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1. Kinematics and multiband period–luminosity–metallicity relation of RR Lyrae stars via statistical parallax

Author: T D Muhie, A K Dambis, L N Berdnikov, A Y Kniazev, and E K Grebel
Published: 2021
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2. H α morphologies of star clusters: a LEGUS study of H ii region evolution time-scales and stochasticity in low-mass clusters

Author: Stephen Hannon, Janice C Lee, B C Whitmore, R Chandar, A Adamo, B Mobasher, A Aloisi, D Calzetti, M Cignoni, D O Cook, D Dale, S Deger, L Della Bruna, D M Elmegreen, D A Gouliermis, K Grasha, E K Grebel, A Herrero, D A Hunter, K E Johnson, R Kennicutt, H Kim, E Sacchi, L Smith, D Thilker, J Turner, R A M Walterbos, and A Wofford
Published: 2019
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3. TYC 8606-2025-1: a mild barium star surrounded by the ejecta of a very late thermal pulse

Author: V V Gvaramadze, Yu V Pakhomov, A Y Kniazev, T A Ryabchikova, N Langer, L Fossati, and E K Grebel
Published: 2019
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4. Star cluster catalogues for the LEGUS dwarf galaxies

Author: D O Cook, J C Lee, A Adamo, H Kim, R Chandar, B C Whitmore, A Mok, J E Ryon, D A Dale, D Calzetti, J E Andrews, A Aloisi, G Ashworth, S N Bright, T M Brown, C Christian, M Cignoni, G C Clayton, R da Silva, S E de Mink, C L Dobbs, B G Elmegreen, D M Elmegreen, A S Evans, M Fumagalli, J S Gallagher, D A Gouliermis, K Grasha, E K Grebel, A Herrero, D A Hunter, E I Jensen, K E Johnson, L Kahre, R C Kennicutt, M R Krumholz, N J Lee, D Lennon, S Linden, C Martin, M Messa, P Nair, A Nota, G Östlin, R C Parziale, A Pellerin, M W Regan, E Sabbi, E Sacchi, D Schaerer, D Schiminovich, F Shabani, F A Slane, J Small, C L Smith, L J Smith, S Taibi, D A Thilker, I C de la Torre, M Tosi, J A Turner, L Ubeda, S D Van Dyk, R AM Walterbos, and A Wofford
Published: 2019
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5. The spatial relation between young star clusters and molecular clouds in M51 with LEGUS

Author: K Grasha, D Calzetti, A Adamo, R C Kennicutt, B G Elmegreen, M Messa, D A Dale, K Fedorenko, S Mahadevan, E K Grebel, M Fumagalli, H Kim, C L Dobbs, D A Gouliermis, G Ashworth, J S Gallagher, L J Smith, M Tosi, B C Whitmore, E Schinnerer, D Colombo, A Hughes, A K Leroy, and S E Meidt
Published: 2018
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6. Milky Way archaeology using RR Lyrae and type II Cepheids. II. High-velocity RR Lyrae stars and Milky Way mass

Author: Z. Prudil, A. J. Koch-Hansen, B. Lemasle, E. K. Grebel, T. Marchetti, C. J. Hansen, J. Crestani, V. F. Braga, G. Bono, B. Chaboyer, M. Fabrizio, M. Dall’Ora, and C. E. Martínez-Vázquez
Subjects: Space and Planetary Science, Settore FIS/05, Astronomy and Astrophysics
Abstract: We report the discovery of high-velocity candidates among RR Lyrae stars found in the Milky Way halo. We identified nine RR Lyrae stars with Galactocentric velocities exceeding the local escape velocity based on the assumed Galaxy potential. Furthermore, based on a close examination of their orbits’, we ruled out their ejection location in the Milky Way disk and bulge. The spatial distribution revealed that seven out of nine pulsators overlap with the position of the Sagittarius stellar stream. Two out of these seven RR Lyrae stars can be tentatively linked to the Sagittarius dwarf spheroidal galaxy on the basis of their orbits. Focusing on the high-velocity tail of the RR Lyrae velocity distribution, we estimated the escape velocity in the Solar neighborhood to be vesc = 512−37+94 km s−1 (4 to 12 kpc); and beyond the Solar neighborhood as vesc = 436−22+44 km s−1 and vesc = 393−26+53 km s−1 (for distances between 12 to 20 kpc and 20 to 28 kpc), respectively. We utilized three escape velocity estimates together with the local circular velocity to estimate the Milky Way mass. The resulting measurement M200 = 0.83−0.16+0.29 × 1012 M⊙ falls on the lower end of the current Milky Way mass estimates, but once corrected for the likely bias in the escape velocity (an increase of approximately 10% in terms of the escape velocity), our mass estimate yields M200 = 1.26−0.22+0.40 × 1012 M⊙, which is in agreement with estimates based on different diagnostics of the Milky Way (MW) mass. The MW mass of within 20 kpc then corresponds to MMW(r −0.1+0.2 × 1011 M⊙ without any correction for bias, and MMW(r −0.1+0.2 × 1011 M⊙ corrected for a likely offset in escape velocities.
Published: 2022

7. The Gaia-ESO Public Spectroscopic Survey: Motivation, implementation, GIRAFFE data processing, analysis, and final data products

Author: G. Gilmore, S. Randich, C. C. Worley, A. Hourihane, A. Gonneau, G. G. Sacco, J. R. Lewis, L. Magrini, P. François, R. D. Jeffries, S. E. Koposov, A. Bragaglia, E. J. Alfaro, C. Allende Prieto, R. Blomme, A. J. Korn, A. C. Lanzafame, E. Pancino, A. Recio-Blanco, R. Smiljanic, S. Van Eck, T. Zwitter, T. Bensby, E. Flaccomio, M. J. Irwin, E. Franciosini, L. Morbidelli, F. Damiani, R. Bonito, E. D. Friel, J. S. Vink, L. Prisinzano, U. Abbas, D. Hatzidimitriou, E. V. Held, C. Jordi, E. Paunzen, A. Spagna, R. J. Jackson, J. Maíz Apellániz, M. Asplund, P. Bonifacio, S. Feltzing, J. Binney, J. Drew, A. M. N. Ferguson, G. Micela, I. Negueruela, T. Prusti, H.-W. Rix, A. Vallenari, M. Bergemann, A. R. Casey, P. de Laverny, A. Frasca, V. Hill, K. Lind, L. Sbordone, S. G. Sousa, V. Adibekyan, E. Caffau, S. Daflon, D. K. Feuillet, M. Gebran, J. I. Gonzalez Hernandez, G. Guiglion, A. Herrero, A. Lobel, T. Merle, Š. Mikolaitis, D. Montes, T. Morel, G. Ruchti, C. Soubiran, H. M. Tabernero, G. Tautvaišienė, G. Traven, M. Valentini, M. Van der Swaelmen, S. Villanova, C. Viscasillas Vázquez, A. Bayo, K. Biazzo, G. Carraro, B. Edvardsson, U. Heiter, P. Jofré, G. Marconi, C. Martayan, T. Masseron, L. Monaco, N. A. Walton, S. Zaggia, V. Aguirre Børsen-Koch, J. Alves, L. Balaguer-Nunez, P. S. Barklem, D. Barrado, M. Bellazzini, S. R. Berlanas, A. S. Binks, A. Bressan, R. Capuzzo-Dolcetta, L. Casagrande, L. Casamiquela, R. S. Collins, V. D'Orazi, M. L. L. Dantas, V. P. Debattista, E. Delgado-Mena, P. Di Marcantonio, A. Drazdauskas, N. W. Evans, B. Famaey, M. Franchini, Y. Frémat, X. Fu, D. Geisler, O. Gerhard, E. A. González Solares, E. K. Grebel, M. L. Gutiérrez Albarrán, F. Jiménez-Esteban, H. Jönsson, T. Khachaturyants, G. Kordopatis, J. Kos, N. Lagarde, H.-G. Ludwig, L. Mahy, M. Mapelli, E. Marfil, S. L. Martell, S. Messina, A. Miglio, I. Minchev, A. Moitinho, J. Montalban, M. J. P. F. G. Monteiro, C. Morossi, N. Mowlavi, A. Mucciarelli, D. N. A. Murphy, N. Nardetto, S. Ortolani, F. Paletou, J. Palouš, J. C. Pickering, A. Quirrenbach, P. Re Fiorentin, J. I. Read, D. Romano, N. Ryde, N. Sanna, W. Santos, G. M. Seabroke, L. Spina, M. Steinmetz, E. Stonkuté, E. Sutorius, F. Thévenin, M. Tosi, M. Tsantaki, N. Wright, R. F. G. Wyse, M. Zoccali, J. Zorec, D. B. Zucker, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Universidad de Alicante. Departamento de Física Aplicada, Astrofísica Estelar (AE), Ministerio de Ciencia e Innovación (España), European Commission, European Research Council, and German Research Foundation
Subjects: stars, astro-ph.SR, stars: abundances, astro-ph.GA, kinematics and dynamics, FOS: Physical sciences, Surveys, CHEMICAL-COMPOSITION, STELLAR SPECTRA, stellar content, spectroscopic, methods, spectroscopic [Techniques], Astronomi, astrofysik och kosmologi, surveys, Astronomy, Astrophysics and Cosmology, stellar content [Galaxy], observational [Methods], observational, EQUIVALENT WIDTHS, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), Earth and Planetary Astrophysics (astro-ph.EP), CALIBRATION, DWARF SPHEROIDAL GALAXY, Galaxy: stellar content, abundances, BLUE STARS, Astronomy and Astrophysics, kinematics and dynamics [Galaxy], Astrophysics - Astrophysics of Galaxies, EVOLUTION, NLTE-MODELS, Galaxy, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), abundances [Stars], astro-ph.EP, BLANKETED MODEL ATMOSPHERES, methods: observational, techniques, Astrophysics - Instrumentation and Methods for Astrophysics, Galaxy: kinematics and dynamics, techniques: spectroscopic, FGK BENCHMARK STARS, astro-ph.IM, Astrophysics - Earth and Planetary Astrophysics
Abstract: Full list of authors: Gilmore, G.; Randich, S.; Worley, C. C.; Hourihane, A.; Gonneau, A.; Sacco, G. G.; Lewis, J. R.; Magrini, L.; Francois, P.; Jeffries, R. D.; Koposov, S. E.; Bragaglia, A.; Alfaro, E. J.; Allende Prieto, C.; Blomme, R.; Korn, A. J.; Lanzafame, A. C.; Pancino, E.; Recio-Blanco, A.; Smiljanic, R.; Van Eck, S.; Zwitter, T.; Bensby, T.; Flaccomio, E.; Irwin, M. J.; Franciosini, E.; Morbidelli, L.; Damiani, F.; Bonito, R.; Friel, E. D.; Vink, J. S.; Prisinzano, L.; Abbas, U.; Hatzidimitriou, D.; Held, E., V; Jordi, C.; Paunzen, E.; Spagna, A.; Jackson, R. J.; Maiz Apellaniz, J.; Asplund, M.; Bonifacio, P.; Feltzing, S.; Binney, J.; Drew, J.; Ferguson, A. M. N.; Micela, G.; Negueruela, I; Prusti, T.; Rix, H-W; Vallenari, A.; Bergemann, M.; Casey, A. R.; de Laverny, P.; Frasca, A.; Hill, V; Lind, K.; Sbordone, L.; Sousa, S. G.; Adibekyan, V; Caffau, E.; Daflon, S.; Feuillet, D. K.; Gebran, M.; Gonzalez Hernandez, J., I; Guiglion, G.; Herrero, A.; Lobel, A.; Montes, D.; Morel, T.; Ruchti, G.; Soubiran, C.; Tabernero, H. M.; Tautvaisiene, G.; Traven, G.; Valentini, M.; Van der Swaelmen, M.; Villanova, S.; Vazquez, C. Viscasillas; Bayo, A.; Biazzo, K.; Carraro, G.; Edvardsson, B.; Heiter, U.; Jofre, P.; Marconi, G.; Martayan, C.; Masseron, T.; Monaco, L.; Walton, N. A.; Zaggia, S.; Borsen-Koch, V. Aguirre; Alves, J.; Balaguer-Nunez, L.; Barklem, P. S.; Barrado, D.; Bellazzini, M.; Berlanas, S. R.; Binks, A. S.; Bressan, A.; Capuzzo-Dolcetta, R.; Casagrande, L.; Casamiquela, L.; Collins, R. S.; D'Orazi, V; Dantas, M. L. L.; Debattista, V. P.; Delgado-Mena, E.; Di Marcantonio, P.; Drazdauskas, A.; Evans, N. W.; Famaey, B.; Franchini, M.; Fremat, Y.; Fu, X.; Geisler, D.; Gerhard, O.; Solares, E. A. Gonzalez; Grebel, E. K.; Gutierrez Albarran, M. L.; Jimenez-Esteban, F.; Jonsson, H.; Khachaturyants, T.; Kordopatis, G.; Kos, J.; Lagarde, N.; Ludwig, H-G; Mahy, L.; Mapelli, M.; Marfil, E.; Martell, S. L.; Messina, S.; Miglio, A.; Minchev, I; Moitinho, A.; Montalban, J.; Monteiro, M. J. P. F. G.; Morossi, C.; Mowlavi, N.; Mucciarelli, A.; Murphy, D. N. A.; Nardetto, N.; Ortolani, S.; Paletou, F.; Palous, J.; Pickering, J. C.; Quirrenbach, A.; Fiorentin, P. Re; Read, J., I; Romano, D.; Ryde, N.; Sanna, N.; Santos, W.; Seabroke, G. M.; Spina, L.; Steinmetz, M.; Stonkute, E.; Sutorius, E.; Thevenin, F.; Tosi, M.; Tsantaki, M.; Wright, N.; Wyse, R. F. G.; Zoccali, M.; Zorec, J.; Zucker, D. B.-- This is an Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited., Context. The Gaia-ESO Public Spectroscopic Survey is an ambitious project designed to obtain astrophysical parameters and elemental abundances for 100 000 stars, including large representative samples of the stellar populations in the Galaxy, and a well-defined sample of 60 (plus 20 archive) open clusters. We provide internally consistent results calibrated on benchmark stars and star clusters, extending across a very wide range of abundances and ages. This provides a legacy data set of intrinsic value, and equally a large wide-ranging dataset that is of value for the homogenisation of other and future stellar surveys and Gaia's astrophysical parameters. Aims. This article provides an overview of the survey methodology, the scientific aims, and the implementation, including a description of the data processing for the GIRAFFE spectra. A companion paper introduces the survey results. Methods. Gaia-ESO aspires to quantify both random and systematic contributions to measurement uncertainties. Thus, all available spectroscopic analysis techniques are utilised, each spectrum being analysed by up to several different analysis pipelines, with considerable effort being made to homogenise and calibrate the resulting parameters. We describe here the sequence of activities up to delivery of processed data products to the ESO Science Archive Facility for open use. Results. The Gaia-ESO Survey obtained 202 000 spectra of 115 000 stars using 340 allocated VLT nights between December 2011 and January 2018 from GIRAFFE and UVES. © G. Gilmore et al. 2022. Conclusions. The full consistently reduced final data set of spectra was released through the ESO Science Archive Facility in late 2020, with the full astrophysical parameters sets following in 2022. A companion article reviews the survey implementation, scientific highlights, the open cluster survey, and data products., Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 188.B-3002. These data products have been processed by the Cambridge Astronomy Survey Unit (CASU) at the Institute of Astronomy, University of Cambridge, and by the FLAMES/UVES reduction team at INAF/Osservatorio Astrofisico di Arcetri. Public access to the data products is via the ESO SAF, and the Gaia-ESO Survey Data Archive, prepared and hosted by the Wide Field Astronomy Unit, Institute for Astronomy, University of Edinburgh, which is funded by the UK Science and Technology Facilities Council. This work was partly supported by the European Union FP7 programme through ERC grant number 320360 and by the Leverhulme Trust through grant RPG-2012-541. We acknowledge the support from INAF and Ministero dell’ Istruzione, dell’ Università’ e della Ricerca (MIUR) in the form of the grant “Premiale VLT 2012”. The project presented here benefited in development from discussions held during the Gaia-ESO workshops and conferences supported by the ESF (European Science Foundation) through the GREAT Research Network Programme. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. R.S. acknowledges support from the National Science Centre, Poland (2014/15/B/ST9/03981). This work was partly supported by the INAF grant for mainstream projects: “Enhancing the legacy of the Gaia-ESO Survey for open cluster science”. F.J.E. acknowledges financial support from the Spanish MINECO/FEDER through the grant AYA2017-84089 and MDM-2017-0737 at Centro de Astrobiología (CSIC-INTA), Unidad de Excelencia María de Maeztu, and from the European Union’s Horizon 2020 research and innovation programme under Grant Agreement no. 824064 through the ESCAPE – the European Science Cluster of Astronomy and Particle Physics ESFRI Research Infrastructures project. T.B. was funded by the “The New Milky Way” project grant from the Knut and Alice Wallenberg Foundation. S.R.B. acknowledges support by the Spanish Government under grants AYA2015-68012-C2-2-P and PGC2018-093741-B-C21/C22 (MICIU/AEI/FEDER, UE). W.J.S. acknowledges CAPES for a PhD studentship. J.M.A. acknowledges support from the Spanish Government Ministerio de Ciencia e Innovación through grants AYA2013-40611-P, AYA2016-75931-C2-2-P, and PGC2018-095049-B-C22. T.M. and others from STAR institute, Liege, Belgium are grateful to Belgian F.R.S.-FNRS for support, and are also indebted for an ESA/PRODEX Belspo contract related to the Gaia Data Processing and Analysis Consortium and for support through an ARC grant for Concerted Research Actions financed by the Federation Wallonie-Brussels.. This research has been partially supported by the following grants: MIUR Premiale “Gaia-ESO survey” (PI S. Randich), MIUR Premiale “MiTiC: Mining the Cosmos” (PI B. Garilli), the ASI-INAF contract 2014-049-R.O: “Realizzazione attività tecniche/scientifiche presso ASDC” (PI Angelo Antonelli), Fondazione Cassa di Risparmio di Firenze, progetto: “Know the star, know the planet” (PI E. Pancino), and Progetto Main Stream INAF: “Chemo-dynamics of globular clusters: the Gaia revolution” (PI E. Pancino). V.A. acknowledges the support from Fundação para a Ciência e Tecnologia (FCT) through Investigador FCT contract nr. IF/00650/2015/CP1273/CT0001. A.J.K. acknowledges support by the Swedish National Space Agency (SNSA). A.B. acknowledges support by ANID, – Millennium Science Initiative Program – NCN19_171, and FONDECYT regular 1190748. E.M. acknowledges financial support from the Spanish State Research Agency (AEI) through project MDM-2017-0737 Unidad de Excelencia “María de Maeztu” – Centro de Astrobiología (CSIC-INTA). T.Z. acknowledges financial support of the Slovenian Research Agency (research core funding no. P1-0188) and the European Space Agency (Prodex Experiment Arrangement No. C4000127986). P.J. acknowledges support FONDECYT Regular 1200703. The work of I.N. is partially supported by the Spanish Government Ministerio de Ciencia, Innovación y Universidades under grant PGC2018-093741-B-C21 (MICIU/AEI/FEDER, UE). Funding for this work has been provided by the ARC Future Fellowship FT160100402. C.A.P. acknowledges financial support from the Spanish Government through research grants MINECO AYA 2014-56359-P, MINECO AYA2017-86389-P, and MICINN PID2020-117493GB-I00. S.F. was supported by the grants 2011-5042 and 2016-03412 from the Swedish Research Council and the project grant “The New Milky Way” from the Knut and Alice Wallenberg Foundation. C.A.S.U. is supported through STFC grants: ST/H004157/1, ST/J00541X/1, ST/M007626/1, ST/N005805/1, ST/T003081/1. Work reported here benefited from support through the GREAT-ITN FP7 project Grant agreement ID: 264895. D.K.F. acknowledges funds from the Alexander von Humboldt Foundation in the framework of the Sofja Kovalevskaja Award endowed by the Federal Ministry of Education and Research and the grant 2016-03412 from the Swedish Research Council. A.H. acknowledges support from the Spanish Government Ministerio de Ciencia e Innovación and ERD Funds through grants PGC-2018-091 3741-B-C22 and CEX2019-000920-S. X.F. acknowledges the support of China Postdoctoral Science Foundation 2020M670023. M.L.L.D. acknowledges the Polish NCN grant number 2019/34/E/ST9/00133. Part of this work was funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) – Project-ID 138713538 – SFB 881 (“The Milky Way System”, subproject A09). M.Z. acknowledges support from the National Agency for Research and Development (ANID) grants: FONDECYT Regular 1191505, Millennium Institute of Astrophysics ICN12-009, BASAL Center for Astrophysics and Associated Technologies AFB-170002. R.B. acknowledges support from the project PRIN-INAF 2019 “Spectroscopically Tracing the Disk Dispersal Evolution”. H.M.T. acknowledges financial support from the Agencia Estatal de Investigación of the Ministerio de Ciencia, Innovación y Universidades through projects PID2019-109522GB-C51,54/AEI/10.13039/501100011033, and the Centre of Excellence “María de Maeztu” award to Centro de Astrobiología (MDM-2017-0737). J.I.G.H. acknowledges financial support from the Spanish Ministry of Science and Innovation (MICINN) project AYA2017-86389-P, and also from the Spanish MICINN under 2013 Ramѳn y Cajal program RYC-2013-14875. V.P.D. is supported by STFC Consolidated grant ST/R000786/1. N.L. acknowledges financial support from “Programme National de Physique Stellaire” (PNPS) and the “Programme National Cosmology et Galaxies (PNCG)” of CNRS/INSU, France. A.R.C. is supported in part by the Australian Research Council through a Discovery Early Career Researcher Award (DE190100656). Parts of this research were supported by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013. P.S.B. is supported by the Swedish Research Council through individual project grants with contract Nos. 2016-03765 and 2020-03404. A.M. acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement no. 772293 – project ASTEROCHRONOMETRY). J.P. was supported by the project RVO: 67985815. E.D.M. acknowledges the support from FCT through the research grants UIDB/04434/2020 & UIDP/04434/2020 and through Investigador FCT contract IF/00849/2015/CP1273/CT0003. This work was (partially) supported by the Spanish Ministry of Science, Innovation and University (MICIU/FEDER, UE) through grant RTI2018-095076-B-C21, and the Institute of Cosmos Sciences University of Barcelona (ICCUB, Unidad de Excelencia 'María de Maeztu’) through grant CEX2019-000918-M. S.L.M. acknowledges the support of the UNSW Scientia Fellowship program and the Australian Research Council through Discovery Project grant DP180101791. GT acknowledges financial support of the Slovenian Research Agency (research core funding No. P1-0188) and the European Space Agency (Prodex Experiment Arrangement No. C4000127986). S.G.S acknowledges the support from FCT through Investigador FCT contract nr. CEECIND/00826/2018 and POPH/FSE (EC). H.G.L. acknowledges financial support by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) – Project-ID 138713538 – SFB 881 (“The Milky Way System”, subproject A04). This work was (partially) supported by the Spanish Ministry of Science, Innovation and University (MICIU/FEDER, UE) through grant RTI2018-095076-B-C21, and the Institute of Cosmos Sciences University of Barcelona (ICCUB, Unidad de Excelencia ’María de Maeztu’) through grant CEX2019-000918-M. T.K. is supported by STFC Consolidated grant ST/R000786/1. M.V. acknowledges the support of the Deutsche Forschungsgemeinschaft (DFG, project number: 428473034). T.M. is supported by a grant from the Fondation ULB. We acknowledge financial support from the Universidad Complutense de Madrid (UCM) and by the Spanish Ministerio de Ciencia, Innovación y Universidades, Ministerio de Economía y Competitividad, from project AYA2016-79425-C3-1-P and PID2019-109522GB-C5[4]/AEI/10.13039/501100011033. U.H. acknowledges support from the Swedish National Space Agency (SNSA/Rymdstyrelsen). D.G. gratefully acknowledges support from the Chilean Centro de Excelencia en Astrofísica y Tecnologías Afines (CATA) BASAL grant AFB-170002. D.G. also acknowledges financial support from the Dirección de Investigación y Desarrollo de la Universidad de La Serena through the Programa de Incentivo a la Investigación de Académicos (PIA-DIDULS). A. Lobel acknowledges support in part by the Belgian Federal Science Policy Office under contract No. BR/143/A2/BRASS. We acknowledge financial support from the Universidad Complutense de Madrid (UCM) and by the Spanish Ministerio de Ciencia, Innovación y Universidades, Ministerio de Economía y Competitividad, from project AYA2016-79425-C3-1-P and PID2019-109522GB-C5[4]/AEI/10.13039/501100011033. A.M. acknowledges the support from the Portuguese Fundação para a Ciência e a Tecnologia (FCT) through the Portuguese Strategic Programme UID/FIS/00099/2019 for CENTRA. T.M. acknowledges financial support from the Spanish Ministry of Science and Innovation (MICINN) through the Spanish State Research Agency, under the Severo Ochoa Program 2020-2023 (CEX2019-000920-S). E.J.A. acknowledges funding from the State Agency for Research of the Spanish MCIU through the “Center of Excellence Severo Ochoa” award to the Instituto de Astrofísica de An- dalucía (SEV-2017-0709).
Published: 2022
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8. Ca II Triplet Spectroscopy of Small Magellanic Cloud Red Giants. V. Abundances and Velocities for 12 Massive Clusters

