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First demonstration of improving laser propagation inside the spherical hohlraums by using the cylindrical laser entrance hole

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Matter and Radiation at Extremes 2016年第1期1卷 2-7页

作者： Wenyi Huo Zhichao Li Dong Yang Ke Lan Jie Liu Guoli Ren Sanwei Li Zhiwen Yang Liang Guo Lifei Hou Xuefei Xie Yukun Li Keli Deng Zheng Yuan Xiayu Zhan Guanghui Yuan Haijun Zhang Baibin Jiang Lizhen Huang Kai Du Runchang Zhao Ping Li Wei Wang Jingqin Su Yongkun Ding Xiantu He Weiyan Zhang Institute of Applied Physics and Computational Mathematics Beijing 100088China Research Center of Laser Fusion Chinese Academy of Engineering PhysicsMianyang 621900China Center for Applied Physics and Technology Peking UniversityBeijing 100871China Collaborative Innovation Center of IFSA Shanghai Jiao Tong UniversityShanghai 200240China China Academy of Engineering Physics Mianyang 621900China

The octahedral spherical hohlraums have natural superiority in maintaining high radiation symmetry during the entire capsule implosion process in indirect drive inertial confinement ***,in contrast to the cylindrical hohlraums,the narrow space between the laser beams and the spherical hohlraum wall is usually *** this Letter,we address this crucial issue and report our experimental work conducted on the SGIII-prototype laser facility which unambiguously demonstrates that a simple design of cylindrical laser entrance hole(LEH)can dramatically improve the laser propagation inside the spherical *** addition,the laser beam deflection in the hohlraum is observed for the first time in the *** 2-dimensional simulation results also verify qualitatively the advantages of the spherical hohlraums with cylindrical *** results imply the prospect of adopting the cylindrical LEHs in future spherical ignition hohlraum design.

关键词： Spherical hohlraum Laser propagation Cylindrical laser entrance hole Laser spot movement

An overview from hygroscopic aerosols to cloud droplets: The HygrA-CD campaign in the Athens basin

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Science of The Total Environment 2017年 574卷 216-233页

作者： A. Papayannis A. Argyrouli A. Bougiatioti E. Remoundaki S. Vratolis A. Nenes S. Solomos M. Komppula E. Giannakaki J. Kalogiros R. Banks K. Eleftheriadis E. Mantas E. Diapouli C.G. Tzanis S. Kazadzis I. Binietoglou L. Labzovskii C.S. Zerefos Laser Remote Sensing Unit Physics Department School of Applied Mathematics and Physical Sciences National Technical University of Athens 15780 Zografou Greece School of Earth & Atmospheric Sciences Georgia Institute of Technology Atlanta 30332 GA USA Laboratory of Environmental Science and Engineering School of Mining and Metallurgical Engineering National Technical University of Athens 15780 Zografou Greece ERL INRSTES N.C.S.R. Demokritos 15310 Agia Paraskevi Attiki Greece ICE-HT Foundation for Research and Technology Hellas 26504 Patras Greece Institute of Environmental Research and Sustainable Development National Observatory of Athens Athens Greece School of Chemical & Biomolecular Engineering Georgia Institute of Technology Atlanta 30332 GA USA Institute for Astronomy Astrophysics Space Applications and Remote Sensing National Observatory of Athens Athens Greece Finnish Meteorological Institute Kuopio Finland Department of Environmental Physics and Meteorology Faculty of Physics University of Athens Athens Greece Barcelona Supercomputing Center-Centro Nacional de Supercomputación (BSC-CNS) Earth Sciences Department Jordi Girona 29 Edificio Nexus II Barcelona Spain Environmental Modelling Laboratory Polytechnic University of Catalonia Barcelona Spain Climate Research Group Division of Environmental Physics and Meteorology Department of Physics National and Kapodistrian University of Athens 15784 Athens Greece Physikalisch-Meteorologisches Observatorium Davos World Radiation Center Switzerland National Institute of Research and Development for Optoelectronics Magurele Romania Research Center of Ecological Safety Russian Academy of Sciences St. Petersburg Russia Biomedical Research Foundation of the Academy of Athens Athens Greece Navarino Environmental Observatory (N.E.O.) Messinia Greece

