[{"publication":"The Astrophysical Journal","month":"09","article_number":"140","oa_version":"Preprint","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"date_published":"2019-09-11T00:00:00Z","type":"journal_article","oa":1,"publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","main_file_link":[{"url":"https://arxiv.org/abs/1903.09167","open_access":"1"}],"author":[{"first_name":"Leindert A.","last_name":"Boogaard","full_name":"Boogaard, Leindert A."},{"full_name":"Decarli, Roberto","first_name":"Roberto","last_name":"Decarli"},{"first_name":"Jorge","last_name":"González-López","full_name":"González-López, Jorge"},{"first_name":"Paul","last_name":"van der Werf","full_name":"van der Werf, Paul"},{"last_name":"Walter","first_name":"Fabian","full_name":"Walter, Fabian"},{"full_name":"Bouwens, Rychard","first_name":"Rychard","last_name":"Bouwens"},{"first_name":"Manuel","last_name":"Aravena","full_name":"Aravena, Manuel"},{"full_name":"Carilli, Chris","last_name":"Carilli","first_name":"Chris"},{"first_name":"Franz Erik","last_name":"Bauer","full_name":"Bauer, Franz Erik"},{"first_name":"Jarle","last_name":"Brinchmann","full_name":"Brinchmann, Jarle"},{"first_name":"Thierry","last_name":"Contini","full_name":"Contini, Thierry"},{"first_name":"Pierre","last_name":"Cox","full_name":"Cox, Pierre"},{"full_name":"da Cunha, Elisabete","last_name":"da Cunha","first_name":"Elisabete"},{"full_name":"Daddi, Emanuele","first_name":"Emanuele","last_name":"Daddi"},{"full_name":"Díaz-Santos, Tanio","first_name":"Tanio","last_name":"Díaz-Santos"},{"first_name":"Jacqueline","last_name":"Hodge","full_name":"Hodge, Jacqueline"},{"first_name":"Hanae","last_name":"Inami","full_name":"Inami, Hanae"},{"full_name":"Ivison, Rob","last_name":"Ivison","first_name":"Rob"},{"full_name":"Maseda, Michael","first_name":"Michael","last_name":"Maseda"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X"},{"full_name":"Oesch, Pascal","last_name":"Oesch","first_name":"Pascal"},{"last_name":"Popping","first_name":"Gergö","full_name":"Popping, Gergö"},{"full_name":"Riechers, Dominik","first_name":"Dominik","last_name":"Riechers"},{"first_name":"Joop","last_name":"Schaye","full_name":"Schaye, Joop"},{"first_name":"Sander","last_name":"Schouws","full_name":"Schouws, Sander"},{"full_name":"Smail, Ian","first_name":"Ian","last_name":"Smail"},{"first_name":"Axel","last_name":"Weiss","full_name":"Weiss, Axel"},{"full_name":"Wisotzki, Lutz","last_name":"Wisotzki","first_name":"Lutz"},{"full_name":"Bacon, Roland","first_name":"Roland","last_name":"Bacon"},{"last_name":"Cortes","first_name":"Paulo C.","full_name":"Cortes, Paulo C."},{"last_name":"Rix","first_name":"Hans-Walter","full_name":"Rix, Hans-Walter"},{"first_name":"Rachel S.","last_name":"Somerville","full_name":"Somerville, Rachel S."},{"full_name":"Swinbank, Mark","first_name":"Mark","last_name":"Swinbank"},{"first_name":"Jeff","last_name":"Wagg","full_name":"Wagg, Jeff"}],"issue":"2","_id":"11514","scopus_import":"1","title":"The ALMA spectroscopic survey in the HUDF: Nature and physical properties of gas-mass selected galaxies using MUSE spectroscopy","intvolume":" 882","publication_status":"published","article_processing_charge":"No","date_created":"2022-07-06T13:31:35Z","quality_controlled":"1","article_type":"original","publisher":"IOP Publishing","external_id":{"arxiv":["1903.09167"]},"date_updated":"2022-07-19T09:50:55Z","year":"2019","citation":{"ista":"Boogaard LA, Decarli R, González-López J, van der Werf P, Walter F, Bouwens R, Aravena M, Carilli C, Bauer FE, Brinchmann J, Contini T, Cox P, da Cunha E, Daddi E, Díaz-Santos T, Hodge J, Inami H, Ivison R, Maseda M, Matthee JJ, Oesch P, Popping G, Riechers D, Schaye J, Schouws S, Smail I, Weiss A, Wisotzki L, Bacon R, Cortes PC, Rix H-W, Somerville RS, Swinbank M, Wagg J. 2019. The ALMA spectroscopic survey in the HUDF: Nature and physical properties of gas-mass selected galaxies using MUSE spectroscopy. The Astrophysical Journal. 882(2), 140.","short":"L.A. Boogaard, R. Decarli, J. González-López, P. van der Werf, F. Walter, R. Bouwens, M. Aravena, C. Carilli, F.E. Bauer, J. Brinchmann, T. Contini, P. Cox, E. da Cunha, E. Daddi, T. Díaz-Santos, J. Hodge, H. Inami, R. Ivison, M. Maseda, J.J. Matthee, P. Oesch, G. Popping, D. Riechers, J. Schaye, S. Schouws, I. Smail, A. Weiss, L. Wisotzki, R. Bacon, P.C. Cortes, H.-W. Rix, R.S. Somerville, M. Swinbank, J. Wagg, The Astrophysical Journal 882 (2019).","mla":"Boogaard, Leindert A., et al. “The ALMA Spectroscopic Survey in the HUDF: Nature and Physical Properties of Gas-Mass Selected Galaxies Using MUSE Spectroscopy.” The Astrophysical Journal, vol. 882, no. 2, 140, IOP Publishing, 2019, doi:10.3847/1538-4357/ab3102.","ieee":"L. A. Boogaard et al., “The ALMA spectroscopic survey in the HUDF: Nature and physical properties of gas-mass selected galaxies using MUSE spectroscopy,” The Astrophysical Journal, vol. 882, no. 2. IOP Publishing, 2019.","chicago":"Boogaard, Leindert A., Roberto Decarli, Jorge González-López, Paul van der Werf, Fabian Walter, Rychard Bouwens, Manuel Aravena, et al. “The ALMA Spectroscopic Survey in the HUDF: Nature and Physical Properties of Gas-Mass Selected Galaxies Using MUSE Spectroscopy.” The Astrophysical Journal. IOP Publishing, 2019. https://doi.org/10.3847/1538-4357/ab3102.","apa":"Boogaard, L. A., Decarli, R., González-López, J., van der Werf, P., Walter, F., Bouwens, R., … Wagg, J. (2019). The ALMA spectroscopic survey in the HUDF: Nature and physical properties of gas-mass selected galaxies using MUSE spectroscopy. The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/ab3102","ama":"Boogaard LA, Decarli R, González-López J, et al. The ALMA spectroscopic survey in the HUDF: Nature and physical properties of gas-mass selected galaxies using MUSE spectroscopy. The Astrophysical Journal. 2019;882(2). doi:10.3847/1538-4357/ab3102"},"abstract":[{"lang":"eng","text":"We discuss the nature and physical properties of gas-mass selected galaxies in the ALMA spectroscopic survey (ASPECS) of the Hubble Ultra Deep Field (HUDF). We capitalize on the deep optical integral-field spectroscopy from the Multi Unit Spectroscopic Explorer (MUSE) HUDF Survey and multiwavelength data to uniquely associate all 16 line emitters, detected in the ALMA data without preselection, with rotational transitions of carbon monoxide (CO). We identify 10 as CO(2–1) at 1 < z < 2, 5 as CO(3–2) at 2 < z < 3, and 1 as CO(4–3) at z = 3.6. Using the MUSE data as a prior, we identify two additional CO(2–1) emitters, increasing the total sample size to 18. We infer metallicities consistent with (super-)solar for the CO-detected galaxies at z ≤ 1.5, motivating our choice of a Galactic conversion factor between CO luminosity and molecular gas mass for these galaxies. Using deep Chandra imaging of the HUDF, we determine an X-ray AGN fraction of 20% and 60% among the CO emitters at z ∼ 1.4 and z ∼ 2.6, respectively. Being a CO-flux-limited survey, ASPECS-LP detects molecular gas in galaxies on, above, and below the main sequence (MS) at z ∼ 1.4. For stellar masses ≥1010 (1010.5) ${M}_{\\odot }$, we detect about 40% (50%) of all galaxies in the HUDF at 1 < z < 2 (2 < z < 3). The combination of ALMA and MUSE integral-field spectroscopy thus enables an unprecedented view of MS galaxies during the peak of galaxy formation."}],"doi":"10.3847/1538-4357/ab3102","arxiv":1,"day":"11","extern":"1","volume":882,"acknowledgement":"We are grateful to the referee for providing a constructive report. L.A.B. wants to thank Madusha L.P. Gunawardhana for her help with platefit. Based on observations collected at the European Southern Observatory under ESO programme(s): 094.A-2089(B), 095.A-0010(A), 096.A-0045(A), and 096.A-0045(B). This paper makes use of the following ALMA data: ADS/JAO.ALMA#2016.1.00324.L. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), 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. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.\r\n\r\n\"Este trabajo contó con el apoyo de CONICYT+Programa de Astronomía+ Fondo CHINA-CONICYT\" J.G-L. acknowledges partial support from ALMA-CONICYT project 31160033. F.E.B. acknowledges support from CONICYT grant Basal AFB-170002 (FEB), and the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS (FEB). J.B. acknowledges support by Fundação para a Ciência e a Tecnologia (FCT) through national funds (UID/FIS/04434/2013) and Investigador FCT contract IF/01654/2014/CP1215/CT0003., and by FEDER through COMPETE2020 (POCI-01-0145-FEDER-007672). T.D-S. acknowledges support from ALMA-CONYCIT project 31130005 and FONDECYT project 1151239. J.H. acknowledges support of the VIDI research programme with project number 639.042.611, which is (partly) financed by the Netherlands Organization for Scientific Research (NWO). D.R. acknowledges support from the National Science Foundation under grant No. AST-1614213. I.R.S. acknowledges support from the ERC Advanced Grant DUSTYGAL (321334) and STFC (ST/P000541/1)\r\n\r\nWork on Gnuastro has been funded by the Japanese MEXT scholarship and its Grant-in-Aid for Scientific Research (21244012, 24253003), the ERC advanced grant 339659-MUSICOS, European Union's Horizon 2020 research and innovation programme under Marie Sklodowska-Curie grant agreement No. 721463 to the SUNDIAL ITN, and from the Spanish MINECO under grant No. AYA2016-76219-P."},{"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1903.08171"}],"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","type":"journal_article","date_published":"2019-08-21T00:00:00Z","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"oa":1,"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"language":[{"iso":"eng"}],"publication":"The Astrophysical Journal","oa_version":"Preprint","article_number":"124","month":"08","volume":881,"acknowledgement":"We thank the anonymous referee for constructive comments and suggestions. We thank Max Gronke for comments on an earlier version of this paper. L.V. acknowledges funding from the European Union’s Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement No. 746119. 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), 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. Based on observations obtained with the Very Large Telescope, programs 294.A-5018, 097.A-0943, and 99.A-0462. Based on observations made with the NASA/ESA Hubble Space Telescope, obtained (from the Data Archive) at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program No. 14699.","extern":"1","year":"2019","citation":{"apa":"Matthee, J. J., Sobral, D., Boogaard, L. A., Röttgering, H., Vallini, L., Ferrara, A., … Mobasher, B. (2019). Resolved UV and [C ii] structures of luminous galaxies within the epoch of reionization. The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/ab2f81","ama":"Matthee JJ, Sobral D, Boogaard LA, et al. Resolved UV and [C ii] structures of luminous galaxies within the epoch of reionization. The Astrophysical Journal. 2019;881(2). doi:10.3847/1538-4357/ab2f81","chicago":"Matthee, Jorryt J, D. Sobral, L. A. Boogaard, H. Röttgering, L. Vallini, A. Ferrara, A. Paulino-Afonso, F. Boone, D. Schaerer, and B. Mobasher. “Resolved UV and [C Ii] Structures of Luminous Galaxies within the Epoch of Reionization.” The Astrophysical Journal. IOP Publishing, 2019. https://doi.org/10.3847/1538-4357/ab2f81.","ieee":"J. J. Matthee et al., “Resolved UV and [C ii] structures of luminous galaxies within the epoch of reionization,” The Astrophysical Journal, vol. 881, no. 2. IOP Publishing, 2019.","short":"J.J. Matthee, D. Sobral, L.A. Boogaard, H. Röttgering, L. Vallini, A. Ferrara, A. Paulino-Afonso, F. Boone, D. Schaerer, B. Mobasher, The Astrophysical Journal 881 (2019).","mla":"Matthee, Jorryt J., et al. “Resolved UV and [C Ii] Structures of Luminous Galaxies within the Epoch of Reionization.” The Astrophysical Journal, vol. 881, no. 2, 124, IOP Publishing, 2019, doi:10.3847/1538-4357/ab2f81.","ista":"Matthee JJ, Sobral D, Boogaard LA, Röttgering H, Vallini L, Ferrara A, Paulino-Afonso A, Boone F, Schaerer D, Mobasher B. 2019. Resolved UV and [C ii] structures of luminous galaxies within the epoch of reionization. The Astrophysical Journal. 881(2), 124."},"date_updated":"2022-08-18T10:19:48Z","external_id":{"arxiv":["1903.08171"]},"day":"21","doi":"10.3847/1538-4357/ab2f81","arxiv":1,"abstract":[{"text":"We present new deep ALMA and Hubble Space Telescope (HST)/WFC3 observations of MASOSA and VR7, two luminous Lyα emitters (LAEs) at z = 6.5, for which the UV continuum levels differ by a factor of four. No IR dust continuum emission is detected in either, indicating little amounts of obscured star formation and/or high dust temperatures. MASOSA, with a UV luminosity M1500 = −20.9, compact size, and very high Lyα ${\\mathrm{EW}}_{0}\\approx 145\\,\\mathring{\\rm A} $, is undetected in [C ii] to a limit of L[C ii] < 2.2 × 107 L⊙, implying a metallicity Z ≲ 0.07 Z⊙. Intriguingly, our HST data indicate a red UV slope β = −1.1 ± 0.7, at odds with the low dust content. VR7, which is a bright (M1500 = −22.4) galaxy with moderate color (β = −1.4 ± 0.3) and Lyα EW0 = 34 Å, is clearly detected in [C ii] emission (S/N = 15). VR7's rest-frame UV morphology can be described by two components separated by ≈1.5 kpc and is globally more compact than the [C ii] emission. The global [C ii]/UV ratio indicates Z ≈ 0.2 Z⊙, but there are large variations in the UV/[C ii] ratio on kiloparsec scales. We also identify diffuse, possibly outflowing, [C ii]-emitting gas at ≈100 km s−1 with respect to the peak. VR7 appears to be assembling its components at a slightly more evolved stage than other luminous LAEs, with outflows already shaping its direct environment at z ∼ 7. Our results further indicate that the global [C ii]−UV relation steepens at SFR < 30 M⊙ yr−1, naturally explaining why the [C ii]/UV ratio is anticorrelated with Lyα EW in many, but not all, observed LAEs.","lang":"eng"}],"quality_controlled":"1","publisher":"IOP Publishing","article_type":"original","scopus_import":"1","_id":"11515","issue":"2","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","first_name":"Jorryt J","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X"},{"first_name":"D.","last_name":"Sobral","full_name":"Sobral, D."},{"last_name":"Boogaard","first_name":"L. A.","full_name":"Boogaard, L. A."},{"full_name":"Röttgering, H.","last_name":"Röttgering","first_name":"H."},{"last_name":"Vallini","first_name":"L.","full_name":"Vallini, L."},{"last_name":"Ferrara","first_name":"A.","full_name":"Ferrara, A."},{"last_name":"Paulino-Afonso","first_name":"A.","full_name":"Paulino-Afonso, A."},{"last_name":"Boone","first_name":"F.","full_name":"Boone, F."},{"last_name":"Schaerer","first_name":"D.","full_name":"Schaerer, D."},{"first_name":"B.","last_name":"Mobasher","full_name":"Mobasher, B."