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1. Studying Type II supernovae as cosmological standard candles using the Dark Energy Survey

Author

Michael Schubnell, Josh Frieman, K. Honscheid, David Brooks, David J. James, Jochen Weller, Santiago González-Gaitán, A. Roodman, Pablo Fosalba, B. E. Tucker, M. E. C. Swanson, Ryan J. Foley, T. M. C. Abbott, J. Carretero, Tamara M. Davis, Karl Glazebrook, Daniel Thomas, E. J. Sanchez, V. Scarpine, Sunayana Bhargava, A. A. Plazas, M. Costanzi, Claudia P. Gutiérrez, Felipe Menanteau, Marcos Lima, Shantanu Desai, Mario Hamuy, Daniela Carollo, Marcelle Soares-Santos, Gregory Tarle, Edward Macaulay, Juan Estrada, Anais Möller, A. R. Walker, M. A. G. Maia, Mathew Smith, Tenglin Li, D. L. Burke, F. Forster, Daniel Scolnic, W. G. Hartley, B. Flaugher, Enrique Gaztanaga, Santiago Avila, Peter J. Brown, Samuel Hinton, Antonella Palmese, G. Gutierrez, T. de Jaeger, Michel Aguena, Daniel Gruen, J. De Vicente, Geraint F. Lewis, Ramon Miquel, P. Doel, H. T. Diehl, Alexei V. Filippenko, N. E. Sommer, Alex Drlica-Wagner, A. Carnero Rosell, M. Carrasco Kind, J. Annis, J. Gschwend, S. Allam, Robert A. Gruendl, F. Paz-Chinchón, D. J. Brout, T. F. Eifler, I. Sevilla-Noarbe, S. Everett, Douglas L. Tucker, Kyler Kuehn, B. Nichol, N. Kuropatkin, E. Suchyta, T. N. Varga, L. N. da Costa, M. Sako, Cosimo Inserra, D. L. Hollowood, S. Serrano, Richard Kessler, Juan Garcia-Bellido, E. Bertin, Lluís Galbany, Martin Crocce, R. D. Wilkinson, A. K. Romer, Laboratoire de Physique de Clermont (LPC), Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Centre National de la Recherche Scientifique (CNRS), de Jaeger, T., Galbany, L., González-Gaitán, S., Kessler, R., Filippenko, A. V., Förster, F., Hamuy, M., Brown, P. J., Davis, T. M., Gutiérrez, C. P., Inserra, C., Lewis, G. F., Möller, A., Scolnic, D., Smith, M., Brout, D., Carollo, D., Foley, R. J., Glazebrook, K., Hinton, S. R., Macaulay, E., Nichol, B., Sako, M., Sommer, N. E., Tucker, B. E., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Costanzi, M., Crocce, M., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Drlica-Wagner, A., Eifler, T. F., Estrada, J., Everett, S., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., T. S., Li, Lima, M., Maia, M. A. G., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Romer, A. K., Roodman, A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Varga, T. N., Walker, A. R., Weller, J., Wilkinson, R., and Des, Collaboration

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), ) distance scale [(Cosmology], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Computer Science::Computational Geometry, 7. Clean energy, 01 natural sciences, symbols.namesake, 0103 physical sciences, Range (statistics), distances and redshifts [Galaxies], Astrophysics::Solar and Stellar Astrophysics, distances and redshift [galaxies], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, 4. Education, Cosmic distance ladder, (stars:) supernovae: general, Astronomy and Astrophysics, Redshift, Term (time), (cosmology:) distance scale, Supernova, 13. Climate action, Space and Planetary Science, ) supernovae: general [(Stars], AGLOMERADOS DE GALÁXIAS, Dark energy, symbols, galaxies: distances and redshifts, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Hubble's law, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Despite vast improvements in the measurement of the cosmological parameters, the nature of dark energy and an accurate value of the Hubble constant (H0) in the Hubble–Lemaˆıtre law remain unknown. To break the current impasse, it is necessary to develop as many independent techniques as possible, such as the use of Type II supernovae (SNe II). The goal of this paper is to demonstrate the utility of SNe II for deriving accurate extragalactic distances, which will be an asset for the next generation of telescopes where more-distant SNe II will be discovered. More specifically, we present a sample from the Dark Energy Survey Supernova Program (DES-SN) consisting of 15 SNe II with photometric and spectroscopic information spanning a redshift range up to 0.35. Combining our DES SNe with publicly available samples, and using the standard candle method (SCM), we construct the largest available Hubble diagram with SNe II in the Hubble flow (70 SNe II) and find an observed dispersion of 0.27 mag. We demonstrate that adding a colour term to the SN II standardization does not reduce the scatter in the Hubble diagram. Although SNe II are viable as distance indicators, this work points out important issues for improving their utility as independent extragalactic beacons: find new correlations, define a more standard subclass of SNe II, construct new SN II templates, and dedicate more observing time to high-redshift SNe II. Finally, for the first time, we perform simulations to estimate the redshift-dependent distance-modulus bias due to selection effects., National Science Foundation (NSF) AST-1211916, TABASGO Foundation, Gary and Cynthia Bengier, Christopher R. Redlich Fund, Sylvia and Jim Katzman Foundation, Miller Institute for Basic Research in Science (UC Berkeley) - European Union 839090, Spanish grant PGC2018-095317-B-C21, European Union (EU), EU/FP7-ERC grant 615929, National Science Foundation (NSF), Hyper Suprime-Cam (HSC) collaboration includes the astronomical communities of Japan, Princeton University, Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), University of Tokyo, High Energy Accelerator Research Organization (KEK), FIRST programme from the Japanese Cabinet Office, Ministry of Education, Culture, Sports, Science and Technology, Japan (MEXT), Ministry of Education, Culture, Sports, Science and Technology, Japan (MEXT) Japan Society for the Promotion of Science, Japan Science & Technology Agency (JST), Toray Industries, Inc., Institute for Astronomy (the University of Hawaii), Max Planck Society Foundation CELLEX, National Central University of Taiwan, Space Telescope Science Institute, National Aeronautics & Space Administration (NASA) NNX08AR22G, National Science Foundation (NSF) AST-1238877, University of Maryland, Eotvos Lorand University (ELTE), National Aeronautics & Space Administration (NASA), W.M. Keck Foundation, National Research Council of Canada, Centre National de la Recherche Scientifique (CNRS), Science & Technology Facilities Council (STFC), National Research Council, Comision Nacional de Investigacion Cientifica y Tecnologica (CONICYT), Australian Research Council, National Council for Scientific and Technological Development (CNPq), Consejo Nacional de Investigaciones Cientificas y Tecnicas (CONICET) GN-2005A-Q11 GN-2005B-Q-7 GN-2006A-Q-7 GS-2005A-Q-11 GS-2005BQ-6 GS-2008B-Q-56, United States Department of Energy (DOE), Spanish Government, Higher Education Funding Council for England, National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, Ohio State University, Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University, Ciencia Tecnologia e Inovacao (FINEP), Fundacao Carlos Chagas Filho de Amparo, Conselho Nacional de Desenvolvimento Cient'tronomy at Texas AM University, German Research Foundation (DFG), University of Portsmouth, OzDES Membership Consortium, National Science Foundation (NSF) AST-1138766 AST-1536171 AYA2015-71825 ESP2015-66861 FPA2015-68048 SEV2016-0588 SEV-2016-0597, European Union - CERCA programme of the Generalitat de Catalunya, European Research Council (ERC), European Research Council (ERC) 240672 291329 306478, National Council for Scientific and Technological Development (CNPq) 465376/2014-2, United States Department of Energy (DOE) DE-AC02-05CH11231