The international experimental campaign Hygroscopic Aerosols to Cloud Droplets (HygrA-CD), organized in the Greater Athens Area (GAA), Greece from 15 May to 22 June 2014, aimed to study the physico-chemical properties of aerosols and their impact on the formation of clouds in the convective Planetary Boundary Layer (PBL). We found that under continental (W-NW-N) and Etesian (NE) synoptic wind flow and with a deep moist PBL (~ 2–2.5 km height), mixed hygroscopic (anthropogenic, biomass burning and marine) particles arrive over the GAA, and contribute to the formation of convective non-precipitating PBL clouds (with droplets of ~ 16–20 μm mean diameter) with vertical extent up to 500 m. Under these conditions, high updraft velocities (1–2 m s − 1 ) and cloud condensation nuclei (CCN) concentrations (~ 2000 cm − 3 at 1% supersaturation), generated clouds with an estimated cloud droplet number of ~ 600 cm − 3 . Under Saharan wind flow conditions (S-SW) a shallow PBL (< 1–1.2 km height) develops, leading to much higher CCN concentrations (~ 3500–5000 cm − 3 at 1% supersaturation) near the ground; updraft velocities, however, were significantly lower, with an estimated maximum cloud droplet number of ~ 200 cm − 3 and without observed significant PBL cloud formation. The largest contribution to cloud droplet number variance is attributed to the updraft velocity variability, followed by variances in aerosol number concentration.

关键词： Aerosol Raman lidar Doppler lidar Precipitation radar SMPS CCN Aerosol chemical properties WRF FLEXPART model Cloud development Cloud droplet number HygrA-CD Athens Greece

Prime-Cam: A first-light instrument for the CCAT-prime telescope

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arXiv 2018年

作者： Vavagiakis, E.M. Ahmed, Z. Ali, A. Basu, K. Battaglia, N. Bertoldi, F. Bond, R. Bustos, R. Chapman, S.C. Chung, D. Coppi, G. Cothard, N.F. Dicker, S. Duell, C.J. Duff, S.M. Erler, J. Fich, M. Galitzki, N. Gallardo, P.A. Henderson, S.W. Herter, T.L. Hilton, G. Hubmayr, J. Irwin, K.D. Koopman, B.J. McMahon, J. Murray, N. Niemack, M.D. Nikola, T. Nolta, M. Orlowski-Scherer, J. Parshley, S.C. Riechers, D.A. Rossi, K. Scott, D. Sierra, C. Silva-Feaver, M. Simon, S.M. Stacey, G.J. Stevens, J.R. Ullom, J.N. Vissers, M.R. Walker, S. Wollack, E.J. Xu, Z. Zhu, N. Department of Physics Cornell University IthacaNY14853 United States Kavli Institute for Particle Astrophysics and Cosmology SLAC National Accelerator Laboratory Menlo ParkCA94025 United States Department of Physics University of California Berkeley BerkeleyCA94720 United States Argelander Institute for Astronomy University of Bonn BonnD-53121 Germany Department of Astronomy Cornell University IthacaNY14853 United States Center for Computational Astrophysics Simons Foundation NYCNY10010 United States Canadian Institute for Theoretical Astrophysics University of Toronto TorontoON Canada Facultad de Ingeniería Universidad Católica de la Santísima Concepción Concepción Chile Department of Physics and Astronomy University of British Columbia VancouverBC Canada National Research Council Herzberg Astronomy and Astrophysics VictoriaBC Canada Department of Physics Stanford University StanfordCA94305 United States Department of Applied and Engineering Physics Cornell University IthacaNY14853 United States Department of Physics and Astronomy University of Pennsylvania PhiladelphiaPA19104 United States Department of Physics and Astronomy University of Waterloo WaterlooON Canada Department of Physics UCSD La JollaCA92093 United States Quantum Sensors Group National Institute of Standards and Technology BoulderCO80305 United States Kavli Institute for Particle Astrophysics and Cosmology Stanford University StanfordCA94305 United States Department of Physics University of Michigan Ann ArborMI48109 United States Cornell Center for Astrophysics and Planetary Science Cornell University IthacaNY14853 United States Department of Applied Physics University of Michigan Ann ArborMI48109 United States Department of Astrophysical and Planetary Sciences University of Colorado Boulder BoulderCO80309 United States NASA/Goddard Space Flight Center GreenbeltMD20771 United States

CCAT-prime will be a 6-meter aperture telescope operating from sub-mm to mm wavelengths, located at 5600 meters elevation on Cerro Chajnantor in the Atacama Desert in Chile. Its novel crossed-Dragone optical design will deliver a high throughput, wide field of view capable of illuminating much larger arrays of sub-mm and mm detectors than can existing telescopes. We present an overview of the motivation and design of Prime-Cam, a first-light instrument for CCAT-prime. Prime-Cam will house seven instrument modules in a 1.8 meter diameter cryostat, cooled by a dilution refrigerator. The optical elements will consist of silicon lenses, and the instrument modules can be individually optimized for particular science goals. The current design enables both broadband, dual-polarization measurements and narrow-band, Fabry-Perot spectroscopic imaging using multichroic transition-edge sensor (TES) bolometers operating between 190 and 450 GHz. It also includes broadband kinetic induction detectors (KIDs) operating at 860 GHz. This wide range of frequencies will allow excellent characterization and removal of galactic foregrounds, which will enable precision measurements of the sub-mm and mm sky. Prime-Cam will be used to constrain cosmology via the Sunyaev-Zeldovich effects, map the intensity of [CII] 158 µm emission from the Epoch of Reionization, measure Cosmic Microwave Background polarization and foregrounds, and characterize the star formation history over a wide range of redshifts. More information about CCAT-prime can be found at ***. Copyright © 2018, The Authors. All rights reserved.

