day":"17","language":[{"iso":"eng"}],"month":"07","article_number":"A78","date_published":"2018-07-17T00:00:00Z","author":[{"first_name":"Ylva Louise Linsdotter","last_name":"Götberg","orcid":"0000-0002-6960-6911","full_name":"Götberg, Ylva Louise Linsdotter","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d"},{"full_name":"de Mink, S. E.","last_name":"de Mink","first_name":"S. E."},{"last_name":"Groh","first_name":"J. H.","full_name":"Groh, J. H."},{"full_name":"Kupfer, T.","first_name":"T.","last_name":"Kupfer"},{"full_name":"Crowther, P. A.","last_name":"Crowther","first_name":"P. A."},{"last_name":"Zapartas","first_name":"E.","full_name":"Zapartas, E."},{"last_name":"Renzo","first_name":"M.","full_name":"Renzo, M."}],"doi":"10.1051/0004-6361/201732274","date_updated":"2023-08-09T11:22:17Z","article_processing_charge":"No","scopus_import":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"quality_controlled":"1"},{"article_number":"031060","quality_controlled":"1","keyword":["General Physics and Astronomy"],"scopus_import":"1","article_processing_charge":"No","date_updated":"2023-08-22T07:42:07Z","doi":"10.1103/physrevx.8.031060","author":[{"id":"71b4d059-2a03-11ee-914d-dfa3beed6530","full_name":"Baykusheva, Denitsa Rangelova","last_name":"Baykusheva","first_name":"Denitsa Rangelova"},{"full_name":"Wörner, Hans Jakob","first_name":"Hans Jakob","last_name":"Wörner"}],"date_published":"2018-07-01T00:00:00Z","publication_status":"published","main_file_link":[{"url":"https://doi.org/10.1103/PhysRevX.8.031060","open_access":"1"}],"intvolume":"         8","month":"07","language":[{"iso":"eng"}],"day":"01","date_created":"2023-08-10T06:34:48Z","oa_version":"Published Version","publisher":"American Physical Society","publication":"Physical Review X","title":"Chiral discrimination through bielliptical high-harmonic spectroscopy","extern":"1","abstract":[{"lang":"eng","text":"Molecular chirality plays an essential role in most biochemical processes. The observation and quantification of chirality-sensitive signals, however, remains extremely challenging, especially on ultrafast timescales and in dilute media. Here, we describe the experimental realization of an all-optical and ultrafast scheme for detecting chiral dynamics in molecules. This technique is based on high-harmonic generation by a combination of two-color counterrotating femtosecond laser pulses with polarization states tunable from linear to circular. We demonstrate two different implementations of chiral-sensitive high-harmonic spectroscopy on an ensemble of randomly oriented methyloxirane molecules in the gas phase. Using two elliptically polarized fields, we observe that the ellipticities maximizing the harmonic signal reach up to \r\n4.4\r\n±\r\n0.2\r\n%\r\n (at 17.6 eV). Using two circularly polarized fields, we observe circular dichroisms ranging up to \r\n13\r\n±\r\n6\r\n%\r\n (28.3–33.1 eV). Our theoretical analysis confirms that the observed chiral response originates from subfemtosecond electron dynamics driven by the magnetic component of the driving laser field. This assignment is supported by the experimental observation of a strong intensity dependence of the chiral effects and its agreement with theory. We moreover report and explain a pronounced variation of the signal strength and dichroism with the driving-field ellipticities and harmonic orders. Finally, we demonstrate the sensitivity of the experimental observables to the shape of the electron hole. This technique for chiral discrimination will yield femtosecond temporal resolution when integrated in a pump-probe scheme and subfemtosecond resolution on chiral charge migration in a self-probing scheme."