Author: "Zhe MA" / Topic: physics - Searchworks@Jio Institute Digital Library Search Results

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109 results on '"Zhe MA"'

1. Ab initio calculated dynamic structural factors and optical properties of beryllium along the Hugoniot

Author: Wei-Jie Li, Jie Zhou, Zi Li, Yunliang Zhu, Han-Dong Hu, Hao Ma, Zhe Ma, Cong Wang, and Ping Zhang
Subjects: Physics, QC1-999
Abstract: Beryllium is an ablator material used in inertial-confinement fusion and hypervelocity impact studies. The thermoelastic properties, structural factors, and optical properties of beryllium are important in these studies. In this paper, the static structural factors, ion–ion dynamic structural factors, adiabatic velocity, and optical properties of beryllium along the Hugoniot were calculated by ab initio simulations. The static structural factors show that beryllium atoms were randomly distributed. The dynamic structural factors extracted the dispersion relation for collective excitation via the scattering function. By collecting the peak position of the dynamic structural factors, the dispersion relation and adiabatic sound velocity were derived by definition. Using the calculated equation of state, the thermoelastic properties and adiabatic sound velocity have been derived. The two calculated methods for adiabatic sound velocity were verified to be equivalent.
Published: 2023
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2. An Image Edge Detection Algorithm Based on an Artificial Plant Community

Author: Zhengying Cai, Zhe Ma, Ziyi Zuo, Yafei Xiang, and Mingtao Wang
Subjects: image edge detection, image processing, artificial intelligence, plant community, Technology, Engineering (General). Civil engineering (General), TA1-2040, Biology (General), QH301-705.5, Physics, QC1-999, Chemistry, QD1-999
Abstract: Image edge detection is a difficult task, because it requires the accurate removal of irrelevant pixels, while retaining important pixels that describe the image’s structural properties. Here, an artificial plant community algorithm is proposed to aid in the solving of the image edge detection problem. First, the image edge detection problem is modeled as an objective function of an artificial plant community searching for water sources and nutrients. After many iterations, the artificial plant community is concentrated in habitable areas that are rich in water sources and nutrients, that is, the image edges, and the nonhabitable zones that are not suitable for living are deserted, that is, the nonedges. Second, an artificial plant community algorithm is designed to solve the objective function by simulating the growth process of a true plant community. The living behavior of the artificial plant community includes three operations: seeding, growing, and fruiting. The individuals in the plant community also correspond to three forms, namely seeds, individuals, and fruit. There are three fitness comparisons in each iteration. The first fitness comparison of each iteration is carried out during the seeding operation. Only the fruit with higher fitness levels in the last iteration can become seeds, while the fruit with low fitness levels die, and some new seeds are randomly generated. The second fitness comparison is implemented in the growing operation. Only the seeds with higher fitness levels can become individuals, but the seeds with lower fitness levels will die; thus, the community size will decrease. The third fitness comparison is in the fruiting operation, where the individual with the greatest fitness can produce an identical fruit through parthenogenesis, and the individuals with higher fitness levels can learn from each other and produce more fruit, so the population size can be restored. Through the continuous cycle of these three operations, the artificial plant community will finally determine the edge pixels and delete the nonedge pixels. Third, the experiment results reveal how the proposed algorithm generates the edge image, and the comparative results demonstrate that the proposed artificial plant community algorithm can effectively solve the image edge detection problems. Finally, this study and some limitations are summarized, and future directions are suggested. The proposed algorithm is expected to act as a new research tool for solving various complex problems.
Published: 2023
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3. Broadband Generalized Sidelobe Canceler Beamforming Applied to Ultrasonic Imaging

Author: Jiake Li, Zhe Ma, Lei Mao, Zhengjun Wang, Yi Wang, Huaiyu Cai, and Xiaodong Chen
Subjects: adaptive beamforming, wavelet, phased array, lateral resolution, Technology, Engineering (General). Civil engineering (General), TA1-2040, Biology (General), QH301-705.5, Physics, QC1-999, Chemistry, QD1-999
Abstract: A broadband generalized sidelobe canceler (Broadband-GSC) application for near-field beamforming is proposed. This approach is implemented in the wavelet domain. Broadband-GSC provides a set of complex, adapted apodization weights for each wavelet subband. The proposed method constrains interference and noise signal to improve the lateral resolution with only one single emission. Performance of the proposed beamforming is tested on simulated data obtained with Field II. Experiments have proved that the new beamforming can significantly increase the image quality compared with delay-and-sum (DAS) and synthetic aperture (SA). Imaging of scattering points show that Broadband-GSC improves the lateral resolution by 43.2% and 58.0% compared with SA and DAS, respectively. Meanwhile，Broadband-GSC reduces the peak sidelobe level by 11.6 dB and 26.4 dB compared with SA and DAS, respectively. Plane wave emission experiment indicates that Broadband-GSC can improve the lateral resolution by 44.2% compared with DAS. Furthermore, the new beamforming introduces the possibility for higher frame-rate and higher investigation depth with increased lateral resolution.
Published: 2020
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4. Effects of model incompleteness on the drift-scan calibration of radio telescopes

Author: Phil Bull, David DeBoer, Adam P. Beardsley, Nipanjana Patra, Ziyaad Halday, Nima Razavi-Ghods, Nicholas S. Kern, Aaron R. Parsons, Piyanat Kittiwisit, Kingsley Gale-Sides, Robert Pascua, Max Tegmark, Judd D. Bowman, Adam Lanman, Samantha Pieterse, James Robnett, Peter Sims, Gianni Bernardi, Peter K. G. Williams, Miguel F. Morales, Chris Carilli, Saul A. Kohn, Zara Abdurashidova, Eloy de Lera Acedo, Zaki S. Ali, Steven R. Furlanetto, Abraham R. Neben, Eunice Matsetela, Randall Fritz, Bojan Nikolic, Aaron Ewall-Wice, Bryna J. Hazelton, Deepthi Gorthi, Richard F. Bradley, Matthew Kolopanis, Jon Ringuette, Brian Glendenning, Matt Dexter, Joshua S. Dillon, Carina Cheng, Paul La Plante, Austin Julius, S. H. Carey, Nithyanandan Thyagarajan, Haoxuan Zheng, David B. Lewis, Mario G. Santos, Daniel C. Jacobs, Joshua Kerrigan, Steven G. Murray, Cresshim Malgas, Jack Hickish, Adrian Liu, James E. Aguirre, Nicolas Fagnoni, Jacob Burba, Yanga Balfour, Lourence Malan, Craig Smith, Raul A. Monsalve, Bradley Greig, Jonathan C. Pober, Andrei Mesinger, Jasper Grobbelaar, Tashalee S. Billings, Zachary E. Martinot, Telalo Lekalake, Matthys Maree, B. K. Gehlot, David MacMahon, Yin-Zhe Ma, Mathakane Molewa, Paul Alexander, Kathryn Rosie, Tshegofalang Mosiane, Nivedita Mahesh, John Ely, Jacqueline N. Hewitt, Angelo Syce, Gehlot, B. K., Jacobs, D. C., Bowman, J. D., Mahesh, N., Murray, S. G., Kolopanis, M., Beardsley, A. P., Abdurashidova, Z., Aguirre, J. E., Alexander, P., Ali, Z. S., Balfour, Y., Bernardi, G., Billings, T. S., Bradley, R. F., Bull, P., Burba, J., Carey, S., Carilli, C. L., Cheng, C., Deboer, D. R., Dexter, M., De Lera Acedo, E., Dillon, J. S., Ely, J., Ewall-Wice, A., Fagnoni, N., Fritz, R., Furlanetto, S. R., Gale-Sides, K., Glendenning, B., Gorthi, D., Greig, B., Grobbelaar, J., Halday, Z., Hazelton, B. J., Hewitt, J. N., Hickish, J., Julius, A., Kern, N. S., Kerrigan, J., Kittiwisit, P., Kohn, S. A., Lanman, A., La Plante, P., Lekalake, T., Lewis, D., Liu, A., Ma, Y. -Z., Macmahon, D., Malan, L., Malgas, C., Maree, M., Martinot, Z. E., Matsetela, E., Mesinger, A., Molewa, M., Monsalve, R. A., Morales, M. F., Mosiane, T., Neben, A. R., Nikolic, B., Parsons, A. R., Pascua, R., Patra, N., Pieterse, S., Pober, J. C., Razavi-Ghods, N., Ringuette, J., Robnett, J., Rosie, K., Santos, M. G., Sims, P., Smith, C., Syce, A., Tegmark, M., Thyagarajan, N., Williams, P. K. G., Zheng, H., ITA, and USA
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, media_common.quotation_subject, statistical [methods], FOS: Physical sciences, 01 natural sciences, Radio telescope, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Calibration, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Reionization, 0105 earth and related environmental sciences, Remote sensing, media_common, Physics, COSMIC cancer database, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, interferometric [techniques], interferometer [instrumentation], Interferometry, Amplitude, 13. Climate action, Space and Planetary Science, Sky, data analysi [methods], dark ages, reionization, first star, Antenna (radio), Astrophysics - Instrumentation and Methods for Astrophysics, miscellaneou [instrumentation], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Precision calibration poses challenges to experiments probing the redshifted 21-cm signal of neutral hydrogen from the Cosmic Dawn and Epoch of Reionization (z~30-6). In both interferometric and global signal experiments, systematic calibration is the leading source of error. Though many aspects of calibration have been studied, the overlap between the two types of instruments has received less attention. We investigate the sky based calibration of total power measurements with a HERA dish and an EDGES style antenna to understand the role of auto-correlations in the calibration of an interferometer and the role of sky in calibrating a total power instrument. Using simulations we study various scenarios such as time variable gain, incomplete sky calibration model, and primary beam model. We find that temporal gain drifts, sky model incompleteness, and beam inaccuracies cause biases in the receiver gain amplitude and the receiver temperature estimates. In some cases, these biases mix spectral structure between beam and sky resulting in spectrally variable gain errors. Applying the calibration method to the HERA and EDGES data, we find good agreement with calibration via the more standard methods. Although instrumental gains are consistent with beam and sky errors similar in scale to those simulated, the receiver temperatures show significant deviations from expected values. While we show that it is possible to partially mitigate biases due to model inaccuracies by incorporating a time-dependent gain model in calibration, the resulting errors on calibration products are larger and more correlated. Completely addressing these biases will require more accurate sky and primary beam models., Comment: 16 pages, 13 figures, 1 table; accepted for publication in MNRAS main journal
Published: 2021

5. Recovering the 21-cm signal from simulated FAST intensity maps

Author: Elimboto Yohana, Di Li, Wei-Ming Dai, Yin-Zhe Ma, and Xuelei Chen
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Aperture, media_common.quotation_subject, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Standard deviation, Radio telescope, 0103 physical sciences, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Physics, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Intensity mapping, Astronomy and Astrophysics, Atmospheric noise, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), Principal component analysis, Astrophysics - Instrumentation and Methods for Astrophysics, Intensity (heat transfer), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The 21-cm intensity mapping (IM) of neutral hydrogen (HI) is a promising tool to probe the large-scale structures. Sky maps of 21-cm intensities can be highly contaminated by different foregrounds, such as Galactic synchrotron radiation, free-free emission, extragalactic point sources, and atmospheric noise. We here present a model of foreground components and a method of removal, especially to quantify the potential of Five-hundred-meter Aperture Spherical radio Telescope (FAST) for measuring HI IM. We consider 1-year observational time with the survey area of $20,000\,{\rm deg}^{2}$ to capture significant variations of the foregrounds across both the sky position and angular scales relative to the HI signal. We first simulate the observational sky and then employ the Principal Component Analysis (PCA) foreground separation technique. We show that by including different foregrounds, thermal and $1/f$ noises, the value of the standard deviation between reconstructed 21-cm IM map and the input pure 21-cm signal is $\Delta T = 0.034\,{\rm mK}$, which is well under control. The eigenmode-based analysis shows that the underlying HI eigenmode is just less than $1$ per cent level of the total sky components. By subtracting the PCA cleaned foreground+noise map from the total map, we show that PCA method can recover HI power spectra for FAST with high accuracy., Comment: 14 pages, 11 figures, MNRAS in press
Published: 2021