Author: M. C. Parisi, L. V. Gramajo, D. Geisler, B. Dias, J. J. Clariá, G. Da Costa, and E. K. Grebel
Subjects: Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract: We aim to analyze the chemical evolution of the Small Magellanic Cloud adding 12 additional clusters to our existing sample having accurate and homogeneously derived metallicities. We are particularly interested in seeing if there is any correlation between age and metallicity for the different structural components to which the clusters belong. Spectroscopic metallicities of red giant stars are derived from the measurement of the equivalent width of the near-IR calcium triplet lines. Cluster membership analysis was carried out using criteria that include radial velocities, metallicities, proper motions and distance from the cluster center. The mean cluster radial velocity and metallicity were determined with a typical error of 2.1 km/s and 0.03 dex, respectively. We added this information to that available in the literature for other clusters studied with the same method, compiling a final sample of 48 clusters with metallicities homogeneously determined. Clusters of the final sample are distributed in an area of ~ 70 deg^2 and cover an age range from 0.4 Gyr to 10.5 Gyr. The metallicity distribution of our new cluster sample shows a lower probability of being bimodal than suggested in previous studies. The separate chemical analysis of clusters in the six components (Main Body, Counter-Bridge, West Halo, Wing/Bridge, Northern Bridge and Southern Bridge) shows that only clusters belonging to the Northern Bridge appear to trace a V-Shape, showing a clear inversion of the metallicity gradient in the outer regions. There is a suggestion of a metallicity gradient in the West Halo, similar to that previously found for field stars. It presents, however, a very large uncertainty. Also, clusters belonging to the West Halo, Wing/Bridge and Southern Bridge exhibit a well-defined age-metallicity relation with relatively little scatter in abundance at fixed age compared to other regions., Comment: 16 pages, 18 figures,Accepted for publication in A&A
Published: 2022
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9. Star Cluster Formation and Evolution in M101: An Investigation with the Legacy Extragalactic UV Survey

Author: S. T. Linden, G. Perez, D. Calzetti, S. Maji, M. Messa, B. C. Whitmore, R. Chandar, A. Adamo, K. Grasha, D. O. Cook, B. G. Elmegreen, D. A. Dale, E. Sacchi, E. Sabbi, E. K. Grebel, and L. Smith
Subjects: Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: We present Hubble Space Telescope WFC3/UVIS (F275W, F336W) and ACS/WFC optical (F435W, F555W, and F814W) observations of the nearby grand-design spiral galaxy M101 as part of the Legacy Extragalactic UV Survey (LEGUS). Compact sources detected in at least four bands were classified by both human experts and the convolutional neural network StarcNet. Human experts classified the 2,351 brightest sources, retrieving $N_{c} = 965$ star clusters. StarcNet, trained on LEGUS data not including M101, classified all 4,725 sources detected in four bands, retrieving $N_{c} = 2,270$ star clusters. The combined catalog represents the most complete census to date of compact star clusters in M101. We find that for the 2,351 sources with both a visual- and ML-classification StarcNet is able to reproduce the human classifications at high levels of accuracy ($\sim 80-90\%$), which is equivalent to the level of agreement between human classifiers in LEGUS. The derived cluster age distribution implies a disruption rate of $dN/d\tau \propto \tau^{-0.45 \pm 0.14}$ over $10^{7} < \tau < 10^{8.5}$yr for cluster masses $\geq 10^{3.55} M_{\odot}$ for the central region of M101 and $dN/d\tau \propto \tau^{-0.02 \pm 0.15}$ for cluster masses $\geq 10^{3.38} M_{\odot}$ in the northwest region of the galaxy. The trends we recover are weaker than those of other nearby spirals (e.g. M51) and starbursts, consistent with the M101 environment having a lower-density interstellar medium, and providing evidence in favor of environmentally-dependent cluster disruption in the central, southeast, and northwest regions of M101., Comment: 24 pages, 18 figures, 3 tables. Accepted for publication in the Astrophysical Journal
Published: 2022
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10. The Gaia -ESO Public Spectroscopic Survey: Implementation, data products, open cluster survey, science, and legacy

Author: S. Randich, G. Gilmore, L. Magrini, G. G. Sacco, R. J. Jackson, R. D. Jeffries, C. C. Worley, A. Hourihane, A. Gonneau, C. Viscasillas Vazquez, E. Franciosini, J. R. Lewis, E. J. Alfaro, C. Allende Prieto, T. Bensby, R. Blomme, A. Bragaglia, E. Flaccomio, P. François, M. J. Irwin, S. E. Koposov, A. J. Korn, A. C. Lanzafame, E. Pancino, A. Recio-Blanco, R. Smiljanic, S. Van Eck, T. Zwitter, M. Asplund, P. Bonifacio, S. Feltzing, J. Binney, J. Drew, A. M. N. Ferguson, G. Micela, I. Negueruela, T. Prusti, H.-W. Rix, A. Vallenari, A. Bayo, M. Bergemann, K. Biazzo, G. Carraro, A. R. Casey, F. Damiani, A. Frasca, U. Heiter, V. Hill, P. Jofré, P. de Laverny, K. Lind, G. Marconi, C. Martayan, T. Masseron, L. Monaco, L. Morbidelli, L. Prisinzano, L. Sbordone, S. G. Sousa, S. Zaggia, V. Adibekyan, R. Bonito, E. Caffau, S. Daflon, D. K. Feuillet, M. Gebran, J. I. Gonzalez Hernandez, G. Guiglion, A. Herrero, A. Lobel, J. Maiz Apellaniz, T. Merle, Š. Mikolaitis, D. Montes, T. Morel, C. Soubiran, L. Spina, H. M. Tabernero, G. Tautvaišiene, G. Traven, M. Valentini, M. Van der Swaelmen, S. Villanova, N. J. Wright, U. Abbas, V. Aguirre Børsen-Koch, J. Alves, L. Balaguer-Nunez, P. S. Barklem, D. Barrado, S. R. Berlanas, A. S. Binks, A. Bressan, R. Capuzzo-Dolcetta, L. Casagrande, L. Casamiquela, R. S. Collins, V. D'Orazi, M. L. L. Dantas, V. P. Debattista, E. Delgado-Mena, P. Di Marcantonio, A. Drazdauskas, N. W. Evans, B. Famaey, M. Franchini, Y. Frémat, E. D. Friel, X. Fu, D. Geisler, O. Gerhard, E. A. Gonzalez Solares, E. K. Grebel, M. L. Gutierrez Albarran, D. Hatzidimitriou, E. V. Held, F. Jiménez-Esteban, H. Jönsson, C. Jordi, T. Khachaturyants, G. Kordopatis, J. Kos, N. Lagarde, L. Mahy, M. Mapelli, E. Marfil, S. L. Martell, S. Messina, A. Miglio, I. Minchev, A. Moitinho, J. Montalban, M. J. P. F. G. Monteiro, C. Morossi, N. Mowlavi, A. Mucciarelli, D. N. A. Murphy, N. Nardetto, S. Ortolani, F. Paletou, J. Palouš, E. Paunzen, J. C. Pickering, A. Quirrenbach, P. Re Fiorentin, J. I. Read, D. Romano, N. Ryde, N. Sanna, W. Santos, G. M. Seabroke, A. Spagna, M. Steinmetz, E. Stonkuté, E. Sutorius, F. Thévenin, M. Tosi, M. Tsantaki, J. S. Vink, N. Wright, R. F. G. Wyse, M. Zoccali, J. Zorec, D. B. Zucker, N. A. Walton, Universidad de Alicante. Departamento de Física Aplicada, Astrofísica Estelar (AE), Ministerio de Ciencia e Innovación (España), European Commission, European Research Council, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)
Subjects: astro-ph.SR, astro-ph.GA, FOS: Physical sciences, Techniques: spectroscopic, Surveys, fundamental parameters [Stars], VELOCITY DISPERSION PROFILES, spectroscopic [Techniques], Astronomi, astrofysik och kosmologi, Astronomy, Astrophysics and Cosmology, LITHIUM DEPLETION, TRUMPLER 20, Solar and Stellar Astrophysics (astro-ph.SR), Stars: fundamental parameters, general [Open clusters and associations], Stars: abundances, Astronomy and Astrophysics, Open clusters and associations: general, INNER-DISK, CHEMICAL ABUNDANCES, Astrophysics - Astrophysics of Galaxies, GAMMA VELORUM CLUSTER, Astrophysics - Solar and Stellar Astrophysics, [SDU]Sciences of the Universe [physics], Space and Planetary Science, SURVEY MEMBERSHIP PROBABILITIES, Astrophysics of Galaxies (astro-ph.GA), SURVEY GALACTIC EVOLUTION, abundances [Stars], 6TH DATA RELEASE, MILKY-WAY, Catalogs
Abstract: Full list of authors: Randich, S.; Gilmore, G.; Magrini, L.; Sacco, G. G.; Jackson, R. J.; Jeffries, R. D.; Worley, C. C.; Hourihane, A.; Gonneau, A.; Vazquez, C. Viscasillas; Franciosini, E.; Lewis, J. R.; Alfaro, E. J.; Allende Prieto, C.; Bensby, T.; Blomme, R.; Bragaglia, A.; Flaccomio, E.; Francois, P.; Irwin, M. J.; Koposov, S. E.; Korn, A. J.; Lanzafame, A. C.; Pancino, E.; Recio-Blanco, A.; Smiljanic, R.; Van Eck, S.; Zwitter, T.; Asplund, M.; Bonifacio, P.; Feltzing, S.; Binney, J.; Drew, J.; Ferguson, A. M. N.; Micela, G.; Negueruela, I; Prusti, T.; Rix, H-W; Vallenari, A.; Bayo, A.; Bergemann, M.; Biazzo, K.; Carraro, G.; Casey, A. R.; Damiani, F.; Frasca, A.; Heiter, U.; Hill, V; Jofre, P.; de Laverny, P.; Lind, K.; Marconi, G.; Martayan, C.; Masseron, T.; Monaco, L.; Morbidelli, L.; Prisinzano, L.; Sbordone, L.; Sousa, S. G.; Zaggia, S.; Adibekyan, V; Bonito, R.; Caffau, E.; Daflon, S.; Feuillet, D. K.; Gebran, M.; Gonzalez Hernandez, J., I; Guiglion, G.; Herrero, A.; Lobel, A.; Maiz Apellaniz, J.; Montes, D.; Morel, T.; Soubiran, C.; Spina, L.; Tabernero, H. M.; Traven, G.; Valentini, M.; Van der Swaelmen, M.; Villanova, S.; Wright, N. J.; Abbas, U.; Borsen-Koch, V. Aguirre; Alves, J.; Balaguer-Nunez, L.; Barklem, P. S.; Barrado, D.; Berlanas, S. R.; Binks, A. S.; Bressan, A.; Capuzzo-Dolcetta, R.; Casagrande, L.; Casamiquela, L.; Collins, R. S.; D'Orazi, V; Dantas, M. L. L.; Debattista, V. P.; Delgado-Mena, E.; Di Marcantonio, P.; Drazdauskas, A.; Evans, N. W.; Famaey, B.; Franchini, M.; Fremat, Y.; Friel, E. D.; Fu, X.; Geisler, D.; Gerhard, O.; Solares, E. A. Gonzalez; Grebel, E. K.; Gutierrez Albarran, M. L.; Hatzidimitriou, D.; Held, E., V; Jimenez-Esteban, F.; Jonsson, H.; Jordi, C.; Khachaturyants, T.; Kordopatis, G.; Kos, J.; Lagarde, N.; Mahy, L.; Mapelli, M.; Marfil, E.; Martell, S. L.; Messina, S.; Miglio, A.; Minchev, I; Moitinho, A.; Montalban, J.; Monteiro, M. J. P. F. G.; Morossi, C.; Mowlavi, N.; Mucciarelli, A.; Murphy, D. N. A.; Nardetto, N.; Ortolani, S.; Paletou, F.; Palous, J.; Paunzen, E.; Pickering, J. C.; Quirrenbach, A.; Fiorentin, P. Re; Read, J., I; Romano, D.; Ryde, N.; Sanna, N.; Santos, W.; Seabroke, G. M.; Spagna, A.; Steinmetz, M.; Stonkute, E.; Sutorius, E.; Thevenin, F.; Tosi, M.; Tsantaki, M.; Vink, J. S.; Wright, N.; Wyse, R. F. G.; Zoccali, M.; Zorec, J.; Zucker, D. B.; Walton, N. A., Context. In the last 15 years different ground-based spectroscopic surveys have been started (and completed) with the general aim of delivering stellar parameters and elemental abundances for large samples of Galactic stars, complementing Gaia astrometry. Among those surveys, the Gaia-ESO Public Spectroscopic Survey, the only one performed on a 8m class telescope, was designed to target 100 000 stars using FLAMES on the ESO VLT (both Giraffe and UVES spectrographs), covering all the Milky Way populations, with a special focus on open star clusters. Aims. This article provides an overview of the survey implementation (observations, data quality, analysis and its success, data products, and releases), of the open cluster survey, of the science results and potential, and of the survey legacy. A companion article reviews the overall survey motivation, strategy, Giraffe pipeline data reduction, organisation, and workflow. Methods. We made use of the information recorded and archived in the observing blocks; during the observing runs; in a number of relevant documents; in the spectra and master catalogue of spectra; in the parameters delivered by the analysis nodes and the working groups; in the final catalogue; and in the science papers. Based on these sources, we critically analyse and discuss the output and products of the Survey, including science highlights. We also determined the average metallicities of the open clusters observed as science targets and of a sample of clusters whose spectra were retrieved from the ESO archive. Results. The Gaia-ESO Survey has determined homogeneous good-quality radial velocities and stellar parameters for a large fraction of its more than 110 000 unique target stars. Elemental abundances were derived for up to 31 elements for targets observed with UVES. Lithium abundances are delivered for about 1/3 of the sample. The analysis and homogenisation strategies have proven to be successful; several science topics have been addressed by the Gaia-ESO consortium and the community, with many highlight results achieved. Conclusions. The final catalogue will be released through the ESO archive in the first half of 2022, including the complete set of advanced data products. In addition to these results, the Gaia-ESO Survey will leave a very important legacy, for several aspects and for many years to come. © ESO 2022., Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under programmes ID 188.B-3002, 193-B-0936, and 197.B-1074. These data products have been processed by the Cambridge Astronomy Survey Unit (CASU) at the Institute of Astronomy, University of Cambridge, and by the FLAMES/UVES reduction team at INAF-Osservatorio Astrofisico di Arcetri. Public access to the data products is via the ESO Archive, and the Gaia-ESO Survey Data Archive, prepared and hosted by the Wide Field Astronomy Unit, Institute for Astronomy, University of Edinburgh, which is funded by the UK Science and Technology Facilities Council. This work was partly supported by the European Union FP7 programme through ERC grant number 320360 and by the Leverhulme Trust through grant RPG-2012-541. We acknowledge the support from INAF PRIN and Ministero dell’ Universitá e della Ricerca (MUR) in the form of the grant “Premiale VLT 2012” and “Premiale Mitic”. This work was partly supported by the INAF grant for mainstream projects: “Enhancing the legacy of the Gaia-ESO Survey for open cluster science”. The project presented here benefited in development from discussions held during the Gaia-ESO workshops and conferences supported by the ESF (European Science Foundation) through the GREAT Research Network Programme. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. R. Smiljanic acknowledges support from the National Science Centre, Poland (2014/15/B/ST9/03981). F.J.E. acknowledges financial support from the Spanish MINECO/FEDER through the grant AYA2017-84089 and MDM-2017-0737 at Centro de Astrobiología (CSIC-INTA), Unidad de Excelencia Mar a de Maeztu, and from the European Union’s Horizon 2020 research and innovation programme under Grant Agreement no. 824064 through the ESCAPE - The European Science Cluster of Astronomy & Particle Physics ESFRI Research Infrastructures project. T.B. was funded by the “The New Milky Way” project grant from the Knut and Alice Wallenberg Foundation. S.R.B. acknowledges support by the Spanish Government under grants AYA2015-68012-C2-2-P and PGC2018-093741-B-C21/C22 (MICIU/AEI/FEDER, UE). W.J.S. acknowledges CAPES for a PhD studentship. J.M.A. acknowledges support from the Spanish Government Ministerio de Ciencia e Innovaciόn through grants AYA2013-40611-P, AYA2016-75931-C2-2-P, and PGC2018-095049-B-C22. T.M. and others from STAR institute, Liege, Belgium are grateful to Belgian F.R.S.-FNRS for support, and are also indebted for an ESA/PRODEX Belspo contract related to the Gaia Data Processing and Analysis Consortium and for support through an ARC grant for Concerted Research Actions financed by the Federation Wallonie-Brussels. This research has been partially supported by the ASI-INAF contract 2014-049-R.O: “Realizzazione attività tecniche/scientifiche presso ASDC” (PI Angelo Antonelli). V.A.acknowledges the support from Fundação para a Ciência e Tecnologia (FCT) through Investigador FCT contract nr. IF/00650/2015/CP1273/CT0001. AJK acknowledges support by the Swedish National Space Agency (SNSA). AB acknowledges support by ANID, – Millennium Science Initiative Program – NCN19_171, and FONDECYT regular 1190748. E.M. acknowledges financial support from the Spanish State Research Agency (AEI) through project MDM-2017-0737 Unidad de Excelencia “María de Maeztu” – Centro de Astrobiología (CSIC-INTA). T.Z. acknowledges financial support of the Slovenian Research Agency (research core funding no. P1-0188) and the European Space Agency (Prodex Experiment Arrangement No. C4000127986). P.J. acknowledges support FONDECYT Regular 1200703. The work of I.N. is partially supported by the Spanish Government Ministerio de Ciencia, Innovaciόn y Universidades under grant PGC2018-093741-B-C21 (MICIU/AEI/FEDER, UE). Funding for this work has been provided by the ARC Future Fellowship FT160100402. CAP acknowledges financial support from the Spanish Government through research grants MINECO AYA 2014-56359-P, MINECO AYA2017-86389-P, and MICINN PID2020-117493GB-I00. S.F. was supported by the grants 2011-5042 and 2016- 03412 from the Swedish Research Council and the project grant “The New Milky Way” from the Knut and Alice Wallenberg Foundation. CASU is supported through STFC grants: ST/H004157/1, ST/J00541X/1, ST/M007626/1, ST/N005805/1, ST/T003081/1. Work reported here benefited from support through the GREAT-ITN FP7 project Grant agreement ID: 264895. DKF acknowledges funds from the Alexander von Humboldt Foundation in the framework of the Sofja Kovalevskaja Award endowed by the Federal Ministry of Education and Research and the grant 2016-03412 from the Swedish Research Council. A.H. acknowledges support from the Spanish Government Ministerio de Ciencia e Innovaciόn and ERD Funds through grants PGC-2018-091 3741-B-C22 and CEX2019-000920-S. X.F. acknowledge the support of China Postdoctoral Science Foundation 2020M670023. M.L.L. Dantas acknowledges the Polish NCN grant number 2019/34/E/ST9/00133. Part of this work was funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) – Project-ID 138713538 – SFB 881 (“The Milky Way System”, subproject A09). M.Z. acknowledge support from the National Agency for Research and Development (ANID) grants: FONDECYT Regular 1191505, Millennium Institute of Astrophysics ICN12-009, BASAL Center for Astrophysics and Associated Technologies AFB-170002. R.B. acknowledges support from the project PRIN-INAF 2019 “Spectroscopically Tracing the Disk Dispersal Evolution”. HMT acknowledges financial support from the Agencia Estatal de Investigaciόn of the Ministerio de Ciencia, Innovaciόn y Universidades through projects PID2019-109522GB-C51,54/AEI/10.13039/501100011033, and the Centre of Excellence “María de Maeztu” award to Centro de Astrobiología (MDM-2017-0737). JIGH acknowledges financial support from the Spanish Ministry of Science and Innovation (MICINN) project AYA2017-86389-P, and also from the Spanish MICINN under 2013 Ramøn y Cajal program RYC-2013-14875. V.P.D. is supported by STFC Consolidated grant ST/R000786/1. N.L. acknowledges financial support from “Programme National de Physique Stellaire” (PNPS) and the “Programme National Cosmology et Galaxies (PNCG)” of CNRS/INSU, France. A.R.C. is supported in part by the Australian Research Council through a Discovery Early Career Researcher Award (DE190100656). Parts of this research were supported by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013. PSB is Supported by the Swedish Research Council through individual project grants with contract Nos. 2016-03765 and 2020-03404. A.M. acknowledges funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement no. 772293 - project ASTEROCHRONOMETRY). J.P. was supported by the project RVO: 67985815. E.D.M. acknowledges the support from FCT through the research grants UIDB/04434/2020 & UIDP/04434/2020 and through Investigator FCT contract IF/00849/2015/CP1273/CT0003. This work was (partially) supported by the Spanish Ministry of Science, Innovation and University (MICIU/FEDER, UE) through grant RTI2018-095076-B-C21, and the Institute of Cosmos Sciences University of Barcelona (ICCUB, Unidad de Excelencia “María de Maeztu”) through grant CEX2019-000918-M. S.L.M. acknowledges the support of the UNSW Scientia Fellowship program and the Australian Research Council through Discovery Project grant DP180101791. G.T. acknowledges financial support of the Slovenian Research Agency (research core funding no. P1-0188) and the European Space Agency (Prodex Experiment Arrangement No. C4000127986). S.G.S. acknowledges the support from FCT through Investigador FCT contract no. CEECIND/00826/2018 and POPH/FSE (EC). H.G.L. acknowledges financial support by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) - Project-ID 138713538 – SFB 881 (“The Milky Way System”, subproject A04). This work was (partially) supported by the Spanish Ministry of Science, Innovation and University (MICIU/FEDER, UE) through grant RTI2018-095076-B-C21, and the Institute of Cosmos Sciences University of Barcelona (ICCUB, Unidad de Excelencia “María de Maeztu”) through grant CEX2019-000918-M. T.K. is supported by STFC Consolidated grant ST/R000786/1. M.V. acknowledges the support of the Deutsche Forschungsgemeinschaft (DFG, project number: 428473034). T.M. is supported by a grant from the Fondation ULB. We acknowledge financial support from the Universidad Complutense de Madrid (UCM) and by the Spanish Ministerio de Ciencia, Innovaciόn y Universidades, Ministerio de Economía y Competitividad, from project AYA2016-79425-C3-1-P and PID2019-109522GB-C5[4]/AEI/10.13039/501100011033. U.H. acknowledges support from the Swedish National Space Agency (SNSA/Rymdstyrelsen). D.G. gratefully acknowledges support from the Chilean Centro de Excelencia en Astrofίsica y Tecnologías Afines (CATA) BASAL grant AFB-170002. D.G. also acknowledges financial support from the Direcciόn de Investigaciόn y Desarrollo de la Universidad de La Serena through the Programa de Incentivo a la Investigaciόn de Académicos (PIA-DIDULS). A. Lobel acknowledges support in part by the Belgian Federal Science Policy Office under contract no. BR/143/A2/BRASS. We acknowledge financial support from the Universidad Complutense de Madrid (UCM) and by the Spanish Ministerio de Ciencia, Innovaciόn y Universidades, Ministerio de Economía y Competitividad, from project AYA2016-79425-C3-1-P and PID2019-109522GB-C5[4]/AEI/10.13039/501100011033. AM acknowledges the support from the Portuguese Fundação para a Ciência e a Tecnologia (FCT) through the Portuguese Strategic Programme UID/FIS/00099/2019 for CENTRA. T.M. acknowledges financial support from the Spanish Ministry of Science and Innovation (MICINN) through the Spanish State Research Agency, under the Severo Ochoa Program 2020-2023 (CEX2019-000920-S). E.J.A. acknowledges funding from the State Agency for Research of the Spanish MCIU through the “Center of Excellence Severo Ochoa” award to the Instituto de Astrofisica de Andalucia (SEV-2017-0709).
Published: 2022
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11. Neutron-capture elements in dwarf galaxies