}],"year":"2018","_id":"14003","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","type":"journal_article","volume":8,"publication_identifier":{"eissn":["2160-3308"]},"citation":{"apa":"Baykusheva, D. R., &#38; Wörner, H. J. (2018). Chiral discrimination through bielliptical high-harmonic spectroscopy. <i>Physical Review X</i>. American Physical Society. <a href=\"https://doi.org/10.1103/physrevx.8.031060\">https://doi.org/10.1103/physrevx.8.031060</a>","chicago":"Baykusheva, Denitsa Rangelova, and Hans Jakob Wörner. “Chiral Discrimination through Bielliptical High-Harmonic Spectroscopy.” <i>Physical Review X</i>. American Physical Society, 2018. <a href=\"https://doi.org/10.1103/physrevx.8.031060\">https://doi.org/10.1103/physrevx.8.031060</a>.","ieee":"D. R. Baykusheva and H. J. Wörner, “Chiral discrimination through bielliptical high-harmonic spectroscopy,” <i>Physical Review X</i>, vol. 8, no. 3. American Physical Society, 2018.","mla":"Baykusheva, Denitsa Rangelova, and Hans Jakob Wörner. “Chiral Discrimination through Bielliptical High-Harmonic Spectroscopy.” <i>Physical Review X</i>, vol. 8, no. 3, 031060, American Physical Society, 2018, doi:<a href=\"https://doi.org/10.1103/physrevx.8.031060\">10.1103/physrevx.8.031060</a>.","ista":"Baykusheva DR, Wörner HJ. 2018. Chiral discrimination through bielliptical high-harmonic spectroscopy. Physical Review X. 8(3), 031060.","short":"D.R. Baykusheva, H.J. Wörner, Physical Review X 8 (2018).","ama":"Baykusheva DR, Wörner HJ. Chiral discrimination through bielliptical high-harmonic spectroscopy. <i>Physical Review X</i>. 2018;8(3). doi:<a href=\"https://doi.org/10.1103/physrevx.8.031060\">10.1103/physrevx.8.031060</a>"},"issue":"3","article_type":"original","oa":1,"status":"public"},{"article_number":"1806","scopus_import":"1","keyword":["General Physics and Astronomy","General Biochemistry","Genetics and Molecular Biology","General Chemistry","Multidisciplinary"],"quality_controlled":"1","date_published":"2018-05-04T00:00:00Z","author":[{"full_name":"Bräuning, Bastian","last_name":"Bräuning","first_name":"Bastian"},{"first_name":"Eva","last_name":"Bertosin","full_name":"Bertosin, Eva"},{"id":"dfec9381-4341-11ee-8fd8-faa02bba7d62","full_name":"Praetorius, Florian M","last_name":"Praetorius","first_name":"Florian M"},{"first_name":"Christian","last_name":"Ihling","full_name":"Ihling, Christian"},{"full_name":"Schatt, Alexandra","first_name":"Alexandra","last_name":"Schatt"},{"first_name":"Agnes","last_name":"Adler","full_name":"Adler, Agnes"},{"last_name":"Richter","first_name":"Klaus","full_name":"Richter, Klaus"},{"full_name":"Sinz, Andrea","last_name":"Sinz","first_name":"Andrea"},{"full_name":"Dietz, Hendrik","first_name":"Hendrik","last_name":"Dietz"},{"first_name":"Michael","last_name":"Groll","full_name":"Groll, Michael"}],"doi":"10.1038/s41467-018-04139-2","date_updated":"2023-11-07T11:46:12Z","article_processing_charge":"No","intvolume":"         9","main_file_link":[{"url":"https://doi.org/10.1038/s41467-018-04139-2","open_access":"1"}],"publication_status":"published","language":[{"iso":"eng"}],"month":"05","pmid":1,"day":"04","oa_version":"Published Version","date_created":"2023-09-06T12:07:33Z","title":"Structure and mechanism of the two-component α-helical pore-forming toxin YaxAB","publication":"Nature Communications","publisher":"Springer Nature","abstract":[{"lang":"eng","text":"Pore-forming toxins (PFT) are virulence factors that transform from soluble to membrane-bound states. The Yersinia YaxAB system represents a family of binary α-PFTs with orthologues in human, insect, and plant pathogens, with unknown structures. YaxAB was shown to be cytotoxic and likely involved in pathogenesis, though the molecular basis for its two-component lytic mechanism remains elusive. Here, we present crystal structures of YaxA and YaxB, together with a cryo-electron microscopy map of the YaxAB complex. Our structures reveal a pore predominantly composed of decamers of YaxA–YaxB heterodimers. Both subunits bear membrane-active moieties, but only YaxA is capable of binding to membranes by itself. YaxB can subsequently be recruited to membrane-associated YaxA and induced to present its lytic transmembrane helices. Pore formation can progress by further oligomerization of YaxA–YaxB dimers. Our results allow for a comparison between pore assemblies belonging to the wider ClyA-like family of α-PFTs, highlighting diverse pore architectures."