Published
2020
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2. Arbitrarily many independent observers can share the nonlocality of a single maximally entangled qubit pair

Author

Peter J. Brown, Roger Colbeck, Laboratoire de l'Informatique du Parallélisme (LIP), Centre National de la Recherche Scientifique (CNRS)-Université de Lyon-Institut National de Recherche en Informatique et en Automatique (Inria)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Department of Mathematics, University of York, University of York [York, UK], École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Recherche en Informatique et en Automatique (Inria)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), and ANR-18-CE47-0011,ACOM,Une Théorie Algorithmique de la Communcation(2018)

Subjects
Discrete mathematics, Quantum Physics, Class (set theory), Computer science, FOS: Physical sciences, General Physics and Astronomy, CHSH inequality, 01 natural sciences, Constructive, Quantum nonlocality, Alice and Bob, [PHYS.QPHY]Physics [physics]/Quantum Physics [quant-ph], Bell's theorem, Qubit, 0103 physical sciences, Quantum Physics (quant-ph), 010306 general physics, Randomness, Computer Science::Cryptography and Security
Abstract

Alice and Bob each have half of a pair of entangled qubits. Bob measures his half and then passes his qubit to a second Bob who measures again and so on. The goal is to maximize the number of Bobs that can have an expected violation of the Clauser-Horne-Shimony-Holt (CHSH) Bell inequality with the single Alice. This scenario was introduced in [Phys. Rev. Lett. 114, 250401 (2015)] where the authors mentioned evidence that when the Bobs act independently and with unbiased inputs then at most two of them can expect to violate the CHSH inequality with Alice. Here we show that, contrary to this evidence, arbitrarily many independent Bobs can have an expected CHSH violation with the single Alice. Our proof is constructive and our measurement strategies can be generalized to work with a larger class of two-qubit states that includes all pure entangled two-qubit states. Since violation of a Bell inequality is necessary for device-independent tasks, our work represents a step towards an eventual understanding of the limitations on how much device-independent randomness can be robustly generated from a single pair of qubits., 4+7 pages, 2 figures, v2: minor updates to match published version

Published
2020
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3. Photometric and Spectroscopic Properties of Type Ia Supernova 2018oh with Early Excess Emission from the $Kepler$ 2 Observations

Author

Jakob Nordin, D. Bersier, Gautham Narayan, Dan Kasen, Zhihao Chen, R. S. Post, B. Cseh, J. Van Cleve, James M. DerKacy, L. Denneau, Lluís Galbany, M. Redick, A. Rest, Krisztián Sárneczky, Subhash Bose, Curtis McCully, Hanna Sai, B. C. Kaiser, E. Baron, C. A. Peterson, J. Vinicius de Miranda Cardoso, Jeffrey L. Coughlin, A. Razza, M. Packard, Steven Williams, G. Beerman, M. Muszynski, Cs. Kalup, B. Elsaesser, O. Hanyecz, G. Csörnyei, Iair Arcavi, J. Moffatt, Isobel Hook, Wenxiong Li, A. Villar, J. Kampmeier, Robert L. Mutel, César Rojas-Bravo, K. A. Larson, Liming Rui, R. Gangopadhyay, B. Csák, S. Margheim, Peter A. Milne, Cosimo Inserra, Subo Dong, Thomas W.-S. Holoien, Jennifer E. Andrews, J. Burke, Han Lin, Jun Mo, Jessie L. Dotson, Kaicheng Zhang, John C Wheeler, J. Palmerio, J. S. Brown, R. M. Larsen, Kate Maguire, H. Flewelling, Katie Auchettl, Danfeng Xiang, K. C. Chambers, Ori D. Fox, Attila Bódi, S. Holmbo, András Pál, C. McGinn, Edward J. Shaya, John L. Tonry, Xulin Zhao, Xiaojia Zhang, E. A. Magnier, M. Hanley, Yen-Chen Pan, Bernadett Ignácz, B. Stalder, R. Szabó, K. M. McCalmont-Everton, G. Zsidi, Joshua S. Reding, J. A. Muñoz, Geert Barentsen, Daichi Hiramatsu, K. Steward, Brad E. Tucker, J. Brimacombe, K. W. Smith, A. Zenteno, R. J. Foley, J. V. Shields, I. Rajmon, Jozsef Vinko, Xiaofeng Wang, Charles D. Kilpatrick, Steven Villanueva, A. Wheaton, B. Spencer, Ann Marie Cody, Peter J. Brown, T. Weschler, L. Migliorini, Xue Li, Claudia P. Gutiérrez, Fang Huang, Saurabh Jha, R. Bjella, C. Labonde, Benjamin J. Shappee, Mark Willman, D. Tallon, V. Nystrom, Tianmeng Zhang, Griffin Hosseinzadeh, S. Flynn, Long Wang, David A. Coulter, David J. Sand, Georgios Dimitriadis, D. O. Jones, J. J. Hermes, Thomas Barclay, Christopher Bilinski, H. Weiland, Réka Könyves-Tóth, Régis Cartier, Steve B. Howell, Peter M. Garnavich, Kim Griest, J. L. Prieto, S. E. Ross, Mark E. Huber, Zs. Bognár, Róbert Szakáts, R. Kloetzel, Krzysztof Z. Stanek, Christopher S. Kochanek, Stefano Valenti, Christina Hedges, G. Castillo, Todd A. Thompson, Ping Chen, C. Z. Waters, L. Kohnert, Adam G. Riess, Nathan Smith, T. B. Lowe, Anthony L. Piro, L. H. Reedy, Levente Kriskovics, Linyi Li, Maria R. Drout, Dale Andrew Howell, A. N. Heinze, A. Ordasi, Stephen J. Smartt, Patrick J. Vallely, A. S. B. Schultz, Joanna Bulger, Michael Gully-Santiago, Jujia Zhang, Ádám Sódor, D. Osborne, Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
DATA RELEASE, ULTRAVIOLET, FACTORY OBSERVATIONS, FOS: Physical sciences, Astrophysics, Type (model theory), medicine.disease_cause, SN 2011FE, 01 natural sciences, Luminosity, Photometry (optics), individual (SN 2018oh) [supernovae], supernovae: general, CIRCUMSTELLAR MATERIAL, 0103 physical sciences, medicine, SPECTRA, Absorption (logic), Ejecta, 010303 astronomy & astrophysics, supernovae: individual, QC, Solar and Stellar Astrophysics (astro-ph.SR), QB, LIGHT CURVES, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, HIGH-VELOCITY FEATURES, 010308 nuclear & particles physics, Astronomy and Astrophysics, Light curve, Supernova, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, IMPROVED DISTANCES, WHITE-DWARF MODELS, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], general [supernovae], Ultraviolet
Abstract

