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29 results on '"Department of Physics and Astronomy [Victoria]"'

1. Roadmap for metal nanoparticles in radiation therapy: current status, translational challenges, and future directions

Author: Karl T. Butterworth, Yaser Hadi Gholami, Kyle Bromma, Vincent Favaudon, Zdenka Kuncic, Jason R. Cook, Udoka Ibeh, Stéphane Lucas, Stephen J. McMahon, E. Gargioni, Sandrine Lacombe, Kevin M. Prise, Anne-Catherine Heuskin, Léon Sanche, Yaroslav Stanishevskiy, Olivier Tillement, Bijay Singh, Henry M. Smilowitz, Sang Hyun Cho, J Donald Payne, Needa A. Virani, Erika Porcel, Ross Berbeco, Wonmo Sung, Félicien Hespeels, Benedikt Rudek, Dmitry Nevozhay, Wassana Yantasee, Hans Rabus, Devika B. Chithrani, Wilfred Ngwa, Sébastien Penninckx, François Lux, Konstantin V Sokolov, Sharif M Ridwan, Jan Schuemann, H L Byrne, Alexander F. Bagley, Sunil Krishnan, James F. Hainfeld, Srinivas Sridhar, Sijumon Kunjachan, Department of Radiation Oncology [Boston], Harvard Medical School [Boston] (HMS)-Massachusetts General Hospital [Boston], The University of Texas M.D. Anderson Cancer Center [Houston], Brigham & Women’s Hospital [Boston] (BWH), Harvard Medical School [Boston] (HMS), Dana-Farber Cancer Institute [Boston], Department of Physics and Astronomy [Victoria], University of Victoria [Canada] (UVIC), Centre for Cancer Research and Cell Biology, Queen's University [Belfast] (QUB), School of Physics [Sydney], The University of Sydney, NanoHybrids, Inc. [Austin], Signalisation, radiobiologie et cancer, Institut Curie [Paris]-Institut National de la Santé et de la Recherche Médicale (INSERM)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Universitaetsklinikum Hamburg-Eppendorf = University Medical Center Hamburg-Eppendorf [Hamburg] (UKE), Nanoprobes, Inc, Namur Research Institute for Life Sciences (NARILIS), Institut des Sciences Moléculaires d'Orsay (ISMO), Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), NH TherAguix SA [Meylan], Formation, élaboration de nanomatériaux et cristaux (FENNEC), Institut Lumière Matière [Villeurbanne] (ILM), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon, Far Eastern Federal University (FEFU), Aurorad, Inc [Houston], Physikalisch-Technische Bundesanstalt [Berlin] (PTB), University of Connecticut Health Center [Farmington], Boston University [Boston] (BU), Université de Sherbrooke (UdeS), Northeastern University [Boston], Rice University [Houston], Department of Biomedical Engineering, The University of Texas at Austin, University of Texas at Austin [Austin], Oregon Health and Science University [Portland] (OHSU), and Mayo Clinic [Jacksonville]
Subjects: theranostics, Computer science, medicine.medical_treatment, Metal nanoparticles, Nanotechnology, Theranostic Nanomedicine, Modelling, 030218 nuclear medicine & medical imaging, 03 medical and health sciences, [SPI]Engineering Sciences [physics], 0302 clinical medicine, SDG 3 - Good Health and Well-being, Vaccine adjuvant, medicine, Theranostic Nanomedicine/methods, Nanoparticle imaging, Humans, [CHIM]Chemical Sciences, Hyperthermia, Radiology, Nuclear Medicine and imaging, metal nanoparticles, radiotherapy, [PHYS]Physics [physics], Radiological and Ultrasound Technology, Radiotherapy, Induced, Radiation dose, modeling, Hyperthermia, Induced, Theranostics, Therapeutic applications of nanoparticles, Radiation therapy, therapeutic applications of nanoparticles, Hyperthermia induced, 030220 oncology & carcinogenesis, Drug delivery, Metal Nanoparticles/therapeutic use, immunotherapy, Immunotherapy, nanoparticle imaging
Abstract: International audience; This roadmap outlines the potential roles of metallic nanoparticles (MNPs) in the field of radiation therapy. MNPs made up of a wide range of materials (from Titanium, Z = 22, to Bismuth, Z = 83) and a similarly wide spectrum of potential clinical applications, including diagnostic, therapeutic (radiation dose enhancers, hyperthermia inducers, drug delivery vehicles, vaccine adjuvants, photosensitizers, enhancers of immunotherapy) and theranostic (combining both diagnostic and therapeutic), are being fabricated and evaluated. This roadmap covers contributions from experts in these topics summarizing their view of the current status and challenges, as well as expected advancements in technology to address these challenges.
Published: 2020
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2. The Pristine Inner Galaxy Survey (PIGS) II: Uncovering the most metal-poor populations in the inner Milky Way

Author: Geraint F. Lewis, Jeffrey D. Simpson, Nicolas F. Martin, Zhen Wan, David Aguado, Kim A. Venn, Daniel B. Zucker, Anke Arentsen, Carlos Allende Prieto, Lyudmila Mashonkina, Rubén Sánchez-Janssen, Jonay I. González Hernández, Else Starkenburg, J. E. O'Connell, Julio F. Navarro, K. Youakim, Roger E. Cohen, Guillaume F. Thomas, Doug Geisler, Raymond G. Carlberg, Mathias Schultheis, Vanessa Hill, Leibniz Institute for Astrophysics Potsdam (AIP), 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), Institute of Astronomy, University of Cambridge, Universidad de La Laguna [Tenerife - SP] (ULL), Joseph Louis LAGRANGE (LAGRANGE), Centre National de la Recherche Scientifique (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)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA), University of British Columbia (UBC), Department of Astronomy and Astrophysics [Universty of Toronto], University of Toronto, Leibniz-Institut für Astrophysik Potsdam (AIP), Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), Macquarie University, Instituto de Astrofisica de Canarias (IAC), Departamento de Astrofísica [La laguna], 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, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Victoria], University of Victoria [Canada] (UVIC), Institute of Astronomy of the Russian Academy of Sciences (INASAN), Russian Academy of Sciences [Moscow] (RAS), UK Astronomy Technology Centre (UK ATC), Science and Technology Facilities Council (STFC), NRC Herzberg Astronomy and Astrophysics, Conseil National de Recherches Canada (CNRC), Sydney Institute for Astronomy (SIfA), The University of Sydney, School of Physics [UNSW Sydney] (UNSW), University of New South Wales [Sydney] (UNSW), Space Telescope Science Institute (STSci), Departamento de Astronomía [Concepción], Universidad de Concepción - University of Concepcion [Chile], Instituto de Investigación Multidisciplinario en Ciencia y Tecnología, Universidad de La Serena (USERENA), Departamento de Física y Astronomía [La Serena], Astronomy, and Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, Nice, France.
Subjects: Metallicity, Milky Way, FOS: Physical sciences, Astrophysics, 01 natural sciences, Galaxy: bulge, Photometry (optics), techniques: photometric, Bulge, 0103 physical sciences, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), ComputingMilieux_MISCELLANEOUS, Physics, Galaxy: stellar content, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Cosmic distance ladder, Astronomy and Astrophysics, stars: Population II, Horizontal branch, Astrophysics - Astrophysics of Galaxies, Galaxy, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], stars: fundamental parameters, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], techniques: spectroscopic
Abstract: Metal-poor stars are important tools for tracing the early history of the Milky Way, and for learning about the first generations of stars. Simulations suggest that the oldest metal-poor stars are to be found in the inner Galaxy. Typical bulge surveys, however, lack low metallicity ([Fe/H] < -1.0) stars because the inner Galaxy is predominantly metal-rich. The aim of the Pristine Inner Galaxy Survey (PIGS) is to study the metal-poor and very metal-poor (VMP, [Fe/H] < -2.0) stars in this region. In PIGS, metal-poor targets for spectroscopic follow-up are selected from metallicity-sensitive CaHK photometry from the CFHT. This work presents the ~250 deg^2 photometric survey as well as intermediate-resolution spectroscopic follow-up observations for ~8000 stars using AAOmega on the AAT. The spectra are analysed using two independent tools: ULySS with an empirical spectral library, and FERRE with a library of synthetic spectra. The comparison between the two methods enables a robust determination of the stellar parameters and their uncertainties. We present a sample of 1300 VMP stars -- the largest sample of VMP stars in the inner Galaxy to date. Additionally, our spectroscopic dataset includes ~1700 horizontal branch stars, which are useful metal-poor standard candles. We furthermore show that PIGS photometry selects VMP stars with unprecedented efficiency: 86%/80% (lower/higher extinction) of the best candidates satisfy [Fe/H] < -2.0, as do 80%/63% of a larger, less strictly selected sample. We discuss future applications of this unique dataset that will further our understanding of the chemical and dynamical evolution of the innermost regions of our Galaxy., accepted for publication in MNRAS, 17 pages, 9 figures
Published: 2020
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3. The Pristine survey – IX. CFHT ESPaDOnS spectroscopic analysis of 115 bright metal-poor candidate stars

Author: Carmela Lardo, Christopher Sneden, Nicolas F. Martin, Else Starkenburg, Federico Sestito, Julio F. Navarro, Rubén Sánchez Janssen, Jonay I. Gonzalez-Hernandez, Collin Kielty, Pascale Jablonka, Anke Arentsen, K. Youakim, Raymond G. Carlberg, Lyudmilla Mashonkina, Piercarlo Bonifacio, Kim A. Venn, Vanessa Hill, G. F. Thomas, Elisabetta Caffau, David Aguado, Khyati Malhan, Department of Physics and Astronomy [Victoria], University of Victoria [Canada] (UVIC), 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), Leibniz Institute for Astrophysics Potsdam (AIP), Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), 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), 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, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), EPFL Laboratoire d’astrophysique, Ecole Polytechnique Fédérale de Lausanne (EPFL), Institute of Astronomy of the Russian Academy of Sciences (INASAN), Russian Academy of Sciences [Moscow] (RAS), Department of Astronomy [Austin], University of Texas at Austin [Austin], National Research Council Herzberg Astronomy and Astrophysics, Instituto de Astrofisica de Canarias (IAC), Departamento de Astrofísica [La laguna], Universidad de La Laguna [Tenerife - SP] (ULL), UK Astronomy Technology Centre (UK ATC), Science and Technology Facilities Council (STFC), Department of Astronomy and Astrophysics [Universty of Toronto], University of Toronto, The Oskar Klein Centre for Cosmoparticle Physics and Department of Physics, Stockholm University, Venn K.A., Kielty C.L., Sestito F., Starkenburg E., Martin N., Aguado D.S., Arentsen A., Bonifacio P., Caffau E., Hill V., Jablonka P., Lardo C., Mashonkina L., Navarro J.F., Sneden C., Thomas G., Youakim K., Gonzalez-Hernandez J.I., Janssen R.S., Carlberg R., Malhan K., University of British Columbia (UBC), Institute of Astronomy, University of Cambridge, 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), Centre National de la Recherche Scientifique (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)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA), and Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, Nice, France.
Subjects: Star, stars: abundances, Milky Way, stars: kinematics and dynamics, 1st stars, Stellar content -Galaxy, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, fe, lte line formation, hamburg/eso survey, Abundance, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010306 general physics, Spectroscopy, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, milky-way, Astrophysics::Galaxy Astrophysics, Population II, Physics, stellar halo, [PHYS]Physics [physics], Galaxy: stellar content, galactic bar, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Galactic Center, Astronomy and Astrophysics, stars: Population II, Kinematics and dynamic, model atmospheres, Galaxy, Stars, Narrow band, Hamburg/ESO Survey, 13. Climate action, Space and Planetary Science, Galaxy: abundances, chemical-composition, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Galaxy: kinematics and dynamics
Abstract: A chemo-dynamical analysis of 115 metal-poor candidate stars selected from the narrow-band Pristine photometric survey is presented based on CFHT high-resolution ESPaDOnS spectroscopy. We have discovered 28 new bright (V < 15) stars with [Fe/H] < −2.5 and 5 with [Fe/H] < −3.0 for success rates of 40 (28/70) and 19 per cent (5/27), respectively. A detailed model atmosphere analysis is carried out for the 28 new metal-poor stars. Stellar parameters were determined from SDSS photometric colours, Gaia DR2 parallaxes, MESA/MIST stellar isochrones, and the initial Pristine survey metallicities, following a Bayesian inference method. Chemical abundances are determined for 10 elements (Na, Mg, Ca, Sc, Ti, Cr, Fe, Ni, Y, and Ba). Most stars show chemical abundance patterns that are similar to the normal metal-poor stars in the Galactic halo; however, we also report the discoveries of a new r-process-rich star, a new CEMP-s candidate with [Y/Ba] > 0, and a metal-poor star with very low [Mg/Fe]. The kinematics and orbits for all of the highly probable metal-poor candidates are determined by combining our precision radial velocities with Gaia DR2 proper motions. Some stars show unusual kinematics for their chemistries, including planar orbits, unbound orbits, and highly elliptical orbits that plunge deeply into the Galactic bulge (Rperi < 0.5 kpc); also, eight stars have orbital energies and actions consistent with the Gaia-Enceladus accretion event. This paper contributes to our understanding of the complex chemo-dynamics of the metal-poor Galaxy, and increases the number of known bright metal-poor stars available for detailed nucleosynthetic studies.
Published: 2020
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4. Pristine dwarf galaxy survey – I. A detailed photometric and spectroscopic study of the very metal-poor Draco II satellite