}],"extern":"1","_id":"14284","year":"2018","volume":9,"type":"journal_article","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"ieee":"B. Bräuning <i>et al.</i>, “Structure and mechanism of the two-component α-helical pore-forming toxin YaxAB,” <i>Nature Communications</i>, vol. 9. Springer Nature, 2018.","chicago":"Bräuning, Bastian, Eva Bertosin, Florian M Praetorius, Christian Ihling, Alexandra Schatt, Agnes Adler, Klaus Richter, Andrea Sinz, Hendrik Dietz, and Michael Groll. “Structure and Mechanism of the Two-Component α-Helical Pore-Forming Toxin YaxAB.” <i>Nature Communications</i>. Springer Nature, 2018. <a href=\"https://doi.org/10.1038/s41467-018-04139-2\">https://doi.org/10.1038/s41467-018-04139-2</a>.","apa":"Bräuning, B., Bertosin, E., Praetorius, F. M., Ihling, C., Schatt, A., Adler, A., … Groll, M. (2018). Structure and mechanism of the two-component α-helical pore-forming toxin YaxAB. <i>Nature Communications</i>. Springer Nature. <a href=\"https://doi.org/10.1038/s41467-018-04139-2\">https://doi.org/10.1038/s41467-018-04139-2</a>","ama":"Bräuning B, Bertosin E, Praetorius FM, et al. Structure and mechanism of the two-component α-helical pore-forming toxin YaxAB. <i>Nature Communications</i>. 2018;9. doi:<a href=\"https://doi.org/10.1038/s41467-018-04139-2\">10.1038/s41467-018-04139-2</a>","ista":"Bräuning B, Bertosin E, Praetorius FM, Ihling C, Schatt A, Adler A, Richter K, Sinz A, Dietz H, Groll M. 2018. Structure and mechanism of the two-component α-helical pore-forming toxin YaxAB. Nature Communications. 9, 1806.","mla":"Bräuning, Bastian, et al. “Structure and Mechanism of the Two-Component α-Helical Pore-Forming Toxin YaxAB.” <i>Nature Communications</i>, vol. 9, 1806, Springer Nature, 2018, doi:<a href=\"https://doi.org/10.1038/s41467-018-04139-2\">10.1038/s41467-018-04139-2</a>.","short":"B. Bräuning, E. Bertosin, F.M. Praetorius, C. Ihling, A. Schatt, A. Adler, K. Richter, A. Sinz, H. Dietz, M. Groll, Nature Communications 9 (2018)."},"publication_identifier":{"issn":["2041-1723"]},"status":"public","oa":1,"article_type":"original","external_id":{"pmid":["29728606"]}},{"year":"2018","_id":"10362","user_id":"8b945eb4-e2f2-11eb-945a-df72226e66a9","type":"journal_article","volume":12,"page":"1508-1518","publication_identifier":{"eissn":["1936-086X"],"issn":["1936-0851"]},"citation":{"short":"P.D.E. Fisher, Q. Shen, B. Akpinar, L.K. Davis, K.K.H. Chung, D. Baddeley, A. Šarić, T.J. Melia, B.W. Hoogenboom, C. Lin, C.P. Lusk, ACS Nano 12 (2018) 1508–1518.","mla":"Fisher, Patrick D. Ellis, et al. “A Programmable DNA Origami Platform for Organizing Intrinsically Disordered Nucleoporins within Nanopore Confinement.” <i>ACS Nano</i>, vol. 12, no. 2, American Chemical Society, 2018, pp. 1508–18, doi:<a href=\"https://doi.org/10.1021/acsnano.7b08044\">10.1021/acsnano.7b08044</a>.","ista":"Fisher PDE, Shen Q, Akpinar B, Davis LK, Chung KKH, Baddeley D, Šarić A, Melia TJ, Hoogenboom BW, Lin C, Lusk CP. 2018. A Programmable DNA origami platform for organizing intrinsically disordered nucleoporins within nanopore confinement. ACS Nano. 12(2), 1508–1518.","ama":"Fisher PDE, Shen Q, Akpinar B, et al. A Programmable DNA origami platform for organizing intrinsically disordered nucleoporins within nanopore confinement. <i>ACS Nano</i>. 2018;12(2):1508-1518. doi:<a href=\"https://doi.org/10.1021/acsnano.7b08044\">10.1021/acsnano.7b08044</a>","apa":"Fisher, P. D. E., Shen, Q., Akpinar, B., Davis, L. K., Chung, K. K. H., Baddeley, D., … Lusk, C. P. (2018). A Programmable DNA origami platform for organizing intrinsically disordered nucleoporins within nanopore confinement. <i>ACS Nano</i>. American Chemical Society. <a href=\"https://doi.org/10.1021/acsnano.7b08044\">https://doi.org/10.1021/acsnano.7b08044</a>","ieee":"P. D. E. Fisher <i>et al.