}],"date_created":"2022-07-06T13:38:15Z","article_processing_charge":"No","publication_status":"published","intvolume":" 881","title":"Resolved UV and [C ii] structures of luminous galaxies within the epoch of reionization"},{"article_type":"original","publisher":"IOP Publishing","quality_controlled":"1","title":"A giant Lyα nebula and a small-scale clumpy outflow in the system of the exotic quasar J0952+0114 unveiled by MUSE","intvolume":" 880","publication_status":"published","date_created":"2022-07-06T13:50:33Z","article_processing_charge":"No","author":[{"last_name":"Marino","first_name":"Raffaella Anna","full_name":"Marino, Raffaella Anna"},{"first_name":"Sebastiano","last_name":"Cantalupo","full_name":"Cantalupo, Sebastiano"},{"full_name":"Pezzulli, Gabriele","last_name":"Pezzulli","first_name":"Gabriele"},{"first_name":"Simon J.","last_name":"Lilly","full_name":"Lilly, Simon J."},{"full_name":"Gallego, Sofia","first_name":"Sofia","last_name":"Gallego"},{"first_name":"Ruari","last_name":"Mackenzie","full_name":"Mackenzie, Ruari"},{"first_name":"Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"first_name":"Jarle","last_name":"Brinchmann","full_name":"Brinchmann, Jarle"},{"full_name":"Bouché, Nicolas","first_name":"Nicolas","last_name":"Bouché"},{"full_name":"Feltre, Anna","first_name":"Anna","last_name":"Feltre"},{"full_name":"Muzahid, Sowgat","first_name":"Sowgat","last_name":"Muzahid"},{"last_name":"Schroetter","first_name":"Ilane","full_name":"Schroetter, Ilane"},{"full_name":"Johnson, Sean D.","last_name":"Johnson","first_name":"Sean D."},{"full_name":"Nanayakkara, Themiya","first_name":"Themiya","last_name":"Nanayakkara"}],"issue":"1","_id":"11516","scopus_import":"1","extern":"1","acknowledgement":"We thank Lutz Wisotzki for stimulating discussions. This work is based on observations taken at ESO/VLT in Paranal and we would like to thank the ESO staff for their assistance and support during the MUSE GTO campaigns. This work was supported by the Swiss National Science Foundation. This research made use of Astropy, a community-developed core PYTHON package for astronomy (Astropy Collaboration et al. 2013), NumPy and SciPy (Oliphant 2007), Matplotlib (Hunter 2007), IPython (Perez & Granger 2007), and of the NASA Astrophysics Data System Bibliographic Services. S.C. and G.P. gratefully acknowledge support from Swiss National Science Foundation grant PP00P2−163824. A.F. acknowledges support from the ERC via Advanced Grant under grants agreement no. 339659-MUSICOS. J.B. 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. S.D.J. is supported by a NASA Hubble Fellowship (HST-HF2-51375.001-A). T.N. acknowledges the Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO) top grant TOP1.16.057.","volume":880,"abstract":[{"text":"The well-known quasar SDSS J095253.83+011421.9 (J0952+0114) at z = 3.02 has one of the most peculiar spectra discovered so far, showing the presence of narrow Lyα and broad metal emission lines. Although recent studies have suggested that a proximate damped Lyα absorption (PDLA) system causes this peculiar spectrum, the origin of the gas associated with the PDLA is unknown. Here we report the results of observations with the Multi Unit Spectroscopic Explorer (MUSE) that reveal a new giant (≈100 physical kpc) Lyα nebula. The detailed analysis of the Lyα velocity, velocity dispersion, and surface brightness profiles suggests that the J0952+0114 Lyα nebula shares similar properties with other QSO nebulae previously detected with MUSE, implying that the PDLA in J0952+0144 is covering only a small fraction of the solid angle of the QSO emission. We also detected bright and spectrally narrow C iv λ1550 and He ii λ1640 extended emission around J0952+0114 with velocity centroids similar to the peak of the extended and central narrow Lyα emission. The presence of a peculiarly bright, unresolved, and relatively broad He ii λ1640 emission in the central region at exactly the same PDLA redshift hints at the possibility that the PDLA originates in a clumpy outflow with a bulk velocity of about 500 km s−1. The smaller velocity dispersion of the large-scale Lyα emission suggests that the high-speed outflow is confined to the central region. Lastly, the derived spatially resolved He ii/Lyα and C iv/Lyα maps show a positive gradient with the distance to the QSO, hinting at a non-homogeneous distribution of the ionization parameter.","lang":"eng"}],"doi":"10.3847/1538-4357/ab2881","arxiv":1,"day":"24","external_id":{"arxiv":["1906.06347"]},"date_updated":"2022-08-18T10:20:18Z","year":"2019","citation":{"apa":"Marino, R. A., Cantalupo, S., Pezzulli, G., Lilly, S. J., Gallego, S., Mackenzie, R., … Nanayakkara, T. (2019). A giant Lyα nebula and a small-scale clumpy outflow in the system of the exotic quasar J0952+0114 unveiled by MUSE. The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/ab2881","ama":"Marino RA, Cantalupo S, Pezzulli G, et al. A giant Lyα nebula and a small-scale clumpy outflow in the system of the exotic quasar J0952+0114 unveiled by MUSE. The Astrophysical Journal. 2019;880(1). doi:10.3847/1538-4357/ab2881","chicago":"Marino, Raffaella Anna, Sebastiano Cantalupo, Gabriele Pezzulli, Simon J. Lilly, Sofia Gallego, Ruari Mackenzie, Jorryt J Matthee, et al. “A Giant Lyα Nebula and a Small-Scale Clumpy Outflow in the System of the Exotic Quasar J0952+0114 Unveiled by MUSE.” The Astrophysical Journal. IOP Publishing, 2019. https://doi.org/10.3847/1538-4357/ab2881.","ieee":"R. A. Marino et al., “A giant Lyα nebula and a small-scale clumpy outflow in the system of the exotic quasar J0952+0114 unveiled by MUSE,” The Astrophysical Journal, vol. 880, no. 1. IOP Publishing, 2019.","mla":"Marino, Raffaella Anna, et al. “A Giant Lyα Nebula and a Small-Scale Clumpy Outflow in the System of the Exotic Quasar J0952+0114 Unveiled by MUSE.” The Astrophysical Journal, vol. 880, no. 1, 47, IOP Publishing, 2019, doi:10.3847/1538-4357/ab2881.","short":"R.A. Marino, S. Cantalupo, G. Pezzulli, S.J. Lilly, S. Gallego, R. Mackenzie, J.J. Matthee, J. Brinchmann, N. Bouché, A. Feltre, S. Muzahid, I. Schroetter, S.D. Johnson, T. Nanayakkara, The Astrophysical Journal 880 (2019).","ista":"Marino RA, Cantalupo S, Pezzulli G, Lilly SJ, Gallego S, Mackenzie R, Matthee JJ, Brinchmann J, Bouché N, Feltre A, Muzahid S, Schroetter I, Johnson SD, Nanayakkara T. 2019. A giant Lyα nebula and a small-scale clumpy outflow in the system of the exotic quasar J0952+0114 unveiled by MUSE. The Astrophysical Journal. 880(1), 47."},"language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"month":"07","article_number":"47","oa_version":"Preprint","publication":"The Astrophysical Journal","status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1906.06347"}],"oa":1,"publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"date_published":"2019-07-24T00:00:00Z","type":"journal_article"},{"quality_controlled":"1","publisher":"IOP Publishing","article_type":"original","scopus_import":"1","_id":"11517","issue":"2","author":[{"full_name":"Wang, Enci","first_name":"Enci","last_name":"Wang"},{"full_name":"Lilly, Simon J.","first_name":"Simon J.","last_name":"Lilly"},{"first_name":"Gabriele","last_name":"Pezzulli","full_name":"Pezzulli, Gabriele"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J"}],"article_processing_charge":"No","date_created":"2022-07-07T08:38:24Z","publication_status":"published","intvolume":" 877","title":"On the elevation and suppression of star formation within galaxies","acknowledgement":"We are grateful to the anonymous referee for their thoughtful and constructive review of the paper and their several suggestions (including the analysis of Section 3.4), which have improved the paper. This research has been supported by the Swiss National Science Foundation.\r\n\r\nFunding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS website is www.sdss.org.\r\n\r\nSDSS-IV is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration, including the Brazilian Participation Group, the Carnegie Institution for Science, Carnegie Mellon University, the Chilean Participation Group, the French Participation Group, Harvard-Smithsonian Center for Astrophysics, Instituto de Astrofísica de Canarias, the Johns Hopkins University, Kavli Institute for the Physics and Mathematics of the Universe (IPMU)/University of Tokyo, Lawrence Berkeley National Laboratory, Leibniz Institut für Astrophysik Potsdam (AIP), Max-Planck-Institut für Astronomie (MPIA Heidelberg), Max-Planck-Institut für Astrophysik (MPA Garching), Max-Planck-Institut für Extraterrestrische Physik (MPE), National Astronomical Observatory of China, New Mexico State University, New York University, University of Notre Dame, Observatário Nacional/MCTI, the Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, Universidad Nacional Autónoma de México, University of Arizona, University of Colorado Boulder, University of Oxford, University of Portsmouth, University of Utah, University of Virginia, University of Washington, University of Wisconsin, Vanderbilt University, and Yale University","volume":877,"extern":"1","year":"2019","citation":{"apa":"Wang, E., Lilly, S. J., Pezzulli, G., & Matthee, J. J. (2019). On the elevation and suppression of star formation within galaxies. The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/ab1c5b","ama":"Wang E, Lilly SJ, Pezzulli G, Matthee JJ. On the elevation and suppression of star formation within galaxies. The Astrophysical Journal. 2019;877(2). doi:10.3847/1538-4357/ab1c5b","ieee":"E. Wang, S. J. Lilly, G. Pezzulli, and J. J. Matthee, “On the elevation and suppression of star formation within galaxies,” The Astrophysical Journal, vol. 877, no. 2. IOP Publishing, 2019.","chicago":"Wang, Enci, Simon J. Lilly, Gabriele Pezzulli, and Jorryt J Matthee. “On the Elevation and Suppression of Star Formation within Galaxies.” The Astrophysical Journal. IOP Publishing, 2019. https://doi.org/10.3847/1538-4357/ab1c5b.","mla":"Wang, Enci, et al. “On the Elevation and Suppression of Star Formation within Galaxies.” The Astrophysical Journal, vol. 877, no. 2, 132, IOP Publishing, 2019, doi:10.3847/1538-4357/ab1c5b.","short":"E. Wang, S.J. Lilly, G. Pezzulli, J.J. Matthee, The Astrophysical Journal 877 (2019).","ista":"Wang E, Lilly SJ, Pezzulli G, Matthee JJ. 2019. On the elevation and suppression of star formation within galaxies. The Astrophysical Journal. 877(2), 132."},"date_updated":"2022-08-18T10:19:08Z","external_id":{"arxiv":["1901.10276"]},"day":"04","arxiv":1,"doi":"10.3847/1538-4357/ab1c5b","abstract":[{"text":"To understand star formation in galaxies, we investigate the star formation rate (SFR) surface density (ΣSFR) profiles for galaxies, based on a well-defined sample of 976 star-forming MaNGA galaxies. We find that the typical ΣSFR profiles within 1.5Re of normal SF galaxies can be well described by an exponential function for different stellar mass intervals, while the sSFR profile shows positive gradients, especially for more massive SF galaxies. This is due to the more pronounced central cores or bulges rather than the onset of a `quenching' process. While galaxies that lie significantly above (or below) the star formation main sequence (SFMS) show overall an elevation (or suppression) of ΣSFR at all radii, this central elevation (or suppression) is more pronounced in more massive galaxies. The degree of central enhancement and suppression is quite symmetric, suggesting that both the elevation and suppression of star formation are following the same physical processes. Furthermore, we find that the dispersion in ΣSFR within and across the population is found to be tightly correlated with the inferred gas depletion time, whether based on the stellar surface mass density or the orbital dynamical time. This suggests that we are seeing the response of a simple gas-regulator system to variations in the accretion rate. This is explored using a heuristic model that can quantitatively explain the dependence of σ(ΣSFR) on gas depletion timescale. Variations in accretion rate are progressively more damped out in regions of low star-formation efficiency leading to a reduced amplitude of variations in star-formation.","lang":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"language":[{"iso":"eng"}],"publication":"The Astrophysical Journal","oa_version":"Preprint","article_number":"132","month":"06","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1901.10276"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","type":"journal_article","date_published":"2019-06-04T00:00:00Z","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"oa":1},{"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: haloes","galaxies: high-redshift","galaxies: star formation","cosmology: observations","large-scale structure of Universe"],"language":[{"iso":"eng"}],"month":"10","oa_version":"Preprint","publication":"Monthly Notices of the Royal Astronomical Society","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","main_file_link":[{"url":"https://arxiv.org/abs/1811.00556","open_access":"1"}],"oa":1,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"type":"journal_article","date_published":"2019-10-01T00:00:00Z","article_type":"original","publisher":"Oxford University Press","quality_controlled":"1","page":"555-573","intvolume":" 489","title":"The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities","date_created":"2022-07-07T13:01:03Z","article_processing_charge":"No","publication_status":"published","issue":"1","author":[{"full_name":"Khostovan, A A","last_name":"Khostovan","first_name":"A A"},{"last_name":"Sobral","first_name":"D","full_name":"Sobral, D"},{"full_name":"Mobasher, B","last_name":"Mobasher","first_name":"B"},{"full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"full_name":"Cochrane, R K","first_name":"R K","last_name":"Cochrane"},{"first_name":"N","last_name":"Chartab","full_name":"Chartab, N"},{"full_name":"Jafariyazani, M","last_name":"Jafariyazani","first_name":"M"},{"full_name":"Paulino-Afonso, A","first_name":"A","last_name":"Paulino-Afonso"},{"last_name":"Santos","first_name":"S","full_name":"Santos, S"},{"first_name":"J","last_name":"Calhau","full_name":"Calhau, J"}],"scopus_import":"1","_id":"11535","extern":"1","volume":489,"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).","abstract":[{"lang":"eng","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."}],"day":"01","arxiv":1,"doi":"10.1093/mnras/stz2149","external_id":{"arxiv":["1811.00556"]},"year":"2019","citation":{"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.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2019. https://doi.org/10.1093/mnras/stz2149.","ieee":"A. A. Khostovan et al., “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, 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. Monthly Notices of the Royal Astronomical Society. 2019;489(1):555-573. doi:10.1093/mnras/stz2149","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. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stz2149","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.","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.” Monthly Notices of the Royal Astronomical Society, vol. 489, no. 1, Oxford University Press, 2019, pp. 555–73, doi:10.1093/mnras/stz2149.","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."