Author: Nicolas F. Martin, Nicolas Longeard, Eline Tolstoy, D. S. Aguado, Patrick Côté, Pascale Jablonka, Else Starkenburg, K. Youakim, Jonay I. González Hernández, Rubén Sánchez-Janssen, Marla Geha, Kim A. Venn, Julio F. Navarro, Anke Arentsen, R. Michael Rich, Raymond G. Carlberg, Michelle L. M. Collins, Benjamin P M Laevens, Rodrigo A. Ibata, Vanessa Hill, 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), Franche-Comté Électronique Mécanique, Thermique et Optique - Sciences et Technologies (UMR 6174) (FEMTO-ST), Université de Technologie de Belfort-Montbeliard (UTBM)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Baltimore], Johns Hopkins University (JHU), National Research Council of Canada (NRC), 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, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Department of Physics and Astronomy [Victoria], University of Victoria [Canada] (UVIC), and Astronomy
Subjects: na-o anticorrelation, ursa-major, Proper motion, globular-cluster, Metallicity, Milky Way, FOS: Physical sciences, Astrophysics, 01 natural sciences, Photometry (optics), faint, 0103 physical sciences, galaxies: individual: Draco II, Omega Centauri, 010303 astronomy & astrophysics, Dwarf galaxy, [PHYS]Physics [physics], Physics, milky-way satellite, omega-centauri, 010308 nuclear & particles physics, horizontal branches, Velocity dispersion, Astronomy and Astrophysics, galaxies: dwarf, Astrophysics - Astrophysics of Galaxies, stellar-systems, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Globular cluster, Local Group, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: dwarf, galaxies: individual: Draco II, Local Group, Astrophysics - Astrophysics of Galaxies, discovery
Abstract: We present a detailed study of the faint Milky Way satellite Draco II (Dra II) from deep CFHT/MegaCam broadband $g$ and $i$ photometry and narrow-band metallicity-sensitive CaHK observations, along with follow-up Keck II/DEIMOS multi-object spectroscopy. Forward modeling of the deep photometry allows us to refine the structural and photometric properties of Dra II: the distribution of stars in colour-magnitude space implies Dra II is old (13.5 $ \pm 0.5 $ Gyr), very metal poor, very faint ($ L_V = 180 ^{+124}_{-72} L_\odot $), and at a distance $d = 21.5 \pm 0.4$ kpc. The narrow-band, metallicity-sensitive CaHK Pristine photometry confirms this very low metallicity ([Fe/H]$ = -2.7 \pm 0.1$ dex). Even though our study benefits from a doubling of the spectroscopic sample size compared to previous investigations, the velocity dispersion of the system is still only marginally resolved ($\sigma_{vr}, Comment: Accepted for publication in MNRAS
Published: 2018
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5. SEASTAR : a mission to study ocean submesoscale dynamics and small-scale atmosphere-ocean processes in coastal, shelf and polar seas

Author: Gommenginger, Christine, Chapron, Bertrand, Hogg, Andy, Buckingham, Christian, Fox-Kemper, Baylor, Eriksson, Leif, Soulat, Francois, Ubelmann, Clement, Ocampo-Torres, Francisco, Nardelli, Bruno Buongiorno, Griffin, David, Lopez-Dekker, Paco, Knudsen, Per, Andersen, Ole, Stenseng, Lars, Stapleton, Neil, Perrie, William, Violante-Carvalho, Nelson, Schulz-Stellenfleth, Johannes, Woolf, Isern-Fontanet, Jordi, Ardhuin, Fabrice, Klein, Patrice, Mouche, Alexis, Pascual, Ananda, Capet, Xavier, Hauser, Daniele, Stoffelen, Morrow, Rosemary, Aouf, Lotfi, Breivik, Oyvind, Lee-Lueng, Johannessen, Johnny A., Aksenov, Yevgeny, Bricheno, Lucy, Hirschi, Joel, Martin, Adrien C. H., Adrian P., Nurser, George, Polton, Jeff, Wolf, Judith, Johnsens, Harald, Soloviev, Alexander, Jacobs, Gregg A., Collard, Groom, Steve, Kudryavtsev, Vladimir, Wilkin, John, Navarro, Victor, Babanin, Alex, Matthew, Siddorn, Saulter, Andrew, Rippeth, Tom, Emery, Bill, Maximenko, Nikolai, Romeiser, Roland, Graber, Hans, Azcarate, Aida Alvera, Hughes, Chris W., Vandemark, Doug, da Silva, Jose, Van Leeuwen, Peter Jan, Naveira-Garabato, Alberto, Gemmrich, Mahadevan, Amala, Marquez, Munro, Yvonne, Doody, Sam, Burbidge, Geoff, National Oceanography Centre [Southampton] (NOC), University of Southampton, Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER), Research School of Earth Sciences [Canberra] (RSES), Australian National University (ANU), Institut Universitaire Européen de la Mer (IUEM), Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Brest (UBO)-Centre National de la Recherche Scientifique (CNRS), Department of Earth, Environmental and Planetary Sciences [Providence], Brown University, Collecte Localisation Satellites (CLS), Centro de Investigacion Científica y de Educacion Superior de Ensenada, Consiglio Nazionale delle Ricerche [Bologna] (CNR), Commonwealth Scientific and Industrial Research Organisation [Canberra] (CSIRO), Department of Geoscience and Remote Sensing [Delft], Delft University of Technology (TU Delft), National Space Institute [Lyngby] (DTU Space), Danmarks Tekniske Universitet = Technical University of Denmark (DTU), Department of Planning [Aalborg], Aalborg University [Denmark] (AAU), Defence Science and Technology Laboratory (Dstl), Ministry of Defence (UK) (MOD), Institut océanographique Bedford - Bedford Oceanographic Institute [Dartmouth, Canada] (IOB), Department or Ocean Engineering [Rio de Janeiro], Universidade Federal do Rio de Janeiro (UFRJ), Institut für Küstenforschung / Institute of Coastal Research, Helmholtz-Zentrum Geesthacht (GKSS), School of Energy, Geoscience, Infrastruture and Society (EGIS), Heriot-Watt University [Edinburgh] (HWU), Institute of Marine Sciences / Institut de Ciències del Mar [Barcelona] (ICM), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Institut Mediterrani d'Estudis Avancats (IMEDEA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Universidad de las Islas Baleares (UIB), Processus et interactions de fine échelle océanique (PROTEO), Laboratoire d'Océanographie et du Climat : Expérimentations et Approches Numériques (LOCEAN), Muséum national d'Histoire naturelle (MNHN)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Institut Pierre-Simon-Laplace (IPSL (FR_636)), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-Centre National d'Études Spatiales [Toulouse] (CNES)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-École polytechnique (X)-Centre National d'Études Spatiales [Toulouse] (CNES)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Muséum national d'Histoire naturelle (MNHN)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Institut Pierre-Simon-Laplace (IPSL (FR_636)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-École polytechnique (X)-Centre National d'Études Spatiales [Toulouse] (CNES)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), SPACE - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Royal Netherlands Meteorological Institute (KNMI), Laboratoire d'études en Géophysique et océanographie spatiales (LEGOS), 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)-Observatoire Midi-Pyrénées (OMP), 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), Météo-France Direction Interrégionale Sud-Est (DIRSE), Météo-France, Norwegian Meteorological Institute [Oslo] (MET), Geophysical Institute [Bergen] (GFI / BiU), University of Bergen (UiB), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Nansen Environmental and Remote Sensing Center [Bergen] (NERSC), National Oceanography Centre (NOC), National Oceanographic Centre [Liverpool] (NOC ), Northern Research Institute Tromsø (NORUT), Halmos College of Natural Sciences and Oceanography, Nova Southeastern University (NSU), Naval Research Laboratory (NRL), OceanDataLab, Plymouth Marine Laboratory (PML), Satellite Oceanography Laboratory [St Petersburg] (SOLab), Russian State Hydrometeorological University [St.Petersburg] (RSHU), Department of Marine and Coastal Sciences [New Brunswick], School of Environmental and Biological Sciences [New Brunswick], Rutgers, The State University of New Jersey [New Brunswick] (RU), Rutgers University System (Rutgers)-Rutgers University System (Rutgers)-Rutgers, The State University of New Jersey [New Brunswick] (RU), Rutgers University System (Rutgers)-Rutgers University System (Rutgers), Starlab SLU [Barcelona, Spain], Department of Infrastructure Engineering [Melbourne], Melbourne School of Engineering [Melbourne], University of Melbourne-University of Melbourne, Met Office Hadley Centre for Climate Change (MOHC), United Kingdom Met Office [Exeter], School of Ocean Sciences [Menai Bridge], Bangor University, Colorado Center for Astrodynamics Research (CCAR), University of Colorado [Boulder], School of Ocean and Earth Science and Technology (SOEST), University of Hawai‘i [Mānoa] (UHM), Rosenstiel School of Marine and Atmospheric Science (RSMAS), University of Miami [Coral Gables], GeoHydrodynamics and Environment Research (GHER), Université de Liège, Department of Earth Ocean and Ecological Sciences [Liverpool], University of Liverpool, College of Engineering and Physical Dciences [UNH Durham] (CEPS), University of New Hampshire (UNH), Departamento de Geociencias, Ambiente e Ordenamento do Territorio (DGAOT), Universidade do Porto = University of Porto, Department of Meteorology [Reading], University of Reading (UOR), Department of Atmospheric Science [Fort Collins], Colorado State University [Fort Collins] (CSU), Ocean and Earth Science [Southampton], University of Southampton-National Oceanography Centre (NOC), Department of Physics and Astronomy [Victoria], University of Victoria [Canada] (UVIC), Woods Hole Oceanographic Institution (WHOI), Airbus Defence and Space Ltd [Portsmouth], Centre for Earth Observation Instrumentation (UK), European Commission, Institut Français de Recherche pour l'Exploitation de la Mer - Brest (IFREMER Centre de Bretagne), Technical University of Denmark [Lyngby] (DTU), Institut Pierre-Simon-Laplace (IPSL (FR_636)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-Centre National d'Études Spatiales [Toulouse] (CNES)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-Centre National d'Études Spatiales [Toulouse] (CNES)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Institut de Recherche pour le Développement (IRD)-Muséum national d'Histoire naturelle (MNHN)-Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université (SU)-Institut Pierre-Simon-Laplace (IPSL (FR_636)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-Centre National d'Études Spatiales [Toulouse] (CNES)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Institut de Recherche pour le Développement (IRD)-Muséum national d'Histoire naturelle (MNHN)-Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université (SU), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Météo France, Plymouth Marine Laboratory, and Universidade do Porto
Subjects: 0106 biological sciences, air sea interactions, lcsh:QH1-199.5, 010504 meteorology & atmospheric sciences, Mixed layer, Marginal Ice Zone (MIZ), Oceanography, 01 natural sciences, Remote Sensing, Wind wave, SDG 13 - Climate Action, Cryosphere, lcsh:Science, Submesocale, Physics::Atmospheric and Oceanic Physics, SDG 15 - Life on Land, Water Science and Technology, [SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere, Global and Planetary Change, geography.geographical_feature_category, marginal ice zone, dynamics, Ocean color, Climatology, coastal marginal ice zone, satellite, Air-sea interactions, coastal, Ocean Engineering, submesoscale, lcsh:General. Including nature conservation, geographical distribution, Aquatic Science, Physics::Geophysics, along-track interferometry, SDG 14 - Life Below Water, 14. Life underwater, 0105 earth and related environmental sciences, geography, Continental shelf, 010604 marine biology & hydrobiology, Ocean current, Along-track (AT) interferometry, Sea surface temperature, upper ocean dynamics, 13. Climate action, Polar seas, lcsh:Q, radar
Abstract: 7 pages, 2 figures, High-resolution satellite images of ocean color and sea surface temperature reveal an abundance of ocean fronts, vortices and filaments at scales below 10 km but measurements of ocean surface dynamics at these scales are rare. There is increasing recognition of the role played by small scale ocean processes in ocean-atmosphere coupling, upper-ocean mixing and ocean vertical transports, with advanced numerical models and in situ observations highlighting fundamental changes in dynamics when scales reach 1 km. Numerous scientific publications highlight the global impact of small oceanic scales on marine ecosystems, operational forecasts and long-term climate projections through strong ageostrophic circulations, large vertical ocean velocities and mixed layer re-stratification. Small-scale processes particularly dominate in coastal, shelf and polar seas where they mediate important exchanges between land, ocean, atmosphere and the cryosphere, e.g., freshwater, pollutants. As numerical models continue to evolve toward finer spatial resolution and increasingly complex coupled atmosphere-wave-ice-ocean systems, modern observing capability lags behind, unable to deliver the high-resolution synoptic measurements of total currents, wind vectors and waves needed to advance understanding, develop better parameterizations and improve model validations, forecasts and projections. SEASTAR is a satellite mission concept that proposes to directly address this critical observational gap with synoptic two-dimensional imaging of total ocean surface current vectors and wind vectors at 1 km resolution and coincident directional wave spectra. Based on major recent advances in squinted along-track Synthetic Aperture Radar interferometry, SEASTAR is an innovative, mature concept with unique demonstrated capabilities, seeking to proceed toward spaceborne implementation within Europe and beyond, CG and AM received funding from the United Kingdom Centre for Earth Observation Instrumentation SEASTAR+ project (Contract No. RP10G0435A02). PVL was supported by the European Research Council (ERC) CUNDA project 694509 under the European Union Horizon 2020 Research and Innovation Program
Published: 2019
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6. OSSOS. VIII. The Transition Between Two Size Distribution Slopes in the Scattering Disk

Author: Ying-Tung Chen, Nathan A. Kaib, J. M. Petit, Samantha Lawler, Cory Shankman, Wesley C. Fraser, Kathryn Volk, Brett Gladman, Jj Kavelaars, Michele T. Bannister, Stephen Gwyn, Mike Alexandersen, NRC Herzberg Institute of Astrophysics, National Research Council of Canada (NRC), City of Toronto, Toronto, ON, Department of Physics and Astronomy [Victoria], University of Victoria [Canada] (UVIC), Institute of Astronomy and Astrophysics, Academia Sinica, Taipei, Astrophysics Research Centre [Belfast] (ARC), Queen's University [Belfast] (QUB), Department of Physics and Astronomy, The University of British Columbia, Vancouver, BC, 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), Université de Franche-Comté (UFC), and Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Science and engineering, FOS: Physical sciences, Astronomy and Astrophysics, general [Kuiper belt], 01 natural sciences, Archaeology, Space and Planetary Science, Research council, 0103 physical sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract: The scattering trans-Neptunian Objects (TNOs) can be measured to smaller sizes than any other distant small-body population. We use the largest sample yet obtained, 68 discoveries, primarily by the Outer Solar System Origins Survey (OSSOS), to constrain the slope of its luminosity distribution, with sensitivity to much fainter absolute $H$ magnitudes than previous work. Using the analysis technique in Shankman et al. (2016), we confirm that a single slope for the $H$-distribution is not an accurate representation of the scattering TNOs and Centaurs, and that a break in the distribution is required, in support of previous conclusions. A bright-end slope of $\alpha_b=0.9$ transitioning to a faint-end slope $\alpha_f$ of 0.4-0.5 with a differential number contrast $c$ from 1 (a knee) to 10 (a divot) provides an acceptable match to our data. We find that break magnitudes $H_b$ of 7.7 and 8.3, values both previously suggested for dynamically hot Kuiper belt populations, are equally non-rejectable for a range of $\alpha_f$ and $c$ in our statistical analysis. Our preferred divot $H$-distribution transitions to $\alpha_f=0.5$ with a divot of contrast $c=3$ at $H_b=8.3$, while our preferred knee $H$-distribution transitions to $\alpha_f=0.4$ at $H_b=7.7$. The intrinsic population of scattering TNOs required to match the OSSOS detections is $3\times10^6$ for $H_r, Comment: accepted for publication in AJ
Published: 2018
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7. Dwarfs or Giants? Stellar Metallicities and Distances from ugrizG Multiband Photometry