6. Planck 2018 results

Author: Antony Lewis, X. Dupac, James R. Fergusson, François R. Bouchet, Diego Molinari, E. Martínez-González, Jean-François Cardoso, L. Salvati, Jörg P. Rachen, Krzysztof M. Gorski, K. Ganga, A. Marcos-Caballero, C. Combet, Hannu Kurki-Suonio, E. Di Valentino, Jose M. Diego, L. Montier, Jan Hamann, J. F. Macías-Pérez, E. Franceschi, Charles R. Lawrence, M. Douspis, Erminia Calabrese, E. P. S. Shellard, Frederico Arroja, M. Le Jeune, P. Vielva, Andrea Zacchei, Graca Rocha, Martina Gerbino, Zhiqi Huang, Davide Maino, Adam Moss, Ricardo Genova-Santos, D. Tavagnacco, M. López-Caniego, A. A. Fraisse, M. Tenti, F. Piacentini, J.-P. Bernard, P. de Bernardis, Tiziana Trombetti, L. Toffolatti, Soumen Basak, F. Elsner, J.-L. Puget, Benjamin D. Wandelt, Julian Borrill, R. B. Barreiro, Gabriel Jung, Michele Liguori, S. Galeotta, Will Handley, F. Cuttaia, G. Polenta, R. C. Butler, K. Kiiveri, Anthony Lasenby, Alessandro Melchiorri, Reijo Keskitalo, A. J. Banday, M.-A. Miville-Deschênes, A. Renzi, P. Bielewicz, F. Oppizzi, Yashar Akrami, Anthony Challinor, B. Casaponsa, E. Keihänen, Gianmarco Maggio, B. P. Crill, Nicola Bartolo, B. Van Tent, Fabrizio Villa, Francesca Perrotta, F. K. Hansen, J. B. Kim, G. Sirri, Andrei V. Frolov, Michele Maris, J. A. Tauber, M. Savelainen, D. Herranz, A.-S. Suur-Uski, Yabebal Fantaye, Sabino Matarrese, M. Migliaccio, M. Tomasi, M. Bucher, Nicola Vittorio, J. Valiviita, V. Lindholm, W. C. Jones, Douglas Scott, R. Fernandez-Cobos, D. Paoletti, Marco Bersanelli, Torsten A. Enßlin, A. Moneti, M. Frailis, Carlo Baccigalupi, V. Pettorino, François Levrier, E. Hivon, J. Aumont, B. Racine, A. Mennella, G. Patanchon, Alessandro Gruppuso, Ingunn Kathrine Wehus, M. Reinecke, J.-M. Delouis, P. D. Meerburg, Massimiliano Lattanzi, Jose Alberto Rubino-Martin, N. Mandolesi, Chiara Sirignano, Kendrick M. Smith, Andrew H. Jaffe, Peter Meinhold, J.-M. Lamarre, A. de Rosa, G. de Zotti, B. Partridge, J. González-Nuevo, A. Ducout, Locke D. Spencer, M. Ashdown, H. K. Eriksen, Martin Kunz, Mathieu Remazeilles, Jon E. Gudmundsson, L. P. L. Colombo, Jason D. McEwen, Mario Ballardini, Peter G. Martin, George Efstathiou, Serge Gratton, Carlo Burigana, Nicoletta Krachmalnicoff, Yin-Zhe Ma, Jacques Delabrouille, Fabio Finelli, L. Pagano, N. Mauri, S. Dusini, Andrea Zonca, R. A. Sunyaev, P. B. Lilje, Luca Stanco, H. C. Chiang, K. Benabed, J. R. Bond, B. Ruiz-Granados, O. Doré, Paolo Natoli, Maresuke Shiraishi, Moritz Münchmeyer, S. Galli, Gianluca Morgante, Astrophysique, Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), 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), 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), University of Parma = Università degli studi di Parma [Parme, Italie], Canadian Institute for Theoretical Astrophysics (CITA), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Patrimoine, Littérature, Histoire (PLH), Université Toulouse - Jean Jaurès (UT2J), AstroParticule et Cosmologie (APC (UMR_7164)), 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)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Universidade Aberta [Lisboa], Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Dipartimento di Fisica [Roma La Sapienza], Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Laboratory for Phytosanitary Diagnostics and Forecasts, All-Russian Institute for Plant Protection, Russian Academy of Sciences [Moscow] (RAS), Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées, Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] (AOSS), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), ICRA and Physics Department, Dipartimento di Fisica 'G. Galilei', Universita degli Studi di Padova, University of Cambridge [UK] (CAM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), 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), 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), Commissariat à l'énergie atomique et aux énergies alternatives - Laboratoire d'Electronique et de Technologie de l'Information (CEA-LETI), Direction de Recherche Technologique (CEA) (DRT (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), University of Manchester [Manchester], University of British Columbia (UBC), Laboratoire de neurobiologie cellulaire et moléculaire (NBCM), Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Planck Collaboration, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université (SU)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2020-....] (UGA [2020-....])-Institut polytechnique de Grenoble - Grenoble Institute of Technology [2020-....] (Grenoble INP [2020-....]), Université Grenoble Alpes [2020-....] (UGA [2020-....]), Sorbonne Université (SU)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Planck, Department of Physics, Helsinki Institute of Physics, Universidad de Cantabria, Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-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), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de physique de l'ENS - ENS Paris (LPENS), Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), High-Energy Frontier, Van Swinderen Institute for Particle Physics and G, Ministerio de Economía y Competitividad (España), Consejo Superior de Investigaciones Científicas (España), European Commission, European Research Council, European Space Agency, Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, 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), Università degli studi di Parma = University of Parma (UNIPR), Université de Toulouse (UT)-Université de Toulouse (UT), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Padova = University of Padua (Unipd), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Y. Akrami, F. Arroja, M. Ashdown, J. Aumont, C. Baccigalupi, M. Ballardini, A. J. Banday, R. B. Barreiro, N. Bartolo, S. Basak, K. Benabed, J. -P. Bernard, M. Bersanelli, P. Bielewicz, J. R. Bond, J. Borrill, F. R. Bouchet, M. Bucher, C. Burigana, R. C. Butler, E. Calabrese, J. -F. Cardoso, B. Casaponsa, A. Challinor, H. C. Chiang, L. P. L. Colombo, C. Combet, B. P. Crill, F. Cuttaia, P. de Bernardi, A. de Rosa, G. de Zotti, J. Delabrouille, J. -M. Deloui, E. Di Valentino, J. M. Diego, O. Doré, M. Douspi, A. Ducout, X. Dupac, S. Dusini, G. Efstathiou, F. Elsner, T. A. Enßlin, H. K. Eriksen, Y. Fantaye, J. Fergusson, R. Fernandez-Cobo, F. Finelli, M. Fraili, A. A. Fraisse, E. Franceschi, A. Frolov, S. Galeotta, K. Ganga, R. T. Génova-Santo, M. Gerbino, J. González-Nuevo, K. M. Górski, S. Gratton, A. Gruppuso, J. E. Gudmundsson, J. Hamann, W. Handley, F. K. Hansen, D. Herranz, E. Hivon, Z. Huang, A. H. Jaffe, W. C. Jone, G. Jung, E. Keihänen, R. Keskitalo, K. Kiiveri, J. Kim, N. Krachmalnicoff, M. Kunz, H. Kurki-Suonio, J. -M. Lamarre, A. Lasenby, M. Lattanzi, C. R. Lawrence, M. Le Jeune, F. Levrier, A. Lewi, M. Liguori, P. B. Lilje, V. Lindholm, M. López-Caniego, Y. -Z. Ma, J. F. Macías-Pérez, G. Maggio, D. Maino, N. Mandolesi, A. Marcos-Caballero, M. Mari, P. G. Martin, E. Martínez-González, S. Matarrese, N. Mauri, J. D. McEwen, P. D. Meerburg, P. R. Meinhold, A. Melchiorri, A. Mennella, M. Migliaccio, M. -A. Miville-Deschêne, D. Molinari, A. Moneti, L. Montier, G. Morgante, A. Mo, M. Münchmeyer, P. Natoli, F. Oppizzi, L. Pagano, D. Paoletti, B. Partridge, G. Patanchon, F. Perrotta, V. Pettorino, F. Piacentini, G. Polenta, J. -L. Puget, J. P. Rachen, B. Racine, M. Reinecke, M. Remazeille, A. Renzi, G. Rocha, J. A. Rubiño-Martín, B. Ruiz-Granado, L. Salvati, M. Savelainen, D. Scott, E. P. S. Shellard, M. Shiraishi, C. Sirignano, G. Sirri, K. Smith, L. D. Spencer, L. Stanco, R. Sunyaev, A. -S. Suur-Uski, J. A. Tauber, D. Tavagnacco, M. Tenti, L. Toffolatti, M. Tomasi, T. Trombetti, J. Valiviita, B. Van Tent, P. Vielva, F. Villa, N. Vittorio, B. D. Wandelt, I. K. Wehu, A. Zacchei, A. Zonca, 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, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)
Subjects: High Energy Physics - Theory, cosmological model, Astronomy, Cosmic microwave background, POLARIZATION ANISOTROPIES, cosmic background radiation: polarization, Astrophysics, cosmic background radiation, Cosmic background radiation, Early Universe, 01 natural sciences, 7. Clean energy, expansion: multipole, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology (hep-ph), cosmology: theory, 3-POINT CORRELATION-FUNCTION, observations [Cosmology], data analysis [Methods], 010303 astronomy & astrophysics, TEMPERATURE, Physics, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], hep-th, formation, hep-ph, early Universe, CMB cold spot, inflation: model, High Energy Physics - Phenomenology, scale dependence, non-Gaussianity, symbols, Sunyaev-Zel'dovich effect, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], astro-ph.CO, Trispectrum, Astrophysics - Cosmology and Nongalactic Astrophysics, Particle physics, data analysis method, Cosmology and Nongalactic Astrophysics (astro-ph.CO), satellite: Planck, gr-qc, FOS: Physical sciences, PREDICTIONS, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Sunyaev–Zel'dovich effect, Separable space, NO, isocurvature, symbols.namesake, trispectrum, Settore FIS/05 - Astronomia e Astrofisica, parity: violation, gravitation: lens, statistical analysis, theory [Cosmology], Non-Gaussianity, 0103 physical sciences, BISPECTRUM, INFRARED BACKGROUND ANISOTROPIES, structure, bispectrum: scale dependence, Planck, cosmic background radiation: bispectrum, inflation, FAST ESTIMATOR, numerical calculations, non-Gaussianity: primordial, 010308 nuclear & particles physics, ISOCURVATURE PERTURBATIONS, Astronomy and Astrophysics, stability, 115 Astronomy, Space science, Inflation, methods: data analysis, boundary condition, cosmic background radiation: temperature, Cosmology: observations, Cosmology: theory, Methods: data analysis, High Energy Physics - Theory (hep-th), 13. Climate action, Space and Planetary Science, axion, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], cosmology: observations, Cosmic background radiation, Cosmology: observations, Cosmology: theory, Early Universe, Inflation, Methods: data analysis, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Bispectrum
Abstract: Planck Collaboration: et al., arXiv:1905.05697v1, We analyse the Planck full-mission cosmic microwave background (CMB) temperature and E-mode polarization maps to obtain constraints on primordial non-Gaussianity (NG). We compare estimates obtained from separable template-fitting, binned, and optimal modal bispectrum estimators, finding consistent values for the local, equilateral, and orthogonal bispectrum amplitudes. Our combined temperature and polarization analysis produces the following final results: fNLlocal = −0.9 ± 5.1; fNLequil = −26 ± 47; and fNLortho = −38 ± 24 (68% CL, statistical). These results include low-multipole (4 ≤ ℓ < 40) polarization data that are not included in our previous analysis. The results also pass an extensive battery of tests (with additional tests regarding foreground residuals compared to 2015), and they are stable with respect to our 2015 measurements (with small fluctuations, at the level of a fraction of a standard deviation, which is consistent with changes in data processing). Polarization-only bispectra display a significant improvement in robustness; they can now be used independently to set primordial NG constraints with a sensitivity comparable to WMAP temperature-based results and they give excellent agreement. In addition to the analysis of the standard local, equilateral, and orthogonal bispectrum shapes, we consider a large number of additional cases, such as scale-dependent feature and resonance bispectra, isocurvature primordial NG, and parity-breaking models, where we also place tight constraints but do not detect any signal. The non-primordial lensing bispectrum is, however, detected with an improved significance compared to 2015, excluding the null hypothesis at 3.5σ. Beyond estimates of individual shape amplitudes, we also present model-independent reconstructions and analyses of the Planck CMB bispectrum. Our final constraint on the local primordial trispectrum shape is gNLlocal = (−5.8 ± 6.5) × 104 (68% CL, statistical), while constraints for other trispectrum shapes are also determined. Exploiting the tight limits on various bispectrum and trispectrum shapes, we constrain the parameter space of different early-Universe scenarios that generate primordial NG, including general single-field models of inflation, multi-field models (e.g. curvaton models), models of inflation with axion fields producing parity-violation bispectra in the tensor sector, and inflationary models involving vector-like fields with directionally-dependent bispectra. Our results provide a high-precision test for structure-formation scenarios, showing complete agreement with the basic picture of the ΛCDM cosmology regarding the statistics of the initial conditions, with cosmic structures arising from adiabatic, passive, Gaussian, and primordial seed perturbations., The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and ERC and PRACE (EU).
Published: 2020

7. Coherent OTDR Using Flexible All-Digital Orthogonal Phase Code Pulse for Distributed Sensing

Author: Zhenyang Ding, Tiegen Liu, Shuang Wang, Kun Liu, Junfeng Jiang, Wenjie Chen, Tianhua Xu, and Zhe Ma
Subjects: Physics, coherent OTDR, General Computer Science, Acoustics, Optical fiber sensors, General Engineering, interference, Phase Code, Optical time-domain reflectometer, Distributed acoustic sensing, Interference (wave propagation), Signal, Amplitude, optical pulses, distributed sensing, Modulation, Waveform, General Materials Science, lcsh:Electrical engineering. Electronics. Nuclear engineering, phase detection, lcsh:TK1-9971
Abstract: A coherent optical time-domain reflectometer (COTDR) using flexible all-digital orthogonal phase code pulse is proposed for distributed acoustic sensing. All-digital orthogonal phase code pulse with frequency shift and time shift is used as probe. Coherent detection and balance photodetector are used to amplify interference signal and get rid of its direct-current (DC) component. The new scheme needs only single channel detection while keeping sampling frequency. Amplitude triangle modulation and frequency linear sweep modulation waveform are used for system performance investigation. The experiments on 15.4 km optical fiber showed that waveform information can be recovered well. The all-digital orthogonal phase code pulse will provide a flexible solution for different application requirement.
Published: 2020

8. Planck 2018 results: XII. Galactic astrophysics using polarized dust emission

Author: E. Di Valentino, A. Marcos-Caballero, M. Frailis, Carlo Baccigalupi, François Levrier, N. Mauri, Jason D. McEwen, X. Dupac, Carlo Burigana, Nicoletta Krachmalnicoff, K. Benabed, J. R. Bond, Vincent Guillet, Jose Alberto Rubino-Martin, L. Polastri, Alessandro Melchiorri, Andrea Bracco, G. de Zotti, J. González-Nuevo, P. B. Lilje, E. Martínez-González, P. de Bernardis, Yashar Akrami, S. Galli, J. Aumont, Marian Douspis, M. Maris, Martina Gerbino, L. Toffolatti, Rashid Sunyaev, E. Franceschi, Guillaume Patanchon, A. Mangilli, Edith Falgarone, J.-M. Delouis, Anthony Lasenby, Jörg P. Rachen, M. Migliaccio, M. Bucher, Douglas Scott, M. Ashdown, H. K. Eriksen, K. Ganga, Jose M. Diego, J. A. Tauber, M. Savelainen, E. Keihänen, Gianluca Morgante, B. P. Crill, F. Cuttaia, Charles R. Lawrence, C. Combet, N. Mandolesi, Fabrizio Villa, Nabila Aghanim, D. Herranz, M. Tenti, F. Vansyngel, S. Galeotta, James J. Bock, B. Van Tent, L. P. L. Colombo, Andrew H. Jaffe, Clive Dickinson, B. Ruiz-Granados, A.-S. Suur-Uski, M. Le Jeune, Philip Lubin, J. Kim, J. F. Macías-Pérez, Mario Ballardini, F. Boulanger, Davide Maino, A. A. Fraisse, W. C. Jones, Ranga-Ram Chary, Andrea Zacchei, Tiziana Trombetti, Tuhin Ghosh, M.-A. Miville-Deschênes, Graca Rocha, George Efstathiou, Sabino Matarrese, J. Valiviita, Nicola Vittorio, V. Lindholm, Valeria Pettorino, A. J. Banday, Katia Ferrière, A. Moneti, Franz Elsner, Jacques Delabrouille, Yabebal Fantaye, R. B. Barreiro, A. Mennella, N. Bartolo, L. Montier, Michele Liguori, P. Vielva, F. K. Hansen, Fabio Finelli, G. Roudier, F. Piacentini, M. Tomasi, K. Kiiveri, Erminia Calabrese, Guilaine Lagache, C. Rosset, M. I. R. Alves, M. Sandri, Jean-François Cardoso, Peter G. Martin, Marco Bersanelli, M. López-Caniego, Zhiqi Huang, Andrei V. Frolov, François R. Bouchet, Julien Carron, George Helou, L. Salvati, J.-P. Bernard, Adam Moss, Gregory M. Green, J.-L. Puget, Benjamin D. Wandelt, Julian Borrill, Will Handley, S. Basak, Ricardo Genova-Santos, Ingunn Kathrine Wehus, O. Doré, Paolo Natoli, D. Tavagnacco, Massimiliano Lattanzi, G. Polenta, A. Renzi, Diego Molinari, G. Maggio, R. Fernandez-Cobos, Reijo Keskitalo, P. Bielewicz, M. Reinecke, Martin Kunz, Mathieu Remazeilles, Jon E. Gudmundsson, C. Sirignano, Francesco Forastieri, L. Pagano, Andrea Zonca, H. C. Chiang, Francesca Perrotta, Torsten A. Enßlin, Serge Gratton, Yin-Zhe Ma, Eric Hivon, D. Paoletti, Alessandro Gruppuso, J.-M. Lamarre, A. Ducout, Hannu Kurki-Suonio, I. Ristorcelli, Krzysztof M. Gorski, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - 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), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), 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)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2020-....] (UGA [2020-....])-Institut polytechnique de Grenoble - Grenoble Institute of Technology [2020-....] (Grenoble INP [2020-....]), Université Grenoble Alpes [2020-....] (UGA [2020-....]), Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), 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), 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), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Planck, Astrophysique, Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), 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), University of Parma = Università degli studi di Parma [Parme, Italie], Computing and Mathematical Sciences [Pasadena]], California Institute of Technology (CALTECH), Canadian Institute for Theoretical Astrophysics (CITA), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Patrimoine, Littérature, Histoire (PLH), Université Toulouse - Jean Jaurès (UT2J), Laboratoire de Recherche en Informatique (LRI), CentraleSupélec-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), CentraleSupélec, Universidade Aberta [Lisboa], Centre National d'Études Spatiales [Toulouse] (CNES), Infrared Processing and Analysis Center (IPAC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Dipartimento di Fisica [Roma La Sapienza], Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), 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)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Laboratory for Phytosanitary Diagnostics and Forecasts, All-Russian Institute for Plant Protection, Russian Academy of Sciences [Moscow] (RAS), Institut National Polytechnique (Toulouse) (Toulouse INP), Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] (AOSS), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, ICRA and Physics Department, Dipartimento di Fisica 'G. Galilei', Universita degli Studi di Padova, Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), University of Manchester [Manchester], Venetian Institute Molecular Medicine (VIMM), University of British Columbia (UBC), Laboratoire de neurobiologie cellulaire et moléculaire (NBCM), Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Planck Collaboration, Aghanim N., Akrami Y., Alves M.I.R., 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., Bock J.J., Bond J.R., Borrill J., Bouchet F.R., Boulanger F., Bracco A., Bucher M., Burigana C., Calabrese E., Cardoso J.-F., Carron J., Chary R.-R., Chiang H.C., Colombo L.P.L., Combet C., Crill B.P., Cuttaia F., De Bernardis P., De Zotti G., Delabrouille J., Delouis J.-M., Di Valentino E., Dickinson C., Diego J.M., Dore O., Douspis M., Ducout A., Dupac X., Efstathiou G., Elsner F., Ensslin T.A., Eriksen H.K., Falgarone E., Fantaye Y., Fernandez-Cobos R., Ferriere K., Finelli F., Forastieri F., Frailis M., Fraisse A.A., Franceschi E., Frolov A., Galeotta S., Galli S., Ganga K., Genova-Santos R.T., Gerbino M., Ghosh T., Gonzalez-Nuevo J., Gorski K.M., Gratton S., Green G., Gruppuso A., Gudmundsson J.E., Guillet V., Handley W., Hansen F.K., Helou G., Herranz D., Hivon E., Huang Z., Jaffe A.H., Jones W.C., Keihanen E., Keskitalo R., Kiiveri K., Kim J., Krachmalnicoff N., Kunz M., Kurki-Suonio H., Lagache G., Lamarre J.-M., Lasenby A., Lattanzi M., Lawrence C.R., Le Jeune M., Levrier F., Liguori M., Lilje P.B., Lindholm V., Lopez-Caniego M., Lubin P.M., Ma Y.-Z., Macias-Perez J.F., Maggio G., Maino D., Mandolesi N., Mangilli A., Marcos-Caballero A., Maris M., Martin P.G., Martinez-Gonzalez E., Matarrese S., Mauri N., McEwen J.D., Melchiorri A., Mennella A., Migliaccio M., Miville-Deschenes M.-A., Molinari D., Moneti A., Montier L., Morgante G., Moss A., Natoli P., Pagano L., Paoletti D., Patanchon G., Perrotta F., Pettorino V., Piacentini F., Polastri L., Polenta G., Puget J.-L., Rachen J.P., Reinecke M., Remazeilles M., Renzi A., Ristorcelli I., Rocha G., Rosset C., Roudier G., Rubino-Martin J.A., Ruiz-Granados B., Salvati L., Sandri M., Savelainen M., Scott D., Sirignano C., Sunyaev R., Suur-Uski A.-S., Tauber J.A., Tavagnacco D., Tenti M., Toffolatti L., Tomasi M., Trombetti T., Valiviita J., Vansyngel F., Van Tent B., Vielva P., Villa F., Vittorio N., Wandelt B.D., Wehus I.K., Zacchei A., Zonca A., Ministerio de Economía y Competitividad (España), Consejo Superior de Investigaciones Científicas (España), European Commission, European Research Council, European Space Agency, Agence Nationale de la Recherche (France), Universidad de Cantabria, Department of Physics, Helsinki Institute of Physics, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire de physique de l'ENS - ENS Paris (LPENS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, 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), Università degli studi di Parma = University of Parma (UNIPR), Université de Toulouse (UT)-Université de Toulouse (UT), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT), Università degli Studi di Padova = University of Padua (Unipd), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), ANR-17-CE31-0022,BxB,Champs B interstellaires et modes B de l'inflation(2017), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), 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), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and 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)
Subjects: STARLIGHT, Astronomy, Inverse, Astrophysics, magnetic fields, 7. Clean energy, 01 natural sciences, Polarization, DISTANT STARS, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, media_common, Physics, Turbulence, extinction, ISM [Submillimeter], Astrophysics::Instrumentation and Methods for Astrophysics, MAGNETIC-FIELD, CLOUDS, Galaxy: ISM, LATITUDES, Polarization (waves), STATISTICS, Magnetic field, ISM: dust, symbols, INTERSTELLAR POLARIZATION, submillimeter: ISM, dust, local insterstellar matter, COMPONENT SEPARATION, GRAIN ALIGNMENT, Local insterstellar matter, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, polarization, turbulence, Astrophysics::Cosmology and Extragalactic Astrophysics, NO, symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, DISPERSION, Dust, Extinction, Local insterstellar matter, Magnetic fields, Polarization, Submillimeter: ISM, Turbulence, 0103 physical sciences, Computer Science::Symbolic Computation, Planck, Dust, extinction, Astrophysics::Galaxy Astrophysics, 010308 nuclear & particles physics, Molecular cloud, Astronomy and Astrophysics, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, submillimetre: ISM, 13. Climate action, Space and Planetary Science, Sky, Magnetic fields, Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Dust emission
Abstract: Planck Collaboration: et al., Observations of the submillimetre emission from Galactic dust, in both total intensity I and polarization, have received tremendous interest thanks to the Planck full-sky maps. In this paper we make use of such full-sky maps of dust polarized emission produced from the third public release of Planck data. As the basis for expanding on astrophysical studies of the polarized thermal emission from Galactic dust, we present full-sky maps of the dust polarization fraction p, polarization angle ψ, and dispersion function of polarization angles 𝒮. The joint distribution (one-point statistics) of p and NH confirms that the mean and maximum polarization fractions decrease with increasing NH. The uncertainty on the maximum observed polarization fraction, pmax = 22.0−1.4+3.5% at 353 GHz and 80′ resolution, is dominated by the uncertainty on the Galactic emission zero level in total intensity, in particular towards diffuse lines of sight at high Galactic latitudes. Furthermore, the inverse behaviour between p and 𝒮 found earlier is seen to be present at high latitudes. This follows the 𝒮 ∝ p−1 relationship expected from models of the polarized sky (including numerical simulations of magnetohydrodynamical turbulence) that include effects from only the topology of the turbulent magnetic field, but otherwise have uniform alignment and dust properties. Thus, the statistical properties of p, ψ, and 𝒮 for the most part reflect the structure of the Galactic magnetic field. Nevertheless, we search for potential signatures of varying grain alignment and dust properties. First, we analyse the product map 𝒮 × p, looking for residual trends. While the polarization fraction p decreases by a factor of 3−4 between NH = 1020 cm−2 and NH = 2 × 1022 cm−2, out of the Galactic plane, this product 𝒮 × p only decreases by about 25%. Because 𝒮 is independent of the grain alignment efficiency, this demonstrates that the systematic decrease in p with NH is determined mostly by the magnetic-field structure and not by a drop in grain alignment. This systematic trend is observed both in the diffuse interstellar medium (ISM) and in molecular clouds of the Gould Belt. Second, we look for a dependence of polarization properties on the dust temperature, as we would expect from the radiative alignment torque (RAT) theory. We find no systematic trend of 𝒮 × p with the dust temperature Td, whether in the diffuse ISM or in the molecular clouds of the Gould Belt. In the diffuse ISM, lines of sight with high polarization fraction p and low polarization angle dispersion 𝒮 tend, on the contrary, to have colder dust than lines of sight with low p and high 𝒮. We also compare the Planck thermal dust polarization with starlight polarization data in the visible at high Galactic latitudes. The agreement in polarization angles is remarkable, and is consistent with what we expect from the noise and the observed dispersion of polarization angles in the visible on the scale of the Planck beam. The two polarization emission-to-extinction ratios, RP/p and RS/V, which primarily characterize dust optical properties, have only a weak dependence on the column density, and converge towards the values previously determined for translucent lines of sight. We also determine an upper limit for the polarization fraction in extinction, pV/E(B − V), of 13% at high Galactic latitude, compatible with the polarization fraction p ≈ 20% observed at 353 GHz. Taken together, these results provide strong constraints for models of Galactic dust in diffuse gas., The research leading to these results has received funding from the European Research Council under the European Union’s Horizon 2020 Research & Innovation Framework Programme/ERC grant agreement ERC-2016-ADG-742719. This research has received funding from the Agence Nationale de la Recherche (ANR-17-CE31-0022). The Planck Collaboration acknowledges the support of ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU).
Published: 2020