Author: M. Reichert, C. J. Hansen, M. Hanke, Á. Skúladóttir, A. Arcones, E. K. Grebel
Published: 2020
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12. On the Oosterhoff dichotomy in the Galactic bulge: I. spatial distribution

Author: Z Prudil, I Dékány, M Catelan, R Smolec, E K Grebel, and M Skarka
Subjects: Astrophysics - Solar and Stellar Astrophysics, 010308 nuclear & particles physics, Space and Planetary Science, 0103 physical sciences, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 010303 astronomy & astrophysics, 01 natural sciences, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics
Abstract: We present a study of the Oosterhoff (Oo) dichotomy in the Galactic bulge using 8\,141 fundamental mode RR~Lyrae stars. We used public photometric data from the Optical Gravitational Lensing Experiment (OGLE) and the Vista Variables in the V\'ia L\'actea survey (VVV). We carefully selected fundamental mode stars without modulation and without association with any globular cluster located toward the Galactic bulge. Subsequently, we identified and separated the Oosterhoff groups I and II on the basis of their period-amplitude distribution and using a relation fitted to the Oosterhoff I locus. Both Oosterhoff groups were then compared to observations of two bulge globular clusters and with models of stellar pulsation and evolution. We found that some of the variables classified as Oo\,II belong to a third Oo group. The Oosterhoff II variables are more metal-poor on average, more massive, and cooler than their Oosterhoff I counterparts. The analysis of their spatial distribution shows a systematic difference between \textit{foreground}, central and \textit{background} regions in the occurrence of the Oosterhoff II group. The difference between the Oo\,I and II groups is also seen in their distance distributions with respect to the Galactic bar, but neither group is associated with the bar., Comment: 18 pages, 12 figures. Accepted for publication in MNRAS
Published: 2019

13. Legacy extraGalactic UV survey with the Hubble space telescope : stellar cluster catalogs and first insights into cluster formation and evolution in NGC 628

Author: A. Adamo, J. E. Ryon, M. Messa, H. Kim, K. Grasha, D. O. Cook, D. Calzetti, J. C. Lee, B. C. Whitmore, B. G. Elmegreen, L. Ubeda, L. J. Smith, S. N. Bright, A. Runnholm, J. E. Andrews, M. Fumagalli, D. A. Gouliermis, L. Kahre, P. Nair, D. Thilker, R. Walterbos, A. Wofford, A. Aloisi, G. Ashworth, T. M. Brown, R. Chandar, C. Christian, M. Cignoni, G. C. Clayton, D. A. Dale, S. E. de Mink, C. Dobbs, D. M. Elmegreen, A. S. Evans, J. S. Gallagher III, E. K. Grebel, A. Herrero, D. A. Hunter, K. E. Johnson, R. C. Kennicutt, M. R. Krumholz, D. Lennon, K. Levay, C. Martin, A. Nota, G. Östlin, A. Pellerin, J. Prieto, M. W. Regan, E. Sabbi, E. Sacchi, D. Schaerer, D. Schiminovich, F. Shabani, M. Tosi, S. D. Van Dyk, E. Zackrisson, Adamo, A, Ryon, J, Messa, M, Kim, H, Grasha, K, Cook, D, Calzetti, D, Lee, J, Whitmore, B, Elmegreen, B, Ubeda, L, Smith, L, Bright, S, Runnholm, A, Andrews, J, Fumagalli, M, Gouliermis, D, Kahre, L, Nair, P, Thilker, D, Walterbos, R, Wofford, A, Aloisi, A, Ashworth, G, Brown, T, Chandar, R, Christian, C, Cignoni, M, Clayton, G, Dale, D, De Mink, S, Dobbs, C, Elmegreen, D, Evans, A, Gallagher, J, Grebel, E, Herrero, A, Hunter, D, Johnson, K, Kennicutt, R, Krumholz, M, Lennon, D, Levay, K, Martin, C, Nota, A, Ostlin, G, Pellerin, A, Prieto, J, Regan, M, Sabbi, E, Sacchi, E, Schaerer, D, Schiminovich, D, Shabani, F, Tosi, M, Van Dyk, S, Zackrisson, E, and Low Energy Astrophysics (API, FNWI)
Subjects: Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Photometry (optics), galaxies: individual (NGC 628, M74), Hubble space telescope, 0103 physical sciences, Cluster (physics), Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy), Physics, Spiral galaxy, stars: formation, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, galaxies: star clusters: general, galaxies: star formation, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: individual (NGC 628, Spectral energy distribution, Low Mass, M74)
Abstract: We report the large effort which is producing comprehensive high-level young star cluster (YSC) catalogues for a significant fraction of galaxies observed with the Legacy ExtraGalactic UV Survey (LEGUS) Hubble treasury program. We present the methodology developed to extract cluster positions, verify their genuine nature, produce multiband photometry (from NUV to NIR), and derive their physical properties via spectral energy distribution fitting analyses. We use the nearby spiral galaxy NGC628 as a test case for demonstrating the impact that LEGUS will have on our understanding of the formation and evolution of YSCs and compact stellar associations within their host galaxy. Our analysis of the cluster luminosity function from the UV to the NIR finds a steepening at the bright end and at all wavelengths suggesting a dearth of luminous clusters. The cluster mass function of NGC628 is consistent with a power-law distribution of slopes $\sim -2$ and a truncation of a few times $10^5$ M$_\odot$. After their formation YSCs and compact associations follow different evolutionary paths. YSCs survive for a longer timeframe, confirming their being potentially bound systems. Associations disappear on time scales comparable to hierarchically organized star-forming regions, suggesting that they are expanding systems. We find mass-independent cluster disruption in the inner region of NGC628, while in the outer part of the galaxy there is little or no disruption. We observe faster disruption rates for low mass ($\leq$ $10^4$ M$_\odot$) clusters suggesting that a mass-dependent component is necessary to fully describe the YSC disruption process in NGC628., accepted for publication in ApJ; 27 pages; complete stellar cluster catalogues will be released in June 2017 at https://legus.stsci.edu
Published: 2017

14. RAVE stars in K2. I. Improving RAVE red giants spectroscopy using asteroseismology from K2 Campaign 1

Author: M. Valentini, C. Chiappini, G. R. Davies, Y. P. Elsworth, B. Mosser, M. N. Lund, A. Miglio, W. J. Chaplin, T. S. Rodrigues, C. Boeche, M. Steinmetz, G. Matijevič, G. Kordopatis, J. Bland-Hawthorn, U. Munari, O. Bienaymé, K. C. Freeman, B. K. Gibson, G. Gilmore, E. K. Grebel, A. Helmi, A. Kunder, P. McMillan, J. Navarro, Q. A. Parker, W. Reid, G. Seabroke, S. Sharma, A. Siviero, F. Watson, R. F. G. Wyse, T. Zwitter, A. Mott, Astronomy, Gilmore, Gerard [0000-0003-4632-0213], Apollo - University of Cambridge Repository, Leibniz-Institut für Astrophysik Potsdam (AIP), School of Physics and Astronomy, University of Birmingham [Birmingham], Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Universidade Federal de São Paulo (UNIFESP), Leibniz-Institut DSMZ-Deutsche Sammlung von Mikroorganismen und Zellkulturen GmbH / Leibniz Institute DSMZ-German Collection of Microorganisms and Cell Cultures (DSMZ), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), Departament Llenguatges i Sistemes Informatics, Universitat Politècnica de Catalunya [Barcelona] (UPC), Cargill, Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), University of Ljubljana, Federal University of Sao Paulo (Unifesp), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), and Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: oscillations [stars], stars: abundances, Calibration (statistics), fundamental parameters [stars], FOS: Physical sciences, KEPLER FIELD, Astrophysics, EFFECTIVE TEMPERATURES, 01 natural sciences, Asteroseismology, surveys, ATMOSPHERIC PARAMETERS, 0103 physical sciences, Solar-like oscillations, VELOCITY EXPERIMENT RAVE, Spectroscopy, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), ComputingMilieux_MISCELLANEOUS, Physics, [PHYS]Physics [physics], 010308 nuclear & particles physics, ELEMENTAL ABUNDANCES, stars: late-type, Astronomy and Astrophysics, GALACTIC ARCHAEOLOGY, Astrophysics - Astrophysics of Galaxies, STELLAR PARAMETERS, abundances [stars], 1ST DATA RELEASE, Stars, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, AGE-METALLICITY RELATION, Astrophysics of Galaxies (astro-ph.GA), MILKY-WAY, late-type [stars], spectroscopic [techniques], stars: oscillations, stars: fundamental parameters, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Data release, techniques: spectroscopic
Abstract: We present a set of 87 RAVE stars with detected solar like oscillations, observed during Campaign 1 of the K2 mission (RAVE K2-C1 sample). This dataset provides a useful benchmark for testing the gravities provided in RAVE Data Release 4 (DR4), and is key for the calibration of the RAVE Data Release 5 (DR5). In the present work, we use two different pipelines, GAUFRE (Valentini et al. 2013) and Sp_Ace (Boeche & Grebel 2016), to determine atmospheric parameters and abundances by fixing log(g) to the seismic one. Our strategy ensures highly consistent values among all stellar parameters, leading to more accurate chemical abundances. A comparison of the chemical abundances obtained here with and without the use of seismic log(g) information has shown that an underestimated (overestimated) gravity leads to an underestimated (overestimated) elemental abundance (e.g. [Mg/H] is underestimated by ~0.25 dex when the gravity is underestimated by 0.5 dex). We then perform a comparison between the seismic gravities and the spectroscopic gravities presented in the RAVE DR4 catalogue, extracting a calibration for log(g) of RAVE giants in the colour interval 0.50, Comment: 20 pages, 27 figures, accepted
Published: 2017
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15. Diffuse interstellar bands in RAVE survey spectra

Author: U. Munari, L. Tomasella, M. Fiorucci, O. Bienaymé, J. Binney, J. Bland-Hawthorn, C. Boeche, R. Campbell, K. C. Freeman, B. Gibson, G. Gilmore, E. K. Grebel, A. Helmi, J. F. Navarro, Q. A. Parker, G. M. Seabroke, A. Siebert, A. Siviero, M. Steinmetz, F. G. Watson, M. Williams, R. F. G. Wyse, T. Zwitter, and University of Groningen
Subjects: FULLERENES, DATA RELEASE, FOS: Physical sciences, LINES, Astrophysics, Spectral line, POLYCYCLIC AROMATIC-HYDROCARBONS, surveys, ISM : general, ANGSTROM, VELOCITY EXPERIMENT RAVE, Line (formation), Physics, SPECTROSCOPY, Diffuse interstellar band, Wavelength range, Astrophysics (astro-ph), Astronomy and Astrophysics, CARRIERS, Galaxy, Interstellar medium, AO-0235+164, Stars, Wavelength, Space and Planetary Science, ISM : lines and bands, SYSTEM
Abstract: We have used spectra of hot stars from the RAVE Survey in order to investigate the visibility and properties of five diffuse interstellar bands previously reported in the literature. The RAVE spectroscopic survey for Galactic structure and kinematics records CCD spectra covering the 8400-8800 Ang wavelength region at 7500 resolving power. The spectra are obtained with the UK Schmidt at the AAO, equipped with the 6dF multi-fiber positioner. The DIB at 8620.4 Ang is by far the strongest and cleanest of all DIBs occurring within the RAVE wavelength range, with no interference by underlying absorption stellar lines in hot stars. It correlates so tightly with reddening that it turns out to be a reliable tool to measure it, following the relation E(B-V) = 2.72 (+/- 0.03) x E.W.(Ang), valid throughout the general interstellar medium of our Galaxy. The presence of a DIB at 8648 Ang is confirmed. Its intensity appears unrelated to reddening, in agreement with scanty and preliminary reports available in the literature, and its measurability is strongly compromised by severe blending with underlying stellar HeI doublet at 8649 Ang. The two weak DIBS at 8531 and 8572 Ang do not appear real and should actually be blends of underlying stellar lines. The very weak DIB at 8439 Ang cannot be resolved within the profile of the much stronger underlying hydrogen Paschen 18 stellar line., Accepted in press by A&A
Published: 2008
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16. A statistical study of binary and multiple clusters in the LMC

Author: E. K. Grebel, Andrea Dieball, and H. Müller
Subjects: Physics, media_common.quotation_subject, Astrophysics (astro-ph), Monte Carlo method, FOS: Physical sciences, Binary number, Astronomy and Astrophysics, Astrophysics, Spatial distribution, Distance modulus, Star cluster, Distribution (mathematics), Space and Planetary Science, Sky, Cluster (physics), media_common
Abstract: Based on the Bica et al. (1999) catalogue we studied the star cluster system of the LMC and provide a new catalogue of all binary and multiple cluster candidates found. We performed Monte Carlo simulations and produced artificial cluster distributions that we compared with the real one in order to check how many of the found cluster pairs and groups can be expected statistically due to chance superposition on the plane of the sky. We found that, depending on the cluster density, between 56% (bar region) and 12% (outer LMC) of the detected pairs can be explained statistically. We studied in detail the properties of the multiple cluster candidates. The binary cluster candidates seem to show a tendency to form with components of similar size. When possible, we studied the age structure of the cluster groups and found that the multiple clusters are predominantly young with only a few cluster groups older than 300 Myr. The spatial distribution of the cluster pairs and groups coincides with the distribution of clusters in general; however, old groups or groups with large internal age differences are mainly located in the densely populated bar region. Thus, they can easily be explained as chance superpositions. Our findings show that a formation scenario through tidal capture is not only unlikely due to the low probability of close encounters of star clusters, and thus the even lower probability of tidal capture, but the few groups with large internal age differences can easily be explained with projection effects. We favour a formation scenario as suggested by Fujimoto & Kumai (1997) in which the components of a binary cluster formed together and thus should be coeval or have small age differences compatible with cluster formation time scales., 19 pages, including 15 figures, accepted for publication in A&A, minor corrections (1 reference removed form the abstract)
Published: 2002
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17. Interaction between the IGM and a dwarf galaxy