Author: Stephen Gwyn, Laura Ferrarese, Jean-Charles Cuillandre, Raymond G. Carlberg, Julio F. Navarro, Patrick Côté, Jaclyn Jensen, Guillaume F. Thomas, Nicholas Fantin, Nicolas F. Martin, Vincent Hénault-Brunet, Rubén Sánchez-Janssen, Else Starkenburg, Céline Reylé, Sebastien Fabbro, Alan W. McConnachie, Ariane Lançon, Rodrigo A. Ibata, Nicholaas Annau, Hossen Teimoorinia, Geraint F. Lewis, Benoit Famaey, NRC Herzberg Astronomy and Astrophysics, Conseil National de Recherches Canada (CNRC), Department of Physics and Astronomy [Victoria], University of Victoria [Canada] (UVIC), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), 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), Leibniz Institute for Astrophysics Potsdam (AIP), Department of Astronomy and Astrophysics [Universty of Toronto], University of Toronto, NRC Herzberg Institute of Astrophysics, National Research Council of Canada (NRC), The University of Sydney, Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), UK Astronomy Technology Centre (UK ATC), Science and Technology Facilities Council (STFC), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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), ANR-18-CE31-0017,Pristine,Pristine — Sondage des premières étoiles Galactiques(2018), and Université de Strasbourg (UNISTRA)
Subjects: Physics, Milky Way stellar halo, 010504 meteorology & atmospheric sciences, Metallicity, Milky Way, Stellar photometry, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Red giant stars, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Milky Way Galaxy, 01 natural sciences, Photometry (astronomy), Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, Distance measure, 0105 earth and related environmental sciences
Abstract: International audience; We present a new fully data-driven algorithm that uses photometric data from the Canada-France-Imaging-Survey (CFIS; u), Pan-STARRS 1 (PS1; griz), and Gaia (G) to discriminate between dwarf and giant stars and to estimate their distances and metallicities. The algorithm is trained and tested using the SDSS/SEGUE spectroscopic dataset and Gaia photometric/astrometric dataset. At [Fe/H]< −1.2, the algorithm succeeds in identifying more than 70% of the giants in the training/test set, with a dwarf contamination fraction below 30% (with respect to the SDSS/SEGUE dataset). The photometric metallicity estimates have uncertainties better than 0.2 dex when compared with the spectroscopic measurements. The distances estimated by the algorithm are valid out to a distance of at least ∼ 80 kpc without requiring any prior on the stellar distribution, and have fully independent uncertainities that take into account both random and systematic errors. These advances allow us to estimate these stellar parameters for approximately 12 million stars in the photometric dataset. This will enable studies involving the chemical mapping of the distant outer disc and the stellar halo, including their kinematics using the Gaia proper motions. This type of algorithm can be applied in the Southern hemisphere to the first release of LSST data, thus providing an almost complete view of the external components of our Galaxy out to at least ∼ 80 kpc. Critical to the success of these efforts will be ensuring well-defined spectroscopic training sets that sample a broad range of stellar parameters with minimal biases. A catalogue containing the training/test set and all relevant parameters within the public footprint of CFIS is available online.
Published: 2019
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8. Photometric Calibration of the Supernova Legacy Survey Fields

Author: Raymond G. Carlberg, Christophe Balland, Julien Guy, Stéphane Basa, Alex Conley, Reynald Pain, Nicolas Regnault, Christopher J. Pritchet, D. Fouchez, Jean-Charles Cuillandre, D. Hardin, Isobel Hook, D. A. Howell, Pierre Astier, K. Perrett, Mark Sullivan, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy and Astrophysics [Universty of Toronto], University of Toronto, Canada-France-Hawaii Telescope Corporation (CFHT), National Research Council of Canada (NRC)-Centre National de la Recherche Scientifique (CNRS)-University of Hawai'i [Honolulu] (UH), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), University of Oxford Astrophysics, Department of Physics and Astronomy [Victoria], University of Victoria [Canada] (UVIC), SNLS, Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, law.invention, Telescope, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], techniques: photometric, law, 0103 physical sciences, Calibration, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Vega, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Stars, Cardinal point, 13. Climate action, Space and Planetary Science, cosmology: observations, Magnitude (astronomy), Dark energy, Supernova Legacy Survey, Astrophysics::Earth and Planetary Astrophysics, methods: observational, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the photometric calibration of the Supernova Legacy Survey (SNLS) fields. The SNLS aims at measuring the distances to SNe Ia at (0.3, Comment: 46 pages, 23 figures. Accepted by Astronomy and Astrophysics. Online material available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/ or alternatively from: http://supernovae.in2p3.fr/snls3/regnault09_cds.tar.gz
Published: 2016
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9. A census of dense cores in the Taurus L1495 cloud from the Herschel Gould Belt Survey

Author: Glenn J. White, Ph. André, Stefano Pezzuto, Alexander Men'shchikov, P. Palmeirim, M. Benedettini, Matthew Joseph Griffin, D. Bresnahan, J. Di Francesco, A. Roy, Sarah Sadavoy, Kenneth A. Marsh, Davide Elia, Nicola Schneider, Luigi Spinoglio, Jason M. Kirk, Derek Ward-Thompson, Nicolas Peretto, Frédérique Motte, Vera Könyves, University of California [Los Angeles] (UCLA), University of California (UC), Jeremiah Horrocks Insitute, University of Central Lancashire [Preston] (UCLAN), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), 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), School of Physics and Astronomy [Cardiff], Cardiff University, Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Jeremiah Horrocks Institute for Mathematics, Physics and Astronomy [Preston], Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Department of Physics and Astronomy [Victoria], University of Victoria [Canada] (UVIC), Faculty of Informatics [Lugano], Università della Svizzera italiana = University of Italian Switzerland (USI), Laboratoire Pierre Aigrain (LPA), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS-PSL), 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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Herzberg Institute of Astrophysics, National Research Council of Canada (NRC), University Hospital of Cologne [Cologne], FORMATION STELLAIRE 2016, 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), SLAC National Accelerator Laboratory (SLAC), Stanford University, University of California, 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), Université Pierre et Marie Curie - Paris 6 (UPMC)-Université Paris Diderot - Paris 7 (UPD7)-Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Università della Svizzera italiana (USI), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Stanford Linear Accelerator Center (SLAC), and Stanford University [Stanford]
Subjects: Initial mass function, FOS: Physical sciences, F500, Astrophysics, 01 natural sciences, Volume density, Stars formation, submillimetre, L1495, 0103 physical sciences, ISM individual objects, Black-body radiation, 010303 astronomy & astrophysics, QC, Solar and Stellar Astrophysics (astro-ph.SR), QB, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], local interstellar matter, 010308 nuclear & particles physics, Turbulence, Luminosity function, Astronomy, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, ISM clouds, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Mass function, Astrophysics of Galaxies (astro-ph.GA), Log-normal distribution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We present a catalogue of dense cores in a $\sim 4^\circ\times2^\circ$ field of the Taurus star-forming region, inclusive of the L1495 cloud, derived from Herschel SPIRE and PACS observations in the 70 $\mu$m, 160 $\mu$m, 250 $\mu$m, 350 $\mu$m, and 500 $\mu$m continuum bands. Estimates of mean dust temperature and total mass are derived using modified blackbody fits to the spectral energy distributions. We detect 525 starless cores of which $\sim10$-20% are gravitationally bound and therefore presumably prestellar. Our census of unbound objects is $\sim85$% complete for $M>0.015\,M_\odot$ in low density regions ($A_V\stackrel{0.1\,M_\odot$ overall. The prestellar core mass function (CMF) is consistent with lognormal form, resembling the stellar system initial mass function, as has been reported previously. All of the inferred prestellar cores lie on filamentary structures whose column densities exceed the expected threshold for filamentary collapse, in agreement with previous reports. Unlike the prestellar CMF, the unbound starless CMF is not lognormal, but instead is consistent with a power-law form below $0.3\,M_\odot$ and shows no evidence for a low-mass turnover. It resembles previously reported mass distributions for CO clumps at low masses ($M\stackrel{, Comment: 17 pages, 12 figures. Accepted for publication in MNRAS
Published: 2016
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10. Both asymmetric mitotic segregation and cell-to-cell invasion are required for stable germline transmission of Wolbachia in filarial nematodes

Author: Shigehiko Uni, Mark J. Taylor, Coralie Martin, William J. Sullivan, Frédéric Landmann, Odile Bain, Centre National de la Recherche Scientifique (CNRS), Molécules de Communication et Adaptation des Micro-organismes (MCAM), Muséum national d'Histoire naturelle (MNHN)-Centre National de la Recherche Scientifique (CNRS), Sorbonne Université (SU), Department of Physics and Astronomy [Victoria], University of Victoria [Canada] (UVIC), University of California [Santa Cruz] (UCSC), and University of California
Subjects: QH301-705.5, Somatic cell, Science, Biology, General Biochemistry, Genetics and Molecular Biology, Germline, 03 medical and health sciences, Mutualism, qx_301, parasitic diseases, qx_203, Biology (General), Symbiosis, Mitosis, ComputingMilieux_MISCELLANEOUS, Tropism, 030304 developmental biology, Genetics, 0303 health sciences, Bacteria, 030306 microbiology, Embryo, Blastomere, biochemical phenomena, metabolism, and nutrition, biology.organism_classification, Embryonic stem cell, qx_45, Parasite, [SDV.MP]Life Sciences [q-bio]/Microbiology and Parasitology, bacteria, Wolbachia, qu_350, Filarial nematodes, General Agricultural and Biological Sciences, Research Article
Abstract: Summary Parasitic filarial nematodes that belong to the Onchocercidae family live in mutualism with Wolbachia endosymbionts. We developed whole-mount techniques to follow the segregation patterns of Wolbachia through the somatic and germline lineages of four filarial species. These studies reveal multiple evolutionarily conserved mechanisms that are required for Wolbachia localization to the germline. During the initial embryonic divisions, Wolbachia segregate asymmetrically such that they concentrate in the posteriorly localized P2 blastomere, a precursor to the adult germline and hypodermal lineages. Surprisingly, in the next division they are excluded from the germline precursor lineage. Rather, they preferentially segregate to the C blastomere, a source of posterior hypodermal cells. Localization to the germline is accomplished by a distinct mechanism in which Wolbachia invade first the somatic gonadal cells close to the ovarian distal tip cell, the nematode stem cell niche, from the hypodermis. This tropism is associated with a cortical F-actin disruption, suggesting an active engulfment. Significantly, germline invasion occurs only in females, explaining the lack of Wolbachia in the male germline. Once in the syncytial environment of the ovaries, Wolbachia rely on the rachis to multiply and disperse into the germ cells. The utilization of cell-to-cell invasion for germline colonization may indicate an ancestral mode of horizontal transfer that preceded the acquisition of the mutualism.
Published: 2012
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11. A census of dense cores in the Aquila cloud complex: SPIRE/PACS observations from the Herschel Gould Belt survey⋆,⋆⋆,⋆⋆⋆