9. Increase measurement range, distance, and speed of optical fiber distribution acoustic sensing

Author: Zhe Ma, Yixuan Wang, Shuang Wang, Guanghua Liang, Tiegen Liu, Kun Liu, and Junfeng Jiang
Subjects: Physics, Optical fiber, Sideband, Fiber Bragg grating, law, Acoustics, Bandwidth (signal processing), Phase (waves), Physics::Optics, Demodulation, Distributed acoustic sensing, Frequency modulation, law.invention
Abstract: Distributed acoustic sensing technology has unique advantage in diverse applications, such as seismology, mineral exploration, and so on. We explored the methods to increase measurement range, distance and speed, which are the most important requirement for field deployment. Heterogeneous sideband linear frequency modulated optical pulse with different frequency modulated bandwidth was used to realize simultaneous measurement of acoustic events in different dynamic ranges. Weak fiber Bragg gratings and phase of constructed single frequency were proposed for long distance sensing. Fast processing algorithm based on a graphics processing unit for a linear frequency modulation pulse demodulation was realized. The experiment results verified our methods well.
Published: 2021

10. 1/f Noise Analysis for FAST HI Intensity Mapping Drift-Scan Experiment

Author: Shifan Zuo, Guilaine Lagache, Xuelei Chen, Fengquan Wu, W. Hu, Yougang Wang, Mario G. Santos, Yichao Li, Bo Zhang, Yin-Zhe Ma, Ming Zhu, 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), National Astronomical Observatories [Beijing] (NAOC), Chinese Academy of Sciences [Beijing] (CAS), Peking University [Beijing], A*MIDEX, ERC CONCERTO (grant agreement ID 788212), and European Project: 788212,CONCERTO
Subjects: Physics, Noise power, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Intensity mapping, FOS: Physical sciences, Spectral density, Astronomy and Astrophysics, Low frequency, Coupling (probability), 01 natural sciences, Noise (electronics), Spectral line, Computational physics, Space and Planetary Science, 0103 physical sciences, Singular value decomposition, 010306 general physics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics
Abstract: We investigate the 1/f noise of the Five-hundred-meter Aperture Spherical Telescope (FAST) receiver system using drift-scan data from an intensity mapping pilot survey. All the 19 beams have 1/f fluctuations with similar structures. Both the temporal and the 2D power spectrum densities are estimated. The correlations directly seen in the time series data at low frequency $f$ are associated with the sky signal, perhaps due to a coupling between the foreground and the system response. We use Singular Value Decomposition (SVD) to subtract the foreground. By removing the strongest components, the measured 1/f noise power can be reduced significantly. With 20 modes subtraction, the knee frequency of the 1/f noise in a 10 MHz band is reduced to $1.8 \times 10^{-3}\Hz$, well below the thermal noise over 500-seconds time scale. The 2D power spectra show that the 1/f-type variations are restricted to a small region in the time-frequency space and the correlations in frequency can be suppressed with SVD modes subtraction. The residual 1/f noise after the SVD mode subtraction is uncorrelated in frequency, and a simple noise diode frequency-independent calibration of the receiver gain at 8s interval does not affect the results. The 1/f noise can be important for HI intensity mapping, we estimate that the 1/f noise has a knee frequency $(f_{k}) \sim$ 6 $\times$ 10$^{-4}$Hz, and time and frequency correlation spectral indices $(\alpha) \sim 0.65$, $(\beta) \sim 0.8$ after the SVD subtraction of 30 modes. This can bias the HI power spectrum measurement by 10 percent., Comment: 13 pages,17 figures, MNRAS accepted
Published: 2021

11. Constraining AGN feedback model with SZ profile

Author: Hideki Tanimura, Gary Hinshaw, Ian G. McCarthy, Ludovic Van Waerbeke, Nabila Aghanim, Yin-Zhe Ma, Alexander Mead, Tilman Tröster, Alireza Hojjati, Bruno Moraes, Institut d'astrophysique spatiale (IAS), and Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Physics, QC1-999, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, 13. Climate action, 0103 physical sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Relativistic jets from AGN have a wide range of impacts on galaxy groups and clusters and are key for understanding their formation and physical properties. However, this non-gravitational process is not well understood. Galaxy groups with shallow gravitational potentials are ideal laboratories to study and constrain the AGN feedback model. We studied hot gas in ~66,000 SDSS LRG halos with an average halo mass of 3 x 10^13 Msun using the Planck tSZ map. We have detected their average tSZ radial profile at ~17 sigma and compared it with the cosmo-OWLS cosmological hydrodynamical simulations with different AGN feedback models. The best agreement has been obtained for the AGN 8.0 model in the simulations. We have also compared our measured tSZ profile with the prediction from the universal pressure profile assuming the self-similar relation and found them consistent if the model accounts for the clustering of neighboring haloes via a two-halo term., Comment: To appear in the Proceedings of the International Conference entitled "mm Universe @ NIKA2", Rome (Italy), June 2021, EPJ Web of conferences
Published: 2021

12. Baryon Acoustic Oscillations from Integrated Neutral Gas Observations: an instrument to observe the 21cm hydrogen line in the redshift range 0.13 $<$ z $<$ 0.45 -- status update

Author: CARLOS A. WUENSCHE, ELCIO ABDALLA, FILIPE ABDALLA, LUCIANO BAROSI, BIN WANG, RUI AN, JOÃO A. M. BARRETOS, RICHARD BATTYE, FRANCISCO A. BRITO, IAN BROWNE, DANIEL CORREIA, ANDRÉ A. COSTA, JACQUES DELABROUILLE, CLIVE DICKINSON, CHANG FENG, ELISA G. M. FERREIRA, KARIN FORNAZIER, GIANCARLO DE GASPERIS, PRISCILA GUTIERREZ, STUART HARPER, RICARDO G. LANDIM, VINCENZO LICCARDO, YIN-ZHE MA, TELMO MACHADO, BRUNO MAFFEI, ALESSANDRO MARINS, MILENA M. M. MENDES, EDUARDO MERICIA, CHRISTIAN MONSTEIN, PABLO MOTTA, CAMILA NOVAES, CARLOS H. OTOBONE, MICHAEL PEEL, AMILCAR R. QUEIROZ, CHRISTOPHER RADCLIFFE, MATHIEU REMAZEILLES, RAFAEL M. G. RIBEIRO, YU SANG, JULIANA F. R. SANTOS, LARISSA SANTOS, MARCELO. V. SANTOS, CHENXI SHAN, GUSTAVO B. SILVA, FREDERICO VIEIRA, JORDANY VIEIRA, THYRSO VILLELA, LINFENG XIAO, WEIQIANG YANG, JIAJUN ZHANG, XUE ZHANG, ZENGHAO ZHU, AstroParticule et Cosmologie (APC (UMR_7164)), 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)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut d'astrophysique spatiale (IAS), and Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES)
Subjects: Science, media_common.quotation_subject, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, radio astronomy, 01 natural sciences, law.invention, Telescope, Radio telescope, law, 0103 physical sciences, 010303 astronomy & astrophysics, media_common, Physics, baryon acoustic oscillations, Multidisciplinary, BAO, 010308 nuclear & particles physics, Equation of state (cosmology), 21cm cosmology, Astrophysics::Instrumentation and Methods for Astrophysics, Redshift, Sky, Dark energy, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Hydrogen line, Baryon acoustic oscillations, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: BINGO (BAO from Integrated Neutral Gas Observations) is a unique radio telescope designed to map the intensity of neutral hydrogen distribution at cosmological distances, making the first detection of Baryon Acoustic Oscillations (BAO) in the frequency band 980 MHz - 1260 MHz, corresponding to a redshift range 0.127 < z < 0.449. BAO is one of the most powerful probes of cosmological parameters and BINGO was designed to detect the BAO signal to a level that makes it possible to put new constraints on the equation of state of dark energy. The telescope will be built in Paraíba, Brazil and consists of two \thicksim 40m mirrors, a feedhorn array of 50 horns, and no moving parts, working as a drift-scan instrument. It will cover a 15^{\circ} declination strip centered at \sim \delta =-15^{\circ}, mapping \sim 5400 square degrees in the sky. The BINGO consortium is led by University of São Paulo with co-leadership at National Institute for Space Research and Campina Grande Federal University (Brazil). Telescope subsystems have already been fabricated and tested, and the dish and structure fabrication are expected to start in late 2020, as well as the road and terrain preparation., Anais da Academia Brasileira de Ciências, 93, ISSN:0001-3765, ISSN:1678-2690
Published: 2021

13. Effect of the PTO Damping Force on the 2D Oscillating Buoy Wave Energy Converter Integrated into a Pile-Restrained Floating Breakwater

Author: Yong Cheng, Gangjun Zhai, Yanjun Mao, and Zhe Ma
Subjects: Optimal design, Physics, Work (thermodynamics), Coulomb damping, Buoy, 020209 energy, Mechanical Engineering, Computational Mechanics, 02 engineering and technology, Mechanics, 01 natural sciences, 010305 fluids & plasmas, Power (physics), Mechanics of Materials, 0103 physical sciences, 0202 electrical engineering, electronic engineering, information engineering, Coulomb, Potential flow, Parametric statistics
Abstract: The aim of the study is to evaluate the parametric effect of a power take-off (PTO) system on an integration system of an oscillating buoy wave energy device with a pile-restrained floating breakwater. To consider the viscous effect, the study is carried out with three conditions using OpenFOAM, i.e., the linear optimal PTO system, the fixed PTO damping coefficient, and the Coulomb PTO system. The results show that the maximum wave energy capture ratio (CWR) of the device can merely reach 0.35 in the present work, when considering the viscous effect. This result is smaller than that obtained from potential flow. In addition, the linear optimal PTO coefficient under viscous flow should be larger than the theoretical optimal coefficient in terms of the potential flow. A comparison of the Coulomb damping model and the linear damping model also shows that the Coulomb damping model has a good performance in terms of both wave energy capture efficiency and coastal protection. Hence, the effect of the PTO system on such an integration system can be an essential factor to achieve an optimal design.
Published: 2019

14. Fully nonlinear simulation of wave–current interaction with an oscillating wave surge converter

Author: Yong Cheng, Chunyan Ji, Zhe Ma, and Gangjun Zhai
Subjects: Physics, Mechanical Engineering, media_common.quotation_subject, Coordinate system, 020101 civil engineering, Ocean Engineering, Natural frequency, 02 engineering and technology, Mechanics, Oceanography, Inertia, 0201 civil engineering, Nonlinear system, Mechanics of Materials, Free surface, Fluid dynamics, Boundary element method, Wave–current interaction, media_common
Abstract: On the basis of a time-domain HOBEM (higher-order boundary element method), a two-dimensional (2D) fully nonlinear numerical model is developed to investigate the wave energy capturing efficiency of an OWSC (oscillating wave surge converter) in the presence of uniform currents. In the model, the wave energy is extracted through a linear external damping coefficient, and the natural frequency of the OWSC is tuned to the wave characteristics by introducing an elastic and inertia coefficient. On the free surface, a five-point fourth order Lagrangian interpolation method is applied to determine the redistribution of meshes, and a rotation scheme of spatial coordinate system is employed to tackle the discontinuity of flux at the intersection points. The wave loads on the wetted body surface are then evaluated using two auxiliary functions through which the mutual dependence of body motion and fluid flow is decoupled. The present model is validated against the published experimental and numerical results for an OWSC in large motion excited by nonlinear waves. Simulations are performed to capture the hydrodynamic behavior of the OWSC with different currents. Numerical results are also provided to show the behavior dependence on the design parameters, such as current velocities, wave conditions, geometric characteristics and mechanical properties.
Published: 2019

15. Coherent Phase-sensitive Optical Time Domain Reflectometer Based on Digital Orthogonal Pulses

Author: Zhe Ma, Zhenyang Ding, Tiegen Liu, Wenjie Chen, Tianhua Xu, Junfeng Jiang, Kun Liu, and Shuang Wang
Subjects: Physics, Optical fiber, Physics::Instrumentation and Detectors, Phase sensitive, business.industry, Detector, Phase diversity, Optical time-domain reflectometer, law.invention, Optics, law, Phase noise, Demodulation, business
Abstract: A coherent phase-sensitive optical time domain reflectometer (COTDR) based on digital orthogonal pulses is proposed. The digital orthogonal pulses provide phase diversity demodulation with a single detector and system sampling frequency will not reduce.
Published: 2021