</i>, “A Programmable DNA origami platform for organizing intrinsically disordered nucleoporins within nanopore confinement,” <i>ACS Nano</i>, vol. 12, no. 2. American Chemical Society, pp. 1508–1518, 2018.","chicago":"Fisher, Patrick D. Ellis, Qi Shen, Bernice Akpinar, Luke K. Davis, Kenny Kwok Hin Chung, David Baddeley, Anđela Šarić, et al. “A Programmable DNA Origami Platform for Organizing Intrinsically Disordered Nucleoporins within Nanopore Confinement.” <i>ACS Nano</i>. American Chemical Society, 2018. <a href=\"https://doi.org/10.1021/acsnano.7b08044\">https://doi.org/10.1021/acsnano.7b08044</a>."},"issue":"2","external_id":{"pmid":["29350911"]},"article_type":"original","status":"public","acknowledgement":"We thank J. Edel and members of the Lusk, Lin and Hoogenboom lab for discussion and acknowledge A. Pyne and R. Thorogate for support carrying out the AFM experiments. This work was funded by the NIH (R21GM109466 to CPL, CL and TJM, DP2GM114830 to CL, RO1GM105672 to CPL, and T32GM007223 to PDEF) and the UK Engineering and Physical Sciences Research Council (EP/L015277/1, EP/L504889/1, and EP/M028100/1).","date_created":"2021-11-26T15:15:00Z","oa_version":"None","publisher":"American Chemical Society","publication":"ACS Nano","title":"A Programmable DNA origami platform for organizing intrinsically disordered nucleoporins within nanopore confinement","extern":"1","abstract":[{"text":"Nuclear pore complexes (NPCs) form gateways that control molecular exchange between the nucleus and the cytoplasm. They impose a diffusion barrier to macromolecules and enable the selective transport of nuclear transport receptors with bound cargo. The underlying mechanisms that establish these permeability properties remain to be fully elucidated but require unstructured nuclear pore proteins rich in Phe-Gly (FG)-repeat domains of different types, such as FxFG and GLFG. While physical modeling and in vitro approaches have provided a framework for explaining how the FG network contributes to the barrier and transport properties of the NPC, it remains unknown whether the number and/or the spatial positioning of different FG-domains along a cylindrical, ∼40 nm diameter transport channel contributes to their collective properties and function. To begin to answer these questions, we have used DNA origami to build a cylinder that mimics the dimensions of the central transport channel and can house a specified number of FG-domains at specific positions with easily tunable design parameters, such as grafting density and topology. We find the overall morphology of the FG-domain assemblies to be dependent on their chemical composition, determined by the type and density of FG-repeat, and on their architectural confinement provided by the DNA cylinder, largely consistent with here presented molecular dynamics simulations based on a coarse-grained polymer model. In addition, high-speed atomic force microscopy reveals local and reversible FG-domain condensation that transiently occludes the lumen of the DNA central channel mimics, suggestive of how the NPC might establish its permeability properties.","lang":"eng"}],"publication_status":"published","intvolume":"        12","month":"01","language":[{"iso":"eng"}],"day":"19","pmid":1,"quality_controlled":"1","keyword":["general physics and astronomy"],"scopus_import":"1","article_processing_charge":"No","date_updated":"2021-11-26T15:57:02Z","doi":"10.1021/acsnano.7b08044","date_published":"2018-01-19T00:00:00Z","author":[{"full_name":"Fisher, Patrick D. Ellis","first_name":"Patrick D. Ellis","last_name":"Fisher"},{"full_name":"Shen, Qi","first_name":"Qi","last_name":"Shen"},{"last_name":"Akpinar","first_name":"Bernice","full_name":"Akpinar, Bernice"},{"full_name":"Davis, Luke K.","first_name":"Luke K.","last_name":"Davis"},{"full_name":"Chung, Kenny Kwok Hin","last_name":"Chung","first_name":"Kenny Kwok