Author: Vera Könyves, P. Didelon, Matthew James Griffin, T. Hill, P. Palmeirim, Alexander Men'shchikov, Doris Arzoumanian, Stefano Pezzuto, Sarah Sadavoy, Kenneth A. Marsh, Glenn J. White, Ph. André, E. Schisano, Yoshito Shimajiri, J. Di Francesco, L. Spinoglio, Sylvain Bontemps, Peter G. Martin, Milena Benedettini, J.-Ph. Bernard, Nicola Schneider, Derek Ward-Thompson, Kazi L.J. Rygl, Jason M. Kirk, Frédérique Motte, A. Roy, Anaëlle Maury, Bilal Ladjelate, Helene Roussel, Q. Nguyen Luong, Nicolas Peretto, Davide Elia, 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 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), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, FORMATION STELLAIRE 2015, 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)-Centre National de la Recherche Scientifique (CNRS), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University [Cambridge]-Smithsonian Institution, Department of Physics and Astronomy [Victoria], University of Victoria [Canada] (UVIC), School of Physics and Astronomy [Cardiff], Cardiff University, Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Institut de recherche en astrophysique et planétologie (IRAP), 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 de la Recherche Scientifique (CNRS), Joint ALMA Observatory (JAO), National Radio Astronomy Observatory (NRAO)-European Southern Observatory (ESO), Jeremiah Horrocks Institute for Mathematics, Physics and Astronomy [Preston], University of Central Lancashire [Preston] (UCLAN), Canadian Institute for Theoretical Astrophysics (CITA), 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), INAF - Osservatorio Astronomico di Bologna (OABO), Department of Physics and Astronomy [Milton Keynes], The Open University [Milton Keynes] (OU), ANR-11-BS56-0010,STARFICH,Vers une vision unifiée de la formation stellaire dans les galaxies : Origine de la structure filamentaire du milieu interstellaire, des cœurs pré-stellaires et des amas protostellaires vus avec Herschel(2011), European Project: 291294,EC:FP7:ERC,ERC-2011-ADG_20110209,ORISTARS(2012), European Project: 267934,EC:FP7:ERC,ERC-2010-AdG_20100224,MISTIC(2011), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], San Pedro de Atacama Celestial Explorations (SPACE), San Pedro de Atacama Celestial Explorations, University of California [Los Angeles] (UCLA), University of California, Service des Photons, Atomes et Molécules (SPAM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Procédés, Matériaux et Energie Solaire (PROMES), Université de Perpignan Via Domitia (UPVD)-Centre National de la Recherche Scientifique (CNRS), SLAC National Accelerator Laboratory (SLAC), Stanford University, Stanford Linear Accelerator Center (SLAC), Stanford University [Stanford], Smithsonian Institution-Harvard University [Cambridge], Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO)-National Radio Astronomy Observatory (NRAO), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), 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-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Harvard University-Smithsonian Institution, 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), ITA, GBR, FRA, DEU, CAN, CHL, JPN, and NLD
Subjects: Initial mass function, ISM: structure, Stars: formation, Young stellar object, FOS: Physical sciences, Budget control, F500, Efficiency, Astrophysics, Surveys, Population statistics, ISM : clouds, 7. Clean energy, Submillimeter: isms, Gravitation, ISM: individual objects, Functions, Protostar, Spatial distribution, QB, Physics, Star formation, Information dissemination, Molecular cloud, Astronomy and Astrophysics, Stars, Astrophysics - Astrophysics of Galaxies, Spire, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Coremaking, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA]
Abstract: We present and discuss the results of the Herschel Gould Belt survey (HGBS) observations in an 11 deg2 area of the Aquila molecular cloud complex at d 260 pc, imaged with the SPIRE and PACS photometric cameras in parallel mode from 70 μm to 500 μm. Using the multi-scale, multi-wavelength source extraction algorithm getsources, we identify a complete sample of starless dense cores and embedded (Class 0-I) protostars in this region, and analyze their global properties and spatial distributions. We find a total of 651 starless cores, 60% ± 10% of which are gravitationally bound prestellar cores, and they will likely form stars inthe future. We also detect 58 protostellar cores. The core mass function (CMF) derived for the large population of prestellar cores is very similar in shape to the stellar initial mass function (IMF), confirming earlier findings on a much stronger statistical basis and supporting the view that there is a close physical link between the stellar IMF and the prestellar CMF. The global shift in mass scale observed between the CMF and the IMF is consistent with a typical star formation efficiency of 40% at the level of an individual core. By comparing the numbers of starless cores in various density bins to the number of young stellar objects (YSOs), we estimate that the lifetime of prestellar cores is 1 Myr, which is typically 4 times longer than the core free-fall time, and that it decreases with average core density. We find a strong correlation between the spatial distribution of prestellar cores and the densest filaments observed in the Aquila complex. About 90% of the Herschel-identified prestellar cores are located above a background column density corresponding to AV 7, and 75% of them lie within filamentary structures with supercritical masses per unit length ≳16 M☉/pc. These findings support a picture wherein the cores making up the peak of the CMF (and probably responsible for the base of the IMF) result primarily from the gravitational fragmentation of marginally supercritical filaments. Given that filaments appear to dominate the mass budget of dense gas at AV> 7, our findings also suggest that the physics of prestellar core formation within filaments is responsible for a characteristic "efficiency" {SFR/M_dense ̃ 5+2-2 × 10-8 yr-1} for the star formation process in dense gas. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.Figures 18, 19, and Appendices are available in electronic form at http://www.aanda.orgHerschel column density and temperature maps (FITS format) and full Tables A.1 and A.2 are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/584/A91
Published: 2015
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12. The binary fraction of planetary nebula central stars: II. A larger sample and improved technique for the infrared excess search

Author: Douchin, D., De Marco, O., Frew, D.j., Jacoby, G.h., JASNIEWICZ, Gérard, Fitzgerald, M., Passy, J.c., Harmer, D., Hillwig, T., Moe, M., Macquarie University [Sydney], 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), Giant Magellan Telescope Corporation, Department of Physics and Astronomy [Victoria], University of Victoria [Canada] (UVIC), Kitt Peak National Observatory (KPNO), National Optical Astronomy Observatory (NOAO), Department of Physics and Astronomy [Valparaiso], Valparaiso University, Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University [Cambridge]-Smithsonian Institution, and Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2)
Subjects: Stars: evolution, Stars: statistics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Binaries: general, Planetary nebulae: general, Surveys, Techniques: photometric
Abstract: International audience; There is no conclusive explanation of why ˜80 per cent of planetary nebulae (PNe) are non-spherical. In the Binary Hypothesis, a binary interaction is a preferred channel to form a non-spherical PN. A fundamental step to corroborate or disprove the Binary Hypothesis is to estimate the binary fraction of central stars of PNe (CSPNe) and compare it with a prediction based on the binary fraction of the progenitor, main-sequence population. In this paper, the second in a series, we search for spatially unresolved I- and J-band flux excess in an extended sample of 34 CSPN by a refined measurement technique with a better quantification of the uncertainties. The detection rate of I- (J-)band flux excess is 32 ± 16 per cent (50 ± 24 per cent). This result is very close to what was obtained in Paper I with a smaller sample. We account conservatively for unobserved cool companions down to brown dwarf luminosities, increasing these fractions to 40 ± 20 per cent (62 ± 30 per cent). This step is very sensitive to the adopted brightness limit of our survey. Accounting for visual companions increases the binary fraction to 46 ± 23 per cent (71 ± 34 per cent). These figures are lower than in Paper I. The error bars are better quantified, but still unacceptably large. Taken at face value, the current CSPN binary fraction is in line with the main-sequence progenitor population binary fraction. However, including white dwarfs companions could increase this fraction by as much as 13 (21) per cent points.
Published: 2015
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13. Avoiding progenitor bias: The structural and mass evolution of Brightest Group and Cluster Galaxies in Hierarchical models since z~1

Author: Vincent Bouillot, Ravi K. Sheth, Simona Mei, Lauriane Delaye, Rossella Licitra, Begoña Ascaso, Marc Huertas-Company, Stewart Buchan, Alessandro Rettura, Anand Raichoor, Jorge Moreno, Mariangela Bernardi, Francesco Shankar, Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Department of Astronomy [Pasadena], California Institute of Technology (CALTECH), Cosmologie: Origine et Structures, Laboratoire Univers et Théories (LUTH (UMR_8102)), 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)-Université Paris Diderot - Paris 7 (UPD7)-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)-Université Paris Diderot - Paris 7 (UPD7), Department of Physics and Astronomy [Victoria], University of Victoria [Canada] (UVIC), Galaxies, Etoiles, Physique, Instrumentation (GEPI), 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), Department of Physics and Astronomy [Philadelphia], University of Pennsylvania [Philadelphia], Observatoire de Paris, Université Paris sciences et lettres (PSL), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), and PSL Research University (PSL)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, media_common.quotation_subject, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, cosmology: theory, 0103 physical sciences, Galaxy formation and evolution, 010303 astronomy & astrophysics, galaxies: statistics, Astrophysics::Galaxy Astrophysics, media_common, Physics, Effective radius, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), Halo, galaxies: evolution, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The mass and structural evolution of massive galaxies is one of the hottest topics in galaxy formation. This is because it may reveal invaluable insights into the still debated evolutionary processes governing the growth and assembly of spheroids. However, direct comparison between models and observations is usually prevented by the so-called "progenitor bias", i.e., new galaxies entering the observational selection at later epochs, thus eluding a precise study of how pre-existing galaxies actually evolve in size. To limit this effect, we here gather data on high-redshift brightest group and cluster galaxies, evolve their (mean) host halo masses down to z=0 along their main progenitors, and assign as their "descendants" local SDSS central galaxies matched in host halo mass. At face value, the comparison between high redshift and local data suggests a noticeable increase in stellar mass of a factor of >2 since z~1, and of >2.5 in mean effective radius. We then compare the inferred stellar mass and size growth with those predicted by hierarchical models for central galaxies, selected at high redshifts to closely match the halo and stellar mass bins as in the data. Only hierarchical models characterized by very limited satellite stellar stripping and parabolic orbits are capable of broadly reproducing the stellar mass and size increase of a factor ~2-4 observed in cluster galaxies since z ~1. The predicted, average (major) merger rate since z~1 is in good agreement with the latest observational estimates., 9 pages, 5 figures. ApJ, in press. Additional (minor) editing included in text and figure captions
Published: 2015
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14. Possible link between the power spectrum of interstellar filaments and the origin of the prestellar core mass function

Author: Davide Elia, Stefano Pezzuto, Vera Konyves, Frédérique Motte, Y. Shimajiri, Bilal Ladjelate, J. Di Francesco, Ph. André, A. Roy, Nicola Schneider, Derek Ward-Thompson, Tracey Hill, M. Benedettini, P. Palmeirim, G. J. White, Eugenio Schisano, Nicolas Peretto, F. Louvet, Luigi Spinoglio, Doris Arzoumanian, 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 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), School of Physics and Astronomy [Cardiff], Cardiff University, FORMATION STELLAIRE 2015, 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)-Centre National de la Recherche Scientifique (CNRS), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Department of Physics and Astronomy [Victoria], University of Victoria [Canada] (UVIC), Joint ALMA Observatory (JAO), National Radio Astronomy Observatory (NRAO)-European Southern Observatory (ESO), Departamento de Astronomía, Universidad de Chile, Jeremiah Horrocks Institute for Mathematics, Physics and Astronomy [Preston], University of Central Lancashire [Preston] (UCLAN), Department of Physics and Astronomy [Milton Keynes], The Open University [Milton Keynes] (OU), ANR-11-BS56-0010,STARFICH,Vers une vision unifiée de la formation stellaire dans les galaxies : Origine de la structure filamentaire du milieu interstellaire, des cœurs pré-stellaires et des amas protostellaires vus avec Herschel(2011), European Project: 291294,EC:FP7:ERC,ERC-2011-ADG_20110209,ORISTARS(2012), European Southern Observatory (ESO)-National Radio Astronomy Observatory (NRAO), Universidad de Chile = University of Chile [Santiago] (UCHILE), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), 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), and Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES)
Subjects: Initial mass function, Evolution, ISM: structure, Stars: formation, Characteristic indices, FOS: Physical sciences, F500, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Spectral line, Power spectrum, Compressible turbulence, Gravitation, Protein filament, Functions, Mass functions, QC, Astrophysics::Galaxy Astrophysics, Physics, Turbulence, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Molecular cloud, Gaussian-like distributions, Spectral density, Astronomy and Astrophysics, Empirical correlations, Astrophysics - Astrophysics of Galaxies, Stars, Spectrum analysis, Amplitude, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA)
Abstract: Two major features of the prestellar CMF are: 1) a broad peak below 1 Msun, presumably corresponding to a mean gravitational fragmentation scale, and 2) a characteristic power-law slope, very similar to the Salpeter slope of the stellar initial mass function (IMF) at the high-mass end. While recent Herschel observations have shown that the peak of the prestellar CMF is close to the thermal Jeans mass in marginally supercritical filaments, the origin of the power-law tail of the CMF/IMF at the high-mass end is less clear. Inutsuka (2001) proposed a theoretical scenario in which the origin of the power-law tail can be understood as resulting from the growth of an initial spectrum of density perturbations seeded along the long axis of filaments by interstellar turbulence. Here, we report the statistical properties of the line-mass fluctuations of filaments in nearby molecular clouds observed with Herschel using a 1-D power spectrum analysis. The observed filament power spectra were fitted by a power-law function $(P_{true}(s) \propto s^{\alpha})$ after removing the effect of beam convolution at small scales. A Gaussian-like distribution of power-spectrum slopes was found centered at -1.6, close to that of the one-dimensional velocity power spectrum generated by subsonic Kolomogorov turbulence (-1.67). An empirical correlation, $P^{0.5}(s_0) \propto ^{1.4 \pm 0.1} $, was also found between the amplitude of each filament power spectrum $P(s_0)$ and the mean column density along the filament $$. Finally, the dispersion of line-mass fluctuations along each filament $\sigma_{\rm M_{line}}$ was found to scale with the physical length $L$ of the filament, roughly as $\sigma_{M_{line}} \propto L^{0.7}$. Overall, our results are consistent with the suggestion that the bulk of the CMF/IMF results from the gravitational fragmentation of filaments., Comment: 10 pages, 12 figures, Accepted for publication in Astronomy and Astrophysics journal
Published: 2015
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15. Environmental dependence of bulge-dominated galaxy sizes in hierarchical models of galaxy formation. Comparison with the local Universe

Author: Ravi K. Sheth, L. Delaye, Andrea Cattaneo, Pierluigi Monaco, Simona Mei, Anand Raichoor, Francesco Shankar, Rossella Licitra, F. Fontanot, Jorge Moreno, Mariangela Bernardi, Marc Huertas-Company, 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), Department of Physics and Astronomy [Victoria], University of Victoria [Canada] (UVIC), Heidelberger Institut für Theoretische Studien (H-ITS), Dipartimento di Fisica, Università degli Studi di Trieste, Università degli studi di Trieste, Department of Physics and Astronomy [Philadelphia], University of Pennsylvania [Philadelphia], Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), F., Shankar, S., Mei, M., Huertas Company, J., Moreno, F., Fontanot, Monaco, Pierluigi, M., Bernardi, A., Cattaneo, R., Sheth, R., Licitra, L., Delaye, A., Raichoor, Università degli studi di Trieste = University of Trieste, University of Pennsylvania, and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy merger, galaxies: bulges, 01 natural sciences, Peculiar galaxy, cosmology: theory, Galaxy group, 0103 physical sciences, Galaxy formation and evolution, Satellite galaxy, statistic [galaxies], Brightest cluster galaxy, 010303 astronomy & astrophysics, Lenticular galaxy, galaxies: statistics, evolution [galaxies], Astrophysics::Galaxy Astrophysics, Physics, [PHYS]Physics [physics], theory [cosmology], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Galaxy, galaxies: evolution, galaxies: structure, Space and Planetary Science, bulge [galaxies], structure [galaxies], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We compare state-of-the-art semi-analytic models of galaxy formation as well as advanced sub-halo abundance matching models with a large sample of early-type galaxies from SDSS at z < 0.3. We focus our attention on the dependence of median sizes of central galaxies on host halo mass. The data do not show any difference in the structural properties of early-type galaxies with environment, at fixed stellar mass. All hierarchical models considered in this work instead tend to predict a moderate to strong environmental dependence, with the median size increasing by a factor of about 1.5-3 when moving from low to high mass host haloes. At face value the discrepancy with the data is highly significant, especially at the cluster scale, for haloes above log Mhalo > 14. The convolution with (correlated) observational errors reduces some of the tension. Despite the observational uncertainties, the data tend to disfavour hierarchical models characterized by a relevant contribution of disc instabilities to the formation of spheroids, strong gas dissipation in (major) mergers, short dynamical friction timescales, and very short quenching timescales in infalling satellites. We also discuss a variety of additional related issues, such as the slope and scatter in the local size-stellar mass relation, the fraction of gas in local early-type galaxies, and the general predictions on satellite galaxies., 27 pages, 14 figures, 2 tables. MNRAS, in press
Published: 2014
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16. The Canada–France ecliptic plane survey—full data release : the orbital structure of the Kuiper Belt