关键词： Fabry-Perot interferometers

Preparation of logically labeled pure states with only two turns for bulk quantum computation

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arXiv 2017年

作者： Xin, Tao Hao, Liang Hou, Shi-Yao Feng, Guan-Ru Long, Gui-Lu State Key Laboratory of Low-dimensional Quantum Physics and Department of Physics Tsinghua University Beijing100084 China Tsinghua National Laboratory of Information Science and Technology Beijing100084 China Institute of Applied Physics and Computational Mathematics Beijing100094 China Microsystem and Terahertz Research Center China Academy of Engineering Physics Chengdu610200 China Institute of Electronic Engineering China Academy of Engineering Physics Mianyang621999 China Institute for Quantum Computing WaterlooONN2L 3G1 Canada Department of Physics and Astronomy University of Waterloo WaterlooONN2L 3G1 Canada Innovative Center of Quantum Matter Beijing100084 China

Quantum state preparation plays an equally important role with quantum operations and measurements in quantum information processing. The previous methods of preparing initial state for bulk quantum computation all have inevitable disadvantages, such as, requiring multiple experiments, causing loss of signals, or requiring molecules with restrictive structure. In this work, three kinds of quantum circuits are introduced to prepare the pseudo-pure states of (n − 1) qubits in the Hilbert space of n coupled spins which merely need the assist of one ancilla spin and two experiments independent of n. Being without gradient fields effectively avoids the reduction of the signals. Our methods have no special requirements on the structure of the used molecules. To test these methods more comprehensively, we experimentally demonstrate the preparation of the labeled pseudo-pure states using heteronuclear 2-qubit and homonuclear 4-qubit nuclear magnetic resonance quantum information processor. Copyright © 2017, The Authors. All rights reserved.

关键词： Molecules

First Investigation on the Radiation Field of the Spherical Hohlraum

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Physical Review Letters 2016年第2期117卷 025002-025002页

作者： Wen Yi Huo (霍文义) Zhichao Li (李志超) Yao-Hua Chen (陈耀桦) Xuefei Xie (谢旭飞) Ke Lan (蓝可) Jie Liu (刘杰) Guoli Ren (任国利) Yongsheng Li (李永升) Yonggang Liu (刘永刚) Xiaohua Jiang (蒋小华) Dong Yang (杨冬) Sanwei Li (李三伟) Liang Guo (郭亮) Huan Zhang (章欢) Lifei Hou (侯立飞) Huabing Du (杜华冰) Xiaoshi Peng (彭晓世) Tao Xu (徐涛) Chaoguang Li (李朝光) Xiayu Zhan (詹夏宇) Guanghui Yuan (袁光辉) Haijun Zhang (张海军) Baibin Jiang (蒋柏斌) Lizhen Huang (黄丽珍) Kai Du (杜凯) Runchang Zhao (赵润昌) Ping Li (李平) Wei Wang (王伟) Jingqin Su (粟敬钦) Yongkun Ding (丁永坤) Xian-Tu He (贺贤土) Weiyan Zhang (张维岩) Institute of Applied Physics and Computational Mathematics Beijing 100088 China Research Center of Laser Fusion Chinese Academy of Engineering Physics Mianyang 621900 China Collaborative Innovation Center of IFSA Shanghai Jiao Tong University Shanghai 200240 China Center for Applied Physics and Technology Peking University Beijing 100871 China Chinese Academy of Engineering Physics Mianyang 621900 China

The first spherical hohlraum energetics experiment is accomplished on the SGIII-prototype laser facility. In the experiment, the radiation temperature is measured by using an array of flat-response x-ray detectors (FXRDs) through a laser entrance hole at four different angles. The radiation temperature and M-band fraction inside the hohlraum are determined by the shock wave technique. The experimental observations indicate that the radiation temperatures measured by the FXRDs depend on the observation angles and are related to the view field. According to the experimental results, the conversion efficiency of the vacuum spherical hohlraum is in the range from 60% to 80%. Although this conversion efficiency is less than the conversion efficiency of the near vacuum hohlraum on the National Ignition Facility, it is consistent with that of the cylindrical hohlraums used on the NOVA and the SGIII-prototype at the same energy scale.

