[{"article_processing_charge":"Yes (in subscription journal)","issue":"4","oa":1,"date_updated":"2024-01-23T12:33:50Z","title":"Linking UV spectral properties of MUSE Ly α emitters at <i>z</i> ≳ 3 to Lyman continuum escape","has_accepted_license":"1","intvolume":"       527","language":[{"iso":"eng"}],"publication":"Monthly Notices of the Royal Astronomical Society","arxiv":1,"author":[{"first_name":"Ivan","full_name":"Kramarenko, Ivan","last_name":"Kramarenko","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4"},{"full_name":"Kerutt, J","first_name":"J","last_name":"Kerutt"},{"last_name":"Verhamme","full_name":"Verhamme, A","first_name":"A"},{"full_name":"Oesch, P A","first_name":"P A","last_name":"Oesch"},{"last_name":"Barrufet","full_name":"Barrufet, L","first_name":"L"},{"first_name":"Jorryt J","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X"},{"last_name":"Kusakabe","full_name":"Kusakabe, H","first_name":"H"},{"full_name":"Goovaerts, I","first_name":"I","last_name":"Goovaerts"},{"first_name":"T T","full_name":"Thai, T T","last_name":"Thai"}],"month":"02","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","file":[{"file_name":"2024_MNAstronomSoc_Kramarenko.pdf","file_id":"14879","checksum":"9d02df4035c4951cf63dee0db1e462e9","success":1,"date_updated":"2024-01-23T12:30:45Z","date_created":"2024-01-23T12:30:45Z","creator":"dernst","content_type":"application/pdf","file_size":4521738,"access_level":"open_access","relation":"main_file"}],"oa_version":"Published Version","day":"01","type":"journal_article","status":"public","year":"2024","acknowledgement":"We thank the anonymous referee for the constructive feedback that helped to improve the manuscript. We thank Michael Maseda, Daniel Schaerer, Charlotte Simmonds, and Rashmi Gottumukkala for useful comments and productive discussions. We also thank the organizers and participants of the 24th MUSE Science Busy Week in Leiden. IGK acknowledges an Excellence Master Fellowship granted by the Faculty of Science of the University of Geneva. This work has received funding from the Swiss State Secretariat for Education, Research and Innovation (SERI) under contract number MB22.00072, as well as from the Swiss National Science Foundation (SNSF) through project grant number 200020_207349 and SNSF Professorship grant number 190079. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant number 140. This paper is based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programmes 094.A-0289(B), 095.A-0010(A), 096.A-0045(A), 096.A-0045(B), 094.A-0205, 095.A-0240, 096.A-0090, 097.A-0160, and 098.A-0017. We made extensive use of several open-source software packages and we are thankful to the respective authors for sharing their work: NUMPY (Harris et al. 2020), ASTROPY (Astropy Collaboration 2022), MATPLOTLIB (Hunter 2007), IPYTHON (Perez & Granger 2007), and TOPCAT (Taylor 2005).","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"date_created":"2024-01-22T08:22:17Z","citation":{"mla":"Kramarenko, Ivan, et al. “Linking UV Spectral Properties of MUSE Ly α Emitters at <i>z</i> ≳ 3 to Lyman Continuum Escape.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 527, no. 4, Oxford University Press, 2024, pp. 9853–71, doi:<a href=\"https://doi.org/10.1093/mnras/stad3853\">10.1093/mnras/stad3853</a>.","chicago":"Kramarenko, Ivan, J Kerutt, A Verhamme, P A Oesch, L Barrufet, Jorryt J Matthee, H Kusakabe, I Goovaerts, and T T Thai. “Linking UV Spectral Properties of MUSE Ly α Emitters at <i>z</i> ≳ 3 to Lyman Continuum Escape.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2024. <a href=\"https://doi.org/10.1093/mnras/stad3853\">https://doi.org/10.1093/mnras/stad3853</a>.","ista":"Kramarenko I, Kerutt J, Verhamme A, Oesch PA, Barrufet L, Matthee JJ, Kusakabe H, Goovaerts I, Thai TT. 2024. Linking UV spectral properties of MUSE Ly α emitters at <i>z</i> ≳ 3 to Lyman continuum escape. Monthly Notices of the Royal Astronomical Society. 527(4), 9853–9871.","short":"I. Kramarenko, J. Kerutt, A. Verhamme, P.A. Oesch, L. Barrufet, J.J. Matthee, H. Kusakabe, I. Goovaerts, T.T. Thai, Monthly Notices of the Royal Astronomical Society 527 (2024) 9853–9871.","ama":"Kramarenko I, Kerutt J, Verhamme A, et al. Linking UV spectral properties of MUSE Ly α emitters at <i>z</i> ≳ 3 to Lyman continuum escape. <i>Monthly Notices of the Royal Astronomical Society</i>. 2024;527(4):9853-9871. doi:<a href=\"https://doi.org/10.1093/mnras/stad3853\">10.1093/mnras/stad3853</a>","ieee":"I. Kramarenko <i>et al.</i>, “Linking UV spectral properties of MUSE Ly α emitters at <i>z</i> ≳ 3 to Lyman continuum escape,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 527, no. 4. Oxford University Press, pp. 9853–9871, 2024.","apa":"Kramarenko, I., Kerutt, J., Verhamme, A., Oesch, P. A., Barrufet, L., Matthee, J. J., … Thai, T. T. (2024). Linking UV spectral properties of MUSE Ly α emitters at <i>z</i> ≳ 3 to Lyman continuum escape. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stad3853\">https://doi.org/10.1093/mnras/stad3853</a>"},"_id":"14852","article_type":"original","file_date_updated":"2024-01-23T12:30:45Z","doi":"10.1093/mnras/stad3853","publication_status":"published","tmp":{"name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","short":"CC BY (4.0)","image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"ddc":["520"],"abstract":[{"text":"The physical conditions giving rise to high escape fractions of ionizing radiation (LyC fesc) in star-forming galaxies – most likely protagonists of cosmic reionization – are not yet fully understood. Using the VLT/MUSE observations of ∼1400 Ly α emitters at 2.9 &amp;lt; z &amp;lt; 6.7, we compare stacked rest-frame UV spectra of candidates for LyC leakers and non-leakers selected based on their Ly α profiles. We find that the stacks of potential LyC leakers, i.e. galaxies with narrow, symmetric Ly α profiles with small peak separation, generally show (i) strong nebular O iii]λ1666, [Si iii]λ1883, and [C iii]λ1907 +C iii]λ1909 emission, indicating a high-ionization state of the interstellar medium (ISM); (ii) high equivalent widths of He iiλ1640 (∼1 − 3 Å), suggesting the presence of hard ionizing radiation fields; (iii) Si ii*λ1533 emission, revealing substantial amounts of neutral hydrogen off the line of sight; (iv) high C ivλλ1548,1550 to [C iii]λ1907 +C iii]λ1909 ratios (C iv/C iii] ≳0.75) , signalling the presence of low column density channels in the ISM. In contrast, the stacks with broad, asymmetric Ly α profiles with large peak separation show weak nebular emission lines, low He iiλ1640 equivalent widths (≲1 Å), and low C iv/C iii] (≲0.25), implying low-ionization states and high-neutral hydrogen column densities. Our results suggest that C iv/C iii] might be sensitive to the physical conditions that govern LyC photon escape, providing a promising tool for identification of ionizing sources among star-forming galaxies in the epoch of reionization.","lang":"eng"}],"external_id":{"arxiv":["2305.07044"]},"date_published":"2024-02-01T00:00:00Z","publisher":"Oxford University Press","quality_controlled":"1","volume":527,"page":"9853-9871","department":[{"_id":"GradSch"},{"_id":"JoMa"}]},{"external_id":{"arxiv":["2305.07337"]},"abstract":[{"lang":"eng","text":"Thorne–Żytkow objects (TŻO) are potential end products of the merger of a neutron star with a non-degenerate star. In this work, we have computed the first grid of evolutionary models of TŻOs with the MESA stellar evolution code. With these models, we predict several observational properties of TŻOs, including their surface temperatures and luminosities, pulsation periods, and nucleosynthetic products. We expand the range of possible TŻO solutions to cover 3.45≲log(Teff/K)≲3.65 and 4.85≲log(L/L⊙)≲5.5⁠. Due to the much higher densities our TŻOs reach compared to previous models, if TŻOs form we expect them to be stable over a larger mass range than previously predicted, without exhibiting a gap in their mass distribution. Using the GYRE stellar pulsation code we show that TŻOs should have fundamental pulsation periods of 1000–2000 d, and period ratios of ≈0.2–0.3. Models computed with a large 399 isotope fully coupled nuclear network show a nucleosynthetic signal that is different to previously predicted. We propose a new nucleosynthetic signal to determine a star’s status as a TŻO: the isotopologues 44TiO2 and 44TiO⁠, which will have a shift in their spectral features as compared to stable titanium-containing molecules. We find that in the local Universe (∼SMC metallicities and above) TŻOs show little heavy metal enrichment, potentially explaining the difficulty in finding TŻOs to-date."}],"publication_status":"published","extern":"1","page":"1692-1709","volume":524,"quality_controlled":"1","publisher":"Oxford University Press","date_published":"2023-09-01T00:00:00Z","date_created":"2023-08-21T10:13:56Z","citation":{"apa":"Farmer, R., Renzo, M., Götberg, Y. L. L., Bellinger, E., Justham, S., &#38; de Mink, S. E. (2023). Observational predictions for Thorne–Żytkow objects. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stad1977\">https://doi.org/10.1093/mnras/stad1977</a>","chicago":"Farmer, R, M Renzo, Ylva Louise Linsdotter Götberg, E Bellinger, S Justham, and S E de Mink. “Observational Predictions for Thorne–Żytkow Objects.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2023. <a href=\"https://doi.org/10.1093/mnras/stad1977\">https://doi.org/10.1093/mnras/stad1977</a>.","mla":"Farmer, R., et al. “Observational Predictions for Thorne–Żytkow Objects.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 524, no. 2, Oxford University Press, 2023, pp. 1692–709, doi:<a href=\"https://doi.org/10.1093/mnras/stad1977\">10.1093/mnras/stad1977</a>.","ista":"Farmer R, Renzo M, Götberg YLL, Bellinger E, Justham S, de Mink SE. 2023. Observational predictions for Thorne–Żytkow objects. Monthly Notices of the Royal Astronomical Society. 524(2), 1692–1709.","ama":"Farmer R, Renzo M, Götberg YLL, Bellinger E, Justham S, de Mink SE. Observational predictions for Thorne–Żytkow objects. <i>Monthly Notices of the Royal Astronomical Society</i>. 2023;524(2):1692-1709. doi:<a href=\"https://doi.org/10.1093/mnras/stad1977\">10.1093/mnras/stad1977</a>","ieee":"R. Farmer, M. Renzo, Y. L. L. Götberg, E. Bellinger, S. Justham, and S. E. de Mink, “Observational predictions for Thorne–Żytkow objects,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 524, no. 2. Oxford University Press, pp. 1692–1709, 2023.","short":"R. Farmer, M. Renzo, Y.L.L. Götberg, E. Bellinger, S. Justham, S.E. de Mink, Monthly Notices of the Royal Astronomical Society 524 (2023) 1692–1709."},"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"year":"2023","doi":"10.1093/mnras/stad1977","article_type":"original","_id":"14104","day":"01","oa_version":"Preprint","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2305.07337"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"month":"09","author":[{"first_name":"R","full_name":"Farmer, R","last_name":"Farmer"},{"last_name":"Renzo","first_name":"M","full_name":"Renzo, M"},{"last_name":"Götberg","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","orcid":"0000-0002-6960-6911","full_name":"Götberg, Ylva Louise Linsdotter","first_name":"Ylva Louise Linsdotter"},{"full_name":"Bellinger, E","first_name":"E","last_name":"Bellinger"},{"full_name":"Justham, S","first_name":"S","last_name":"Justham"},{"first_name":"S E","full_name":"de Mink, S E","last_name":"de Mink"}],"arxiv":1,"type":"journal_article","status":"public","intvolume":"       524","scopus_import":"1","title":"Observational predictions for Thorne–Żytkow objects","date_updated":"2023-08-21T12:12:48Z","oa":1,"issue":"2","article_processing_charge":"No","publication":"Monthly Notices of the Royal Astronomical Society","language":[{"iso":"eng"}]},{"intvolume":"       517","scopus_import":"1","title":"The effects of surface fossil magnetic fields on massive star evolution: IV. Grids of models at Solar, LMC, and SMC metallicities","issue":"2","article_processing_charge":"No","oa":1,"date_updated":"2023-08-21T12:02:17Z","publication":"Monthly Notices of the Royal Astronomical Society","language":[{"iso":"eng"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa_version":"Preprint","main_file_link":[{"url":"https://arxiv.org/abs/2209.06350","open_access":"1"}],"day":"01","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"month":"12","arxiv":1,"author":[{"first_name":"Z","full_name":"Keszthelyi, Z","last_name":"Keszthelyi"},{"full_name":"de Koter, A","first_name":"A","last_name":"de Koter"},{"full_name":"Götberg, Ylva Louise Linsdotter","first_name":"Ylva Louise Linsdotter","last_name":"Götberg","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","orcid":"0000-0002-6960-6911"},{"last_name":"Meynet","full_name":"Meynet, G","first_name":"G"},{"last_name":"Brands","full_name":"Brands, S A","first_name":"S A"},{"last_name":"Petit","first_name":"V","full_name":"Petit, V"},{"full_name":"Carrington, M","first_name":"M","last_name":"Carrington"},{"last_name":"David-Uraz","first_name":"A","full_name":"David-Uraz, A"},{"last_name":"Geen","first_name":"S T","full_name":"Geen, S T"},{"last_name":"Georgy","first_name":"C","full_name":"Georgy, C"},{"full_name":"Hirschi, R","first_name":"R","last_name":"Hirschi"},{"last_name":"Puls","full_name":"Puls, J","first_name":"J"},{"full_name":"Ramalatswa, K J","first_name":"K J","last_name":"Ramalatswa"},{"last_name":"Shultz","first_name":"M E","full_name":"Shultz, M E"},{"full_name":"ud-Doula, A","first_name":"A","last_name":"ud-Doula"}],"status":"public","type":"journal_article","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"citation":{"apa":"Keszthelyi, Z., de Koter, A., Götberg, Y. L. L., Meynet, G., Brands, S. A., Petit, V., … ud-Doula, A. (2022). The effects of surface fossil magnetic fields on massive star evolution: IV. Grids of models at Solar, LMC, and SMC metallicities. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stac2598\">https://doi.org/10.1093/mnras/stac2598</a>","ista":"Keszthelyi Z, de Koter A, Götberg YLL, Meynet G, Brands SA, Petit V, Carrington M, David-Uraz A, Geen ST, Georgy C, Hirschi R, Puls J, Ramalatswa KJ, Shultz ME, ud-Doula A. 2022. The effects of surface fossil magnetic fields on massive star evolution: IV. Grids of models at Solar, LMC, and SMC metallicities. Monthly Notices of the Royal Astronomical Society. 517(2), 2028–2055.","mla":"Keszthelyi, Z., et al. “The Effects of Surface Fossil Magnetic Fields on Massive Star Evolution: IV. Grids of Models at Solar, LMC, and SMC Metallicities.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 517, no. 2, Oxford University Press, 2022, pp. 2028–55, doi:<a href=\"https://doi.org/10.1093/mnras/stac2598\">10.1093/mnras/stac2598</a>.","chicago":"Keszthelyi, Z, A de Koter, Ylva Louise Linsdotter Götberg, G Meynet, S A Brands, V Petit, M Carrington, et al. “The Effects of Surface Fossil Magnetic Fields on Massive Star Evolution: IV. Grids of Models at Solar, LMC, and SMC Metallicities.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2022. <a href=\"https://doi.org/10.1093/mnras/stac2598\">https://doi.org/10.1093/mnras/stac2598</a>.","short":"Z. Keszthelyi, A. de Koter, Y.L.L. Götberg, G. Meynet, S.A. Brands, V. Petit, M. Carrington, A. David-Uraz, S.T. Geen, C. Georgy, R. Hirschi, J. Puls, K.J. Ramalatswa, M.E. Shultz, A. ud-Doula, Monthly Notices of the Royal Astronomical Society 517 (2022) 2028–2055.","ama":"Keszthelyi Z, de Koter A, Götberg YLL, et al. The effects of surface fossil magnetic fields on massive star evolution: IV. Grids of models at Solar, LMC, and SMC metallicities. <i>Monthly Notices of the Royal Astronomical Society</i>. 2022;517(2):2028-2055. doi:<a href=\"https://doi.org/10.1093/mnras/stac2598\">10.1093/mnras/stac2598</a>","ieee":"Z. Keszthelyi <i>et al.</i>, “The effects of surface fossil magnetic fields on massive star evolution: IV. Grids of models at Solar, LMC, and SMC metallicities,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 517, no. 2. Oxford University Press, pp. 2028–2055, 2022."