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2. Results of the KRUSTY Warm Critical Experiments

Author

David I. Poston, Marc A. Gibson, Patrick R. Mclure, and Rene G. Sanchez

Subjects
Engineering (General)
Abstract

The Kilowatt Reactor Using Stirling TechnologY (KRUSTY) was a prototypic nuclear-powered test of a 5-kW(thermal) Kilopower space reactor. This paper presents results from the KRUSTY warm critical experiments, which were completed prior to the final system test. The first set of criticals comprised cold or zero-power criticals; i.e., the core was not heated by fission power. These were followed by three warm criticals, where fission power heated the core to 200°C, 300°C, and 450°C, respectively. These criticals provided the data, confidence, and regulatory framework that were needed to proceed with the KRUSTY nuclear system test. The criticals also provided valuable data for the benchmarking of codes applicable to all nuclear systems. Finally, a comparison of KRUSTY results to pretest predictions is provided, and overall, the models matched the experimental results very closely.

Published
2020
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3. NEW OBSERVATIONS OF

Author

L. Pentericci, E. Vanzella, A. Fontana, M. Castellano, T. Treu, A. Mesinger, M. Dijkstra, A. Grazian, M. Bradač, C. Conselice, S. Cristiani, J. Dunlop, A. Galametz, M. Giavalisco, E. Giallongo, A. Koekemoer, R. McLure, R. Maiolino, D. Paris, and P. Santini

Published
2014

5. MOONS: the Multi-Object Optical and Near-infrared Spectrograph for the VLT

Author

M. Cirasuolo, J. Afonso, M. Carollo, H. Flores, R. Maiolino, E. Oliva, S. Paltani, Leonardo Vanzi, Christopher Evans, M. Abreu, David Atkinson, C. Babusiaux, Steven Beard, F. Bauer, M. Bellazzini, Ralf Bender, P. Best, N. Bezawada, P. Bonifacio, A. Bragaglia, I. Bryson, D. Busher, A. Cabral, K. Caputi, M. Centrone, F. Chemla, A. Cimatti, M-R. Cioni, G. Clementini, J. Coelho, D. Crnojevic, E. Daddi, J. Dunlop, S. Eales, S. Feltzing, A. Ferguson, M. Fisher, A. Fontana, J. Fynbo, B. Garilli, G. Gilmore, A. Glauser, I. Guinouard, F. Hammer, P. Hastings, A. Hess, R. Ivison, P. Jagourel, M. Jarvis, L. Kaper, G. Kauffman, A. T. Kitching, A. Lawrence, D. Lee, B. Lemasle, G. Licausi, S. Lilly, D. Lorenzetti, D. Lunney, F. Mannucci, R. McLure, D. Minniti, D. Montgomery, B. Muschielok, K. Nandra, R. Navarro, P. Norberg, S. Oliver, L. Origlia, N. Padilla, J. Peacock, F. Pedichini, J. Peng, L. Pentericci, J. Pragt, M. Puech, S. Randich, P. Rees, A. Renzini, N. Ryde, M. Rodrigues, I. Roseboom, F. Royer, R. Saglia, A. Sanchez, R. Schiavon, H. Schnetler, D. Sobral, R. Speziali, D. Sun, R. Stuik, A. Taylor, W. Taylor, S. Todd, E. Tolstoy, M. Torres, M. Tosi, E. Vanzella, L. Venema, F. Vitali, M. Wegner, M. Wells, V. Wild, G. Wright, G. Zamorani, M. Zoccali, Astronomy, 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), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), and Low Energy Astrophysics (API, FNWI)

Subjects
Physics, [PHYS]Physics [physics], Very Large Telescope, Galactic astronomy, Milky Way, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astrophysics, Large Synoptic Survey Telescope, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy, Redshift, Galaxy formation and evolution, Astrophysics::Earth and Planetary Astrophysics, Spectral resolution, Astrophysics::Galaxy Astrophysics
Abstract