关键词： Implosion symmetry Indirect drive Target design & fabrication Laser inertial confinement

The Atacama Cosmology Telescope: A measurement of the cosmic microwave background power spectra at 98 and 150 GHZ

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arXiv 2020年

作者： Choi, Steve K. Hasselfield, Matthew Ho, Shuay-Pwu Patty Koopman, Brian Lungu, Marius Abitbol, Maximilian H. Addison, Graeme E. Ade, Peter A.R. Aiola, Simone Alonso, David Amiri, Mandana Amodeo, Stefania Angile, Elio Austermann, Jason E. Baildon, Taylor Battaglia, Nick Beall, James A. Bean, Rachel Becker, Daniel T. Bond, J. Richard Bruno, Sarah Marie Calabrese, Erminia Calafut, Victoria Campusano, Luis E. Carrero, Felipe Chesmore, Grace E. Cho, Hsiao-Mei Clark, Susan E. Cothard, Nicholas F. Crichton, Devin Crowley, Kevin T. Darwish, Omar Datta, Rahul Denison, Edward V. Devlin, Mark J. Duell, Cody J. Duff, Shannon M. Duivenvoorden, Adriaan J. Dunkley, Jo Dünner, Rolando Essinger-Hileman, Thomas Fankhanel, Max Ferraro, Simone Fox, Anna E. Fuzia, Brittany Gallardo, Patricio A. Gluscevic, Vera Golec, Joseph E. Grace, Emily Gralla, Megan Guan, Yilun Hall, Kirsten Halpern, Mark Han, Dongwon Hargrave, Peter Henderson, Shawn Hensley, Brandon Hill, J. Colin Hilton, Gene C. Hilton, Matt Hincks, Adam D. Hložek, Renée Hubmayr, Johannes Huffenberger, Kevin M. Hughes, John P. Infante, Leopoldo Irwin, Kent Jackson, Rebecca Klein, Jeff Knowles, Kenda Kosowsky, Arthur Lakey, Victoria Li, Dale Li, Yaqiong Li, Zack Lokken, Martine Louis, Thibaut MacInnis, Amanda Madhavacheril, Mathew Maldonado, Felipe Mallaby-Kay, Maya Marsden, Danica Maurin, Loïc McMahon, Jeff Menanteau, Felipe Moodley, Kavilan Morton, Tim Naess, Sigurd Namikawa, Toshiya Nati, Federico Newburgh, Laura Nibarger, John P. Nicola, Andrina Niemack, Michael D. Nolta, Michael R. Orlowski-Sherer, John Page, Lyman A. Pappas, Christine G. Partridge, Bruce Phakathi, Phumlani Prince, Heather Puddu, Roberto Qu, Frank J. Rivera, Jesus Robertson, Naomi Rojas, Felipe Salatino, Maria Schaan, Emmanuel Schillaci, Alessandro Schmitt, Benjamin L. Sehgal, Neelima Sherwin, Blake D. Sierra, Carlos Sievers, Jon Sifon, Cristobal Sikhosana, Precious Simon, Sara Spergel, David N. Staggs, Suzanne T. Stevens, Jason Storer, Emilie Sunder, Dhaneshwar D. Switzer, Eric R. Thorne, Ben Thornton, Robe Department of Physics Cornell University IthacaNY14853 United States Department of Astronomy Cornell University IthacaNY14853 United States Joseph Henry Laboratories of Physics Jadwin Hall Princeton University PrincetonNJ08544 United States Center for Computational Astrophysics Flatiron Institute 162 5th Avenue New YorkNY10010 United States Department of Astronomy and Astrophysics The Pennsylvania State University University ParkPA16802 United States Institute for Gravitation and the Cosmos The Pennsylvania State University University ParkPA16802 United States Department of Physics Yale University 217 Prospect St New HavenCT06511 United States Department of Physics and Astronomy University of Pennsylvania 209 South 33rd Street PhiladelphiaPA19104 United States Department of Physics University of Oxford Keble Road OxfordOX1 3RH United Kingdom Dept. of Physics and Astronomy The Johns Hopkins University 3400 N. Charles St. BaltimoreMD21218-2686 United States School of Physics and Astronomy Cardiff University The Parade Wales CardiffCF24 3AA United Kingdom Department of Physics and Astronomy University of British Columbia VancouverBCV6T 1Z4 Canada NIST Quantum Devices Group 325 Broadway Mailcode 817.03 BoulderCO80305 United States Department of Physics University of Michigan Ann Arbor48103 United States Canadian Institute for Theoretical Astrophysics University of Toronto TorontoONM5S 3H8 Canada Universidad de Chile Dept Astronomía Casilla Santiago36-D Chile Sociedad Radiosky Asesorías de Ingeniería Limitada Camino a Toconao 145-A Ayllu de Solor San Pedro de Atacama Chile Department of Physics University of Chicago ChicagoIL60637 United States SLAC National Accelerator Laboratory 2575 Sand Hill Road Menlo ParkCA94025 United States Institute for Advanced Study 1 Einstein Dr PrincetonNJ08540 United States Department of Applied and Engineering Physics Cornell University IthacaNY14853 United States Astrophysics Res