},"date_created":"2023-08-03T10:10:37Z","year":"2022","doi":"10.1093/mnras/stac2598","_id":"13452","article_type":"original","abstract":[{"lang":"eng","text":"Magnetic fields can drastically change predictions of evolutionary models of massive stars via mass-loss quenching, magnetic braking, and efficient angular momentum transport, which we aim to quantify in this work. We use the MESA software instrument to compute an extensive main-sequence grid of stellar structure and evolution models, as well as isochrones, accounting for the effects attributed to a surface fossil magnetic field. The grid is densely populated in initial mass (3–60 M⊙), surface equatorial magnetic field strength (0–50 kG), and metallicity (representative of the Solar neighbourhood and the Magellanic Clouds). We use two magnetic braking and two chemical mixing schemes and compare the model predictions for slowly rotating, nitrogen-enriched (‘Group 2’) stars with observations in the Large Magellanic Cloud. We quantify a range of initial field strengths that allow for producing Group 2 stars and find that typical values (up to a few kG) lead to solutions. Between the subgrids, we find notable departures in surface abundances and evolutionary paths. In our magnetic models, chemical mixing is always less efficient compared to non-magnetic models due to the rapid spin-down. We identify that quasi-chemically homogeneous main sequence evolution by efficient mixing could be prevented by fossil magnetic fields. We recommend comparing this grid of evolutionary models with spectropolarimetric and spectroscopic observations with the goals of (i) revisiting the derived stellar parameters of known magnetic stars, and (ii) observationally constraining the uncertain magnetic braking and chemical mixing schemes."}],"external_id":{"arxiv":["2209.06350"]},"publication_status":"published","volume":517,"quality_controlled":"1","extern":"1","page":"2028-2055","date_published":"2022-12-01T00:00:00Z","publisher":"Oxford University Press"},{"title":"The effects of surface fossil magnetic fields on massive star evolution: IV. Grids of models at solar, LMC, and SMC metallicities","issue":"2","article_processing_charge":"No","oa":1,"date_updated":"2023-08-22T13:18:34Z","intvolume":"       517","scopus_import":"1","language":[{"iso":"eng"}],"publication":"Monthly Notices of the Royal Astronomical Society","arxiv":1,"author":[{"last_name":"Keszthelyi","full_name":"Keszthelyi, Z.","first_name":"Z."},{"full_name":"Koter, A. de","first_name":"A. de","last_name":"Koter"},{"last_name":"Götberg","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","orcid":"0000-0002-6960-6911","first_name":"Ylva Louise Linsdotter","full_name":"Götberg, Ylva Louise Linsdotter"},{"full_name":"Meynet, G.","first_name":"G.","last_name":"Meynet"},{"last_name":"Brands","first_name":"S. A.","full_name":"Brands, S. A."},{"last_name":"Petit","first_name":"V.","full_name":"Petit, V."},{"full_name":"Carrington, M.","first_name":"M.","last_name":"Carrington"},{"last_name":"A. David-Uraz","full_name":"A. David-Uraz, A. David-Uraz","first_name":"A. David-Uraz"},{"full_name":"Geen, S. T.","first_name":"S. T.","last_name":"Geen"},{"last_name":"Georgy","first_name":"C.","full_name":"Georgy, C."},{"last_name":"Hirschi","first_name":"R.","full_name":"Hirschi, R."},{"last_name":"Puls","full_name":"Puls, J.","first_name":"J."},{"first_name":"K. J.","full_name":"Ramalatswa, K. J.","last_name":"Ramalatswa"},{"first_name":"M. E.","full_name":"Shultz, M. E.","last_name":"Shultz"},{"first_name":"A. ud-Doula","full_name":"A. ud-Doula, A. ud-Doula","last_name":"A. ud-Doula"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/stac2598"}],"oa_version":"Published Version","day":"01","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"month":"12","status":"public","type":"journal_article","date_created":"2023-08-21T10:11:21Z","citation":{"short":"Z. Keszthelyi, A. de Koter, Y.L.L. Götberg, G. Meynet, S.A. Brands, V. Petit, M. Carrington, A.D.-U. A. David-Uraz, S.T. Geen, C. Georgy, R. Hirschi, J. Puls, K.J. Ramalatswa, M.E. Shultz, A. ud-Doula A. ud-Doula, Monthly Notices of the Royal Astronomical Society 517 (2022) 2028–2055.","ieee":"Z. Keszthelyi <i>et al.</i>, “The effects of surface fossil magnetic fields on massive star evolution: IV. Grids of models at solar, LMC, and SMC metallicities,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 517, no. 2. Oxford Academic, pp. 2028–2055, 2022.","ama":"Keszthelyi Z, Koter A de, Götberg YLL, et al. The effects of surface fossil magnetic fields on massive star evolution: IV. Grids of models at solar, LMC, and SMC metallicities. <i>Monthly Notices of the Royal Astronomical Society</i>. 2022;517(2):2028-2055. doi:<a href=\"https://doi.org/10.1093/mnras/stac2598\">10.1093/mnras/stac2598</a>","ista":"Keszthelyi Z, Koter A de, Götberg YLL, Meynet G, Brands SA, Petit V, Carrington M, A. David-Uraz AD-U, Geen ST, Georgy C, Hirschi R, Puls J, Ramalatswa KJ, Shultz ME, A. ud-Doula A ud-Doula. 2022. The effects of surface fossil magnetic fields on massive star evolution: IV. Grids of models at solar, LMC, and SMC metallicities. Monthly Notices of the Royal Astronomical Society. 517(2), 2028–2055.","chicago":"Keszthelyi, Z., A. de Koter, Ylva Louise Linsdotter Götberg, G. Meynet, S. A. Brands, V. Petit, M. Carrington, et al. “The Effects of Surface Fossil Magnetic Fields on Massive Star Evolution: IV. Grids of Models at Solar, LMC, and SMC Metallicities.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford Academic, 2022. <a href=\"https://doi.org/10.1093/mnras/stac2598\">https://doi.org/10.1093/mnras/stac2598</a>.","mla":"Keszthelyi, Z., et al. “The Effects of Surface Fossil Magnetic Fields on Massive Star Evolution: IV. Grids of Models at Solar, LMC, and SMC Metallicities.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 517, no. 2, Oxford Academic, 2022, pp. 2028–55, doi:<a href=\"https://doi.org/10.1093/mnras/stac2598\">10.1093/mnras/stac2598</a>.","apa":"Keszthelyi, Z., Koter, A. de, Götberg, Y. L. L., Meynet, G., Brands, S. A., Petit, V., … A. ud-Doula, A. ud-Doula. (2022). The effects of surface fossil magnetic fields on massive star evolution: IV. Grids of models at solar, LMC, and SMC metallicities. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford Academic. <a href=\"https://doi.org/10.1093/mnras/stac2598\">https://doi.org/10.1093/mnras/stac2598</a>"},"year":"2022","article_type":"original","_id":"14098","doi":"10.1093/mnras/stac2598","publication_status":"published","abstract":[{"lang":"eng","text":"Magnetic fields can drastically change predictions of evolutionary models of massive stars via mass-loss quenching, magnetic braking, and efficient angular momentum transport, which we aim to quantify in this work. We use the MESA software instrument to compute an extensive main-sequence grid of stellar structure and evolution models, as well as isochrones, accounting for the effects attributed to a surface fossil magnetic field. The grid is densely populated in initial mass (3–60 M⊙), surface equatorial magnetic field strength (0–50 kG), and metallicity (representative of the Solar neighbourhood and the Magellanic Clouds). We use two magnetic braking and two chemical mixing schemes and compare the model predictions for slowly rotating, nitrogen-enriched (‘Group 2’) stars with observations in the Large Magellanic Cloud. We quantify a range of initial field strengths that allow for producing Group 2 stars and find that typical values (up to a few kG) lead to solutions. Between the subgrids, we find notable departures in surface abundances and evolutionary paths. In our magnetic models, chemical mixing is always less efficient compared to non-magnetic models due to the rapid spin-down. We identify that quasi-chemically homogeneous main sequence evolution by efficient mixing could be prevented by fossil magnetic fields. We recommend comparing this grid of evolutionary models with spectropolarimetric and spectroscopic observations with the goals of (i) revisiting the derived stellar parameters of known magnetic stars, and (ii) observationally constraining the uncertain magnetic braking and chemical mixing schemes."}],"external_id":{"arxiv":["2209.06350"]},"quality_controlled":"1","volume":517,"extern":"1","page":"2028-2055","date_published":"2022-12-01T00:00:00Z","publisher":"Oxford Academic"},{"keyword":["galaxies: high-redshift","intergalactic medium","cosmology: observations","dark ages","reionization","first stars","ultraviolet: galaxies"],"citation":{"apa":"Matthee, J. J., Naidu, R. P., Pezzulli, G., Gronke, M., Sobral, D., Oesch, P. A., … Röttgering, H. (2022). (Re)Solving reionization with Lyα: How bright Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stac801\">https://doi.org/10.1093/mnras/stac801</a>","short":"J.J. Matthee, R.P. Naidu, G. Pezzulli, M. Gronke, D. Sobral, P.A. Oesch, M. Hayes, D. Erb, D. Schaerer, R. Amorín, S. Tacchella, A.P.-A. Ana Paulino-Afonso, M. Llerena, J. Calhau, H. Röttgering, Monthly Notices of the Royal Astronomical Society 512 (2022) 5960–5977.","ieee":"J. J. Matthee <i>et al.</i>, “(Re)Solving reionization with Lyα: How bright Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 512, no. 4. Oxford University Press, pp. 5960–5977, 2022.","ama":"Matthee JJ, Naidu RP, Pezzulli G, et al. (Re)Solving reionization with Lyα: How bright Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background. <i>Monthly Notices of the Royal Astronomical Society</i>. 2022;512(4):5960-5977. doi:<a href=\"https://doi.org/10.1093/mnras/stac801\">10.1093/mnras/stac801</a>","mla":"Matthee, Jorryt J., et al. “(Re)Solving Reionization with Lyα: How Bright Lyα Emitters Account for the z ≈ 2 − 8 Cosmic Ionizing Background.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 512, no. 4, Oxford University Press, 2022, pp. 5960–77, doi:<a href=\"https://doi.org/10.1093/mnras/stac801\">10.1093/mnras/stac801</a>.","ista":"Matthee JJ, Naidu RP, Pezzulli G, Gronke M, Sobral D, Oesch PA, Hayes M, Erb D, Schaerer D, Amorín R, Tacchella S, Ana Paulino-Afonso AP-A, Llerena M, Calhau J, Röttgering H. 2022. (Re)Solving reionization with Lyα: How bright Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background. Monthly Notices of the Royal Astronomical Society. 512(4), 5960–5977.","chicago":"Matthee, Jorryt J, Rohan P. Naidu, Gabriele Pezzulli, Max Gronke, David Sobral, Pascal A. Oesch, Matthew Hayes, et al. “(Re)Solving Reionization with Lyα: How Bright Lyα Emitters Account for the z ≈ 2 − 8 Cosmic Ionizing Background.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2022. <a href=\"https://doi.org/10.1093/mnras/stac801\">https://doi.org/10.1093/mnras/stac801</a>."},"date_created":"2022-07-07T09:21:30Z","year":"2022","acknowledgement":"We thank an anonymous referee for an encouraging and constructive report that helped improving the quality of this work. We acknowledge illuminating conversations with Xiaohan Wu, Chris Cain, Anna-Christina Eilers, Simon Lilly and Ruari Mackenzie. RPN gratefully acknowledges an Ashford Fellowship granted by Harvard University. MG was supported by NASA through the NASA Hubble Fellowship grant HST-HF2-51409. PO acknowledges support from the Swiss National Science Foundation through the SNSF Professorship grant 190079. GP acknowledges support from the Netherlands Research School for Astronomy (NOVA). MH is fellow of the Knut and Alice Wallenberg Foundation. DE is supported by the US National Science Foundation (NSF) through Astronomy & Astrophysics grant AST-1909198. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant No. 140. RA acknowledges support from Fondecyt Regular Grant 1202007. ST is supported by the 2021 Research Fund 1.210134.01 of UNIST (Ulsan National Institute of Science & Technology). MLl acknowledges support from the ANID/Scholarship Program/Doctorado Nacional/2019-21191036. JC acknowledges support from the Spanish Ministry of Science and Innovation, project PID2019-107408GB-C43 (ESTALLIDOS) and from Gobierno de Canarias through EU FEDER funding, project PID2020010050.","doi":"10.1093/mnras/stac801","article_type":"original","_id":"11521","abstract":[{"text":"The cosmic ionizing emissivity from star-forming galaxies has long been anchored to UV luminosity functions. Here, we introduce an emissivity framework based on Lyα emitters (LAEs), which naturally hones in on the subset of galaxies responsible for the ionizing background due to the intimate connection between production and escape of Lyα and LyC photons. Using constraints on the escape fractions of bright LAEs (LLyα > 0.2L*) at z ≈ 2 obtained from resolved Lyα profiles, and arguing for their redshift-invariance, we show that: (i) quasars and LAEs together reproduce the relatively flat emissivity at z ≈ 2–6, which is non-trivial given the strong evolution in both the star formation density and quasar number density at these epochs and (ii) LAEs produce late and rapid reionization between z ≈ 6−9 under plausible assumptions. Within this framework, the >10 × rise in the UV population-averaged fesc between z ≈ 3–7 naturally arises due to the same phenomena that drive the growing LAE fraction with redshift. Generally, a LAE dominated emissivity yields a peak in the distribution of the ionizing budget with UV luminosity as reported in latest simulations. Using our adopted parameters (⁠fesc=50 per cent⁠, ξion = 1025.9 Hz erg−1 for half the bright LAEs), a highly ionizing minority of galaxies with MUV < −17 accounts for the entire ionizing budget from star-forming galaxies. Rapid flashes of LyC from such rare galaxies produce a ‘disco’ ionizing background. We conclude proposing tests to further develop our suggested Lyα-anchored formalism.","lang":"eng"}],"external_id":{"arxiv":["2110.11967"]},"publication_status":"published","volume":512,"quality_controlled":"1","page":"5960-5977","extern":"1","date_published":"2022-06-01T00:00:00Z","publisher":"Oxford University Press","scopus_import":"1","intvolume":"       512","title":"(Re)Solving reionization with Lyα: How bright Lyα emitters account for the z ≈ 2 − 8 cosmic ionizing background","article_processing_charge":"No","issue":"4","oa":1,"date_updated":"2022-08-18T10:42:47Z","publication":"Monthly Notices of the Royal Astronomical Society","language":[{"iso":"eng"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2110.11967"}],"day":"01","oa_version":"Preprint","month":"06","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"arxiv":1,"author":[{"first_name":"Jorryt J","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee"},{"last_name":"Naidu","full_name":"Naidu, Rohan P.","first_name":"Rohan P."},{"last_name":"Pezzulli","full_name":"Pezzulli, Gabriele","first_name":"Gabriele"},{"full_name":"Gronke, Max","first_name":"Max","last_name":"Gronke"},{"last_name":"Sobral","full_name":"Sobral, David","first_name":"David"},{"last_name":"Oesch","full_name":"Oesch, Pascal A.","first_name":"Pascal A."},{"full_name":"Hayes, Matthew","first_name":"Matthew","last_name":"Hayes"},{"last_name":"Erb","full_name":"Erb, Dawn","first_name":"Dawn"},{"last_name":"Schaerer","full_name":"Schaerer, Daniel","first_name":"Daniel"},{"full_name":"Amorín, Ricardo","first_name":"Ricardo","last_name":"Amorín"},{"last_name":"Tacchella","first_name":"Sandro","full_name":"Tacchella, Sandro"},{"last_name":"Ana Paulino-Afonso","full_name":"Ana Paulino-Afonso, Ana Paulino-Afonso","first_name":"Ana Paulino-Afonso"},{"full_name":"Llerena, Mario","first_name":"Mario","last_name":"Llerena"},{"last_name":"Calhau","first_name":"João","full_name":"Calhau, João"},{"full_name":"Röttgering, Huub","first_name":"Huub","last_name":"Röttgering"}],"status":"public","type":"journal_article"},{"doi":"10.1093/mnras/stab2762","_id":"11522","article_type":"original","keyword":["dark ages","reionization","first stars","intergalactic medium","galaxies: formation"],"citation":{"short":"M. Gronke, P. Ocvirk, C. Mason, J.J. Matthee, S.E.I. Bosman, J.G. Sorce, J. Lewis, K. Ahn, D. Aubert, T. Dawoodbhoy, I.T. Iliev, P.R. Shapiro, G. Yepes, Monthly Notices of the Royal Astronomical Society 508 (2021) 3697–3709.","ieee":"M. Gronke <i>et al.