Author: V. Lora, A. C. Raga, and E. K. Grebel
Subjects: Física, Astronomía y Matemáticas, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxies, Astrophysics - Astrophysics of Galaxies, ISM, Astrophysics::Galaxy Astrophysics, dwarf, methods
Abstract: Dwarf Galaxies are the most common objects in the Universe and are believed to contain large amounts of dark matter. There are mainly three morphologic types of dwarf galaxies: dwarf ellipticals, dwarf spheroidals and dwarf irregulars. Dwarf irregular galaxies are particularly interesting in dwarf galaxy evolution, since dwarf spheroidal predecessors could have been very similar to them. Therefore, a mechanism linked to gas-loss in dwarf irregulars should be observed, i.e. ram pressure stripping. In this paper, we study the interaction between the ISM of a dwarf galaxy, and a flowing IGM. We derive the weak-shock, plasmon solution corresponding to the balance between the post-bow shock pressure and the pressure of the stratified ISM (which we assume follows the fixed stratification of a gravitationally dominant dark matter halo). We compare our model with previously published numerical simulations and with the observed shape of the HI cloud around the Ho II and Pegasus dwarf irregular galaxies. We show that such a comparison provides a straightforward way for estimating the Mach number of the impinging flow., 9 pages, 5 figures. Accepted for publication in RevMexAA
Published: 2014

18. A Curious New Milky Way Satellite in Ursa Major

Author: D. B. Zucker, V. Belokurov, N. W. Evans, J. T. Kleyna, M. J. Irwin, M. I. Wilkinson, M. Fellhauer, D. M. Bramich, G. Gilmore, H. J. Newberg, B. Yanny, J. A. Smith, P. C. Hewett, E. F. Bell, H.-W. Rix, O. Y. Gnedin, S. Vidrih, R. F. G. Wyse, B. Willman, E. K. Grebel, D. P. Schneider, T. C. Beers, A. Y. Kniazev, J. C. Barentine, H. Brewington, J. Brinkmann, M. Harvanek, S. J. Kleinman, J. Krzesinski, D. Long, A. Nitta, and S. A. Snedden
Subjects: Physics, Ursa Major, education.field_of_study, Stellar population, Metallicity, Milky Way, Population, Astrophysics (astro-ph), Local Group, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Galaxy, Space and Planetary Science, Satellite galaxy, education
Abstract: In this Letter, we study a localized stellar overdensity in the constellation of Ursa Major, first identified in Sloan Digital Sky Survey (SDSS) data and subsequently followed up with Subaru imaging. Its color-magnitude diagram (CMD) shows a well-defined sub-giant branch, main sequence and turn-off, from which we estimate a distance of ~30 kpc and a projected size of ~250 x 125 pc. The CMD suggests a composite population with some range in metallicity and/or age. Based on its extent and stellar population, we argue that this is a previously unknown satellite galaxy of the Milky Way, hereby named Ursa Major II (UMa II) after its constellation. Using SDSS data, we find an absolute magnitude of M_V \~ -3.8, which would make it the faintest known satellite galaxy. UMa II's isophotes are irregular and distorted with evidence for multiple concentrations; this suggests that the satellite is in the process of disruption., Comment: 4 pages, 4 figures, submitted to ApJ Letters
Published: 2006
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19. Steps toward determination of the size and structure of the broad-line region in active galactic nuclei. 6: Variability of NGC 3783 from ground-based data

Author: G. M. Stirpe, C. Winge, B. Altieri, D. Alloin, E. L. Aguero, G. C. Anupama, R. Ashley, R. Bertram, J. H. Calderon, R. M. Catchpole, R. L. M. Corradi, E. Covino, H. A. Dottori, M. W. Feast, K. K. Ghosh, R. Gil Hutton, I. S. Glass, E. K. Grebel, L. Jorda, C. Koen, C. D. Laney, M. Maia, F. Marang, Y. D. Mayya, N. Morrell, Y. Nakada, M. G. Pastoriza, A. K. Pati, D. Pelat, B. M. Peterson, T. P. Prabhu, G. Roberts, R. Sagar, I. Salamanca, K. Sekiguchi, T. Storchi-Bergmann, A. Subramaniam, H. Van Winckel, F. van Wyk, M. Villada, R. M. Wagner, P. A. Whitelock, H. Winkler, J. Clavel, M. Dietrich, W. Kollatschny, P. T. O'Brien, G. C. Perola, M. C. Recondo-Gonzalez, P. Rodriguez-Pascual, and M. Santos-Lleo
Subjects: Physics, Active galactic nucleus, 010504 meteorology & atmospheric sciences, Continuum (measurement), Lag, Astronomy and Astrophysics, Astrophysics, Light curve, 01 natural sciences, Galaxy, Space and Planetary Science, Ionization, 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract: The Seyfert 1 galaxy NGC 3783 was intensely monitored between 1991 December and 1992 August. We present the results from the ground-based observations in the optical and near-IR, which complement the data-set from the IUE, discussed elsewhere. Spectroscopic and photometric data from many observatories were combined in order to obtain well sampled light curves of the continuum and of H-Beta. During the campaign the source varied significantly. The light curves of the optical continuum and of H-Beta are similar to those obtained with the IUE. The near-IR flux did not vary significantly except for an increase at the end of the campaign. The optical continuum and the flux of H-Beta lag the UV continuum by 1 day or less and by 8 days respectively. These results confirm that the continuum variations are simultaneous or have a very small lag across the entire UV-optical range, and that the lines of NGC 3783 respond to ionizing continuum variations with less delay than those of NGC 5548. As in NGC 5548, the lag of H-Beta is greater than those of the high ionization lines.
Published: 1994
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20. Star Formation Histories of the LEGUS Dwarf Galaxies. III. The Nonbursty Nature of 23 Star-forming Dwarf Galaxies.

Author: M. Cignoni, E. Sacchi, M. Tosi, A. Aloisi, D. O. Cook, D. Calzetti, J. C. Lee, E. Sabbi, D. A. Thilker, A. Adamo, D. A. Dale, B. G. Elmegreen, J. S. Gallagher III, E. K. Grebel, K. E. Johnson, M. Messa, L. J. Smith, and L. Ubeda
Subjects: STAR formation, ACTIVE galaxies, DWARF galaxies, STELLAR mass, SPACE telescopes, INDEPENDENT sets
Abstract: We derive the recent star formation histories (SFHs) of 23 active dwarf galaxies using Hubble Space Telescope observations from the Legacy Extragalactic UV Survey. We apply a color–magnitude diagram (CMD) fitting technique using two independent sets of stellar models, PARSEC-COLIBRI and MIST. Despite the nonnegligible recent activity, none of the 23 star-forming dwarfs show enhancements in the last 100 Myr larger than three times the 100 Myr average. The unweighted mean of the individual SFHs in the last 100 Myr is also consistent with a rather constant activity, irrespective of the atomic gas fraction. We confirm previous results that for dwarf galaxies, the CMD-based average star formation rates (SFRs) are generally higher than the FUV-based SFRs. For half of the sample, the 60 Myr average CMD-based SFR is more than two times the FUV SFR. In contrast, we find remarkable agreement between the 10 Myr average CMD-based SFR and the Hα-based SFR. Finally, using core helium-burning stars of intermediate mass, we study the pattern of star formation spatial progression over the past 60 Myr and speculate on the possible triggers and connections of the star formation activity with the environment in which these galaxies live. Approximately half of our galaxies show spatial progression of star formation in the last 60 Myr and/or very recent diffuse and off-center activity compared to RGB stars. [ABSTRACT FROM AUTHOR]
Published: 2019
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21. An ALMA/HST Study of Millimeter Dust Emission and Star Clusters.

Author: J. A. Turner, D. A. Dale, A. Adamo, D. Calzetti, K. Grasha, E. K. Grebel, K. E. Johnson, J. C. Lee, L. J. Smith, and I. Yoon
Subjects: SPIRAL galaxies, DUST, STAR clusters, STELLAR mass, SPACE telescopes, SPATIAL variation, DISK galaxies
Abstract: We present results from a joint ALMA/HST study of the nearby spiral galaxy NGC 628. We combine the Hubble Space Telescope (HST) Legacy ExtraGalactic UV Survey (LEGUS) database of over 1000 stellar clusters in NGC 628 with ALMA Cycle 4 mm/submillimeter observations of the cold dust continuum that span ∼15 kpc2 including the nuclear region and western portions of the galaxy’s disk. The resolution—1.″1 or approximately 50 pc at the distance of NGC 628—allows us to constrain the spatial variations in the slope of the millimeter dust continuum as a function of the ages and masses of the nearby stellar clusters. Our results indicate an excess of dust emission in the millimeter, assuming a typical cold dust model for a normal star-forming galaxy, but little correlation of the dust continuum slope with stellar cluster age or mass. For the depth and spatial coverage of these observations, we cannot substantiate the millimeter/submillimeter excess arising from the processing of dust grains by the local interstellar radiation field. We detect a bright unknown source in NGC 628 in ALMA bands 4 and 7 with no counterparts at other wavelengths from ancillary data. We speculate this is possibly a dust-obscured supernova. [ABSTRACT FROM AUTHOR]
Published: 2019
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22. Cold, Old, and Metal-poor: New Stellar Substructures in the Milky Way’s Dwarf Spheroidals.

Author: V. Lora, E. K. Grebel, S. Schmeja, and A. Koch
Subjects: *MILKY Way, *DWARF galaxies, *ELLIPTICAL galaxies, *SPANNING trees, *STAR formation
Abstract: Dwarf spheroidal galaxies (dSph) orbiting the Milky Way are complex objects often with complicated star formation histories and internal dynamics. In this work, we search for stellar substructures in four of the classical dSph satellites of the Milky Way: Sextans, Carina, Leo I, and Leo II. We apply two methods to search for stellar substructure: the minimum spanning tree method, which helps us find and quantify spatially connected structures, and the “brute-force” method, which is able to find elongated stellar substructures. We detected the previously known substructure in Sextans and also found a new stellar substructure within Sextans. Furthermore, we identified a new stellar substructure close to the core radius of the Carina dwarf galaxy. We report a detection of one substructure in Leo I and two in Leo II, but we note that we are dealing with a low number of stars in the samples used. Such old stellar substructures in dSphs could help us shed light on the nature of the dark matter halos, within which such structures form, evolve, and survive. [ABSTRACT FROM AUTHOR]
Published: 2019
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23. Star Formation Histories of the LEGUS Dwarf Galaxies. II. Spatially Resolved Star Formation History of the Magellanic Irregular NGC 4449.

Author: E. Sacchi, B. G. Elmegreen, D. A. Gouliermis, E. K. Grebel, D. A. Hunter, L. J. Smith, D. A. Thilker, M. Tosi, F. Annibali, M. Cignoni, A. Aloisi, E. Sabbi, L. Ubeda, B. C. Whitmore, D. Calzetti, K. Grasha, J. C. Lee, A. Adamo, and D. A. Dale
Subjects: IRREGULAR galaxies, GALAXY formation, ASTRONOMICAL photometry, STAR formation, STARBURSTS
Abstract: We present a detailed study of the Magellanic irregular galaxy NGC 4449 based on both archival and new photometric data from the Legacy Extragalactic UV Survey, obtained with the Hubble Space Telescope Advanced Camera for Surveys and Wide Field Camera 3. Thanks to its proximity (D = 3.82 ± 0.27 Mpc), we reach stars 3 mag fainter than the tip of the red giant branch in the F814W filter. The recovered star formation history (SFH) spans the whole Hubble time, but due to the age–metallicity degeneracy of the red giant branch stars, it is robust only over the lookback time reached by our photometry, i.e., ∼3 Gyr. The most recent peak of star formation (SF) is around 10 Myr ago. The average surface density SF rate over the whole galaxy lifetime is 0.01 M⊙ yr−1 kpc−2. From our study, it emerges that NGC 4449 has experienced a fairly continuous SF regime in the last 1 Gyr, with peaks and dips whose SF rates differ only by a factor of a few. The very complex and disturbed morphology of NGC 4449 makes it an interesting galaxy for studies of the relationship between interactions and starbursts, and our detailed and spatially resolved analysis of its SFH does indeed provide some hints on the connection between these two phenomena in this peculiar dwarf galaxy. [ABSTRACT FROM AUTHOR]
Published: 2018
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24. LAMOST DR1: Stellar Parameters and Chemical Abundances with SP_Ace.

Author: C. Boeche, M. C. Smith, E. K. Grebel, J. Zhong, J. L. Hou, L. Chen, and D. Stello
Published: 2018
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25. Star Formation Histories of the LEGUS Dwarf Galaxies. I. Recent History of NGC 1705, NGC 4449, and Holmberg II.

Author: M. Cignoni, E. Sacchi, A. Aloisi, M. Tosi, D. Calzetti, J. C. Lee, E. Sabbi, A. Adamo, D. O. Cook, D. A. Dale, B. G. Elmegreen, J. S. Gallagher III, D. A. Gouliermis, K. Grasha, E. K. Grebel, D. A. Hunter, K. E. Johnson, M. Messa, L. J. Smith, and D. A. Thilker
Subjects: DWARF galaxies, STAR formation, STELLAR evolution, DWARF stars, STELLAR initial mass function
Abstract: We use Hubble Space Telescope observations from the Legacy Extragalactic UV Survey to reconstruct the recent star formation histories (SFHs) of three actively star-forming dwarf galaxies, NGC 4449, Holmberg II, and NGC 1705, from their UV color–magnitude diagrams (CMDs). We apply a CMD fitting technique using two independent sets of stellar isochrones, PARSEC-COLIBRI and MIST, to assess the uncertainties related to stellar evolution modeling. Irrespective of the adopted stellar models, all three dwarfs are found to have had almost constant star formation rates (SFRs) in the last 100–200 Myr, with modest enhancements (a factor of ∼2) above the 100 Myr averaged SFR. Significant differences among the three dwarfs are found in terms of the overall SFR, the timing of the most recent peak, and the SFR/area. The initial mass function of NGC 1705 and Holmberg II is consistent with a Salpeter slope down to ≈5 M⊙, whereas it is slightly flatter, s = −2.0, in NGC 4449. The SFHs derived with the two different sets of stellar models are consistent with each other, except for some quantitative details, attributable to their input assumptions. They also share the drawback that all synthetic diagrams predict a clear separation in color between the upper main-sequence and helium-burning stars, which is not apparent in the data. Since neither differential reddening, which is significant in NGC 4449, nor unresolved binaries appear to be sufficient to fill the gap, we suggest this calls for a revision of both sets of stellar evolutionary tracks. [ABSTRACT FROM AUTHOR]
Published: 2018
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26. Extinction Maps and Dust-to-gas Ratios in Nearby Galaxies with LEGUS.

Author: L. Kahre, R. A. Walterbos, H. Kim, D. Thilker, D. Calzetti, J. C. Lee, E. Sabbi, L. Ubeda, A. Aloisi, M. Cignoni, D. O. Cook, D. A. Dale, B. G. Elmegreen, D. M. Elmegreen, M. Fumagalli, J. S. Gallagher III, D. A. Gouliermis, K. Grasha, E. K Grebel, and D. A. Hunter
Subjects: SPECTRAL energy distribution, DWARF planets, OPTICAL images, BAYESIAN analysis, PHOTOMETRY
Abstract: We present a study of the dust-to-gas ratios in five nearby galaxies: NGC 628 (M74), NGC 6503, NGC 7793, UGC 5139 (Holmberg I), and UGC 4305 (Holmberg II). Using Hubble Space Telescope broadband WFC3/UVIS UV and optical images from the Treasury program Legacy ExtraGalactic UV Survey (LEGUS) combined with archival HST/Advanced Camera for Surveys data, we correct thousands of individual stars for extinction across these five galaxies using an isochrone-matching (reddening-free Q) method. We generate extinction maps for each galaxy from the individual stellar extinctions using both adaptive and fixed resolution techniques and correlate these maps with neutral H i and CO gas maps from the literature, including the H i Nearby Galaxy Survey and the HERA CO-Line Extragalactic Survey. We calculate dust-to-gas ratios and investigate variations in the dust-to-gas ratio with galaxy metallicity. We find a power-law relationship between dust-to-gas ratio and metallicity, consistent with other studies of dust-to-gas ratio compared to metallicity. We find a change in the relation when H2 is not included. This implies that underestimation of in low-metallicity dwarfs from a too-low CO-to-H2 conversion factor XCO could have produced too low a slope in the derived relationship between dust-to-gas ratio and metallicity. We also compare our extinctions to those derived from fitting the spectral energy distribution (SED) using the Bayesian Extinction and Stellar Tool for NGC 7793 and find systematically lower extinctions from SED fitting as compared to isochrone matching. [ABSTRACT FROM AUTHOR]
Published: 2018
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27. The Resolved Stellar Populations in the LEGUS Galaxies1.

Author: E. Sabbi, D. Calzetti, L. Ubeda, A. Adamo, M. Cignoni, D. Thilker, A. Aloisi, B. G. Elmegreen, D. M. Elmegreen, D. A. Gouliermis, E. K. Grebel, M. Messa, L. J. Smith, M. Tosi, A. Dolphin, J. E. Andrews, G. Ashworth, S. N. Bright, T. M. Brown, and R. Chandar
Published: 2018
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28. Hierarchical Star Formation in Turbulent Media: Evidence from Young Star Clusters.

Author: K. Grasha, B. G. Elmegreen, D. Calzetti, A. Adamo, A. Aloisi, S. N. Bright, D. O. Cook, D. A. Dale, M. Fumagalli, J. S. Gallagher III, D. A. Gouliermis, E. K. Grebel, L. Kahre, H. Kim, M. R. Krumholz, J. C. Lee, M. Messa, J. E. Ryon, and L. Ubeda
Subjects: STAR formation, TURBULENCE, AGE of stars, STAR clusters, ASTROPHYSICS
Abstract: We present an analysis of the positions and ages of young star clusters in eight local galaxies to investigate the connection between the age difference and separation of cluster pairs. We find that star clusters do not form uniformly but instead are distributed so that the age difference increases with the cluster pair separation to the 0.25–0.6 power, and that the maximum size over which star formation is physically correlated ranges from ∼200 pc to ∼1 kpc. The observed trends between age difference and separation suggest that cluster formation is hierarchical both in space and time: clusters that are close to each other are more similar in age than clusters born further apart. The temporal correlations between stellar aggregates have slopes that are consistent with predictions of turbulence acting as the primary driver of star formation. The velocity associated with the maximum size is proportional to the galaxy’s shear, suggesting that the galactic environment influences the maximum size of the star-forming structures. [ABSTRACT FROM AUTHOR]
Published: 2017
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29. Effective Radii of Young, Massive Star Clusters in Two LEGUS Galaxies.

Author: J. E. Ryon, J. S. Gallagher, L. J. Smith, A. Adamo, D. Calzetti, S. N. Bright, M. Cignoni, D. O. Cook, D. A. Dale, B. E. Elmegreen, M. Fumagalli, D. A. Gouliermis, K. Grasha, E. K. Grebel, H. Kim, M. Messa, D. Thilker, and L. Ubeda
Subjects: STAR clusters, SUPERGIANT stars, STELLAR density (Stellar population), GALAXY clusters, EXTRAGALACTIC distances
Abstract: We present a study of the effective (half-light) radii and other structural properties of a systematically selected sample of young, massive star clusters (≥5 × 103 and ≤200 Myr) in two nearby spiral galaxies, NGC 628 and NGC 1313. We use Hubble Space Telescope (HST) WFC3/UVIS and archival ACS/WFC data obtained by the Legacy Extragalactic UV Survey (LEGUS), an HST Treasury Program. We measure effective radii with GALFIT, a two-dimensional image-fitting package, and with a new technique to estimate effective radii from the concentration index of observed clusters. The distribution of effective radii from both techniques spans ∼0.5–10 pc and peaks at 2–3 pc for both galaxies. We find slight positive correlations between effective radius and cluster age in both galaxies, but no significant relationship between effective radius and galactocentric distance. Clusters in NGC 1313 display a mild increase in effective radius with cluster mass, but the trend disappears when the sample is divided into age bins. We show that the vast majority of the clusters in both galaxies are much older than their dynamical times, suggesting they are gravitationally bound objects. We find that about half of the clusters in NGC 628 are underfilling their Roche lobes, based on their Jacobi radii. Our results suggest that the young, massive clusters in NGC 628 and NGC 1313 are expanding, due to stellar mass loss or two-body relaxation, and are not significantly influenced by the tidal fields of their host galaxies. [ABSTRACT FROM AUTHOR]
Published: 2017
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30. The Hierarchical Distribution of the Young Stellar Clusters in Six Local Star-forming Galaxies.