We present the temperature and polarization angular power spectra of the CMB measured by the Atacama Cosmology Telescope (ACT) from 5400 deg2 of the 2013-2016 survey, which covers >15000 deg2 at 98 and 150 GHz. For this analysis we adopt a blinding strategy to help avoid confirmation bias and, related to this, show numerous checks for systematic error done before unblinding. Using the likelihood for the cosmological analysis we constrain secondary sources of anisotropy and foreground emission, and derive a "CMB-only" spectrum that extends to = 4000. At large angular scales, foreground emission at 150 GHz is ∼1% of TT and EE within our selected regions and consistent with that found by Planck. Using the same likelihood, we obtain the cosmological parameters for ΛCDM for the ACT data alone with a prior on the optical depth of τ = 0.065 ± 0.015. ΛCDM is a good fit. The best-fit model has a reduced χ2 of 1.07 (PTE = 0.07) with H0 = 67.9 ± 1.5 km/s/Mpc. We show that the lensing BB signal is consistent with ΛCDM and limit the celestial EB polarization angle to ψP = −0.07◦ ± 0.09◦. We directly cross correlate ACT with Planck and observe generally good agreement but with some discrepancies in TE. All data on which this analysis is based will be publicly released. Copyright © 2020, The Authors. All rights reserved.

关键词： Cosmology

The Atacama Cosmology Telescope: DR4 maps and cosmological parameters

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arXiv 2020年

作者： Aiola, Simone Calabrese, Erminia Maurin, Loïc Naess, Sigurd Schmitt, Benjamin L. Abitbol, Maximilian H. Addison, Graeme E. Ade, Peter A.R. Alonso, David Amiri, Mandana Amodeo, Stefania Angile, Elio Austermann, Jason E. Baildon, Taylor Battaglia, Nick Beall, James A. Bean, Rachel Becker, Daniel T. Bond, J. Richard Bruno, Sarah Marie Calafut, Victoria Campusano, Luis E. Carrero, Felipe Chesmore, Grace E. Cho, Hsiao-Mei Choi, Steve K. Clark, Susan E. Cothard, Nicholas F. Crichton, Devin Crowley, Kevin T. Darwish, Omar Datta, Rahul Denison, Edward V. Devlin, Mark J. Duell, Cody J. Duff, Shannon M. Duivenvoorden, Adriaan J. Dunkley, Jo Dünner, Rolando Essinger-Hileman, Thomas Fankhanel, Max Ferraro, Simone Fox, Anna E. Fuzia, Brittany Gallardo, Patricio A. Gluscevic, Vera Golec, Joseph E. Grace, Emily Gralla, Megan Guan, Yilun Hall, Kirsten Halpern, Mark Han, Dongwon Hargrave, Peter Hasselfield, Matthew Helton, Jakob M. Henderson, Shawn Hensley, Brandon Hill, J. Colin Hilton, Gene C. Hilton, Matt Hincks, Adam D. Hložek, Renée Ho, Shuay-Pwu Patty Hubmayr, Johannes Huffenberger, Kevin M. Hughes, John P. Infante, Leopoldo Irwin, Kent Jackson, Rebecca Klein, Jeff Knowles, Kenda Koopman, Brian Kosowsky, Arthur Lakey, Victoria Li, Dale Li, Yaqiong Li, Zack Lokken, Martine Louis, Thibaut Lungu, Marius MacInnis, Amanda Madhavacheril, Mathew Maldonado, Felipe Mallaby-Kay, Maya Marsden, Danica McMahon, Jeff Menanteau, Felipe Moodley, Kavilan Morton, Tim Namikawa, Toshiya Nati, Federico Newburgh, Laura Nibarger, John P. Nicola, Andrina Niemack, Michael D. Nolta, Michael R. Orlowski-Sherer, John Page, Lyman A. Pappas, Christine G. Partridge, Bruce Phakathi, Phumlani Pisano, Giampaolo Prince, Heather Puddu, Roberto Qu, Frank J. Rivera, Jesus Robertson, Naomi Rojas, Felipe Salatino, Maria Schaan, Emmanuel Schillaci, Alessandro Sehgal, Neelima Sherwin, Blake D. Sierra, Carlos Sievers, Jon Sifon, Cristobal Sikhosana, Precious Simon, Sara Spergel, David N. Staggs, Suzanne T. Stevens, Jason Storer, Emilie Sunder, Dhaneshwar D. Switzer, Center for Computational Astrophysics Flatiron Institute 162 5th Avenue New YorkNY10010 United States Joseph Henry Laboratories of Physics Jadwin Hall Princeton University PrincetonNJ08544 United States School of Physics and Astronomy Cardiff University The Parade Wales CardiffCF24 3AA United Kingdom Université Paris-Saclay CNRS Institut d'astrophysique spatiale Orsay 91405 France Instituto de Astrofísica Centro de Astro-Ingeniería Facultad de Fìsica Pontificia Universidad Católica de Chile Av. Vicuña Mackenna 4860 Macul Santiago7820436 Chile Department of Physics and Astronomy University of Pennsylvania 209 South 33rd Street PhiladelphiaPA19104 United States Department of Physics University of Oxford Keble Road OxfordOX1 3RH United Kingdom Dept. of Physics and Astronomy The Johns Hopkins University 3400 N. Charles St. BaltimoreMD21218-2686 United States Department of Physics and Astronomy University of British Columbia VancouverBCV6T 1Z4 Canada Department of Astronomy Cornell University IthacaNY14853 United States NIST Quantum Devices Group 325 Broadway Mailcode 817.03 BoulderCO80305 United States Department of Physics University of Michigan Ann Arbor48103 United States Canadian Institute for Theoretical Astrophysics University of Toronto TorontoONM5S 3H8 Canada Universidad de Chile Dept Astronomía Casilla Santiago36-D Chile Sociedad Radiosky Asesorías de Ingeniería Limitada Camino a Toconao 145-A Ayllu de Solor San Pedro de Atacama Chile Department of Physics University of Chicago ChicagoIL60637 United States SLAC National Accelerator Laboratory 2575 Sand Hill Road Menlo ParkCA94025 United States Department of Physics Cornell University IthacaNY14853 United States Institute for Advanced Study 1 Einstein Dr PrincetonNJ08540 United States Department of Applied and Engineering Physics Cornell University IthacaNY14853 United States Astrophysics Research Centre School of Mathematics Statistics and Computer Scie