</i>, “Lyman-α transmission properties of the intergalactic medium in the CoDaII simulation,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 508, no. 3. Oxford University Press, pp. 3697–3709, 2021.","ama":"Gronke M, Ocvirk P, Mason C, et al. Lyman-α transmission properties of the intergalactic medium in the CoDaII simulation. <i>Monthly Notices of the Royal Astronomical Society</i>. 2021;508(3):3697-3709. doi:<a href=\"https://doi.org/10.1093/mnras/stab2762\">10.1093/mnras/stab2762</a>","ista":"Gronke M, Ocvirk P, Mason C, Matthee JJ, Bosman SEI, Sorce JG, Lewis J, Ahn K, Aubert D, Dawoodbhoy T, Iliev IT, Shapiro PR, Yepes G. 2021. Lyman-α transmission properties of the intergalactic medium in the CoDaII simulation. Monthly Notices of the Royal Astronomical Society. 508(3), 3697–3709.","mla":"Gronke, Max, et al. “Lyman-α Transmission Properties of the Intergalactic Medium in the CoDaII Simulation.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 508, no. 3, Oxford University Press, 2021, pp. 3697–709, doi:<a href=\"https://doi.org/10.1093/mnras/stab2762\">10.1093/mnras/stab2762</a>.","chicago":"Gronke, Max, Pierre Ocvirk, Charlotte Mason, Jorryt J Matthee, Sarah E I Bosman, Jenny G Sorce, Joseph Lewis, et al. “Lyman-α Transmission Properties of the Intergalactic Medium in the CoDaII Simulation.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2021. <a href=\"https://doi.org/10.1093/mnras/stab2762\">https://doi.org/10.1093/mnras/stab2762</a>.","apa":"Gronke, M., Ocvirk, P., Mason, C., Matthee, J. J., Bosman, S. E. I., Sorce, J. G., … Yepes, G. (2021). Lyman-α transmission properties of the intergalactic medium in the CoDaII simulation. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stab2762\">https://doi.org/10.1093/mnras/stab2762</a>"},"date_created":"2022-07-07T09:30:21Z","year":"2021","acknowledgement":"The authors thank the referee for constructive feedback that improved the outcome of this study. We are grateful to Antoinette Songaila Cowie for sharing the ‘NEPLA4’ spectrum with us. This research has made use of NASA’s Astrophysics Data System, and many open source projects such as trident (Hummels et al. 2017), IPython (Pérez & Granger 2007), SciPy (Virtanen et al. 2019), NumPy (Walt et al. 2011), matplotlib (Hunter 2007), pandas (McKinney 2010), and the yt-project (Turk et al. 2011). MG was supported by NASA through the NASA Hubble Fellowship grant HST-HF2-51409 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. MG acknowledges support from NASA grants HST-GO-15643.017, and HST-AR15797.001 as well as XSEDE grant TG-AST180036. CAM acknowledges support by NASA Headquarters through the NASA Hubble Fellowship grant HST-HF2-51413.001-A. PRS was supported in part by U.S. NSF grant AST-1009799, NASA grant NNX11AE09G, and supercomputer resources from NSF XSEDE grant TG AST090005 and the Texas Advanced Computing Center (TACC) at The University of Texas at Austin. JM acknowledges a Zwicky Prize Fellowship from ETH Zurich. GY acknowledges financial support by MICIU/FEDER under project grant PGC2018-094975-C21. SEIB acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 669253). ITI was supported by the Science and Technology Facilities Council [grants ST/I000976/1, ST/F002858/1, ST/P000525/1, and ST/T000473/1]; and The Southeast Physics Network (SEPNet). KA was supported by NRF2016R1D1A1B04935414 and NRF-2016R1A5A1013277. KA also appreciates APCTP for its hospitality during completion of this work. PO acknowledges support from the French ANR funded project ORAGE (ANR-14-CE33-0016). ND and DA acknowledge funding from the French ANR for project ANR-12-JS05- 0001 (EMMA). The CoDa II simulation was performed at Oak Ridge National Laboratory/Oak Ridge Leadership Computing Facility on the Titan supercomputer (INCITE 2016 award AST031). Processing was performed on the Eos and Rhea clusters. Resolution study simulations were performed on Piz Daint at the Swiss National Supercomputing Center (PRACE Tier 0 award, project id pr37). The authors would like to acknowledge the High Performance Computing center of the University of Strasbourg for supporting this work by providing scientific support and access to computing resources. Part of the computing resources were funded by the Equipex EquipMeso project (Programme Investissements d’Avenir) and the CPER Alsacalcul/Big Data.","quality_controlled":"1","volume":508,"extern":"1","page":"3697-3709","date_published":"2021-12-01T00:00:00Z","publisher":"Oxford University Press","abstract":[{"text":"The decline in abundance of Lyman-α (Lyα) emitting galaxies at z ≳ 6 is a powerful and commonly used probe to constrain the progress of cosmic reionization. We use the CODAII simulation, which is a radiation hydrodynamic simulation featuring a box of ∼94 comoving Mpc side length, to compute the Lyα transmission properties of the intergalactic medium (IGM) at z ∼ 5.8 to 7. Our results mainly confirm previous studies, i.e. we find a declining Lyα transmission with redshift and a large sightline-to-sightline variation. However, motivated by the recent discovery of blue Lyα peaks at high redshift, we also analyse the IGM transmission on the blue side, which shows a rapid decline at z ≳ 6 of the blue transmission. This low transmission can be attributed not only to the presence of neutral regions but also to the residual neutral hydrogen within ionized regions, for which a density even as low as nHI∼10−9cm−3 (sometimes combined with kinematic effects) leads to a significantly reduced visibility. Still, we find that ∼1 per cent of sightlines towards M1600AB ∼ −21 galaxies at z ∼ 7 are transparent enough to allow a transmission of a blue Lyα peak. We discuss our results in the context of the interpretation of observations.","lang":"eng"}],"external_id":{"arxiv":["2004.14496"]},"publication_status":"published","publication":"Monthly Notices of the Royal Astronomical Society","language":[{"iso":"eng"}],"scopus_import":"1","intvolume":"       508","title":"Lyman-α transmission properties of the intergalactic medium in the CoDaII simulation","issue":"3","article_processing_charge":"No","oa":1,"date_updated":"2022-08-18T10:45:56Z","status":"public","type":"journal_article","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa_version":"Preprint","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2004.14496"}],"day":"01","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"month":"12","arxiv":1,"author":[{"last_name":"Gronke","full_name":"Gronke, Max","first_name":"Max"},{"last_name":"Ocvirk","full_name":"Ocvirk, Pierre","first_name":"Pierre"},{"first_name":"Charlotte","full_name":"Mason, Charlotte","last_name":"Mason"},{"full_name":"Matthee, Jorryt J","first_name":"Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Bosman","first_name":"Sarah E I","full_name":"Bosman, Sarah E I"},{"full_name":"Sorce, Jenny G","first_name":"Jenny G","last_name":"Sorce"},{"last_name":"Lewis","first_name":"Joseph","full_name":"Lewis, Joseph"},{"last_name":"Ahn","first_name":"Kyungjin","full_name":"Ahn, Kyungjin"},{"last_name":"Aubert","first_name":"Dominique","full_name":"Aubert, Dominique"},{"first_name":"Taha","full_name":"Dawoodbhoy, Taha","last_name":"Dawoodbhoy"},{"last_name":"Iliev","first_name":"Ilian T","full_name":"Iliev, Ilian T"},{"first_name":"Paul R","full_name":"Shapiro, Paul R","last_name":"Shapiro"},{"full_name":"Yepes, Gustavo","first_name":"Gustavo","last_name":"Yepes"}]},{"article_type":"original","_id":"11523","doi":"10.1093/mnras/stab1304","citation":{"ieee":"J. J. Matthee <i>et al.</i>, “The X-SHOOTER Lyman α survey at z = 2 (XLS-z2) I: What makes a galaxy a Lyman α emitter?,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 505, no. 1. Oxford University Press, pp. 1382–1412, 2021.","ama":"Matthee JJ, Sobral D, Hayes M, et al. The X-SHOOTER Lyman α survey at z = 2 (XLS-z2) I: What makes a galaxy a Lyman α emitter? <i>Monthly Notices of the Royal Astronomical Society</i>. 2021;505(1):1382-1412. doi:<a href=\"https://doi.org/10.1093/mnras/stab1304\">10.1093/mnras/stab1304</a>","short":"J.J. Matthee, D. Sobral, M. Hayes, G. Pezzulli, M. Gronke, D. Schaerer, R.P. Naidu, H. Röttgering, J. Calhau, A. Paulino-Afonso, S. Santos, R. Amorín, Monthly Notices of the Royal Astronomical Society 505 (2021) 1382–1412.","mla":"Matthee, Jorryt J., et al. “The X-SHOOTER Lyman α Survey at z = 2 (XLS-Z2) I: What Makes a Galaxy a Lyman α Emitter?” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 505, no. 1, Oxford University Press, 2021, pp. 1382–412, doi:<a href=\"https://doi.org/10.1093/mnras/stab1304\">10.1093/mnras/stab1304</a>.","ista":"Matthee JJ, Sobral D, Hayes M, Pezzulli G, Gronke M, Schaerer D, Naidu RP, Röttgering H, Calhau J, Paulino-Afonso A, Santos S, Amorín R. 2021. The X-SHOOTER Lyman α survey at z = 2 (XLS-z2) I: What makes a galaxy a Lyman α emitter? Monthly Notices of the Royal Astronomical Society. 505(1), 1382–1412.","chicago":"Matthee, Jorryt J, David Sobral, Matthew Hayes, Gabriele Pezzulli, Max Gronke, Daniel Schaerer, Rohan P Naidu, et al. “The X-SHOOTER Lyman α Survey at z = 2 (XLS-Z2) I: What Makes a Galaxy a Lyman α Emitter?” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2021. <a href=\"https://doi.org/10.1093/mnras/stab1304\">https://doi.org/10.1093/mnras/stab1304</a>.","apa":"Matthee, J. J., Sobral, D., Hayes, M., Pezzulli, G., Gronke, M., Schaerer, D., … Amorín, R. (2021). The X-SHOOTER Lyman α survey at z = 2 (XLS-z2) I: What makes a galaxy a Lyman α emitter? <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stab1304\">https://doi.org/10.1093/mnras/stab1304</a>"},"date_created":"2022-07-07T09:33:39Z","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: formation","galaxies: ISM","galaxies: starburst","dark ages","reionization","first stars"],"acknowledgement":"We thank the referee for constructive comments and suggestions. We thank Dawn Erb, Ruari Mackenzie, Ivan Oteo, Ryan Sanders, and Johannes Zabl for useful discussions and suggestions. It is a pleasure to thank the ESO User Support, in particular Giacomo Beccari, Carlo Manara, John Pritchard, Marina Rejkuba, and Lowell Tacconi-Garman for assistance in the preparation and execution of the observations. Based on observations obtained with the VLT, programs 084.A-0303, 088.A-0672, 091.A-0413, 091.A-0546, 092.A0774, 097.A-0153, 098.A-0819, 099.A-0758, 099.A-0254, 101.B0779, and 102.A-0652. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by CALET and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. Based on observations made with the NASA/ESA HST through programs 9133, 9367, 11694, and 12471, and obtained from the Hubble Legacy Archive, which is a collaboration between the Space Telescope Science Institute (STScI/NASA), the Space Telescope European Coordinating Facility (ST-ECF/ESA), and the Canadian Astronomy Data Centre (CADC/NRC/CSA). This work is based on observations taken by the CANDELS Multi-Cycle Treasury Program with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. MG was supported by NASA through the NASA Hubble Fellowship grant HST-HF2-51409 and acknowledges support from HST grants\r\nHST-GO-15643.017-A, HST-AR-15039.003-A, and XSEDE grant TG-AST180036. GP acknowledges support from the Netherlands Research School for Astronomy (NOVA). RA acknowledges the support of ANID FONDECYT Regular Grant 1202007. We gratefully acknowledge the PYTHON programming language, its NUMPY, MATPLOTLIB, SCIPY, LMFIT (Jones et al. 2001; Hunter 2007; van der Walt, Colbert & Varoquaux 2011), PANDAS (McKinney 2010), and ASTROPY (Astropy Collaboration 2013) packages, and the TOPCAT analysis tool (Taylor 2013). Dedicated to the memory of A. C. J.Matthee (1953–2020).","year":"2021","page":"1382-1412","extern":"1","volume":505,"quality_controlled":"1","publisher":"Oxford University Press","date_published":"2021-07-01T00:00:00Z","publication_status":"published","external_id":{"arxiv":["2102.07779"]},"abstract":[{"lang":"eng","text":"We present the first results from the X-SHOOTER Lyman α survey at z = 2 (XLS-z2). XLS-z2 is a deep spectroscopic survey of 35 Lyman α emitters (LAEs) utilizing ≈90 h of exposure time with Very Large Telescope/X-SHOOTER and covers rest-frame Ly α to H α emission with R ≈ 4000. We present the sample selection, the observations, and the data reduction. Systemic redshifts are measured from rest-frame optical lines for 33/35 sources. In the stacked spectrum, our LAEs are characterized by an interstellar medium with little dust, a low metallicity, and a high ionization state. The ionizing sources are young hot stars that power strong emission lines in the optical and high-ionization lines in the ultraviolet (UV). The LAEs exhibit clumpy UV morphologies and have outflowing kinematics with blueshifted Si II absorption, a broad [O III] component, and a red-skewed Ly α line. Typically, 30 per cent of the Ly α photons escape, of which one quarter on the blue side of the systemic velocity. A fraction of Ly α photons escape directly at the systemic suggesting clear channels enabling an ≈10 per cent escape of ionizing photons, consistent with an inference based on Mg II. A combination of a low effective H I column density, a low dust content, and young starburst determines whether a star-forming galaxy is observed as an LAE. The first is possibly related to outflows and/or a fortunate viewing angle, while we find that the latter two in LAEs are typical for their stellar mass of 109 M⊙."}],"language":[{"iso":"eng"}],"publication":"Monthly Notices of the Royal Astronomical Society","title":"The X-SHOOTER Lyman α survey at z = 2 (XLS-z2) I: What makes a galaxy a Lyman α emitter?","oa":1,"date_updated":"2022-08-18T10:49:00Z","article_processing_charge":"No","issue":"1","scopus_import":"1","intvolume":"       505","type":"journal_article","status":"public","author":[{"orcid":"0000-0003-2871-127X","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","first_name":"Jorryt J"},{"last_name":"Sobral","full_name":"Sobral, David","first_name":"David"},{"first_name":"Matthew","full_name":"Hayes, Matthew","last_name":"Hayes"},{"first_name":"Gabriele","full_name":"Pezzulli, Gabriele","last_name":"Pezzulli"},{"first_name":"Max","full_name":"Gronke, Max","last_name":"Gronke"},{"full_name":"Schaerer, Daniel","first_name":"Daniel","last_name":"Schaerer"},{"first_name":"Rohan P","full_name":"Naidu, Rohan P","last_name":"Naidu"},{"full_name":"Röttgering, Huub","first_name":"Huub","last_name":"Röttgering"},{"full_name":"Calhau, João","first_name":"João","last_name":"Calhau"},{"full_name":"Paulino-Afonso, Ana","first_name":"Ana","last_name":"Paulino-Afonso"},{"last_name":"Santos","first_name":"Sérgio","full_name":"Santos, Sérgio"},{"full_name":"Amorín, Ricardo","first_name":"Ricardo","last_name":"Amorín"}],"arxiv":1,"day":"01","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2102.07779"}],"oa_version":"Preprint","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"month":"07"},{"acknowledgement":"This research made use of Astropy, a community developed core Python package for Astronomy (Astropy Collaboration et al. 2013). topcat, a graphical tool for manipulating tabular data, was also utilized in this analysis (Taylor 2005). SG would like to thank Nastasha Wijers for the discussion on the column density distribution in EAGLE. SC gratefully acknowledges support from Swiss National Science Foundation grants PP00P2 163824 and PP00P2 190092, and from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme grant agreement No 864361. GP acknowledges support from the Swiss National Science Foundation (SNF) and from the Netherlands Research School for Astronomy (NOVA).","year":"2021","citation":{"mla":"Santos, S., et al. “The Evolution of the UV Luminosity and Stellar Mass Functions of Lyman-α Emitters from z ∼ 2 to z ∼ 6.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 505, no. 1, Oxford University Press, 2021, pp. 1117–34, doi:<a href=\"https://doi.org/10.1093/mnras/stab1218\">10.1093/mnras/stab1218</a>.","ista":"Santos S, Sobral D, Butterworth J, Paulino-Afonso A, Ribeiro B, da Cunha E, Calhau J, Khostovan AA, Matthee JJ, Arrabal Haro P. 2021. The evolution of the UV luminosity and stellar mass functions of Lyman-α emitters from z ∼ 2 to z ∼ 6. Monthly Notices of the Royal Astronomical Society. 