Supernova (SN) 2018oh (ASASSN-18bt) is the first spectroscopically-confirmed type Ia supernova (SN Ia) observed in the $Kepler$ field. The $Kepler$ data revealed an excess emission in its early light curve, allowing to place interesting constraints on its progenitor system (Dimitriadis et al. 2018, Shappee et al. 2018b). Here, we present extensive optical, ultraviolet, and near-infrared photometry, as well as dense sampling of optical spectra, for this object. SN 2018oh is relatively normal in its photometric evolution, with a rise time of 18.3$\pm$0.3 days and $\Delta$m$_{15}(B)=0.96\pm$0.03 mag, but it seems to have bluer $B - V$ colors. We construct the "uvoir" bolometric light curve having peak luminosity as 1.49$\times$10$^{43}$erg s$^{-1}$, from which we derive a nickel mass as 0.55$\pm$0.04M$_{\odot}$ by fitting radiation diffusion models powered by centrally located $^{56}$Ni. Note that the moment when nickel-powered luminosity starts to emerge is +3.85 days after the first light in the Kepler data, suggesting other origins of the early-time emission, e.g., mixing of $^{56}$Ni to outer layers of the ejecta or interaction between the ejecta and nearby circumstellar material or a non-degenerate companion star. The spectral evolution of SN 2018oh is similar to that of a normal SN Ia, but is characterized by prominent and persistent carbon absorption features. The C II features can be detected from the early phases to about 3 weeks after the maximum light, representing the latest detection of carbon ever recorded in a SN Ia. This indicates that a considerable amount of unburned carbon exists in the ejecta of SN 2018oh and may mix into deeper layers., Comment: 48 pages, 23 figures. This paper is part of a coordinated effort between groups. Accepted for publication in ApJ

Published
2019
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4. The Weddell Gyre, Southern Ocean: Present Knowledge and Future Challenges

Author

Oliver J. Lechtenfeld, A. C. Naveira Garabato, Sunke Schmidtko, Boris P. Koch, Matthew R. Mazloff, Maria Vernet, Walter Geibert, Tore Hattermann, Ariane Verdy, Christian Haas, Claus-Dieter Hillenbrand, Volker Strass, Judith Hauck, M.M. Rutgers Loeff, Oliver Huhn, Loïc Jullion, Michael P. Meredith, Sinhue Torres-Valdes, Clara Jule Marie Hoppe, Peter Croot, Dorothee C. E. Bakker, Peter J. Brown, Mario Hoppema, Hartmut Hellmer, Ilka Peeken, Eva-Maria Nöthig, Wilfried Jokat, J. A. Brearley, Michael Schröder, Institut méditerranéen d'océanologie (MIO), and Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS)

Subjects
010504 meteorology & atmospheric sciences, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, Prime meridian, 010502 geochemistry & geophysics, 01 natural sciences, law.invention, Atmosphere, regional models, law, Ocean gyre, Sea ice, 14. Life underwater, oceanography, 0105 earth and related environmental sciences, geography, Weddell Sea, geography.geographical_feature_category, Polar night, Ocean current, Weddell Gyre, Westerlies, Circumpolar star, long-termsampling, Geophysics, Oceanography, 13. Climate action, [SDU]Sciences of the Universe [physics], Environmental science, Antarctica
Abstract

International audience; The Weddell Gyre (WG) is one of the main oceanographic features of the Southern Ocean south of the Antarctic Circumpolar Current which plays an influential role in global ocean circulation as well as gas exchange with the atmosphere. We review the state-of-the art knowledge concerning the WG from an interdisciplinary perspective, uncovering critical aspects needed to understand this system's role in shaping the future evolution of oceanic heat and carbon uptake over the next decades. The main limitations in our knowledge are related to the conditions in this extreme and remote environment, where the polar night, very low air temperatures, and presence of sea ice year-round hamper field and remotely sensed measurements. We highlight the importance of winter and under-ice conditions in the southern WG, the role that new technology will play to overcome present-day sampling limitations, the importance of the WG connectivity to the low-latitude oceans and atmosphere, and the expected intensification of the WG circulation as the westerly winds intensify. Greater international cooperation is needed to define key sampling locations that can be visited by any research vessel in the region. Existing transects sampled since the 1980s along the Prime Meridian and along an East-West section at 62°S should be maintained with regularity to provide answers to the relevant questions. This approach will provide long-term data to determine trends and will improve representation of processes for regional, Antarctic-wide, and global modeling efforts—thereby enhancing predictions of the WG in global ocean circulation and climate.