MOONS is a new Multi-Object Optical and Near-infrared Spectrograph selected by ESO as a third generation instrument for the Very Large Telescope (VLT). The grasp of the large collecting area offered by the VLT (8.2m diameter), combined with the large multiplex and wavelength coverage (optical to near-IR: 0.8μm - 1.8μm) of MOONS will provide the European astronomical community with a powerful, unique instrument able to pioneer a wide range of Galactic, Extragalactic and Cosmological studies and provide crucial follow-up for major facilities such as Gaia, VISTA, Euclid and LSST. MOONS has the observational power needed to unveil galaxy formation and evolution over the entire history of the Universe, from stars in our Milky Way, through the redshift desert, and up to the epoch of very first galaxies and re-ionization of the Universe at redshift z>8-9, just few million years after the Big Bang. On a timescale of 5 years of observations, MOONS will provide high quality spectra for >3M stars in our Galaxy and the local group, and for 1-2M galaxies at z>1 (SDSS-like survey), promising to revolutionise our understanding of the Universe. The baseline design consists of ~1000 fibers deployable over a field of view of ~500 square arcmin, the largest patrol field offered by the Nasmyth focus at the VLT. The total wavelength coverage is 0.8μm-1.8μm and two resolution modes: medium resolution and high resolution. In the medium resolution mode (R~4,000-6,000) the entire wavelength range 0.8μm-1.8μm is observed simultaneously, while the high resolution mode covers simultaneously three selected spectral regions: one around the CaII triplet (at R~8,000) to measure radial velocities, and two regions at R~20,000 one in the J-band and one in the H-band, for detailed measurements of chemical abundances. © (2014) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE). Downloading of the abstract is permitted for personal use only.

Published
2014
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6. Improved constraints on the expansion rate of the Universe up to z similar to 1.1 from the spectroscopic evolution of cosmic chronometers

Author

Piero Rosati, J. F. Le Borgne, C. Knobel, Laurence Tresse, James Dunlop, S. Foucaud, K. Kovac, Angela Bongiorno, Michele Moresco, G. Zamorani, Lidia Tasca, Daniela Vergani, Preethi Nair, Marc Kamionkowski, C. Diener, Olga Cucciati, Graziano Coppa, Lucia Pozzetti, S. Bardelli, Michele Cirasuolo, Anton M. Koekemoer, Ross J. McLure, C. López-Sanjuan, Niraj Welikala, Vincenzo Mainieri, C. M. Carollo, Rongmon Bordoloi, Andrea Cimatti, Raul Jimenez, Licia Verde, John D. Silverman, F. Lamareille, Karina Caputi, H. J. Pearce, Masayuki Tanaka, Luke A. Barnes, A. Iovino, Jean-Paul Kneib, S. de la Torre, William G. Hartley, V. Presotto, Christian Maier, L. de Ravel, E. J. Bradshaw, S. Lilly, Yingjie Peng, Robert Chuter, P. Kampczyk, M. Mignoli, H. J. McCracken, Bianca Garilli, Adam Stanford, Marco Scodeggio, Italo Balestra, P. Franzetti, Omar Almaini, Thierry Contini, R. Pello, Enrique Pérez-Montero, V. Le Brun, Raphael Gobat, A. Cappi, Micol Bolzonella, Alvio Renzini, Daniel Stern, Pascal Oesch, O. Le Fèvre, E. Zucca, Dipartimento di Astronomia, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Department of Chemical Engineering, Columbia University, Columbia University [New York], INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), SUPA, Institute for Astronomy, University of Edinburgh, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Departament d'Astronomia i Meteorologia [Barcelona], Universitat de Barcelona (UB), INAF - Osservatorio Astronomico di Brera (OAB), University of Chicago, Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Ecole Polytechnique Fédérale de Lausanne (EPFL), 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), Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), INAF - Osservatorio Astronomico di Padova (OAPD), INAF- Milano, INAF - Osservatorio Astronomico di Trieste (OAT), 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), College of Computing (GATECH), Georgia Institute of Technology [Atlanta], AUTRES, Dipartimento di Fisica, Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB)-Università degli Studi di Milano = University of Milan (UNIMI), Laboratoire Léon Brillouin (LLB - UMR 12), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Hunan Normal University (HNU), Università degli studi di Trieste = University of Trieste, INAF - Osservatorio Astrofisico di Arcetri (OAA), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Space Telescope Science Institute (STSci), 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), Universitat de Barcelona, 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), California Institute of Technology (CALTECH)-NASA, Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), 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), Università degli Studi di Milano-Bicocca [Milano] (UNIMIB)-Università degli Studi di Milano [Milano] (UNIMI), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay, Hunan Normal University, Università degli studi di Trieste, Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Università di Bologna [Bologna] (UNIBO), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut de Ciènces del Cosmos (ICC), Universitat de Barcelona (UB)-Universitat de Barcelona (UB), Istituto Nazionale di Astrofisica - Osservatorio Astronomico di Brera (INAF), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Università degli studi di Milano [Milano]-Università di Milano-Bicocca, Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), M. Moresco, A. Cimatti, R. Jimenez, L. Pozzetti, G. Zamorani, M. Bolzonella, J. Dunlop, F. Lamareille, M. Mignoli, H. Pearce, P. Rosati, D. Stern, L. Verde, E. Zucca, C.M. Carollo, T. Contini, J.-P. Kneib, O. Le Fevre, S.J. Lilly, V. Mainieri, A. Renzini, M. Scodeggio, I. Balestra, R. Gobat, R. McLure, S. Bardelli, A. Bongiorno, K. Caputi, O. Cucciati, S. de la Torre, L. de Ravel, P. Franzetti, B. Garilli, A. Iovino, P. Kampczyk, C. Knobel, K. Kovac, J.-F. Le Borgne, V. Le Brun, C. Maier, R. Pello', Y. Peng, E. Perez-Montero, V. Presotto, J.D. Silverman, M. Tanaka, L.A.M. Tasca, L. Tresse, D. Vergani, O. Almaini, L. Barne, R. Bordoloi, E. Bradshaw, A. Cappi, R. Chuter, M. Cirasuolo, G. Coppa, C. Diener, S. Foucaud, W. Hartley, M. Kamionkowski, A.M. Koekemoer, C. Lopez-Sanjuan, H.J. McCracken, P. Nair, P. Oesch, A. Stanford, and N. Welikala