505(1), 1117–1134.","chicago":"Santos, S, D Sobral, J Butterworth, A Paulino-Afonso, B Ribeiro, E da Cunha, J Calhau, A A Khostovan, Jorryt J Matthee, and P Arrabal Haro. “The Evolution of the UV Luminosity and Stellar Mass Functions of Lyman-α Emitters from z ∼ 2 to z ∼ 6.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2021. <a href=\"https://doi.org/10.1093/mnras/stab1218\">https://doi.org/10.1093/mnras/stab1218</a>.","short":"S. Santos, D. Sobral, J. Butterworth, A. Paulino-Afonso, B. Ribeiro, E. da Cunha, J. Calhau, A.A. Khostovan, J.J. Matthee, P. Arrabal Haro, Monthly Notices of the Royal Astronomical Society 505 (2021) 1117–1134.","ama":"Santos S, Sobral D, Butterworth J, et al. The evolution of the UV luminosity and stellar mass functions of Lyman-α emitters from z ∼ 2 to z ∼ 6. <i>Monthly Notices of the Royal Astronomical Society</i>. 2021;505(1):1117-1134. doi:<a href=\"https://doi.org/10.1093/mnras/stab1218\">10.1093/mnras/stab1218</a>","ieee":"S. Santos <i>et al.</i>, “The evolution of the UV luminosity and stellar mass functions of Lyman-α emitters from z ∼ 2 to z ∼ 6,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 505, no. 1. Oxford University Press, pp. 1117–1134, 2021.","apa":"Santos, S., Sobral, D., Butterworth, J., Paulino-Afonso, A., Ribeiro, B., da Cunha, E., … Arrabal Haro, P. (2021). The evolution of the UV luminosity and stellar mass functions of Lyman-α emitters from z ∼ 2 to z ∼ 6. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stab1218\">https://doi.org/10.1093/mnras/stab1218</a>"},"date_created":"2022-07-07T10:02:59Z","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","galaxies: luminosity function","mass function"],"article_type":"original","_id":"11524","doi":"10.1093/mnras/stab1218","publication_status":"published","external_id":{"arxiv":["2105.00007"]},"abstract":[{"text":"We measure the evolution of the rest-frame UV luminosity function (LF) and the stellar mass function (SMF) of Lyman-α (Ly α) emitters (LAEs) from z ∼ 2 to z ∼ 6 by exploring ∼4000 LAEs from the SC4K sample. We find a correlation between Ly α luminosity (LLy α) and rest-frame UV (MUV), with best fit MUV=−1.6+0.2−0.3log10(LLyα/ergs−1)+47+12−11 and a shallower relation between LLy α and stellar mass (M⋆), with best fit log10(M⋆/M⊙)=0.9+0.1−0.1log10(LLyα/ergs−1)−28+4.0−3.8⁠. An increasing LLy α cut predominantly lowers the number density of faint MUV and low M⋆ LAEs. We estimate a proxy for the full UV LFs and SMFs of LAEs with simple assumptions of the faint end slope. For the UV LF, we find a brightening of the characteristic UV luminosity (M∗UV⁠) with increasing redshift and a decrease of the characteristic number density (Φ*). For the SMF, we measure a characteristic stellar mass (⁠M∗⋆/M⊙⁠) increase with increasing redshift, and a Φ* decline. However, if we apply a uniform luminosity cut of log10(LLyα/ergs−1)≥43.0⁠, we find much milder to no evolution in the UV and SMF of LAEs. The UV luminosity density (ρUV) of the full sample of LAEs shows moderate evolution and the stellar mass density (ρM) decreases, with both being always lower than the total ρUV and ρM of more typical galaxies but slowly approaching them with increasing redshift. Overall, our results indicate that both ρUV and ρM of LAEs slowly approach the measurements of continuum-selected galaxies at z > 6, which suggests a key role of LAEs in the epoch of reionization.","lang":"eng"}],"publisher":"Oxford University Press","date_published":"2021-07-01T00:00:00Z","extern":"1","page":"1117-1134","volume":505,"quality_controlled":"1","date_updated":"2022-08-18T10:51:47Z","oa":1,"article_processing_charge":"No","issue":"1","title":"The evolution of the UV luminosity and stellar mass functions of Lyman-α emitters from z ∼ 2 to z ∼ 6","scopus_import":"1","intvolume":"       505","language":[{"iso":"eng"}],"publication":"Monthly Notices of the Royal Astronomical Society","author":[{"last_name":"Santos","full_name":"Santos, S","first_name":"S"},{"last_name":"Sobral","full_name":"Sobral, D","first_name":"D"},{"first_name":"J","full_name":"Butterworth, J","last_name":"Butterworth"},{"last_name":"Paulino-Afonso","full_name":"Paulino-Afonso, A","first_name":"A"},{"full_name":"Ribeiro, B","first_name":"B","last_name":"Ribeiro"},{"last_name":"da Cunha","full_name":"da Cunha, E","first_name":"E"},{"first_name":"J","full_name":"Calhau, J","last_name":"Calhau"},{"full_name":"Khostovan, A A","first_name":"A A","last_name":"Khostovan"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X","first_name":"Jorryt J","full_name":"Matthee, Jorryt J"},{"full_name":"Arrabal Haro, P","first_name":"P","last_name":"Arrabal Haro"}],"arxiv":1,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"month":"07","oa_version":"Preprint","day":"01","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2105.00007"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","type":"journal_article","status":"public"},{"_id":"11525","article_type":"original","doi":"10.1093/mnras/stab796","date_created":"2022-07-07T10:07:11Z","citation":{"mla":"Gallego, Sofia G., et al. “Constraining the Cosmic UV Background at z &#62; 3 with MUSE Lyman-α Emission Observations.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 504, no. 1, Oxford University Press, 2021, pp. 16–32, doi:<a href=\"https://doi.org/10.1093/mnras/stab796\">10.1093/mnras/stab796</a>.","ista":"Gallego SG, Cantalupo S, Sarpas S, Duboeuf B, Lilly S, Pezzulli G, Marino RA, Matthee JJ, Wisotzki L, Schaye J, Richard J, Kusakabe H, Mauerhofer V. 2021. Constraining the cosmic UV background at z &#62; 3 with MUSE Lyman-α emission observations. Monthly Notices of the Royal Astronomical Society. 504(1), 16–32.","chicago":"Gallego, Sofia G, Sebastiano Cantalupo, Saeed Sarpas, Bastien Duboeuf, Simon Lilly, Gabriele Pezzulli, Raffaella Anna Marino, et al. “Constraining the Cosmic UV Background at z &#62; 3 with MUSE Lyman-α Emission Observations.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2021. <a href=\"https://doi.org/10.1093/mnras/stab796\">https://doi.org/10.1093/mnras/stab796</a>.","short":"S.G. Gallego, S. Cantalupo, S. Sarpas, B. Duboeuf, S. Lilly, G. Pezzulli, R.A. Marino, J.J. Matthee, L. Wisotzki, J. Schaye, J. Richard, H. Kusakabe, V. Mauerhofer, Monthly Notices of the Royal Astronomical Society 504 (2021) 16–32.","ama":"Gallego SG, Cantalupo S, Sarpas S, et al. Constraining the cosmic UV background at z &#62; 3 with MUSE Lyman-α emission observations. <i>Monthly Notices of the Royal Astronomical Society</i>. 2021;504(1):16-32. doi:<a href=\"https://doi.org/10.1093/mnras/stab796\">10.1093/mnras/stab796</a>","ieee":"S. G. Gallego <i>et al.</i>, “Constraining the cosmic UV background at z &#62; 3 with MUSE Lyman-α emission observations,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 504, no. 1. Oxford University Press, pp. 16–32, 2021.","apa":"Gallego, S. G., Cantalupo, S., Sarpas, S., Duboeuf, B., Lilly, S., Pezzulli, G., … Mauerhofer, V. (2021). Constraining the cosmic UV background at z &#62; 3 with MUSE Lyman-α emission observations. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stab796\">https://doi.org/10.1093/mnras/stab796</a>"},"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"acknowledgement":"This research made use of Astropy, a community developed core Python package for Astronomy (Astropy Collaboration et al. 2013). topcat, a graphical tool for manipulating tabular data, was also utilized in this analysis (Taylor 2005). SG would like to thank Nastasha Wijers for the discussion on the column density distribution in EAGLE. SC gratefully acknowledges support from Swiss National Science Foundation grants PP00P2 163824 and PP00P2 190092, and from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme grant agreement No 864361. GP acknowledges support from the Swiss National Science Foundation (SNF) and from the Netherlands Research School for Astronomy (NOVA).","year":"2021","page":"16-32","extern":"1","quality_controlled":"1","volume":504,"publisher":"Oxford University Press","date_published":"2021-06-01T00:00:00Z","publication_status":"published","external_id":{"arxiv":["2103.09250"]},"abstract":[{"lang":"eng","text":"The intensity of the Cosmic UV background (UVB), coming from all sources of ionizing photons such as star-forming galaxies and quasars, determines the thermal evolution and ionization state of the intergalactic medium (IGM) and is, therefore, a critical ingredient for models of cosmic structure formation. Most of the previous estimates are based on the comparison between observed and simulated Lyman-α forest. We present the results of an independent method to constrain the product of the UVB photoionization rate and the covering fraction of Lyman limit systems (LLSs) by searching for the fluorescent Lyman-α emission produced by self-shielded clouds. Because the expected surface brightness is well below current sensitivity limits for direct imaging, we developed a new method based on 3D stacking of the IGM around Lyman-α emitting galaxies (LAEs) between 2.9 < z < 6.6 using deep MUSE observations. Combining our results with covering fractions of LLSs obtained from mock cubes extracted from the EAGLE simulation, we obtain new and independent constraints on the UVB at z > 3 that are consistent with previous measurements, with a preference for relatively low UVB intensities at z = 3, and which suggest a non-monotonic decrease of ΓH I with increasing redshift between 3 < z < 5. This could suggest a possible tension between some UVB models and current observations which however require deeper and wider observations in Lyman-α emission and absorption to be confirmed. Assuming instead a value of UVB from current models, our results constrain the covering fraction of LLSs at 3 < z < 4.5 to be less than 25 per cent within 150 kpc from LAEs."}],"language":[{"iso":"eng"}],"publication":"Monthly Notices of the Royal Astronomical Society","title":"Constraining the cosmic UV background at z > 3 with MUSE Lyman-α emission observations","oa":1,"date_updated":"2022-08-18T10:54:19Z","issue":"1","article_processing_charge":"No","scopus_import":"1","intvolume":"       504","status":"public","type":"journal_article","author":[{"last_name":"Gallego","first_name":"Sofia G","full_name":"Gallego, Sofia G"},{"full_name":"Cantalupo, Sebastiano","first_name":"Sebastiano","last_name":"Cantalupo"},{"full_name":"Sarpas, Saeed","first_name":"Saeed","last_name":"Sarpas"},{"last_name":"Duboeuf","full_name":"Duboeuf, Bastien","first_name":"Bastien"},{"full_name":"Lilly, Simon","first_name":"Simon","last_name":"Lilly"},{"last_name":"Pezzulli","first_name":"Gabriele","full_name":"Pezzulli, Gabriele"},{"full_name":"Marino, Raffaella Anna","first_name":"Raffaella Anna","last_name":"Marino"},{"orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","full_name":"Matthee, Jorryt J","first_name":"Jorryt J"},{"full_name":"Wisotzki, Lutz","first_name":"Lutz","last_name":"Wisotzki"},{"full_name":"Schaye, Joop","first_name":"Joop","last_name":"Schaye"},{"full_name":"Richard, Johan","first_name":"Johan","last_name":"Richard"},{"first_name":"Haruka","full_name":"Kusakabe, Haruka","last_name":"Kusakabe"},{"first_name":"Valentin","full_name":"Mauerhofer, Valentin","last_name":"Mauerhofer"}],"arxiv":1,"day":"01","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2103.09250"}],"oa_version":"Preprint","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"month":"06"},{"title":"Revealing the impact of quasar luminosity on giant Lyα nebulae","oa":1,"date_updated":"2022-08-18T10:56:28Z","article_processing_charge":"No","issue":"1","scopus_import":"1","intvolume":"       502","language":[{"iso":"eng"}],"publication":"Monthly Notices of the Royal Astronomical Society","author":[{"last_name":"Mackenzie","first_name":"Ruari","full_name":"Mackenzie, Ruari"},{"last_name":"Pezzulli","full_name":"Pezzulli, Gabriele","first_name":"Gabriele"},{"full_name":"Cantalupo, Sebastiano","first_name":"Sebastiano","last_name":"Cantalupo"},{"first_name":"Raffaella A","full_name":"Marino, Raffaella A","last_name":"Marino"},{"last_name":"Lilly","first_name":"Simon","full_name":"Lilly, Simon"},{"last_name":"Muzahid","full_name":"Muzahid, Sowgat","first_name":"Sowgat"},{"orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","full_name":"Matthee, Jorryt J","first_name":"Jorryt J"},{"last_name":"Schaye","full_name":"Schaye, Joop","first_name":"Joop"},{"first_name":"Lutz","full_name":"Wisotzki, Lutz","last_name":"Wisotzki"}],"arxiv":1,"day":"01","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2010.12589"}],"oa_version":"Preprint","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"month":"03","status":"public","type":"journal_article","date_created":"2022-07-07T10:11:15Z","citation":{"apa":"Mackenzie, R., Pezzulli, G., Cantalupo, S., Marino, R. A., Lilly, S., Muzahid, S., … Wisotzki, L. (2021). Revealing the impact of quasar luminosity on giant Lyα nebulae. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staa3277\">https://doi.org/10.1093/mnras/staa3277</a>","chicago":"Mackenzie, Ruari, Gabriele Pezzulli, Sebastiano Cantalupo, Raffaella A Marino, Simon Lilly, Sowgat Muzahid, Jorryt J Matthee, Joop Schaye, and Lutz Wisotzki. “Revealing the Impact of Quasar Luminosity on Giant Lyα Nebulae.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2021. <a href=\"https://doi.org/10.1093/mnras/staa3277\">https://doi.org/10.1093/mnras/staa3277</a>.","ista":"Mackenzie R, Pezzulli G, Cantalupo S, Marino RA, Lilly S, Muzahid S, Matthee JJ, Schaye J, Wisotzki L. 2021. Revealing the impact of quasar luminosity on giant Lyα nebulae. Monthly Notices of the Royal Astronomical Society. 502(1), 494–509.","mla":"Mackenzie, Ruari, et al. “Revealing the Impact of Quasar Luminosity on Giant Lyα Nebulae.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 502, no. 1, Oxford University Press, 2021, pp. 494–509, doi:<a href=\"https://doi.org/10.1093/mnras/staa3277\">10.1093/mnras/staa3277</a>.","ieee":"R. Mackenzie <i>et al.</i>, “Revealing the impact of quasar luminosity on giant Lyα nebulae,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 502, no. 1. Oxford University Press, pp. 494–509, 2021.","ama":"Mackenzie R, Pezzulli G, Cantalupo S, et al. Revealing the impact of quasar luminosity on giant Lyα nebulae. <i>Monthly Notices of the Royal Astronomical Society</i>. 2021;502(1):494-509. doi:<a href=\"https://doi.org/10.1093/mnras/staa3277\">10.1093/mnras/staa3277</a>","short":"R. Mackenzie, G. Pezzulli, S. Cantalupo, R.A. Marino, S. Lilly, S. Muzahid, J.J. Matthee, J. Schaye, L. Wisotzki, Monthly Notices of the Royal Astronomical Society 502 (2021) 494–509."