Hin"},{"full_name":"Baddeley, David","first_name":"David","last_name":"Baddeley"},{"orcid":"0000-0002-7854-2139","last_name":"Šarić","first_name":"Anđela","id":"bf63d406-f056-11eb-b41d-f263a6566d8b","full_name":"Šarić, Anđela"},{"full_name":"Melia, Thomas J.","first_name":"Thomas J.","last_name":"Melia"},{"full_name":"Hoogenboom, Bart W.","first_name":"Bart W.","last_name":"Hoogenboom"},{"last_name":"Lin","first_name":"Chenxiang","full_name":"Lin, Chenxiang"},{"full_name":"Lusk, C. Patrick","last_name":"Lusk","first_name":"C. Patrick"}]},{"publication":"Physical Review Letters","title":"Quantitative transport measurements of fractional quantum Hall energy gaps in edgeless graphene devices","publisher":"American Physical Society","date_created":"2022-01-14T12:15:47Z","oa_version":"Preprint","arxiv":1,"abstract":[{"text":"Owing to their wide tunability, multiple internal degrees of freedom, and low disorder, graphene heterostructures are emerging as a promising experimental platform for fractional quantum Hall (FQH) studies. Here, we report FQH thermal activation gap measurements in dual graphite-gated monolayer graphene devices fabricated in an edgeless Corbino geometry. In devices with substrate-induced sublattice splitting, we find a tunable crossover between single- and multicomponent FQH states in the zero energy Landau level. Activation gaps in the single-component regime show excellent agreement with numerical calculations using a single broadening parameter \r\nΓ≈7.2K. In the first excited Landau level, in contrast, FQH gaps are strongly influenced by Landau level mixing, and we observe an unexpected valley-ordered state at integer filling ν=−4.","lang":"eng"}],"extern":"1","volume":121,"user_id":"8b945eb4-e2f2-11eb-945a-df72226e66a9","type":"journal_article","_id":"10626","year":"2018","oa":1,"status":"public","acknowledgement":"We thank Cory Dean, S. Chen, Y. Zeng, M. Yankowitz, and J. Li for discussing their unpublished data and for sharing the stack inversion technique. The authors acknowledge further discussions of the results with I. Sodemann, M. Zaletel, C. Nayak, and J. Jain. A. F. Y., H. P., H. Z., and E. M. S. were supported by the ARO under awards 69188PHH and MURI W911NF-17-1-0323. A portion of this work was performed at the National High Magnetic Field Laboratory, which is supported by National Science Foundation Cooperative Agreement No. DMR-1644779 and the State of Florida. K. W. and T. T. acknowledge support from the Elemental Strategy Initiative conducted by the MEXT, Japan, and JSPS KAKENHI Grant No. JP15K21722. E. M. S. acknowledges the support of the Elings Prize Fellowship in Science of the California Nanosystems Institute at the University of California, Santa Barbara. A. F. Y. acknowledges the support of the David and Lucile Packard Foundation.","issue":"22","article_type":"original","external_id":{"arxiv":["1805.04199"]},"citation":{"chicago":"Polshyn, Hryhoriy, H. Zhou, E. M. Spanton, T. Taniguchi, K. Watanabe, and A. F. Young. “Quantitative Transport Measurements of Fractional Quantum Hall Energy Gaps in Edgeless Graphene Devices.” <i>Physical Review Letters</i>. American Physical Society, 2018. <a href=\"https://doi.org/10.1103/physrevlett.121.226801\">https://doi.org/10.1103/physrevlett.121.226801</a>.","ieee":"H. Polshyn, H. Zhou, E. M. Spanton, T. Taniguchi, K. Watanabe, and A. F. Young, “Quantitative transport measurements of fractional quantum Hall energy gaps in edgeless graphene devices,” <i>Physical Review Letters</i>, vol. 121, no. 22. American Physical Society, 2018.","apa":"Polshyn, H., Zhou, H., Spanton, E. M., Taniguchi, T., Watanabe, K., &#38; Young, A. F. (2018). Quantitative transport measurements of fractional quantum Hall energy gaps in edgeless graphene devices. <i>Physical Review Letters</i>. American Physical Society. <a href=\"https://doi.org/10.1103/physrevlett.121.226801\">https://doi.org/10.1103/physrevlett.121.226801</a>","ama":"Polshyn H, Zhou H, Spanton EM, Taniguchi T, Watanabe K, Young AF. Quantitative transport measurements of fractional quantum Hall energy gaps in edgeless graphene devices. <i>Physical Review Letters</i>. 