We present new arcminute-resolution maps of the Cosmic Microwave Background temperature and polarization anisotropy from the Atacama Cosmology Telescope, using data taken from 2013-2016 at 98 and 150 GHz. The maps cover more than 17,000 deg2, the deepest 600 deg2 with noise levels below 10µK-arcmin. We use the power spectrum derived from almost 6,000 deg2 of these maps to constrain cosmology. The ACT data enable a measurement of the angular scale of features in both the divergence-like polarization and the temperature anisotropy, tracing both the velocity and density at last-scattering. From these one can derive the distance to the last-scattering surface and thus infer the local expansion rate, H0. By combining ACT data with large-scale information from WMAP we measure H0 = 67.6±1.1 km/s/Mpc, at 68% confidence, in excellent agreement with the independently-measured Planck satellite estimate (from ACT alone we find H0 = 67.9 ±1.5 km/s/Mpc). The ΛCDM model provides a good fit to the ACT data, and we find no evidence for deviations: both the spatial curvature, and the departure from the standard lensing signal in the spectrum, are zero to within 1σ;the number of relativistic species, the primordial Helium fraction, and the running of the spectral index are consistent with ΛCDM predictions to within 1.5-2.2σ. We compare ACT, WMAP, and Planck at the parameter level and find good consistency;we investigate how the constraints on the correlated spectral index and baryon density parameters readjust when adding CMB large-scale information that ACT does not measure. The DR4 products presented here will be publicly released on the NASA Legacy Archive for Microwave Background Data Analysis. Copyright © 2020, The Authors. All rights reserved.

关键词： Cosmology

Planck intermediate results. LV. reliability and thermal properties of high-frequency sources in the second planck catalogue of compact sources