},"keyword":["Space and Planetary Science","Astronomy and Astrophysics","techniques: imaging spectroscopy","intergalactic medium","quasars: emission lines","quasars: general"],"acknowledgement":"The authors thank Daichi Kashino, for providing access to unpublished zCOSMOS Deep data, and Jakob S. den Brok for sharing code used in den Brok et al. (2020). GP and SC acknowledge the support of the Swiss National Science Foundation [grant PP00P2163824]. SM is supported by the Experienced Researchers Fellowship, Alexander von Humboldt-Stiftung, Germany. This work is based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under the MUSE GTO programme. The major analysis and production of figures in this work was conducted in Python, using standard libraries which include NumPy (Harris et al. 2020), SciPy (Virtanen et al. 2020), Matplotlib (Hunter 2007) and the interactive command shell IPython (Pérez & Granger 2007). This research also made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013), and Photutils, an Astropy package for detection and photometry of astronomica sources (Bradley et al. 2019). The python interface dustmaps (Green 2018) was used to query galactic extinction maps. topcat, a graphical tool for manipulating tabular data, was also utilized in this analysis (Taylor 2005). This research has made use of the \"Aladin sky atlas\" developed at CDS, Strasbourg Observatory, France (Bonnarel et al. 2000).","year":"2021","article_type":"original","_id":"11526","doi":"10.1093/mnras/staa3277","publication_status":"published","external_id":{"arxiv":["2010.12589"]},"abstract":[{"text":"We present the results from a MUSE survey of twelve z ≃ 3.15 quasars, which were selected to be much fainter (20 < iSDSS < 23) than in previous studies of giant Ly α nebulae around the brightest quasars (16.6 < iAB < 18.7). We detect H I Ly α nebulae around 100 per cent of our target quasars, with emission extending to scales of at least 60 physical kpc, and up to 190 pkpc. We explore correlations between properties of the nebulae and their host quasars, with the goal of connecting variations in the properties of the illuminating QSO to the response in nebular emission. We show that the surface brightness profiles of the nebulae are similar to those of nebulae around bright quasars, but with a lower normalization. Our targeted quasars are on average 3.7 mag (≃30 times) fainter in UV continuum than our bright reference sample, and yet the nebulae around them are only 4.3 times fainter in mean Ly α surface brightness, measured between 20 and 50 pkpc. We find significant correlations between the surface brightness of the nebula and the luminosity of the quasar in both UV continuum and Ly α. The latter can be interpreted as evidence for a substantial contribution from unresolved inner parts of the nebulae to the narrow components seen in the Ly α lines of some of our faint quasars, possibly from the inner circumgalactic medium or from the host galaxy’s interstellar medium.","lang":"eng"}],"extern":"1","page":"494-509","quality_controlled":"1","volume":502,"publisher":"Oxford University Press","date_published":"2021-03-01T00:00:00Z"},{"intvolume":"       493","scopus_import":"1","title":"Sensitivity of the lower edge of the pair-instability black hole mass gap to the treatment of time-dependent convection","date_updated":"2023-08-09T12:53:37Z","oa":1,"article_processing_charge":"No","issue":"3","publication":"Monthly Notices of the Royal Astronomical Society","language":[{"iso":"eng"}],"oa_version":"Published Version","main_file_link":[{"url":"https://doi.org/10.1093/mnras/staa549","open_access":"1"}],"day":"04","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"month":"04","author":[{"last_name":"Renzo","first_name":"M","full_name":"Renzo, M"},{"last_name":"Farmer","first_name":"R J","full_name":"Farmer, R J"},{"full_name":"Justham, S","first_name":"S","last_name":"Justham"},{"last_name":"de Mink","full_name":"de Mink, S E","first_name":"S E"},{"full_name":"Götberg, Ylva Louise Linsdotter","first_name":"Ylva Louise Linsdotter","orcid":"0000-0002-6960-6911","last_name":"Götberg","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d"},{"first_name":"P","full_name":"Marchant, P","last_name":"Marchant"}],"arxiv":1,"status":"public","type":"journal_article","date_created":"2023-08-03T10:13:20Z","citation":{"apa":"Renzo, M., Farmer, R. J., Justham, S., de Mink, S. E., Götberg, Y. L. L., &#38; Marchant, P. (2020). Sensitivity of the lower edge of the pair-instability black hole mass gap to the treatment of time-dependent convection. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staa549\">https://doi.org/10.1093/mnras/staa549</a>","ieee":"M. Renzo, R. J. Farmer, S. Justham, S. E. de Mink, Y. L. L. Götberg, and P. Marchant, “Sensitivity of the lower edge of the pair-instability black hole mass gap to the treatment of time-dependent convection,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 493, no. 3. Oxford University Press, pp. 4333–4341, 2020.","ama":"Renzo M, Farmer RJ, Justham S, de Mink SE, Götberg YLL, Marchant P. Sensitivity of the lower edge of the pair-instability black hole mass gap to the treatment of time-dependent convection. <i>Monthly Notices of the Royal Astronomical Society</i>. 2020;493(3):4333-4341. doi:<a href=\"https://doi.org/10.1093/mnras/staa549\">10.1093/mnras/staa549</a>","short":"M. Renzo, R.J. Farmer, S. Justham, S.E. de Mink, Y.L.L. Götberg, P. Marchant, Monthly Notices of the Royal Astronomical Society 493 (2020) 4333–4341.","ista":"Renzo M, Farmer RJ, Justham S, de Mink SE, Götberg YLL, Marchant P. 2020. Sensitivity of the lower edge of the pair-instability black hole mass gap to the treatment of time-dependent convection. Monthly Notices of the Royal Astronomical Society. 493(3), 4333–4341.","mla":"Renzo, M., et al. “Sensitivity of the Lower Edge of the Pair-Instability Black Hole Mass Gap to the Treatment of Time-Dependent Convection.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 493, no. 3, Oxford University Press, 2020, pp. 4333–41, doi:<a href=\"https://doi.org/10.1093/mnras/staa549\">10.1093/mnras/staa549</a>.","chicago":"Renzo, M, R J Farmer, S Justham, S E de Mink, Ylva Louise Linsdotter Götberg, and P Marchant. “Sensitivity of the Lower Edge of the Pair-Instability Black Hole Mass Gap to the Treatment of Time-Dependent Convection.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2020. <a href=\"https://doi.org/10.1093/mnras/staa549\">https://doi.org/10.1093/mnras/staa549</a>."},"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"year":"2020","doi":"10.1093/mnras/staa549","article_type":"original","_id":"13465","external_id":{"arxiv":["2002.08200"]},"abstract":[{"lang":"eng","text":"Gravitational-wave detections are now probing the black hole (BH) mass distribution, including the predicted pair-instability mass gap. These data require robust quantitative predictions, which are challenging to obtain. The most massive BH progenitors experience episodic mass ejections on time-scales shorter than the convective turnover time-scale. This invalidates the steady-state assumption on which the classic mixing length theory relies. We compare the final BH masses computed with two different versions of the stellar evolutionary code MESA\r\n⁠: (i) using the default implementation of Paxton et al. (2018) and (ii) solving an additional equation accounting for the time-scale for convective deceleration. In the second grid, where stronger convection develops during the pulses and carries part of the energy, we find weaker pulses. This leads to lower amounts of mass being ejected and thus higher final BH masses of up to ∼5M⊙\r\n⁠. The differences are much smaller for the progenitors that determine the maximum mass of BHs below the gap. This prediction is robust at MBH,max≃48M⊙\r\n⁠, at least within the idealized context of this study. This is an encouraging indication that current models are robust enough for comparison with the present-day gravitational-wave detections. However, the large differences between individual models emphasize the importance of improving the treatment of convection in stellar models, especially in the light of the data anticipated from the third generation of gravitational-wave detectors."}],"publication_status":"published","page":"4333-4341","extern":"1","quality_controlled":"1","volume":493,"publisher":"Oxford University Press","date_published":"2020-04-04T00:00:00Z"},{"publication_status":"published","external_id":{"arxiv":["1910.03593"]},"abstract":[{"text":"Ly α emission lines are typically found to be redshifted with respect to the systemic redshifts of galaxies, likely due to resonant scattering of Ly α photons. Here, we measure the average velocity offset for a sample of 96 z ≈ 3.3 Ly α emitters (LAEs) with a median Ly α flux (luminosity) of ≈10−17 erg cm−2 s−1 (⁠≈1042 erg s−1⁠) and a median star formation rate (SFR) of ≈1.3 M⊙ yr−1 (not corrected for possible dust extinction), detected by the Multi-Unit Spectroscopic Explorer as part of our MUSEQuBES circumgalactic medium (CGM) survey. By postulating that the stacked CGM absorption profiles of these LAEs, probed by eight background quasars, must be centred on the systemic redshift, we measure an average velocity offset, Voffset = 171\\pm 8 km s−1, between the Ly α emission peak and the systemic redshift. The observed Voffset is lower by factors of ≈1.4 and ≈2.6 compared to the velocity offsets measured for narrow-band-selected LAEs and Lyman break galaxies, respectively, which probe galaxies with higher masses and SFRs. Consistent with earlier studies based on direct measurements for individual objects, we find that the Voffset is correlated with the full width at half-maximum of the red peak of the Ly α line, and anticorrelated with the rest-frame equivalent width. Moreover, we find that Voffset is correlated with SFR with a sub-linear scaling relation, Voffset∝SFR0.16±0.03⁠. Adopting the mass scaling for main-sequence galaxies, such a relation suggests that Voffset scales with the circular velocity of the dark matter haloes hosting the LAEs.","lang":"eng"}],"publisher":"Oxford University Press","date_published":"2020-08-01T00:00:00Z","page":"1013-1022","extern":"1","quality_controlled":"1","volume":496,"acknowledgement":"We thank the anonymous referee for useful suggestions. This study is based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programme(s): 094.A-0131(B), 095.A 0200(A), 096.A0222(A), 097.A-0089(A), and 099.A-0159(A). SM acknowledges support from the Alexander von Humboldt Foundation, Germany. SM thanks Christian Herenz for useful discussion. SC gratefully acknowledges support from Swiss National Science Foundation grant PP00P2 163824. JB acknowledges support by FCT/MCTES through national funds by grant UID/FIS/04434/2019 and through Investigador FCT Contract No. IF/01654/2014/CP1215/CT0003. NB and JZ acknowledge support from ANR grant ANR-17-CE31- 0017 (3DGasFlows). AC and JR acknowledge support from the ERC starting grant 336736-CALENDS. MA acknowledges support from European Union’s H2020 Marie Skłodowska-Curie Actions grant 721463 to the SUNDIAL ITN, and from the Spanish Ministry of Economy and Competitiveness (MINECO) under grant number AYA2016-76219-P. MA also acknowledges support from the Fundacion BBVA under its 2017 programme of assistance to ´scientific research groups, for the project ‘Using machine-learning techniques to drag galaxies from the noise in deep imaging’. FL and AV acknowledge support from the ERC starting grant ERC757258-TRIPLE.","year":"2020","citation":{"apa":"Muzahid, S., Schaye, J., Marino, R. A., Cantalupo, S., Brinchmann, J., Contini, T., … Verhamme, A. (2020). MUSEQuBES: Calibrating the redshifts of Lyα emitters using stacked circumgalactic medium absorption profiles. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staa1347\">https://doi.org/10.1093/mnras/staa1347</a>","short":"S. Muzahid, J. Schaye, R.A. Marino, S. Cantalupo, J. Brinchmann, T. Contini, M. Wendt, L. Wisotzki, J. Zabl, N. Bouché, M. Akhlaghi, H.-W. Chen, A. Claeyssens, S. Johnson, F. Leclercq, M. Maseda, J.J. Matthee, J. Richard, T. Urrutia, A. Verhamme, Monthly Notices of the Royal Astronomical Society 496 (2020) 1013–1022.","ieee":"S. Muzahid <i>et al.</i>, “MUSEQuBES: Calibrating the redshifts of Lyα emitters using stacked circumgalactic medium absorption profiles,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 496, no. 2. Oxford University Press, pp. 1013–1022, 2020.","ama":"Muzahid S, Schaye J, Marino RA, et al. MUSEQuBES: Calibrating the redshifts of Lyα emitters using stacked circumgalactic medium absorption profiles. <i>Monthly Notices of the Royal Astronomical Society</i>. 2020;496(2):1013-1022. doi:<a href=\"https://doi.org/10.1093/mnras/staa1347\">10.1093/mnras/staa1347</a>","chicago":"Muzahid, Sowgat, Joop Schaye, Raffaella Anna Marino, Sebastiano Cantalupo, Jarle Brinchmann, Thierry Contini, Martin Wendt, et al. “MUSEQuBES: Calibrating the Redshifts of Lyα Emitters Using Stacked Circumgalactic Medium Absorption Profiles.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2020. <a href=\"https://doi.org/10.1093/mnras/staa1347\">https://doi.org/10.1093/mnras/staa1347</a>.","mla":"Muzahid, Sowgat, et al. “MUSEQuBES: Calibrating the Redshifts of Lyα Emitters Using Stacked Circumgalactic Medium Absorption Profiles.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 496, no. 2, Oxford University Press, 2020, pp. 1013–22, doi:<a href=\"https://doi.org/10.1093/mnras/staa1347\">10.1093/mnras/staa1347</a>.","ista":"Muzahid S, Schaye J, Marino RA, Cantalupo S, Brinchmann J, Contini T, Wendt M, Wisotzki L, Zabl J, Bouché N, Akhlaghi M, Chen H-W, Claeyssens A, Johnson S, Leclercq F, Maseda M, Matthee JJ, Richard J, Urrutia T, Verhamme A. 2020. MUSEQuBES: Calibrating the redshifts of Lyα emitters using stacked circumgalactic medium absorption profiles. Monthly Notices of the Royal Astronomical Society. 496(2), 1013–1022."},"date_created":"2022-07-07T10:20:11Z","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: haloes","galaxies: high-redshift","quasars: absorption lines"],"related_material":{"link":[{"url":"https://doi.org/10.1093/mnras/staa2668","relation":"erratum"}]},"_id":"11528","article_type":"original","doi":"10.1093/mnras/staa1347","author":[{"first_name":"Sowgat","full_name":"Muzahid, Sowgat","last_name":"Muzahid"},{"last_name":"Schaye","full_name":"Schaye, Joop","first_name":"Joop"},{"last_name":"Marino","full_name":"Marino, Raffaella Anna","first_name":"Raffaella Anna"},{"last_name":"Cantalupo","full_name":"Cantalupo, Sebastiano","first_name":"Sebastiano"},{"last_name":"Brinchmann","first_name":"Jarle","full_name":"Brinchmann, Jarle"},{"full_name":"Contini, Thierry","first_name":"Thierry","last_name":"Contini"},{"last_name":"Wendt","first_name":"Martin","full_name":"Wendt, Martin"},{"first_name":"Lutz","full_name":"Wisotzki, Lutz","last_name":"Wisotzki"},{"full_name":"Zabl, Johannes","first_name":"Johannes","last_name":"Zabl"},{"last_name":"Bouché","first_name":"Nicolas","full_name":"Bouché, Nicolas"},{"last_name":"Akhlaghi","full_name":"Akhlaghi, Mohammad","first_name":"Mohammad"},{"last_name":"Chen","first_name":"Hsiao-Wen","full_name":"Chen, Hsiao-Wen"},{"first_name":"Adélaîde","full_name":"Claeyssens, Adélaîde","last_name":"Claeyssens"},{"last_name":"Johnson","first_name":"Sean","full_name":"Johnson, Sean"},{"last_name":"Leclercq","first_name":"Floriane","full_name":"Leclercq, Floriane"},{"first_name":"Michael","full_name":"Maseda, Michael","last_name":"Maseda"},{"full_name":"Matthee, Jorryt J","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X"},{"full_name":"Richard, Johan","first_name":"Johan","last_name":"Richard"},{"full_name":"Urrutia, Tanya","first_name":"Tanya","last_name":"Urrutia"},{"last_name":"Verhamme","first_name":"Anne","full_name":"Verhamme, Anne"}],"arxiv":1,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"month":"08","oa_version":"Preprint","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1910.03593"}],"day":"01","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","type":"journal_article","date_updated":"2022-08-18T11:00:24Z","oa":1,"article_processing_charge":"No","issue":"2","title":"MUSEQuBES: Calibrating the redshifts of Lyα emitters using stacked circumgalactic medium absorption profiles","scopus_import":"1","intvolume":"       496","language":[{"iso":"eng"}],"publication":"Monthly Notices of the Royal Astronomical Society"},{"publication":"Monthly Notices of the Royal Astronomical Society","language":[{"iso":"eng"}],"intvolume":"       498","scopus_import":"1","title":"The nature of CR7 revealed with MUSE: A young starburst powering extended Ly α emission at z = 6.6","oa":1,"date_updated":"2022-08-18T11:04:05Z","article_processing_charge":"No","issue":"2","type":"journal_article","status":"public","oa_version":"Preprint","day":"01","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2008.01731"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"month":"10","author":[{"orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","full_name":"Matthee, Jorryt J","first_name":"Jorryt J"},{"full_name":"Pezzulli, Gabriele","first_name":"Gabriele","last_name":"Pezzulli"},{"first_name":"Ruari","full_name":"Mackenzie, Ruari","last_name":"Mackenzie"},{"last_name":"Cantalupo","full_name":"Cantalupo, Sebastiano","first_name":"Sebastiano"},{"last_name":"Kusakabe","first_name":"Haruka","full_name":"Kusakabe, Haruka"},{"last_name":"Leclercq","first_name":"Floriane","full_name":"Leclercq, Floriane"},{"full_name":"Sobral, David","first_name":"David","last_name":"Sobral"},{"last_name":"Richard","full_name":"Richard, Johan","first_name":"Johan"},{"last_name":"Wisotzki","first_name":"Lutz","full_name":"Wisotzki, Lutz"},{"last_name":"Lilly","full_name":"Lilly, Simon","first_name":"Simon"},{"last_name":"Boogaard","full_name":"Boogaard, Leindert","first_name":"Leindert"},{"last_name":"Marino","full_name":"Marino, Raffaella","first_name":"Raffaella"},{"full_name":"Maseda, Michael","first_name":"Michael","last_name":"Maseda"},{"first_name":"Themiya","full_name":"Nanayakkara, Themiya","last_name":"Nanayakkara"}],"arxiv":1,"doi":"10.1093/mnras/staa2550","article_type":"original","_id":"11529","date_created":"2022-07-07T10:36:01Z","citation":{"short":"J.J. Matthee, G. Pezzulli, R. Mackenzie, S. Cantalupo, H. Kusakabe, F. Leclercq, D. Sobral, J. Richard, L. Wisotzki, S. Lilly, L. Boogaard, R. Marino, M. Maseda, T. Nanayakkara, Monthly Notices of the Royal Astronomical Society 498 (2020) 3043–3059.","ieee":"J. J. Matthee <i>et al.