},"date_updated":"2022-08-19T06:38:42Z"},{"oa_version":"Preprint","month":"03","publication":"Monthly Notices of the Royal Astronomical Society","keyword":["Space and Planetary Science","Astronomy and Astrophysics : galaxies: evolution","galaxies: formation","galaxies: star formation","cosmology: theory"],"language":[{"iso":"eng"}],"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"oa":1,"type":"journal_article","date_published":"2019-03-01T00:00:00Z","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1805.05956"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","article_processing_charge":"No","date_created":"2022-07-08T07:48:31Z","publication_status":"published","intvolume":" 484","title":"The origin of scatter in the star formation rate–stellar mass relation","scopus_import":"1","_id":"11540","issue":"1","author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","last_name":"Matthee"},{"full_name":"Schaye, Joop","first_name":"Joop","last_name":"Schaye"}],"publisher":"Oxford University Press","article_type":"original","quality_controlled":"1","page":"915-932","day":"01","doi":"10.1093/mnras/stz030","arxiv":1,"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."}],"year":"2019","citation":{"mla":"Matthee, Jorryt J., and Joop Schaye. “The Origin of Scatter in the Star Formation Rate–Stellar Mass Relation.” Monthly Notices of the Royal Astronomical Society, vol. 484, no. 1, Oxford University Press, 2019, pp. 915–32, doi:10.1093/mnras/stz030.","short":"J.J. Matthee, J. Schaye, Monthly Notices of the Royal Astronomical Society 484 (2019) 915–932.","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. Monthly Notices of the Royal Astronomical Society. 2019;484(1):915-932. doi:10.1093/mnras/stz030","apa":"Matthee, J. J., & Schaye, J. (2019). The origin of scatter in the star formation rate–stellar mass relation. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stz030","ieee":"J. J. Matthee and J. Schaye, “The origin of scatter in the star formation rate–stellar mass relation,” Monthly Notices of the Royal Astronomical Society, vol. 484, no. 1. Oxford University Press, pp. 915–932, 2019.","chicago":"Matthee, Jorryt J, and Joop Schaye. “The Origin of Scatter in the Star Formation Rate–Stellar Mass Relation.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2019. https://doi.org/10.1093/mnras/stz030."},"date_updated":"2022-08-19T06:42:43Z","external_id":{"arxiv":["1805.05956"]},"volume":484,"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).","extern":"1"},{"title":"On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components","intvolume":" 482","publication_status":"published","article_processing_charge":"No","date_created":"2022-07-08T10:40:05Z","author":[{"full_name":"Sobral, David","first_name":"David","last_name":"Sobral"},{"first_name":"Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"full_name":"Brammer, Gabriel","last_name":"Brammer","first_name":"Gabriel"},{"first_name":"Andrea","last_name":"Ferrara","full_name":"Ferrara, Andrea"},{"full_name":"Alegre, Lara","last_name":"Alegre","first_name":"Lara"},{"last_name":"Röttgering","first_name":"Huub","full_name":"Röttgering, Huub"},{"full_name":"Schaerer, Daniel","first_name":"Daniel","last_name":"Schaerer"},{"first_name":"Bahram","last_name":"Mobasher","full_name":"Mobasher, Bahram"},{"full_name":"Darvish, Behnam","last_name":"Darvish","first_name":"Behnam"}],"issue":"2","_id":"11541","scopus_import":"1","article_type":"original","publisher":"Oxford University Press","page":"2422-2441","quality_controlled":"1","abstract":[{"text":"We present new Hubble Space Telescope (HST)/WFC3 observations and re-analyse VLT data to unveil the continuum, variability, and rest-frame ultraviolet (UV) lines of the multiple UV clumps of the most luminous Lyα emitter at z = 6.6, CR7 (COSMOS Redshift 7). Our re-reduced, flux-calibrated X-SHOOTER spectra of CR7 reveal an He II emission line in observations obtained along the major axis of Lyα emission with the best seeing conditions. He II is spatially offset by ≈+0.8 arcsec from the peak of Lyα emission, and it is found towards clump B. Our WFC3 grism spectra detects the UV continuum of CR7’s clump A, yielding a power law with β=−2.5+0.6−0.7 and MUV=−21.87+0.25−0.20. No significant variability is found for any of the UV clumps on their own, but there is tentative (≈2.2 σ) brightening of CR7 in F110W as a whole from 2012 to 2017. HST grism data fail to robustly detect rest-frame UV lines in any of the clumps, implying fluxes ≲2×10−17 erg s−1 cm−2 (3σ). We perform CLOUDY modelling to constrain the metallicity and the ionizing nature of CR7. CR7 seems to be actively forming stars without any clear active galactic nucleus activity in clump A, consistent with a metallicity of ∼0.05–0.2 Z⊙. Component C or an interclump component between B and C may host a high ionization source. Our results highlight the need for spatially resolved information to study the formation and assembly of early galaxies.","lang":"eng"}],"arxiv":1,"doi":"10.1093/mnras/sty2779","day":"01","external_id":{"arxiv":["1710.08422"]},"date_updated":"2022-08-19T06:49:36Z","citation":{"ama":"Sobral D, Matthee JJ, Brammer G, et al. On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components. Monthly Notices of the Royal Astronomical Society. 2019;482(2):2422-2441. doi:10.1093/mnras/sty2779","apa":"Sobral, D., Matthee, J. J., Brammer, G., Ferrara, A., Alegre, L., Röttgering, H., … Darvish, B. (2019). On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/sty2779","ieee":"D. Sobral et al., “On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components,” Monthly Notices of the Royal Astronomical Society, vol. 482, no. 2. Oxford University Press, pp. 2422–2441, 2019.","chicago":"Sobral, David, Jorryt J Matthee, Gabriel Brammer, Andrea Ferrara, Lara Alegre, Huub Röttgering, Daniel Schaerer, Bahram Mobasher, and Behnam Darvish. “On the Nature and Physical Conditions of the Luminous Ly α Emitter CR7 and Its Rest-Frame UV Components.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2019. https://doi.org/10.1093/mnras/sty2779.","short":"D. Sobral, J.J. Matthee, G. Brammer, A. Ferrara, L. Alegre, H. Röttgering, D. Schaerer, B. Mobasher, B. Darvish, Monthly Notices of the Royal Astronomical Society 482 (2019) 2422–2441.","mla":"Sobral, David, et al. “On the Nature and Physical Conditions of the Luminous Ly α Emitter CR7 and Its Rest-Frame UV Components.” Monthly Notices of the Royal Astronomical Society, vol. 482, no. 2, Oxford University Press, 2019, pp. 2422–41, doi:10.1093/mnras/sty2779.","ista":"Sobral D, Matthee JJ, Brammer G, Ferrara A, Alegre L, Röttgering H, Schaerer D, Mobasher B, Darvish B. 2019. On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components. Monthly Notices of the Royal Astronomical Society. 482(2), 2422–2441."},"year":"2019","extern":"1","acknowledgement":"We thank the anonymous reviewer for the numerous detailed comments that led us to greatly improve the quality, extent, and statistical robustness of this work. DS acknowledges financial support from the Netherlands Organisation for Scientific research through a Veni fellowship. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. AF acknowledges support from the ERC Advanced Grant INTERSTELLAR H2020/740120. BD acknowledges financial support from NASA through the Astrophysics Data Analysis Program, grant number NNX12AE20G and the National Science Foundation, grant number 1716907. We are thankful for several discussions and constructive comments from Johannes Zabl, Eros Vanzella, Bo Milvang-Jensen, Henry McCracken, Max Gronke, Mark Dijkstra, Richard Ellis, and Nicolas Laporte. We also thank Umar Burhanudin and Izzy Garland for taking part in the XGAL internship in Lancaster and for exploring the HST grism data independently. Based on observations obtained with HST/WFC3 programs 12578, 14495, and 14596. Based on observations of the National Japanese Observatory with the Suprime-Cam on the Subaru telescope (S14A-086) on the big island of Hawaii. This work is based in part on data products produced at TERAPIX available at the Canadian Astronomy Data Centre as part of the Canada–France–Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme IDs 294.A-5018, 294.A-5039, 092.A 0786, 093.A-0561, 097.A0043, 097.A-0943, 098.A-0819, 298.A-5012, and 179.A-2005, and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. The authors acknowledge the award of service time (SW2014b20) on the William Herschel Telescope (WHT). WHT and its service programme are operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. This research was supported by the Munich Institute for Astro- and Particle Physics of the DFG cluster of excellence ‘Origin and Structure of the Universe’. We have benefitted immensely from the public available programming language PYTHON, including NUMPY and SCIPY (Jones et al. 2001; Van Der Walt, Colbert & Varoquaux 2011), MATPLOTLIB (Hunter 2007), ASTROPY (Astropy Collaboration et al. 2013), and the TOPCAT analysis program (Taylor 2013). This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France. All data used for this paper are publicly available, and we make all reduced data available with the refereed paper.","volume":482,"month":"01","oa_version":"Preprint","publication":"Monthly Notices of the Royal Astronomical Society","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","galaxies: ISM","cosmology: observations","dark ages","reionization","first stars","early Universe"],"oa":1,"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"date_published":"2019-01-01T00:00:00Z","type":"journal_article","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1710.08422"}]},{"language":[{"iso":"eng"}],"keyword":["Astronomy and Astrophysics"],"publication":"Frontiers in Astronomy and Space Sciences","month":"07","article_number":"46","oa_version":"Preprint","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1907.01415"}],"date_published":"2019-07-10T00:00:00Z","type":"journal_article","oa":1,"publication_identifier":{"eissn":["2296-987X"]},"quality_controlled":"1","article_type":"original","publisher":"Frontiers Media","author":[{"full_name":"Mathur, Savita","first_name":"Savita","last_name":"Mathur"},{"full_name":"García, Rafael A.","first_name":"Rafael A.","last_name":"García"},{"id":"d9edb345-f866-11ec-9b37-d119b5234501","orcid":"0000-0003-0142-4000","full_name":"Bugnet, Lisa Annabelle","first_name":"Lisa Annabelle","last_name":"Bugnet"},{"full_name":"Santos, Ângela R.G.","first_name":"Ângela R.G.","last_name":"Santos"},{"full_name":"Santiago, Netsha","last_name":"Santiago","first_name":"Netsha"},{"first_name":"Paul G.","last_name":"Beck","full_name":"Beck, Paul G."}],"_id":"11613","scopus_import":"1","title":"Revisiting the impact of stellar magnetic activity on the detectability of solar-like oscillations by Kepler","intvolume":" 6","publication_status":"published","article_processing_charge":"No","date_created":"2022-07-18T14:00:36Z","extern":"1","acknowledgement":"This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Partly Based on observations obtained with the HERMES spectrograph on the Mercator Telescope, which was supported by the Research Foundation—Flanders (FWO), Belgium, the Research Council of KU Leuven, Belgium, the Fonds National de la Recherche Scientifique (F.R.S.-FNRS), Belgium, the Royal Observatory of Belgium, the Observatoire de Genève, Switzerland, and the Thüringer Landessternwarte Tautenburg, Germany. SM acknowledges support by the National Aeronautics and Space Administration under Grant NNX15AF13G, by the National Science Foundation grant AST-1411685, and the Ramon y Cajal fellowship number RYC-2015-17697. RG acknowledges the support from PLATO and GOLF CNES grants. ÂS acknowledges the support from National Aeronautics and Space Administration under Grant NNX17AF27G. PB acknowledges the support of the MINECO under the fellowship program Juan de la Cierva Incorporacion (IJCI-2015-26034).","volume":6,"external_id":{"arxiv":["1907.01415"]},"date_updated":"2022-08-22T07:29:55Z","citation":{"chicago":"Mathur, Savita, Rafael A. García, Lisa Annabelle Bugnet, Ângela R.G. Santos, Netsha Santiago, and Paul G. Beck. “Revisiting the Impact of Stellar Magnetic Activity on the Detectability of Solar-like Oscillations by Kepler.” Frontiers in Astronomy and Space Sciences. Frontiers Media, 2019. https://doi.org/10.3389/fspas.2019.00046.","ieee":"S. Mathur, R. A. García, L. A. Bugnet, Â. R. G. Santos, N. Santiago, and P. G. Beck, “Revisiting the impact of stellar magnetic activity on the detectability of solar-like oscillations by Kepler,” Frontiers in Astronomy and Space Sciences, vol. 6. Frontiers Media, 2019.","apa":"Mathur, S., García, R. A., Bugnet, L. A., Santos, Â. R. G., Santiago, N., & Beck, P. G. (2019). Revisiting the impact of stellar magnetic activity on the detectability of solar-like oscillations by Kepler. Frontiers in Astronomy and Space Sciences. Frontiers Media. https://doi.org/10.3389/fspas.2019.00046","ama":"Mathur S, García RA, Bugnet LA, Santos ÂRG, Santiago N, Beck PG. Revisiting the impact of stellar magnetic activity on the detectability of solar-like oscillations by Kepler. Frontiers in Astronomy and Space Sciences. 2019;6. doi:10.3389/fspas.2019.00046","ista":"Mathur S, García RA, Bugnet LA, Santos ÂRG, Santiago N, Beck PG. 2019. Revisiting the impact of stellar magnetic activity on the detectability of solar-like oscillations by Kepler. Frontiers in Astronomy and Space Sciences. 6, 46.","mla":"Mathur, Savita, et al. “Revisiting the Impact of Stellar Magnetic Activity on the Detectability of Solar-like Oscillations by Kepler.” Frontiers in Astronomy and Space Sciences, vol. 6, 46, Frontiers Media, 2019, doi:10.3389/fspas.2019.00046.","short":"S. Mathur, R.A. García, L.A. Bugnet, Â.R.G. Santos, N. Santiago, P.G. Beck, Frontiers in Astronomy and Space Sciences 6 (2019)."