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arXiv 2020年

作者： Akrami, Y. Ashdown, M. Aumont, J. Baccigalupi, C. Ballardini, M. Banday, A.J. Barreiro, R.B. Bartolo, N. Basak, S. Benabed, K. Bernard, J.-P. Bersanelli, M. Bielewicz, P. Bond, J.R. Borrill, J. Bouchet, F.R. Burigana, C. Calabrese, E. Carvalho, P. Chiang, H.C. Crill, B.P. Cuttaia, F. de Rosa, A. de Zotti, G. Delabrouille, J. Delouis, J.-M. Di Valentino, E. Diego, J.M. Dupac, X. Dusini, S. Efstathiou, G. Elsner, F. Enßlin, T.A. Eriksen, H.K. Fernandez-Cobos, R. Finelli, F. Fraisse, A.A. Franceschi, E. Frolov, A. Galeotta, S. Ganga, K. Gerbino, M. González-Nuevo, J. Górski, K.M. Gratton, S. Gruppuso, A. Gudmundsson, J.E. Handley, W. Hansen, F.K. Herranz, D. Hivon, E. Hobson, M. Huang, Z. Jones, W.C. Keihänen, E. Keskitalo, R. Kim, J. Kisner, T.S. Krachmalnicoff, N. Kunz, M. Kurki-Suonio, H. Lamarre, J.-M. Lasenby, A. Lattanzi, M. Lawrence, C.R. Le Jeune, M. Lilje, P.B. Lindholm, V. López-Caniego, M. Ma, Y.-Z. Macías-Pérez, J.F. Maggio, G. Mandolesi, N. Marcos-Caballero, A. Maris, M. Martin, P.G. Martínez-González, E. Matarrese, S. Mauri, N. McEwen, J.D. Migliaccio, M. Molinari, D. Moneti, A. Montier, L. Morgante, G. Natoli, P. Paoletti, D. Partridge, B. Perrotta, F. Pettorino, V. Piacentini, F. Polenta, G. Puget, J.-L. Rachen, J.P. Reinecke, M. Remazeilles, M. Renzi, A. Rocha, G. Roudier, G. Ruiz-Granados, B. Savelainen, M. Scott, D. Sirri, G. Spencer, L.D. Suur-Uski, A.-S. Tauber, J.A. Tavagnacco, D. Tenti, M. Toffolatti, L. Tomasi, M. Trombetti, T. Valiviita, J. van Tent, B. Vielva, P. Villa, F. Wehus, I.K. Zacchei, A. Zonca, A. AIM CEA CNRS Université Paris-Saclay Université Paris-Diderot Sorbonne Paris Cité Gif-sur-YvetteF-91191 France APC AstroParticule et Cosmologie Université Paris Diderot CNRS/IN2P3 CEA/lrfu Observatoire de Paris Sorbonne Paris Cité 10 rue Alice Domon et Léonie Duquet Paris Cedex 1375205 France African Institute for Mathematical Sciences 6-8 Melrose Road Muizenberg Cape Town South Africa Astrophysics Group Cavendish Laboratory University of Cambridge J J Thomson Avenue CambridgeCB3 0HE United Kingdom Astrophysics & Cosmology Research Unit School of Mathematics Statistics & Computer Science University of KwaZulu-Natal Westville Campus Private Bag X54001 Durban4000 South Africa CITA University of Toronto 60 St. George St. TorontoONM5S 3H8 Canada CMDLABS Cambridge Machines Deep Learning and Bayesian Systems Ltd 22 Wycombe End Beaconsfield BuckinghamshireHP9 1NB United Kingdom CNRS IRAP 9 Av. colonel Roche BP 44346 Toulouse cedex 4F-31028 France California Institute of Technology PasadenaCA United States Computational Cosmology Center Lawrence Berkeley National Laboratory BerkeleyCA United States Département de Physique Théorique Université de Genève 24 Quai E. Ansermet Genève 41211 Switzerland Département de Physique École normale supérieure PSL Research University CNRS 24 rue Lhomond Paris75005 France La Laguna TenerifeE-38206 Spain Departamento de Física Universidad de Oviedo C/ Federico García Lorca 18 Oviedo Spain Department of Astrophysics IMAPP Radboud University P.O. Box 9010 Nijmegen6500 GL Netherlands Department of Physics & Astronomy University of British Columbia 6224 Agricultural Road VancouverBC Canada Department of Physics & Astronomy University of the Western Cape Cape Town7535 South Africa Department of Physics Gustaf Hällströmin katu 2a University of Helsinki Helsinki Finland Department of Physics Princeton University PrincetonNJ United States Dipartimento di Fisica e Astronomia G. Galilei Univ

We describe an extension of the most recent version of the Planck Catalogue of Compact Sources (PCCS2), produced using a new multi-band Bayesian Extraction and Estimation Package (BeeP). BeeP assumes that the compact sources present in PCCS2 at 857 GHz have a dust-like spectral energy distribution (SED), which leads to emission at both lower and higher frequencies, and adjusts the parameters of the source and its SED to fit the emission observed in Planck’s three highest frequency channels at 353, 545, and 857 GHz, as well as the IRIS map at 3000 GHz. In order to reduce confusion regarding diffuse cirrus emission, BeeP’s data model includes a description of the background emission surrounding each source, and it adjusts the confidence in the source parameter extraction based on the statistical properties of the spatial distribution of the background emission. BeeP produces the following three new sets of parameters for each source: (a) fits to a modified blackbody (MBB) thermal emission model of the source;(b) SED-independent source flux densities at each frequency considered;and (c) fits to an MBB model of the background in which the source is embedded. BeeP also calculates, for each source, a reliability parameter, which takes into account confusion due to the surrounding cirrus. This parameter can be used to extract sub-samples of high-frequency sources with statistically well-understood properties. We define a high-reliability subset (BeeP/base), containing 26 083 sources (54.1 % of the total PCCS2 catalogue), the majority of which have no information on reliability in the PCCS2. We describe the characteristics of this specific high-quality subset of PCCS2 and its validation against other data sets, specifically for: the sub-sample of PCCS2 located in low-cirrus areas;the Planck Catalogue of Galactic Cold Clumps (GCC);the Herschel GAMA15-field catalogue;and the temperature- and spectral-index-reconstructed dust maps obtained with Planck’s Generalized Needlet Int