</i>, “The nature of CR7 revealed with MUSE: A young starburst powering extended Ly α emission at z = 6.6,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 498, no. 2. Oxford University Press, pp. 3043–3059, 2020.","ama":"Matthee JJ, Pezzulli G, Mackenzie R, et al. The nature of CR7 revealed with MUSE: A young starburst powering extended Ly α emission at z = 6.6. <i>Monthly Notices of the Royal Astronomical Society</i>. 2020;498(2):3043-3059. doi:<a href=\"https://doi.org/10.1093/mnras/staa2550\">10.1093/mnras/staa2550</a>","chicago":"Matthee, Jorryt J, Gabriele Pezzulli, Ruari Mackenzie, Sebastiano Cantalupo, Haruka Kusakabe, Floriane Leclercq, David Sobral, et al. “The Nature of CR7 Revealed with MUSE: A Young Starburst Powering Extended Ly α Emission at z = 6.6.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2020. <a href=\"https://doi.org/10.1093/mnras/staa2550\">https://doi.org/10.1093/mnras/staa2550</a>.","ista":"Matthee JJ, Pezzulli G, Mackenzie R, Cantalupo S, Kusakabe H, Leclercq F, Sobral D, Richard J, Wisotzki L, Lilly S, Boogaard L, Marino R, Maseda M, Nanayakkara T. 2020. The nature of CR7 revealed with MUSE: A young starburst powering extended Ly α emission at z = 6.6. Monthly Notices of the Royal Astronomical Society. 498(2), 3043–3059.","mla":"Matthee, Jorryt J., et al. “The Nature of CR7 Revealed with MUSE: A Young Starburst Powering Extended Ly α Emission at z = 6.6.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 498, no. 2, Oxford University Press, 2020, pp. 3043–59, doi:<a href=\"https://doi.org/10.1093/mnras/staa2550\">10.1093/mnras/staa2550</a>.","apa":"Matthee, J. J., Pezzulli, G., Mackenzie, R., Cantalupo, S., Kusakabe, H., Leclercq, F., … Nanayakkara, T. (2020). The nature of CR7 revealed with MUSE: A young starburst powering extended Ly α emission at z = 6.6. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staa2550\">https://doi.org/10.1093/mnras/staa2550</a>"},"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","dark ages","reionization","first stars","cosmology: observations"],"year":"2020","page":"3043-3059","extern":"1","volume":498,"quality_controlled":"1","publisher":"Oxford University Press","date_published":"2020-10-01T00:00:00Z","external_id":{"arxiv":["2008.01731"]},"abstract":[{"lang":"eng","text":"CR7 is among the most luminous Ly α emitters (LAEs) known at z = 6.6 and consists of at least three UV components that are surrounded by Ly α emission. Previous studies have suggested that it may host an extreme ionizing source. Here, we present deep integral field spectroscopy of CR7 with VLT/Multi Unit Spectroscopic Explorer (MUSE). We measure extended emission with a similar halo scale length as typical LAEs at z ≈ 5. CR7’s Ly α halo is clearly elongated along the direction connecting the multiple components, likely tracing the underlying gas distribution. The Ly α emission originates almost exclusively from the brightest UV component, but we also identify a faint kinematically distinct Ly α emitting region nearby a fainter component. Combined with new near-infrared data, the MUSE data show that the rest-frame Ly α equivalent width (EW) is ≈100 Å. This is a factor 4 higher than the EW measured in low-redshift analogues with carefully matched Ly α profiles (and thus arguably H I column density), but this EW can plausibly be explained by star formation. Alternative scenarios requiring active galactic nucleus (AGN) powering are also disfavoured by the narrower and steeper Ly α spectrum and much smaller IR to UV ratio compared to obscured AGN in other Ly α blobs. CR7’s Ly α emission, while extremely luminous, resembles the emission in more common LAEs at lower redshifts very well and is likely powered by a young metal-poor starburst."}],"publication_status":"published"},{"intvolume":"       495","scopus_import":"1","title":"Probing the AGN unification model at redshift z ∼ 3 with MUSE observations of giant Lyα nebulae","oa":1,"date_updated":"2022-08-18T11:17:47Z","article_processing_charge":"No","issue":"2","publication":"Monthly Notices of the Royal Astronomical Society","language":[{"iso":"eng"}],"oa_version":"Preprint","day":"01","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2005.01732"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","month":"06","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"author":[{"last_name":"den Brok","first_name":"J S","full_name":"den Brok, J S"},{"last_name":"Cantalupo","first_name":"S","full_name":"Cantalupo, S"},{"last_name":"Mackenzie","full_name":"Mackenzie, R","first_name":"R"},{"last_name":"Marino","first_name":"R A","full_name":"Marino, R A"},{"last_name":"Pezzulli","full_name":"Pezzulli, G","first_name":"G"},{"orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","full_name":"Matthee, Jorryt J","first_name":"Jorryt J"},{"first_name":"S D","full_name":"Johnson, S D","last_name":"Johnson"},{"last_name":"Krumpe","full_name":"Krumpe, M","first_name":"M"},{"first_name":"T","full_name":"Urrutia, T","last_name":"Urrutia"},{"first_name":"W","full_name":"Kollatschny, W","last_name":"Kollatschny"}],"arxiv":1,"status":"public","type":"journal_article","citation":{"apa":"den Brok, J. S., Cantalupo, S., Mackenzie, R., Marino, R. A., Pezzulli, G., Matthee, J. J., … Kollatschny, W. (2020). Probing the AGN unification model at redshift z ∼ 3 with MUSE observations of giant Lyα nebulae. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staa1269\">https://doi.org/10.1093/mnras/staa1269</a>","ieee":"J. S. den Brok <i>et al.</i>, “Probing the AGN unification model at redshift z ∼ 3 with MUSE observations of giant Lyα nebulae,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 495, no. 2. Oxford University Press, pp. 1874–1887, 2020.","ama":"den Brok JS, Cantalupo S, Mackenzie R, et al. Probing the AGN unification model at redshift z ∼ 3 with MUSE observations of giant Lyα nebulae. <i>Monthly Notices of the Royal Astronomical Society</i>. 2020;495(2):1874-1887. doi:<a href=\"https://doi.org/10.1093/mnras/staa1269\">10.1093/mnras/staa1269</a>","short":"J.S. den Brok, S. Cantalupo, R. Mackenzie, R.A. Marino, G. Pezzulli, J.J. Matthee, S.D. Johnson, M. Krumpe, T. Urrutia, W. Kollatschny, Monthly Notices of the Royal Astronomical Society 495 (2020) 1874–1887.","ista":"den Brok JS, Cantalupo S, Mackenzie R, Marino RA, Pezzulli G, Matthee JJ, Johnson SD, Krumpe M, Urrutia T, Kollatschny W. 2020. Probing the AGN unification model at redshift z ∼ 3 with MUSE observations of giant Lyα nebulae. Monthly Notices of the Royal Astronomical Society. 495(2), 1874–1887.","mla":"den Brok, J. S., et al. “Probing the AGN Unification Model at Redshift z ∼ 3 with MUSE Observations of Giant Lyα Nebulae.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 495, no. 2, Oxford University Press, 2020, pp. 1874–87, doi:<a href=\"https://doi.org/10.1093/mnras/staa1269\">10.1093/mnras/staa1269</a>.","chicago":"den Brok, J S, S Cantalupo, R Mackenzie, R A Marino, G Pezzulli, Jorryt J Matthee, S D Johnson, M Krumpe, T Urrutia, and W Kollatschny. “Probing the AGN Unification Model at Redshift z ∼ 3 with MUSE Observations of Giant Lyα Nebulae.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2020. <a href=\"https://doi.org/10.1093/mnras/staa1269\">https://doi.org/10.1093/mnras/staa1269</a>."},"date_created":"2022-07-07T10:40:17Z","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: active","galaxies: high-redshift","intergalactic medium","quasars: emission lines","quasars: general"],"acknowledgement":"SC and GP gratefully acknowledge support from Swiss National Science Foundation grant PP00P2 163824. MK acknowledges support by DLR500R1904.","year":"2020","doi":"10.1093/mnras/staa1269","article_type":"original","_id":"11530","external_id":{"arxiv":["2005.01732"]},"abstract":[{"lang":"eng","text":"A prediction of the classic active galactic nucleus (AGN) unification model is the presence of ionization cones with different orientations depending on the AGN type. Confirmations of this model exist for present times, but it is less clear in the early Universe. Here, we use the morphology of giant Ly α nebulae around AGNs at redshift z ∼ 3 to probe AGN emission and therefore the validity of the AGN unification model at this redshift. We compare the spatial morphology of 19 nebulae previously found around type I AGNs with a new sample of four Ly α nebulae detected around type II AGNs. Using two independent techniques, we find that nebulae around type II AGNs are more asymmetric than around type I, at least at radial distances r > 30 physical kpc (pkpc) from the ionizing source. We conclude that the type I and type II AGNs in our sample show evidence of different surrounding ionizing geometries. This suggests that the classical AGN unification model is also valid for high-redshift sources. Finally, we discuss how the lack of asymmetry in the inner parts (r ≲ 30 pkpc) and the associated high values of the He II to Ly α ratios in these regions could indicate additional sources of (hard) ionizing radiation originating within or in proximity of the AGN host galaxies. This work demonstrates that the morphologies of giant Ly α nebulae can be used to understand and study the geometry of high-redshift AGNs on circumnuclear scales and it lays the foundation for future studies using much larger statistical samples."}],"publication_status":"published","page":"1874-1887","extern":"1","quality_controlled":"1","volume":495,"publisher":"Oxford University Press","date_published":"2020-06-01T00:00:00Z"},{"status":"public","type":"journal_article","arxiv":1,"author":[{"last_name":"Maseda","full_name":"Maseda, Michael V","first_name":"Michael V"},{"last_name":"Bacon","first_name":"Roland","full_name":"Bacon, Roland"},{"last_name":"Lam","full_name":"Lam, Daniel","first_name":"Daniel"},{"orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","full_name":"Matthee, Jorryt J","first_name":"Jorryt J"},{"last_name":"Brinchmann","full_name":"Brinchmann, Jarle","first_name":"Jarle"},{"last_name":"Schaye","full_name":"Schaye, Joop","first_name":"Joop"},{"last_name":"Labbe","first_name":"Ivo","full_name":"Labbe, Ivo"},{"first_name":"Kasper B","full_name":"Schmidt, Kasper B","last_name":"Schmidt"},{"last_name":"Boogaard","full_name":"Boogaard, Leindert","first_name":"Leindert"},{"last_name":"Bouwens","first_name":"Rychard","full_name":"Bouwens, Rychard"},{"last_name":"Cantalupo","full_name":"Cantalupo, Sebastiano","first_name":"Sebastiano"},{"full_name":"Franx, Marijn","first_name":"Marijn","last_name":"Franx"},{"full_name":"Hashimoto, Takuya","first_name":"Takuya","last_name":"Hashimoto"},{"first_name":"Hanae","full_name":"Inami, Hanae","last_name":"Inami"},{"last_name":"Kusakabe","first_name":"Haruka","full_name":"Kusakabe, Haruka"},{"full_name":"Mahler, Guillaume","first_name":"Guillaume","last_name":"Mahler"},{"first_name":"Themiya","full_name":"Nanayakkara, Themiya","last_name":"Nanayakkara"},{"last_name":"Richard","full_name":"Richard, Johan","first_name":"Johan"},{"first_name":"Lutz","full_name":"Wisotzki, Lutz","last_name":"Wisotzki"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","day":"01","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/staa622"}],"oa_version":"Published Version","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"month":"04","language":[{"iso":"eng"}],"publication":"Monthly Notices of the Royal Astronomical Society","title":"Elevated ionizing photon production efficiency in faint high-equivalent-width Lyman-α emitters","issue":"4","article_processing_charge":"No","oa":1,"date_updated":"2022-08-18T11:23:27Z","intvolume":"       493","scopus_import":"1","volume":493,"quality_controlled":"1","extern":"1","page":"5120-5130","date_published":"2020-04-01T00:00:00Z","publisher":"Oxford University Press","publication_status":"published","abstract":[{"text":"While low-luminosity galaxies dominate number counts at all redshifts, their contribution to cosmic reionization is poorly understood due to a lack of knowledge of their physical properties. We isolate a sample of 35 z ≈ 4–5 continuum-faint Lyman-α emitters from deep VLT/MUSE spectroscopy and directly measure their H α emission using stacked Spitzer/IRAC Ch. 1 photometry. Based on Hubble Space Telescope imaging, we determine that the average UV continuum magnitude is fainter than −16 (≈ 0.01 L⋆), implying a median Lyman-α equivalent width of 259 Å. By combining the H α measurement with the UV magnitude, we determine the ionizing photon production efficiency, ξion, a first for such faint galaxies. The measurement of log10 (ξion [Hz erg−1]) = 26.28 (⁠+0.28−0.40⁠) is in excess of literature measurements of both continuum- and emission line-selected samples, implying a more efficient production of ionizing photons in these lower luminosity, Lyman-α-selected systems. We conclude that this elevated efficiency can be explained by stellar populations with metallicities between 4 × 10−4 and 0.008, with light-weighted ages less than 3 Myr.","lang":"eng"}],"external_id":{"arxiv":["2002.11117"]},"_id":"11531","article_type":"original","doi":"10.1093/mnras/staa622","keyword":["Space and Planetary Science","Astronomy and Astrophysics","Galaxies: evolution","Galaxies: high-redshift","Galaxies: ISM"],"citation":{"apa":"Maseda, M. V., Bacon, R., Lam, D., Matthee, J. J., Brinchmann, J., Schaye, J., … Wisotzki, L. (2020). Elevated ionizing photon production efficiency in faint high-equivalent-width Lyman-α emitters. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staa622\">https://doi.org/10.1093/mnras/staa622</a>","short":"M.V. Maseda, R. Bacon, D. Lam, J.J. Matthee, J. Brinchmann, J. Schaye, I. Labbe, K.B. Schmidt, L. Boogaard, R. Bouwens, S. Cantalupo, M. Franx, T. Hashimoto, H. Inami, H. Kusakabe, G. Mahler, T. Nanayakkara, J. Richard, L. Wisotzki, Monthly Notices of the Royal Astronomical Society 493 (2020) 5120–5130.","ama":"Maseda MV, Bacon R, Lam D, et al. Elevated ionizing photon production efficiency in faint high-equivalent-width Lyman-α emitters. <i>Monthly Notices of the Royal Astronomical Society</i>. 2020;493(4):5120-5130. doi:<a href=\"https://doi.org/10.1093/mnras/staa622\">10.1093/mnras/staa622</a>","ieee":"M. V. Maseda <i>et al.</i>, “Elevated ionizing photon production efficiency in faint high-equivalent-width Lyman-α emitters,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 493, no. 4. Oxford University Press, pp. 5120–5130, 2020.","chicago":"Maseda, Michael V, Roland Bacon, Daniel Lam, Jorryt J Matthee, Jarle Brinchmann, Joop Schaye, Ivo Labbe, et al. “Elevated Ionizing Photon Production Efficiency in Faint High-Equivalent-Width Lyman-α Emitters.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2020. <a href=\"https://doi.org/10.1093/mnras/staa622\">https://doi.org/10.1093/mnras/staa622</a>.","mla":"Maseda, Michael V., et al. “Elevated Ionizing Photon Production Efficiency in Faint High-Equivalent-Width Lyman-α Emitters.