16. Planck 2018 results: VI. Cosmological parameters (Corrigendum)

Author: Jose M. Diego, F. Piacentini, Soumen Basak, M. Frailis, Carlo Baccigalupi, M. Ashdown, H. K. Eriksen, François Levrier, E. Hivon, Reijo Keskitalo, L. Pagano, Hannu Kurki-Suonio, A. Renzi, F. Cuttaia, F. R. Bouchet, F. Villa, R. Fernandez-Cobos, L. Montier, Charles R. Lawrence, R. B. Barreiro, Simon D. M. White, Jean-François Cardoso, Tuhin Ghosh, A. Mennella, Nabila Aghanim, Zhiqi Huang, Hans Ulrik Nørgaard-Nielsen, P. Vielva, R. C. Butler, K. M. Górski, K. Kiiveri, Gianmarco Maggio, P. de Bernardis, Luca Valenziano, Steven Gratton, Lloyd Knox, Andrea Zacchei, Jonathan Aumont, F. K. Hansen, P. Bielewicz, Guilaine Lagache, Jörg P. Rachen, S. R. Hildebrandt, Antony Lewis, M. López-Caniego, D. Herranz, M. Le Jeune, N. Mandolesi, Julien Lesgourgues, Benjamin D. Wandelt, Julian Borrill, Peter G. Martin, Will Handley, L. Vibert, Jens Chluba, Peter Meinhold, Michele Liguori, Jan Hamann, G. Roudier, Diego Molinari, Andrei V. Frolov, J.-M. Delouis, J. González-Nuevo, Aurelien A. Fraisse, M. Sandri, Ingunn Kathrine Wehus, M. Tenti, B. P. Crill, J.-L. Puget, L. Salvati, X. Dupac, Massimiliano Lattanzi, Karim Benabed, Locke D. Spencer, Paolo Natoli, Francesco Forastieri, Nicola Bartolo, Erminia Calabrese, J.-P. Bernard, Marzieh Farhang, J. F. Macías-Pérez, Nicola Vittorio, V. Lindholm, A.-S. Suur-Uski, Adam Moss, E. Franceschi, W. C. Jones, P. Lemos, A. Karakci, D. Tavagnacco, Ricardo Genova-Santos, Tiziana Trombetti, B. Van Tent, Alessandro Gruppuso, Marius Millea, Graca Rocha, Sabino Matarrese, Theodore Kisner, Richard A. Battye, M. Martinelli, A. J. Banday, D. Contreras, J.-M. Lamarre, Ken Ganga, B. Partridge, Yabebal Fantaye, Jan Tauber, N. Mauri, J. J. Bock, Martin Kunz, E. Martínez-González, Jose Alberto Rubino-Martin, A. Ducout, Mathieu Remazeilles, S. Galeotta, Marian Douspis, Chiara Sirignano, O. Doré, Jon E. Gudmundsson, G. de Zotti, Hiranya V. Peiris, Yashar Akrami, Anthony Challinor, Michele Maris, M. Savelainen, Francesca Perrotta, P. B. Lilje, Torsten A. Enßlin, Valeria Pettorino, M. Tomasi, Jacques Delabrouille, Martin Reinecke, Marco Bersanelli, J. B. Kim, G. Sirri, Yin-Zhe Ma, E. P. S. Shellard, Fabio Finelli, S. Dusini, Andrea Zonca, H. C. Chiang, Martin White, M. Bucher, Douglas Scott, A. Mangilli, A. Marcos-Caballero, L. P. L. Colombo, Mario Ballardini, Daniela Paoletti, Jussi Valiviita, George Efstathiou, F. Boulanger, G. Polenta, Julien Carron, L. Toffolatti, Anthony Lasenby, Martina Gerbino, E. Keihänen, Andrew H. Jaffe, Marc-Antoine Miville-Deschênes, Philip Lubin, Davide Maino, M. Lilley, M. Migliaccio, J. R. Bond, B. Ruiz-Granados, Jason D. McEwen, Carlo Burigana, Nicoletta Krachmalnicoff, James R. Fergusson, Subhasish Mitra, C. Combet, R. A. Sunyaev, E. Di Valentino, G. Patanchon, L. Polastri, Alessandro Melchiorri, S. Galli, Gianluca Morgante, Franz Elsner, C. Rosset, and Universidad de Cantabria
Subjects: Physics, Numerical error, 010308 nuclear & particles physics, Astronomy, Cosmological parameters, Astronomy and Astrophysics, Astrophysics, Cosmic background radiation, 01 natural sciences, Upper and lower bounds, Errata, addenda, Combinatorics, symbols.namesake, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Optical depth (astrophysics), symbols, Planck, 010306 general physics
Abstract: Author(s): Aghanim, N; Akrami, Y; Ashdown, M; Aumont, J; Baccigalupi, C; Ballardini, M; Banday, AJ; Barreiro, RB; Bartolo, N; Basak, S; Battye, R; Benabed, K; Bernard, JP; Bersanelli, M; Bielewicz, P; Bock, JJ; Bond, JR; Borrill, J; Bouchet, FR; Boulanger, F; Bucher, M; Burigana, C; Butler, RC; Calabrese, E; Cardoso, JF; Carron, J; Challinor, A; Chiang, HC; Chluba, J; Colombo, LPL; Combet, C; Contreras, D; Crill, BP; Cuttaia, F; De Bernardis, P; De Zotti, G; Delabrouille, J; Delouis, JM; DI Valentino, E; DIego, JM; Dore, O; Douspis, M; Ducout, A; Dupac, X; Dusini, S; Efstathiou, G; Elsner, F; Enslin, TA; Eriksen, HK; Fantaye, Y; Farhang, M; Fergusson, J; Fernandez-Cobos, R; Finelli, F; Forastieri, F; Frailis, M; Fraisse, AA; Franceschi, E; Frolov, A; Galeotta, S; Galli, S; Ganga, K; Genova-Santos, RT; Gerbino, M; Ghosh, T; Gonzalez-Nuevo, J; Gorski, KM; Gratton, S; Gruppuso, A; Gudmundsson, JE; Hamann, J; Handley, W; Hansen, FK; Herranz, D; Hildebrandt, SR; Hivon, E; Huang, Z; Jaffe, AH; Jones, WC; Karakci, A; Keihanen, E; Keskitalo, R; Kiiveri, K; Kim, J; Kisner, TS | Abstract: In the original version, the bounds given in Eqs. (87a) and (87b) on the contribution to the early-time optical depth, (15,30), contained a numerical error in deriving the 95th percentile from the Monte Carlo samples. The corrected 95% upper bounds are: τ(15,30) l 0:018 (lowE, flat τ(15, 30), FlexKnot), (1) τ(15, 30) l 0:023 (lowE, flat knot, FlexKnot): (2) These bounds are a factor of 3 larger than the originally reported results. Consequently, the new bounds do not significantly improve upon previous results from Planck data presented in Millea a Bouchet (2018) as was stated, but are instead comparable. Equations (1) and (2) give results that are now similar to those of Heinrich a Hu (2021), who used the same Planck 2018 data to derive a 95% upper bound of 0.020 using the principal component analysis (PCA) model and uniform priors on the PCA mode amplitudes.
Published: 2021

17. Reconciling Hubble constant discrepancy from holographic dark energy

Author: Hong-Jian He, Yin-Zhe Ma, and Wei-Ming Dai
Subjects: High Energy Physics - Theory, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic microwave background, Cosmic background radiation, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, symbols.namesake, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010306 general physics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Galaxy, Redshift, Baryon, Black hole, High Energy Physics - Phenomenology, High Energy Physics - Theory (hep-th), symbols, Dark energy, Astrophysics - Cosmology and Nongalactic Astrophysics, Hubble's law
Abstract: Holographic dark energy (HDE) describes the vacuum energy in a cosmic IR region whose total energy saturates the limit of avoiding the collapse into a black hole. HDE predicts that the dark energy equation of the state transiting from greater than the $-1$ regime to less than $-1$, accelerating the Universe slower at the early stage and faster at the late stage. We propose the HDE as a new {\it physical} resolution to the Hubble constant discrepancy between the cosmic microwave background (CMB) and local measurements. With Planck CMB and galaxy baryon acoustic oscillation (BAO) data, we fit the HDE prediction of the Hubble constant as $H_0^{}\!=\, 71.54\pm1.78\,\mathrm{km\,s^{-1} Mpc^{-1}}$, consistent with local $H_0^{}$ measurements by LMC Cepheid Standards (R19) at $1.4\sigma$ level. Combining Planck+BAO+R19, we find the HDE parameter $c=0.51\pm0.02$ and $H_0^{}\! = 73.12\pm 1.14\,\mathrm{km \,s^{-1} Mpc^{-1}}$, which fits cosmological data at all redshifts. Future CMB and large-scale structure surveys will further test the holographic scenario., Comment: Published version in PRD Rapid Communication, 6 pages, 5 figures, 2 tables. All results and conclusions are unchanged, only minor refinements, references added
Published: 2020

18. Interacting system NGC 7805/6 (Arp 112) and its tidal dwarf galaxy candidate

Author: Mridweeka Singh, T. C. Scott, Chandreyee Sengupta, Zhen-Xing Fu, Bikram Pradhan, Yin-Zhe Ma, Ramya Sethuram, and Kuntal Misra
Subjects: Physics, Giant Metrewave Radio Telescope, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar population, 010308 nuclear & particles physics, Star formation, Metallicity, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, law.invention, Telescope, Space and Planetary Science, law, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, 010303 astronomy & astrophysics, Dwarf galaxy, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present results from our Giant Metrewave Radio Telescope (GMRT) HI, Himalayan Chandra Telescope (HCT) Halpha, 1m Sampurnanand Telescope (ST) and 1.3m Devasthal Fast Optical Telescope (DFOT) deep optical observations of NGC 7805/6 (Arp 112) system to test KUG 2359+311's tidal dwarf galaxy (TDG) candidacy and explore the properties of the interacting system. Our GMRT HI map shows no HI detection associated with KUG 2359+311, nor any HI tail or bridge-like structure connecting KUG 2359+311 to the NGC 7805/6 system. Our HCT Halpha image on the other hand, shows strong detections in KUG 2359+311, with net SFR ~ 0.035$\pm 0.009 {\rm M}_{\odot}\,{\rm yr}^{-1}$. The Halpha data constrains the redshift of KUG 2359+311 to $0.00 \le z \le 0.043$, compared to the redshift of NGC 7806 of ~ 0.015. TDGs detected to date have all been HI rich, and displayed HI, ionised gas and stellar tidal debris trails (bridges or tails) linking them to their parent systems. But neither our HI data nor our optical images, while three magnitudes deeper than SDSS, reveal tidal trail connecting KUG 2359+311 to NGC 7805/6. Lack of HI , presence of an old stellar population, ongoing star formation, reasonably high SFR compared to normal dwarf galaxies suggest that KUG 2359+311 may not be an Arp 112 TDG. It is most likely a case of a regular gas-rich dwarf galaxy undergoing a morphological transformation after having lost its entire gas content to an interaction with the Arp 112 system. Redshift and metallicity from future spectroscopic observations of KUG 2359+311 would help clarify the nature of this enigmatic structure., Accepted in RAA
Published: 2020

19. Redundant-baseline calibration of the hydrogen epoch of reionization array

Author: Adrian Liu, Craig Smith, Paul Alexander, John Ely, Deepthi Gorthi, Nithyanandan Thyagarajan, Steven G. Murray, Joshua S. Dillon, Bryna J. Hazelton, Phil Bull, Nipanjana Patra, Jon Ringuette, Zara Abdurashidova, Ziyaad Halday, Aaron R. Parsons, Bradley Greig, Lourence Malan, Angelo Syce, Gianni Bernardi, Piyanat Kittiwisit, Austin Julius, Daniel C. Jacobs, Kingsley Gale-Sides, Jack Hickish, Yin-Zhe Ma, Jonathan C. Pober, Kathryn Rosie, Adam P. Beardsley, Robert Pascua, Peter K. G. Williams, Cresshim Malgas, S. H. Carey, Jacob Burba, Nicolas Fagnoni, David MacMahon, Andrei Mesinger, Jasper Grobbelaar, Yanga Balfour, Joshua Kerrigan, Max Tegmark, Richard F. Bradley, Matthew Kolopanis, David DeBoer, Abraham R. Neben, Mario G. Santos, Randall Fritz, Jacqueline N. Hewitt, Tashalee S. Billings, Zachary E. Martinot, Eunice Matsetela, Saul A. Kohn, David Lewis, Peter Sims, Mathakane Molewa, Naomi Orosz, Steven R. Furlanetto, Paul La Plante, Chuneeta D. Nunhokee, Matt Dexter, Tshegofalang Mosiane, Nicholas S. Kern, Judd D. Bowman, Samantha Pieterse, Max E. Lee, James E. Aguirre, Nima Razavi-Ghods, Miguel F. Morales, Zaki S. Ali, Bojan Nikolic, Aaron Ewall-Wice, Chris Carilli, Eloy de Lera Acedo, James Robnett, Brian Glendenning, Carina Cheng, Matthys Maree, Telalo Lekalake, Haoxuan Zheng, Adam Lanman, ITA, USA, ZAF, Dillon, J. S., Lee, M., Ali, Z. S., Parsons, A. R., Orosz, N., Nunhokee, C. D., La Plante, P., Beardsley, A. P., Kern, N. S., Abdurashidova, Z., Aguirre, J. E., Alexander, P., Balfour, Y., Bernardi, G., Billings, T. S., Bowman, J. D., Bradley, R. F., Bull, P., Burba, J., Carey, S., Carilli, C. L., Cheng, C., Deboer, D. R., Dexter, M., de Lera Acedo, E., Ely, J., Ewall-Wice, A., Fagnoni, N., Fritz, R., Furlanetto, S. R., Gale-Sides, K., Glendenning, B., Gorthi, D., Greig, B., Grobbelaar, J., Halday, Z., Hazelton, B. J., Hewitt, J. N., Hickish, J., Jacobs, D. C., Julius, A., Kerrigan, J., Kittiwisit, P., Kohn, S. A., Kolopanis, M., Lanman, A., Lekalake, T., Lewis, D., Liu, A., Ma, Y. -Z., Macmahon, D., Malan, L., Malgas, C., Maree, M., Martinot, Z. E., Matsetela, E., Mesinger, A., Molewa, M., Morales, M. F., Mosiane, T., Murray, S., Neben, A. R., Nikolic, B., Pascua, R., Patra, N., Pieterse, S., Pober, J. C., Razavi-Ghods, N., Ringuette, J., Robnett, J., Rosie, K., Santos, M. G., Sims, P., Smith, C., Syce, A., Tegmark, M., Thyagarajan, N., Williams, P. K. G., Zheng, H., Alexander, Paul [0000-0002-0292-9513], De Lera Acedo, Eloy [0000-0001-8530-6989], Nikolic, Bojan [0000-0001-7168-2705], Razavi-Ghods, Nima [0000-0003-2930-5396], and Apollo - University of Cambridge Repository
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Calibration (statistics), interferometers [instrumentation], first stars, Degrees of freedom (statistics), FOS: Physical sciences, Astronomy & Astrophysics, 01 natural sciences, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Astronomical interferometer, dark ages, reionization, first stars, dark ages, instrumentation: interferometers, 010303 astronomy & astrophysics, Reionization, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, 010308 nuclear & particles physics, Noise (signal processing), Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, HERA, Interferometry, Dark ages, reionization, first star, Space and Planetary Science, astro-ph.CO, reionization, Antenna (radio), Astrophysics - Instrumentation and Methods for Astrophysics, Algorithm, Astronomical and Space Sciences, Astrophysics - Cosmology and Nongalactic Astrophysics, astro-ph.IM
Abstract: In 21 cm cosmology, precision calibration is key to the separation of the neutral hydrogen signal from very bright but spectrally-smooth astrophysical foregrounds. The Hydrogen Epoch of Reionization Array (HERA), an interferometer specialized for 21 cm cosmology and now under construction in South Africa, was designed to be largely calibrated using the self-consistency of repeated measurements of the same interferometric modes. This technique, known as "redundant-baseline calibration" resolves most of the internal degrees of freedom in the calibration problem. It assumes, however, on antenna elements with identical primary beams placed precisely on a redundant grid. In this work, we review the detailed implementation of the algorithms enabling redundant-baseline calibration and report results with HERA data. We quantify the effects of real-world non-redundancy and how they compare to the idealized scenario in which redundant measurements differ only in their noise realizations. Finally, we study how non-redundancy can produce spurious temporal structure in our calibration solutions--both in data and in simulations--and present strategies for mitigating that structure., Comment: 24 Pages, 19 Figures. Updated to match the accepted MNRAS version
Published: 2020

20. Virtual-block-array phase analysis for distributed acoustic sensors with a high signal-to-noise ratio reconstruction waveform

Author: Wenjie Chen, Tianhua Xu, Tiegen Liu, Yongning Zhang, Shuanghao Wang, Kun Liu, Panpan Niu, Junfeng Jiang, Shuang Wang, and Zhe Ma
Subjects: Physics, Mean squared error, business.industry, Pulse (signal processing), Process (computing), 02 engineering and technology, 021001 nanoscience & nanotechnology, 01 natural sciences, Signal, Atomic and Molecular Physics, and Optics, 010309 optics, Optics, Signal-to-noise ratio, Fiber Bragg grating, 0103 physical sciences, Waveform, 0210 nano-technology, business, Block (data storage)
Abstract: A virtual-block-array phase analysis method is proposed for the fiber-optic distributed acoustic sensor. The sensing fiber is divided into a serial of discrete virtual blocks according to the pulse spatial length. The phase variation caused by acoustic events is obtained by combining the operation of the temporal differential process between traces and local spatial average in virtual blocks. The linear frequency-modulated probe pulse produces phase compensation effects at the event location. High signal-to-noise ratio (SNR) measurement is verified by simulation and experiment. The reconstructed waveform of 1.5 kHz sinusoidal signal showed a root mean square error of 0.0359 and an SNR of 47.28 dB.
Published: 2020