Published
2019
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5. SN 2012fr: Ultraviolet, Optical, and Near-Infrared Light Curves of a Type Ia Supernova Observed Within a Day of Explosion

Author

David Rabinowitz, C. Baltay, Wendy L. Freedman, Peter Nugent, Richard Scalzo, M. Childress, Damien Turpin, Peter Hoeflich, Christopher Cain, Nicholas B. Suntzeff, Nidia Morrell, Emma S. Walker, S. Castellon, Brian P. Schmidt, E. Conseil, Carlos Contreras, Alain Klotz, Maximilian Stritzinger, Gastón Folatelli, Brad E. Tucker, Christopher R. Burns, Eric Hsiao, Peter J. Brown, Kevin Krisciunas, C. Corco, Benjamin J. Shappee, S. Parker, Anthony L. Piro, J. Serón, S. E. Persson, Mario Hamuy, Mark M. Phillips, C. Gonzalez, Abdo Campillay, E. Baron, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-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), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie ( IRAP ), and Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS )

Subjects
Infrared, DELAY-TIME DISTRIBUTION, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Ciencias Físicas, CHEMICAL EVOLUTION, Astrophysics, medicine.disease_cause, 01 natural sciences, Atomic, Physical Chemistry, purl.org/becyt/ford/1 [https], Particle and Plasma Physics, 010303 astronomy & astrophysics, Ultraviolet radiation, Physics, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), supernovae: individual (SN 2012fr), Visible radiation, Supernova, IMPROVED DISTANCES, Astrophysics - High Energy Astrophysical Phenomena, Astronomical and Space Sciences, CIENCIAS NATURALES Y EXACTAS, Physical Chemistry (incl. Structural), INDIVIDUAL (SN 2012FR) [SUPERNOVAE], MAXIMUM BRIGHTNESS, FOS: Physical sciences, Astronomy & Astrophysics, NEBULAR-PHASE SPECTRA, GENERAL [SUPERNOVAE], supernovae: general, ABUNDANCE RATIOS, individual [supernovae], 0103 physical sciences, medicine, Nuclear, WHITE-DWARFS, supernovae: individual, Near infrared light, 010308 nuclear & particles physics, STANDARD STARS, Molecular, Astronomy and Astrophysics, purl.org/becyt/ford/1.3 [https], Astronomía, Space and Planetary Science, DIGITAL SKY SURVEY, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Near infrared radiation, Ultraviolet, HUBBLE CONSTANT
Abstract

We present detailed ultraviolet, optical, and near-infrared light curves of the Type Ia supernova (SN) 2012fr, which exploded in the Fornax cluster member NGC 1365. These precise high-cadence light curves provide a dense coverage of the flux evolution from −12 to +140 days with respect to the epoch of B-band maximum (tBmax). Supplementary imaging at the earliest epochs reveals an initial slow and nearly linear rise in luminosity with a duration of ∼2.5 days, followed by a faster rising phase that is well reproduced by an explosion model with a moderate amount of 56Ni mixing in the ejecta. From our analysis of the light curves, we conclude that: (i) the explosion occurred 1800 Å) luminosity was 16.5 ± 0.6 days, (iii) the supernova suffered little or no host-galaxy dust reddening, (iv) the peak luminosity in both the optical and near-infrared was consistent with the bright end of normal Type Ia diversity, and (v) 0.60 ± 0.15 M⊙ of 56Ni was synthesized in the explosion. Despite its normal luminosity, SN 2012fr displayed unusually prevalent high-velocity Ca II and Si II absorption features, and a nearly constant photospheric velocity of the Si II λ6355 line at ∼12,000 km s-1 that began ∼5 days before tBmax. We also highlight some of the other peculiarities in the early phase photometry and the spectral evolution. SN 2012fr also adds to a growing number of Type Ia supernovae that are hosted by galaxies with direct Cepheid distance measurements., Facultad de Ciencias Astronómicas y Geofísicas, Instituto de Astrofísica de La Plata

Published
2018
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6. The thermodynamic balance of the Weddell Gyre

Author

Sheldon Bacon, Peter J. Brown, Paul R. Holland, Loïc Jullion, Michael P. Meredith, Alberto C. Naveira Garabato, Jan D. Zika, National Oceanography Centre [Southampton] (NOC), University of Southampton, Laboratoire des Écoulements Géophysiques et Industriels [Grenoble] (LEGI ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Institut méditerranéen d'océanologie (MIO), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), British Antarctic Survey (BAS), Natural Environment Research Council (NERC), National Oceanography Centre (NOC), and Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN)

Subjects
0301 basic medicine, Weddell Sea Bottom Water, [SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere, geography, Water mass, geography.geographical_feature_category, Buoyancy, 010504 meteorology & atmospheric sciences, engineering.material, 01 natural sciences, Salinity, 03 medical and health sciences, 030104 developmental biology, Geophysics, Antarctic Bottom Water, Oceanography, Ocean gyre, Circumpolar deep water, engineering, Sea ice, General Earth and Planetary Sciences, 14. Life underwater, Geology, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract

The thermodynamic balance of the Weddell Gyre is assessed from an inverse estimate of the circulation across the gyre's rim. The gyre experiences a weak net buoyancy gain that arises from a leading-order cancellation between two opposing contributions, linked to two cells of water mass transformation and diapycnal overturning. The lower cell involves a cooling-driven densification of 8.4 ± 2.0 Sv of Circumpolar Deep Water and Antarctic Bottom Water near the gyre's southern and western margins. The upper cell entails a freshening-driven conversion of 4.9 ± 2.0 Sv of Circumpolar Deep Water into lighter upper-ocean waters within the gyre interior. The distinct role of salinity between the two cells stems from opposing salinity changes induced by sea ice production, meteoric sources and admixture of fresh upper-ocean waters in the lower cell, which contrasts with coherent reductions in salinity associated with sea ice melting and meteoric sources in the upper cell.