2018;121(22). doi:<a href=\"https://doi.org/10.1103/physrevlett.121.226801\">10.1103/physrevlett.121.226801</a>","mla":"Polshyn, Hryhoriy, et al. “Quantitative Transport Measurements of Fractional Quantum Hall Energy Gaps in Edgeless Graphene Devices.” <i>Physical Review Letters</i>, vol. 121, no. 22, 226801, American Physical Society, 2018, doi:<a href=\"https://doi.org/10.1103/physrevlett.121.226801\">10.1103/physrevlett.121.226801</a>.","short":"H. Polshyn, H. Zhou, E.M. Spanton, T. Taniguchi, K. Watanabe, A.F. Young, Physical Review Letters 121 (2018).","ista":"Polshyn H, Zhou H, Spanton EM, Taniguchi T, Watanabe K, Young AF. 2018. Quantitative transport measurements of fractional quantum Hall energy gaps in edgeless graphene devices. Physical Review Letters. 121(22), 226801."},"publication_identifier":{"eissn":["1079-7114"],"issn":["0031-9007"]},"article_number":"226801","date_published":"2018-11-28T00:00:00Z","author":[{"id":"edfc7cb1-526e-11ec-b05a-e6ecc27e4e48","full_name":"Polshyn, Hryhoriy","orcid":"0000-0001-8223-8896","last_name":"Polshyn","first_name":"Hryhoriy"},{"full_name":"Zhou, H.","first_name":"H.","last_name":"Zhou"},{"first_name":"E. M.","last_name":"Spanton","full_name":"Spanton, E. M."},{"full_name":"Taniguchi, T.","last_name":"Taniguchi","first_name":"T."},{"full_name":"Watanabe, K.","last_name":"Watanabe","first_name":"K."},{"first_name":"A. F.","last_name":"Young","full_name":"Young, A. F."}],"article_processing_charge":"No","date_updated":"2022-01-14T13:48:35Z","doi":"10.1103/physrevlett.121.226801","keyword":["general physics and astronomy"],"scopus_import":"1","quality_controlled":"1","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1805.04199"}],"intvolume":"       121","publication_status":"published","day":"28","month":"11","language":[{"iso":"eng"}]},{"date_created":"2022-04-07T07:45:50Z","oa_version":"Published Version","publication":"Nature Communications","title":"Nucleolar expansion and elevated protein translation in premature aging","publisher":"Springer Nature","abstract":[{"lang":"eng","text":"Premature aging disorders provide an opportunity to study the mechanisms that drive aging. In Hutchinson-Gilford progeria syndrome (HGPS), a mutant form of the nuclear scaffold protein lamin A distorts nuclei and sequesters nuclear proteins. We sought to investigate protein homeostasis in this disease. Here, we report a widespread increase in protein turnover in HGPS-derived cells compared to normal cells. We determine that global protein synthesis is elevated as a consequence of activated nucleoli and enhanced ribosome biogenesis in HGPS-derived fibroblasts. Depleting normal lamin A or inducing mutant lamin A expression are each sufficient to drive nucleolar expansion. We further show that nucleolar size correlates with donor age in primary fibroblasts derived from healthy individuals and that ribosomal RNA production increases with age, indicating that nucleolar size and activity can serve as aging biomarkers. While limiting ribosome biogenesis extends lifespan in several systems, we show that increased ribosome biogenesis and activity are a hallmark of premature aging."}],"extern":"1","_id":"11065","year":"2017","volume":8,"user_id":"72615eeb-f1f3-11ec-aa25-d4573ddc34fd","type":"journal_article","citation":{"mla":"Buchwalter, Abigail, and Martin Hetzer. “Nucleolar Expansion and Elevated Protein Translation in Premature Aging.” <i>Nature Communications</i>, vol. 8, 328, Springer Nature, 2017, doi:<a href=\"https://doi.org/10.1038/s41467-017-00322-z\">10.1038/s41467-017-00322-z</a>.","ista":"Buchwalter A, Hetzer M. 2017. Nucleolar expansion and elevated protein translation in premature aging. Nature Communications. 8, 328.","short":"A. Buchwalter, M. Hetzer, Nature Communications 8 (2017).","ama":"Buchwalter A, Hetzer M. Nucleolar expansion and elevated protein translation in premature aging. <i>Nature Communications</i>. 