21. The neutral hydrogen distribution in large-scale haloes from 21-cm intensity maps

Author: Yin-Zhe Ma and Denis Tramonte
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Galaxy, Redshift, Radio telescope, Space and Planetary Science, Brightness temperature, Content (measure theory), Satellite galaxy, Halo, Intensity (heat transfer), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We detect the neutral hydrogen (HI) radial brightness temperature profile in large-scale haloes by stacking 48,430 galaxies selected from the 2dFGRS catalogue onto a set of 21-cm intensity maps obtained with the Parkes radio telescope, spanning a total area of $\sim$1,300 $\text{deg}^2$ on the sky and covering the redshift range $0.06\lesssim z\lesssim 0.10$. Maps are obtained by removing both 10 and 20 foreground modes in the principal component analysis. We perform the stack at the map level and extract the profile from a circularly symmetrised version of the halo emission. We detect the HI halo emission with the significance $12.5\sigma$ for the 10-mode and $13.5\sigma$ for the 20-mode removed maps at the profile peak. We jointly fit for the observed halo mass $M_{\rm v}$ and the normalisation $c_{0,\rm HI}$ for the HI concentration parameter against the reconstructed profiles, using functional forms for the HI halo abundance proposed in the literature. We find $\log_{10}{(M_{\rm v}/\text{M}_{\odot})} = 16.1^{+0.1}_{-0.2}$, $c_{0,\rm HI}=3.5^{+0.7}_{-1.0}$ for the 10-mode and $\log_{10}{(M_{\rm v}/\text{M}_{\odot})} = 16.5^{+0.1}_{-0.2}$, $c_{0,\rm HI}=5.3^{+1.1}_{-1.7}$ for the 20-mode removed maps. These estimates show the detection of the integrated contribution from multiple galaxies located inside very massive haloes. We also consider sub-samples of 13,979 central and 34,361 satellite 2dF galaxies separately, and obtain marginal differences suggesting satellite galaxies are HI-richer. This work shows for the first time the feasibility of testing theoretical models for the HI halo content directly on profiles extracted from 21-cm maps and opens future possibilities for exploiting upcoming HI intensity-mapping data., Comment: 20 pages, 13 figures. Accepted for publication in MNRAS
Published: 2020

22. Planck 2018 results

Author: Jean-François Cardoso, A. A. Fraisse, P. Vielva, A. J. Banday, Charles R. Lawrence, Yabebal Fantaye, Alessandro Gruppuso, Krzysztof M. Gorski, J.-L. Puget, B. D. Wandelt, Guilaine Lagache, A. Mangilli, M. López-Caniego, P. de Bernardis, R. B. Barreiro, M.-A. Miville-Deschênes, Matthieu Tristram, K. Kiiveri, M. Frailis, Carlo Baccigalupi, François Levrier, E. Hivon, S. Galli, J. Aumont, François R. Bouchet, A. Renzi, Reijo Keskitalo, Michele Liguori, Sabino Matarrese, Diego Molinari, M. Ashdown, A. Mennella, Nabila Aghanim, F. K. Hansen, A. Ducout, E. Martínez-González, J.-M. Lamarre, B. Partridge, Gianluca Morgante, Yashar Akrami, Anthony Challinor, H. K. Eriksen, L. P. L. Colombo, L. Pagano, L. Patrizii, Marian Douspis, J.-M. Delouis, O. Perdereau, Alessandro Melchiorri, X. Dupac, N. Mandolesi, Andrew H. Jaffe, Hannu Kurki-Suonio, J. A. Tauber, M. Savelainen, M. Tomasi, Mario Ballardini, George Efstathiou, Nicola Bartolo, Andrea Zonca, H. C. Chiang, N. Mauri, O. Doré, L. Vibert, Theodore Kisner, Steven Gratton, Marco Bersanelli, Andrei V. Frolov, L. Salvati, Erminia Calabrese, A. Moneti, L. Montier, J. B. Kim, A.-S. Suur-Uski, Martina Gerbino, G. Sirri, Tuhin Ghosh, J. F. Macías-Pérez, F. Boulanger, P. B. Lilje, J. Valiviita, G. Patanchon, Adam Moss, Ricardo Genova-Santos, M. Migliaccio, Graca Rocha, Zhiqi Huang, C. Combet, E. Falgarone, Valeria Pettorino, Ingunn Kathrine Wehus, M. Bucher, Douglas Scott, D. Tavagnacco, M. Sandri, Jacques Delabrouille, S. Mottet, G. Roudier, J. González-Nuevo, L. Toffolatti, Davide Maino, Julian Borrill, Massimiliano Lattanzi, Will Handley, Jörg P. Rachen, M. Tenti, Anthony Lasenby, Fabio Finelli, E. Keihänen, Tiziana Trombetti, E. Di Valentino, Francesca Perrotta, Sophie Henrot-Versille, E. Franceschi, Gianmarco Maggio, F. Cuttaia, Fabrizio Villa, J.-P. Bernard, Torsten A. Enßlin, D. Herranz, D. Paoletti, Paolo Natoli, A. Karakci, F. Vansyngel, P. Bielewicz, W. C. Jones, Julien Carron, Peter G. Martin, S. Galeotta, Yin-Zhe Ma, K. Benabed, K. Ganga, Jose M. Diego, J. R. Bond, F. Piacentini, Soumen Basak, M. Reinecke, R. A. Sunyaev, Chiara Sirignano, G. de Zotti, F. Couchot, Franz Elsner, B. P. Crill, B. Van Tent, Nicola Vittorio, V. Lindholm, Jason D. McEwen, Martin Kunz, Carlo Burigana, Nicoletta Krachmalnicoff, Mathieu Remazeilles, Jon E. Gudmundsson, A. de Rosa, Locke D. Spencer, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), 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), Canadian Institute for Theoretical Astrophysics (CITA), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), 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)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Dipartimento di Fisica [Roma La Sapienza], Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), 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), Dipartimento di Fisica 'G. Galilei', Universita degli Studi di Padova, 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), University of Manchester [Manchester], University of British Columbia (UBC), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Planck Collaboration, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Sud - Paris 11 (UP11), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), Sorbonne Université (SU)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2020-....] (UGA [2020-....])-Institut polytechnique de Grenoble - Grenoble Institute of Technology [2020-....] (Grenoble INP [2020-....]), Université Grenoble Alpes [2020-....] (UGA [2020-....]), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Planck, Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), 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), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), 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), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Université Toulouse III - Paul Sabatier (UT3), Aghanim N., 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., Boulanger F., Bucher M., Burigana C., Calabrese E., Cardoso J.-F., Carron J., Challinor A., Chiang H.C., Colombo L.P.L., Combet C., Couchot F., Crill B.P., Cuttaia F., De Bernardis P., De Rosa A., De Zotti G., Delabrouille J., Delouis J.-M., Di Valentino E., Diego J.M., Dore O., Douspis M., Ducout A., Dupac X., Efstathiou G., Elsner F., Ensslin T.A., Eriksen H.K., Falgarone E., Fantaye Y., Finelli F., Frailis M., Fraisse A.A., Franceschi E., Frolov A., Galeotta S., Galli S., Ganga K., Genova-Santos R.T., Gerbino M., Ghosh T., Gonzalez-Nuevo J., Gorski K.M., Gratton S., Gruppuso A., Gudmundsson J.E., Handley W., Hansen F.K., Henrot-Versille S., Herranz D., Hivon E., Huang Z., Jaffe A.H., Jones W.C., Karakci A., Keihanen E., Keskitalo R., Kiiveri K., Kim J., Kisner T.S., Krachmalnicoff N., Kunz M., Kurki-Suonio H., Lagache G., Lamarre J.-M., Lasenby A., Lattanzi M., Lawrence C.R., Levrier F., Liguori M., Lilje P.B., Lindholm V., Lopez-Caniego M., Ma Y.-Z., Macias-Perez J.F., Maggio G., Maino D., Mandolesi N., Mangilli A., Martin P.G., Martinez-Gonzalez E., Matarrese S., Mauri N., McEwen J.D., Melchiorri A., Mennella A., Migliaccio M., Miville-Deschenes M.-A., Molinari D., Moneti A., Montier L., Morgante G., Moss A., Mottet S., Natoli P., Pagano L., Paoletti D., Partridge B., Patanchon G., Patrizii L., Perdereau O., Perrotta F., Pettorino V., Piacentini F., Puget J.-L., Rachen J.P., Reinecke M., Remazeilles M., Renzi A., Rocha G., Roudier G., Salvati L., Sandri M., Savelainen M., Scott D., Sirignano C., Sirri G., Spencer L.D., Sunyaev R., Suur-Uski A.-S., Tauber J.A., Tavagnacco D., Tenti M., Toffolatti L., Tomasi M., Tristram M., Trombetti T., Valiviita J., Vansyngel F., Van Tent B., Vibert L., Vielva P., Villa F., Vittorio N., Wandelt B.D., Wehus I.K., Zonca A., Ministerio de Economía y Competitividad (España), Consejo Superior de Investigaciones Científicas (España), European Commission, European Research Council, European Space Agency, Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-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)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), 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), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Università degli Studi di Padova = University of Padua (Unipd), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Universidad de Cantabria, Department of Physics, Helsinki Institute of Physics, and Doctoral Programme in Particle Physics and Universe Sciences
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astronomy, Cosmic microwave background, Cosmic background radiation, FOS: Physical sciences, Astrophysics, cosmic background radiation, Surveys, 01 natural sciences, Cosmology: observation, NO, symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, surveys, 0103 physical sciences, Calibration, Planck, observations [Cosmology], data analysis [Methods], 010303 astronomy & astrophysics, Reionization, LATITUDE MOLECULAR GAS, Physics, SPECTRUM, 010308 nuclear & particles physics, cosmology: observations, methods: data analysis, Settore FIS/05, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, 115 Astronomy, Space science, Computational physics, MODEL, Dipole, Amplitude, SKY MAPS, Cosmic background radiation, Cosmology: observations, Methods: data analysis, Surveys, Space and Planetary Science, SEPARATION, symbols, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics, Methods: data analysi
Abstract: Planck Collaboration: et al., This paper presents the High Frequency Instrument (HFI) data processing procedures for the Planck 2018 release. Major improvements in mapmaking have been achieved since the previous Planck 2015 release, many of which were used and described already in an intermediate paper dedicated to the Planck polarized data at low multipoles. These improvements enabled the first significant measurement of the reionization optical depth parameter using Planck-HFI data. This paper presents an extensive analysis of systematic effects, including the use of end-to-end simulations to facilitate their removal and characterize the residuals. The polarized data, which presented a number of known problems in the 2015 Planck release, are very significantly improved, especially the leakage from intensity to polarization. Calibration, based on the cosmic microwave background (CMB) dipole, is now extremely accurate and in the frequency range 100–353 GHz reduces intensity-to-polarization leakage caused by calibration mismatch. The Solar dipole direction has been determined in the three lowest HFI frequency channels to within one arc minute, and its amplitude has an absolute uncertainty smaller than 0.35 μK, an accuracy of order 10−4. This is a major legacy from the Planck HFI for future CMB experiments. The removal of bandpass leakage has been improved for the main high-frequency foregrounds by extracting the bandpass-mismatch coefficients for each detector as part of the mapmaking process; these values in turn improve the intensity maps. This is a major change in the philosophy of “frequency maps”, which are now computed from single detector data, all adjusted to the same average bandpass response for the main foregrounds. End-to-end simulations have been shown to reproduce very well the relative gain calibration of detectors, as well as drifts within a frequency induced by the residuals of the main systematic effect (analogue-to-digital convertor non-linearity residuals). Using these simulations, we have been able to measure and correct the small frequency calibration bias induced by this systematic effect at the 10−4 level. There is no detectable sign of a residual calibration bias between the first and second acoustic peaks in the CMB channels, at the 10−3 level., The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planckcollaboration.
Published: 2020

23. Testing interacting dark matter and dark energy model with cosmological data

Author: Yin-Zhe Ma, Jiajun Zhang, Gong Cheng, Fengquan Wu, and Xuelei Chen
Subjects: High Energy Physics - Theory, Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Dark matter, Cosmic microwave background, Cosmic background radiation, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, Galaxy, Baryon, High Energy Physics - Theory (hep-th), Observational cosmology, 0103 physical sciences, Dark energy, Baryon acoustic oscillations, 010306 general physics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We investigate the model of dark matter-dark energy (DM-DE) interaction with coupling strength proportional to the multiplication of dark sector densities with different power indices $Q = \gamma \rho_{\rm c}^{\alpha} \rho_{\rm d}^{\beta}$. We first investigate the modification of the cosmic expansion history, and then further develop the formalism to take into account the cosmological perturbations and dark matter temperature evolution. We then use the latest observational cosmology data, including cosmic microwave background (CMB) data, baryon acoustic oscillations (BAO) data, redshift-space distortion (RSD) data and Type Ia supernovae (SNe) data to constrain the model parameters. We find in the phantom region, a positive $\alpha$ is preferred by the data above $2\, \sigma$ statistic significance. If we choose the power indices to be integers or half-integers for {\it plausible} physics of particle interaction, the allowed values within $1\, \sigma$ confidence regions are $\alpha = 0.5$ and $\beta = 0, 0.5, 1$. The inclusion of BAO and RSD data from large-scale structure and SNe data improves the constraints significantly. Our model predicts lower values of $f(z) \sigma_8(z)$ at $z, Comment: 12 pages, 8 figures, PRD accepted
Published: 2020

24. Mimicking an expanding universe by optical interference in a helicoid waveguide

Author: Runqiu He, Guo-Hua Liang, Rong G. Cai, Shining Zhu, Hui Liu, and Yin-Zhe Ma
Subjects: Physics, Helicoid, business.industry, Wave packet, Physics::Optics, 02 engineering and technology, 021001 nanoscience & nanotechnology, 01 natural sciences, Atomic and Molecular Physics, and Optics, Cosmology, Redshift, law.invention, Metric expansion of space, 010309 optics, Lens (optics), Optics, law, Surface wave, 0103 physical sciences, Mathematics::Differential Geometry, 0210 nano-technology, business, Nonlinear Sciences::Pattern Formation and Solitons, Waveguide
Abstract: According to modern cosmology, expansion of the universe is due to the metric changing of spacetime itself. Here, we propose to mimic an expanding universe by utilizing optical interference and helicoid waveguides. The evolution of interference pattern in the helicoid waveguide is investigated theoretically and experimentally. For precise measurements, we design an air helicoid waveguide which allows us to investigate the wave front of laser beams from the waveguide. Redshift of a Gaussian wave packet in the expanding universe is demonstrated with high precision, showing that the helicoid waveguide acts as a parabolic gradient index lens exactly. The proposed waveguide structure can be used as an efficient waveguide adapter.
Published: 2020

25. How much primordial tensor mode is allowed?

Author: Jun-Qing Xia, Moumita Aich, Wei-Ming Dai, and Yin-Zhe Ma
Subjects: Physics, Particle physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Expansion rate, 010308 nuclear & particles physics, Gravitational wave, Cosmic microwave background, FOS: Physical sciences, Sigma, Spectral density, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, symbols.namesake, Amplitude, 0103 physical sciences, symbols, Neutrino, Planck, 010306 general physics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The presence of a significant amount of gravitational radiation in the early Universe affects the total energy density and hence the expansion rate in the early epoch. In this work, we develop a physical model to connect the parameter of relativistic degree of freedom $N_\mathrm{eff}$ with the amplitude and shape of primordial tensor power spectrum, and use the CMB temperature and polarization data from {\it Planck} and BICEP2/KECK Array, and the primordial deuterium measurement from damped Lyman-$\alpha$ (DLA) systems to constrain this model. We find that with this extra relation $\Delta N_{\rm eff}(r,n_{\rm t})$, the tensor-to-scalar ratio $r$ is constrained to be $r, Comment: 12 pages, 7 figures
Published: 2020

26. Probing Dark Matter with Future CMB Measurements

Author: Yu Gao, Yin-Zhe Ma, and Junsong Cang
Subjects: Physics, Particle physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Annihilation, 010308 nuclear & particles physics, Cosmic microwave background, Dark matter, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Lambda, 01 natural sciences, Redshift, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, 010306 general physics, Reionization, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Dark Matter (DM) annihilation and decay during the Dark Ages can affect the cosmic ionization history and leave imprints in the Cosmic Microwave Background (CMB) anisotropy spectra. CMB polarization anisotropy can be sensitive to such energy injection at higher redshifts and help reducing degeneracy with primordial spectral parameters in $\Lambda$CDM and astrophysical ionization processes during reionization. In light of a number of upcoming CMB polarization experiments, such as AdvACTPol, AliCPT, CLASS, Simons Observatory, Simons Array, SPT-3G, we estimate their prospective sensitivity in probing dark matter annihilation and decay signals. We find that future missions have 95\% C.L. projected limits on DM decay and annihilation rates to orders of $\Gamma_\chi (\tau_{\chi}^{-1}) \sim 10^{-27}{\rm{s}}^{-1}$ and $\left/m_{\chi} \sim 10^{-29}{\rm{cm^3s^{-1}GeV^{-1}}}$ respectively, significantly improving the sensitivity to DM from current experimental bounds., Comment: 10 pages, 4 figures, 4 tables. Accepted by Physical Review D, experimental specification updated
Published: 2020