Author: Olivier Mousis, Jean-Marc Petit, Brian G. Marsden, Allyson Bieryla, Philippe Rousselot, Paula Gabriela Benavídez, Gilbert Mars, Matthew J. Taylor, Matthew L.N. Ashby, Joel Wm. Parker, Guillermo Bernabeu, Adriano Campo Bagatin, Christa Van Laerhoven, Brett Gladman, R. Lynne Jones, Phil D. Nicholson, Jj Kavelaars, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Astronomía y Astrofísica, 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), Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Université Nice Sophia Antipolis (... - 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, 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), Fisheries and Oceans Canada (COOGER), Department of Space Studies [Boulder], Southwest Research Institute [Boulder] (SwRI), Department of Physics and Astronomy [Vancouver], University of British Columbia (UBC), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University [Cambridge]-Smithsonian Institution, SwRI Planetary Science Directorate [Boulder], Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), DLO Winand Staring Centre, Departamento de Fisica, Ingenieria de Sistemas y Teoria de la Señal [Alicante] (DFESTS), Universidad de Alicante, Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Petit, Jean-Marc, NRC Herzberg Institute of Astrophysics, National Research Council of Canada (NRC), Department of Planetary Sciences [Tucson], University of Arizona, Cornell University [New York], Smithsonian Institution-Harvard University [Cambridge], Department of Physics and Astronomy [Victoria], University of Victoria [Canada] (UVIC), and PICS Canada #4638
Subjects: Absolute magnitude, 010504 meteorology & atmospheric sciences, PACS 96.30.Xa, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], media_common.quotation_subject, Population, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, [SDU.ASTR.EP] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astrophysics, general [Kuiper Belt], Surveys, 01 natural sciences, Latitude, surveys, Física Aplicada, 0103 physical sciences, Kuiper Belt, education, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, media_common, Earth and Planetary Astrophysics (astro-ph.EP), Physics, education.field_of_study, Component (thermodynamics), Ecliptic, Resonance, Astronomy and Astrophysics, [PHYS.ASTR.EP] Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Distribution (mathematics), 13. Climate action, Space and Planetary Science, Sky, Kuiper Belt: general, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the orbital distribution of the trans-neptunian objects (TNOs) discovered during the Canada-France Ecliptic Plane Survey, whose discovery phase ran from early 2003 until early 2007. The follow-up observations started just after the first discoveries and extended until late 2009. We obtained characterized observations of 321 sq.deg. of sky to depths in the range g ~ 23.5--24.4 AB mag. We provide a database of 169 TNOs with high-precision dynamical classification and known discovery efficiency. Using this database, we find that the classical belt is a complex region with sub-structures that go beyond the usual splitting of inner (interior to 3:2 mean-motion resonance [MMR]), outer (exterior to 2:1 MMR), and main (in between). The main classical belt (a=40--47 AU) needs to be modeled with at least three components: the `hot' component with a wide inclination distribution and two `cold' components (stirred and kernel) with much narrower inclination distributions. The hot component must have a significantly shallower absolute magnitude (Hg) distribution than the other two components. With 95% confidence, there are 8000+1800-1600 objects in the main belt with Hg, 59 pages, 9 figures, 7 tables
Published: 2011
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17. A Sagittarius-induced origin for the Monoceros ring

Author: Michel-Dansac, Leo, Abadi, Mario G., Navarro, Julio F., Steinmetz, Matthias, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Instituto de Astronomía Teórica y Experimental (IATE), Consejo Nacional de Investigaciones Científicas y Técnicas [Buenos Aires] (CONICET)-Universidad Nacional de Córdoba [Argentina], Department of Physics and Astronomy [Victoria], University of Victoria [Canada] (UVIC), CCIN2P3, École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Universidad Nacional de Córdoba [Argentina]-Consejo Nacional de Investigaciones Científicas y Técnicas [Buenos Aires] (CONICET)
Subjects: galaxies: individual: Sagittarius, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy: halo, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Astrophysics of Galaxies (astro-ph.GA), galaxies: stellar content, Local Group, Astrophysics::Earth and Planetary Astrophysics, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Galaxy: kinematics and dynamics, Galaxy: structure, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Monoceros ring is a collection of stars in nearly-circular orbits at roughly 18 kpc from the Galactic center. It may have originated (i) as the response of the disc to perturbations excited by satellite companions or (ii) from the tidal debris of a disrupted dwarf galaxy. The metallicity of Monoceros stars differs from that of disc stars at comparable Galactocentric distances, an observation that disfavours the first scenario. On the other hand, circular orbits are difficult to accommodate in the tidal-disruption scenario, since it requires a satellite which at the time of disruption was itself in a nearly circular orbit. Such satellite could not have formed at the location of the ring and, given its low mass, dynamical friction is unlikely to have played a major role in its orbital evolution. We search cosmological simulations for low-mass satellites in nearly-circular orbits and find that they result, almost invariably, from orbital changes induced by collisions with more massive satellites: the radius of the circular orbit thus traces the galactocentric distance of the collision. Interestingly, the Sagittarius dwarf, one of the most luminous satellites of the Milky Way, is in a polar orbit that crosses the Galactic plane at roughly the same Galactocentric distance as Monoceros. We use idealized simulations to demonstrate that an encounter with Sagittarius might well have led to the circularization and subsequent tidal demise of the progenitor of the Monoceros ring., Comment: 6 pages, 4 figures, to match version published in MNRAS Letters (http://onlinelibrary.wiley.com/doi/10.1111/j.1745-3933.2011.01035.x/abstract)
Published: 2011
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18. Photometric redshifts for type Ia supernovae in the supernova legacy survey

Author: Julien Guy, S. Pascal, V. Ruhlmann-Kleider, R. Pain, Alex Conley, Pierre Astier, G. Bazin, I. M. Hook, C. Balland, C. J. Pritchet, D. A. Howell, Nathalie Palanque-Delabrouille, R. G. Carlberg, D. Fouchez, Nicolas Regnault, K. Perrett, Stéphane Basa, D. Hardin, Jeffrey A. Rich, Mark Sullivan, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy and Astrophysics [Universty of Toronto], University of Toronto, Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), University of Oxford Astrophysics, Department of Physics and Astronomy [Victoria], University of Victoria [Canada] (UVIC), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)
Subjects: Physics, 010308 nuclear & particles physics, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Light curve, 01 natural sciences, methods: data analysis, Redshift, Galaxy, Photometry (optics), [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Supernova, surveys, 13. Climate action, Space and Planetary Science, stars: supernovae: general, cosmology: observations, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Supernova Legacy Survey, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We present a sample of 485 photometrically identified Type Ia supernova candidates mined from the first three years of data of the CFHT SuperNova Legacy Survey (SNLS). The images were submitted to a deferred processing independent of the SNLS real-time detection pipeline. Light curves of all transient events were reconstructed in the gM, rM, iM and z M filters and submitted to automated sequential cuts in order to identify possible supernovae. Pure noise and long-term variable events were rejected by light curve shape criteria. Type Ia supernova identification relied on event characteristics fitted to their light curves assuming the events to be normal SNe Ia. The light curve fitter SALT2 was used for this purpose, assigning host galaxy photometric redshifts to the tested events. The selected sample of 485 candidates is one magnitude deeper than that allowed by the SNLS spectroscopic identification. The contamination by supernovae of other types is estimated to be 4%. Testing Hubble diagram residuals with this enlarged sample allows us to measure the Malmquist bias due to spectroscopic selections directly. The result is fully consistent with the precise Monte Carlo based estimate used to correct SN Ia distance moduli in the SNLS 3-year cosmological analyses. This paper demonstrates the feasibility of a photometric selection of high redshift supernovae with known host galaxy redshifts, opening interesting prospects for cosmological analyses from future large photometric SN Ia surveys. © 2011 ESO.
Published: 2010
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19. The Kuiper Belt Luminosity Function from m(R)=21 to 26

Author: Jean-Marc Petit, Jj Kavelaars, M. Holman, Chris Pritchet, Tommy Grav, J. Macwilliams, R.L. Jones, Wesley C. Fraser, Brett Gladman, NRC Herzberg Institute of Astrophysics, National Research Council of Canada (NRC), Department of Physics and Astronomy [Victoria], University of Victoria [Canada] (UVIC), Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Université Nice Sophia Antipolis (... - 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, 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), 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), and Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)
Subjects: Physics, Solar System, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], media_common.quotation_subject, Astrophysics (astro-ph), Ecliptic, Astronomy, Flux, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Albedo, 01 natural sciences, Power law, Astron, Space and Planetary Science, Sky, 0103 physical sciences, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Luminosity function (astronomy), media_common
Abstract: We have performed an ecliptic imaging survey of the Kuiper belt with our deepest and widest field achieving a limiting flux of m(g') = 26.4, with a sky coverage of 3.0 square-degrees. This is the largest coverage of any other Kuiper belt survey to this depth. We detect 72 objects, two of which have been previously observed. We have improved the Bayesian maximum likelihood fitting technique presented in Gladman et al. (1998) to account for calibration and sky density variations and have used this to determine the luminosity function of the Kuiper belt. Combining our detections with previous surveys, we find the luminosity function is well represented by a single power-law with slope alpha = 0.65 +/- 0.05 and an on ecliptic sky density of 1 object per square-degree brighter than m(R)=23.42 +/- 0.13. Assuming constant albedos, this slope suggests a differential size-distribution slope of 4.25 +/- 0.25, which is steeper than the Dohnanyi slope of 3.5 expected if the belt is in a state of collisional equilibrium. We find no evidence for a roll-over or knee in the luminosity function and reject such models brightward of m(R) ~ 24.6., 50 Pages, 8 Figures
Published: 2008
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20. Verifying the Cosmological Utility of Type Ia Supernovae: Implications of a Dispersion in the Ultraviolet Spectra

Author: Isobel Hook, Reynald Pain, D. A. Howell, Peter Nugent, Julien Guy, Nicolas Regnault, Dominique Fouchez, D. Hardin, Stéphane Basa, Mark Sullivan, A. Conley, Raymond G. Carlberg, Christopher J. Pritchet, Christophe Balland, David D. Balam, Pierre Astier, Avishay Gal-Yam, K. Perrett, Richard S. Ellis, California Institute of Technology (CALTECH), Department of Astronomy and Astrophysics [Universty of Toronto], University of Toronto, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), University of Oxford Astrophysics, Department of Physics and Astronomy [Victoria], University of Victoria [Canada] (UVIC), SNLS, Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)
Subjects: supernovae type Ia cosmology, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Metallicity, Extinction (astronomy), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Surveys, 01 natural sciences, Cosmology, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Stars: Supernovae: General, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Astrophysics (astro-ph), Astronomy and Astrophysics, Light curve, Galaxy, Redshift, Supernova, 13. Climate action, Space and Planetary Science, Cosmology: Cosmological Parameters, Supernova Legacy Survey
Abstract: We analyze the mean rest-frame ultraviolet (UV) spectrum of Type Ia Supernovae (SNe Ia) and its dispersion using high signal-to-noise Keck-I/LRIS-B spectroscopy for a sample of 36 events at intermediate redshift (z=0.5) discovered by the Canada-France-Hawaii Telescope Supernova Legacy Survey (SNLS). We introduce a new method for removing host galaxy contamination in our spectra, exploiting the comprehensive photometric coverage of the SNLS SNe and their host galaxies, thereby providing the first quantitative view of the UV spectral properties of a large sample of distant SNe Ia. Although the mean SN Ia spectrum has not evolved significantly over the past 40% of cosmic history, precise evolutionary constraints are limited by the absence of a comparable sample of high quality local spectra. Within the high-redshift sample, we discover significant UV spectral variations and exclude dust extinction as the primary cause by examining trends with the optical SN color. Although progenitor metallicity may drive some of these trends, the variations we see are much larger than predicted in recent models and do not follow expected patterns. An interesting new result is a variation seen in the wavelength of selected UV features with phase. We also demonstrate systematic differences in the SN Ia spectral features with SN light curve width in both the UV and the optical. We show that these intrinsic variations could represent a statistical limitation in the future use of high-redshift SNe Ia for precision cosmology. We conclude that further detailed studies are needed, both locally and at moderate redshift where the rest-frame UV can be studied precisely, in order that future missions can confidently be planned to fully exploit SNe Ia as cosmological probes [ABRIDGED]., Accepted for publication in ApJ
Published: 2008
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21. Gemini Spectroscopy of Supernovae from the Supernova Legacy Survey: Improving High-Redshift Supernova Selection and Classification