关键词： Extraction

The atacama cosmology telescope: Component-separated maps of CMB temperature and the thermal Sunyaev-Zel'dovich effect

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arXiv 2019年

作者： Madhavacheril, Mathew S. Hill, J. Colin Nss, Sigurd Addison, Graeme E. Aiola, Simone Baildon, Taylor Battaglia, Nicholas Bean, Rachel Bond, J. Richard Calabrese, Erminia Calafut, Victoria Choi, Steve K. Darwish, Omar Devlin, Mark J. Dunkley, Joanna Dunner, Rolando Ferraro, Simone Gallardo, Patricio A. Halpern, Mark Han, Dongwon Hasseleld, Matthew Hilton, Matt Hincks, Adam D. Hlozek, Renee Ho, Shuay-Pwu Patty Huffenberger, Kevin M. Hughes, John P. Koopman, Brian J. Kosowsky, Arthur Lokken, Martine Louis, Thibaut Lungu, Marius MacInnis, Amanda Maurin, Loic McMahon, Jeffrey J. Moodley, Kavilan Nati, Federico Niemack, Michael D. Page, Lyman A. Partridge, Bruce Robertson, Naomi Sehgal, Neelima Schaan, Emmanuel Schillaci, Alessandro Sherwin, Blake D. Sifon, Cristobal Simon, Sara M. Spergel, David N. Staggs, Suzanne T. Storer, Emilie R. van Engelen, Alexander Vavagiakis, Eve M. Wollack, Edward J. Xu, Zhilei Centre for the Universe Perimeter Institute for Theoretical Physics WaterlooONN2L2Y5 Canada Department of Astrophysical Sciences Princeton University 4 Ivy Lane PrincetonNJ08544 United States Department of Physics Columbia University 550 West 120th Street New YorkNY10027 United States Center for Computational Astrophysics Flatiron Institute 162 5th Avenue New YorkNY10010 United States School of Natural Sciences Institute for Advanced Study PrincetonNJ08540 United States Department of Physics and Astronomy Johns Hopkins University BaltimoreMD21218 United States Department of Physics University of Michigan Ann Arbor48103 United States Department of Astronomy Cornell University IthacaNY14853 United States Canadian Institute for Theoretical Astrophysics University of Toronto 60 St. George St. TorontoONM5S3H8 Canada School of Physics and Astronomy Cardiff University Parade CardiffCF243AA United Kingdom Department of Applied Mathematics and Theoretical Physics University of Cambridge Wilberforce Road CambridgeCB30WA United Kingdom Department of Physics and Astronomy University of Pennsylvania 209 South 33rd Street PhiladelphiaPA19104 United States Joseph Henry Laboratories of Physics Jadwin Hall Princeton University PrincetonNJ08544 United States Instituto de Astrofisica Centro de Astro-Ingenieria Facultad de Fisica Ponticia Universidad Catolica de Chile Av. Vicuna Mackenna 4860 Macul Santiago7820436 Physics Division Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Department of Physics Cornell University 109 Clark Hall IthacaNY14853 United States Department of Physics and Astronomy University of British Columbia VancouverBCV6T1Z1 Canada Physics and Astronomy Department Stony Brook University Stony BrookNY11794 United States Astrophysics & Cosmology Research Unit School of Mathematics Statistics & Computer Science University of KwaZulu-Natal Westville Campus Durban4041 South Africa Department of A

Optimal analyses of many signals in the cosmic microwave background (CMB) require maplevel extraction of individual components in the microwave sky, rather than measurements at the power spectrum level alone. To date, nearly all map-level component separation in CMB analyses has been performed exclusively using satellite data. In this paper, we implement a component separation method based on the internal linear combination (ILC) approach which we have designed to optimally account for the anisotropic noise (in the 2D Fourier domain) often found in groundbased CMB experiments. Using this method, we combine multi-frequency data from the Planck satellite and the Atacama Cosmology Telescope Polarimeter (ACTPol) to construct the first widearea, arcminute-resolution component-separated maps (covering ≈ 2100 sq. deg.) of the CMB temperature anisotropy and the thermal Sunyaev-Zel'dovich (tSZ) effect sourced by the inverse-Compton scattering of CMB photons off hot, ionized gas. Our ILC pipeline allows for explicit deprojection of various contaminating signals, including a modified blackbody approximation of the cosmic infrared background (CIB) spectral energy distribution. The cleaned CMB maps will be a useful resource for CMB lensing reconstruction, kinematic SZ cross-correlations, and primordial non-Gaussianity studies. The tSZ maps will be used to study the pressure profiles of galaxies, groups, and clusters through cross-correlations with halo catalogs, with dust contamination controlled via CIB deprojection. The data products described in this paper will be made available on LAMBDA. Copyright © 2019, The Authors. All rights reserved.

关键词： Cosmology