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 493, no. 4, Oxford University Press, 2020, pp. 5120–30, doi:<a href=\"https://doi.org/10.1093/mnras/staa622\">10.1093/mnras/staa622</a>.","ista":"Maseda MV, Bacon R, Lam D, Matthee JJ, Brinchmann J, Schaye J, Labbe I, Schmidt KB, Boogaard L, Bouwens R, Cantalupo S, Franx M, Hashimoto T, Inami H, Kusakabe H, Mahler G, Nanayakkara T, Richard J, Wisotzki L. 2020. Elevated ionizing photon production efficiency in faint high-equivalent-width Lyman-α emitters. Monthly Notices of the Royal Astronomical Society. 493(4), 5120–5130."},"date_created":"2022-07-07T10:46:41Z","year":"2020","acknowledgement":"We would like to thank the anonymous referee for a thoughtful report and suggestions that have improved this manuscript. We are also grateful to everyone involved in the Spitzer Space Telescope mission and everyone at the Spitzer Science Center: we are truly fortunate to have been able to use data from this facility. J. B. acknowledges support by FCT/MCTES through national funds by this grant UID/FIS/04434/2019 and through the Investigador FCT contract no. IF/01654/2014/CP1215/CT0003. S. C. gratefully acknowledges support from Swiss National Science Foundation grant PP00P2 163824. We would also like to thank Mauro Stefanon for his assistance with de-blending the IRAC photometry, Pieter van Dokkum for a number of useful suggestions, and Daniel Schaerer for information regarding the stellar population models. This study is based on observations made with ESO telescopes at the La Silla Paranal Observatory under programs IDs 094.A-2089(B), 095.A0010(A), 096.A-0045(A), and 096.A-0045(B)."},{"intvolume":"       493","scopus_import":"1","oa":1,"date_updated":"2022-08-18T11:27:43Z","issue":"1","article_processing_charge":"No","title":"The evolution of rest-frame UV properties, Ly α EWs, and the SFR–stellar mass relation at z ∼ 2–6 for SC4K LAEs","publication":"Monthly Notices of the Royal Astronomical Society","language":[{"iso":"eng"}],"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"month":"03","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1910.02959"}],"day":"01","oa_version":"Preprint","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","author":[{"last_name":"Santos","full_name":"Santos, S","first_name":"S"},{"last_name":"Sobral","first_name":"D","full_name":"Sobral, D"},{"last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","first_name":"Jorryt J"},{"last_name":"Calhau","first_name":"J","full_name":"Calhau, J"},{"first_name":"E","full_name":"da Cunha, E","last_name":"da Cunha"},{"last_name":"Ribeiro","full_name":"Ribeiro, B","first_name":"B"},{"full_name":"Paulino-Afonso, A","first_name":"A","last_name":"Paulino-Afonso"},{"last_name":"Arrabal Haro","first_name":"P","full_name":"Arrabal Haro, P"},{"last_name":"Butterworth","full_name":"Butterworth, J","first_name":"J"}],"arxiv":1,"type":"journal_article","status":"public","acknowledgement":"We thank the anonymous referee for the valuable feedback that significantly improved the quality and clarity of this paper. SS and JC acknowledge studentships from Lancaster University. APA acknowledges support from Fundação para a Ciência e a Tecnologia through the project PTDC/FISAST/31546/2017. The authors would like to thank Ali Khostovan, Sara Perez Sanchez, Alex Bennett and Tom Rose for contributions and discussions in the early stages of this work. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by CALET and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. Finally, the authors acknowledge the unique value of the publicly available analysis software TOPCAT (Taylor 2005) and publicly available programming language Python, including the numpy, pyfits, matplotlib, scipy and astropy (Astropy Collaboration et al. 2013) packages. This work is based on the public SC4K sample of LAEs (Sobral et al. 2018a) and we release the full catalogue with all the photometry and properties derived in this paper, in electronic format, along with the relevant tables.","year":"2020","date_created":"2022-07-07T12:05:23Z","citation":{"short":"S. Santos, D. Sobral, J.J. Matthee, J. Calhau, E. da Cunha, B. Ribeiro, A. Paulino-Afonso, P. Arrabal Haro, J. Butterworth, Monthly Notices of the Royal Astronomical Society 493 (2020) 141–160.","ieee":"S. Santos <i>et al.</i>, “The evolution of rest-frame UV properties, Ly α EWs, and the SFR–stellar mass relation at z ∼ 2–6 for SC4K LAEs,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 493, no. 1. Oxford University Press, pp. 141–160, 2020.","ama":"Santos S, Sobral D, Matthee JJ, et al. The evolution of rest-frame UV properties, Ly α EWs, and the SFR–stellar mass relation at z ∼ 2–6 for SC4K LAEs. <i>Monthly Notices of the Royal Astronomical Society</i>. 2020;493(1):141-160. doi:<a href=\"https://doi.org/10.1093/mnras/staa093\">10.1093/mnras/staa093</a>","chicago":"Santos, S, D Sobral, Jorryt J Matthee, J Calhau, E da Cunha, B Ribeiro, A Paulino-Afonso, P Arrabal Haro, and J Butterworth. “The Evolution of Rest-Frame UV Properties, Ly α EWs, and the SFR–Stellar Mass Relation at z ∼ 2–6 for SC4K LAEs.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2020. <a href=\"https://doi.org/10.1093/mnras/staa093\">https://doi.org/10.1093/mnras/staa093</a>.","mla":"Santos, S., et al. “The Evolution of Rest-Frame UV Properties, Ly α EWs, and the SFR–Stellar Mass Relation at z ∼ 2–6 for SC4K LAEs.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 493, no. 1, Oxford University Press, 2020, pp. 141–60, doi:<a href=\"https://doi.org/10.1093/mnras/staa093\">10.1093/mnras/staa093</a>.","ista":"Santos S, Sobral D, Matthee JJ, Calhau J, da Cunha E, Ribeiro B, Paulino-Afonso A, Arrabal Haro P, Butterworth J. 2020. The evolution of rest-frame UV properties, Ly α EWs, and the SFR–stellar mass relation at z ∼ 2–6 for SC4K LAEs. Monthly Notices of the Royal Astronomical Society. 493(1), 141–160.","apa":"Santos, S., Sobral, D., Matthee, J. J., Calhau, J., da Cunha, E., Ribeiro, B., … Butterworth, J. (2020). The evolution of rest-frame UV properties, Ly α EWs, and the SFR–stellar mass relation at z ∼ 2–6 for SC4K LAEs. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staa093\">https://doi.org/10.1093/mnras/staa093</a>"},"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: formation","galaxies: high-redshift","galaxies: star formation"],"doi":"10.1093/mnras/staa093","_id":"11533","article_type":"original","external_id":{"arxiv":["1910.02959"]},"abstract":[{"text":"We explore deep rest-frame UV to FIR data in the COSMOS field to measure the individual spectral energy distributions (SED) of the ∼4000 SC4K (Sobral et al.) Lyman α (Ly α) emitters (LAEs) at z ∼ 2–6. We find typical stellar masses of 109.3 ± 0.6 M⊙ and star formation rates (SFR) of SFRSED=4.4+10.5−2.4 M⊙ yr−1 and SFRLyα=5.9+6.3−2.6 M⊙ yr−1, combined with very blue UV slopes of β=−2.1+0.5−0.4⁠, but with significant variations within the population. MUV and β are correlated in a similar way to UV-selected sources, but LAEs are consistently bluer. This suggests that LAEs are the youngest and/or most dust-poor subset of the UV-selected population. We also study the Ly α rest-frame equivalent width (EW0) and find 45 ‘extreme’ LAEs with EW0 > 240 Å (3σ), implying a low number density of (7 ± 1) × 10−7 Mpc−3. Overall, we measure little to no evolution of the Ly α EW0 and scale length parameter (w0), which are consistently high (EW0=140+280−70 Å, w0=129+11−11 Å) from z ∼ 6 to z ∼ 2 and below. However, w0 is anticorrelated with MUV and stellar mass. Our results imply that sources selected as LAEs have a high Ly α escape fraction (fesc,Ly α) irrespective of cosmic time, but fesc,Ly α is still higher for UV-fainter and lower mass LAEs. The least massive LAEs (<109.5 M⊙) are typically located above the star formation ‘main sequence’ (MS), but the offset from the MS decreases towards z ∼ 6 and towards 1010 M⊙. Our results imply a lack of evolution in the properties of LAEs across time and reveals the increasing overlap in properties of LAEs and UV-continuum selected galaxies as typical star-forming galaxies at high redshift effectively become LAEs.","lang":"eng"}],"publication_status":"published","publisher":"Oxford University Press","date_published":"2020-03-01T00:00:00Z","page":"141-160","extern":"1","quality_controlled":"1","volume":493},{"quality_controlled":"1","volume":492,"page":"1778-1790","extern":"1","date_published":"2020-02-01T00:00:00Z","publisher":"Oxford University Press","abstract":[{"text":"The observed properties of the Lyman-α (Ly α) emission line are a powerful probe of neutral gas in and around galaxies. We present spatially resolved Ly α spectroscopy with VLT/MUSE targeting VR7, a UV-luminous galaxy at z = 6.532 with moderate Ly α equivalent width (EW0 ≈ 38 Å). These data are combined with deep resolved [CII]158μm spectroscopy obtained with ALMA and UV imaging from HST and we also detect UV continuum with MUSE. Ly α emission is clearly detected with S/N ≈ 40 and FWHM of 374 km s−1. Ly α and [C II] are similarly extended beyond the UV, with effective radius reff = 2.1 ± 0.2 kpc for a single exponential model or reff,Lyα,halo=3.45+1.08−0.87 kpc when measured jointly with the UV continuum. The Ly α profile is broader and redshifted with respect to the [C II] line (by 213 km s−1), but there are spatial variations that are qualitatively similar in both lines and coincide with resolved UV components. This suggests that the emission originates from two components with plausibly different H I column densities. We place VR7 in the context of other galaxies at similar and lower redshift. The Ly α halo scale length is similar at different redshifts and velocity shifts with respect to the systemic are typically smaller. Overall, we find little indications of a more neutral vicinity at higher redshift. This means that the local (∼10 kpc) neutral gas conditions that determine the observed Ly α properties in VR7 resemble the conditions in post-reionization galaxies.","lang":"eng"}],"external_id":{"arxiv":["1909.06376"]},"publication_status":"published","doi":"10.1093/mnras/stz3554","_id":"11534","article_type":"original","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","dark ages","reionization","first stars","cosmology: observations"],"citation":{"ieee":"J. J. Matthee <i>et al.</i>, “Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 ,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 492, no. 2. Oxford University Press, pp. 1778–1790, 2020.","ama":"Matthee JJ, Sobral D, Gronke M, et al. Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 . <i>Monthly Notices of the Royal Astronomical Society</i>. 2020;492(2):1778-1790. doi:<a href=\"https://doi.org/10.1093/mnras/stz3554\">10.1093/mnras/stz3554</a>","short":"J.J. Matthee, D. Sobral, M. Gronke, G. Pezzulli, S. Cantalupo, H. Röttgering, B. Darvish, S. Santos, Monthly Notices of the Royal Astronomical Society 492 (2020) 1778–1790.","mla":"Matthee, Jorryt J., et al. “Resolved Lyman-α Properties of a Luminous Lyman-Break Galaxy in a Large Ionized Bubble at z = 6.53 .” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 492, no. 2, Oxford University Press, 2020, pp. 1778–90, doi:<a href=\"https://doi.org/10.1093/mnras/stz3554\">10.1093/mnras/stz3554</a>.","chicago":"Matthee, Jorryt J, David Sobral, Max Gronke, Gabriele Pezzulli, Sebastiano Cantalupo, Huub Röttgering, Behnam Darvish, and Sérgio Santos. “Resolved Lyman-α Properties of a Luminous Lyman-Break Galaxy in a Large Ionized Bubble at z = 6.53 .” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2020. <a href=\"https://doi.org/10.1093/mnras/stz3554\">https://doi.org/10.1093/mnras/stz3554</a>.","ista":"Matthee JJ, Sobral D, Gronke M, Pezzulli G, Cantalupo S, Röttgering H, Darvish B, Santos S. 2020. Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 . Monthly Notices of the Royal Astronomical Society. 492(2), 1778–1790.","apa":"Matthee, J. J., Sobral, D., Gronke, M., Pezzulli, G., Cantalupo, S., Röttgering, H., … Santos, S. (2020). Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 . <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stz3554\">https://doi.org/10.1093/mnras/stz3554</a>"},"date_created":"2022-07-07T12:21:36Z","year":"2020","acknowledgement":"We thank the referee for their suggestions and constructive comments that helped to improve the presentation of our results. Based on observations obtained with the Very Large Telescope, program 99.A-0462. Based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program #14699. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2017.1.01451.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. MG acknowledges support from NASA grant NNX17AK58G. GP and SC gratefully acknowledge support from Swiss National Science Foundation grant PP00P2 163824. BD acknowledges financial support from the National Science Foundation, grant number 1716907. We have benefited greatly from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, SCIPY (Jones et al. 2001; Hunter 2007; van der Walt, Colbert & Varoquaux 2011) and ASTROPY (Astropy Collaboration 2013) packages, the astronomical imaging tools SEXTRACTOR, SWARP, and SCAMP (Bertin & Arnouts 1996; Bertin 2006, 2010) and the TOPCAT analysis tool (Taylor 2013).","status":"public","type":"journal_article","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"url":"https://arxiv.org/abs/1909.06376","open_access":"1"}],"day":"01","oa_version":"Preprint","month":"02","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"arxiv":1,"author":[{"first_name":"Jorryt J","full_name":"Matthee, Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X"},{"last_name":"Sobral","first_name":"David","full_name":"Sobral, David"},{"last_name":"Gronke","full_name":"Gronke, Max","first_name":"Max"},{"last_name":"Pezzulli","full_name":"Pezzulli, Gabriele","first_name":"Gabriele"},{"last_name":"Cantalupo","first_name":"Sebastiano","full_name":"Cantalupo, Sebastiano"},{"full_name":"Röttgering, Huub","first_name":"Huub","last_name":"Röttgering"},{"last_name":"Darvish","full_name":"Darvish, Behnam","first_name":"Behnam"},{"last_name":"Santos","full_name":"Santos, Sérgio","first_name":"Sérgio"}],"publication":"Monthly Notices of the Royal Astronomical Society","language":[{"iso":"eng"}],"intvolume":"       492","scopus_import":"1","title":"Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 ","issue":"2","article_processing_charge":"No","oa":1,"date_updated":"2022-08-18T11:29:53Z"},{"_id":"11539","article_type":"original","doi":"10.1093/mnras/staa476","acknowledgement":"JM acknowledges the support of a Huygens PhD fellowship from Leiden University. We thank Camila Correa for help analysing snipshot merger trees. We thank the anonymous referee for constructive comments. We also thank Jarle Brinchmann, Rob Crain, Antonios Katsianis, Paola Popesso, and David Sobral for discussions and suggestions. We also thank the participants of the Lorentz Center workshop ‘A Decade of the Star-Forming Main Sequence’ held on 2017 September 4–8, for discussions and ideas. We have benefited from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, and SCIPY (Hunter 2007) packages and the TOPCAT analysis tool (Taylor 2013).","year":"2020","date_created":"2022-07-08T07:34:10Z","citation":{"apa":"Calhau, J., Sobral, D., Santos, S., Matthee, J. J., Paulino-Afonso, A., Stroe, A., … Adams, B. (2020). The X-ray and radio activity of typical and luminous Ly α emitters from z ∼ 2 to z ∼ 6: Evidence for a diverse, evolving population. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staa476\">https://doi.org/10.1093/mnras/staa476</a>","chicago":"Calhau, João, David Sobral, Sérgio Santos, Jorryt J Matthee, Ana Paulino-Afonso, Andra Stroe, Brooke Simmons, Cassandra Barlow-Hall, and Benjamin Adams. “The X-Ray and Radio Activity of Typical and Luminous Ly α Emitters from z ∼ 2 to z ∼ 6: Evidence for a Diverse, Evolving Population.