Published
2016
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7. A uniform, quality controlled Surface Ocean CO2 Atlas (SOCAT)

Author

Denis Pierrot, Aki Murata, Truls Johannessen, Benjamin Pfeil, A. Nakadate, S. Hankin, Jeremy Malczyk, Ludger Mintrop, X. A. Padín, Jerry Tjiputra, Are Olsen, Abdirahman M Omar, C.S. Wong, Robert M. Key, Wei-Jun Cai, Steve D Jones, Burke Hales, Reiner Schlitzer, Rainer Sieger, Siv K. Lauvset, Francisco P. Chavez, Peter Landschützer, G.-H. Park, Christopher L. Sabine, Liliane Merlivat, Mario Hoppema, Ray F. Weiss, Helmuth Thomas, Dorothee C. E. Bakker, Taro Takahashi, Ute Schuster, C. Miyazaki, Maria Hood, K. Tedesco, Richard G. J. Bellerby, Maciej Telszewski, Alexander Kozyr, V. V. S. S. Sarma, Tobias Steinhoff, Douglas Vandemark, Takashi Midorikawa, Jacqueline Boutin, Bronte Tilbrook, Juana Magdalena Santana-Casiano, Ansley Manke, Nathalie Lefèvre, Joe Salisbury, Nick J. Hardman-Mountford, David J. Hydes, Alberto Borges, R. Wanninkhof, Heather Koyuk, T. Veness, Masao Ishii, Yukihiro Nojiri, Andrew J. Watson, K. Paterson, T. Suzuki, Simone R. Alin, Melchor González-Dávila, N. R. Bates, Aida F. Ríos, Alain Poisson, Christoph Heinze, Richard A. Feely, Andrew Lenton, Birgit Schneider, Christopher W. Hunt, A. Lourantou, Catherine Goyet, Andrea J. Fassbender, Peter J. Brown, C. Cosca, Nicolas Metzl, S. Nakaoka, J. Akl, Arne Körtzinger, Fiz F. Pérez, Ingunn Skjelvan, Y. Nakano, A. Chen, Hisayuki Yoshikawa-Inoue, Couplage physique-biogéochimie-carbone (PHYBIOCAR), Laboratoire d'Océanographie et du Climat : Expérimentations et Approches Numériques (LOCEAN), Muséum national d'Histoire naturelle (MNHN)-Institut de Recherche pour le Développement (IRD)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut 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)-Université Paris Diderot - Paris 7 (UPD7)-École polytechnique (X)-Centre National d'Études Spatiales [Toulouse] (CNES)-Sorbonne Université (SU)-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)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-École polytechnique (X)-Centre National d'Études Spatiales [Toulouse] (CNES)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Muséum national d'Histoire naturelle (MNHN)-Institut de Recherche pour le Développement (IRD)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut 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)-Université Paris Diderot - Paris 7 (UPD7)-École polytechnique (X)-Centre National d'Études Spatiales [Toulouse] (CNES)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Échanges dans la couche de surface : des pôles aux tropiques (SURF), Instituto de Investigaciones Marinas, Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Muséum national d'Histoire naturelle (MNHN)-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)-Université Paris Diderot - Paris 7 (UPD7)-École polytechnique (X)-Centre National d'Études Spatiales [Toulouse] (CNES)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), and 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)-Université Paris Diderot - Paris 7 (UPD7)-École polytechnique (X)-Centre National d'Études Spatiales [Toulouse] (CNES)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Muséum national d'Histoire naturelle (MNHN)-Institut Pierre-Simon-Laplace (IPSL (FR_636))

Subjects
0106 biological sciences, Meteorology, 010504 meteorology & atmospheric sciences, Surface ocean, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], [SDE.MCG]Environmental Sciences/Global Changes, Cruise, [PHYS.PHYS.PHYS-GEO-PH]Physics [physics]/Physics [physics]/Geophysics [physics.geo-ph], computer.software_genre, Data type, 01 natural sciences, 14. Life underwater, lcsh:Environmental sciences, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, lcsh:GE1-350, Data collection, Database, Uniform - quality, Atlas (topology), 010604 marine biology & hydrobiology, lcsh:QE1-996.5, lcsh:Geology, Data point, Data access, 13. Climate action, General Earth and Planetary Sciences, computer
Abstract

19 páginas, 6 tablas, 4 figuras.-- B. Pfeil ... et al.-- Proyecto Carbochange.-- Distribuido bajo licencia Creative Commons, A well-documented, publicly available, global data set of surface ocean carbon dioxide (CO2) parameters has been called for by international groups for nearly two decades. The Surface Ocean CO2 Atlas (SOCAT) project was initiated by the international marine carbon science community in 2007 with the aim of providing a comprehensive, publicly available, regularly updated, global data set of marine surface CO2, which had been subject to quality control (QC). Many additional CO2 data, not yet made public via the Carbon Dioxide Information Analysis Center (CDIAC), were retrieved from data originators, public websites and other data centres. All data were put in a uniform format following a strict protocol. Quality control was carried out according to clearly defined criteria. Regional specialists performed the quality control, using state-of-the-art web-based tools, specially developed for accomplishing this global team effort. SOCAT version 1.5 was made public in September 2011 and holds 6.3 million quality controlled surface CO2 data points from the global oceans and coastal seas, spanning four decades (1968–2007). Three types of data products are available: individual cruise files, a merged complete data set and gridded products. With the rapid expansion of marine CO2 data collection and the importance of quantifying net global oceanic CO2 uptake and its changes, sustained data synthesis and data access are priorities., Bjerknes Centre for Climate Research, University of Bergen, Uni Research (Norway), US National Oceanic and Atmospheric Administration, University of Washington, Oak Ridge National Laboratory (US), University of East Anglia (UEA, UK), PANGAEA

Published
2013
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8. The Ninth Data Release of the Sloan Digital Sky Survey: First Spectroscopic Data from the SDSS-III Baryon Oscillation Spectroscopic Survey