2017;8. doi:<a href=\"https://doi.org/10.1038/s41467-017-00322-z\">10.1038/s41467-017-00322-z</a>","apa":"Buchwalter, A., &#38; Hetzer, M. (2017). Nucleolar expansion and elevated protein translation in premature aging. <i>Nature Communications</i>. Springer Nature. <a href=\"https://doi.org/10.1038/s41467-017-00322-z\">https://doi.org/10.1038/s41467-017-00322-z</a>","chicago":"Buchwalter, Abigail, and Martin Hetzer. “Nucleolar Expansion and Elevated Protein Translation in Premature Aging.” <i>Nature Communications</i>. Springer Nature, 2017. <a href=\"https://doi.org/10.1038/s41467-017-00322-z\">https://doi.org/10.1038/s41467-017-00322-z</a>.","ieee":"A. Buchwalter and M. Hetzer, “Nucleolar expansion and elevated protein translation in premature aging,” <i>Nature Communications</i>, vol. 8. Springer Nature, 2017."},"publication_identifier":{"issn":["2041-1723"]},"oa":1,"status":"public","external_id":{"pmid":["28855503"]},"article_type":"original","article_number":"328","keyword":["General Physics and Astronomy","General Biochemistry","Genetics and Molecular Biology","General Chemistry"],"scopus_import":"1","quality_controlled":"1","author":[{"full_name":"Buchwalter, Abigail","last_name":"Buchwalter","first_name":"Abigail"},{"id":"86c0d31b-b4eb-11ec-ac5a-eae7b2e135ed","full_name":"HETZER, Martin W","orcid":"0000-0002-2111-992X","last_name":"HETZER","first_name":"Martin W"}],"date_published":"2017-08-30T00:00:00Z","article_processing_charge":"No","date_updated":"2022-07-18T08:33:03Z","doi":"10.1038/s41467-017-00322-z","intvolume":"         8","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1038/s41467-017-00322-z"}],"publication_status":"published","month":"08","language":[{"iso":"eng"}],"pmid":1,"day":"30"},{"_id":"11518","year":"2017","volume":851,"type":"journal_article","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"ama":"Matthee JJ, Sobral D, Boone F, et al. ALMA reveals metals yet no dust within multiple components in CR7. <i>The Astrophysical Journal</i>. 2017;851(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/aa9931\">10.3847/1538-4357/aa9931</a>","short":"J.J. Matthee, D. Sobral, F. Boone, H. Röttgering, D. Schaerer, M. Girard, A. Pallottini, L. Vallini, A. Ferrara, B. Darvish, B. Mobasher, The Astrophysical Journal 851 (2017).","mla":"Matthee, Jorryt J., et al. “ALMA Reveals Metals yet No Dust within Multiple Components in CR7.” <i>The Astrophysical Journal</i>, vol. 851, no. 2, 145, IOP Publishing, 2017, doi:<a href=\"https://doi.org/10.3847/1538-4357/aa9931\">10.3847/1538-4357/aa9931</a>.","ista":"Matthee JJ, Sobral D, Boone F, Röttgering H, Schaerer D, Girard M, Pallottini A, Vallini L, Ferrara A, Darvish B, Mobasher B. 2017. ALMA reveals metals yet no dust within multiple components in CR7. The Astrophysical Journal. 851(2), 145.","ieee":"J. J. Matthee <i>et al.</i>, “ALMA reveals metals yet no dust within multiple components in CR7,” <i>The Astrophysical Journal</i>, vol. 851, no. 2. IOP Publishing, 2017.","chicago":"Matthee, Jorryt J, D. Sobral, F. Boone, H. Röttgering, D. Schaerer, M. Girard, A. Pallottini, et al. “ALMA Reveals Metals yet No Dust within Multiple Components in CR7.” <i>The Astrophysical Journal</i>. IOP Publishing, 2017. <a href=\"https://doi.org/10.3847/1538-4357/aa9931\">https://doi.org/10.3847/1538-4357/aa9931</a>.","apa":"Matthee, J. J., Sobral, D., Boone, F., Röttgering, H., Schaerer, D., Girard, M., … Mobasher, B. (2017). ALMA reveals metals yet no dust within multiple components in CR7. <i>The Astrophysical Journal</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/1538-4357/aa9931\">https://doi.org/10.3847/1538-4357/aa9931</a>"},"publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"status":"public","oa":1,"acknowledgement":"We thank the referee for their constructive comments, which have helped improve the quality and clarity of this work. We thank Raffaella Schneider for comments on an earlier version of this paper. We thank Leindert Boogaard, Steven Bos, Rychard Bouwens, and Renske Smit for discussions. J.M. acknowledges the support of a Huygens PhD fellowship from Leiden University. D.S. acknowledges financial support from the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship and from Lancaster University through an Early Career Internal Grant A100679. A.F. acknowledges support from the ERC Advanced Grant INTERSTELLAR H2020/740120. B.D. acknowledges financial support from NASA through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 294.A-5018. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2015.1.00122.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ.","article_type":"original","external_id":{"arxiv":["1709.06569"]},"issue":"2","oa_version":"Preprint","date_created":"2022-07-07T08:48:04Z","title":"ALMA reveals metals yet no dust within multiple components in CR7","publication":"The Astrophysical Journal","publisher":"IOP Publishing","abstract":[{"text":"We present spectroscopic follow-up observations of CR7 with ALMA, targeted at constraining the infrared (IR) continuum and [C II]158 mm line-emission at high spatial resolution matched to the HST/WFC3 imaging. CR7 is a luminous Lyα emitting galaxy at z = 6.6 that consists of three separated UV-continuum components. Our observations reveal several well-separated components of [C II] emission. The two most luminous components in [C II] coincide with the brightest UV components (A and B), blueshifted by »150 km s−1 with respect to the\r\npeak of Lyα emission. Other [C II] components are observed close to UV clumps B and C and are blueshifted by »300 and ≈80 km s−1 with respect to the systemic redshift. We do not detect FIR continuum emission due to dust with a 3σ limiting luminosity LIR T L d 35 K 3.1 10 = <´ 10 ( ) . This allows us to mitigate uncertainties in the dust-corrected SFR and derive SFRs for the three UV clumps A, B, and C of 28, 5, and 7 M yr−1. All clumps have [C II] luminosities consistent within the scatter observed in the local relation between SFR and L[ ] C II , implying that strong Lyα emission does not necessarily anti-correlate with [C II] luminosity. Combining\r\nour measurements with the literature, we show that galaxies with blue UV slopes have weaker [C II] emission at fixed SFR, potentially due to their lower metallicities and/or higher photoionization. Comparison with hydrodynamical simulations suggests that CR7ʼs clumps have metallicities of 0.1 Z Z 0.2 < < . The observed ISM structure of CR7 indicates that we are likely witnessing the build up of a central galaxy in the early universe through complex accretion of satellites.","lang":"eng"}],"extern":"1","arxiv":1,"intvolume":"       851","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1709.06569"}],"publication_status":"published","language":[{"iso":"eng"}],"month":"12","day":"21","article_number":"145","scopus_import":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics","dark ages","reionization","first stars – galaxies: formation – galaxies: high-redshift – galaxies: ISM – galaxies: kinematics and dynamics"],"quality_controlled":"1","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J"},{"first_name":"D.","last_name":"Sobral","full_name":"Sobral, D."},{"full_name":"Boone, F.","first_name":"F.","last_name":"Boone"},{"full_name":"Röttgering, H.","last_name":"Röttgering","first_name":"H."},{"last_name":"Schaerer","first_name":"D.","full_name":"Schaerer, D."},{"last_name":"Girard","first_name":"M.","full_name":"Girard, M."},{"first_name":"A.","last_name":"Pallottini","full_name":"Pallottini, A."},{"first_name":"L.","last_name":"Vallini","full_name":"Vallini, L."},{"full_name":"Ferrara, A.","last_name":"Ferrara","first_name":"A."},{"full_name":"Darvish, B.","first_name":"B.","last_name":"Darvish"},{"full_name":"Mobasher, B.","last_name":"Mobasher","first_name":"B."}],"date_published":"2017-12-21T00:00:00Z","doi":"10.3847/1538-4357/aa9931","date_updated":"2022-08-18T10:23:35Z","article_processing_charge":"No"}]