Author: K. Grasha, D. Calzetti, A. Adamo, H. Kim, B. G. Elmegreen, D. A. Gouliermis, D. A. Dale, M. Fumagalli, E. K. Grebel, K. E. Johnson, L. Kahre, R. C. Kennicutt, M. Messa, A. Pellerin, J. E. Ryon, L. J. Smith, F. Shabani, D. Thilker, and L. Ubeda
Subjects: STAR clusters, STELLAR evolution, OPTICAL images, INTERSTELLAR medium, ROGUE planets
Abstract: We present a study of the hierarchical clustering of the young stellar clusters in six local (3–15 Mpc) star-forming galaxies using Hubble Space Telescope broadband WFC3/UVIS UV and optical images from the Treasury Program LEGUS (Legacy ExtraGalactic UV Survey). We identified 3685 likely clusters and associations, each visually classified by their morphology, and we use the angular two-point correlation function to study the clustering of these stellar systems. We find that the spatial distribution of the young clusters and associations are clustered with respect to each other, forming large, unbound hierarchical star-forming complexes that are in general very young. The strength of the clustering decreases with increasing age of the star clusters and stellar associations, becoming more homogeneously distributed after ∼40–60 Myr and on scales larger than a few hundred parsecs. In all galaxies, the associations exhibit a global behavior that is distinct and more strongly correlated from compact clusters. Thus, populations of clusters are more evolved than associations in terms of their spatial distribution, traveling significantly from their birth site within a few tens of Myr, whereas associations show evidence of disruption occurring very quickly after their formation. The clustering of the stellar systems resembles that of a turbulent interstellar medium that drives the star formation process, correlating the components in unbound star-forming complexes in a hierarchical manner, dispersing shortly after formation, suggestive of a single, continuous mode of star formation across all galaxies. [ABSTRACT FROM AUTHOR]
Published: 2017
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31. THE RADIAL VELOCITY EXPERIMENT (RAVE): FIFTH DATA RELEASE.

Author: Andrea Kunder, Georges Kordopatis, Matthias Steinmetz, Tomaž Zwitter, Paul J. McMillan, Luca Casagrande, Harry Enke, Jennifer Wojno, Marica Valentini, Cristina Chiappini, Gal Matijevič, Alessandro Siviero, Patrick de Laverny, Alejandra Recio-Blanco, Albert Bijaoui, Rosemary F. G. Wyse, James Binney, E. K. Grebel, Amina Helmi, and Paula Jofre
Published: 2017
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32. CHROMOSPHERICALLY ACTIVE STARS IN THE RAVE SURVEY. II. YOUNG DWARFS IN THE SOLAR NEIGHBORHOOD.

Author: M. Žerjal, T. Zwitter, G. Matijevič, E. K. Grebel, G. Kordopatis, U. Munari, G. Seabroke, M. Steinmetz, J. Wojno, O. Bienaymé, J. Bland-Hawthorn, C. Conrad, K. C. Freeman, B. K. Gibson, G. Gilmore, A. Kunder, J. Navarro, Q. A. Parker, W. Reid, and A. Siviero
Subjects: STELLAR chromospheres, DWARF stars, FIELD emission, STELLAR dynamics, WAVELENGTH measurement
Abstract: A large sample of over 38,000 chromospherically active candidate solar-like stars and cooler dwarfs from the RAVE survey is addressed in this paper. An improved activity identification with respect to the previous study was introduced to build a catalog of field stars in the solar neighborhood with an excess emission flux in the calcium infrared triplet wavelength region. The central result of this work is the calibration of the age–activity relation for main-sequence dwarfs in a range from a few up to a few Gyr. It enabled an order of magnitude age estimation of the entire active sample. Almost 15,000 stars are shown to be younger than and ∼2000 younger than . The young age of the most active stars is confirmed by their position off the main sequence in the J − K versus diagram showing strong ultraviolet excess, mid-infrared excess in the J − K versus diagram, and very cool temperatures (). They overlap with the reference pre-main-sequence RAVE stars often displaying X-ray emission. The activity level increasing with the color reveals their different nature from the solar-like stars and probably represents an underlying dynamo-generating magnetic fields in cool stars. Of the RAVE objects from DR5, 50% are found in the TGAS catalog and supplemented with accurate parallaxes and proper motions by Gaia. This makes the database of a large number of young stars in a combination with RAVE’s radial velocities directly useful as a tracer of the very recent large-scale star formation history in the solar neighborhood. The data are available online in the Vizier database. [ABSTRACT FROM AUTHOR]
Published: 2017
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33. HUBBLE TARANTULA TREASURY PROJECT. V. THE STAR CLUSTER HODGE 301: THE OLD FACE OF 30 DORADUS.

Author: M. Cignoni, E. Sabbi, R. P. Van Der Marel, D. J. Lennon, M. Tosi, E. K. Grebel, J. S. Gallagher Iii, A. Aloisi, G. De Marchi, D. A. Gouliermis, S. Larsen, N. Panagia, and L. J. Smith
Subjects: STAR clusters, STELLAR evolution, MAGELLANIC clouds, GALAXIES
Abstract: Based on color–magnitude diagrams (CMDs) from the Hubble Space Telescope Hubble Tarantula Treasury Project (HTTP) survey, we present the star formation history of Hodge 301, the oldest star cluster in the Tarantula Nebula. The HTTP photometry extends faint enough to reach, for the first time, the cluster pre-main sequence (PMS) turn-on, where the PMS joins the main sequence. Using the location of this feature, along with synthetic CMDs generated with the latest PARSEC models, we find that Hodge 301 is older than previously thought, with an age between 26.5 and 31.5 Myr. From this age, we also estimate that between 38 and 61 Type II supernovae exploded in the region. The same age is derived from the main sequence turn-off, whereas the age derived from the post-main sequence stars is younger and between 20 and 25 Myr. Other relevant parameters are a total stellar mass of ≈8800 ± 800 M⊙ and average reddening E(B − V) ≈ 0.22–0.24 mag, with a differential reddening δE(B − V) ≈ 0.04 mag. [ABSTRACT FROM AUTHOR]
Published: 2016
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34. THE EXTENDED SPATIAL DISTRIBUTION OF GLOBULAR CLUSTERS IN THE CORE OF THE FORNAX CLUSTER.

Author: R. D’Abrusco, M. Cantiello, M. Paolillo, V. Pota, N. R. Napolitano, L. Limatola, M. Spavone, A. Grado, E. Iodice, M. Capaccioli, R. Peletier, G. Longo, M. Hilker, S. Mieske, E. K. Grebel, T. Lisker, C. Wittmann, G. van de Ven, P. Schipani, and G. Fabbiano
Published: 2016
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35. HUBBLE TARANTULA TREASURY PROJECT. III. PHOTOMETRIC CATALOG AND RESULTING CONSTRAINTS ON THE PROGRESSION OF STAR FORMATION IN THE 30 DORADUS REGION.

Author: E. Sabbi, D. J. Lennon, J. Anderson, M. Cignoni, R. P. van der Marel, D. Zaritsky, G. De Marchi, N. Panagia, D. A. Gouliermis, E. K. Grebel, J. S. Gallagher III, L. J. Smith, H. Sana, A. Aloisi, M. Tosi, C. J. Evans, H. Arab, M. Boyer, S. E. de Mink, and K. Gordon
Published: 2016
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36. THE SPATIAL DISTRIBUTION OF THE YOUNG STELLAR CLUSTERS IN THE STAR-FORMING GALAXY NGC 628.

Author: K. Grasha, D. Calzetti, A. Adamo, H. Kim, B. G. Elmegreen, D. A. Gouliermis, A. Aloisi, S. N. Bright, C. Christian, M. Cignoni, D. A. Dale, C. Dobbs, D. M. Elmegreen, M. Fumagalli, J. S. Gallagher III, E. K. Grebel, K. E. Johnson, J. C. Lee, M. Messa, and L. J. Smith
Subjects: STAR clusters, STELLAR evolution, INTERSTELLAR medium, NEBULAE
Abstract: We present a study of the spatial distribution of the stellar cluster populations in the star-forming galaxy NGC 628. Using Hubble Space Telescope broadband WFC3/UVIS UV and optical images from the Treasury Program LEGUS (Legacy ExtraGalactic UV Survey), we have identified 1392 potential young ( Myr) stellar clusters within the galaxy using a combination of visual inspection and automatic selection. We investigate the clustering of these young stellar clusters and quantify the strength and change of clustering strength with scale using the two-point correlation function. We also investigate how image boundary conditions and dust lanes affect the observed clustering. The distribution of the clusters is well fit by a broken power law with negative exponent α. We recover a weighted mean index of for all spatial scales below the break at 3.″3 (158 pc at a distance of 9.9 Mpc) and an index of above 158 pc for the accumulation of all cluster types. The strength of the clustering increases with decreasing age and clusters older than 40 Myr lose their clustered structure very rapidly and tend to be randomly distributed in this galaxy, whereas the mass of the star cluster has little effect on the clustering strength. This is consistent with results from other studies that the morphological hierarchy in stellar clustering resembles the same hierarchy as the turbulent interstellar medium. [ABSTRACT FROM AUTHOR]
Published: 2015
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37. HUBBLE TARANTULA TREASURY PROJECT. II. THE STAR-FORMATION HISTORY OF THE STARBURST REGION NGC 2070 IN 30 DORADUS.

Author: M. Cignoni, E. Sabbi, R. P. van der Marel, M. Tosi, D. Zaritsky, J. Anderson, D. J. Lennon, A. Aloisi, G. de Marchi, D. A. Gouliermis, E. K. Grebel, L. J. Smith, and P. Zeidler
Subjects: STAR formation, LARGE magellanic cloud, GALAXIES, STAR clusters, HR diagrams
Abstract: We present a study of the recent star formation (SF) of 30 Doradus in the Large Magellanic Cloud (LMC) using the panchromatic imaging survey Hubble Tarantula Treasury Project. In this paper we focus on the stars within 20 pc of the center of 30 Doradus, the starburst region NGC 2070. We recovered the SF history by comparing deep optical and near-infrared color–magnitude diagrams (CMDs) with state-of-the-art synthetic CMDs generated with the latest PAdova and TRieste Stellar Evolution Code (PARSEC) models, which include all stellar phases from pre-main-sequence to post-main-sequence. For the first time in this region we are able to measure the SF using intermediate- and low-mass stars simultaneously. Our results suggest that NGC 2070 experienced prolonged activity. In particular, we find that the SF in the region (1) exceeded the average LMC rate ≈ 20 Myr ago, (2) accelerated dramatically ≈ 7 Myr ago, and (3) reached a peak value 1–3 Myr ago. We did not find significant deviations from a Kroupa initial mass function down to . The average internal reddening is found to be between 0.3 and 0.4 mag. [ABSTRACT FROM AUTHOR]
Published: 2015
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38. THE IMPRINTS OF THE GALACTIC BAR ON THE THICK DISK WITH RAVE.

Author: T. Antoja, G. Monari, A. Helmi, O. Bienaymé, J. Bland-Hawthorn, B. Famaey, B. K. Gibson, E. K. Grebel, G. Kordopatis, U. Munari, J. Navarro, Q. Parker, W. A. Reid, G. Seabroke, M. Steinmetz, and T. Zwitter
Published: 2015
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39. THE ABUNDANCE PROPERTIES OF NEARBY LATE-TYPE GALAXIES. II. THE RELATION BETWEEN ABUNDANCE DISTRIBUTIONS AND SURFACE BRIGHTNESS PROFILES.

Author: L. S. Pilyugin, E. K. Grebel, I. A. Zinchenko, and A. Y. Kniazev
Published: 2014
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40. Gaia Data Release 1: Testing parallaxes with local Cepheids and RR Lyrae stars