Author

Christopher P. Ahn, Rachael Alexandroff, Carlos Allende Prieto, Scott F. Anderson, Timothy Anderton, Brett H. Andrews, Éric Aubourg, Stephen Bailey, Eduardo Balbinot, Rory Barnes, Julian Bautista, Timothy C. Beers, Alessandra Beifiori, Andreas A. Berlind, Vaishali Bhardwaj, Dmitry Bizyaev, Cullen H. Blake, Michael R. Blanton, Michael Blomqvist, John J. Bochanski, Adam S. Bolton, Arnaud Borde, Jo Bovy, W. N. Brandt, J. Brinkmann, Peter J. Brown, Joel R. Brownstein, Kevin Bundy, N. G. Busca, William Carithers, Aurelio R. Carnero, Michael A. Carr, Dana I. Casetti-Dinescu, Yanmei Chen, Cristina Chiappini, Johan Comparat, Natalia Connolly, Justin R. Crepp, Stefano Cristiani, Rupert A. C. Croft, Antonio J. Cuesta, Luiz N. da Costa, James R. A. Davenport, Kyle S. Dawson, Roland de Putter, Nathan De Lee, Timothée Delubac, Saurav Dhital, Anne Ealet, Garrett L. Ebelke, Edward M. Edmondson, Daniel J. Eisenstein, S. Escoffier, Massimiliano Esposito, Michael L. Evans, Xiaohui Fan, Bruno Femenía Castellá, Emma Fernández Alvar, Leticia D. Ferreira, N. Filiz Ak, Hayley Finley, Scott W. Fleming, Andreu Font-Ribera, Peter M. Frinchaboy, D. A. García-Hernández, A. E. García Pérez, Jian Ge, R. Génova-Santos, Bruce A. Gillespie, Léo Girardi, Jonay I. González Hernández, Eva K. Grebel, James E. Gunn, Hong Guo, Daryl Haggard, Jean-Christophe Hamilton, David W. Harris, Suzanne L. Hawley, Frederick R. Hearty, Shirley Ho, David W. Hogg, Jon A. Holtzman, Klaus Honscheid, J. Huehnerhoff, Inese I. Ivans, Željko Ivezić, Heather R. Jacobson, Linhua Jiang, Jonas Johansson, Jennifer A. Johnson, Guinevere Kauffmann, David Kirkby, Jessica A. Kirkpatrick, Mark A. Klaene, Gillian R. Knapp, Jean-Paul Kneib, Jean-Marc Le Goff, Alexie Leauthaud, Khee-Gan Lee, Young Sun Lee, Daniel C. Long, Craig P. Loomis, Sara Lucatello, Britt Lundgren, Robert H. Lupton, Bo Ma, Zhibo Ma, Nicholas MacDonald, Claude E. Mack, Suvrath Mahadevan, Marcio A. G. Maia, Steven R. Majewski, Martin Makler, Elena Malanushenko, Viktor Malanushenko, A. Manchado, Rachel Mandelbaum, Marc Manera, Claudia Maraston, Daniel Margala, Sarah L. Martell, Cameron K. McBride, Ian D. McGreer, Richard G. McMahon, Brice Ménard, Sz. Meszaros, Jordi Miralda-Escudé, Antonio D. Montero-Dorta, Francesco Montesano, Heather L. Morrison, Demitri Muna, Jeffrey A. Munn, Hitoshi Murayama, Adam D. Myers, A. F. Neto, Duy Cuong Nguyen, Robert C. Nichol, David L. Nidever, Pasquier Noterdaeme, Sebastián E. Nuza, Ricardo L. C. Ogando, Matthew D. Olmstead, Daniel J. Oravetz, Russell Owen, Nikhil Padmanabhan, Nathalie Palanque-Delabrouille, Kaike Pan, John K. Parejko, Prachi Parihar, Isabelle Pâris, Petchara Pattarakijwanich, Joshua Pepper, Will J. Percival, Ismael Pérez-Fournon, Ignasi Pérez-Ràfols, Patrick Petitjean, Janine Pforr, Matthew M. Pieri, Marc H. Pinsonneault, G. F. Porto de Mello, Francisco Prada, Adrian M. Price-Whelan, M. Jordan Raddick, Rafael Rebolo, James Rich, Gordon T. Richards, Annie C. Robin, Helio J. Rocha-Pinto, Constance M. Rockosi, Natalie A. Roe, Ashley J. Ross, Nicholas P. Ross, Graziano Rossi, J. A. Rubiño-Martin, Lado Samushia, J. Sanchez Almeida, Ariel G. Sánchez, Basílio Santiago, Conor Sayres, David J. Schlegel, Katharine J. Schlesinger, Sarah J. Schmidt, Donald P. Schneider, Mathias Schultheis, Axel D. Schwope, C. G. Scóccola, Uros Seljak, Erin Sheldon, Yue Shen, Yiping Shu, Jennifer Simmerer, Audrey E. Simmons, Ramin A. Skibba, M. F. Skrutskie, A. Slosar, Flavia Sobreira, Jennifer S. Sobeck, Keivan G. Stassun, Oliver Steele, Matthias Steinmetz, Michael A. Strauss, Alina Streblyanska, Nao Suzuki, Molly E. C. Swanson, Tomer Tal, Aniruddha R. Thakar, Daniel Thomas, Benjamin A. Thompson, Jeremy L. Tinker, Rita Tojeiro, Christy A. Tremonti, M. Vargas Magaña, Licia Verde, Matteo Viel, Shailendra K. Vikas, Nicole P. Vogt, David A. Wake, Ji Wang, Benjamin A. Weaver, David H. Weinberg, Benjamin J. Weiner, Andrew A. West, Martin White, John C. Wilson, John P. Wisniewski, W. M. Wood-Vasey, Brian Yanny, Christophe Yèche, Donald G. York, O. Zamora, Gail Zasowski, Idit Zehavi, Gong-Bo Zhao, Zheng Zheng, Guangtun Zhu, Joel C. Zinn, APC - Cosmologie, 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)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-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)-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), AstroParticule et Cosmologie (APC (UMR_7164)), 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), BOSS, Instituto de Astrofisica de Canarias (IAC), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Elon University [NC, USA], Department of Astronomy [Seattle], University of Washington [Seattle], The University of Notre Dame [Sydney], Apache point observatory, 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), Département de Physique des Particules (ex SPP) (DPhP), 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, Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), 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), Unité Scientifique de la Station de Nançay (USN), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), 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 d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), Universitat de Barcelona, Observatoire des Sciences de l'Univers en région Centre (OSUC), and Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Atles, Astrophysics, Surveys, 01 natural sciences, Astronomical spectroscopy, Via láctea, Observatory, Observacions astronòmiques, Physical Sciences and Mathematics, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, media_common, Mapeamentos astronômicos, Physics, [PHYS]Physics [physics], Astrophysics::Instrumentation and Methods for Astrophysics, Atlases, Astrometry, Cosmology, atlases, Instrumentation and Methods for Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Astronomical observations, Cosmology and Gravitation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], media_common.quotation_subject, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, catalogs, surveys, Formacao de galaxias, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Instrumentation and Methods for Astrophysics (astro-ph.IM), Spectrograph, Astrophysics::Galaxy Astrophysics, Cosmologia, 010308 nuclear & particles physics, Astronomy and Astrophysics, Quasar, Cosmology and Extragalactic Astrophysics, Espectroscòpia, Galaxy, Spectrum analysis, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Stars, Space and Planetary Science, Sky, Catalogs, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