},"year":"2019","abstract":[{"text":"Over 2,000 stars were observed for 1 month with a high enough cadence in order to look for acoustic modes during the survey phase of the Kepler mission. Solar-like oscillations have been detected in about 540 stars. The question of why no oscillations were detected in the remaining stars is still open. Previous works explained the non-detection of modes with the high level of magnetic activity of the stars. However, the sample of stars studied contained some classical pulsators and red giants that could have biased the results. In this work, we revisit this analysis on a cleaner sample of main-sequence solar-like stars that consists of 1,014 stars. First we compute the predicted amplitude of the modes of that sample and for the stars with detected oscillation and compare it to the noise at high frequency in the power spectrum. We find that the stars with detected modes have an amplitude to noise ratio larger than 0.94. We measure reliable rotation periods and the associated photometric magnetic index for 684 stars out of the full sample and in particular for 323 stars where the amplitude of the modes is predicted to be high enough to be detected. We find that among these 323 stars 32% of them have a level of magnetic activity larger than the Sun during its maximum activity, explaining the non-detection of acoustic modes. Interestingly, magnetic activity cannot be the primary reason responsible for the absence of detectable modes in the remaining 68% of the stars without acoustic modes detected and with reliable rotation periods. Thus, we investigate metallicity, inclination angle of the rotation axis, and binarity as possible causes of low mode amplitudes. Using spectroscopic observations for a subsample, we find that a low metallicity could be the reason for suppressed modes. No clear correlation with binarity nor inclination is found. We also derive the lower limit for our photometric activity index (of 20–30 ppm) below which rotation and magnetic activity are not detected. Finally, with our analysis we conclude that stars with a photometric activity index larger than 2,000 ppm have 98.3% probability of not having oscillations detected.","lang":"eng"}],"doi":"10.3389/fspas.2019.00046","arxiv":1,"day":"10"},{"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"language":[{"iso":"eng"}],"publication":"Astronomy & Astrophysics","article_number":"A79","month":"04","oa_version":"Preprint","status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"url":"https://arxiv.org/abs/1902.09854","open_access":"1"}],"type":"journal_article","date_published":"2019-04-19T00:00:00Z","oa":1,"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"quality_controlled":"1","article_type":"original","publisher":"EDP Science","author":[{"id":"d9edb345-f866-11ec-9b37-d119b5234501","orcid":"0000-0003-0142-4000","full_name":"Bugnet, Lisa Annabelle","first_name":"Lisa Annabelle","last_name":"Bugnet"},{"full_name":"García, R. A.","first_name":"R. A.","last_name":"García"},{"full_name":"Mathur, S.","last_name":"Mathur","first_name":"S."},{"full_name":"Davies, G. R.","last_name":"Davies","first_name":"G. R."},{"last_name":"Hall","first_name":"O. J.","full_name":"Hall, O. J."},{"full_name":"Lund, M. N.","last_name":"Lund","first_name":"M. N."},{"full_name":"Rendle, B. M.","first_name":"B. M.","last_name":"Rendle"}],"scopus_import":"1","_id":"11614","intvolume":" 624","title":"FliPerClass: In search of solar-like pulsators among TESS targets","article_processing_charge":"No","date_created":"2022-07-18T14:13:34Z","publication_status":"published","extern":"1","volume":624,"acknowledgement":"We thank the enitre T’DA team for useful comments and discussions, in particular Andrew Tkachenko. We also acknowledge Marc Hon, Keaton Bell, and James Kuszlewicz for useful comments on the manuscript. L.B. and R.A.G. acknowledge the support from PLATO and GOLF CNES grants. S.M. acknowledges support by the Ramon y Cajal fellowship number RYC-2015-17697. O.J.H. and B.M.R. acknowledge the support of the UK Science and Technology Facilities Council (STFC). M.N.L. acknowledges the support of the ESA PRODEX programme (PEA 4000119301). Funding for the Stellar Astrophysics Centre is provided by the Danish National Research Foundation (Grant DNRF106).","external_id":{"arxiv":["1902.09854"]},"year":"2019","citation":{"mla":"Bugnet, Lisa Annabelle, et al. “FliPerClass: In Search of Solar-like Pulsators among TESS Targets.” Astronomy & Astrophysics, vol. 624, A79, EDP Science, 2019, doi:10.1051/0004-6361/201834780.","short":"L.A. Bugnet, R.A. García, S. Mathur, G.R. Davies, O.J. Hall, M.N. Lund, B.M. Rendle, Astronomy & Astrophysics 624 (2019).","ista":"Bugnet LA, García RA, Mathur S, Davies GR, Hall OJ, Lund MN, Rendle BM. 2019. FliPerClass: In search of solar-like pulsators among TESS targets. Astronomy & Astrophysics. 624, A79.","apa":"Bugnet, L. A., García, R. A., Mathur, S., Davies, G. R., Hall, O. J., Lund, M. N., & Rendle, B. M. (2019). FliPerClass: In search of solar-like pulsators among TESS targets. Astronomy & Astrophysics. EDP Science. https://doi.org/10.1051/0004-6361/201834780","ama":"Bugnet LA, García RA, Mathur S, et al. FliPerClass: In search of solar-like pulsators among TESS targets. Astronomy & Astrophysics. 2019;624. doi:10.1051/0004-6361/201834780","chicago":"Bugnet, Lisa Annabelle, R. A. García, S. Mathur, G. R. Davies, O. J. Hall, M. N. Lund, and B. M. Rendle. “FliPerClass: In Search of Solar-like Pulsators among TESS Targets.” Astronomy & Astrophysics. EDP Science, 2019. https://doi.org/10.1051/0004-6361/201834780.","ieee":"L. A. Bugnet et al., “FliPerClass: In search of solar-like pulsators among TESS targets,” Astronomy & Astrophysics, vol. 624. EDP Science, 2019."},"date_updated":"2022-08-22T07:32:51Z","abstract":[{"text":"The NASA Transiting Exoplanet Survey Satellite (TESS) is about to provide full-frame images of almost the entire sky. The amount of stellar data to be analysed represents hundreds of millions stars, which is several orders of magnitude more than the number of stars observed by the Convection, Rotation and planetary Transits satellite (CoRoT), and NASA Kepler and K2 missions. We aim at automatically classifying the newly observed stars with near real-time algorithms to better guide the subsequent detailed studies. In this paper, we present a classification algorithm built to recognise solar-like pulsators among classical pulsators. This algorithm relies on the global amount of power contained in the power spectral density (PSD), also known as the flicker in spectral power density (FliPer). Because each type of pulsating star has a characteristic background or pulsation pattern, the shape of the PSD at different frequencies can be used to characterise the type of pulsating star. The FliPer classifier (FliPerClass) uses different FliPer parameters along with the effective temperature as input parameters to feed a ML algorithm in order to automatically classify the pulsating stars observed by TESS. Using noisy TESS-simulated data from the TESS Asteroseismic Science Consortium (TASC), we classify pulsators with a 98% accuracy. Among them, solar-like pulsating stars are recognised with a 99% accuracy, which is of great interest for a further seismic analysis of these stars, which are like our Sun. Similar results are obtained when we trained our classifier and applied it to 27-day subsets of real Kepler data. FliPerClass is part of the large TASC classification pipeline developed by the TESS Data for Asteroseismology (T’DA) classification working group.","lang":"eng"}],"day":"19","arxiv":1,"doi":"10.1051/0004-6361/201834780"},{"publication":"Monthly Notices of the Royal Astronomical Society","oa_version":"Preprint","month":"06","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","asteroseismology","methods: data analysis","techniques: image processing","stars: oscillations","stars: statistics"],"date_published":"2019-06-01T00:00:00Z","type":"journal_article","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"oa":1,"main_file_link":[{"url":"https://arxiv.org/abs/1903.00115","open_access":"1"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","_id":"11615","scopus_import":"1","author":[{"last_name":"Hon","first_name":"Marc","full_name":"Hon, Marc"},{"first_name":"Dennis","last_name":"Stello","full_name":"Stello, Dennis"},{"full_name":"García, Rafael A","last_name":"García","first_name":"Rafael A"},{"last_name":"Mathur","first_name":"Savita","full_name":"Mathur, Savita"},{"full_name":"Sharma, Sanjib","last_name":"Sharma","first_name":"Sanjib"},{"first_name":"Isabel L","last_name":"Colman","full_name":"Colman, Isabel L"},{"first_name":"Lisa Annabelle","last_name":"Bugnet","orcid":"0000-0003-0142-4000","full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501"}],"issue":"4","publication_status":"published","date_created":"2022-07-18T14:26:03Z","article_processing_charge":"No","title":"A search for red giant solar-like oscillations in all Kepler data","intvolume":" 485","page":"5616-5630","quality_controlled":"1","publisher":"Oxford University Press","article_type":"original","date_updated":"2022-08-22T07:35:19Z","year":"2019","citation":{"ieee":"M. Hon et al., “A search for red giant solar-like oscillations in all Kepler data,” Monthly Notices of the Royal Astronomical Society, vol. 485, no. 4. Oxford University Press, pp. 5616–5630, 2019.","chicago":"Hon, Marc, Dennis Stello, Rafael A García, Savita Mathur, Sanjib Sharma, Isabel L Colman, and Lisa Annabelle Bugnet. “A Search for Red Giant Solar-like Oscillations in All Kepler Data.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2019. https://doi.org/10.1093/mnras/stz622.","apa":"Hon, M., Stello, D., García, R. A., Mathur, S., Sharma, S., Colman, I. L., & Bugnet, L. A. (2019). A search for red giant solar-like oscillations in all Kepler data. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stz622","ama":"Hon M, Stello D, García RA, et al. A search for red giant solar-like oscillations in all Kepler data. Monthly Notices of the Royal Astronomical Society. 2019;485(4):5616-5630. doi:10.1093/mnras/stz622","ista":"Hon M, Stello D, García RA, Mathur S, Sharma S, Colman IL, Bugnet LA. 2019. A search for red giant solar-like oscillations in all Kepler data. Monthly Notices of the Royal Astronomical Society. 485(4), 5616–5630.","short":"M. Hon, D. Stello, R.A. García, S. Mathur, S. Sharma, I.L. Colman, L.A. Bugnet, Monthly Notices of the Royal Astronomical Society 485 (2019) 5616–5630.","mla":"Hon, Marc, et al. “A Search for Red Giant Solar-like Oscillations in All Kepler Data.” Monthly Notices of the Royal Astronomical Society, vol. 485, no. 4, Oxford University Press, 2019, pp. 5616–30, doi:10.1093/mnras/stz622."},"external_id":{"arxiv":["1903.00115"]},"arxiv":1,"doi":"10.1093/mnras/stz622","day":"01","abstract":[{"lang":"eng","text":"The recently published Kepler mission Data Release 25 (DR25) reported on ∼197 000 targets observed during the mission. Despite this, no wide search for red giants showing solar-like oscillations have been made across all stars observed in Kepler’s long-cadence mode. In this work, we perform this task using custom apertures on the Kepler pixel files and detect oscillations in 21 914 stars, representing the largest sample of solar-like oscillating stars to date. We measure their frequency at maximum power, νmax, down to νmax≃4μHz and obtain log (g) estimates with a typical uncertainty below 0.05 dex, which is superior to typical measurements from spectroscopy. Additionally, the νmax distribution of our detections show good agreement with results from a simulated model of the Milky Way, with a ratio of observed to predicted stars of 0.992 for stars with 10<νmax<270μHz. Among our red giant detections, we find 909 to be dwarf/subgiant stars whose flux signal is polluted by a neighbouring giant as a result of using larger photometric apertures than those used by the NASA Kepler science processing pipeline. We further find that only 293 of the polluting giants are known Kepler targets. The remainder comprises over 600 newly identified oscillating red giants, with many expected to belong to the Galactic halo, serendipitously falling within the Kepler pixel files of targeted stars."}],"volume":485,"acknowledgement":"Funding for this Discovery mission is provided by NASA’s Science mission Directorate. We thank the entire Kepler team without whom this investigation would not be possible. DS is the recipient of an Australian Research Council Future Fellowship (project number FT1400147). RAG acknowledges the support from CNES. SM acknowledges support from NASA grant NNX15AF13G, NSF grant AST-1411685, and the Ramon y Cajal fellowship number RYC-2015-17697. ILC acknowledges scholarship support from the University of Sydney. We would like to thank Nicholas Barbara and Timothy Bedding for providing us with a list of variable stars that helped to validate a number of detections in this study. We also thank the group at the University of Sydney for fruitful discussions. Finally, we gratefully acknowledge the support of NVIDIA Corporation with the donation of the Titan Xp GPU used for this research.","extern":"1"},{"author":[{"full_name":"Huber, Daniel","last_name":"Huber","first_name":"Daniel"},{"first_name":"William J.","last_name":"Chaplin","full_name":"Chaplin, William J."},{"last_name":"Chontos","first_name":"Ashley","full_name":"Chontos, Ashley"},{"last_name":"Kjeldsen","first_name":"Hans","full_name":"Kjeldsen, Hans"},{"full_name":"Christensen-Dalsgaard, Jørgen","first_name":"Jørgen","last_name":"Christensen-Dalsgaard"},{"first_name":"Timothy R.","last_name":"Bedding","full_name":"Bedding, Timothy R."},{"full_name":"Ball, Warrick","last_name":"Ball","first_name":"Warrick"},{"last_name":"Brahm","first_name":"Rafael","full_name":"Brahm, Rafael"},{"full_name":"Espinoza, Nestor","first_name":"Nestor","last_name":"Espinoza"},{"full_name":"Henning, Thomas","first_name":"Thomas","last_name":"Henning"},{"full_name":"Jordán, Andrés","first_name":"Andrés","last_name":"Jordán"},{"full_name":"Sarkis, Paula","first_name":"Paula","last_name":"Sarkis"},{"full_name":"Knudstrup, Emil","first_name":"Emil","last_name":"Knudstrup"},{"full_name":"Albrecht, Simon","first_name":"Simon","last_name":"Albrecht"},{"last_name":"Grundahl","first_name":"Frank","full_name":"Grundahl, Frank"},{"first_name":"Mads Fredslund","last_name":"Andersen","full_name":"Andersen, Mads Fredslund"},{"full_name":"Pallé, Pere L.","first_name":"Pere L.","last_name":"Pallé"},{"first_name":"Ian","last_name":"Crossfield","full_name":"Crossfield, Ian"},{"full_name":"Fulton, Benjamin","last_name":"Fulton","first_name":"Benjamin"},{"last_name":"Howard","first_name":"Andrew W.","full_name":"Howard, Andrew W."},{"full_name":"Isaacson, Howard T.","first_name":"Howard T.","last_name":"Isaacson"},{"last_name":"Weiss","first_name":"Lauren M.","full_name":"Weiss, Lauren M."},{"last_name":"Handberg","first_name":"Rasmus","full_name":"Handberg, Rasmus"},{"full_name":"Lund, Mikkel N.","last_name":"Lund","first_name":"Mikkel N."},{"full_name":"Serenelli, Aldo M.","last_name":"Serenelli","first_name":"Aldo M."},{"full_name":"Rørsted Mosumgaard, Jakob","last_name":"Rørsted Mosumgaard","first_name":"Jakob"},{"last_name":"Stokholm","first_name":"Amalie","full_name":"Stokholm, Amalie"},{"first_name":"Allyson","last_name":"Bieryla","full_name":"Bieryla, Allyson"},{"full_name":"Buchhave, Lars A.","first_name":"Lars A.","last_name":"Buchhave"},{"full_name":"Latham, David W.","last_name":"Latham","first_name":"David W."},{"first_name":"Samuel N.","last_name":"Quinn","full_name":"Quinn, Samuel N."},{"first_name":"Eric","last_name":"Gaidos","full_name":"Gaidos, Eric"},{"last_name":"Hirano","first_name":"Teruyuki","full_name":"Hirano, Teruyuki"},{"last_name":"Ricker","first_name":"George R.","full_name":"Ricker, George R."},{"first_name":"Roland K.","last_name":"Vanderspek","full_name":"Vanderspek, Roland K."