Author: Gaia Collaboration, Clementini, G., Eyer, L., Ripepi, V., Marconi, M., Muraveva, T., Garofalo, A., Sarro, L. M., Palmer, M., Luri, X., Molinaro, R., Rimoldini, L., Szabados, L., Musella, I., Anderson, R. I., Prusti, T., Bruijne, J. H. J., Brown, A. G. A., Vallenari, A., Babusiaux, C., Bailer-Jones, C. A. L., Bastian, U., Biermann, M., Evans, D. W., Jansen, F., Jordi, C., Klioner, S. A., Lammers, U., Lindegren, L., Mignard, F., Panem, C., Pourbaix, D., Randich, S., Sartoretti, P., Siddiqui, H. I., Soubiran, C., Valette, V., Leeuwen, F., Walton, N. A., Aerts, C., Arenou, F., Cropper, M., Drimmel, R., Høg, E., Katz, D., Lattanzi, M. G., O Mullane, W., Grebel, E. K., Holland, A. D., Huc, C., Passot, X., Perryman, M., Bramante, L., Cacciari, C., Castañeda, J., Chaoul, L., Cheek, N., Angeli, F., Fabricius, C., Guerra, R., Hernández, J., Jean-Azntoine-Piccolo, A., Masana, E., Messineo, R., Mowlavi, N., Nienartowicz, K., Ordóñez-Blanco, D., Panuzzo, P., Portell, J., Richards, P. J., Riello, M., Seabroke, G. M., Tanga, P., Thévenin, F., Torra, J., Els, S. G., Gracia-Abril, G., Comoretto, G., Garcia-Reinaldos, M., Lock, T., Mercier, E., Altmann, M., Andrae, R., Astraatmadja, T. L., Bellas-Velidis, I., Benson, K., Berthier, J., Blomme, R., Busso, G., Carry, B., Cellino, A., Cowell, S., Creevey, O., Cuypers, J., Davidson, M., Ridder, J., Torres, A., Delchambre, L., Oro, A., Ducourant, C., Frémat, Y., García-Torres, M., Gosset, E., Halbwachs, J. -L, Hambly, N. C., Harrison, D. L., Hauser, M., Hestroffer, D., Hodgkin, S. T., Huckle, H. E., Hutton, A., Jasniewicz, G., Jordan, S., Kontizas, M., Korn, A. J., Lanzafame, A. C., Manteiga, M., Moitinho, A., Muinonen, K., Osinde, J., Pancino, E., Pauwels, T., Petit, J. -M, Recio-Blanco, A., Robin, A. C., Siopis, C., Smith, M., Smith, K. W., Sozzetti, A., Thuillot, W., Reeven, W., Viala, Y., Abbas, U., Abreu Aramburu, A., Accart, S., Aguado, J. J., Allan, P. M., Allasia, W., Altavilla, G., Álvarez, M. A., Alves, J., Andrei, A. H., Anglada Varela, E., Antiche, E., Antoja, T., Antón, S., Arcay, B., Bach, N., Baker, S. G., Balaguer-Núñez, L., Barache, C., Barata, C., Barbier, A., Barblan, F., Barrado Y Navascués, D., Barros, M., Barstow, M. A., Becciani, U., Bellazzini, M., Bello García, A., Belokurov, V., Bendjoya, P., Berihuete, A., Bianchi, L., Bienaymé, O., Billebaud, F., Blagorodnova, N., Blanco-Cuaresma, S., Boch, T., Bombrun, A., Borrachero, R., Bouquillon, S., Bourda, G., Bouy, H., Bragaglia, A., Breddels, M. A., Brouillet, N., Brüsemeister, T., Bucciarelli, B., Burgess, P., Burgon, R., Burlacu, A., Busonero, D., Buzzi, R., Caffau, E., Cambras, J., Campbell, H., Cancelliere, R., Cantat-Gaudin, T., Carlucci, T., Carrasco, J. M., Castellani, M., Charlot, P., Charnas, J., Chiavassa, A., Clotet, M., Cocozza, G., Collins, R. S., Costigan, G., Crifo, F., Cross, N. J. G., Crosta, M., Crowley, C., Dafonte, C., Damerdji, Y., Dapergolas, A., David, P., David, M., Cat, P., Felice, F., Laverny, P., Luise, F., March, R., Souza, R., Debosscher, J., Del Pozo, E., Delbo, M., Delgado, A., Delgado, H. E., Di Matteo, P., Diakite, S., Distefano, E., Dolding, C., Dos Anjos, S., Drazinos, P., Durán, J., Dzigan, Y., Edvardsson, B., Enke, H., Evans, N. W., Eynard Bontemps, G., Fabre, C., Fabrizio, M., Faigler, S., Falcão, A. J., Farràs Casas, M., Federici, L., Fedorets, G., Fernández-Hernánde, J., Fernique, P., Fienga, A., Figueras, F., Filippi, F., Findeisen, K., Fonti, A., Fouesneau, M., Fraile, E., Fraser, M., Fuchs, J., Gai, M., Galleti, S., Galluccio, L., Garabato, D., García-Sedano, F., Garralda, N., Gavras, P., Gerssen, J., Geyer, R., Gilmore, G., Girona, S., Giuffrida, G., Gomes, M., González-Marcos, A., González-Núñez, J., González-Vidal, J. J., Granvik, M., Guerrier, A., Guillout, P., Guiraud, J., Gúrpide, A., Gutiérrez-Sánchez, R., Guy, L. P., Haigron, R., Hatzidimitriou, D., Haywood, M., Heiter, U., Helmi, A., Hobbs, D., Hofmann, W., Holl, B., Holland, G., Hunt, J. A. S., Hypki, A., Icardi, V., Irwin, M., Jevardat Fombelle, G., Jofré, P., Jonker, P. G., Jorissen, A., Julbe, F., Karampelas, A., Kochoska, A., Kohley, R., Kolenberg, K., Kontizas, E., Koposov, S. E., Kordopatis, G., Koubsky, P., Krone-Martins, A., Kudryashova, M., Kull, I., Bachchan, R. K., Lacoste-Seris, F., Lanza, A. F., Lavigne, J. -B, Le Poncin-Lafitte, C., Lebreton, Y., Lebzelter, T., Leccia, S., Leclerc, N., Lecoeur-Taibi, I., Lemaitre, V., Lenhardt, H., Leroux, F., Liao, S., Licata, E., Lindstrøm, H. E. P., Lister, T. A., Livanou, E., Lobel, A., Löffler, W., López, M., Lorenz, D., Macdonald, I., Magalhães Fernandes, T., Managau, S., Mann, R. G., Mantelet, G., Marchal, O., Marchant, J. M., Marinoni, S., Marrese, P. M., Marschalkó, G., Marshall, D. J., Martín-Fleitas, J. M., Martino, M., Mary, N., Matijevič, G., Mazeh, T., Mcmillan, P. J., Messina, S., Michalik, D., Millar, N. R., Miranda, B. M. H., Molina, D., Molinaro, M., Molnár, L., Moniez, M., Montegriffo, P., Mor, R., Mora, A., Morbidelli, R., Morel, T., Morgenthaler, S., Morris, D., Mulone, A. F., Narbonne, J., Nelemans, G., Nicastro, L., Noval, L., Ordénovic, C., Ordieres-Meré, J., Osborne, P., Pagani, C., Pagano, I., Pailler, F., Palacin, H., Palaversa, L., Parsons, P., Pecoraro, M., Pedrosa, R., Pentikäinen, H., Pichon, B., Piersimoni, A. M., Pineau, F. -X, Plachy, E., Plum, G., Poujoulet, E., Prša, A., Pulone, L., Ragaini, S., Rago, S., Rambaux, N., Ramos-Lerate, M., Ranalli, P., Rauw, G., Read, A., Regibo, S., Reylé, C., Ribeiro, R. A., Riva, A., Rixon, G., Roelens, M., Romero-Gómez, M., Rowell, N., Royer, F., Ruiz-Dern, L., Sadowski, G., Sagristà Sellés, T., Johannes Sahlmann, Salgado, J., Salguero, E., Sarasso, M., Savietto, H., Schultheis, M., Sciacca, E., Segol, M., Segovia, J. C., Segransan, D., Shih, I-C, Smareglia, R., Smart, R. L., Solano, E., Solitro, F., Sordo, R., Soria Nieto, S., Souchay, J., Spagna, A., Spoto, F., Stampa, U., Steele, I. A., Steidelmüller, H., Stephenson, C. A., Stoev, H., Suess, F. F., Süveges, M., Surdej, J., Szegedi-Elek, E., Tapiador, D., Taris, F., Tauran, G., Taylor, M. B., Teixeira, R., Terrett, D., Tingley, B., Trager, S. C., Turon, C., Ulla, A., Utrilla, E., Valentini, G., Elteren, A., Hemelryck, E., Leeuwen, M., Varadi, M., Vecchiato, A., Veljanoski, J., Via, T., Vicente, D., Vogt, S., Voss, H., Votruba, V., Voutsinas, S., Walmsley, G., Weiler, M., Weingrill, K., Wevers, T., Wyrzykowski, Ł., Yoldas, A., Žerjal, M., Zucker, S., Zurbach, C., Zwitter, T., Alecu, A., Allen, M., Allende Prieto, C., Amorim, A., Anglada-Escudé, G., Arsenijevic, V., Azaz, S., Balm, P., Beck, M., Bernstein, H. -H, Bigot, L., Bijaoui, A., Blasco, C., Bonfigli, M., Bono, G., Boudreault, S., Bressan, A., Brown, S., Brunet, P. -M, Bunclark, P., Buonanno, R., Butkevich, A. G., Carret, C., Carrion, C., Chemin, L., Chéreau, F., Corcione, L., Darmigny, E., Boer, K. S., Teodoro, P., Zeeuw, P. T., Delle Luche, C., Domingues, C. D., Dubath, P., Fodor, F., Frézouls, B., Fries, A., Fustes, D., Fyfe, D., Gallardo, E., Gallegos, J., Gardiol, D., Gebran, M., Gomboc, A., Gómez, A., Grux, E., Gueguen, A., Heyrovsky, A., Hoar, J., Iannicola, G., Isasi Parache, Y., Janotto, A. -M, Joliet, E., Jonckheere, A., Keil, R., Kim, D. -W, Klagyivik, P., Klar, J., Knude, J., Kochukhov, O., Kolka, I., Kos, J., Kutka, A., Lainey, V., Lebouquin, D., Liu, C., Loreggia, D., Makarov, V. V., Marseille, M. G., Martayan, C., Martinez-Rubi, O., Massart, B., Meynadier, F., Mignot, S., Munari, U., Nguyen, A. -T, Nordlander, T., O Flaherty, K. S., Ocvirk, P., Olias Sanz, A., Ortiz, P., Osorio, J., Oszkiewicz, D., Ouzounis, A., Park, P., Pasquato, E., Peltzer, C., Peralta, J., Péturaud, F., Pieniluoma, T., Pigozzi, E., Poels, J., Prat, G., Prod Homme, T., Raison, F., Rebordao, J. M., Risquez, D., Rocca-Volmerange, B., Rosen, S., Ruiz-Fuertes, M. I., Russo, F., Sembay, S., Serraller Vizcaino, I., Short, A., Siebert, A., Silva, H., Sinachopoulos, D., Slezak, E., Soffel, M., Sosnowska, D., Straižys, V., Ter Linden, M., Terrell, D., Theil, S., Tiede, C., Troisi, L., Tsalmantza, P., Tur, D., Vaccari, M., Vachier, F., Valles, P., Hamme, W., Veltz, L., Virtanen, J., Wallut, J. -M, Wichmann, R., Wilkinson, M. I., Ziaeepour, H., Zschocke, S., INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), Geneva Observatory, University of Geneva [Switzerland], INAF - Osservatorio Astronomico di Capodimonte (OAC), Dipartimento di Fisica e Astronomia [Bologna], Università di Bologna [Bologna] (UNIBO), Departamento de Inteligencia Artificial [UPM, Spain] (DIA), Universidad Politécnica de Madrid (UPM), Institut de Ciencies del Cosmos (ICCUB), Universitat de Barcelona (UB), Istituto Nazionale di Astrofisica (Istituto Nazionale di Astrofisica), Istituto Nazionale di Fisica Nucleare (INFN), Konkoly Observatory, Research Centre for Astronomy and Earth Sciences [Budapest], Hungarian Academy of Sciences (MTA)-Hungarian Academy of Sciences (MTA), University of California [Santa Cruz] (UCSC), University of California, Gastroenterology and Hepatology, Academic Medical Center - Academisch Medisch Centrum [Amsterdam] (AMC), University of Amsterdam [Amsterdam] (UvA)-University of Amsterdam [Amsterdam] (UvA), University of Manchester, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Aberystwyth University, Agence Spatiale Européenne (ESA), European Space Agency (ESA), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Human Cancer Genetics Program, Comprehensive Cancer Center-College of Medicine and Public Health [Colombus], Centre National d'Études Spatiales [Toulouse] (CNES), Instituut voor Sterrenkunde [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), University of Illinois at Urbana Champaign (UIUC), University of Illinois at Urbana-Champaign [Urbana], University of Illinois System-University of Illinois System, The Open University [Milton Keynes] (OU), Department of Biomedical, Metabolic and Neural Sciences [Modena], University of Las Palmas de Gran Canaria (ULPGC), Université de Montpellier (UM), Departament de Geodinamica i Geofısica, Facultat de Geologia, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institut Cochin (IC UM3 (UMR 8104 / U1016)), Institut National de la Santé et de la Recherche Médicale (INSERM)-Université Paris Descartes - Paris 5 (UPD5)-Centre National de la Recherche Scientifique (CNRS), European Space Astronomy Centre (ESAC), Professions, institutions, temporalités (PRINTEMPS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - Faculté des Sciences et des Techniques, Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Systèmes de Référence Temps Espace (SYRTE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), National Institute for Subatomic Physics Nikhef [Amsterdam] (NIKHEF), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Commissariat à l'énergie atomique et aux énergies alternatives - Laboratoire d'Electronique et de Technologie de l'Information (CEA-LETI), Direction de Recherche Technologique (CEA) (DRT (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Royal Observatory of Belgium [Brussels] (ROB), Open University of Israël, M2A 2017, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université de Picardie Jules Verne (UPJV), Laboratoire Univers et Particules de Montpellier (LUPM), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Department of Pathology and Cell Biology, Columbia University [New York], Department of Physics and Astronomy [Uppsala], Uppsala University, INAF - Osservatorio Astrofisico di Catania (OACT), Finnish Geospatial Research Institute (FGI), Helsinki Institute of Physics (HIP), University of Helsinki, Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), NASA Goddard Space Flight Center (GSFC), AUTRES, École Centrale de Nantes (ECN), University of Cambridge [UK] (CAM), EURIX (.), Fundaçao Cearense de Meteorologia e Recursos Hidricos, ARHEOINVEST, Universitatea Alexandru Ioan Cuza [Lasi], Institut d'écologie et des sciences de l'environnement de Paris (IEES), Institut National de la Recherche Agronomique (INRA)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Centre National de la Recherche Scientifique (CNRS), Department of Medicine, Icahn School of Medicine at Mount Sinai [New York] (MSSM), Department of Environmental Chemistry, IDAEA-CSIC, Institute of Environmental Assessment and Water Research (IDAEA), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology [2007-2019] (Grenoble INP [2007-2019])-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology [2007-2019] (Grenoble INP [2007-2019])-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Department of Physics and Astronomy [Leicester], University of Leicester, ASP 2017, FORMATION STELLAIRE 2017, Atotech Deutschland GmbH, Atotech, University of New South Wales [Sydney] (UNSW), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France, Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ), Institut de Biologie Intégrative de la Cellule (I2BC), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Institute of Astronomy [Leuven], Centre d'Immunologie et de Maladies Infectieuses (CIMI), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), Department of Computing, Electronics and Mechatronics, Universidad de las Américas [Puebla] (UDLAP), Swansea University, Cognition, Langues, Langage, Ergonomie (CLLE-ERSS), École pratique des hautes études (EPHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Toulouse - Jean Jaurès (UT2J)-Université Bordeaux Montaigne-Centre National de la Recherche Scientifique (CNRS), Scuola Internazionale Superiore di Studi Avanzati / International School for Advanced Studies (SISSA / ISAS), Computational Intelligence Research Group (CA3), Centre of Technology and Systems (CTS), Faculty of Sciences and Technology (FCT NOVA), Universidade Nova de Lisboa = NOVA University of Lisboa (NOVA)-Universidade Nova de Lisboa = NOVA University of Lisboa (NOVA)-Faculty of Sciences and Technology (FCT NOVA), Universidade Nova de Lisboa = NOVA University of Lisboa (NOVA)-Universidade Nova de Lisboa = NOVA University of Lisboa (NOVA)-Faculdade de Ciências e Tecnologia (FCT NOVA), Universidade Nova de Lisboa = NOVA University of Lisboa (NOVA), Géoazur (GEOAZUR 7329), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud]), Università degli Studi di Roma 'La Sapienza' [Rome], Laboratoire pour l'utilisation des lasers intenses (LULI), Université Pierre et Marie Curie - Paris 6 (UPMC)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Astrometry, INAF - Osservatorio Astrofisico di Torino (OATo), Istituto Nazionale di Astrofisica (INAF)-Istituto Nazionale di Astrofisica (INAF), Universidade de Lisboa (ULISBOA), Department of Mechanical, Informatics and Aerospace Engineering [León], Universidad de León [León], Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Sciences Pour l'Oenologie (SPO), Institut National de la Recherche Agronomique (INRA)-Université de Montpellier (UM)-Université Montpellier 1 (UM1)-Institut de Recherche pour le Développement (IRD [Nouvelle-Calédonie])-Institut national d’études supérieures agronomiques de Montpellier (Montpellier SupAgro), Institut national d'enseignement supérieur pour l'agriculture, l'alimentation et l'environnement (Institut Agro)-Institut national d'enseignement supérieur pour l'agriculture, l'alimentation et l'environnement (Institut Agro), Sciences Po Paris - Institut d'études politiques de Paris (IEP Paris), Laboratory of the Institute for Fiscal Studies (IFS), Institute for Fiscal Studies, Department of Physics [Athens], National and Kapodistrian University of Athens = University of Athens (NKUA | UoA), Department of Food & Nutritional Sciences, University of Reading (UOR), Heckscher-Klinikum, Northeast Structural Genomics Consortium, Department of Biological Sciences, Columbia University, New York, New York, USA., SRON Netherlands Institute for Space Research (SRON), Institut d'Astronomie et d'Astrophysique, Université libre de Bruxelles (ULB), Virulence bactérienne et maladies infectieuses (VBMI), Institut National de la Santé et de la Recherche Médicale (INSERM)-Université de Montpellier (UM), Thérapeutiques cliniques et expérimentales des infections (EA 3826) (EA 3826), Université de Nantes - UFR de Médecine et des Techniques Médicales (UFR MEDECINE), Université de Nantes (UN)-Université de Nantes (UN), Service de bactériologie et hygiène hospitalière [Nantes], Université de Nantes (UN)-Centre hospitalier universitaire de Nantes (CHU Nantes), Laboratoire national de métrologie et d'essais - Systèmes de Référence Temps-Espace (LNE - SYRTE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Institut de Physique de Rennes (IPR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Chinese Academy of Sciences [Beijing] (CAS), Atmel Corporation (ATMEL), ATMEL, Astrophysics Research Institute [Liverpool] (ARI), Liverpool John Moores University (LJMU), Institut de Génomique Fonctionnelle de Lyon (IGFL), École normale supérieure - Lyon (ENS Lyon)-Institut National de la Recherche Agronomique (INRA)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), Matériaux, ingénierie et science [Villeurbanne] (MATEIS), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherche sur la Fusion par confinement Magnétique (IRFM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), INAF - Osservatorio Astronomico di Trieste (OAT), Laboratoire SUBATECH Nantes (SUBATECH), Mines Nantes (Mines Nantes)-Université de Nantes (UN)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Universidad de Granada (UGR), RedZinc Services Ltd.[Dublin], Laboratoire de Physico -& Toxico Chimie des systèmes naturels (LPTC), Université Sciences et Technologies - Bordeaux 1-Centre National de la Recherche Scientifique (CNRS), Centre Atlantique de Philosophie (CAPHI), PRES Université Nantes Angers Le Mans (UNAM), GIRM, Instituto Politécnico de Leiria, Institut de Physique et Chimie des Matériaux de Strasbourg (IPCMS), Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique (CNRS), Institut du Cerveau et de la Moëlle Epinière = Brain and Spine Institute (ICM), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de la Santé et de la Recherche Médicale (INSERM)-CHU Pitié-Salpêtrière [AP-HP], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Centre National de la Recherche Scientifique (CNRS), Service de Neurologie [Hôpitaux Civils de Colmar], Hôpitaux Civils Colmar, National Observatory of Athens, Institute for Space Applications and Remote Sensing, Lund Observatory, Lund University [Lund], Laboratoire de Chimie, Catalyse, Polymères et Procédés, R 5265 (C2P2), Centre National de la Recherche Scientifique (CNRS)-École supérieure de Chimie Physique Electronique de Lyon (CPE)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon, Institut de recherche de l'European Business School (IREBS), European Business School Paris (EBS Paris), Département Réseaux, Information, Multimédia (RIM-ENSMSE), École des Mines de Saint-Étienne (Mines Saint-Étienne MSE), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT)-Centre G2I, Department of Biochemical and Chemical Engineering, Technische Universität Dortmund [Dortmund] (TU), Équipes de Recherches Interlangues : Mémoires, Identités, Territoires (ERIMIT), Université de Rennes 2 (UR2), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES), Université Panthéon-Sorbonne - UFR d'Économie (UP1 UFR02), Université Panthéon-Sorbonne (UP1), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Departamento de Astrofisica [Madrid], Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Spanish Virtual Observatory - Observatorio Virtual Español (SVO), Spanish Virtual Observatory - Observatorio Virtual Español, Department of Computer Science, Università degli Studi di Verona, Space Sciences, Technologies and Astrophysics Research Institute (STAR), Université de Liège, University of Toronto, Laboratory of Information, Network and Communication Sciences (LINCS), Institut Mines-Télécom [Paris] (IMT)-Institut National de Recherche en Informatique et en Automatique (Inria)-Université Pierre et Marie Curie - Paris 6 (UPMC), Dipartimento di Fisica, Politecnico di Milano [Milan] (POLIMI), LEI, Wageningen University and Research [Wageningen] (WUR), Karl-Franzens-Universität Graz, Herpetological Section, Zoologisches Forschungsmuseum Alexander Koenig, Chair of Hydrology, University of Freiburg, Department of Astrophysics [Nijmegen], Institute for Mathematics, Astrophysics and Particle Physics (IMAPP), Radboud university [Nijmegen]-Radboud university [Nijmegen], Department of Computer Science [Beer-Sheva], Ben-Gurion University of the Negev (BGU), The MITRE corporation, Laboratory for Systems, Instrumentation and Modeling in Science and Technology for Space and the Environment (University of Lisbon and University of Beira Interior), Technische Universität Dresden (TUD), Laboratori de Bromatologia i Toxicologia, Facultat de Farmàcia, Universitat de València (UV), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Centre for Immunity, Infection and Evolution, School of Biological Sciences, University of Edinburgh, Computer science department [University College London] (UCL-CS), Centre universitaire de Cytométrie, Imagerie et Mathématiques (CIM), Université de Limoges (UNILIM)-CHU Limoges, Department of Gastroenterology and Hepatology, VU University