27. Constraining the redshifts of unlocalised fast radio bursts

Author: Rene P. Breton, Yin-Zhe Ma, and C. R. H. Walker
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Galaxy, Redshift, Space and Planetary Science, Intergalactic medium, 0103 physical sciences, Probability distribution, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics
Abstract: The population of fast radio bursts (FRBs) will continue to diverge into two groups depending on their method of discovery: those which can be localised, and those which cannot. Events potentially less useful for astronomical and cosmological purposes due to limited localisation will accumulate with the advent of new facilities and continued efforts by, e.g., the SUPERB collaboration, which may require afterglows or multi-wavelength counterparts for sub-arcsecond localisation. It is important to exploit these sources to their maximum scientific potential. We perform analysis of FRB dispersion measures (DMs), considering different theoretical FRB progenitors with view to place more rigorous constraints on FRB redshifts, in particular for large statistical samples, via their DMs. We review FRB DM components, and build redshift-scalable probability distributions corresponding to different progenitor scenarios. We combine these components into a framework for obtaining FRB DM probabilities given their redshifts. Taking into account different possibilities for the evolution of progenitors across cosmic time we invert this model, thus deriving redshift constraints. Effects of varying FRB progenitor models are illustrated. While, as expected, host galaxy DM contributions become decreasingly important with increasing redshift, for AGN-like progenitor scenarios they could remain significant out to redshift 3. Constraints are placed on redshifts of catalogued FRBs with various models and increasingly realistic models may be employed as general understanding of FRBs improves. For localised FRBs, we highlight future prospects for disentangling host and intergalactic medium DM components using their respective redshift scaling. We identify a use for large samples of unlocalised FRBs resulting from upcoming flux-limited surveys, such as with CHIME, in mapping out the Milky Way contribution to the DM., 13 pages, 8 figures, submitted for publication in Astronomy & Astrophysics on 04/04/2018
Published: 2020
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28. Probing the cluster pressure profile with thermal Sunyaev-Zeldovich effect and weak lensing cross-correlation

Author: Ludovic Van Waerbeke, Yan Gong, Yin-Zhe Ma, and Tilman Tröster
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Cosmic background radiation, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Radius, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, CMB cold spot, Astrophysics - Astrophysics of Galaxies, Cosmology, symbols.namesake, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Cluster (physics), symbols, Halo, Planck, 010303 astronomy & astrophysics, Weak gravitational lensing, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We confront the universal pressure profile (UPP) proposed by~\citet{Arnaud10} with the recent measurement of the cross-correlation function of the thermal Sunyaev-Zeldovich (tSZ) effect from Planck and weak gravitational lensing measurement from the Red Cluster Sequence lensing survey (RCSLenS). By using the halo model, we calculate the prediction of $\xi^{y-\kappa}$ (lensing convergence and Compton-$y$ parameter) and $\xi^{y-\gamma_{\rm t}}$ (lensing shear and Compton-$y$ parameter) and fit the UPP parameters by using the observational data. We find consistent UPP parameters when fixing the cosmology to either WMAP 9-year or Planck 2018 best-fitting values. The best constrained parameter is the pressure profile concentration $c_{500}=r_{500}/r_{\rm s}$, for which we find $c_{500} = 2.68^{+1.46}_{-0.96}$ (WMAP-9) and $c_{500} = 1.91^{+1.07}_{-0.65}$ (Planck-2018) for the $\xi^{y-\gamma_t}$ estimator. The shape index for the intermediate radius region $\alpha$ parameter is constrained to $\alpha=1.75^{+1.29}_{-0.77}$ and $\alpha = 1.65^{+0.74}_{-0.5}$ for WMAP-9 and Planck-2018 cosmologies, respectively. Propagating the uncertainties of the UPP parameters to pressure profiles results in a factor of $3$ uncertainty in the shape and magnitude. Further investigation shows that most of the signal of the cross-correlation comes from the low-redshift, inner halo profile ($r \leqslant r_{\rm vir}/2$) with halo mass in the range of $10^{14}$--$10^{15}\,{\rm M}_{\odot}$, suggesting that this is the major regime that constitutes the cross-correlation signal between weak lensing and tSZ., Comment: 12 pages, 6 figures, accepted by Monthly Notices of the Royal Astronomical Society
Published: 2020
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29. Planck intermediate results

Author: E. Franceschi, Erminia Calabrese, Michael P. Hobson, Jose M. Diego, S. Galeotta, Yashar Akrami, L. Toffolatti, F. Piacentini, M. Tenti, X. Dupac, Paolo Natoli, M. Ashdown, A. Renzi, M. Savelainen, M. Migliaccio, N. Mandolesi, Eric Hivon, Tiziana Trombetti, J. Aumont, E. Keihänen, Peter G. Martin, Francesca Perrotta, Torsten A. Enßlin, M. López-Caniego, Fabrizio Villa, J.-P. Bernard, J. González-Nuevo, Ingunn Kathrine Wehus, G. de Zotti, Zhiqi Huang, P. Bielewicz, Valeria Pettorino, F. Cuttaia, W. C. Jones, Alessandro Gruppuso, R. Fernandez-Cobos, Julian Borrill, Will Handley, H. K. Eriksen, G. Sirri, Carlo Baccigalupi, R. B. Barreiro, Serge Gratton, J.-M. Delouis, Jacques Delabrouille, Gianluca Morgante, J.-M. Lamarre, Jan Tauber, François Levrier, M. Reinecke, B. P. Crill, Anthony Lasenby, Charles R. Lawrence, B. Van Tent, F. K. Hansen, Yin-Zhe Ma, Douglas Scott, M. Le Jeune, Hannu Kurki-Suonio, Fabio Finelli, L. A. Montier, N. Bartolo, Franz Elsner, M. Tomasi, Martin Kunz, V. Lindholm, Mathieu Remazeilles, Ken Ganga, Andrea Zacchei, P. Vielva, Ted Kisner, Krzysztof M. Gorski, G. Polenta, G. Roudier, E. Di Valentino, A. Marcos-Caballero, Diego Molinari, Jon E. Gudmundsson, Marco Bersanelli, A. De Rosa, Jason D. McEwen, G. Maggio, B. Ruiz-Granados, A.-S. Suur-Uski, François R. Bouchet, John Bond, Carlo Burigana, Nicoletta Krachmalnicoff, A. A. Fraisse, Mario Ballardini, Enrique Martínez-González, Daniela Paoletti, Locke D. Spencer, George Efstathiou, Andrei V. Frolov, N. Mauri, A. J. Banday, Karim Benabed, S. Dusini, Andrea Zonca, P. B. Lilje, H. C. Chiang, J. Kim, Reijo Keskitalo, Jussi Valiviita, M. Maris, P. Carvalho, Martina Gerbino, J. F. Macías-Pérez, Graca Rocha, S. Basak, D. Tavagnacco, A. Moneti, Mario G. Lattanzi, Jörg P. Rachen, J.-L. Puget, Sabino Matarrese, D. Herranz, B. Partridge, Universidad de Cantabria, Ministerio de Economía y Competitividad (España), European Commission, Consejo Superior de Investigaciones Científicas (España), Astrophysique, Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut de recherche en astrophysique et planétologie (IRAP), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - 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), AstroParticule et Cosmologie (APC (UMR_7164)), 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)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université de Brest (UBO), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), 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), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Planck, Université Paris sciences et lettres (PSL), Cavendish Laboratory, University of Cambridge [UK] (CAM), 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), SISSA MathLab [Trieste], University of the Western Cape, Instituto de Física de Cantabria (IFCA), Universidad de Cantabria [Santander]-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Dipartimento di Fisica e Astronomia 'Galileo Galilei', Universita degli Studi di Padova, Indian Institute of Science Education and Research Thiruvananthapuram (IISER TVM), Università degli Studi di Milano [Milano] (UNIMI), Canadian Institute for Theoretical Astrophysics (CITA), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Dipartimento di Fisica e Scienze della Terra [Ferrara], Università degli Studi di Ferrara (UniFE), Istituto di Radioastronomia [Bologna] (IRA), Istituto Nazionale di Astrofisica (INAF), Universidade Federal de Mato Grosso (UFMT), Algorithmes Parallèles et Optimisation (IRIT-APO), Institut de recherche en informatique de Toulouse (IRIT), Université Toulouse 1 Capitole (UT1), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse - Jean Jaurès (UT2J)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse 1 Capitole (UT1), Université Fédérale Toulouse Midi-Pyrénées, Institut National Polytechnique (Toulouse) (Toulouse INP), Princeton University, Oskar Klein Centre [Stockholm], Stockholm University, Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), European Space Astronomy Centre (ESAC), European Space Agency (ESA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Helsinki Institute of Physics (HIP), University of Helsinki, Aalto University, University of British Columbia (UBC), Istituto Nazionale di Fisica Nucleare, Sezione di Bologna (INFN, Sezione di Bologna), Istituto Nazionale di Fisica Nucleare (INFN), Cardiff University, European Space Research and Technology Centre (ESTEC), INAF - Osservatorio Astronomico di Trieste (OAT), Universidad de Oviedo [Oviedo], Istituto Nazionale di Fisica Nucleare [Ferrara] (INFN), Univ Helsinki, Dept Phys, Gustaf Hallstromin Katu 2a,POB 64, FI-00014 Helsinki, Finland, Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Basque Centre for Climate Change (BC3), Institute of Theoretical Astrophysics [Oslo], University of Oslo (UiO), San Diego Supercomputer Center [San Diego], NASA (USA), Planck Collaboration, European Project, 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., Gonzalez-Nuevo J., Gorski 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., Keihanen 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., Levrier F., Lilje P.B., Lindholm V., Lopez-Caniego M., Ma Y.-Z., Macias-Perez J.F., Maggio G., Mandolesi N., Marcos-Caballero A., Maris M., Martin P.G., Martinez-Gonzalez 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., École normale supérieure - Paris (ENS-PSL), 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), University of the Western Cape (UWC), Università degli Studi di Padova = University of Padua (Unipd), Università degli Studi di Milano = University of Milan (UNIMI), Università degli Studi di Ferrara = University of Ferrara (UniFE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université Toulouse Capitole (UT Capitole), Université de Toulouse (UT)-Université de Toulouse (UT)-Université Toulouse - Jean Jaurès (UT2J), Université de Toulouse (UT)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université de Toulouse (UT)-Toulouse Mind & Brain Institut (TMBI), Université Toulouse - Jean Jaurès (UT2J), Université de Toulouse (UT)-Université de Toulouse (UT)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université Toulouse Capitole (UT Capitole), Université de Toulouse (UT), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Laboratoire de physique de l'ENS - ENS Paris (LPENS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Agence Spatiale Européenne = European Space Agency (ESA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Helsingin yliopisto = Helsingfors universitet = University of Helsinki, Department of Physics, Helsinki Institute of Physics, Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), and Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris)
Subjects: Submillimeter: general, Cosmology and Nongalactic Astrophysics (astro-ph.CO), astro-ph.GA, Astronomy, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, general [Submillimeter], 7. Clean energy, 01 natural sciences, Cosmology: observation, NO, symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, Catalogs, Cosmology: observations, Submillimeter: general, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Aerospace engineering, Planck, observations [Cosmology], 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Reliability (statistics), Astrophysics::Galaxy Astrophysics, Physics, HERSCHEL, 010308 nuclear & particles physics, business.industry, PE9_14, COMPONENTS, Cosmology: observations, Astronomy and Astrophysics, 115 Astronomy, Space science, Catalogs, Astrophysics - Astrophysics of Galaxies, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), symbols, astro-ph.CO, Catalog, CLUSTERS, business, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], astro-ph.IM, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Planck Collaboration: et al., 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; the Herschel GAMA15-field catalogue; and the temperature- and spectral-index-reconstructed dust maps obtained with Planck’s Generalized Needlet Internal Linear Combination method. The results of the BeeP extension of PCCS2, which are made publicly available via the Planck Legacy Archive, will enable the study of the thermal properties of well-defined samples of compact Galactic and extragalactic dusty sources., The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and ERC and PRACE (EU).
Published: 2020