},{"first_name":"Sara","last_name":"Seager","full_name":"Seager, Sara"},{"first_name":"Jon M.","last_name":"Jenkins","full_name":"Jenkins, Jon M."},{"full_name":"Winn, Joshua N.","first_name":"Joshua N.","last_name":"Winn"},{"last_name":"Antia","first_name":"H. M.","full_name":"Antia, H. M."},{"first_name":"Thierry","last_name":"Appourchaux","full_name":"Appourchaux, Thierry"},{"last_name":"Basu","first_name":"Sarbani","full_name":"Basu, Sarbani"},{"full_name":"Bell, Keaton J.","first_name":"Keaton J.","last_name":"Bell"},{"first_name":"Othman","last_name":"Benomar","full_name":"Benomar, Othman"},{"first_name":"Alfio","last_name":"Bonanno","full_name":"Bonanno, Alfio"},{"last_name":"Buzasi","first_name":"Derek L.","full_name":"Buzasi, Derek L."},{"full_name":"Campante, Tiago L.","last_name":"Campante","first_name":"Tiago L."},{"full_name":"Çelik Orhan, Z.","last_name":"Çelik Orhan","first_name":"Z."},{"full_name":"Corsaro, Enrico","first_name":"Enrico","last_name":"Corsaro"},{"full_name":"Cunha, Margarida S.","first_name":"Margarida S.","last_name":"Cunha"},{"full_name":"Davies, Guy R.","last_name":"Davies","first_name":"Guy R."},{"first_name":"Sebastien","last_name":"Deheuvels","full_name":"Deheuvels, Sebastien"},{"full_name":"Grunblatt, Samuel K.","first_name":"Samuel K.","last_name":"Grunblatt"},{"first_name":"Amir","last_name":"Hasanzadeh","full_name":"Hasanzadeh, Amir"},{"full_name":"Di Mauro, Maria Pia","first_name":"Maria Pia","last_name":"Di Mauro"},{"full_name":"A. García, Rafael","first_name":"Rafael","last_name":"A. García"},{"full_name":"Gaulme, Patrick","first_name":"Patrick","last_name":"Gaulme"},{"full_name":"Girardi, Léo","last_name":"Girardi","first_name":"Léo"},{"last_name":"Guzik","first_name":"Joyce A.","full_name":"Guzik, Joyce A."},{"full_name":"Hon, Marc","first_name":"Marc","last_name":"Hon"},{"full_name":"Jiang, Chen","last_name":"Jiang","first_name":"Chen"},{"last_name":"Kallinger","first_name":"Thomas","full_name":"Kallinger, Thomas"},{"first_name":"Steven D.","last_name":"Kawaler","full_name":"Kawaler, Steven D."},{"first_name":"James S.","last_name":"Kuszlewicz","full_name":"Kuszlewicz, James S."},{"first_name":"Yveline","last_name":"Lebreton","full_name":"Lebreton, Yveline"},{"last_name":"Li","first_name":"Tanda","full_name":"Li, Tanda"},{"last_name":"Lucas","first_name":"Miles","full_name":"Lucas, Miles"},{"last_name":"Lundkvist","first_name":"Mia S.","full_name":"Lundkvist, Mia S."},{"last_name":"Mann","first_name":"Andrew W.","full_name":"Mann, Andrew W."},{"last_name":"Mathis","first_name":"Stéphane","full_name":"Mathis, Stéphane"},{"full_name":"Mathur, Savita","last_name":"Mathur","first_name":"Savita"},{"full_name":"Mazumdar, Anwesh","first_name":"Anwesh","last_name":"Mazumdar"},{"last_name":"Metcalfe","first_name":"Travis S.","full_name":"Metcalfe, Travis S."},{"last_name":"Miglio","first_name":"Andrea","full_name":"Miglio, Andrea"},{"last_name":"F. G. Monteiro","first_name":"Mário J. P.","full_name":"F. G. Monteiro, Mário J. P."},{"full_name":"Mosser, Benoit","first_name":"Benoit","last_name":"Mosser"},{"full_name":"Noll, Anthony","last_name":"Noll","first_name":"Anthony"},{"last_name":"Nsamba","first_name":"Benard","full_name":"Nsamba, Benard"},{"full_name":"Joel Ong, Jia Mian","last_name":"Joel Ong","first_name":"Jia Mian"},{"first_name":"S.","last_name":"Örtel","full_name":"Örtel, S."},{"full_name":"Pereira, Filipe","last_name":"Pereira","first_name":"Filipe"},{"last_name":"Ranadive","first_name":"Pritesh","full_name":"Ranadive, Pritesh"},{"last_name":"Régulo","first_name":"Clara","full_name":"Régulo, Clara"},{"last_name":"Rodrigues","first_name":"Thaíse S.","full_name":"Rodrigues, Thaíse S."},{"full_name":"Roxburgh, Ian W.","last_name":"Roxburgh","first_name":"Ian W."},{"first_name":"Victor Silva","last_name":"Aguirre","full_name":"Aguirre, Victor Silva"},{"last_name":"Smalley","first_name":"Barry","full_name":"Smalley, Barry"},{"full_name":"Schofield, Mathew","first_name":"Mathew","last_name":"Schofield"},{"first_name":"Sérgio G.","last_name":"Sousa","full_name":"Sousa, Sérgio G."},{"last_name":"Stassun","first_name":"Keivan G.","full_name":"Stassun, Keivan G."},{"first_name":"Dennis","last_name":"Stello","full_name":"Stello, Dennis"},{"last_name":"Tayar","first_name":"Jamie","full_name":"Tayar, Jamie"},{"full_name":"White, Timothy R.","first_name":"Timothy R.","last_name":"White"},{"first_name":"Kuldeep","last_name":"Verma","full_name":"Verma, Kuldeep"},{"last_name":"Vrard","first_name":"Mathieu","full_name":"Vrard, Mathieu"},{"full_name":"Yıldız, M.","first_name":"M.","last_name":"Yıldız"},{"full_name":"Baker, David","first_name":"David","last_name":"Baker"},{"full_name":"Bazot, Michaël","last_name":"Bazot","first_name":"Michaël"},{"full_name":"Beichmann, Charles","first_name":"Charles","last_name":"Beichmann"},{"last_name":"Bergmann","first_name":"Christoph","full_name":"Bergmann, Christoph"},{"first_name":"Lisa Annabelle","last_name":"Bugnet","orcid":"0000-0003-0142-4000","full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501"},{"last_name":"Cale","first_name":"Bryson","full_name":"Cale, Bryson"},{"last_name":"Carlino","first_name":"Roberto","full_name":"Carlino, Roberto"},{"full_name":"Cartwright, Scott M.","first_name":"Scott M.","last_name":"Cartwright"},{"full_name":"Christiansen, Jessie L.","last_name":"Christiansen","first_name":"Jessie L."},{"first_name":"David R.","last_name":"Ciardi","full_name":"Ciardi, David R."},{"full_name":"Creevey, Orlagh","first_name":"Orlagh","last_name":"Creevey"},{"last_name":"Dittmann","first_name":"Jason A.","full_name":"Dittmann, Jason A."},{"first_name":"Jose-Dias Do","last_name":"Nascimento","full_name":"Nascimento, Jose-Dias Do"},{"first_name":"Vincent Van","last_name":"Eylen","full_name":"Eylen, Vincent Van"},{"last_name":"Fürész","first_name":"Gabor","full_name":"Fürész, Gabor"},{"first_name":"Jonathan","last_name":"Gagné","full_name":"Gagné, Jonathan"},{"last_name":"Gao","first_name":"Peter","full_name":"Gao, Peter"},{"full_name":"Gazeas, Kosmas","last_name":"Gazeas","first_name":"Kosmas"},{"last_name":"Giddens","first_name":"Frank","full_name":"Giddens, Frank"},{"first_name":"Oliver J.","last_name":"Hall","full_name":"Hall, Oliver J."},{"first_name":"Saskia","last_name":"Hekker","full_name":"Hekker, Saskia"},{"full_name":"Ireland, Michael J.","first_name":"Michael J.","last_name":"Ireland"},{"full_name":"Latouf, Natasha","last_name":"Latouf","first_name":"Natasha"},{"full_name":"LeBrun, Danny","first_name":"Danny","last_name":"LeBrun"},{"full_name":"Levine, Alan M.","first_name":"Alan M.","last_name":"Levine"},{"first_name":"William","last_name":"Matzko","full_name":"Matzko, William"},{"full_name":"Natinsky, Eva","last_name":"Natinsky","first_name":"Eva"},{"first_name":"Emma","last_name":"Page","full_name":"Page, Emma"},{"first_name":"Peter","last_name":"Plavchan","full_name":"Plavchan, Peter"},{"full_name":"Mansouri-Samani, Masoud","last_name":"Mansouri-Samani","first_name":"Masoud"},{"full_name":"McCauliff, Sean","first_name":"Sean","last_name":"McCauliff"},{"full_name":"Mullally, Susan E.","first_name":"Susan E.","last_name":"Mullally"},{"full_name":"Orenstein, Brendan","first_name":"Brendan","last_name":"Orenstein"},{"full_name":"Soto, Aylin Garcia","first_name":"Aylin Garcia","last_name":"Soto"},{"full_name":"Paegert, Martin","first_name":"Martin","last_name":"Paegert"},{"first_name":"Jennifer L.","last_name":"van Saders","full_name":"van Saders, Jennifer L."},{"last_name":"Schnaible","first_name":"Chloe","full_name":"Schnaible, Chloe"},{"full_name":"Soderblom, David R.","first_name":"David R.","last_name":"Soderblom"},{"first_name":"Róbert","last_name":"Szabó","full_name":"Szabó, Róbert"},{"full_name":"Tanner, Angelle","first_name":"Angelle","last_name":"Tanner"},{"last_name":"Tinney","first_name":"C. G.","full_name":"Tinney, C. G."},{"last_name":"Teske","first_name":"Johanna","full_name":"Teske, Johanna"},{"last_name":"Thomas","first_name":"Alexandra","full_name":"Thomas, Alexandra"},{"last_name":"Trampedach","first_name":"Regner","full_name":"Trampedach, Regner"},{"first_name":"Duncan","last_name":"Wright","full_name":"Wright, Duncan"},{"last_name":"Yuan","first_name":"Thomas T.","full_name":"Yuan, Thomas T."},{"last_name":"Zohrabi","first_name":"Farzaneh","full_name":"Zohrabi, Farzaneh"}],"issue":"6","_id":"11616","scopus_import":"1","title":"A hot Saturn orbiting an oscillating late subgiant discovered by TESS","intvolume":" 157","publication_status":"published","article_processing_charge":"No","date_created":"2022-07-18T14:29:07Z","quality_controlled":"1","article_type":"original","publisher":"IOP Publishing","external_id":{"arxiv":["1901.01643"]},"date_updated":"2022-08-22T07:38:34Z","citation":{"ista":"Huber D et al. 2019. A hot Saturn orbiting an oscillating late subgiant discovered by TESS. The Astronomical Journal. 157(6), 245.","mla":"Huber, Daniel, et al. “A Hot Saturn Orbiting an Oscillating Late Subgiant Discovered by TESS.” The Astronomical Journal, vol. 157, no. 6, 245, IOP Publishing, 2019, doi:10.3847/1538-3881/ab1488.","short":"D. Huber, W.J. Chaplin, A. Chontos, H. Kjeldsen, J. Christensen-Dalsgaard, T.R. Bedding, W. Ball, R. Brahm, N. Espinoza, T. Henning, A. Jordán, P. Sarkis, E. Knudstrup, S. Albrecht, F. Grundahl, M.F. Andersen, P.L. Pallé, I. Crossfield, B. Fulton, A.W. Howard, H.T. Isaacson, L.M. Weiss, R. Handberg, M.N. Lund, A.M. Serenelli, J. Rørsted Mosumgaard, A. Stokholm, A. Bieryla, L.A. Buchhave, D.W. Latham, S.N. Quinn, E. Gaidos, T. Hirano, G.R. Ricker, R.K. Vanderspek, S. Seager, J.M. Jenkins, J.N. Winn, H.M. Antia, T. Appourchaux, S. Basu, K.J. Bell, O. Benomar, A. Bonanno, D.L. Buzasi, T.L. Campante, Z. Çelik Orhan, E. Corsaro, M.S. Cunha, G.R. Davies, S. Deheuvels, S.K. Grunblatt, A. Hasanzadeh, M.P. Di Mauro, R. A. García, P. Gaulme, L. Girardi, J.A. Guzik, M. Hon, C. Jiang, T. Kallinger, S.D. Kawaler, J.S. Kuszlewicz, Y. Lebreton, T. Li, M. Lucas, M.S. Lundkvist, A.W. Mann, S. Mathis, S. Mathur, A. Mazumdar, T.S. Metcalfe, A. Miglio, M.J.P. F. G. Monteiro, B. Mosser, A. Noll, B. Nsamba, J.M. Joel Ong, S. Örtel, F. Pereira, P. Ranadive, C. Régulo, T.S. Rodrigues, I.W. Roxburgh, V.S. Aguirre, B. Smalley, M. Schofield, S.G. Sousa, K.G. Stassun, D. Stello, J. Tayar, T.R. White, K. Verma, M. Vrard, M. Yıldız, D. Baker, M. Bazot, C. Beichmann, C. Bergmann, L.A. Bugnet, B. Cale, R. Carlino, S.M. Cartwright, J.L. Christiansen, D.R. Ciardi, O. Creevey, J.A. Dittmann, J.-D.D. Nascimento, V.V. Eylen, G. Fürész, J. Gagné, P. Gao, K. Gazeas, F. Giddens, O.J. Hall, S. Hekker, M.J. Ireland, N. Latouf, D. LeBrun, A.M. Levine, W. Matzko, E. Natinsky, E. Page, P. Plavchan, M. Mansouri-Samani, S. McCauliff, S.E. Mullally, B. Orenstein, A.G. Soto, M. Paegert, J.L. van Saders, C. Schnaible, D.R. Soderblom, R. Szabó, A. Tanner, C.G. Tinney, J. Teske, A. Thomas, R. Trampedach, D. Wright, T.T. Yuan, F. Zohrabi, The Astronomical Journal 157 (2019).","chicago":"Huber, Daniel, William J. Chaplin, Ashley Chontos, Hans Kjeldsen, Jørgen Christensen-Dalsgaard, Timothy R. Bedding, Warrick Ball, et al. “A Hot Saturn Orbiting an Oscillating Late Subgiant Discovered by TESS.” The Astronomical Journal. IOP Publishing, 2019. https://doi.org/10.3847/1538-3881/ab1488.","ieee":"D. Huber et al., “A hot Saturn orbiting an oscillating late subgiant discovered by TESS,” The Astronomical Journal, vol. 157, no. 6. IOP Publishing, 2019.","apa":"Huber, D., Chaplin, W. J., Chontos, A., Kjeldsen, H., Christensen-Dalsgaard, J., Bedding, T. R., … Zohrabi, F. (2019). A hot Saturn orbiting an oscillating late subgiant discovered by TESS. The Astronomical Journal. IOP Publishing. https://doi.org/10.3847/1538-3881/ab1488","ama":"Huber D, Chaplin WJ, Chontos A, et al. A hot Saturn orbiting an oscillating late subgiant discovered by TESS. The Astronomical Journal. 2019;157(6). doi:10.3847/1538-3881/ab1488"},"year":"2019","abstract":[{"lang":"eng","text":"We present the discovery of HD 221416 b, the first transiting planet identified by the Transiting Exoplanet Survey Satellite (TESS) for which asteroseismology of the host star is possible. HD 221416 b (HIP 116158, TOI-197) is a bright (V = 8.2 mag), spectroscopically classified subgiant that oscillates with an average frequency of about 430 μHz and displays a clear signature of mixed modes. The oscillation amplitude confirms that the redder TESS bandpass compared to Kepler has a small effect on the oscillations, supporting the expected yield of thousands of solar-like oscillators with TESS 2 minute cadence observations. Asteroseismic modeling yields a robust determination of the host star radius (R⋆ = 2.943 ± 0.064 R⊙), mass (M⋆ = 1.212 ± 0.074 M⊙), and age (4.9 ± 1.1 Gyr), and demonstrates that it has just started ascending the red-giant branch. Combining asteroseismology with transit modeling and radial-velocity observations, we show that the planet is a \"hot Saturn\" (Rp = 9.17 ± 0.33 R⊕) with an orbital period of ∼14.3 days, irradiance of F = 343 ± 24 F⊕, and moderate mass (Mp = 60.5 ± 5.7 M⊕) and density (ρp = 0.431 ± 0.062 g cm−3). The properties of HD 221416 b show that the host-star metallicity–planet mass correlation found in sub-Saturns (4–8 R⊕) does not extend to larger radii, indicating that planets in the transition between sub-Saturns and Jupiters follow a relatively narrow range of densities. With a density measured to ∼15%, HD 221416 b is one of the best characterized Saturn-size planets to date, augmenting the small number of known transiting planets around evolved stars and demonstrating the power of TESS to characterize exoplanets and their host stars using asteroseismology."}],"arxiv":1,"doi":"10.3847/1538-3881/ab1488","day":"30","extern":"1","acknowledgement":"The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawai'ian community. We are most fortunate to have the opportunity to conduct observations from this mountain. We thank Andrei Tokovinin for helpful information on the Speckle observations obtained with SOAR. D.H. acknowledges support by the National Aeronautics and Space Administration through the TESS Guest Investigator Program (80NSSC18K1585) and by the National Science Foundation (AST-1717000). A.C. acknowledges support by the National Science Foundation under the Graduate Research Fellowship Program. W.J.C., W.H.B., A.M., O.J.H., and G.R.D. acknowledge support from the Science and Technology Facilities Council and UK Space Agency. H.K. and F.G. acknowledge support from the European Social Fund via the Lithuanian Science Council grant No. 09.3.3-LMT-K-712-01-0103. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (grant DNRF106). A.J. acknowledges support from FONDECYT project 1171208, CONICYT project BASAL AFB-170002, and by the Ministry for the Economy, Development, and Tourism's Programa Iniciativa Científica Milenio through grant IC 120009, awarded to the Millennium Institute of Astrophysics (MAS). R.B. acknowledges support from FONDECYT Post-doctoral Fellowship Project 3180246, and from the Millennium Institute of Astrophysics (MAS). A.M.S. is supported by grants ESP2017-82674-R (MINECO) and SGR2017-1131 (AGAUR). R.A.G. and L.B. acknowledge the support of the PLATO grant from the CNES. The research leading to the presented results has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP72007-2013)ERC grant agreement No. 338251 (StellarAges). S.M. acknowledges support from the European Research Council through the SPIRE grant 647383. This work was also supported by FCT (Portugal) through national funds and by FEDER through COMPETE2020 by these grants: UID/FIS/04434/2013 and POCI-01-0145-FEDER-007672, PTDC/FIS-AST/30389/2017, and POCI-01-0145-FEDER-030389. T.L.C. acknowledges support from the European Union's Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement No. 792848 (PULSATION). E.C. is funded by the European Union's Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement No. 664931. V.S.A. acknowledges support from the Independent Research Fund Denmark (Research grant 7027-00096B). D.S. acknowledges support from the Australian Research Council. S.B. acknowledges NASA grant NNX16AI09G and NSF grant AST-1514676. T.R.W. acknowledges support from the Australian Research Council through grant DP150100250. A.M. acknowledges support from the ERC Consolidator Grant funding scheme (project ASTEROCHRONOMETRY, G.A. n. 772293). S.M. acknowledges support from the Ramon y Cajal fellowship number RYC-2015-17697. M.S.L. is supported by the Carlsberg Foundation (grant agreement No. CF17-0760). A.M. and P.R. acknowledge support from the HBCSE-NIUS programme. J.K.T. and J.T. acknowledge that support for this work was provided by NASA through Hubble Fellowship grants HST-HF2-51399.001 and HST-HF2-51424.001 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. T.S.R. acknowledges financial support from Premiale 2015 MITiC (PI B. Garilli). This project has been supported by the NKFIH K-115709 grant and the Lendület Program of the Hungarian Academy of Sciences, project No. LP2018-7/2018.\r\n\r\nBased on observations made with the Hertzsprung SONG telescope operated on the Spanish Observatorio del Teide on the island of Tenerife by the Aarhus and Copenhagen Universities and by the Instituto de Astrofísica de Canarias. Funding for the TESS mission is provided by NASA's Science Mission directorate. We acknowledge the use of public TESS Alert data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. This research has made use of the Exoplanet Follow-up Observation Program website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST).\r\n\r\nSoftware: Astropy (Astropy Collaboration et al. 2018), Matplotlib (Hunter 2007), DIAMONDS (Corsaro & De Ridder 2014), isoclassify (Huber et al. 2017), EXOFASTv2 (Eastman 2017), ktransit (Barclay 2018).","volume":157,"publication":"The Astronomical Journal","month":"05","article_number":"245","oa_version":"Preprint","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"date_published":"2019-05-30T00:00:00Z","type":"journal_article","oa":1,"publication_identifier":{"issn":["0004-6256"]},"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"url":"https://arxiv.org/abs/1901.01643","open_access":"1"}]},{"doi":"10.3847/1538-4365/ab3b56","arxiv":1,"day":"19","abstract":[{"lang":"eng","text":"Brightness variations due to dark spots on the stellar surface encode information about stellar surface rotation and magnetic activity. In this work, we analyze the Kepler long-cadence data of 26,521 main-sequence stars of spectral types M and K in order to measure their surface rotation and photometric activity level. Rotation-period estimates are obtained by the combination of a wavelet analysis and autocorrelation function of the light curves. Reliable rotation estimates are determined by comparing the results from the different rotation diagnostics and four data sets. We also measure the photometric activity proxy Sph using the amplitude of the flux variations on an appropriate timescale. We report rotation periods and photometric activity proxies for about 60% of the sample, including 4431 targets for which McQuillan et al. did not report a rotation period. For the common targets with rotation estimates in this study and in McQuillan et al., our rotation periods agree within 99%. In this work, we also identify potential polluters, such as misclassified red giants and classical pulsator candidates. Within the parameter range we study, there is a mild tendency for hotter stars to have shorter rotation periods. The photometric activity proxy spans a wider range of values with increasing effective temperature. The rotation period and photometric activity proxy are also related, with Sph being larger for fast rotators. Similar to McQuillan et al., we find a bimodal distribution of rotation periods."}],"date_updated":"2022-08-22T08:10:38Z","year":"2019","citation":{"ieee":"A. R. G. Santos et al., “Surface rotation and photometric activity for Kepler targets. I. M and K main-sequence stars,” The Astrophysical Journal Supplement Series, vol. 244, no. 1. IOP Publishing, 2019.","chicago":"Santos, A. R. G., R. A. García, S. Mathur, Lisa Annabelle Bugnet, J. L. van Saders, T. S. Metcalfe, G. V. A. Simonian, and M. H. Pinsonneault. “Surface Rotation and Photometric Activity for Kepler Targets. I. M and K Main-Sequence Stars.” The Astrophysical Journal Supplement Series. IOP Publishing, 2019. https://doi.org/10.3847/1538-4365/ab3b56.","ama":"Santos ARG, García RA, Mathur S, et al. Surface rotation and photometric activity for Kepler targets. I. M and K main-sequence stars. The Astrophysical Journal Supplement Series. 2019;244(1). doi:10.3847/1538-4365/ab3b56","apa":"Santos, A. R. G., García, R. A., Mathur, S., Bugnet, L. A., van Saders, J. L., Metcalfe, T. S., … Pinsonneault, M. H. (2019). Surface rotation and photometric activity for Kepler targets. I. M and K main-sequence stars. The Astrophysical Journal Supplement Series. IOP Publishing. https://doi.org/10.3847/1538-4365/ab3b56","ista":"Santos ARG, García RA, Mathur S, Bugnet LA, van Saders JL, Metcalfe TS, Simonian GVA, Pinsonneault MH. 2019. Surface rotation and photometric activity for Kepler targets. I. M and K main-sequence stars. The Astrophysical Journal Supplement Series. 244(1), 21.","mla":"Santos, A. R. G., et al. “Surface Rotation and Photometric Activity for Kepler Targets. I. M and K Main-Sequence Stars.” The Astrophysical Journal Supplement Series, vol. 244, no. 1, 21, IOP Publishing, 2019, doi:10.3847/1538-4365/ab3b56.","short":"A.R.G. Santos, R.A. García, S. Mathur, L.A. Bugnet, J.L. van Saders, T.S. Metcalfe, G.V.A. Simonian, M.H. Pinsonneault, The Astrophysical Journal Supplement Series 244 (2019)."},"external_id":{"arxiv":["1908.05222"]},"acknowledgement":"The authors thank Róbert Szabó Paul G. Beck, Katrien Kolenberg, and Isabel L. Colman for helping on the classification of stars. This paper includes data collected by the Kepler mission and obtained from the MAST data archive at the Space Telescope Science Institute (STScI). Funding for the Kepler mission is provided by the National Aeronautics and Space Administration (NASA) Science Mission Directorate. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–26555. A.R.G.S. acknowledges the support from NASA under grant NNX17AF27G. R.A.G. and L.B. acknowledge the support from PLATO and GOLF CNES grants. S.M. acknowledges the support from the Ramon y Cajal fellowship number RYC-2015-17697. T.S.M. acknowledges support from a Visiting Fellowship at the Max Planck Institute for Solar System Research. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program.\r\n\r\nSoftware: KADACS (García et al. 2011), NumPy (van der Walt et al. 2011), SciPy (Jones et al. 2001), Matplotlib (Hunter 2007).\r\n\r\nFacilities: MAST - , Kepler Eclipsing Binary Catalog - , Exoplanet Archive. -","volume":244,"extern":"1","publication_status":"published","article_processing_charge":"No","date_created":"2022-07-19T09:21:58Z","title":"Surface rotation and photometric activity for Kepler targets. I. M and K main-sequence stars","intvolume":" 244","_id":"11623","scopus_import":"1","author":[{"full_name":"Santos, A. R. G.","last_name":"Santos","first_name":"A. R. G."},{"full_name":"García, R. A.","last_name":"García","first_name":"R. A."},{"last_name":"Mathur","first_name":"S.","full_name":"Mathur, S."},{"full_name":"Bugnet, Lisa Annabelle","orcid":"0000-0003-0142-4000","last_name":"Bugnet","first_name":"Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501"},{"last_name":"van Saders","first_name":"J. L.","full_name":"van Saders, J. L."},{"full_name":"Metcalfe, T. S.","last_name":"Metcalfe","first_name":"T. S."},{"full_name":"Simonian, G. V. A.","last_name":"Simonian","first_name":"G. V. A."},{"first_name":"M. H.","last_name":"Pinsonneault","full_name":"Pinsonneault, M. H."}],"issue":"1","publisher":"IOP Publishing","article_type":"original","quality_controlled":"1","publication_identifier":{"issn":["0067-0049"]},"oa":1,"date_published":"2019-09-19T00:00:00Z","type":"journal_article","main_file_link":[{"url":"https://arxiv.org/abs/1908.05222","open_access":"1"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","oa_version":"Preprint","month":"09","article_number":"21","publication":"The Astrophysical Journal Supplement Series","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","methods: data analysis","stars: activity","stars: low-mass","stars: rotation","starspots","techniques: photometric"]},{"language":[{"iso":"eng"}],"keyword":["asteroseismology","rotation","solar-like stars","kepler","machine learning","random forest"],"title":"Determining surface rotation periods of solar-like stars observed by the Kepler mission using machine learning techniques","month":"06","article_number":"1906.09609","oa_version":"Preprint","publication_status":"submitted","article_processing_charge":"No","date_created":"2022-07-20T11:18:53Z","author":[{"full_name":"Breton, S. N.","first_name":"S. N.","last_name":"Breton"},{"full_name":"Bugnet, Lisa Annabelle","orcid":"0000-0003-0142-4000","last_name":"Bugnet","first_name":"Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501"},{"full_name":"Santos, A. R. G.","first_name":"A. R. G.","last_name":"Santos"},{"full_name":"Saux, A. Le","first_name":"A. Le","last_name":"Saux"},{"first_name":"S.","last_name":"Mathur","full_name":"Mathur, S."},{"full_name":"Palle, P. L.","last_name":"Palle","first_name":"P. L."},{"full_name":"Garcia, R. A.","first_name":"R. A.","last_name":"Garcia"}],"_id":"11627","publication":"arXiv","extern":"1","status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"url":"https://arxiv.org/abs/1906.09609","open_access":"1"}],"abstract":[{"lang":"eng","text":"For a solar-like star, the surface rotation evolves with time, allowing in principle to estimate the age of a star from its surface rotation period. Here we are interested in measuring surface rotation periods of solar-like stars observed by the NASA mission Kepler. Different methods have been developed to track rotation signals in Kepler photometric light curves: time-frequency analysis based on wavelet techniques, autocorrelation and composite spectrum. We use the learning abilities of random forest classifiers to take decisions during two crucial steps of the analysis. First, given some input parameters, we discriminate the considered Kepler targets between rotating MS stars, non-rotating MS stars, red giants, binaries and pulsators. We then use a second classifier only on the MS rotating targets to decide the best data analysis treatment."}],"oa":1,"doi":"10.48550/arXiv.1906.09609","arxiv":1,"day":"23","date_published":"2019-06-23T00:00:00Z","type":"preprint","external_id":{"arxiv":["1906.09609"]},"date_updated":"2022-08-22T08:16:53Z","citation":{"short":"S.N. Breton, L.A. Bugnet, A.R.G. Santos, A.L. Saux, S. Mathur, P.L. Palle, R.A. Garcia, ArXiv (n.d.).","mla":"Breton, S. N., et al. “Determining Surface Rotation Periods of Solar-like Stars Observed by the Kepler Mission Using Machine Learning Techniques.” ArXiv, 1906.09609, doi:10.48550/arXiv.1906.09609.","ista":"Breton SN, Bugnet LA, Santos ARG, Saux AL, Mathur S, Palle PL, Garcia RA. Determining surface rotation periods of solar-like stars observed by the Kepler mission using machine learning techniques. arXiv, 1906.09609.","ama":"Breton SN, Bugnet LA, Santos ARG, et al. Determining surface rotation periods of solar-like stars observed by the Kepler mission using machine learning techniques. arXiv. doi:10.48550/arXiv.1906.09609","apa":"Breton, S. N., Bugnet, L. A., Santos, A. R. G., Saux, A. L., Mathur, S., Palle, P. L., & Garcia, R. A. (n.d.). Determining surface rotation periods of solar-like stars observed by the Kepler mission using machine learning techniques. arXiv. https://doi.org/10.48550/arXiv.1906.09609","ieee":"S. N. Breton et al., “Determining surface rotation periods of solar-like stars observed by the Kepler mission using machine learning techniques,” arXiv. .","chicago":"Breton, S. N., Lisa Annabelle Bugnet, A. R. G. Santos, A. Le Saux, S. Mathur, P. L. Palle, and R. A. Garcia. “Determining Surface Rotation Periods of Solar-like Stars Observed by the Kepler Mission Using Machine Learning Techniques.” ArXiv, n.d. https://doi.org/10.48550/arXiv.1906.09609."},"year":"2019"},{"main_file_link":[{"url":"https://doi.org/10.48550/arXiv.1906.09611","open_access":"1"}],"extern":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","date_updated":"2022-08-22T08:20:29Z","citation":{"ista":"Saux AL, Bugnet LA, Mathur S, Breton SN, Garcia RA. Automatic classification of K2 pulsating stars using machine learning techniques. arXiv, 1906.09611.","mla":"Saux, A. Le, et al. “Automatic Classification of K2 Pulsating Stars Using Machine Learning Techniques.” ArXiv, 1906.09611, doi:10.48550/arXiv.1906.09611.","short":"A.L. Saux, L.A. Bugnet, S. Mathur, S.N. Breton, R.A. Garcia, ArXiv (n.d.).","chicago":"Saux, A. Le, Lisa Annabelle Bugnet, S. Mathur, S. N. Breton, and R. A. Garcia. “Automatic Classification of K2 Pulsating Stars Using Machine Learning Techniques.” ArXiv, n.d. https://doi.org/10.48550/arXiv.1906.09611.","ieee":"A. L. Saux, L. A. Bugnet, S. Mathur, S. N. Breton, and R. A. Garcia, “Automatic classification of K2 pulsating stars using machine learning techniques,” arXiv. .","ama":"Saux AL, Bugnet LA, Mathur S, Breton SN, Garcia RA. Automatic classification of K2 pulsating stars using machine learning techniques. arXiv. doi:10.48550/arXiv.1906.09611","apa":"Saux, A. L., Bugnet, L. A., Mathur, S., Breton, S. N., & Garcia, R. A. (n.d.). Automatic classification of K2 pulsating stars using machine learning techniques. arXiv. https://doi.org/10.48550/arXiv.1906.09611"},"year":"2019","date_published":"2019-06-23T00:00:00Z","external_id":{"arxiv":["1906.09611"]},"type":"preprint","doi":"10.48550/arXiv.1906.09611","arxiv":1,"day":"23","abstract":[{"lang":"eng","text":"The second mission of NASA’s Kepler satellite, K2, has collected hundreds of thousands of lightcurves for stars close to the ecliptic plane. This new sample could increase the number of known pulsating stars and then improve our understanding of those stars. For the moment only a few stars have been properly classified and published. In this work, we present a method to automaticly classify K2 pulsating stars using a Machine Learning technique called Random Forest. The objective is to sort out the stars in four classes: red giant (RG), main-sequence Solar-like stars (SL), classical pulsators (PULS) and Other. To do this we use the effective temperatures and the luminosities of the stars as well as the FliPer features, that measures the amount of power contained in the power spectral density. The classifier now retrieves the right classification for more than 80% of the stars."