Author: Saul Perlmutter, D. Fouchez, D. A. Howell, Richard Taillet, Sebastien Fabbro, K. Perrett, Pierre Astier, R. A. Knop, C. J. Pritchet, I. M. Hook, Jeffrey A. Rich, N. Palanque-Delabrouille, Julien Guy, Nicholas A. Walton, R. Pain, D. Balam, R. G. McMahon, Nicolas Regnault, H. Lafoux, R. G. Carlberg, Mark Sullivan, James D. Neill, T. J. Bronder, Éric Aubourg, Stéphane Basa, Department of Astronomy and Astrophysics [Universty of Toronto], University of Toronto, University of Oxford Astrophysics, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre de Physique des Particules de Marseille (CPPM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Department of Physics and Astronomy [Victoria], University of Victoria [Canada] (UVIC), Laboratoire d'Annecy-le-Vieux de Physique Théorique (LAPTH), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), SNLS, Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)
Subjects: Physics, 010308 nuclear & particles physics, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astronomy and Astrophysics, Techniques: Spectroscopic, Astrophysics, Surveys, 01 natural sciences, Cosmology: Observations, Cosmology, Galaxy, Redshift, law.invention, Telescope, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Supernova, Methods: Data Analysis, Stars: Supernovae: General, Space and Planetary Science, law, 0103 physical sciences, Dark energy, Supernova Legacy Survey, Spectroscopy, 010303 astronomy & astrophysics
Abstract: We present new techiques for improving the efficiency of supernova (SN) classification at high redshift using 64 candidates observed at Gemini North and South during the first year of the Supernova Legacy Survey (SNLS). The SNLS is an ongoing five year project with the goal of measuring the equation of state of Dark Energy by discovering and following over 700 high-redshift SNe Ia using data from the Canada-France-Hawaii Telescope Legacy Survey. We achieve an improvement in the SN Ia spectroscopic confirmation rate: at Gemini 71% of candidates are now confirmed as SNe Ia, compared to 54% using the methods of previous surveys. This is despite the comparatively high redshift of this sample, where the median SN Ia redshift is z = 0.81 (0.155 ≤ z ≤ 1.01). These improvements were realized because we use the unprecedented color coverage and lightcurve sampling of the SNLS to predict whether a candidate is an SN Ia and estimate its redshift, before obtaining a spectrum, using a new technique called the “SN photo-z.” In addition, we have improved techniques for galaxy subtraction and SN template � 2 fitting, allowing us to identify candidates even when they are only 15% as bright as the host galaxy. The largest impediment to SN identification is found to be host galaxy contamination of the spectrum – when the SN was at least as bright as the underlying host galaxy the target was identified more than 90% of the time. However, even SNe on bright host galaxies can be easily identified in good seeing conditions. When the image quality was better than 0.55 ′′ , the candidate was identified 88% of the time. Over the five-year course of the survey, using the selection techniques presented here we will be able to add ∼ 170 more confirmed SNe Ia than would be possible using previous methods. Subject headings: cosmology: observations — methods: data analysis — supernovae: general — techniques: spectroscopic — surveys
Published: 2005
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22. Models for Solar Abundance Stars with Gravitational Settling and Radiative Accelerations: Application to M67 and NGC188

Author: Georges Michaud, Jacques Richer, Olivier Richard, Don A. VandenBerg, Département de Physique [Montréal], Université de Montréal (UdeM), Groupe de Recherche en Astronomie et Astrophysique du Languedoc (GRAAL), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Victoria], and University of Victoria [Canada] (UVIC)
Subjects: 010504 meteorology & atmospheric sciences, Opacity, Metallicity, FOS: Physical sciences, Astrophysics, 01 natural sciences, 7. Clean energy, Luminosity, Gravitation, 0103 physical sciences, Radiative transfer, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, Solar mass, Astrophysics (astro-ph), Astronomy and Astrophysics, Stars, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Open cluster
Abstract: Evolutionary models taking into account radiative accelerations, thermal diffusion, and gravitational settling for 28 elements, including all those contributing to OPAL stellar opacities, have been calculated for solar metallicity stars of 0.5 to 1.4 solar masses. The Sun has been used to calibrate the models. Isochrones are fitted to the observed color-magnitude diagrams (CMDs) of M67 and NGC188, and ages of 3.7 and 6.4 Gyr are respectively determined. Convective core overshooting is not required to match the turnoff morphology of either cluster, including the luminosity of the gap in M67, because central convective cores are larger when diffusive processes are treated. This is due mainly to the enhanced helium and metal abundances in the central regions of such models. The observation of solar metallicity open clusters with ages in the range 4.8--5.7Gyr would further test the calculations of atomic diffusion in central stellar regions: according to non-diffusive isochrones, clusters should not have gaps near their main-sequence turnoffs if they are older than ~4.8Gyr, whereas diffusive isochrones predict that gaps should persist up to ages of ~5.7Gyr. Surface abundance isochrones are also calculated. In the case of M67 and NGC188, surface abundance variations are expected to be small. Abundance differences between stars of very similar Teff are expected close to the turnoff, especially for elements between P and Ca. Moreover, in comparison with the results obtained for giants, small generalized underabundances are expected in main-sequence stars. The lithium to beryllium ratio is discussed briefly and compared to observations., 34 pages, 15 figures, Accepted by the Astrophysical Journal
Published: 2004

23. Photon-counting computed tomography of lanthanide contrast agents with a high-flux 330- μ m-pitch cadmium zinc telluride detector in a table-top system.

Author: Dunning CAS, O'Connell J, Robinson SM, Murphy KJ, Frencken AL, van Veggel FCJM, Iniewski K, and Bazalova-Carter M
Abstract: Purpose: We present photon-counting computed tomography (PCCT) imaging of contrast agent triplets similar in atomic number ( Z ) achieved with a high-flux cadmium zinc telluride (CZT) detector. Approach: The table-top PCCT imaging system included a 330 - μ m -pitch CZT detector of size 8 mm × 24 mm 2 capable of using six energy bins. Four 3D-printed 3-cm-diameter phantoms each contained seven 6-mm-diameter vials with water and low and high concentration solutions of various contrast agents. Lanthanum ( Z = 57 ), gadolinium (Gd) ( Z = 64 ), and lutetium ( Z = 71 ) were imaged together and so were iodine ( Z = 53 ), Gd, and holmium ( Z = 67 ). Each phantom was imaged with 1-mm aluminum-filtered 120-kVp cone beam x rays to produce six energy-binned computed tomography (CT) images. Results: K -edge images were reconstructed using a weighted sum of six CT images, which distinguished each contrast agent with a root-mean-square error (RMSE) of < 0.29 % and 0.51% for the 0.5% and 5% concentrations, respectively. Minimal cross-contamination in each K -edge image was seen, with RMSE values < 0.27 % in vials with no contrast. Conclusion: This is the first preliminary demonstration of simultaneously imaging three similar Z contrast agents with a difference in Z as low as 3., (© 2020 Society of Photo-Optical Instrumentation Engineers (SPIE).)
Published: 2020
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24. Search for Electron Antineutrino Appearance in a Long-Baseline Muon Antineutrino Beam.

Author: Abe K, Akutsu R, Ali A, Alt C, Andreopoulos C, Anthony L, Antonova M, Aoki S, Ariga A, Asada Y, Ashida Y, Atkin ET, Awataguchi Y, Ban S, Barbi M, Barker GJ, Barr G, Barrow D, Barry C, Batkiewicz-Kwasniak M, Beloshapkin A, Bench F, Berardi V, Berkman S, Berns L, Bhadra S, Bienstock S, Blondel A, Bolognesi S, Bourguille B, Boyd SB, Brailsford D, Bravar A, Bravo Berguño D, Bronner C, Bubak A, Buizza Avanzini M, Calcutt J, Campbell T, Cao S, Cartwright SL, Catanesi MG, Cervera A, Chappell A, Checchia C, Cherdack D, Chikuma N, Christodoulou G, Coleman J, Collazuol G, Cook L, Coplowe D, Cudd A, Dabrowska A, De Rosa G, Dealtry T, Denner PF, Dennis SR, Densham C, Di Lodovico F, Dokania N, Dolan S, Doyle TA, Drapier O, Dumarchez J, Dunne P, Eklund L, Emery-Schrenk S, Ereditato A, Fernandez P, Feusels T, Finch AJ, Fiorentini GA, Fiorillo G, Francois C, Friend M, Fujii Y, Fujita R, Fukuda D, Fukuda R, Fukuda Y, Fusshoeller K, Gameil K, Giganti C, Golan T, Gonin M, Gorin A, Guigue M, Hadley DR, Haigh JT, Hamacher-Baumann P, Hartz M, Hasegawa T, Hastings NC, Hayashino T, Hayato Y, Hiramoto A, Hogan M, Holeczek J, Hong Van NT, Iacob F, Ichikawa AK, Ikeda M, Ishida T, Ishii T, Ishitsuka M, Iwamoto K, Izmaylov A, Jakkapu M, Jamieson B, Jenkins SJ, Jesús-Valls C, Jiang M, Johnson S, Jonsson P, Jung CK, Kabirnezhad M, Kaboth AC, Kajita T, Kakuno H, Kameda J, Karlen D, Kasetti SP, Kataoka Y, Katori T, Kato Y, Kearns E, Khabibullin M, Khotjantsev A, Kikawa T, Kim H, Kim J, King S, Kisiel J, Knight A, Knox A, Kobayashi T, Koch L, Koga T, Konaka A, Kormos LL, Koshio Y, Kostin A, Kowalik K, Kubo H, Kudenko Y, Kukita N, Kuribayashi S, Kurjata R, Kutter T, Kuze M, Labarga L, Lagoda J, Lamoureux M, Laveder M, Lawe M, Licciardi M, Lindner T, Litchfield RP, Liu SL, Li X, Longhin A, Ludovici L, Lu X, Lux T, Machado LN, Magaletti L, Mahn K, Malek M, Manly S, Maret L, Marino AD, Marti-Magro L, Martin JF, Maruyama T, Matsubara T, Matsushita K, Matveev V, Mavrokoridis K, Mazzucato E, McCarthy M, McCauley N, McFarland KS, McGrew C, Mefodiev A, Metelko C, Mezzetto M, Minamino A, Mineev O, Mine S, Miura M, Molina Bueno L, Moriyama S, Morrison J, Mueller TA, Munteanu L, Murphy S, Nagai Y, Nakadaira T, Nakahata M, Nakajima Y, Nakamura A, Nakamura KG, Nakamura K, Nakayama S, Nakaya T, Nakayoshi K, Nantais C, Ngoc TV, Niewczas K, Nishikawa K, Nishimura Y, Nonnenmacher TS, Nova F, Novella P, Nowak J, Nugent JC, O'Keeffe HM, O'Sullivan L, Odagawa T, Okumura K, Okusawa T, Oser SM, Owen RA, Oyama Y, Palladino V, Palomino JL, Paolone V, Parker WC, Pasternak J, Paudyal P, Pavin M, Payne D, Penn GC, Pickering L, Pidcott C, Pintaudi G, Pinzon Guerra ES, Pistillo C, Popov B, Porwit K, Posiadala-Zezula M, Pritchard A, Quilain B, Radermacher T, Radicioni E, Radics B, Ratoff PN, Reinherz-Aronis E, Riccio C, Rondio E, Roth S, Rubbia A, Ruggeri AC, Ruggles CA, Rychter A, Sakashita K, Sánchez F, Schloesser CM, Scholberg K, Schwehr J, Scott M, Seiya Y, Sekiguchi T, Sekiya H, Sgalaberna D, Shah R, Shaikhiev A, Shaker F, Shaykina A, Shiozawa M, Shorrock W, Shvartsman A, Smirnov A, Smy M, Sobczyk JT, Sobel H, Soler FJP, Sonoda Y, Steinmann J, Suvorov S, Suzuki A, Suzuki SY, Suzuki Y, Sztuc AA, Tada M, Tajima M, Takeda A, Takeuchi Y, Tanaka HK, Tanaka HA, Tanaka S, Thompson LF, Toki W, Touramanis C, Towstego T, Tsui KM, Tsukamoto T, Tzanov M, Uchida Y, Uno W, Vagins M, Valder S, Vallari Z, Vargas D, Vasseur G, Vilela C, Vinning WGS, Vladisavljevic T, Volkov VV, Wachala T, Walker J, Walsh JG, Wang Y, Wark D, Wascko MO, Weber A, Wendell R, Wilking MJ, Wilkinson C, Wilson JR, Wilson RJ, Wood K, Wret C, Yamada Y, Yamamoto K, Yanagisawa C, Yang G, Yano T, Yasutome K, Yen S, Yershov N, Yokoyama M, Yoshida T, Yu M, Zalewska A, Zalipska J, Zaremba K, Zarnecki G, Ziembicki M, Zimmerman ED, Zito M, Zsoldos S, and Zykova A
Abstract: Electron antineutrino appearance is measured by the T2K experiment in an accelerator-produced antineutrino beam, using additional neutrino beam operation to constrain parameters of the Pontecorvo-Maki-Nakagawa-Sakata (PMNS) mixing matrix. T2K observes 15 candidate electron antineutrino events with a background expectation of 9.3 events. Including information from the kinematic distribution of observed events, the hypothesis of no electron antineutrino appearance is disfavored with a significance of 2.40σ and no discrepancy between data and PMNS predictions is found. A complementary analysis that introduces an additional free parameter which allows non-PMNS values of electron neutrino and antineutrino appearance also finds no discrepancy between data and PMNS predictions.
Published: 2020
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25. Search for CP Violation in Neutrino and Antineutrino Oscillations by the T2K Experiment with 2.2×10^{21} Protons on Target.