Subjects
Astrofísica, Cosmology and Nongalactic Astrophysics (astro-ph.CO), galaxy survey, dark energy experiments, Stellar population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Expanding universe, 01 natural sciences, symbols.namesake, Expansió de l'univers, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, Galaxies, Billion years, Galaxy, Redshift, Galàxies, symbols, Elliptical galaxy, Hubble's law, Quintessence, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present new improved constraints on the Hubble parameter H(z) in the redshift range 0.15 < z < 1.1, obtained from the differential spectroscopic evolution of early-type galaxies as a function of redshift. We extract a large sample of early-type galaxies (\sim11000) from several spectroscopic surveys, spanning almost 8 billion years of cosmic lookback time (0.15 < z < 1.42). We select the most massive, red elliptical galaxies, passively evolving and without signature of ongoing star formation. Those galaxies can be used as standard cosmic chronometers, as firstly proposed by Jimenez & Loeb (2002), whose differential age evolution as a function of cosmic time directly probes H(z). We analyze the 4000 �� break (D4000) as a function of redshift, use stellar population synthesis models to theoretically calibrate the dependence of the differential age evolution on the differential D4000, and estimate the Hubble parameter taking into account both statistical and systematical errors. We provide 8 new measurements of H(z) (see Tab. 4), and determine its change in H(z) to a precision of 5-12% mapping homogeneously the redshift range up to z \sim 1.1; for the first time, we place a constraint on H(z) at z \neq 0 with a precision comparable with the one achieved for the Hubble constant (about 5-6% at z \sim 0.2), and covered a redshift range (0.5 < z < 0.8) which is crucial to distinguish many different quintessence cosmologies. These measurements have been tested to best match a ��CDM model, clearly providing a statistically robust indication that the Universe is undergoing an accelerated expansion. This method shows the potentiality to open a new avenue in constrain a variety of alternative cosmologies, especially when future surveys (e.g. Euclid) will open the possibility to extend it up to z \sim 2., 34 pages, 15 figures, 6 tables, published in JCAP. It is a companion to Moresco et al. (2012b, http://arxiv.org/abs/1201.6658) and Jimenez et al. (2012, http://arxiv.org/abs/1201.3608). The H(z) data can be downloaded at http://www.physics-astronomy.unibo.it/en/research/areas/astrophysics/cosmology-with-cosmic-chronometers

Published
2012
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