Medical Center [Amsterdam], Institut National de l'Information Géographique et Forestière [IGN] (IGN), ISDC (ISDC), Laboratoire d'Etudes Sociolinguistiques sur les Contacts de Langues et la Politique Linguistique (LESCLAP), Centre d'Immunologie de Marseille - Luminy (CIML), Aix Marseille Université (AMU)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Clemson], Clemson University, Faculty of Mathematics and Physics [Ljubljana] (FMF), University of Ljubljana, Instituto de Genetica Humana, Pontificia Universidad Javeriana, Universitad de la Sabana, Korea Advanced Institute of Science and Technology (KAIST), Faculty of Pharmacy, Faculty of Information and Communication Technologies, Swinburne University of Technology [Melbourne], Department of Psychiatry, Seaver Autism Center for Research and Treatment, European Southern Observatory (ESO), Centre de Recherches Pétrographiques et Géochimiques (CRPG), Institut national des sciences de l'Univers (INSU - CNRS)-Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), Service d'Endocrinologie, Diabétologie et Maladies Métaboliques (CHU de Dijon), Centre Hospitalier Universitaire de Dijon - Hôpital François Mitterrand (CHU Dijon), Innovalia Association, Department of Physics [Helsinki], Falculty of Science [Helsinki], University of Helsinki-University of Helsinki, Nordic Optical Telescope (NOT), Instituto de Astrofisica de Canarias (IAC), Royal Institute of Technology [Stockholm] (KTH ), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), EconomiX, Université Paris Nanterre (UPN)-Centre National de la Recherche Scientifique (CNRS), Instituto Nacional de Engenharia, Tecnologia e Inovacco (INETI), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Réhabilitation Chirurgicale mini-Invasive et Robotisée de l'Audition, Institut National de la Santé et de la Recherche Médicale (INSERM)-Université Pierre et Marie Curie - Paris 6 (UPMC), Service d'Otologie, Implants auditifs et Chirurgie de la base du crâne [CHU Pitié-Salpêtrière], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-CHU Pitié-Salpêtrière [AP-HP], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP), UNINOVA, Faculdade de Ciências e Tecnologia (FCT NOVA), Universidade Nova de Lisboa = NOVA University of Lisboa (NOVA)-Universidade Nova de Lisboa = NOVA University of Lisboa (NOVA), Sonoita Research Observatory, Biologie du fruit et pathologie (BFP), Université Sciences et Technologies - Bordeaux 1-Institut National de la Recherche Agronomique (INRA)-Université Bordeaux Segalen - Bordeaux 2, Institute of Physical Geodesy, Dipartimento di Astronomia [Padova], Universita degli Studi di Padova, Observatoire astronomique de Strasbourg (OAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique (CNRS), Centre d'études spatiales de la biosphère (CESBIO), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Météo France-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Centre National de la Recherche Scientifique (CNRS), Lohrmann Observatory, Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, Université Paris sciences et lettres (PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université de Rennes (UR), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Bordeaux (UB)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Bordeaux (UB), Centre National de la Recherche Scientifique (CNRS)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud]), Université de Lyon-Université de Lyon-École supérieure de Chimie Physique Electronique de Lyon (CPE)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Recherche en Informatique et en Automatique (Inria)-Institut Mines-Télécom [Paris] (IMT), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de la Santé et de la Recherche Médicale (INSERM), Università di Bologna [Bologna] ( UNIBO ), Institut de Physique et Chimie des Matériaux de Strasbourg ( IPCMS ), Université de Strasbourg ( UNISTRA ) -Centre National de la Recherche Scientifique ( CNRS ) -Matériaux et nanosciences d'Alsace, Université de Strasbourg ( UNISTRA ) -Université de Haute-Alsace (UHA) Mulhouse - Colmar ( Université de Haute-Alsace (UHA) ) -Institut National de la Santé et de la Recherche Médicale ( INSERM ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Strasbourg ( UNISTRA ) -Université de Haute-Alsace (UHA) Mulhouse - Colmar ( Université de Haute-Alsace (UHA) ) -Institut National de la Santé et de la Recherche Médicale ( INSERM ) -Centre National de la Recherche Scientifique ( CNRS ) -Réseau nanophotonique et optique, Université de Strasbourg ( UNISTRA ) -Université de Haute-Alsace (UHA) Mulhouse - Colmar ( Université de Haute-Alsace (UHA) ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Strasbourg ( UNISTRA ), School of Ocean and Earth Science, University of Southampton [Southampton], Istituto Nazionale di Astrofisica ( Istituto Nazionale di Astrofisica ), National Institute for Nuclear Physics ( INFN ), Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Hungarian Academy of Sciences [Budapest], University of California [Santa Cruz] ( UCSC ), Amsterdam Medical Center, Université de Manchester, Agence Spatiale Européenne ( ESA ), European Space Agency ( ESA ), Equipe EES, Ecologie et biologie des interactions ( EBI ), Université de Poitiers-Centre National de la Recherche Scientifique ( CNRS ) -Université de Poitiers-Centre National de la Recherche Scientifique ( CNRS ), Instituut voor Sterrenkunde, Faculteit Wetenschappen, Galaxies, Etoiles, Physique, Instrumentation ( GEPI ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), University of Illinois at Urbana Champaign ( UIUC ), The Open University [Milton Keynes] ( OU ), Centre National d'Etudes Spatiales ( CNES ), Università degli Studi di Modena e Reggio Emilia [Reggio Emilia] ( UNIMORE ), University of Las Palmas de Gran Canaria ( ULPGC ), Université de Montpellier ( UM ), Universitat de Barcelona ( UB ), Astrophysique Interactions Multi-échelles ( AIM - UMR 7158 - UMR E 9005 ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Paris Diderot - Paris 7 ( UPD7 ), Institut Cochin ( UM3 (UMR 8104 / U1016) ), Université Paris Descartes - Paris 5 ( UPD5 ) -Institut National de la Santé et de la Recherche Médicale ( INSERM ) -Centre National de la Recherche Scientifique ( CNRS ), Joseph Louis LAGRANGE ( LAGRANGE ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), AP-HP - Hôpital Cochin Broca Hôtel Dieu [Paris], European Space Astronomy Center ( ESAC ), Professions, institutions, temporalités ( PRINTEMPS ), Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Planétologie et Géodynamique de Nantes ( LPG ), Centre National de la Recherche Scientifique ( CNRS ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Université de Nantes ( UN ), Systèmes de Référence Temps Espace ( SYRTE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Centre National de la Recherche Scientifique ( CNRS ), FOM Instituut voor Subatomaire Fysica Nikhef, Mullard Space Science Laboratory ( MSSL ), University College of London [London] ( UCL ), Laboratoire d'Electronique et des Technologies de l'Information ( CEA-LETI ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Grenoble Alpes [Saint Martin d'Hères], Royal Observatory of Belgium [Brussels], European Space Astronomy Centre, Institut d'astrophysique spatiale ( IAS ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'Astrophysique de Bordeaux [Pessac] ( LAB ), Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Université de Picardie Jules Verne ( UPJV ), Laboratoire Univers et Particules de Montpellier ( LUPM ), Université Montpellier 2 - Sciences et Techniques ( UM2 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université de Montpellier ( UM ) -Centre National de la Recherche Scientifique ( CNRS ), INAF - Osservatorio Astrofisico di Catania ( OACT ), Istituto Nazionale di Astrofisica ( INAF ), Finnish Geospatial Research Institute ( FGI ), Helsinki Institute of Physics ( HIP ), University of Helsinki [Helsinki], GRAMAT ( DAM/GRAMAT ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) ( UTINAM ), Université de Franche-Comté ( UFC ) -Centre National de la Recherche Scientifique ( CNRS ) -Institut national des sciences de l'Univers ( INSU - CNRS ), NASA Goddard Space Flight Center ( GSFC ), Institut de Mécanique Céleste et de Calcul des Ephémérides ( IMCCE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université de Lille-Centre National de la Recherche Scientifique ( CNRS ), Observatoire de Paris - Site de Paris ( OP ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Centre National de la Recherche Scientifique ( CNRS ), École Centrale de Nantes ( ECN ), University of Cambridge [UK] ( CAM ), Univ. A. I. Cuza, Institut d'écologie et des sciences de l'environnement de Paris ( IEES ), Centre National de la Recherche Scientifique ( CNRS ) -Université Paris-Est Créteil Val-de-Marne - Paris 12 ( UPEC UP12 ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de la Recherche Agronomique ( INRA ), Mount Sinai School of Medicine, Spanish National Research Council ( CSIC ), Università degli studi di Catania [Catania], Institut de Planétologie et d'Astrophysique de Grenoble ( IPAG ), Observatoire des Sciences de l'Univers de Grenoble ( OSUG ), Université Joseph Fourier - Grenoble 1 ( UJF ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Grenoble Alpes ( UGA ) -Université Joseph Fourier - Grenoble 1 ( UJF ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Grenoble Alpes ( UGA ) -Centre National de la Recherche Scientifique ( CNRS ), Université Côte d'Azur ( UCA ), University of New South Wales [Sydney] ( UNSW ), Centre de Recherches Anglophones ( CREA (EA 370) ), Université Paris Nanterre ( UPN ), Centre d'étude spatiale des rayonnements ( CESR ), Université Toulouse III - Paul Sabatier ( UPS ), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Observatoire de Haute-Provence ( OHP ), Institut Pythéas ( OSU PYTHEAS ), Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture ( IRSTEA ) -Institut de Recherche pour le Développement ( IRD ) -Aix Marseille Université ( AMU ) -Centre National de la Recherche Scientifique ( CNRS ) -Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture ( IRSTEA ) -Institut de Recherche pour le Développement ( IRD ) -Aix Marseille Université ( AMU ) -Centre National de la Recherche Scientifique ( CNRS ), Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ), Institut de Biologie Intégrative de la Cellule ( I2BC ), Université Paris-Sud - Paris 11 ( UP11 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay-Centre National de la Recherche Scientifique ( CNRS ), Katholieke Universiteit Leuven ( KU Leuven ), UNS-CNRS-Observatoire de la Côte d'Azur, Centre d'Immunologie et de Maladies Infectieuses ( CIMI ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de la Santé et de la Recherche Médicale ( INSERM ) -Centre National de la Recherche Scientifique ( CNRS ), Universidad de las Américas [Puebla] ( UDLAP ), Cognition, Langues, Langage, Ergonomie ( CLLE-ERSS ), École pratique des hautes études ( EPHE ) -Université Toulouse - Jean Jaurès ( UT2J ) -Université Bordeaux Montaigne-Centre National de la Recherche Scientifique ( CNRS ), Scuola Internazionale Superiore di Studi Avanzati / International School for Advanced Studies ( SISSA / ISAS ), Computational Intelligence Research Group [Caparica] ( CA3 ), Universidade Nova de Lisboa ( UNINOVA ) -Centre of Technology and Systems ( CTS ), INAF - Osservatorio Astronomico di Bologna ( OABO ), Géoazur ( GEOAZUR ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de la Côte d'Azur, Laboratoire pour l'utilisation des lasers intenses ( LULI ), Université Paris-Saclay-Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -École polytechnique ( X ) -Centre National de la Recherche Scientifique ( CNRS ), INAF - Osservatorio Astrofisico di Torino ( OATo ), Istituto Nazionale di Astrofisica ( INAF ) -Istituto Nazionale di Astrofisica ( INAF ), Universidade de Lisboa ( ULISBOA ), University of León, Observatoire astronomique de Strasbourg ( ObAS ), Université de Strasbourg ( UNISTRA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Sciences Pour l'Oenologie ( SPO ), Université Montpellier 1 ( UM1 ) -Institut de Recherche pour le Développement ( IRD [Nouvelle-Calédonie] ) -Institut National de la Recherche Agronomique ( INRA ) -Université de Montpellier ( UM ) -Institut national d’études supérieures agronomiques de Montpellier ( Montpellier SupAgro ), Sciences Po Paris - Institut d'études politiques de Paris ( IEP Paris ), Laboratory of the Institute for Fiscal Studies ( IFS ), Department of Physics (Athens), University of Reading ( UOR ), SRON Netherlands Institute for Space Research ( SRON ), Université Libre de Bruxelles [Bruxelles] ( ULB ), The Institute of Environmental Medicine [Stockholm] ( IMM ), Karolinska Institutet [Stockholm], Virulence bactérienne et maladies infectieuses, Université de Montpellier ( UM ) -Institut National de la Santé et de la Recherche Médicale ( INSERM ), Thérapeutiques Cliniques et Expérimentales des Infections, Université de Nantes ( UN ), Université de Nantes ( UN ) -Centre hospitalier universitaire de Nantes ( CHU Nantes ), Laboratoire national de métrologie et d'essais - Systèmes de Référence Temps-Espace ( LNE - SYRTE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Centre National de la Recherche Scientifique ( CNRS ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Centre National de la Recherche Scientifique ( CNRS ), Institut de Physique de Rennes ( IPR ), Université de Rennes 1 ( UR1 ), Université de Rennes ( UNIV-RENNES ) -Université de Rennes ( UNIV-RENNES ) -Centre National de la Recherche Scientifique ( CNRS ), Chinese Academy of Sciences [Beijing] ( CAS ), Atmel Corporation ( ATMEL ), Institut Camille Jordan [Villeurbanne] ( ICJ ), École Centrale de Lyon ( ECL ), Université de Lyon-Université de Lyon-Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Institut National des Sciences Appliquées de Lyon ( INSA Lyon ), Université de Lyon-Institut National des Sciences Appliquées ( INSA ) -Institut National des Sciences Appliquées ( INSA ) -Université Jean Monnet [Saint-Étienne] ( UJM ) -Centre National de la Recherche Scientifique ( CNRS ), Astrophysics Research Institute [Liverpool] ( ARI ), Liverpool John Moores University ( LJMU ), Institut de Génomique Fonctionnelle de Lyon ( IGFL ), École normale supérieure - Lyon ( ENS Lyon ) -Institut National de la Recherche Agronomique ( INRA ) -Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique ( CNRS ), Matériaux, ingénierie et science [Villeurbanne] ( MATEIS ), Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique ( CNRS ) -Institut National des Sciences Appliquées de Lyon ( INSA Lyon ), Université de Lyon-Institut National des Sciences Appliquées ( INSA ) -Institut National des Sciences Appliquées ( INSA ), Institut de Recherche sur la Fusion par confinement Magnétique ( IRFM ), INAF - Osservatorio Astronomico di Trieste ( OAT ), Laboratoire SUBATECH Nantes ( SUBATECH ), Mines Nantes ( Mines Nantes ) -Université de Nantes ( UN ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de l'Accélérateur Linéaire ( LAL ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Universidad de Granada ( UGR ), Laboratoire de Physico -& Toxico Chimie des systèmes naturels ( LPTC ), Université Sciences et Technologies - Bordeaux 1-Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides ( CASSIOPEE ), Centre Atlantique de Philosophie ( CAPHI ), PRES Université Nantes Angers Le Mans ( UNAM ), Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique ( CNRS ), Institut du Cerveau et de la Moëlle Epinière = Brain and Spine Institute ( ICM ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de la Santé et de la Recherche Médicale ( INSERM ) -CHU Pitié-Salpêtrière [APHP]-Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Chimie, Catalyse, Polymères et Procédés, R 5265 ( C2P2 ), Centre National de la Recherche Scientifique ( CNRS ) -École supérieure de Chimie Physique Electronique de Lyon ( CPE ) -Université Claude Bernard Lyon 1 ( UCBL ), Institut de recherche de l'European Business School ( IREBS ), European Business School, Département Réseaux, Information, Multimédia ( RIM-ENSMSE ), École des Mines de Saint-Étienne ( Mines Saint-Étienne MSE ), Institut Mines-Télécom [Paris]-Institut Mines-Télécom [Paris]-Centre G2I, Technische Universität Dortmund [Dortmund] ( TU ), Équipes de Recherches Interlangues : Mémoires, Identités, Territoires ( ERIMIT ), Université de Rennes 2 ( UR2 ), Université de Rennes ( UNIV-RENNES ) -Université de Rennes ( UNIV-RENNES ), Université Panthéon-Sorbonne - UFR d'Économie ( UP1 UFR02 ), Université Panthéon-Sorbonne ( UP1 ), Observatoire Astronomique de l'Université de Genève ( ObsGE ), Université de Genève ( UNIGE ), Centro de Astrobiologia, Departamento de Astrofisica ( INTA-CSIC ), Centro de Astrobiología, Spanish Virtual Observatory - Observatorio Virtual Español ( SVO ), Space Sciences, Technologies and Astrophysics Research Institute ( STAR ), Laboratory of Information, Network and Communication Sciences ( LINCS ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de Recherche en Informatique et en Automatique ( Inria ) -Institut Mines-Télécom [Paris], Politecnico di Milano [Milan], Wageningen University and Research Centre [Wageningen] ( WUR ), Institute for Mathematics, Astrophysics and Particle Physics ( IMAPP ), Ben-Gurion University of the Negev ( BGU ), Ben Gurion University, Laboratory for Systems, Instrumentation and Modeling in Science and Technology for Space and the Environment ( University of Lisbon and University of Beira Interior ), Technische Universität Dresden ( TUD ), Mobilités : Vieillissement, Pathologie, Santé ( COMETE ), Institut National de la Santé et de la Recherche Médicale ( INSERM ) -Université de Caen Normandie ( UNICAEN ), Normandie Université ( NU ) -Normandie Université ( NU ), Universitat de València ( UV ), Max-Planck-Institut für Sonnensystemforschung ( MPS ), Computer science department [University College London] ( UCL-CS ), Centre universitaire de Cytométrie, Imagerie et Mathématiques ( CIM ), Université de Limoges ( UNILIM ) -CHU Limoges, School of psychology, University of Plymouth, Institut National de l'Information Géographique et Forestière [IGN] ( IGN ), ISDC ( ISDC ), Laboratoire d'Etudes Sociolinguistiques sur les Contacts de Langues et la Politique Linguistique ( LESCLAP ), Centre d'Immunologie de Marseille - Luminy ( CIML ), Institut National de la Santé et de la Recherche Médicale ( INSERM ) -Aix Marseille Université ( AMU ) -Centre National de la Recherche Scientifique ( CNRS ), Faculty of Mathematics and Physics [Ljubljana] ( FMF ), Universidad de la Sabana, Korea Advanced Institute of Science and Technology ( KAIST ), Icahn School of Medicine at Mount Sinai [New York], European Southern Observatory ( ESO ), Centre de Recherches Pétrographiques et Géochimiques ( CRPG ), Université de Lorraine ( UL ) -Centre National de la Recherche Scientifique ( CNRS ), Centre Hospitalier Universitaire de Dijon - Hôpital François Mitterrand ( CHU Dijon ), Nordic Optical Telescope ( NOT ), Instituto de Astrofisica de Canarias ( IAC ), Royal Institute of Technology [Stockholm] ( KTH ), Instituto de Astrofísica de Andalucía ( IAA ), Consejo Superior de Investigaciones Científicas [Spain] ( CSIC ), Université Paris Nanterre ( UPN ) -Centre National de la Recherche Scientifique ( CNRS ), Instituto Nacional de Engenharia, Tecnologia e Inovacco ( INETI ), INETI, Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Institut National de la Santé et de la Recherche Médicale ( INSERM ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ), Assistance publique - Hôpitaux de Paris (AP-HP)-CHU Pitié-Salpêtrière [APHP], Institut des sciences analytiques et de physico-chimie pour l'environnement et les materiaux ( IPREM ), Université de Pau et des Pays de l'Adour ( UPPA ) -Centre National de la Recherche Scientifique ( CNRS ), Biologie du fruit et pathologie ( BFP ), Université Bordeaux Segalen - Bordeaux 2-Institut National de la Recherche Agronomique ( INRA ) -Université Sciences et Technologies - Bordeaux 1, Dipartimento di Astronomia, Observatoire astronomique de Strasbourg ( OAS ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique ( CNRS ), Centre d'études spatiales de la biosphère ( CESBIO ), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National d'Etudes Spatiales ( CNES ) -Centre National de la Recherche Scientifique ( CNRS ), Astronomy, Departamento de Inteligencia Artificial, Universidad, National Institute for Nuclear Physics (INFN), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris Descartes - Paris 5 (UPD5)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Planétologie et Géodynamique UMR6112 (LPG), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Nantes - Faculté des Sciences et des Techniques, Université de Nantes (UN)-Université de Nantes (UN)-Université d'Angers (UA), Laboratoire d'Electronique et des Technologies de l'Information (CEA-LETI), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Institut UTINAM (Univers, transport, interfaces, nanostructures, atmosphère et environnement, molécules) (Besançon), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de la