Author: Abe K, Akutsu R, Ali A, Amey J, Andreopoulos C, Anthony L, Antonova M, Aoki S, Ariga A, Ashida Y, Azuma Y, Ban S, Barbi M, Barker GJ, Barr G, Barry C, Batkiewicz M, Bench F, Berardi V, Berkman S, Berner RM, Berns L, Bhadra S, Bienstock S, Blondel A, Bolognesi S, Bourguille B, Boyd SB, Brailsford D, Bravar A, Bronner C, Buizza Avanzini M, Calcutt J, Campbell T, Cao S, Cartwright SL, Catanesi MG, Cervera A, Chappell A, Checchia C, Cherdack D, Chikuma N, Christodoulou G, Coleman J, Collazuol G, Coplowe D, Cudd A, Dabrowska A, De Rosa G, Dealtry T, Denner PF, Dennis SR, Densham C, Di Lodovico F, Dokania N, Dolan S, Drapier O, Duffy KE, Dumarchez J, Dunne P, Emery-Schrenk S, Ereditato A, Fernandez P, Feusels T, Finch AJ, Fiorentini GA, Fiorillo G, Francois C, Friend M, Fujii Y, Fujita R, Fukuda D, Fukuda Y, Gameil K, Giganti C, Gizzarelli F, Golan T, Gonin M, Hadley DR, Haegel L, Haigh JT, Hamacher-Baumann P, Hansen D, Harada J, Hartz M, Hasegawa T, Hastings NC, Hayashino T, Hayato Y, Hiramoto A, Hogan M, Holeczek J, Hosomi F, Ichikawa AK, Ikeda M, Imber J, Inoue T, Intonti RA, Ishida T, Ishii T, Ishitsuka M, Iwamoto K, Izmaylov A, Jamieson B, Jiang M, Johnson S, Jonsson P, Jung CK, Kabirnezhad M, Kaboth AC, Kajita T, Kakuno H, Kameda J, Karlen D, Katori T, Kato Y, Kearns E, Khabibullin M, Khotjantsev A, Kim H, Kim J, King S, Kisiel J, Knight A, Knox A, Kobayashi T, Koch L, Koga T, Koller PP, Konaka A, Kormos LL, Koshio Y, Kowalik K, Kubo H, Kudenko Y, Kurjata R, Kutter T, Kuze M, Labarga L, Lagoda J, Lamoureux M, Lasorak P, Laveder M, Lawe M, Licciardi M, Lindner T, Liptak ZJ, Litchfield RP, Li X, Longhin A, Lopez JP, Lou T, Ludovici L, Lu X, Magaletti L, Mahn K, Malek M, Manly S, Maret L, Marino AD, Martin JF, Martins P, Maruyama T, Matsubara T, Matveev V, Mavrokoridis K, Ma WY, Mazzucato E, McCarthy M, McCauley N, McFarland KS, McGrew C, Mefodiev A, Metelko C, Mezzetto M, Minamino A, Mineev O, Mine S, Missert A, Miura M, Moriyama S, Morrison J, Mueller TA, Murphy S, Nagai Y, Nakadaira T, Nakahata M, Nakajima Y, Nakamura KG, Nakamura K, Nakamura KD, Nakanishi Y, Nakayama S, Nakaya T, Nakayoshi K, Nantais C, Nielsen C, Niewczas K, Nishikawa K, Nishimura Y, Nonnenmacher TS, Novella P, Nowak J, O'Keeffe HM, O'Sullivan L, Okumura K, Okusawa T, Oryszczak W, Oser SM, Owen RA, Oyama Y, Palladino V, Palomino JL, Paolone V, Paudyal P, Pavin M, Payne D, Pickering L, Pidcott C, Pinzon Guerra ES, Pistillo C, Popov B, Porwit K, Posiadala-Zezula M, Pritchard A, Quilain B, Radermacher T, Radicioni E, Ratoff PN, Reinherz-Aronis E, Riccio C, Rondio E, Rossi B, Roth S, Rubbia A, Ruggeri AC, Rychter A, Sakashita K, Sánchez F, Sasaki S, Scantamburlo E, Scholberg K, Schwehr J, Scott M, Seiya Y, Sekiguchi T, Sekiya H, Sgalaberna D, Shah R, Shaikhiev A, Shaker F, Shaw D, Shiozawa M, Smirnov A, Smy M, Sobczyk JT, Sobel H, Sonoda Y, Steinmann J, Stewart T, Stowell P, Suda Y, Suvorov S, Suzuki A, Suzuki SY, Suzuki Y, Sztuc AA, Tacik R, Tada M, Takeda A, Takeuchi Y, Tamura R, Tanaka HK, Tanaka HA, Thakore T, Thompson LF, Toki W, Touramanis C, Tsui KM, Tsukamoto T, Tzanov M, Uchida Y, Uno W, Vagins M, Vallari Z, Vasseur G, Vilela C, Vladisavljevic T, Volkov VV, Wachala T, Walker J, Wang Y, Wark D, Wascko MO, Weber A, Wendell R, Wilking MJ, Wilkinson C, Wilson JR, Wilson RJ, Wret C, Yamada Y, Yamamoto K, Yamasu S, Yanagisawa C, Yang G, Yano T, Yasutome K, Yen S, Yershov N, Yokoyama M, Yoshida T, Yu M, Zalewska A, Zalipska J, Zaremba K, Zarnecki G, Ziembicki M, Zimmerman ED, Zito M, Zsoldos S, and Zykova A
Abstract: The T2K experiment measures muon neutrino disappearance and electron neutrino appearance in accelerator-produced neutrino and antineutrino beams. With an exposure of 14.7(7.6)×10^{20} protons on target in the neutrino (antineutrino) mode, 89 ν_{e} candidates and seven anti-ν_{e} candidates are observed, while 67.5 and 9.0 are expected for δ_{CP}=0 and normal mass ordering. The obtained 2σ confidence interval for the CP-violating phase, δ_{CP}, does not include the CP-conserving cases (δ_{CP}=0, π). The best-fit values of other parameters are sin^{2}θ_{23}=0.526_{-0.036}^{+0.032} and Δm_{32}^{2}=2.463_{-0.070}^{+0.071}×10^{-3} eV^{2}/c^{4}.
Published: 2018
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26. Measurement of Muon Antineutrino Oscillations with an Accelerator-Produced Off-Axis Beam.

Author: Abe K, Andreopoulos C, Antonova M, Aoki S, Ariga A, Assylbekov S, Autiero D, Barbi M, Barker GJ, Barr G, Bartet-Friburg P, Batkiewicz M, Bay F, Berardi V, Berkman S, Bhadra S, Blondel A, Bolognesi S, Bordoni S, Boyd SB, Brailsford D, Bravar A, Bronner C, Buizza Avanzini M, Calland RG, Cao S, Caravaca Rodríguez J, Cartwright SL, Castillo R, Catanesi MG, Cervera A, Cherdack D, Chikuma N, Christodoulou G, Clifton A, Coleman J, Collazuol G, Cremonesi L, Dabrowska A, De Rosa G, Dealtry T, Denner PF, Dennis SR, Densham C, Dewhurst D, Di Lodovico F, Di Luise S, Dolan S, Drapier O, Duffy KE, Dumarchez J, Dytman S, Dziewiecki M, Emery-Schrenk S, Ereditato A, Feusels T, Finch AJ, Fiorentini GA, Friend M, Fujii Y, Fukuda D, Fukuda Y, Furmanski AP, Galymov V, Garcia A, Giffin SG, Giganti C, Gizzarelli F, Gonin M, Grant N, Hadley DR, Haegel L, Haigh MD, Hamilton P, Hansen D, Hara T, Hartz M, Hasegawa T, Hastings NC, Hayashino T, Hayato Y, Helmer RL, Hierholzer M, Hillairet A, Himmel A, Hiraki T, Hirota S, Hogan M, Holeczek J, Horikawa S, Hosomi F, Huang K, Ichikawa AK, Ieki K, Ikeda M, Imber J, Insler J, Intonti RA, Irvine TJ, Ishida T, Ishii T, Iwai E, Iwamoto K, Izmaylov A, Jacob A, Jamieson B, Jiang M, Johnson S, Jo JH, Jonsson P, Jung CK, Kabirnezhad M, Kaboth AC, Kajita T, Kakuno H, Kameda J, Karlen D, Karpikov I, Katori T, Kearns E, Khabibullin M, Khotjantsev A, Kielczewska D, Kikawa T, Kim H, Kim J, King S, Kisiel J, Knight A, Knox A, Kobayashi T, Koch L, Koga T, Konaka A, Kondo K, Kopylov A, Kormos LL, Korzenev A, Koshio Y, Kropp W, Kudenko Y, Kurjata R, Kutter T, Lagoda J, Lamont I, Larkin E, Laveder M, Lawe M, Lazos M, Lindner T, Liptak ZJ, Litchfield RP, Li X, Longhin A, Lopez JP, Ludovici L, Lu X, Magaletti L, Mahn K, Malek M, Manly S, Marino AD, Marteau J, Martin JF, Martins P, Martynenko S, Maruyama T, Matveev V, Mavrokoridis K, Ma WY, Mazzucato E, McCarthy M, McCauley N, McFarland KS, McGrew C, Mefodiev A, Mezzetto M, Mijakowski P, Minamino A, Mineev O, Mine S, Missert A, Miura M, Moriyama S, Mueller TA, Murphy S, Myslik J, Nakadaira T, Nakahata M, Nakamura KG, Nakamura K, Nakamura KD, Nakayama S, Nakaya T, Nakayoshi K, Nantais C, Nielsen C, Nirkko M, Nishikawa K, Nishimura Y, Nowak J, O'Keeffe HM, Ohta R, Okumura K, Okusawa T, Oryszczak W, Oser SM, Ovsyannikova T, Owen RA, Oyama Y, Palladino V, Palomino JL, Paolone V, Patel ND, Pavin M, Payne D, Perkin JD, Petrov Y, Pickard L, Pickering L, Pinzon Guerra ES, Pistillo C, Popov B, Posiadala-Zezula M, Poutissou JM, Poutissou R, Przewlocki P, Quilain B, Radicioni E, Ratoff PN, Ravonel M, Rayner MA, Redij A, Reinherz-Aronis E, Riccio C, Rojas P, Rondio E, Roth S, Rubbia A, Rychter A, Sacco R, Sakashita K, Sánchez F, Sato F, Scantamburlo E, Scholberg K, Schoppmann S, Schwehr J, Scott M, Seiya Y, Sekiguchi T, Sekiya H, Sgalaberna D, Shah R, Shaikhiev A, Shaker F, Shaw D, Shiozawa M, Shirahige T, Short S, Smy M, Sobczyk JT, Sorel M, Southwell L, Stamoulis P, Steinmann J, Stewart T, Suda Y, Suvorov S, Suzuki A, Suzuki K, Suzuki SY, Suzuki Y, Tacik R, Tada M, Takahashi S, Takeda A, Takeuchi Y, Tanaka HK, Tanaka HA, Terhorst D, Terri R, Thakore T, Thompson LF, Tobayama S, Toki W, Tomura T, Touramanis C, Tsukamoto T, Tzanov M, Uchida Y, Vacheret A, Vagins M, Vallari Z, Vasseur G, Wachala T, Wakamatsu K, Walter CW, Wark D, Warzycha W, Wascko MO, Weber A, Wendell R, Wilkes RJ, Wilking MJ, Wilkinson C, Wilson JR, Wilson RJ, Yamada Y, Yamamoto K, Yamamoto M, Yanagisawa C, Yano T, Yen S, Yershov N, Yokoyama M, Yoo J, Yoshida K, Yuan T, Yu M, Zalewska A, Zalipska J, Zambelli L, Zaremba K, Ziembicki M, Zimmerman ED, Zito M, and Żmuda J
Abstract: T2K reports its first measurements of the parameters governing the disappearance of ν[over ¯]_{μ} in an off-axis beam due to flavor change induced by neutrino oscillations. The quasimonochromatic ν[over ¯]_{μ} beam, produced with a peak energy of 0.6 GeV at J-PARC, is observed at the far detector Super-Kamiokande, 295 km away, where the ν[over ¯]_{μ} survival probability is expected to be minimal. Using a data set corresponding to 4.01×10^{20} protons on target, 34 fully contained μ-like events were observed. The best-fit oscillation parameters are sin^{2}(θ[over ¯]_{23})=0.45 and |Δm[over ¯]_{32}^{2}|=2.51×10^{-3} eV^{2} with 68% confidence intervals of 0.38-0.64 and 2.26-2.80×10^{-3} eV^{2}, respectively. These results are in agreement with existing antineutrino parameter measurements and also with the ν_{μ} disappearance parameters measured by T2K.
Published: 2016
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27. Experimental validation of L-shell x-ray fluorescence computed tomography imaging: phantom study.

Author: Bazalova-Carter M, Ahmad M, Xing L, and Fahrig R
Abstract: Thanks to the current advances in nanoscience, molecular biochemistry, and x-ray detector technology, x-ray fluorescence computed tomography (XFCT) has been considered for molecular imaging of probes containing high atomic number elements, such as gold nanoparticles. The commonly used XFCT imaging performed with K-shell x rays appears to have insufficient imaging sensitivity to detect the low gold concentrations observed in small animal studies. Low energy fluorescence L-shell x rays have exhibited higher signal-to-background ratio and appeared as a promising XFCT mode with greatly enhanced sensitivity. The aim of this work was to experimentally demonstrate the feasibility of L-shell XFCT imaging and to assess its achievable sensitivity. We built an experimental L-shell XFCT imaging system consisting of a miniature x-ray tube and two spectrometers, a silicon drift detector (SDD), and a CdTe detector placed at [Formula: see text] with respect to the excitation beam. We imaged a 28-mm-diameter water phantom with 4-mm-diameter Eppendorf tubes containing gold solutions with concentrations of 0.06 to 0.1% Au. While all Au vials were detectable in the SDD L-shell XFCT image, none of the vials were visible in the CdTe L-shell XFCT image. The detectability limit of the presented L-shell XFCT SDD imaging setup was 0.007% Au, a concentration observed in small animal studies.
Published: 2015
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28. Precise measurement of the neutrino mixing parameter θ23 from muon neutrino disappearance in an off-axis beam.