30. Planck 2018 results. VI. Cosmological parameters

Author: M. López-Caniego, Richard A. Battye, Hannu Kurki-Suonio, J. Aumont, Charles R. Lawrence, P. Vielva, E. Martínez-González, François R. Bouchet, L. Montier, K. Ganga, Francesca Perrotta, Lloyd Knox, M. Le Jeune, Jan Hamann, E. Franceschi, M. Tenti, C. Combet, Torsten A. Enßlin, Andrea Zacchei, R. A. Sunyaev, J.-M. Delouis, J. F. Macías-Pérez, Tiziana Trombetti, Zhiqi Huang, Graca Rocha, L. Polastri, Alessandro Melchiorri, A. Mennella, Nabila Aghanim, Sabino Matarrese, Jose Alberto Rubino-Martin, N. Bartolo, Theodore Kisner, Peter Meinhold, L. Salvati, Jose M. Diego, K. Benabed, J.-P. Bernard, J. González-Nuevo, M. Ashdown, H. K. Eriksen, Erminia Calabrese, Olivier Doré, Serge Gratton, G. de Zotti, L. Vibert, J. R. Bond, Marzieh Farhang, Benjamin D. Wandelt, Julian Borrill, L. Toffolatti, F. Piacentini, Yin-Zhe Ma, Will Handley, S. Galeotta, A. Karakci, A. A. Fraisse, Anthony Lasenby, M. Sandri, X. Dupac, G. Sirri, Adam Moss, B. Ruiz-Granados, D. Contreras, A.-S. Suur-Uski, Mario G. Lattanzi, Ricardo Genova-Santos, Jean-François Cardoso, Marian Douspis, G. Polenta, E. Keihänen, A. J. Banday, M. Migliaccio, R. B. Barreiro, B. P. Crill, J. Valiviita, Yabebal Fantaye, B. Van Tent, Tuhin Ghosh, D. Tavagnacco, A. Renzi, Martin White, M. Bucher, Douglas Scott, Jörg P. Rachen, Hans Ulrik Nørgaard-Nielsen, Jason D. McEwen, R. C. Butler, Locke D. Spencer, Nicola Vittorio, V. Lindholm, Fabrizio Villa, K. Kiiveri, Ingunn Kathrine Wehus, Julien Lesgourgues, Hiranya V. Peiris, Reijo Keskitalo, Krzysztof M. Gorski, S. R. Hildebrandt, E. Di Valentino, A. Marcos-Caballero, G. Patanchon, P. de Bernardis, M. Lilley, Simon D. M. White, C. Sirignano, M. Frailis, Carlo Baccigalupi, Francesco Forastieri, W. C. Jones, P. Lemos, François Levrier, E. Hivon, R. Fernandez-Cobos, Carlo Burigana, Nicoletta Krachmalnicoff, D. Herranz, Andrei V. Frolov, M. Tomasi, Marius Millea, J.-L. Puget, Paolo Natoli, James R. Fergusson, D. Paoletti, L. Pagano, M.-A. Miville-Deschênes, Julien Carron, Luca Valenziano, F. K. Hansen, S. Dusini, Andrea Zonca, Bruce Partridge, Jens Chluba, S. Basak, H. C. Chiang, Alessandro Gruppuso, Marco Bersanelli, Peter G. Martin, Martin Kunz, Valeria Pettorino, Mathieu Remazeilles, Jacques Delabrouille, Jon E. Gudmundsson, J.-M. Lamarre, P. Bielewicz, F. Cuttaia, Franz Elsner, G. Roudier, S. Galli, Michele Liguori, Gianluca Morgante, A. Ducout, Fabio Finelli, James J. Bock, M. Reinecke, C. Rosset, Yashar Akrami, Anthony Challinor, Subhabrata Mitra, J. A. Tauber, Matteo Martinelli, M. Savelainen, N. Mauri, E. P. S. Shellard, Antony Lewis, Diego Molinari, G. Maggio, P. B. Lilje, Davide Maino, A. Mangilli, L. P. L. Colombo, Mario Ballardini, N. Mandolesi, Andrew H. Jaffe, Philip Lubin, J. Kim, M. Maris, Martina Gerbino, George Efstathiou, F. Boulanger, Guilaine Lagache, Challinor, Anthony [0000-0003-3479-7823], Fergusson, James [0000-0003-4820-171X], Handley, William [0000-0002-5866-0445], Lasenby, Anthony [0000-0002-8208-6332], Apollo - University of Cambridge Repository, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), 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), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Institut Lagrange de Paris, Sorbonne Universités, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Planck, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Astrophysique, Laboratoire de physique de l'ENS - ENS Paris (LPENS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), 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), Computing and Mathematical Sciences [Pasadena]], California Institute of Technology (CALTECH), Canadian Institute for Theoretical Astrophysics (CITA), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), 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)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Dipartimento di Fisica [Roma La Sapienza], Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Laboratoire d'Océanographie Physique et Spatiale (LOPS), Institut de Recherche pour le Développement (IRD)-Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Brest (UBO)-Centre National de la Recherche Scientifique (CNRS), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Dipartimento di Fisica 'G. Galilei', Università degli Studi di Padova = University of Padua (Unipd), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), University College of London [London] (UCL), University of Manchester [Manchester], University of British Columbia (UBC), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No 725456, CMBSPEC)., Planck Collaboration, European Project: 616170,EC:FP7:ERC,ERC-2013-CoG,COSMOPARS(2014), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), Sorbonne Université (SU)-Observatoire de Paris, Université Paris-Seine-Université Paris-Seine-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2020-....] (UGA [2020-....])-Institut polytechnique de Grenoble - Grenoble Institute of Technology [2020-....] (Grenoble INP [2020-....]), Université Grenoble Alpes [2020-....] (UGA [2020-....]), Sorbonne Université, 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), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Sud - Paris 11 (UP11), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse III - Paul Sabatier (UT3), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Institut de Recherche pour le Développement (IRD)-Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER)-Université de Brest (UBO)-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), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Universita degli Studi di Padova, Sorbonne Université (SU), Science and Technology Facilities Council (STFC), Science and Technology Facilities Council, Universidad de Cantabria, Ministerio de Economía y Competitividad (España), Consejo Superior de Investigaciones Científicas (España), European Commission, European Research Council, European Space Agency, Department of Physics, Helsinki Institute of Physics, 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)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Aghanim N., Akrami Y., Ashdown M., Aumont J., Baccigalupi C., Ballardini M., Banday A.J., Barreiro R.B., Bartolo N., Basak S., Battye R., Benabed K., Bernard J.-P., Bersanelli M., Bielewicz P., Bock J.J., Bond J.R., Borrill J., Bouchet F.R., Boulanger F., Bucher M., Burigana C., Butler R.C., Calabrese E., Cardoso J.-F., Carron J., Challinor A., Chiang H.C., Chluba J., Colombo L.P.L., Combet C., Contreras D., Crill B.P., Cuttaia F., De Bernardis P., De Zotti G., Delabrouille J., Delouis J.-M., Di Valentino E., Diego J.M., Dore O., Douspis M., Ducout A., Dupac X., Dusini S., Efstathiou G., Elsner F., Ensslin T.A., Eriksen H.K., Fantaye Y., Farhang M., Fergusson J., Fernandez-Cobos R., Finelli F., Forastieri F., Frailis M., Fraisse A.A., Franceschi E., Frolov A., Galeotta S., Galli S., Ganga K., Genova-Santos R.T., Gerbino M., Ghosh T., Gonzalez-Nuevo J., Gorski K.M., Gratton S., Gruppuso A., Gudmundsson J.E., Hamann J., Handley W., Hansen F.K., Herranz D., Hildebrandt S.R., Hivon E., Huang Z., Jaffe A.H., Jones W.C., Karakci A., Keihanen E., Keskitalo R., Kiiveri K., Kim J., Kisner T.S., Knox L., Krachmalnicoff N., Kunz M., Kurki-Suonio H., Lagache G., Lamarre J.-M., Lasenby A., Lattanzi M., Lawrence C.R., Le Jeune M., Lemos P., Lesgourgues J., Levrier F., Lewis A., Liguori M., Lilje P.B., Lilley M., Lindholm V., Lopez-Caniego M., Lubin P.M., Ma Y.-Z., Macias-Perez J.F., Maggio G., Maino D., Mandolesi N., Mangilli A., Marcos-Caballero A., Maris M., Martin P.G., Martinelli M., Martinez-Gonzalez E., Matarrese S., Mauri N., McEwen J.D., Meinhold P.R., Melchiorri A., Mennella A., Migliaccio M., Millea M., Mitra S., Miville-Deschenes M.-A., Molinari D., Montier L., Morgante G., Moss A., Natoli P., Norgaard-Nielsen H.U., Pagano L., Paoletti D., Partridge B., Patanchon G., Peiris H.V., Perrotta F., Pettorino V., Piacentini F., Polastri L., Polenta G., Puget J.-L., Rachen J.P., Reinecke M., Remazeilles M., Renzi A., Rocha G., Rosset C., Roudier G., Rubino-Martin J.A., Ruiz-Granados B., Salvati L., Sandri M., Savelainen M., Scott D., Shellard E.P.S., Sirignano C., Sirri G., Spencer L.D., Sunyaev R., Suur-Uski A.-S., Tauber J.A., Tavagnacco D., Tenti M., Toffolatti L., Tomasi M., Trombetti T., Valenziano L., Valiviita J., Van Tent B., Vibert L., Vielva P., Villa F., Vittorio N., Wandelt B.D., Wehus I.K., White M., White S.D.M., Zacchei A., and Zonca A.
Subjects: cosmological model, Astronomy, Cosmic microwave background, INFLATIONARY PARADIGM, cosmic background radiation: polarization, Astrophysics, cosmic background radiation, baryon: oscillation: acoustic, 01 natural sciences, 7. Clean energy, Omega, Cosmology, OSCILLATION SPECTROSCOPIC SURVEY, background: geometry, GALAXY REDSHIFT SURVEY, neutrino: mass, dark energy, 010303 astronomy & astrophysics, matter: density, expansion: adiabatic, Physics, Spectral index, cosmological constant, Hubble constant, Settore FIS/05, Cosmic background radiation, Cosmological parameters, ACCURATE HALO-MODEL, statistical analysis: Bayesian, POWER-SPECTRUM, matter: fluctuation, tension, perturbation: scalar, Physical Sciences, symbols, astro-ph.CO, Neutrino, Astrophysics - Cosmology and Nongalactic Astrophysics, Particle physics, data analysis method, Cosmology and Nongalactic Astrophysics (astro-ph.CO), satellite: Planck, Dark matter, FOS: Physical sciences, cosmic background radiation: spectrum, dark matter: density, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, NO, symbols.namesake, power spectrum: scalar, Settore FIS/05 - Astronomia e Astrofisica, gravitation: lens, 0103 physical sciences, 0201 Astronomical and Space Sciences, Planck, cosmological parameters, Astrophysics::Galaxy Astrophysics, Science & Technology, 010308 nuclear & particles physics, baryon: density, Astronomy and Astrophysics, GROWTH-RATE, stability, 115 Astronomy, Space science, cosmic background radiation: temperature, MICROWAVE BACKGROUND ANISOTROPIES, 13. Climate action, Space and Planetary Science, Cosmic background radiation, Cosmological parameters, PROBE WMAP OBSERVATIONS, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], BARYON ACOUSTIC-OSCILLATIONS, Hubble's law, cosmic background radiation: anisotropy
Abstract: Planck Collaboration: et al., arXiv:1807.06209v3, We present cosmological parameter results from the final full-mission Planck measurements of the cosmic microwave background (CMB) anisotropies, combining information from the temperature and polarization maps and the lensing reconstruction. Compared to the 2015 results, improved measurements of large-scale polarization allow the reionization optical depth to be measured with higher precision, leading to significant gains in the precision of other correlated parameters. Improved modelling of the small-scale polarization leads to more robust constraints on many parameters, with residual modelling uncertainties estimated to affect them only at the 0.5σ level. We find good consistency with the standard spatially-flat 6-parameter ΛCDM cosmology having a power-law spectrum of adiabatic scalar perturbations (denoted “base ΛCDM” in this paper), from polarization, temperature, and lensing, separately and in combination. A combined analysis gives dark matter density Ωch2 = 0.120 ± 0.001, baryon density Ωbh2 = 0.0224 ± 0.0001, scalar spectral index ns = 0.965 ± 0.004, and optical depth τ = 0.054 ± 0.007 (in this abstract we quote 68% confidence regions on measured parameters and 95% on upper limits). The angular acoustic scale is measured to 0.03% precision, with 100θ* = 1.0411 ± 0.0003. These results are only weakly dependent on the cosmological model and remain stable, with somewhat increased errors, in many commonly considered extensions. Assuming the base-ΛCDM cosmology, the inferred (model-dependent) late-Universe parameters are: Hubble constant H0 = (67.4 ± 0.5) km s−1 Mpc−1; matter density parameter Ωm = 0.315 ± 0.007; and matter fluctuation amplitude σ8 = 0.811 ± 0.006. We find no compelling evidence for extensions to the base-ΛCDM model. Combining with baryon acoustic oscillation (BAO) measurements (and considering single-parameter extensions) we constrain the effective extra relativistic degrees of freedom to be Neff = 2.99 ± 0.17, in agreement with the Standard Model prediction Neff = 3.046, and find that the neutrino mass is tightly constrained to ∑mν < 0.12 eV. The CMB spectra continue to prefer higher lensing amplitudes than predicted in base ΛCDM at over 2σ, which pulls some parameters that affect the lensing amplitude away from the ΛCDM model; however, this is not supported by the lensing reconstruction or (in models that also change the background geometry) BAO data. The joint constraint with BAO measurements on spatial curvature is consistent with a flat universe, ΩK = 0.001 ± 0.002. Also combining with Type Ia supernovae (SNe), the dark-energy equation of state parameter is measured to be w0 = −1.03 ± 0.03, consistent with a cosmological constant. We find no evidence for deviations from a purely power-law primordial spectrum, and combining with data from BAO, BICEP2, and Keck Array data, we place a limit on the tensor-to-scalar ratio r0.002 < 0.06. Standard big-bang nucleosynthesis predictions for the helium and deuterium abundances for the base-ΛCDM cosmology are in excellent agreement with observations. The Planck base-ΛCDM results are in good agreement with BAO, SNe, and some galaxy lensing observations, but in slight tension with the Dark Energy Survey’s combined-probe results including galaxy clustering (which prefers lower fluctuation amplitudes or matter density parameters), and in significant, 3.6σ, tension with local measurements of the Hubble constant (which prefer a higher value). Simple model extensions that can partially resolve these tensions are not favoured by the Planck data., The Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU).
Published: 2020

31. Planck 2018 results: V. CMB power spectra and likelihoods

Author: Francesca Perrotta, A. A. Fraisse, Torsten A. Enßlin, A. J. Banday, M. Sandri, Yabebal Fantaye, L. Toffolatti, Serge Gratton, Jean-François Cardoso, Jose Alberto Rubino-Martin, Martin Kunz, Mathieu Remazeilles, Yin-Zhe Ma, G. de Zotti, E. Martínez-González, Anthony Lasenby, E. Keihänen, Jon E. Gudmundsson, N. Mandolesi, Andrew H. Jaffe, J.-L. Puget, Philip Lubin, J. Kim, M.-A. Miville-Deschênes, M. Lilley, Charles R. Lawrence, M. Le Jeune, François R. Bouchet, F. K. Hansen, Krzysztof M. Gorski, E. Di Valentino, L. Montier, Mario G. Lattanzi, A. Moneti, Erminia Calabrese, Andrea Zacchei, B. P. Crill, N. Bartolo, B. Van Tent, Locke D. Spencer, E. Franceschi, Ted Kisner, M. Maris, Martina Gerbino, D. Herranz, A. Marcos-Caballero, N. Mauri, Adam Moss, Hannu Kurki-Suonio, M. Tomasi, Sabino Matarrese, Davide Maino, Nicola Vittorio, V. Lindholm, Ricardo Genova-Santos, Reijo Keskitalo, C. Sirignano, Zhiqi Huang, P. Bielewicz, Jörg P. Rachen, Julien Carron, Y. Giraud-Héraud, X. Dupac, K. Ganga, D. Tavagnacco, Tuhin Ghosh, L. Pagano, S. Galeotta, Hans Ulrik Nørgaard-Nielsen, L. Salvati, Marco Bersanelli, B. Partridge, Jose M. Diego, M. Reinecke, A. Renzi, Ingunn Kathrine Wehus, Benjamin D. Wandelt, Julian Borrill, Will Handley, S. Basak, Andrei V. Frolov, Marian Douspis, Rashid Sunyaev, G. Sirri, F. Piacentini, S. Dusini, Andrea Zonca, H. C. Chiang, S. Galli, Guillaume Patanchon, M. Migliaccio, Jan Hamann, P. B. Lilje, M. Bucher, O. Doré, Paolo Natoli, Douglas Scott, R. Fernandez-Cobos, F. Cuttaia, Hiranya V. Peiris, M. Tenti, James J. Bock, Peter G. Martin, Valeria Pettorino, Gianluca Morgante, Tiziana Trombetti, Jacques Delabrouille, E. P. S. Shellard, R. B. Barreiro, Alessandro Melchiorri, Antony Lewis, R. C. Butler, K. Kiiveri, J. F. Macías-Pérez, C. Combet, Fabio Finelli, Diego Molinari, G. Maggio, A. Mangilli, Graca Rocha, Fabrizio Villa, J.-P. Bernard, M. Frailis, Carlo Baccigalupi, W. C. Jones, Nabila Aghanim, François Levrier, L. P. L. Colombo, Marius Millea, Eric Hivon, Mario Ballardini, D. Paoletti, Franz Elsner, George Efstathiou, C. Rosset, G. Roudier, Alessandro Gruppuso, Michele Liguori, A. Mennella, Yashar Akrami, Anthony Challinor, J.-M. Lamarre, A. Ducout, J. A. Tauber, M. Savelainen, F. Boulanger, P. Vielva, Guilaine Lagache, M. López-Caniego, P. de Bernardis, B. Casaponsa, B. Ruiz-Granados, A.-S. Suur-Uski, J. Valiviita, J. Aumont, J.-M. Delouis, M. Ashdown, H. K. Eriksen, G. Polenta, Peter Meinhold, J. González-Nuevo, K. Benabed, J. R. Bond, A. De Rosa, Jason D. McEwen, Carlo Burigana, Nicoletta Krachmalnicoff, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Astrophysique, Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université (SU)-Université Paris Diderot - Paris 7 (UPD7)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université (SU)-Université Paris Diderot - Paris 7 (UPD7), Institut de recherche en astrophysique et planétologie (IRAP), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - 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), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), 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)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2020-....] (UGA [2020-....])-Institut polytechnique de Grenoble - Grenoble Institute of Technology [2020-....] (Grenoble INP [2020-....]), Université Grenoble Alpes [2020-....] (UGA [2020-....]), Université de Brest (UBO), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Institut Lagrange de Paris, Sorbonne Université, 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), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Planck, Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse III - Paul Sabatier (UT3), 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), Sorbonne Universités, Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Universidad de Cantabria, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), 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), Computing and Mathematical Sciences [Pasadena]], California Institute of Technology (CALTECH), Canadian Institute for Theoretical Astrophysics (CITA), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Dipartimento di Fisica [Roma La Sapienza], Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Laboratoire d'Océanographie Physique et Spatiale (LOPS), Institut de Recherche pour le Développement (IRD)-Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER)-Université de Brest (UBO)-Centre National de la Recherche Scientifique (CNRS), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Dipartimento di Fisica 'G. Galilei', Universita degli Studi di Padova, Sorbonne Université (SU), University College of London [London] (UCL), University of Manchester [Manchester], University of British Columbia (UBC), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Planck Collaboration, Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-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 national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), 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), 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), Aghanim N., 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., Bock J.J., Bond J.R., Borrill J., Bouchet F.R., Boulanger F., Bucher M., Burigana C., Butler R.C., Calabrese E., Cardoso J.-F., Carron J., Casaponsa B., Challinor A., Chiang H.C., Colombo L.P.L., Combet C., Crill B.P., Cuttaia F., De Bernardis P., De Rosa A., De Zotti G., Delabrouille J., Delouis J.-M., Di Valentino E., Diego J.M., Dore O., Douspis M., Ducout A., Dupac X., Dusini S., Efstathiou G., Elsner F., Ensslin T.A., Eriksen H.K., Fantaye Y., Fernandez-Cobos R., Finelli F., Frailis M., Fraisse A.A., Franceschi E., Frolov A., Galeotta S., Galli S., Ganga K., Genova-Santos R.T., Gerbino M., Ghosh T., Giraud-Heraud Y., Gonzalez-Nuevo J., Gorski K.M., Gratton S., Gruppuso A., Gudmundsson J.E., Hamann J., Handley W., Hansen F.K., Herranz D., Hivon E., Huang Z., Jaffe A.H., Jones W.C., Keihanen E., Keskitalo R., Kiiveri K., Kim J., Kisner T.S., Krachmalnicoff N., Kunz M., Kurki-Suonio H., Lagache G., Lamarre J.-M., Lasenby A., Lattanzi M., Lawrence C.R., Le Jeune M., Levrier F., Lewis A., Liguori M., Lilje P.B., Lilley M., Lindholm V., Lopez-Caniego M., Lubin P.M., Ma Y.-Z., Macias-Perez J.F., Maggio G., Maino D., Mandolesi N., Mangilli A., Marcos-Caballero A., Maris M., Martin P.G., Martinez-Gonzalez E., Matarrese S., Mauri N., McEwen J.D., Meinhold P.R., Melchiorri A., Mennella A., Migliaccio M., Millea M., Miville-Deschenes M.-A., Molinari D., Moneti A., Montier L., Morgante G., Moss A., Natoli P., Norgaard-Nielsen H.U., Pagano L., Paoletti D., Partridge B., Patanchon G., Peiris H.V., Perrotta F., Pettorino V., Piacentini F., Polenta G., Puget J.-L., Rachen J.P., Reinecke M., Remazeilles M., Renzi A., Rocha G., Rosset C., Roudier G., Rubino-Martin J.A., Ruiz-Granados B., Salvati L., Sandri M., Savelainen M., Scott D., Shellard E.P.S., Sirignano C., Sirri G., Spencer L.D., Sunyaev R., 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., Vittorio N., Wandelt B.D., Wehus I.K., Zacchei A., Zonca A., Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire de physique de l'ENS - ENS Paris (LPENS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, 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), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Institut de Recherche pour le Développement (IRD)-Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Brest (UBO)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Padova = University of Padua (Unipd), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Department of Physics, Helsinki Institute of Physics, Ministerio de Economía y Competitividad (España), Consejo Superior de Investigaciones Científicas (España), European Commission, European Research Council, and European Space Agency
Subjects: Cosmological parameter, POLARIZATION, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astronomy, Cosmic microwave background, Cosmological parameters, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astronomy & Astrophysics, Residual, Cosmic background radiation, Cosmology: observation, 01 natural sciences, 7. Clean energy, Spectral line, NO, symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, Methods: data analysis, 0103 physical sciences, 0201 Astronomical and Space Sciences, Cosmology: observations, Statistical physics, MICROWAVE, Planck, observations [Cosmology], data analysis [Methods], 010303 astronomy & astrophysics, Reionization, Cosmic background radiation, Cosmological parameters, Cosmology: observations, Methods: data analysis, Physics, 010308 nuclear & particles physics, Spectral density, Astronomy and Astrophysics, 115 Astronomy, Space science, Polarization (waves), 13. Climate action, Space and Planetary Science, PROBE WMAP OBSERVATIONS, symbols, astro-ph.CO, SKY, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Smoothing, APPROXIMATION, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Planck Collaboration: et al., We describe the legacy Planck cosmic microwave background (CMB) likelihoods derived from the 2018 data release. The overall approach is similar in spirit to the one retained for the 2013 and 2015 data release, with a hybrid method using different approximations at low (ℓ < 30) and high (ℓ ≥ 30) multipoles, implementing several methodological and data-analysis refinements compared to previous releases. With more realistic simulations, and better correction and modelling of systematic effects, we can now make full use of the CMB polarization observed in the High Frequency Instrument (HFI) channels. The low-multipole EE cross-spectra from the 100 GHz and 143 GHz data give a constraint on the ΛCDM reionization optical-depth parameter τ to better than 15% (in combination with the TT low-ℓ data and the high-ℓ temperature and polarization data), tightening constraints on all parameters with posterior distributions correlated with τ. We also update the weaker constraint on τ from the joint TEB likelihood using the Low Frequency Instrument (LFI) channels, which was used in 2015 as part of our baseline analysis. At higher multipoles, the CMB temperature spectrum and likelihood are very similar to previous releases. A better model of the temperature-to-polarization leakage and corrections for the effective calibrations of the polarization channels (i.e., the polarization efficiencies) allow us to make full use of polarization spectra, improving the ΛCDM constraints on the parameters θMC, ωc, ωb, and H0 by more than 30%, and ns by more than 20% compared to TT-only constraints. Extensive tests on the robustness of the modelling of the polarization data demonstrate good consistency, with some residual modelling uncertainties. At high multipoles, we are now limited mainly by the accuracy of the polarization efficiency modelling. Using our various tests, simulations, and comparison between different high-multipole likelihood implementations, we estimate the consistency of the results to be better than the 0.5 σ level on the ΛCDM parameters, as well as classical single-parameter extensions for the joint likelihood (to be compared to the 0.3 σ levels we achieved in 2015 for the temperature data alone on ΛCDM only). Minor curiosities already present in the previous releases remain, such as the differences between the best-fit ΛCDM parameters for the ℓ < 800 and ℓ > 800 ranges of the power spectrum, or the preference for more smoothing of the power-spectrum peaks than predicted in ΛCDM fits. These are shown to be driven by the temperature power spectrum and are not significantly modified by the inclusion of the polarization data. Overall, the legacy Planck CMB likelihoods provide a robust tool for constraining the cosmological model and represent a reference for future CMB observations., The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and ERC and PRACE (EU).
Published: 2020