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2020. <a href=\"https://doi.org/10.1093/mnras/staa476\">https://doi.org/10.1093/mnras/staa476</a>.","ista":"Calhau J, Sobral D, Santos S, Matthee JJ, Paulino-Afonso A, Stroe A, Simmons B, Barlow-Hall C, Adams B. 2020. The X-ray and radio activity of typical and luminous Ly α emitters from z ∼ 2 to z ∼ 6: Evidence for a diverse, evolving population. Monthly Notices of the Royal Astronomical Society. 493(3), 3341–3362.","mla":"Calhau, João, et al. “The X-Ray and Radio Activity of Typical and Luminous Ly α Emitters from z ∼ 2 to z ∼ 6: Evidence for a Diverse, Evolving Population.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 493, no. 3, Oxford University Press, 2020, pp. 3341–62, doi:<a href=\"https://doi.org/10.1093/mnras/staa476\">10.1093/mnras/staa476</a>.","short":"J. Calhau, D. Sobral, S. Santos, J.J. Matthee, A. Paulino-Afonso, A. Stroe, B. Simmons, C. Barlow-Hall, B. Adams, Monthly Notices of the Royal Astronomical Society 493 (2020) 3341–3362.","ieee":"J. Calhau <i>et al.</i>, “The X-ray and radio activity of typical and luminous Ly α emitters from z ∼ 2 to z ∼ 6: Evidence for a diverse, evolving population,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 493, no. 3. Oxford University Press, pp. 3341–3362, 2020.","ama":"Calhau J, Sobral D, Santos S, et al. The X-ray and radio activity of typical and luminous Ly α emitters from z ∼ 2 to z ∼ 6: Evidence for a diverse, evolving population. <i>Monthly Notices of the Royal Astronomical Society</i>. 2020;493(3):3341-3362. doi:<a href=\"https://doi.org/10.1093/mnras/staa476\">10.1093/mnras/staa476</a>"},"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: active","galaxies: evolution","galaxies: high-redshift","quasars: supermassive black holes","galaxies: star formation","cosmology: observations","X-rays: galaxies"],"publisher":"Oxford University Press","date_published":"2020-04-01T00:00:00Z","page":"3341-3362","extern":"1","volume":493,"quality_controlled":"1","publication_status":"published","external_id":{"arxiv":["1909.11672"]},"abstract":[{"lang":"eng","text":"Despite recent progress in understanding Ly α emitters (LAEs), relatively little is known regarding their typical black hole activity across cosmic time. Here, we study the X-ray and radio properties of ∼4000 LAEs at 2.2 < z < 6 from the SC4K survey in the COSMOS field. We detect 254 (⁠6.8per cent±0.4per cent⁠) LAEs individually in the X-rays (S/N > 3) with an average luminosity of 1044.31±0.01ergs−1 and average black hole accretion rate (BHAR) of 0.72±0.01 M⊙ yr−1, consistent with moderate to high accreting active galactic neuclei (AGNs). We detect 120 sources in deep radio data (radio AGN fraction of 3.2per cent±0.3per cent⁠). The global AGN fraction (⁠8.6per cent±0.4per cent⁠) rises with Ly α luminosity and declines with increasing redshift. For X-ray-detected LAEs, Ly α luminosities correlate with the BHARs, suggesting that Ly α luminosity becomes a BHAR indicator. Most LAEs (⁠93.1per cent±0.6per cent⁠) at 2 < z < 6 have no detectable X-ray emission (BHARs < 0.017 M⊙ yr−1). The median star formation rate (SFR) of star-forming LAEs from Ly α and radio luminosities is 7.6+6.6−2.8 M⊙ yr−1. The black hole to galaxy growth ratio (BHAR/SFR) for LAEs is <0.0022, consistent with typical star-forming galaxies and the local BHAR/SFR relation. We conclude that LAEs at 2 < z < 6 include two different populations: an AGN population, where Ly α luminosity traces BHAR, and another with low SFRs which remain undetected in even the deepest X-ray stacks but is detected in the radio stacks."}],"language":[{"iso":"eng"}],"publication":"Monthly Notices of the Royal Astronomical Society","date_updated":"2022-08-18T11:25:31Z","oa":1,"issue":"3","article_processing_charge":"No","title":"The X-ray and radio activity of typical and luminous Ly α emitters from z ∼ 2 to z ∼ 6: Evidence for a diverse, evolving population","scopus_import":"1","intvolume":"       493","status":"public","type":"journal_article","author":[{"last_name":"Calhau","first_name":"João","full_name":"Calhau, João"},{"first_name":"David","full_name":"Sobral, David","last_name":"Sobral"},{"last_name":"Santos","first_name":"Sérgio","full_name":"Santos, Sérgio"},{"first_name":"Jorryt J","full_name":"Matthee, Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X"},{"last_name":"Paulino-Afonso","full_name":"Paulino-Afonso, Ana","first_name":"Ana"},{"last_name":"Stroe","first_name":"Andra","full_name":"Stroe, Andra"},{"full_name":"Simmons, Brooke","first_name":"Brooke","last_name":"Simmons"},{"last_name":"Barlow-Hall","first_name":"Cassandra","full_name":"Barlow-Hall, Cassandra"},{"last_name":"Adams","first_name":"Benjamin","full_name":"Adams, Benjamin"}],"arxiv":1,"month":"04","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1909.11672"}],"day":"01","oa_version":"Preprint","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87"},{"external_id":{"arxiv":["1811.00556"]},"abstract":[{"text":"We investigate the clustering and halo properties of ∼5000 Ly α-selected emission-line galaxies (LAEs) from the Slicing COSMOS 4K (SC4K) and from archival NB497 imaging of SA22 split in 15 discrete redshift slices between z ∼ 2.5 and 6. We measure clustering lengths of r0 ∼ 3–6 h−1 Mpc and typical halo masses of ∼1011 M⊙ for our narrowband-selected LAEs with typical LLy α ∼ 1042–43 erg s−1. The intermediate-band-selected LAEs are observed to have r0 ∼ 3.5–15 h−1 Mpc with typical halo masses of ∼1011–12 M⊙ and typical LLy α ∼ 1043–43.6 erg s−1. We find a strong, redshift-independent correlation between halo mass and Ly α luminosity normalized by the characteristic Ly α luminosity, L⋆(z). The faintest LAEs (L ∼ 0.1 L⋆(z)) typically identified by deep narrowband surveys are found in 1010 M⊙ haloes and the brightest LAEs (L ∼ 7 L⋆(z)) are found in ∼5 × 1012 M⊙ haloes. A dependency on the rest-frame 1500 Å UV luminosity, MUV, is also observed where the halo masses increase from 1011 to 1013 M⊙ for MUV ∼ −19 to −23.5 mag. Halo mass is also observed to increase from 109.8 to 1012 M⊙ for dust-corrected UV star formation rates from ∼0.6 to 10 M⊙ yr−1 and continues to increase up to 1013 M⊙ in halo mass, where the majority of those sources are active galactic nuclei. All the trends we observe are found to be redshift independent. Our results reveal that LAEs are the likely progenitors of a wide range of galaxies depending on their luminosity, from dwarf-like, to Milky Way-type, to bright cluster galaxies. LAEs therefore provide unique insight into the early formation and evolution of the galaxies we observe in the local Universe.","lang":"eng"}],"publication_status":"published","page":"555-573","extern":"1","quality_controlled":"1","volume":489,"publisher":"Oxford University Press","date_published":"2019-10-01T00:00:00Z","date_created":"2022-07-07T13:01:03Z","citation":{"apa":"Khostovan, A. A., Sobral, D., Mobasher, B., Matthee, J. J., Cochrane, R. K., Chartab, N., … Calhau, J. (2019). The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stz2149\">https://doi.org/10.1093/mnras/stz2149</a>","ieee":"A. A. Khostovan <i>et al.</i>, “The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 489, no. 1. Oxford University Press, pp. 555–573, 2019.","ama":"Khostovan AA, Sobral D, Mobasher B, et al. The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities. <i>Monthly Notices of the Royal Astronomical Society</i>. 2019;489(1):555-573. doi:<a href=\"https://doi.org/10.1093/mnras/stz2149\">10.1093/mnras/stz2149</a>","short":"A.A. Khostovan, D. Sobral, B. Mobasher, J.J. Matthee, R.K. Cochrane, N. Chartab, M. Jafariyazani, A. Paulino-Afonso, S. Santos, J. Calhau, Monthly Notices of the Royal Astronomical Society 489 (2019) 555–573.","chicago":"Khostovan, A A, D Sobral, B Mobasher, Jorryt J Matthee, R K Cochrane, N Chartab, M Jafariyazani, A Paulino-Afonso, S Santos, and J Calhau. “The Clustering of Typical Ly α Emitters from z ∼ 2.5–6: Host Halo Masses Depend on Ly α and UV Luminosities.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2019. <a href=\"https://doi.org/10.1093/mnras/stz2149\">https://doi.org/10.1093/mnras/stz2149</a>.","mla":"Khostovan, A. A., et al. “The Clustering of Typical Ly α Emitters from z ∼ 2.5–6: Host Halo Masses Depend on Ly α and UV Luminosities.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 489, no. 1, Oxford University Press, 2019, pp. 555–73, doi:<a href=\"https://doi.org/10.1093/mnras/stz2149\">10.1093/mnras/stz2149</a>.","ista":"Khostovan AA, Sobral D, Mobasher B, Matthee JJ, Cochrane RK, Chartab N, Jafariyazani M, Paulino-Afonso A, Santos S, Calhau J. 2019. The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities. Monthly Notices of the Royal Astronomical Society. 489(1), 555–573."},"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"],"acknowledgement":"We thank the anonymous referee for their useful comments and suggestions that helped improve this study. AAK acknowledges that this work was supported by NASA Headquarters under the NASA Earth and Space Science Fellowship Program – Grant NNX16AO92H. JM acknowledges support from the ETH Zwicky fellowship. RKC acknowledges funding from STFC via a studentship. APA acknowledges support from the Fundac¸ao para a Ci ˜ encia e a Tecnologia FCT through the fellowship PD/BD/52706/2014 and the research grant UID/FIS/04434/2013. JC and SS both acknowledge their support from the Lancaster University PhD Fellowship. We have benefited greatly from the publicly available programming language PYTHON, including the NUMPY, SCIPY, MATPLOTLIB, SCIKIT-LEARN, and ASTROPY packages, as well as the TOPCAT analysis program. The SC4K samples used in this paper are all publicly available for use by the community (Sobral et al. 2018a). The catalogue is also available on the COSMOS IPAC website (https://irsa.ipac.caltech.edu/data/COSMOS/overview.html).","year":"2019","doi":"10.1093/mnras/stz2149","article_type":"original","_id":"11535","oa_version":"Preprint","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1811.00556"}],"day":"01","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","month":"10","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"author":[{"last_name":"Khostovan","first_name":"A A","full_name":"Khostovan, A A"},{"last_name":"Sobral","full_name":"Sobral, D","first_name":"D"},{"last_name":"Mobasher","first_name":"B","full_name":"Mobasher, B"},{"first_name":"Jorryt J","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X"},{"last_name":"Cochrane","full_name":"Cochrane, R K","first_name":"R K"},{"full_name":"Chartab, N","first_name":"N","last_name":"Chartab"},{"last_name":"Jafariyazani","first_name":"M","full_name":"Jafariyazani, M"},{"first_name":"A","full_name":"Paulino-Afonso, A","last_name":"Paulino-Afonso"},{"first_name":"S","full_name":"Santos, S","last_name":"Santos"},{"full_name":"Calhau, J","first_name":"J","last_name":"Calhau"}],"arxiv":1,"type":"journal_article","status":"public","intvolume":"       489","scopus_import":"1","title":"The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities","oa":1,"date_updated":"2022-08-19T06:38:42Z","issue":"1","article_processing_charge":"No","publication":"Monthly Notices of the Royal Astronomical Society","language":[{"iso":"eng"}]},{"quality_controlled":"1","volume":484,"extern":"1","page":"915-932","date_published":"2019-03-01T00:00:00Z","publisher":"Oxford University Press","abstract":[{"lang":"eng","text":"Observations have revealed that the star formation rate (SFR) and stellar mass (Mstar) of star-forming galaxies follow a tight relation known as the galaxy main sequence. However, what physical information is encoded in this relation is under debate. Here, we use the EAGLE cosmological hydrodynamical simulation to study the mass dependence, evolution, and origin of scatter in the SFR–Mstar relation. At z = 0, we find that the scatter decreases slightly with stellar mass from 0.35 dex at Mstar ≈ 109 M⊙ to 0.30 dex at Mstar ≳ 1010.5 M⊙. The scatter decreases from z = 0 to z = 5 by 0.05 dex at Mstar ≳ 1010 M⊙ and by 0.15 dex for lower masses. We show that the scatter at z = 0.1 originates from a combination of fluctuations on short time-scales (ranging from 0.2–2 Gyr) that are presumably associated with self-regulation from cooling, star formation, and outflows, but is dominated by long time-scale (∼10 Gyr) variations related to differences in halo formation times. Shorter time-scale fluctuations are relatively more important for lower mass galaxies. At high masses, differences in black hole formation efficiency cause additional scatter, but also diminish the scatter caused by different halo formation times. While individual galaxies cross the main sequence multiple times during their evolution, they fluctuate around tracks associated with their halo properties, i.e. galaxies above/below the main sequence at z = 0.1 tend to have been above/below the main sequence for ≫1 Gyr."}],"external_id":{"arxiv":["1805.05956"]},"publication_status":"published","doi":"10.1093/mnras/stz030","article_type":"original","_id":"11540","keyword":["Space and Planetary Science","Astronomy and Astrophysics : galaxies: evolution","galaxies: formation","galaxies: star formation","cosmology: theory"],"citation":{"apa":"Matthee, J. J., &#38; Schaye, J. (2019). The origin of scatter in the star formation rate–stellar mass relation. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stz030\">https://doi.org/10.1093/mnras/stz030</a>","mla":"Matthee, Jorryt J., and Joop Schaye. “The Origin of Scatter in the Star Formation Rate–Stellar Mass Relation.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 484, no. 1, Oxford University Press, 2019, pp. 915–32, doi:<a href=\"https://doi.org/10.1093/mnras/stz030\">10.1093/mnras/stz030</a>.","chicago":"Matthee, Jorryt J, and Joop Schaye. “The Origin of Scatter in the Star Formation Rate–Stellar Mass Relation.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2019. <a href=\"https://doi.org/10.1093/mnras/stz030\">https://doi.org/10.1093/mnras/stz030</a>.","ista":"Matthee JJ, Schaye J. 2019. The origin of scatter in the star formation rate–stellar mass relation. Monthly Notices of the Royal Astronomical Society. 484(1), 915–932.","ama":"Matthee JJ, Schaye J. The origin of scatter in the star formation rate–stellar mass relation. <i>Monthly Notices of the Royal Astronomical Society</i>. 2019;484(1):915-932. doi:<a href=\"https://doi.org/10.1093/mnras/stz030\">10.1093/mnras/stz030</a>","ieee":"J. J. Matthee and J. Schaye, “The origin of scatter in the star formation rate–stellar mass relation,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 484, no. 1. Oxford University Press, pp. 915–932, 2019.","short":"J.J. Matthee, J. Schaye, Monthly Notices of the Royal Astronomical Society 484 (2019) 915–932."},"date_created":"2022-07-08T07:48:31Z","year":"2019","acknowledgement":"JM acknowledges the support of a Huygens PhD fellowship from Leiden University. We thank Camila Correa for help analysing snipshot merger trees. We thank the anonymous referee for constructive comments. We also thank Jarle Brinchmann, Rob Crain, Antonios Katsianis, Paola Popesso, and David Sobral for discussions and suggestions. We also thank the participants of the Lorentz Center workshop ‘A Decade of the Star-Forming Main Sequence’ held on 2017 September 4–8, for discussions and ideas. We have benefited from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, and SCIPY (Hunter 2007) packages and the TOPCAT analysis tool (Taylor 2013).","type":"journal_article","status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"url":"https://arxiv.org/abs/1805.05956","open_access":"1"}],"day":"01","oa_version":"Preprint","month":"03","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"arxiv":1,"author":[{"full_name":"Matthee, Jorryt J","first_name":"Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X"},{"first_name":"Joop","full_name":"Schaye, Joop","last_name":"Schaye"}],"publication":"Monthly Notices of the Royal Astronomical Society","language":[{"iso":"eng"}],"intvolume":"       484","scopus_import":"1","title":"The origin of scatter in the star formation rate–stellar mass relation","article_processing_charge":"No","issue":"1","oa":1,"date_updated":"2022-08-19T06:42:43Z"}]