The Sloan Digital Sky Survey III (SDSS-III) presents the first spectroscopic data from the Baryon Oscillation Spectroscopic Survey (BOSS). This ninth data release (DR9) of the SDSS project includes 535,995 new galaxy spectra (median z=0.52), 102,100 new quasar spectra (median z=2.32), and 90,897 new stellar spectra, along with the data presented in previous data releases. These spectra were obtained with the new BOSS spectrograph and were taken between 2009 December and 2011 July. In addition, the stellar parameters pipeline, which determines radial velocities, surface temperatures, surface gravities, and metallicities of stars, has been updated and refined with improvements in temperature estimates for stars with T_eff-0.5. DR9 includes new stellar parameters for all stars presented in DR8, including stars from SDSS-I and II, as well as those observed as part of the SDSS-III Sloan Extension for Galactic Understanding and Exploration-2 (SEGUE-2). The astrometry error introduced in the DR8 imaging catalogs has been corrected in the DR9 data products. The next data release for SDSS-III will be in Summer 2013, which will present the first data from the Apache Point Observatory Galactic Evolution Experiment (APOGEE) along with another year of data from BOSS, followed by the final SDSS-III data release in December 2014., 9 figures; 2 tables. Submitted to ApJS. DR9 is available at http://www.sdss3.org/dr9

Published
2012
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9. Type Ia Supernova Carbon Footprints

Author

Cecilia Aragon, K. Paech, A. Canto, S. Bongard, Richard Scalzo, Charling Tao, R. Pereira, G. Smadja, Peter Nugent, M. Kerschhaggl, N. Chotard, E. Gangler, K. Runge, Peter A. Milne, R. Pain, C. Baltay, Chen Wu, Stephen Bailey, Benjamin A. Weaver, M. J. Childress, H. K. Fakhouri, R. C. Thomas, Saul Perlmutter, Y. Copin, C. Buton, Eric Hsiao, David Rubin, S. C. Loken, Peter J. Brown, Emmanuel Pecontal, M. Kowalski, P. Antilogus, Greg Aldering, David Rabinowitz, M. Rigault, 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), Institut de Physique Nucléaire de Lyon (IPNL), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre de Recherche Astrophysique de Lyon (CRAL), 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), NEARBY SUPERNOVA FACTORY, 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), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)

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], FOS: Physical sciences, chemistry.chemical_element, Context (language use), Astrophysics, 01 natural sciences, Spectral line, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Ejecta, 010303 astronomy & astrophysics, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Light curve, Supernova, Wavelength, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], chemistry, 13. Climate action, Space and Planetary Science, Circular symmetry, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Carbon, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present convincing evidence of unburned carbon at photospheric velocities in new observations of 5 Type Ia supernovae (SNe Ia) obtained by the Nearby Supernova Factory. These SNe are identified by examining 346 spectra from 124 SNe obtained before +2.5 d relative to maximum. Detections are based on the presence of relatively strong C II 6580 absorption "notches" in multiple spectra of each SN, aided by automated fitting with the SYNAPPS code. Four of the 5 SNe in question are otherwise spectroscopically unremarkable, with ions and ejection velocities typical of SNe Ia, but spectra of the fifth exhibits high-velocity (v > 20,000 km/s) Si II and Ca II features. On the other hand, the light curve properties are preferentially grouped, strongly suggesting a connection between carbon-positivity and broad band light curve/color behavior: Three of the 5 have relatively narrow light curves but also blue colors, and a fourth may be a dust-reddened member of this family. Accounting for signal-to-noise and phase, we estimate that 22 +10/-6% of SNe Ia exhibit spectroscopic C II signatures as late as -5 d with respect to maximum. We place these new objects in the context of previously recognized carbon-positive SNe Ia, and consider reasonable scenarios seeking to explain a physical connection between light curve properties and the presence of photospheric carbon. We also examine the detailed evolution of the detected carbon signatures and the surrounding wavelength regions to shed light on the distribution of carbon in the ejecta. Our ability to reconstruct the C II 6580 feature in detail under the assumption of purely spherical symmetry casts doubt on a "carbon blobs" hypothesis, but does not rule out all asymmetric models. A low volume filling factor for carbon, combined with line-of-sight effects, seems unlikely to explain the scarcity of detected carbon in SNe Ia by itself., 22 pages, 12 figures. Accepted for publication in The Astrophysical Journal

Published
2011
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10. Optical Observations of the Rapidly Expanding Type Ia Supernova 2007gi