Author: Abe K, Adam J, Aihara H, Akiri T, Andreopoulos C, Aoki S, Ariga A, Ariga T, Assylbekov S, Autiero D, Barbi M, Barker GJ, Barr G, Bass M, Batkiewicz M, Bay F, Bentham SW, Berardi V, Berger BE, Berkman S, Bertram I, Bhadra S, Blaszczyk Fd, Blondel A, Bojechko C, Bordoni S, Boyd SB, Brailsford D, Bravar A, Bronner C, Buchanan N, Calland RG, Caravaca Rodríguez J, Cartwright SL, Castillo R, Catanesi MG, Cervera A, Cherdack D, Christodoulou G, Clifton A, Coleman J, Coleman SJ, Collazuol G, Connolly K, Cremonesi L, Dabrowska A, Danko I, Das R, Davis S, de Perio P, De Rosa G, Dealtry T, Dennis SR, Densham C, Di Lodovico F, Di Luise S, Drapier O, Duboyski T, Duffy K, Dufour F, Dumarchez J, Dytman S, Dziewiecki M, Emery S, Ereditato A, Escudero L, Finch AJ, Floetotto L, Friend M, Fujii Y, Fukuda Y, Furmanski AP, Galymov V, Giffin S, Giganti C, Gilje K, Goeldi D, Golan T, Gonin M, Grant N, Gudin D, Hadley DR, Haesler A, Haigh MD, Hamilton P, Hansen D, Hara T, Hartz M, Hasegawa T, Hastings NC, Hayato Y, Hearty C, Helmer RL, Hierholzer M, Hignight J, Hillairet A, Himmel A, Hiraki T, Hirota S, Holeczek J, Horikawa S, Huang K, Ichikawa AK, Ieki K, Ieva M, Ikeda M, Imber J, Insler J, Irvine TJ, Ishida T, Ishii T, Ives SJ, Iwai E, Iyogi K, Izmaylov A, Jacob A, Jamieson B, Johnson RA, Jo JH, Jonsson P, Jung CK, Kabirnezhad M, Kaboth AC, Kajita T, Kakuno H, Kameda J, Kanazawa Y, Karlen D, Karpikov I, Kearns E, Khabibullin M, Khotjantsev A, Kielczewska D, Kikawa T, Kilinski A, Kim J, Kisiel J, Kitching P, Kobayashi T, Koch L, Kolaceke A, Konaka A, Kormos LL, Korzenev A, Koseki K, Koshio Y, Kreslo I, Kropp W, Kubo H, Kudenko Y, Kumaratunga S, Kurjata R, Kutter T, Lagoda J, Laihem K, Lamont I, Laveder M, Lawe M, Lazos M, Lee KP, Lindner T, Lister C, Litchfield RP, Longhin A, Ludovici L, Macaire M, Magaletti L, Mahn K, Malek M, Manly S, Marino AD, Marteau J, Martin JF, Maruyama T, Marzec J, Mathie EL, Matveev V, Mavrokoridis K, Mazzucato E, McCarthy M, McCauley N, McFarland KS, McGrew C, Metelko C, Mezzetto M, Mijakowski P, Miller CA, Minamino A, Mineev O, Mine S, Missert A, Miura M, Monfregola L, Moriyama S, Mueller TA, Murakami A, Murdoch M, Murphy S, Myslik J, Nagasaki T, Nakadaira T, Nakahata M, Nakai T, Nakamura K, Nakayama S, Nakaya T, Nakayoshi K, Naples D, Nielsen C, Nirkko M, Nishikawa K, Nishimura Y, O'Keeffe HM, Ohta R, Okumura K, Okusawa T, Oryszczak W, Oser SM, Owen RA, Oyama Y, Palladino V, Palomino J, Paolone V, Payne D, Perevozchikov O, Perkin JD, Petrov Y, Pickard L, Pinzon Guerra ES, Pistillo C, Plonski P, Poplawska E, Popov B, Posiadala M, Poutissou JM, Poutissou R, Przewlocki P, Quilain B, Radicioni E, Ratoff PN, Ravonel M, Rayner MA, Redij A, Reeves M, Reinherz-Aronis E, Retiere F, Robert A, Rodrigues PA, Rojas P, Rondio E, Roth S, Rubbia A, Ruterbories D, Sacco R, Sakashita K, Sánchez F, Sato F, Scantamburlo E, Scholberg K, Schoppmann S, Schwehr J, Scott M, Seiya Y, Sekiguchi T, Sekiya H, Sgalaberna D, Shiozawa M, Short S, Shustrov Y, Sinclair P, Smith B, Smith RJ, Smy M, Sobczyk JT, Sobel H, Sorel M, Southwell L, Stamoulis P, Steinmann J, Still B, Suda Y, Suzuki A, Suzuki K, Suzuki SY, Suzuki Y, Szeglowski T, Tacik R, Tada M, Takahashi S, Takeda A, Takeuchi Y, Tanaka HK, Tanaka HA, Tanaka MM, Terhorst D, Terri R, Thompson LF, Thorley A, Tobayama S, Toki W, Tomura T, Totsuka Y, Touramanis C, Tsukamoto T, Tzanov M, Uchida Y, Ueno K, Vacheret A, Vagins M, Vasseur G, Wachala T, Waldron AV, Walter CW, Wark D, Wascko MO, Weber A, Wendell R, Wilkes RJ, Wilking MJ, Wilkinson C, Williamson Z, Wilson JR, Wilson RJ, Wongjirad T, Yamada Y, Yamamoto K, Yanagisawa C, Yen S, Yershov N, Yokoyama M, Yuan T, Yu M, Zalewska A, Zalipska J, Zambelli L, Zaremba K, Ziembicki M, Zimmerman ED, Zito M, and Żmuda J
Abstract: New data from the T2K neutrino oscillation experiment produce the most precise measurement of the neutrino mixing parameter θ23. Using an off-axis neutrino beam with a peak energy of 0.6 GeV and a data set corresponding to 6.57×10(20) protons on target, T2K has fit the energy-dependent νμ oscillation probability to determine oscillation parameters. The 68% confidence limit on sin(2)(θ23) is 0.514(-0.056)(+0.055) (0.511±0.055), assuming normal (inverted) mass hierarchy. The best-fit mass-squared splitting for normal hierarchy is Δm32(2)=(2.51±0.10)×10(-3) eV(2)/c(4) (inverted hierarchy: Δm13(2)=(2.48±0.10)×10(-3) eV(2)/c(4)). Adding a model of multinucleon interactions that affect neutrino energy reconstruction is found to produce only small biases in neutrino oscillation parameter extraction at current levels of statistical uncertainty.
Published: 2014
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29. Observation of electron neutrino appearance in a muon neutrino beam.

Author: Abe K, Adam J, Aihara H, Akiri T, Andreopoulos C, Aoki S, Ariga A, Ariga T, Assylbekov S, Autiero D, Barbi M, Barker GJ, Barr G, Bass M, Batkiewicz M, Bay F, Bentham SW, Berardi V, Berger BE, Berkman S, Bertram I, Bhadra S, Blaszczyk FD, Blondel A, Bojechko C, Bordoni S, Boyd SB, Brailsford D, Bravar A, Bronner C, Buchanan N, Calland RG, Caravaca Rodríguez J, Cartwright SL, Castillo R, Catanesi MG, Cervera A, Cherdack D, Christodoulou G, Clifton A, Coleman J, Coleman SJ, Collazuol G, Connolly K, Cremonesi L, Dabrowska A, Danko I, Das R, Davis S, de Perio P, De Rosa G, Dealtry T, Dennis SR, Densham C, Di Lodovico F, Di Luise S, Drapier O, Duboyski T, Duffy K, Dufour F, Dumarchez J, Dytman S, Dziewiecki M, Emery S, Ereditato A, Escudero L, Finch AJ, Floetotto L, Friend M, Fujii Y, Fukuda Y, Furmanski AP, Galymov V, Gaudin A, Giffin S, Giganti C, Gilje K, Goeldi D, Golan T, Gomez-Cadenas JJ, Gonin M, Grant N, Gudin D, Hadley DR, Haesler A, Haigh MD, Hamilton P, Hansen D, Hara T, Hartz M, Hasegawa T, Hastings NC, Hayato Y, Hearty C, Helmer RL, Hierholzer M, Hignight J, Hillairet A, Himmel A, Hiraki T, Hirota S, Holeczek J, Horikawa S, Huang K, Ichikawa AK, Ieki K, Ieva M, Ikeda M, Imber J, Insler J, Irvine TJ, Ishida T, Ishii T, Ives SJ, Iyogi K, Izmaylov A, Jacob A, Jamieson B, Johnson RA, Jo JH, Jonsson P, Jung CK, Kaboth AC, Kajita T, Kakuno H, Kameda J, Kanazawa Y, Karlen D, Karpikov I, Kearns E, Khabibullin M, Khotjantsev A, Kielczewska D, Kikawa T, Kilinski A, Kim J, Kisiel J, Kitching P, Kobayashi T, Koch L, Kolaceke A, Konaka A, Kormos LL, Korzenev A, Koseki K, Koshio Y, Kreslo I, Kropp W, Kubo H, Kudenko Y, Kumaratunga S, Kurjata R, Kutter T, Lagoda J, Laihem K, Lamont I, Laveder M, Lawe M, Lazos M, Lee KP, Licciardi C, Lindner T, Lister C, Litchfield RP, Longhin A, Ludovici L, Macaire M, Magaletti L, Mahn K, Malek M, Manly S, Marino AD, Marteau J, Martin JF, Maruyama T, Marzec J, Mathie EL, Matveev V, Mavrokoridis K, Mazzucato E, McCarthy M, McCauley N, McFarland KS, McGrew C, Metelko C, Mezzetto M, Mijakowski P, Miller CA, Minamino A, Mineev O, Mine S, Missert A, Miura M, Monfregola L, Moriyama S, Mueller TA, Murakami A, Murdoch M, Murphy S, Myslik J, Nagasaki T, Nakadaira T, Nakahata M, Nakai T, Nakamura K, Nakayama S, Nakaya T, Nakayoshi K, Naples D, Nielsen C, Nirkko M, Nishikawa K, Nishimura Y, O'Keeffe HM, Ohta R, Okumura K, Okusawa T, Oryszczak W, Oser SM, Owen RA, Oyama Y, Palladino V, Paolone V, Payne D, Pearce GF, Perevozchikov O, Perkin JD, Petrov Y, Pickard LJ, Pinzon Guerra ES, Pistillo C, Plonski P, Poplawska E, Popov B, Posiadala M, Poutissou JM, Poutissou R, Przewlocki P, Quilain B, Radicioni E, Ratoff PN, Ravonel M, Rayner MA, Redij A, Reeves M, Reinherz-Aronis E, Retiere F, Robert A, Rodrigues PA, Rojas P, Rondio E, Roth S, Rubbia A, Ruterbories D, Sacco R, Sakashita K, Sánchez F, Sato F, Scantamburlo E, Scholberg K, Schwehr J, Scott M, Seiya Y, Sekiguchi T, Sekiya H, Sgalaberna D, Shiozawa M, Short S, Shustrov Y, Sinclair P, Smith B, Smith RJ, Smy M, Sobczyk JT, Sobel H, Sorel M, Southwell L, Stamoulis P, Steinmann J, Still B, Suda Y, Suzuki A, Suzuki K, Suzuki SY, Suzuki Y, Szeglowski T, Tacik R, Tada M, Takahashi S, Takeda A, Takeuchi Y, Tanaka HK, Tanaka HA, Tanaka MM, Terhorst D, Terri R, Thompson LF, Thorley A, Tobayama S, Toki W, Tomura T, Totsuka Y, Touramanis C, Tsukamoto T, Tzanov M, Uchida Y, Ueno K, Vacheret A, Vagins M, Vasseur G, Wachala T, Waldron AV, Walter CW, Wark D, Wascko MO, Weber A, Wendell R, Wilkes RJ, Wilking MJ, Wilkinson C, Williamson Z, Wilson JR, Wilson RJ, Wongjirad T, Yamada Y, Yamamoto K, Yanagisawa C, Yen S, Yershov N, Yokoyama M, Yuan T, Zalewska A, Zalipska J, Zambelli L, Zaremba K, Ziembicki M, Zimmerman ED, Zito M, and Zmuda J
Abstract: The T2K experiment has observed electron neutrino appearance in a muon neutrino beam produced 295 km from the Super-Kamiokande detector with a peak energy of 0.6 GeV. A total of 28 electron neutrino events were detected with an energy distribution consistent with an appearance signal, corresponding to a significance of 7.3σ when compared to 4.92±0.55 expected background events. In the Pontecorvo-Maki-Nakagawa-Sakata mixing model, the electron neutrino appearance signal depends on several parameters including three mixing angles θ12, θ23, θ13, a mass difference Δm(32)(2) and a CP violating phase δ(CP). In this neutrino oscillation scenario, assuming |Δm(32)(2)|=2.4×10(-3) eV(2), sin(2)θ(23)=0.5, and Δm322>0 (Δm(32)(2)<0), a best-fit value of sin(2)2θ(13)=0.140(-0.032)(+0.038) (0.170(-0.037)(+0.045)) is obtained at δ(CP)=0. When combining the result with the current best knowledge of oscillation parameters including the world average value of θ(13) from reactor experiments, some values of δ(CP) are disfavored at the 90% C.L.
Published: 2014
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29 results on '"Department of Physics and Astronomy [Victoria]"'

1. Roadmap for metal nanoparticles in radiation therapy: current status, translational challenges, and future directions

2. The Pristine Inner Galaxy Survey (PIGS) II: Uncovering the most metal-poor populations in the inner Milky Way

3. The Pristine survey – IX. CFHT ESPaDOnS spectroscopic analysis of 115 bright metal-poor candidate stars

4. Pristine dwarf galaxy survey – I. A detailed photometric and spectroscopic study of the very metal-poor Draco II satellite

5. SEASTAR : a mission to study ocean submesoscale dynamics and small-scale atmosphere-ocean processes in coastal, shelf and polar seas

6. OSSOS. VIII. The Transition Between Two Size Distribution Slopes in the Scattering Disk

7. Dwarfs or Giants? Stellar Metallicities and Distances from ugrizG Multiband Photometry

8. Photometric Calibration of the Supernova Legacy Survey Fields

9. A census of dense cores in the Taurus L1495 cloud from the Herschel Gould Belt Survey

10. Both asymmetric mitotic segregation and cell-to-cell invasion are required for stable germline transmission of Wolbachia in filarial nematodes

11. A census of dense cores in the Aquila cloud complex: SPIRE/PACS observations from the Herschel Gould Belt survey⋆,⋆⋆,⋆⋆⋆

12. The binary fraction of planetary nebula central stars: II. A larger sample and improved technique for the infrared excess search

13. Avoiding progenitor bias: The structural and mass evolution of Brightest Group and Cluster Galaxies in Hierarchical models since z~1

14. Possible link between the power spectrum of interstellar filaments and the origin of the prestellar core mass function

15. Environmental dependence of bulge-dominated galaxy sizes in hierarchical models of galaxy formation. Comparison with the local Universe

16. The Canada–France ecliptic plane survey—full data release : the orbital structure of the Kuiper Belt

17. A Sagittarius-induced origin for the Monoceros ring

18. Photometric redshifts for type Ia supernovae in the supernova legacy survey

19. The Kuiper Belt Luminosity Function from m(R)=21 to 26

20. Verifying the Cosmological Utility of Type Ia Supernovae: Implications of a Dispersion in the Ultraviolet Spectra

21. Gemini Spectroscopy of Supernovae from the Supernova Legacy Survey: Improving High-Redshift Supernova Selection and Classification

22. Models for Solar Abundance Stars with Gravitational Settling and Radiative Accelerations: Application to M67 and NGC188

23. Photon-counting computed tomography of lanthanide contrast agents with a high-flux 330- μ m-pitch cadmium zinc telluride detector in a table-top system.

24. Search for Electron Antineutrino Appearance in a Long-Baseline Muon Antineutrino Beam.

25. Search for CP Violation in Neutrino and Antineutrino Oscillations by the T2K Experiment with 2.2×10^{21} Protons on Target.

26. Measurement of Muon Antineutrino Oscillations with an Accelerator-Produced Off-Axis Beam.

27. Experimental validation of L-shell x-ray fluorescence computed tomography imaging: phantom study.

28. Precise measurement of the neutrino mixing parameter θ23 from muon neutrino disappearance in an off-axis beam.

29. Observation of electron neutrino appearance in a muon neutrino beam.

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29 results on '"Department of Physics and Astronomy [Victoria]"'

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