}],"oa":1,"language":[{"iso":"eng"}],"keyword":["asteroseismology - methods","data analysis - thecniques","machine learning - stars","oscillations"],"_id":"11630","publication":"arXiv","author":[{"full_name":"Saux, A. Le","first_name":"A. Le","last_name":"Saux"},{"first_name":"Lisa Annabelle","last_name":"Bugnet","orcid":"0000-0003-0142-4000","full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501"},{"last_name":"Mathur","first_name":"S.","full_name":"Mathur, S."},{"full_name":"Breton, S. N.","last_name":"Breton","first_name":"S. N."},{"first_name":"R. A.","last_name":"Garcia","full_name":"Garcia, R. A."}],"oa_version":"Preprint","publication_status":"submitted","date_created":"2022-07-21T06:57:10Z","article_processing_charge":"No","month":"06","title":"Automatic classification of K2 pulsating stars using machine learning techniques","article_number":"1906.09611"},{"language":[{"iso":"eng"}],"page":"20","publisher":"Cold Spring Harbor Laboratory","author":[{"last_name":"Sulc","first_name":"Jonathan","full_name":"Sulc, Jonathan"},{"full_name":"Mounier, Ninon","last_name":"Mounier","first_name":"Ninon"},{"first_name":"Felix","last_name":"Günther","full_name":"Günther, Felix"},{"full_name":"Winkler, Thomas","first_name":"Thomas","last_name":"Winkler"},{"last_name":"Wood","first_name":"Andrew R.","full_name":"Wood, Andrew R."},{"full_name":"Frayling, Timothy M.","last_name":"Frayling","first_name":"Timothy M."},{"full_name":"Heid, Iris M.","first_name":"Iris M.","last_name":"Heid"},{"last_name":"Robinson","first_name":"Matthew Richard","full_name":"Robinson, Matthew Richard","orcid":"0000-0001-8982-8813","id":"E5D42276-F5DA-11E9-8E24-6303E6697425"},{"full_name":"Kutalik, Zoltán","first_name":"Zoltán","last_name":"Kutalik"}],"_id":"7782","publication":"bioRxiv","month":"06","title":"Maximum likelihood method quantifies the overall contribution of gene-environment interaction to continuous traits: An application to complex traits in the UK Biobank","article_processing_charge":"No","date_created":"2020-04-30T13:04:26Z","publication_status":"published","oa_version":"Preprint","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","extern":"1","main_file_link":[{"url":"https://doi.org/10.1101/632380 ","open_access":"1"}],"type":"preprint","date_published":"2019-06-14T00:00:00Z","year":"2019","citation":{"ista":"Sulc J, Mounier N, Günther F, Winkler T, Wood AR, Frayling TM, Heid IM, Robinson MR, Kutalik Z. 2019. Maximum likelihood method quantifies the overall contribution of gene-environment interaction to continuous traits: An application to complex traits in the UK Biobank. bioRxiv, .","short":"J. Sulc, N. Mounier, F. Günther, T. Winkler, A.R. Wood, T.M. Frayling, I.M. Heid, M.R. Robinson, Z. Kutalik, BioRxiv (2019).","mla":"Sulc, Jonathan, et al. “Maximum Likelihood Method Quantifies the Overall Contribution of Gene-Environment Interaction to Continuous Traits: An Application to Complex Traits in the UK Biobank.” BioRxiv, Cold Spring Harbor Laboratory, 2019.","ieee":"J. Sulc et al., “Maximum likelihood method quantifies the overall contribution of gene-environment interaction to continuous traits: An application to complex traits in the UK Biobank,” bioRxiv. Cold Spring Harbor Laboratory, 2019.","chicago":"Sulc, Jonathan, Ninon Mounier, Felix Günther, Thomas Winkler, Andrew R. Wood, Timothy M. Frayling, Iris M. Heid, Matthew Richard Robinson, and Zoltán Kutalik. “Maximum Likelihood Method Quantifies the Overall Contribution of Gene-Environment Interaction to Continuous Traits: An Application to Complex Traits in the UK Biobank.” BioRxiv. Cold Spring Harbor Laboratory, 2019.","apa":"Sulc, J., Mounier, N., Günther, F., Winkler, T., Wood, A. R., Frayling, T. M., … Kutalik, Z. (2019). Maximum likelihood method quantifies the overall contribution of gene-environment interaction to continuous traits: An application to complex traits in the UK Biobank. bioRxiv. Cold Spring Harbor Laboratory.","ama":"Sulc J, Mounier N, Günther F, et al. Maximum likelihood method quantifies the overall contribution of gene-environment interaction to continuous traits: An application to complex traits in the UK Biobank. bioRxiv. 2019."},"date_updated":"2021-01-12T08:15:30Z","oa":1,"abstract":[{"lang":"eng","text":"As genome-wide association studies (GWAS) increased in size, numerous gene-environment interactions (GxE) have been discovered, many of which however explore only one environment at a time and may suffer from statistical artefacts leading to biased interaction estimates. Here we propose a maximum likelihood method to estimate the contribution of GxE to complex traits taking into account all interacting environmental variables at the same time, without the need to measure any. This is possible because GxE induces fluctuations in the conditional trait variance, the extent of which depends on the strength of GxE. The approach can be applied to continuous outcomes and for single SNPs or genetic risk scores (GRS). Extensive simulations demonstrated that our method yields unbiased interaction estimates and excellent confidence interval coverage. We also offer a strategy to distinguish specific GxE from general heteroscedasticity (scale effects). Applying our method to 32 complex traits in the UK Biobank reveals that for body mass index (BMI) the GRSxE explains an additional 1.9% variance on top of the 5.2% GRS contribution. However, this interaction is not specific to the GRS and holds for any variable similarly correlated with BMI. On the contrary, the GRSxE interaction effect for leg impedance Embedded Image is significantly (P < 10−56) larger than it would be expected for a similarly correlated variable Embedded Image. We showed that our method could robustly detect the global contribution of GxE to complex traits, which turned out to be substantial for certain obesity measures."}],"day":"14"},{"department":[{"_id":"HeEd"},{"_id":"UlWa"},{"_id":"KrCh"}],"date_created":"2020-06-08T12:25:25Z","article_processing_charge":"No","publication_status":"submitted","oa_version":"Preprint","article_number":"1903.06981","title":"Token swapping on trees","month":"03","publication":"arXiv","_id":"7950","author":[{"last_name":"Biniaz","first_name":"Ahmad","full_name":"Biniaz, Ahmad"},{"full_name":"Jain, Kshitij","first_name":"Kshitij","last_name":"Jain"},{"last_name":"Lubiw","first_name":"Anna","full_name":"Lubiw, Anna"},{"id":"45CFE238-F248-11E8-B48F-1D18A9856A87","full_name":"Masárová, Zuzana","orcid":"0000-0002-6660-1322","last_name":"Masárová","first_name":"Zuzana"},{"full_name":"Miltzow, Tillmann","first_name":"Tillmann","last_name":"Miltzow"},{"first_name":"Debajyoti","last_name":"Mondal","full_name":"Mondal, Debajyoti"},{"first_name":"Anurag Murty","last_name":"Naredla","full_name":"Naredla, Anurag Murty"},{"first_name":"Josef","last_name":"Tkadlec","orcid":"0000-0002-1097-9684","full_name":"Tkadlec, Josef","id":"3F24CCC8-F248-11E8-B48F-1D18A9856A87"},{"full_name":"Turcotte, Alexi","last_name":"Turcotte","first_name":"Alexi"}],"language":[{"iso":"eng"}],"day":"16","arxiv":1,"oa":1,"abstract":[{"lang":"eng","text":"The input to the token swapping problem is a graph with vertices v1, v2, . . . , vn, and n tokens with labels 1,2, . . . , n, one on each vertex. The goal is to get token i to vertex vi for all i= 1, . . . , n using a minimum number of swaps, where a swap exchanges the tokens on the endpoints of an edge.Token swapping on a tree, also known as “sorting with a transposition tree,” is not known to be in P nor NP-complete. We present some partial results:\r\n1. An optimum swap sequence may need to perform a swap on a leaf vertex that has the correct token (a “happy leaf”), disproving a conjecture of Vaughan.\r\n2. Any algorithm that fixes happy leaves—as all known approximation algorithms for the problem do—has approximation factor at least 4/3. Furthermore, the two best-known 2-approximation algorithms have approximation factor exactly 2.\r\n3. A generalized problem—weighted coloured token swapping—is NP-complete on trees, but solvable in polynomial time on paths and stars. In this version, tokens and vertices have colours, and colours have weights. The goal is to get every token to a vertex of the same colour, and the cost of a swap is the sum of the weights of the two tokens involved."}],"year":"2019","citation":{"apa":"Biniaz, A., Jain, K., Lubiw, A., Masárová, Z., Miltzow, T., Mondal, D., … Turcotte, A. (n.d.). Token swapping on trees. arXiv.","ama":"Biniaz A, Jain K, Lubiw A, et al. Token swapping on trees. arXiv.","ieee":"A. Biniaz et al., “Token swapping on trees,” arXiv. .","chicago":"Biniaz, Ahmad, Kshitij Jain, Anna Lubiw, Zuzana Masárová, Tillmann Miltzow, Debajyoti Mondal, Anurag Murty Naredla, Josef Tkadlec, and Alexi Turcotte. “Token Swapping on Trees.” ArXiv, n.d.","short":"A. Biniaz, K. Jain, A. Lubiw, Z. Masárová, T. Miltzow, D. Mondal, A.M. Naredla, J. Tkadlec, A. Turcotte, ArXiv (n.d.).","mla":"Biniaz, Ahmad, et al. “Token Swapping on Trees.” ArXiv, 1903.06981.","ista":"Biniaz A, Jain K, Lubiw A, Masárová Z, Miltzow T, Mondal D, Naredla AM, Tkadlec J, Turcotte A. Token swapping on trees. arXiv, 1903.06981."},"date_updated":"2024-01-04T12:42:08Z","type":"preprint","external_id":{"arxiv":["1903.06981"]},"date_published":"2019-03-16T00:00:00Z","main_file_link":[{"url":"https://arxiv.org/abs/1903.06981","open_access":"1"}],"status":"public","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","related_material":{"record":[{"status":"public","relation":"dissertation_contains","id":"7944"},{"id":"12833","relation":"later_version","status":"public"}]}},{"acknowledgement":"This work was supported by INSERM, CNRS, UDS, Ligue Régionale contre le Cancer, Hôpital de Strasbourg, Association pour la Recherche sur le Cancer (ARC) and Agence Nationale de la Recherche (ANR) grants. P.B.C. was funded by the ANR and by the ARSEP (Fondation pour l'Aide à la Recherche sur la Sclérose en Plaques), and G.T. by governmental and ARC fellowships. This work was also supported by grants from the Ataxia UK (2491) and the NC3R (NC/L000199/1) awarded to M.F. The Institut de Génétique et de Biologie Moléculaire et Cellulaire was also supported by a French state fund through the ANR labex. D.E.S. was funded by Marie Curie Grant CIG 334077/IRTIM. We thank B. Altenhein, K. Brückner, M. Crozatier, L. Waltzer, M. Logan, E. Kurant, R. Reuter, E. Kurucz, J.L Dimarcq, J. Hoffmann, C. Goodman, the DHSB, and the BDSC for reagents and flies. We also thank all of the laboratory members for comments on the manuscript; C. Diebold, C. Delaporte, M. Pezze, the fly, and imaging and antibody facilities for technical assistance; and D. Dembele for help with statistics. In addition, we thank Alison Brewer for help with Luciferase assays.","volume":39,"ddc":["570"],"day":"09","doi":"10.1523/JNEUROSCI.1059-18.2018","abstract":[{"lang":"eng","text":"Despite their different origins, Drosophila glia and hemocytes are related cell populations that provide an immune function. Drosophila hemocytes patrol the body cavity and act as macrophages outside the nervous system whereas glia originate from the neuroepithelium and provide the scavenger population of the nervous system. Drosophila glia are hence the functional orthologs of vertebrate microglia, even though the latter are cells of immune origin that subsequently move into the brain during development. Interestingly, the Drosophila immune cells within (glia) and outside the nervous system (hemocytes) require the same transcription factor Glide/Gcm for their development. This raises the issue of how do glia specifically differentiate in the nervous system and hemocytes in the procephalic mesoderm. The Repo homeodomain transcription factor and pan-glial direct target of Glide/Gcm is known to ensure glial terminal differentiation. Here we show that Repo also takes center stage in the process that discriminates between glia and hemocytes. First, Repo expression is repressed in the hemocyte anlagen by mesoderm-specific factors. Second, Repo ectopic activation in the procephalic mesoderm is sufficient to repress the expression of hemocyte-specific genes. Third, the lack of Repo triggers the expression of hemocyte markers in glia. Thus, a complex network of tissue-specific cues biases the potential of Glide/Gcm. These data allow us to revise the concept of fate determinants and help us understand the bases of cell specification. Both sexes were analyzed.SIGNIFICANCE STATEMENTDistinct cell types often require the same pioneer transcription factor, raising the issue of how does one factor trigger different fates. In Drosophila, glia and hemocytes provide a scavenger activity within and outside the nervous system, respectively. While they both require the Glide/Gcm transcription factor, glia originate from the ectoderm, hemocytes from the mesoderm. Here we show that tissue-specific factors inhibit the gliogenic potential of Glide/Gcm in the mesoderm by repressing the expression of the homeodomain protein Repo, a major glial-specific target of Glide/Gcm. Repo expression in turn inhibits the expression of hemocyte-specific genes in the nervous system. These cell-specific networks secure the establishment of the glial fate only in the nervous system and allow cell diversification."}],"year":"2019","citation":{"ista":"Trébuchet G, Cattenoz PB, Zsámboki J, Mazaud D, Siekhaus DE, Fanto M, Giangrande A. 2019. The Repo homeodomain transcription factor suppresses hematopoiesis in Drosophila and preserves the glial fate. Journal of Neuroscience. 39(2), 238–255.","mla":"Trébuchet, Guillaume, et al. “The Repo Homeodomain Transcription Factor Suppresses Hematopoiesis in Drosophila and Preserves the Glial Fate.” Journal of Neuroscience, vol. 39, no. 2, Society for Neuroscience, 2019, pp. 238–55, doi:10.1523/JNEUROSCI.1059-18.2018.","short":"G. Trébuchet, P.B. Cattenoz, J. Zsámboki, D. Mazaud, D.E. Siekhaus, M. Fanto, A. Giangrande, Journal of Neuroscience 39 (2019) 238–255.","chicago":"Trébuchet, Guillaume, Pierre B Cattenoz, János Zsámboki, David Mazaud, Daria E Siekhaus, Manolis Fanto, and Angela Giangrande. “The Repo Homeodomain Transcription Factor Suppresses Hematopoiesis in Drosophila and Preserves the Glial Fate.” Journal of Neuroscience. Society for Neuroscience, 2019. https://doi.org/10.1523/JNEUROSCI.1059-18.2018.","ieee":"G. Trébuchet et al., “The Repo homeodomain transcription factor suppresses hematopoiesis in Drosophila and preserves the glial fate,” Journal of Neuroscience, vol. 39, no. 2. Society for Neuroscience, pp. 238–255, 2019.","ama":"Trébuchet G, Cattenoz PB, Zsámboki J, et al. The Repo homeodomain transcription factor suppresses hematopoiesis in Drosophila and preserves the glial fate. Journal of Neuroscience. 