Author

Lifan Wang, M. Zhai, Mohan Ganeshalingam, Xu Zhou, R. C. Shang, J. Deng, Thea N. Steele, Tianmeng Zhang, Y. L. Qiu, Xiang-Gao Wang, J. M. Silverman, J. Li, Peter J. Brown, Alexei V. Filippenko, Weidong Li, Tenglin Li, Beaussier, Catherine, Laboratoire d'Astrophysique de Marseille (LAM), 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
Physics, Brightness, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Light curve, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], 01 natural sciences, Galaxy, Spectral line, Photometry (optics), Supernova, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, 0103 physical sciences, Ejecta, 010303 astronomy & astrophysics, Optical observation, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present optical photometry and spectra for the Type Ia supernova (SN Ia) 2007gi in the nearby galaxy NGC 4036. SN 2007gi is characterized by extremely high-velocity (HV) features of the intermediate-mass elements (Si, Ca, and S), with expansion velocities ($v_{\rm exp}$) approaching $\sim$15,500 km s$^{-1}$ near maximum brightness (compared to $\sim$10,600 km s$^{-1}$ for SNe Ia with normal $v_{\rm exp}$). SN 2007gi reached a $B$-band peak magnitude of 13.25$\pm$0.04 mag with a decline rate of $\Delta m_{15}(B)$(true) = 1.33$\pm$0.09 mag. The $B$-band light curve of SN 2007gi demonstrated an interesting two-stage evolution during the nebular phase, with a decay rate of 1.16$\pm$0.05 mag (100 days)$^{-1}$ during $t = 60$--90 days and 1.61$\pm0.04$ mag (100 days)$^{-1}$ thereafter. Such a behavior was also observed in the HV SN Ia 2006X, and might be caused by the interaction between supernova ejecta and circumstellar material (CSM) around HV SNe Ia. Based on a sample of a dozen well-observed $R$-band (or unfiltered) light curves of SNe Ia, we confirm that the HV events may have a faster rise time to maximum than the ones with normal $v_{\rm exp}$., Comment: 30 pages, 10 figures

Published
2010

11. Swift and Chandra Detections of Supernova 2006jc: Evidence for Interaction of the Supernova Shock with a Circumstellar Shell

Author

J. A. Nousek, Alexei V. Filippenko, Roger A. Chevalier, Jochen Greiner, Peter A. Milne, Michael Koss, Stefan Immler, Wayne B. Landsman, Alicia M. Soderberg, Elena Pian, Stephen T. Holland, D. Pooley, Neil Gehrels, Robert Petre, P. W. A. Roming, Filomena Bufano, Luc Dessart, Paolo A. Mazzali, M. Modjaz, David N. Burrows, Nino Panagia, Peter J. Brown, Robert P. Kirshner, Beaussier, Catherine, Laboratoire d'Astrophysique de Marseille (LAM), 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
Physics, 010308 nuclear & particles physics, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Light curve, 01 natural sciences, law.invention, Shock (mechanics), Telescope, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Stars, Supernova, Luminous blue variable, 13. Climate action, Space and Planetary Science, Observatory, law, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, 010303 astronomy & astrophysics, Line (formation)
Abstract

The peculiar Type Ib supernova (SN) 2006jc has been observed with the UV/Optical Telescope (UVOT) and X-Ray Telescope (XRT) on board the Swift observatory over a period of 19 to 183 days after the explosion. Signatures of interaction of the outgoing SN shock with dense circumstellar material (CSM) are detected, such as strong X-ray emission (L_{0.2-10} > E39 erg/s) and the presence of MgII 2800A line emission visible in the UV spectra. In combination with a Chandra observation obtained on day 40 after the explosion, the X-ray light curve is constructed, which shows a unique rise of the X-ray emission by a factor of ~5 over a period of ~4 months, followed by a rapid decline. We interpret the unique X-ray and UV properties as a result of the SN shock interacting with a shell of material that was deposited by an outburst of the SN progenitor two years prior to the explosion. Our results are consistent with the explosion of a Wolf-Rayet star that underwent an episodic mass ejection qualitatively similar to those of luminous blue variable stars prior to its explosion. This led to the formation of a dense (>E7 cm**-3) shell at a distance of ~E16 cm from the site of the explosion, which expands with the WR wind at a velocity of (1300+/-300) km/s., 4 pages, 4 figures, submitted to ApJL (v2)

Published
2008

12. X-Ray, UV, and Optical Observations of Supernova 2006bp with Swift: Detection of Early X-Ray Emission

Author

Michael Koss, L. Dessart, Alicia M. Soderberg, K. W. Weiler, Christopher Williams, Roger A. Chevalier, Elena Pian, David N. Burrows, J. A. Nousek, Peter J. Brown, Stephen T. Holland, Peter A. Milne, D. Pooley, P. W. A. Roming, Stefan Immler, Matthew T. Kelley, Paolo A. Mazzali, Neil Gehrels, Robert Petre, Ken'ichi Nomoto, Wayne B. Landsman, Chris Stockdale, Jochen Greiner, Sergio Campana, Beaussier, Catherine, Laboratoire d'Astrophysique de Marseille (LAM), 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
Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, law.invention, Luminosity, Telescope, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Red supergiant, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Photosphere, 010308 nuclear & particles physics, Astrophysics (astro-ph), Compton scattering, Astronomy and Astrophysics, Supernova, Lorentz factor, 13. Climate action, Space and Planetary Science, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols, Spectral energy distribution
Abstract

We present results on the X-ray and optical/UV emission from the type IIP SN 2006bp and the interaction of the SN shock with its environment, obtained with the X-Ray Telescope (XRT) and UV/Optical Telescope (UVOT) on-board the Swift observatory. SN 2006bp is detected in X-rays at a 4.5 sigma level of significance in the merged XRT data from days 1 to 12 after the explosion. If the X-ray luminosity of (1.8+/-0.4)E39 ergs/s is caused by interaction of the SN shock with circumstellar material (CSM), deposited by a stellar wind from the progenitor's companion star, a mass-loss rate of ~E-05 M_sun/yr is inferred. The mass-loss rate is consistent with the non-detection in the radio with the VLA on days 2, 9, and 11 after the explosion and characteristic of a red supergiant progenitor with a mass around 12-15 M_sun prior to the explosion. In combination with a follow-up XMM-Newton observation obtained on day 21 after the explosion, an X-ray rate of decline with index 1.2+/-0.6 is inferred. Since no other SN has been detected in X-rays prior to the optical peak and since type IIP SNe have an extended 'plateau' phase in the optical, we discuss the scenario that the X-rays might be due to inverse Compton scattering of photospheric optical photons off relativistic electrons produced in circumstellar shocks. However, due to the high required value of the Lorentz factor (~10-100) we conclude that Inverse Compton scattering is an unlikely explanation for the observed X-ray emission. The fast evolution of the optical/ultraviolet spectral energy distribution and the spectral changes observed with Swift reveal the onset of metal line-blanketing and cooling of the expanding photosphere during the first few weeks after the outburst., Comment: 8 pages, 5 figures, accepted for publication in ApJ

Published
2007

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