Recherche Agronomique (INRA), Spanish National Research Council (CSIC), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay, École pratique des hautes études (EPHE)-Université Toulouse - Jean Jaurès (UT2J)-Université Bordeaux Montaigne-Centre National de la Recherche Scientifique (CNRS), Universidade Nova de Lisboa (NOVA)-Universidade Nova de Lisboa (NOVA)-Faculty of Sciences and Technology (FCT NOVA), Universidade Nova de Lisboa (NOVA)-Universidade Nova de Lisboa (NOVA)-Faculdade de Ciências e Tecnologia (FCT NOVA), Universidade Nova de Lisboa (NOVA), Institut national des sciences de l'Univers (INSU - CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud])-Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA), Université Paris-Saclay-Université Pierre et Marie Curie - Paris 6 (UPMC)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Université Montpellier 1 (UM1)-Institut de Recherche pour le Développement (IRD [Nouvelle-Calédonie])-Institut National de la Recherche Agronomique (INRA)-Université de Montpellier (UM)-Institut national d’études supérieures agronomiques de Montpellier (Montpellier SupAgro), Université Libre de Bruxelles [Bruxelles] (ULB), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de la Santé et de la Recherche Médicale (INSERM)-CHU Pitié-Salpêtrière [APHP]-Centre National de la Recherche Scientifique (CNRS), Wageningen University and Research Centre [Wageningen] (WUR), Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Aix Marseille Université (AMU), Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), Assistance publique - Hôpitaux de Paris (AP-HP) (APHP)-CHU Pitié-Salpêtrière [APHP], Institut des sciences analytiques et de physico-chimie pour l'environnement et les materiaux (IPREM), Université de Pau et des Pays de l'Adour (UPPA)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), ITA, GBR, FRA, DEU, ESP, BEL, FIN, Gaia Collaboration, G. Clementini, L. Eyer, V. Ripepi, M. Marconi, T. Muraveva, A. Garofalo, L. M. Sarro, M. Palmer, X. Luri, R. Molinaro, L. Rimoldini, L. Szabado, I. Musella, R. I. Anderson, T. Prusti, J. H. J. de Bruijne, A. G. A. Brown, A. Vallenari, C. Babusiaux, C. A. L. Bailer-Jone, U. Bastian, M. Biermann, D. W. Evan, F. Jansen, C. Jordi, S. A. Klioner, U. Lammer, L. Lindegren, F. Mignard, C. Panem, D. Pourbaix, S. Randich, P. Sartoretti, H. I. Siddiqui, C. Soubiran, V. Valette, F. van Leeuwen, N. A. Walton, C. Aert, F. Arenou, M. Cropper, R. Drimmel, E. Høg, D. Katz, M. G. Lattanzi, W. O'Mullane, E. K. Grebel, A. D. Holland, C. Huc, X. Passot, M. Perryman, L. Bramante, C. Cacciari, J. Castañeda, L. Chaoul, N. Cheek, F. De Angeli, C. Fabriciu, R. Guerra, J. Hernández, A. Jean-Azntoine-Piccolo, E. Masana, R. Messineo, N. Mowlavi, K. Nienartowicz, D. Ordóñez-Blanco, P. Panuzzo, J. Portell, P. J. Richard, M. Riello, G. M. Seabroke, P. Tanga, F. Thévenin, J. Torra, S. G. El, G. Gracia-Abril, G. Comoretto, M. Garcia-Reinaldo, T. Lock, E. Mercier, M. Altmann, R. Andrae, T. L. Astraatmadja, I. Bellas-Velidi, K. Benson, J. Berthier, R. Blomme, G. Busso, B. Carry, A. Cellino, S. Cowell, O. Creevey, J. Cuyper, M. Davidson, J. De Ridder, A. de Torre, L. Delchambre, A. Dell'Oro, C. Ducourant, Y. Frémat, M. García-Torre, E. Gosset, J. -L. Halbwach, N. C. Hambly, D. L. Harrison, M. Hauser, D. Hestroffer, S. T. Hodgkin, H. E. Huckle, A. Hutton, G. Jasniewicz, S. Jordan, M. Kontiza, A. J. Korn, A. C. Lanzafame, M. Manteiga, A. Moitinho, K. Muinonen, J. Osinde, E. Pancino, T. Pauwel, J. -M. Petit, A. Recio-Blanco, A. C. Robin, C. Siopi, M. Smith, K. W. Smith, A. Sozzetti, W. Thuillot, W. van Reeven, Y. Viala, U. Abba, A. Abreu Aramburu, S. Accart, J. J. Aguado, P. M. Allan, W. Allasia, G. Altavilla, M. A. Álvarez, J. Alve, A. H. Andrei, E. Anglada Varela, E. Antiche, T. Antoja, S. Antón, B. Arcay, N. Bach, S. G. Baker, L. Balaguer-Núñez, C. Barache, C. Barata, A. Barbier, F. Barblan, D. Barrado y Navascué, M. Barro, M. A. Barstow, U. Becciani, M. Bellazzini, A. Bello García, V. Belokurov, P. Bendjoya, A. Berihuete, L. Bianchi, O. Bienaymé, F. Billebaud, N. Blagorodnova, S. Blanco-Cuaresma, T. Boch, A. Bombrun, R. Borrachero, S. Bouquillon, G. Bourda, H. Bouy, A. Bragaglia, M. A. Breddel, N. Brouillet, T. Brüsemeister, B. Bucciarelli, P. Burge, R. Burgon, A. Burlacu, D. Busonero, R. Buzzi, E. Caffau, J. Cambra, H. Campbell, R. Cancelliere, T. Cantat-Gaudin, T. Carlucci, J. M. Carrasco, M. Castellani, P. Charlot, J. Charna, A. Chiavassa, M. Clotet, G. Cocozza, R. S. Collin, G. Costigan, F. Crifo, N. J. G. Cro, M. Crosta, C. Crowley, C. Dafonte, Y. Damerdji, A. Dapergola, P. David, M. David, P. De Cat, F. de Felice, P. de Laverny, F. De Luise, R. De March, R. de Souza, J. Debosscher, E. del Pozo, M. Delbo, A. Delgado, H. E. Delgado, P. Di Matteo, S. Diakite, E. Distefano, C. Dolding, S. Dos Anjo, P. Drazino, J. Durán, Y. Dzigan, B. Edvardsson, H. Enke, N. W. Evan, G. Eynard Bontemp, C. Fabre, M. Fabrizio, S. Faigler, A. J. Falcão, M. Farràs Casa, L. Federici, G. Fedoret, J. Fernández-Hernánde, P. Fernique, A. Fienga, F. Figuera, F. Filippi, K. Findeisen, A. Fonti, M. Fouesneau, E. Fraile, M. Fraser, J. Fuch, M. Gai, S. Galleti, L. Galluccio, D. Garabato, F. García-Sedano, N. Garralda, P. Gavra, J. Gerssen, R. Geyer, G. Gilmore, S. Girona, G. Giuffrida, M. Gome, A. González-Marco, J. González-Núñez, J. J. González-Vidal, M. Granvik, A. Guerrier, P. Guillout, J. Guiraud, A. Gúrpide, R. Gutiérrez-Sánchez, L. P. Guy, R. Haigron, D. Hatzidimitriou, M. Haywood, U. Heiter, A. Helmi, D. Hobb, W. Hofmann, B. Holl, G. Holland, J. A. S. Hunt, A. Hypki, V. Icardi, M. Irwin, G. Jevardat de Fombelle, P. Jofré, P. G. Jonker, A. Jorissen, F. Julbe, A. Karampela, A. Kochoska, R. Kohley, K. Kolenberg, E. Kontiza, S. E. Koposov, G. Kordopati, P. Koubsky, A. Krone-Martin, M. Kudryashova, I. Kull, R. K. Bachchan, F. Lacoste-Seri, A. F. Lanza, J. -B. Lavigne, C. Le Poncin-Lafitte, Y. Lebreton, T. Lebzelter, S. Leccia, N. Leclerc, I. Lecoeur-Taibi, V. Lemaitre, H. Lenhardt, F. Leroux, S. Liao, E. Licata, H. E. P. Lindstrøm, T. A. Lister, E. Livanou, A. Lobel, W. Löffler, M. López, D. Lorenz, I. MacDonald, T. Magalhães Fernande, S. Managau, R. G. Mann, G. Mantelet, O. Marchal, J. M. Marchant, S. Marinoni, P. M. Marrese, G. Marschalkó, D. J. Marshall, J. M. Martín-Fleita, M. Martino, N. Mary, G. Matijevič, T. Mazeh, P. J. McMillan, S. Messina, D. Michalik, N. R. Millar, B. M. H. Miranda, D. Molina, M. Molinaro, L. Molnár, M. Moniez, P. Montegriffo, R. Mor, A. Mora, R. Morbidelli, T. Morel, S. Morgenthaler, D. Morri, A. F. Mulone, J. Narbonne, G. Neleman, L. Nicastro, L. Noval, C. Ordénovic, J. Ordieres-Meré, P. Osborne, C. Pagani, I. Pagano, F. Pailler, H. Palacin, L. Palaversa, P. Parson, M. Pecoraro, R. Pedrosa, H. Pentikäinen, B. Pichon, A. M. Piersimoni, F. -X. Pineau, E. Plachy, G. Plum, E. Poujoulet, A. Prša, L. Pulone, S. Ragaini, S. Rago, N. Rambaux, M. Ramos-Lerate, P. Ranalli, G. Rauw, A. Read, S. Regibo, C. Reylé, R. A. Ribeiro, A. Riva, G. Rixon, M. Roelen, M. Romero-Gómez, N. Rowell, F. Royer, L. Ruiz-Dern, G. Sadowski, T. Sagristà Sellé, J. Sahlmann, J. Salgado, E. Salguero, M. Sarasso, H. Savietto, M. Schulthei, E. Sciacca, M. Segol, J. C. Segovia, D. Segransan, I-C. Shih, R. Smareglia, R. L. Smart, E. Solano, F. Solitro, R. Sordo, S. Soria Nieto, J. Souchay, A. Spagna, F. Spoto, U. Stampa, I. A. Steele, H. Steidelmüller, C. A. Stephenson, H. Stoev, F. F. Sue, M. Süvege, J. Surdej, E. Szegedi-Elek, D. Tapiador, F. Tari, G. Tauran, M. B. Taylor, R. Teixeira, D. Terrett, B. Tingley, S. C. Trager, C. Turon, A. Ulla, E. Utrilla, G. Valentini, A. van Elteren, E. Van Hemelryck, M. van Leeuwen, M. Varadi, A. Vecchiato, J. Veljanoski, T. Via, D. Vicente, S. Vogt, H. Vo, V. Votruba, S. Voutsina, G. Walmsley, M. Weiler, K. Weingrill, T. Wever, Ł. Wyrzykowski, A. Yolda, M. Žerjal, S. Zucker, C. Zurbach, T. Zwitter, A. Alecu, M. Allen, C. Allende Prieto, A. Amorim, G. Anglada-Escudé, V. Arsenijevic, S. Azaz, P. Balm, M. Beck, H. -H. Bernstein, L. Bigot, A. Bijaoui, C. Blasco, M. Bonfigli, G. Bono, S. Boudreault, A. Bressan, S. Brown, P. -M. Brunet, P. Bunclark, R. Buonanno, A. G. Butkevich, C. Carret, C. Carrion, L. Chemin, F. Chéreau, L. Corcione, E. Darmigny, K. S. de Boer, P. de Teodoro, P. T. de Zeeuw, C. Delle Luche, C. D. Domingue, P. Dubath, F. Fodor, B. Frézoul, A. Frie, D. Fuste, D. Fyfe, E. Gallardo, J. Gallego, D. Gardiol, M. Gebran, A. Gomboc, A. Gómez, E. Grux, A. Gueguen, A. Heyrovsky, J. Hoar, G. Iannicola, Y. Isasi Parache, A. -M. Janotto, E. Joliet, A. Jonckheere, R. Keil, D. -W. Kim, P. Klagyivik, J. Klar, J. Knude, O. Kochukhov, I. Kolka, J. Ko, A. Kutka, V. Lainey, D. LeBouquin, C. Liu, D. Loreggia, V. V. Makarov, M. G. Marseille, C. Martayan, O. Martinez-Rubi, B. Massart, F. Meynadier, S. Mignot, U. Munari, A. -T. Nguyen, T. Nordlander, K. S. O'Flaherty, P. Ocvirk, A. Olias Sanz, P. Ortiz, J. Osorio, D. Oszkiewicz, A. Ouzouni, P. Park, E. Pasquato, C. Peltzer, J. Peralta, F. Péturaud, T. Pieniluoma, E. Pigozzi, J. Poel, G. Prat, T. Prod'homme, F. Raison, J. M. Rebordao, D. Risquez, B. Rocca-Volmerange, S. Rosen, M. I. Ruiz-Fuerte, F. Russo, S. Sembay, I. Serraller Vizcaino, A. Short, A. Siebert, H. Silva, D. Sinachopoulo, E. Slezak, M. Soffel, D. Sosnowska, V. Straižy, M. ter Linden, D. Terrell, S. Theil, C. Tiede, L. Troisi, P. Tsalmantza, D. Tur, M. Vaccari, F. Vachier, P. Valle, W. Van Hamme, L. Veltz, J. Virtanen, J. -M. Wallut, R. Wichmann, M. I. Wilkinson, H. Ziaeepour, S. Zschocke, Université de Franche-Comté (UFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-CHU Pitié-Salpêtrière [APHP], Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud])-Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA), École normale supérieure - Lyon (ENS Lyon)-Institut National de la Recherche Agronomique (INRA)-Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université Bordeaux Segalen - Bordeaux 2-Institut National de la Recherche Agronomique (INRA)-Université Sciences et Technologies - Bordeaux 1, Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA), ESA Scientific Support Office, and Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS)
Subjects: 010504 meteorology & atmospheric sciences, Cepheid variable, GLOBULAR-CLUSTER DISTANCES, Astronomy, [ SDU.ASTR.GA ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], GRAVITATIONAL LENSING EXPERIMENT, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Paral·laxi, Astrophysics, RR Lyrae variable, variables: RR Lyrae [Stars], 01 natural sciences, Linear transformations, data analysis [Methods], 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, QC, QB, Physics, Clusters of galaxies, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Settore FIS/05, Parallaxes, Cosmic distance ladder, [ SDU.ASTR.IM ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astrometry, distances [Stars], [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], CLASSICAL CEPHEIDS, Astrophysics - Solar and Stellar Astrophysics, variables: Cepheids [Stars], parallaxes, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, astrometry, Mathematical transformations, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Data release, RADIAL-VELOCITY CURVES, Iodine, PERIOD-LUMINOSITY RELATIONS, Cúmuls de galàxies, stars: variables: RR Lyrae, astro-ph.SR, Astrometria, astro-ph.GA, ESTRELAS VARIÁVEIS, FOS: Physical sciences, Methods: data analysis, Stars: distances, Stars: variables: Cepheids, Stars: variables: RR Lyrae, Astronomy and Astrophysics, Space and Planetary Science, Settore FIS/05 - Astronomia e Astrofisica, VARIABLE-STARS, POPULATION-II-CEPHEIDS, 0103 physical sciences, Curve fitting, GALACTIC CEPHEIDS, Parallax, Methods:data analysis, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, stars: distances, stars: variables: Cepheids, methods: data analysis, Astrophysics - Astrophysics of Galaxies, HUBBLE-SPACE-TELESCOPE, Galaxies, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Geometrical optics, Stars, Galàxies, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Photometry (astronomy), Luminance, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), LARGE-MAGELLANIC-CLOUD, Navigations- und Regelungssysteme, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Linear least squares
Abstract: This work has financially been supported by:... the European Commission's Sixth Framework Programme through the European Leadership in Space Astrometry (ELSA) Marie Curie Research Training Network (MRTN-CT-2006-033481), through Marie Curie project PIOF-GA-2009-255267 (SAS-RRL), and through a Marie Curie Transfer-of-Knowledge (ToK) fellowship (MTKD-CT-2004-014188); the European Commission's Seventh Framework Programme through grant FP7-606740 (FP7-SPACE-2013-1) for the Gaia European Network for Improved data User Services (GENIUS) and through grant 264895 for the Gaia Research for European Astronomy Training (GREAT-ITN) network;the Spanish Ministry of Economy MINECO-FEDER through grants AyA2014-55216, AyA2011-24052, E5P2013-48318-C2-R, and E5P2014-55996-C2-R and MDM-2014-0369 of ICCUB (Unidad de Excelencia Maria de Maeztu)..., Clementini, G., Eyer, L., Ripepi, V., Marconi, M., Muraveva, T., Garofalo, A., Sarro, L.M., Palmer, M., Luri, X., Molinaro, R., Rimoldini, L., Szabados, L., Musella, I., Anderson, R.I., Prusti, T., De Bruijne, J.H.J., Brown, A.G.A., Vallenari, A., Babusiaux, C., Bailer-Jones, C.A.L., Bastian, U., Biermann, M., Evans, D.W., Jansen, F., Jordi, C., Klioner, S.A., Lammers, U., Lindegren, L., Mignard, F., Panem, C., Pourbaix, D., Randich, S., Sartoretti, P., Siddiqui, H.I., Soubiran, C., Valette, V., Van Leeuwen, F., Walton, N.A., Aerts, C., Arenou, F., Cropper, M., Drimmel, R., Høg, E., Katz, D., Lattanzi, M.G., O'Mullane, W., Grebel, E.K., Holland, A.D., Huc, C., Passot, X., Perryman, M., Bramante, L., Cacciari, C., Castañeda, J., Chaoul, L., Cheek, N., De Angeli, F., Fabricius, C., Guerra, R., Hernández, J., Jean-Antoine-Piccolo, A., Masana, E., Messineo, R., Mowlavi, N., Nienartowicz, K., Ordóñez-Blanco, D., Panuzzo, P., Portell, J., Richards, P.J., Riello, M., Seabroke, G.M., Tanga, P., Thévenin, F., Torra, J., Els, S.G., Gracia-Abril, G., Comoretto, G., Garcia-Reinaldos, M., Lock, T., Mercier, E., Altmann, M., Andrae, R., Astraatmadja, T.L., Bellas-Velidis, I., Benson, K., Berthier, J., Blomme, R., Busso, G., Carry, B., Cellino, A., Cowell, S., Creevey, O., Cuypers, J., Davidson, M., De Ridder, J., De Torres, A., Delchambre, L., Dell'Oro, A., Ducourant, C., Frémat, Y., García-Torres, M., Gosset, E., Halbwachs, J.-L., Hambly, N.C., Harrison, D.L., Hauser, M., Hestroffer, D., Hodgkin, S.T., Huckle, H.E., Hutton, A., Jasniewicz, G., Jordan, S., Kontizas, M., Korn, A.J., Lanzafame, A.C., Manteiga, M., Moitinho, A., Muinonen, K., Osinde, J., Pancino, E., Pauwels, T., Petit, J.-M., Recio-Blanco, A., Robin, A.C., Siopis, C., Smith, M., Smith, K.W., Sozzetti, A., Thuillot, W., Van Reeven, W., Viala, Y., Abbas, U., Abreu Aramburu, A., Accart, S., Aguado, J.J., Allan, P.M., Allasia, W., Altavilla, G., Álvarez, M.A., Alves, J., Andrei, A.H., Anglada Varela, E., Antiche, E., Antoja, T., Antón, S., Arcay, B., Bach, N., Baker, S.G., Balaguer-Núñez, L., Barache, C., Barata, C., Barbier, A., Barblan, F., Barrado, N.Y., Barros, M., Barstow, M.A., Becciani, U., Bellazzini, M., Bello García, A., Belokurov, V., Bendjoya, P., Berihuete, A., Bianchi, L., Bienaymé, O., Billebaud, F., Blagorodnova, N., Blanco-Cuaresma, S., Boch, T., Bombrun, A., Borrachero, R., Bouquillon, S., Bourda, G., Bragaglia, A., Breddels, M.A., Brouillet, N., Brüsemeister, T., Bucciarelli, B., Burgess, P., Burgon, R., Burlacu, A., Busonero, D., Buzzi, R., Caffau, E., Cambras, J., Campbell, H., Cancelliere, R., Cantat-Gaudin, T., Carlucci, T., Carrasco, J.M., Castellani, M., Charlot, P., Charnas, J., Chiavassa, A., Clotet, M., Cocozza, G., Collins, R.S., Costigan, G., Crifo, F., Cross, N.J.G., Crosta, M., Crowley, C., Dafonte, C., Damerdji, Y., Dapergolas, A., David, P., David, M., De Cat, P., De Felice, F., De Laverny, P., De Luise, F., De March, R., De Souza, R., Debosscher, J., Del Pozo, E., Delbo, M., Delgado, A., Delgado, H.E., Di Matteo, P., Diakite, S., Distefano, E., Dolding, C., Dos Anjos, S., Drazinos, P., Durán, J., Dzigan, Y., Edvardsson, B., Enke, H., Evans, N.W., Eynard Bontemps, G., Fabre, C., Fabrizio, M., Falcão, A.J., Farràs Casas, M., Federici, L., Fedorets, G., Fernández-Hernández, J., Fernique, P., Fienga, A., Figueras, F., Filippi, F., Findeisen, K., Fonti, A., Fouesneau, M., Fraile, E., Fraser, M., Fuchs, J., Gai, M., Galleti, S., Galluccio, L., Garabato, D., García-Sedano, F., Garralda, N., Gavras, P., Gerssen, J., Geyer, R., Gilmore, G., Girona, S., Giuffrida, G., Gomes, M., González-Marcos, A., González-Núñez, J., González-Vidal, J.J., Granvik, M., Guerrier, A., Guillout, P., Guiraud, J., Gúrpide, A., Gutiérrez-Sánchez, R., Guy, L.P., Haigron, R., Hatzidimitriou, D., Haywood, M., Heiter, U., Helmi, A., Hobbs, D., Hofmann, W., Holl, B., Holland, G., Hunt, J.A.S., Hypki, A., Icardi, V., Irwin, M., Jevardat De Fombelle, G., Jofré, P., Jonker, P.G., Jorissen, A., Julbe, F., Karampelas, A., Kochoska, A., Kohley, R., Kolenberg, K., Kontizas, E., Koposov, S.E., Kordopatis, G., Koubsky, P., Krone-Martins, A., Kudryashova, M., Bachchan, R.K., Lacoste-Seris, F., Lanza, A.F., Lavigne, J.-B., Le Poncin-Lafitte, C., Lebreton, Y., Lebzelter, T., Leccia, S., Leclerc, N., Lecoeur-Taibi, I., Lemaitre, V., Lenhardt, H., Leroux, F., Liao, S., Licata, E., Lindstrøm, H.E.P., Lister, T.A., Livanou, E., Lobel, A., Löffler, W., López, M., Lorenz, D., Macdonald, I., Magalhães Fernandes, T., Managau, S., Mann, R.G., Mantelet, G., Marchal, O., Marchant, J.M., Marinoni, S., Marrese, P.M., Marschalkó, G., Marshall, D.J., Martín-Fleitas, J.M., Martino, M., Mary, N., Matijevič, G., McMillan, P.J., Messina, S., Michalik, D., Millar, N.R., Miranda, B.M.H., Molina, D., Molinaro, M., Molnár, L., Moniez, M., Montegriffo, P., Mor, R., Mora, A., Morbidelli, R., Morel, T., Morgenthaler, S., Morris, D., Mulone, A.F., Narbonne, J., Nelemans, G., Nicastro, L., Noval, L., Ordénovic, C., Ordieres-Meré, J., Osborne, P., Pagani, C., Pagano, I., Pailler, F., Palacin, H., Palaversa, L., Parsons, P., Pecoraro, M., Pedrosa, R., Pentikäinen, H., Pichon, B., Piersimoni, A.M., Pineau, F.-X., Plachy, E., Plum, G., Poujoulet, E., Prša, A., Pulone, L., Ragaini, S., Rago, S., Rambaux, N., Ramos-Lerate, M., Ranalli, P., Rauw, G., Read, A., Regibo, S., Reylé, C., Ribeiro, R.A., Riva, A., Rixon, G., Roelens, M., Romero-Gómez, M., Rowell, N., Royer, F., Ruiz-Dern, L., Sadowski, G., Sagristà Sellés, T., Sahlmann, J., Salgado, J., Salguero, E., Sarasso, M., Savietto, H., Schultheis, M., Sciacca, E., Segol, M., Segovia, J.C., Segransan, D., Shih, I.-C., Smareglia, R., Smart, R.L., Solano, E., Solitro, F., Sordo, R., Soria Nieto, S., Souchay, J., Spagna, A., Spoto, F., Stampa, U., Steele, I.A., Steidelmüller, H., Stephenson, C.A., Stoev, H., Suess, F.F., Süveges, M., Surdej, J., Szegedi-Elek, E., Tapiador, D., Taris, F., Tauran, G., Taylor, M.B., Teixeira, R., Terrett, D., Tingley, B., Trager, S.C., Turon, C., Ulla, A., Utrilla, E., Valentini, G., Van Elteren, A., Van Hemelryck, E., Van Leeuwen, M., Varadi, M., Vecchiato, A., Veljanoski, J., Via, T., Vicente, D., Vogt, S., Voss, H., Votruba, V., Voutsinas, S., Walmsley, G., Weiler, M., Weingrill, K., Wevers, T., Wyrzykowski, L., Yoldas, A., Zerjal, M., Zucker, S., Zurbach, C., Zwitter, T., Alecu, A., Allen, M., Allende Prieto, C., Amorim, A., Anglada-Escudé, G., Arsenijevic, V., Azaz, S., Balm, P., Beck, M., Bernstein, H.-H., Bigot, L., Bijaoui, A., Blasco, C., Bonfigli, M., Bono, G., Boudreault, S., Bressan, A., Brown, S., Brunet, P.-M., Bunclark, P., Buonanno, R., Butkevich, A.G., Carret, C., Carrion, C., Chemin, L., Chéreau, F., Corcione, L., Darmigny, E., De Boer, K.S., De Teodoro, P., De Zeeuw, P.T., Delle Luche, C., Domingues, C.D., Dubath, P., Fodor, F., Frézouls, B., Fries, A., Fustes, D., Fyfe, D., Gallardo, E., Gallegos, J., Gardiol, D., Gebran, M., Gomboc, A., Gómez, A., Grux, E., Gueguen, A., Heyrovsky, A., Hoar, J., Iannicola, G., Isasi Parache, Y., Janotto, A.-M., Joliet, E., Jonckheere, A., Keil, R., Kim, D.-W., Klagyivik, P., Klar, J., Knude, J., Kochukhov, O., Kolka, I., Kos, J., Kutka, A., Lainey, V., Lebouquin, D., Liu, C., Loreggia, D., Makarov, V.V., Marseille, M.G., Martayan, C., Martinez-Rubi, O., Massart, B., Meynadier, F., Mignot, S., Munari, U., Nguyen, A.-T., Nordlander, T., O'Flaherty, K.S., Ocvirk, P., Olias Sanz, A., Ortiz, P., Osorio, J., Oszkiewicz, D., Ouzounis, A., Park, P., Pasquato, E., Peltzer, C., Peralta, J., Péturaud, F., Pieniluoma, T., Pigozzi, E., Poels, J., Prat, G., Prod'Homme, T., Raison, F., Rebordao, J.M., Risquez, D., Rocca-Volmerange, B., Rosen, S., Ruiz-Fuertes, M.I., Russo, F., Serraller Vizcaino, I., Short, A., Siebert, A., Silva, H., Sinachopoulos, D., Slezak, E., Soffel, M., Sosnowska, D., StraizYs, V., Ter Linden, M., Terrell, D., Theil, S., Tiede, C., Troisi, L., Tsalmantza, P., Tur, D., Vaccari, M., Vachier, F., Valles, P., Van Hamme, W., Veltz, L., Virtanen, J., Wallut, J.-M., Wichmann, R., Wilkinson, M.I., Ziaeepour, H., Zschocke, S.
Published: 2017
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