2019;39(2):238-255. doi:10.1523/JNEUROSCI.1059-18.2018","apa":"Trébuchet, G., Cattenoz, P. B., Zsámboki, J., Mazaud, D., Siekhaus, D. E., Fanto, M., & Giangrande, A. (2019). The Repo homeodomain transcription factor suppresses hematopoiesis in Drosophila and preserves the glial fate. Journal of Neuroscience. Society for Neuroscience. https://doi.org/10.1523/JNEUROSCI.1059-18.2018"},"date_updated":"2023-09-19T10:10:55Z","external_id":{"pmid":["30504274"],"isi":["000455189900006"]},"isi":1,"publisher":"Society for Neuroscience","article_type":"original","quality_controlled":"1","ec_funded":1,"page":"238-255","file_date_updated":"2020-10-02T09:33:28Z","article_processing_charge":"No","department":[{"_id":"DaSi"}],"date_created":"2018-12-11T11:44:07Z","publication_status":"published","intvolume":" 39","title":"The Repo homeodomain transcription factor suppresses hematopoiesis in Drosophila and preserves the glial fate","scopus_import":"1","_id":"8","pmid":1,"issue":"2","author":[{"last_name":"Trébuchet","first_name":"Guillaume","full_name":"Trébuchet, Guillaume"},{"full_name":"Cattenoz, Pierre B","last_name":"Cattenoz","first_name":"Pierre B"},{"full_name":"Zsámboki, János","last_name":"Zsámboki","first_name":"János"},{"first_name":"David","last_name":"Mazaud","full_name":"Mazaud, David"},{"first_name":"Daria E","last_name":"Siekhaus","orcid":"0000-0001-8323-8353","full_name":"Siekhaus, Daria E","id":"3D224B9E-F248-11E8-B48F-1D18A9856A87"},{"full_name":"Fanto, Manolis","last_name":"Fanto","first_name":"Manolis"},{"first_name":"Angela","last_name":"Giangrande","full_name":"Giangrande, Angela"}],"file":[{"date_updated":"2020-10-02T09:33:28Z","file_name":"2019_JournNeuroscience_Trebuchet.pdf","content_type":"application/pdf","date_created":"2020-10-02T09:33:28Z","file_size":9455414,"checksum":"8f6925eb4cd1e8747d8ea25929c68de6","file_id":"8596","creator":"dernst","success":1,"access_level":"open_access","relation":"main_file"}],"status":"public","user_id":"c635000d-4b10-11ee-a964-aac5a93f6ac1","oa":1,"publist_id":"8048","type":"journal_article","date_published":"2019-01-09T00:00:00Z","language":[{"iso":"eng"}],"project":[{"_id":"2536F660-B435-11E9-9278-68D0E5697425","call_identifier":"FP7","grant_number":"334077","name":"Investigating the role of transporters in invasive migration through junctions"}],"oa_version":"Published Version","month":"01","has_accepted_license":"1","publication":"Journal of Neuroscience"},{"file_date_updated":"2020-07-14T12:48:07Z","page":"723-776","quality_controlled":"1","ec_funded":1,"article_type":"original","publisher":"Springer","author":[{"id":"4DA65CD0-F248-11E8-B48F-1D18A9856A87","full_name":"Deuchert, Andreas","orcid":"0000-0003-3146-6746","last_name":"Deuchert","first_name":"Andreas"},{"orcid":"0000-0002-6781-0521","full_name":"Seiringer, Robert","first_name":"Robert","last_name":"Seiringer","id":"4AFD0470-F248-11E8-B48F-1D18A9856A87"},{"full_name":"Yngvason, Jakob","first_name":"Jakob","last_name":"Yngvason"}],"issue":"2","_id":"80","scopus_import":"1","title":"Bose–Einstein condensation in a dilute, trapped gas at positive temperature","intvolume":" 368","publication_status":"published","date_created":"2018-12-11T11:44:31Z","department":[{"_id":"RoSe"}],"article_processing_charge":"Yes (via OA deal)","ddc":["530"],"volume":368,"isi":1,"external_id":{"isi":["000467796800007"]},"date_updated":"2023-08-24T14:27:51Z","year":"2019","citation":{"chicago":"Deuchert, Andreas, Robert Seiringer, and Jakob Yngvason. “Bose–Einstein Condensation in a Dilute, Trapped Gas at Positive Temperature.” Communications in Mathematical Physics. Springer, 2019. https://doi.org/10.1007/s00220-018-3239-0.","ieee":"A. Deuchert, R. Seiringer, and J. Yngvason, “Bose–Einstein condensation in a dilute, trapped gas at positive temperature,” Communications in Mathematical Physics, vol. 368, no. 2. Springer, pp. 723–776, 2019.","ama":"Deuchert A, Seiringer R, Yngvason J. Bose–Einstein condensation in a dilute, trapped gas at positive temperature. Communications in Mathematical Physics. 2019;368(2):723-776. doi:10.1007/s00220-018-3239-0","apa":"Deuchert, A., Seiringer, R., & Yngvason, J. (2019). Bose–Einstein condensation in a dilute, trapped gas at positive temperature. Communications in Mathematical Physics. Springer. https://doi.org/10.1007/s00220-018-3239-0","ista":"Deuchert A, Seiringer R, Yngvason J. 2019. Bose–Einstein condensation in a dilute, trapped gas at positive temperature. Communications in Mathematical Physics. 368(2), 723–776.","short":"A. Deuchert, R. Seiringer, J. Yngvason, Communications in Mathematical Physics 368 (2019) 723–776.","mla":"Deuchert, Andreas, et al. “Bose–Einstein Condensation in a Dilute, Trapped Gas at Positive Temperature.” Communications in Mathematical Physics, vol. 368, no. 2, Springer, 2019, pp. 723–76, doi:10.1007/s00220-018-3239-0."},"abstract":[{"lang":"eng","text":"We consider an interacting, dilute Bose gas trapped in a harmonic potential at a positive temperature. The system is analyzed in a combination of a thermodynamic and a Gross–Pitaevskii (GP) limit where the trap frequency ω, the temperature T, and the particle number N are related by N∼ (T/ ω) 3→ ∞ while the scattering length is so small that the interaction energy per particle around the center of the trap is of the same order of magnitude as the spectral gap in the trap. We prove that the difference between the canonical free energy of the interacting gas and the one of the noninteracting system can be obtained by minimizing the GP energy functional. We also prove Bose–Einstein condensation in the following sense: The one-particle density matrix of any approximate minimizer of the canonical free energy functional is to leading order given by that of the noninteracting gas but with the free condensate wavefunction replaced by the GP minimizer."}],"doi":"10.1007/s00220-018-3239-0","day":"01","language":[{"iso":"eng"}],"publication":"Communications in Mathematical Physics","has_accepted_license":"1","month":"06","oa_version":"Published Version","project":[{"grant_number":"694227","name":"Analysis of quantum many-body systems","call_identifier":"H2020","_id":"25C6DC12-B435-11E9-9278-68D0E5697425"},{"_id":"25C878CE-B435-11E9-9278-68D0E5697425","call_identifier":"FWF","name":"Structure of the Excitation Spectrum for Many-Body Quantum Systems","grant_number":"P27533_N27"}],"user_id":"4359f0d1-fa6c-11eb-b949-802e58b17ae8","status":"public","file":[{"creator":"dernst","file_id":"5688","relation":"main_file","access_level":"open_access","content_type":"application/pdf","file_name":"2018_CommunMathPhys_Deuchert.pdf","date_updated":"2020-07-14T12:48:07Z","file_size":893902,"checksum":"c7e9880b43ac726712c1365e9f2f73a6","date_created":"2018-12-17T10:34:06Z"}],"date_published":"2019-06-01T00:00:00Z","type":"journal_article","tmp":{"legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"publist_id":"7974","oa":1},{"file_date_updated":"2020-07-14T12:48:08Z","quality_controlled":"1","article_type":"original","publisher":"Public Library of Science","author":[{"full_name":"Currin, Christopher B.","last_name":"Currin","first_name":"Christopher B."},{"last_name":"Khoza","first_name":"Phumlani N.","full_name":"Khoza, Phumlani N."},{"full_name":"Antrobus, Alexander D.","last_name":"Antrobus","first_name":"Alexander D."},{"first_name":"Peter E.","last_name":"Latham","full_name":"Latham, Peter E."},{"orcid":"0000-0003-3295-6181","full_name":"Vogels, Tim P","first_name":"Tim P","last_name":"Vogels","id":"CB6FF8D2-008F-11EA-8E08-2637E6697425"},{"first_name":"Joseph V.","last_name":"Raimondo","full_name":"Raimondo, Joseph V."}],"issue":"7","pmid":1,"_id":"8013","title":"Think: Theory for Africa","intvolume":" 15","publication_status":"published","article_processing_charge":"No","date_created":"2020-06-25T12:50:39Z","extern":"1","ddc":["570"],"volume":15,"external_id":{"pmid":["31295253"]},"date_updated":"2021-01-12T08:16:31Z","citation":{"apa":"Currin, C. B., Khoza, P. N., Antrobus, A. D., Latham, P. E., Vogels, T. P., & Raimondo, J. V. (2019). Think: Theory for Africa. PLOS Computational Biology. Public Library of Science. https://doi.org/10.1371/journal.pcbi.1007049","ama":"Currin CB, Khoza PN, Antrobus AD, Latham PE, Vogels TP, Raimondo JV. Think: Theory for Africa. PLOS Computational Biology. 2019;15(7). doi:10.1371/journal.pcbi.1007049","chicago":"Currin, Christopher B., Phumlani N. Khoza, Alexander D. Antrobus, Peter E. Latham, Tim P Vogels, and Joseph V. Raimondo. “Think: Theory for Africa.” PLOS Computational Biology. Public Library of Science, 2019. https://doi.org/10.1371/journal.pcbi.1007049.","ieee":"C. B. Currin, P. N. Khoza, A. D. Antrobus, P. E. Latham, T. P. Vogels, and J. V. Raimondo, “Think: Theory for Africa,” PLOS Computational Biology, vol. 15, no. 7. Public Library of Science, 2019.","short":"C.B. Currin, P.N. Khoza, A.D. Antrobus, P.E. Latham, T.P. Vogels, J.V. Raimondo, PLOS Computational Biology 15 (2019).","mla":"Currin, Christopher B., et al. “Think: Theory for Africa.” PLOS Computational Biology, vol. 15, no. 7, e1007049, Public Library of Science, 2019, doi:10.1371/journal.pcbi.1007049.","ista":"Currin CB, Khoza PN, Antrobus AD, Latham PE, Vogels TP, Raimondo JV. 2019. Think: Theory for Africa. PLOS Computational Biology. 15(7), e1007049."},"year":"2019","doi":"10.1371/journal.pcbi.1007049","day":"11","language":[{"iso":"eng"}],"publication":"PLOS Computational Biology","has_accepted_license":"1","month":"07","article_number":"e1007049","oa_version":"Published Version","user_id":"D865714E-FA4E-11E9-B85B-F5C5E5697425","status":"public","file":[{"file_id":"8079","creator":"cziletti","relation":"main_file","access_level":"open_access","date_updated":"2020-07-14T12:48:08Z","content_type":"application/pdf","file_name":"2019_PlosCompBio_Currin.pdf","date_created":"2020-07-02T12:22:57Z","file_size":773969,"checksum":"723bdfb6ee5c747cbbb32baf01d17fad"}],"date_published":"2019-07-11T00:00:00Z","type":"journal_article","tmp":{"legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"oa":1,"publication_identifier":{"issn":["1553-7358"]}},{"publication":"Neuroscience and Biobehavioral Reviews","has_accepted_license":"1","month":"06","oa_version":"Published Version","language":[{"iso":"eng"}],"date_published":"2019-06-01T00:00:00Z","type":"journal_article","tmp":{"legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","image":"/images/cc_by.png","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"oa":1,"publication_identifier":{"issn":["0149-7634"]},"user_id":"D865714E-FA4E-11E9-B85B-F5C5E5697425","status":"public","file":[{"creator":"cziletti","file_id":"8080","access_level":"open_access","relation":"main_file","content_type":"application/pdf","file_name":"2019_NeurosBiobehavRev_Manohar.pdf","date_updated":"2020-07-14T12:48:08Z","file_size":1754418,"checksum":"7b972e3d6f7bb3122c8c5648f44e60ca","date_created":"2020-07-02T13:17:52Z"}],"main_file_link":[{"url":"https://doi.org/10.1101/233007 ","open_access":"1"}],"author":[{"full_name":"Manohar, Sanjay G.","last_name":"Manohar","first_name":"Sanjay G."},{"first_name":"Nahid","last_name":"Zokaei","full_name":"Zokaei, Nahid"},{"full_name":"Fallon, Sean J.","last_name":"Fallon","first_name":"Sean J."},{"id":"CB6FF8D2-008F-11EA-8E08-2637E6697425","last_name":"Vogels","first_name":"Tim P","full_name":"Vogels, Tim P","orcid":"0000-0003-3295-6181"},{"last_name":"Husain","first_name":"Masud","full_name":"Husain, Masud"}],"_id":"8014","pmid":1,"title":"Neural mechanisms of attending to items in working memory","intvolume":" 101","publication_status":"published","date_created":"2020-06-25T12:52:13Z","article_processing_charge":"No","file_date_updated":"2020-07-14T12:48:08Z","page":"1-12","quality_controlled":"1","article_type":"original","publisher":"Elsevier ","external_id":{"pmid":["30922977"]},"date_updated":"2021-01-12T08:16:31Z","year":"2019","citation":{"ista":"Manohar SG, Zokaei N, Fallon SJ, Vogels TP, Husain M. 2019. Neural mechanisms of attending to items in working memory. Neuroscience and Biobehavioral Reviews. 101, 1–12.","mla":"Manohar, Sanjay G., et al. “Neural Mechanisms of Attending to Items in Working Memory.” Neuroscience and Biobehavioral Reviews, vol. 101, Elsevier , 2019, pp. 1–12, doi:10.1016/j.neubiorev.2019.03.017.","short":"S.G. Manohar, N. Zokaei, S.J. Fallon, T.P. Vogels, M. Husain, Neuroscience and Biobehavioral Reviews 101 (2019) 1–12.","ieee":"S. G. Manohar, N. Zokaei, S. J. Fallon, T. P. Vogels, and M. Husain, “Neural mechanisms of attending to items in working memory,” Neuroscience and Biobehavioral Reviews, vol. 101. Elsevier , pp. 1–12, 2019.","chicago":"Manohar, Sanjay G., Nahid Zokaei, Sean J. Fallon, Tim P Vogels, and Masud Husain. “Neural Mechanisms of Attending to Items in Working Memory.” Neuroscience and Biobehavioral Reviews. Elsevier , 2019. https://doi.org/10.1016/j.neubiorev.2019.03.017.","ama":"Manohar SG, Zokaei N, Fallon SJ, Vogels TP, Husain M. Neural mechanisms of attending to items in working memory. Neuroscience and Biobehavioral Reviews. 2019;101:1-12. doi:10.1016/j.neubiorev.2019.03.017","apa":"Manohar, S. G., Zokaei, N., Fallon, S. J., Vogels, T. P., & Husain, M. (2019). Neural mechanisms of attending to items in working memory. Neuroscience and Biobehavioral Reviews. Elsevier . https://doi.org/10.1016/j.neubiorev.2019.03.017"},"abstract":[{"text":"Working memory, the ability to keep recently accessed information available for immediate manipulation, has been proposed to rely on two mechanisms that appear difficult to reconcile: self-sustained neural firing, or the opposite—activity-silent synaptic traces. Here we review and contrast models of these two mechanisms, and then show that both phenomena can co-exist within a unified system in which neurons hold information in both activity and synapses. Rapid plasticity in flexibly-coding neurons allows features to be bound together into objects, with an important emergent property being the focus of attention. One memory item is held by persistent activity in an attended or “focused” state, and is thus remembered better than other items. Other, previously attended items can remain in memory but in the background, encoded in activity-silent synaptic traces. This dual functional architecture provides a unified common mechanism accounting for a diversity of perplexing attention and memory effects that have been hitherto difficult to explain in a single theoretical framework.","lang":"eng"}],"doi":"10.1016/j.neubiorev.2019.03.017","day":"01","extern":"1","ddc":["570"],"volume":101}]