32. Fundamental physics with the Square Kilometre Array

Author: Amanda Weltman, Mairi Sakellariadou, Francesca Vidotto, Laura Wolz, M. Méndez-Isla, Hamsa Padmanabhan, Ian Harrison, Jose A. R. Cembranos, Roy Maartens, Philip Bull, R. M. T. Connors, Alkistis Pourtsidou, Chris Clarkson, Peter K. S. Dunsby, A. de la Cruz-Dombriz, Céline Bœhm, Christoph Weniger, Tejaswi Venumadhav, T. Trombetti, Stefano Camera, Katharine Kelley, Signe Riemer-Sørensen, Gianfranco Bertone, J. Silk, Bryan Gaensler, Carlo Burigana, Marcus Brüggen, Julien Larena, Peter J. Quinn, Franco Vazza, Francisco Villaescusa-Navarro, Camille Bonvin, Martin Sahlén, Lijing Shao, Daniele Gaggero, Rennan Barkana, Albert Bosma, Soumya D. Mohanty, Yin-Zhe Ma, Sambatra Andrianomena, Nicolao Fornengo, Alvise Raccanelli, E. Athanassoula, Steven G. Murray, Yue-Fei Wang, José Fonseca, Jonathan R. Pritchard, Fupeng Zhang, David Parkinson, David Bacon, Francesca Calore, Marco Regis, Prasenjit Saha, Ministerio de Economía y Competitividad (España), 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), Laboratoire d'Annecy-le-Vieux de Physique Théorique (LAPTH), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), 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), 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), Weltman, A., Bull, P., Camera, S., Kelley, K., Padmanabhan, H., Pritchard, J., Raccanelli, A., Riemer-Sørensen, S., Shao, L., Andrianomena, S., Athanassoula, E., Bacon, D., Barkana, R., Bertone, G., Bœhm, C., Bonvin, C., Bosma, A., Brüggen, M., Burigana, C., Calore, F., Cembranos, J. A. R., Clarkson, C., Connors, R. M. T., Cruz-Dombriz, Á. de la, Dunsby, P. K. S., Fonseca, J., Fornengo, N., Gaggero, D., Harrison, I., Larena, J., Ma, Y.-Z., Maartens, R., Méndez-Isla, M., Mohanty, S. D., Murray, S., Parkinson, D., Pourtsidou, A., Quinn, P. J., Regis, M., Saha, P., Sahlén, M., Sakellariadou, M., Silk, J., Trombetti, T., Vazza, F., Venumadhav, T., Vidotto, F., Villaescusa-Navarro, F., Wang, Y., Weniger, C., Wolz, L., Zhang, F., Gaensler, B. M., 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)), Commission of the European Communities, and 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)
Subjects: Astrofísica, PULSAR-TIMING PACKAGE, cosmological model, gravitation: model, Astrophysics, 01 natural sciences, Cosmology, SAGITTARIUS-A-ASTERISK, STRONG-FIELD TESTS, High Energy Physics - Phenomenology (hep-ph), CMB SPECTRAL DISTORTIONS, dark energy, 010303 astronomy & astrophysics, pulsar, Physics, COSMIC cancer database, astroparticle physics, cosmology, gravitation, pulsars: general, reionisation, telescopes, ST/L000326/1, Astrophysics::Instrumentation and Methods for Astrophysics, POWER-SPECTRUM, hep-ph, SUPERMASSIVE BLACK-HOLE, High Energy Physics - Phenomenology, Computer Science::Graphics, Physics::Space Physics, Physical Sciences, astro-ph.CO, MILKY-WAY, galaxy: cluster, Astrophysics::Earth and Planetary Astrophysics, GALACTIC SYNCHROTRON EMISSION, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Gravitation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 0299 Other Physical Sciences, interferometer, Dark matter, general [Pulsars], FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, WARM DARK-MATTER, dark matter, Radio telescope, galaxy: formation, 0103 physical sciences, 0201 Astronomical and Space Sciences, ionization, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), STFC, Astroparticle physics, Science & Technology, 010308 nuclear & particles physics, Gravitational wave, RCUK, Astronomy and Astrophysics, Galaxy, gravitational radiation detector, NEUTRAL HYDROGEN, detector: sensitivity, Cosmology and Nongalactic Astrophysics, Square Kilometer Array, general, Space and Planetary Science, gravitational radiation: emission, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Dark energy, pulsars, ST/N000668/1, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], astro-ph.IM
Abstract: Square Kilometre Array: et al., arXiv:1810.02680v3, The Square Kilometre Array (SKA) is a planned large radio interferometer designed to operate over a wide range of frequencies, and with an order of magnitude greater sensitivity and survey speed than any current radio telescope. The SKA will address many important topics in astronomy, ranging from planet formation to distant galaxies. However, in this work, we consider the perspective of the SKA as a facility for studying physics. We review four areas in which the SKA is expected to make major contributions to our understanding of fundamental physics: cosmic dawn and reionisation; gravity and gravitational radiation; cosmology and dark energy; and dark matter and astroparticle physics. These discussions demonstrate that the SKA will be a spectacular physics machine, which will provide many new breakthroughs and novel insights on matter, energy, and spacetime., A. Racanelli has received funding from the People Programme (Marie Curie Actions) of the European Union H2020 Programme under REA grant agreement number 706896 (COSMOFLAGS). Funding for this work was partially provided by the Spanish MINECO under MDM-2014-0369 of ICCUB (Unidad de Excelencia ‘Maria de Maeztu’).
Published: 2020

33. Constraining the optical depth of galaxies and velocity bias with cross-correlation between the kinetic Sunyaev–Zeldovich effect and the peculiar velocity field

Author: Ning Sui, Ping He, Yin-Zhe Ma, and Guo-Dong Gong
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Field (physics), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Function (mathematics), Astrophysics, Correlation function (quantum field theory), Kinetic energy, 01 natural sciences, Galaxy, Space and Planetary Science, 0103 physical sciences, Optical depth (astrophysics), Peculiar velocity, Group velocity, Atomic physics, 010306 general physics, 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We calculate the cross-correlation function $\langle (\Delta T/T)(\mathbf{v}\cdot \mathbf{n}/\sigma_{v}) \rangle$ between the kinetic Sunyaev-Zeldovich (kSZ) effect and the reconstructed peculiar velocity field using linear perturbation theory, to constrain the optical depth $\tau$ and peculiar velocity bias of central galaxies with Planck data. We vary the optical depth $\tau$ and the velocity bias function $b_{v}(k)=1+b(k/k_{0})^{n}$, and fit the model to the data, with and without varying the calibration parameter $y_{0}$ that controls the vertical shift of the correlation function. By constructing a likelihood function and constraining $\tau$, $b$ and $n$ parameters, we find that the quadratic power-law model of velocity bias $b_{v}(k)=1+b(k/k_{0})^{2}$ provides the best-fit to the data. The best-fit values are $\tau=(1.18 \pm 0.24) \times 10^{-4}$, $b=-0.84^{+0.16}_{-0.20}$ and $y_{0}=(12.39^{+3.65}_{-3.66})\times 10^{-9}$ ($68\%$ confidence level). The probability of $b>0$ is only $3.12 \times 10^{-8}$ for the parameter $b$, which clearly suggests a detection of scale-dependent velocity bias. The fitting results indicate that the large-scale ($k \leq 0.1\,h\,{\rm Mpc}^{-1}$) velocity bias is unity, while on small scales the bias tends to become negative. The value of $\tau$ is consistent with the stellar mass--halo mass and optical depth relation proposed in the previous literatures, and the negative velocity bias on small scales is consistent with the peak background-split theory. Our method provides a direct tool to study the gaseous and kinematic properties of galaxies., Comment: 13 pages, 13 figures, 3 tables
Published: 2018

34. Research and Development for HI Intensity Mapping

Author: David Rapetti, Zeeshan Ahmed, Philip Bull, Kavilan Moodley, Lloyd Knox, Moritz Münchmeyer, Laura Newburgh, Alexander A. Kaurov, Joshua S. Dillon, Erin S. Sheldon, Dionysios Karagiannis, Adrian Liu, Daniel C. Jacobs, Evan J. Arena, Paul O'Connor, J. Richard Shaw, Simon Foreman, Kiyoshi Masui, Neelima Sehgal, Peter T. Timbie, Andrei Nomerotski, Dan Green, Tzu-Ching Chang, Alexander van Engelen, Olivier Perdereau, Adam P. Beardsley, Emanuele Castorina, Albert Stebbins, Aaron Ewall-Wice, Simone Ferraro, David Alonso, Paul Stankus, Chris Sheehy, Emily Kuhn, Benjamin Saliwanchik, Gilbert Holder, Kevin Bandura, Thomas McClintock, Tracy R. Slatyer, Dallas Wulf, Romeel Davé, Eva Silverstein, Yin-Zhe Ma, Francisco Villaescusa-Navarro, Anže Slosar, David Parkinson, William Tyndall, Josef Frisch, Gregory S. Tucker, Hamsa Padmanabhan, Reza Ansari, Andrej Obuljen, R. Shirley, and Mustafa A. Amin
Subjects: Physics, 010308 nuclear & particles physics, 0103 physical sciences, Intensity mapping, Hydrogen line, Astronomy, Development (differential geometry), 7. Clean energy, 01 natural sciences
Abstract: The paper outlines research and development needed over the next decade to enable three-dimension mapping of the Universe using the 21 cm line of neutral hydrogen.
Published: 2019

35. Packed Ultra-wideband Mapping Array (PUMA): A Radio Telescope for Cosmology and Transients

Author: Surjeet Rajendran, Emmanuel Schaan, Albert Stebbins, Thomas McClintock, Andrej Obuljen, Joshua S. Dillon, Simone Ferraro, J. Xavier Prochaska, Moritz Münchmeyer, R. Shirley, J. Richard Shaw, Kavilan Moodley, Marilena LoVerde, Cherry Ng, Francisco Villaescusa Navarro, Tzu-Ching Chang, Laura Newburgh, Nicholas Battaglia, David Rapetti, Anze Slosar, Lloyd Knox, Liam Connor, Jonathan Blazek, Eva Silverstein, Zeeshan Ahmed, Hamsa Padmanabhan, Erin S. Sheldon, Cora Dvorkin, Daniel C. Jacobs, Raphael Flauger, Evan J. Arena, Benjamin Saliwanchik, Gilbert Holder, Philip Bull, David Parkinson, Chris Sheehy, Benjamin Wallisch, Mustafa A. Amin, Dan Green, Tracy R. Slatyer, Josef Frisch, Alexander A. Kaurov, Dionysios Karagiannis, Peter T. Timbie, David Alonso, Emanuele Castorina, Kiyoshi Masui, Romeel Davé, Gregory S. Tucker, William Tyndall, Kevin Bandura, Adrian Liu, Paul O'Connor, Alexander van Engelen, Paul Stankus, Simon Foreman, Andrei Nomerotski, Matthew C. Johnson, Yin-Zhe Ma, Neelima Sehgal, and Martin White
Subjects: Physics, 010308 nuclear & particles physics, Intensity mapping, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Redshift, Galaxy, Cosmology, law.invention, Radio telescope, Telescope, law, 0103 physical sciences, Dark energy, 010303 astronomy & astrophysics, Noise (radio)
Abstract: PUMA is a proposal for an ultra-wideband, low-resolution and transit interferometric radio telescope operating at $200-1100\,\mathrm{MHz}$. Its design is driven by six science goals which span three science themes: the physics of dark energy (measuring the expansion history and growth of the universe up to $z=6$), the physics of inflation (constraining primordial non-Gaussianity and primordial features) and the transient radio sky (detecting one million fast radio bursts and following up SKA-discovered pulsars). We propose two array configurations composed of hexagonally close-packed 6m dish arrangements with 50% fill factor. The initial 5,000 element 'petite array' is scientifically compelling, and can act as a demonstrator and a stepping stone to the full 32,000 element 'full array'. Viewed as a 21cm intensity mapping telescope, the program has the noise equivalent of a traditional spectroscopic galaxy survey comprised of 0.6 and 2.5 billion galaxies at a comoving wavenumber of $k=0.5\,h\mathrm{Mpc}^{-1}$ spanning the redshift range $z = 0.3 - 6$ for the petite and full configurations, respectively. At redshifts beyond $z=2$, the 21cm technique is a uniquely powerful way of mapping the universe, while the low-redshift range will allow for numerous cross-correlations with existing and upcoming surveys. This program is enabled by the development of ultra-wideband radio feeds, cost-effective dish construction methods, commodity radio-frequency electronics driven by the telecommunication industry and the emergence of sufficient computing power to facilitate real-time signal processing that exploits the full potential of massive radio arrays. The project has an estimated construction cost of 55 and 330 million FY19 USD for the petite and full array configurations. Including R&D, design, operations and science analysis, the cost rises to 125 and 600 million FY19 USD, respectively.
Published: 2019

36. A Search for Warm/Hot Gas Filaments Between Pairs of SDSS Luminous Red Galaxies

Author: Hideki Tanimura, Tilman Tröster, Nabila Aghanim, Gary Hinshaw, Alexander Mead, Yin-Zhe Ma, Ian G. McCarthy, Ludovic Van Waerbeke, Alireza Hojjati, Institut d'astrophysique spatiale (IAS), and Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Monte Carlo method, FOS: Physical sciences, Electron, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, galaxies: groups: general, 0103 physical sciences, 010303 astronomy & astrophysics, Scaling, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Null (mathematics), Astronomy and Astrophysics, Radius, Galaxy, galaxies: haloes, Space and Planetary Science, galaxies: clusters: general, Product (mathematics), astro-ph.CO, Halo, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We search the Planck data for a thermal Sunyaev-Zel'dovich (tSZ) signal due to gas filaments between pairs of Luminous Red Galaxies (LRG's) taken from the Sloan Digital Sky Survey Data Release 12 (SDSS/DR12). We identify $\sim$260,000 LRG pairs in the DR12 catalog that lie within 6-10 $h^{-1} \mathrm{Mpc}$ of each other in tangential direction and within 6 $h^{-1} \mathrm{Mpc}$ in radial direction. We stack pairs by rotating and scaling the angular positions of each LRG so they lie on a common reference frame, then we subtract a circularly symmetric halo from each member of the pair to search for a residual signal between the pair members. We find a statistically significant (5.3$\sigma$) signal between LRG pairs in the stacked data with a magnitude $\Delta y = (1.31 \pm 0.25) \times 10^{-8}$. The uncertainty is estimated from two Monte Carlo null tests which also establish the reliability of our analysis. Assuming a simple, isothermal, cylindrical filament model of electron over-density with a radial density profile proportional to $r_c/r$ (as determined from simulations), where $r$ is the perpendicular distance from the cylinder axis and $r_c$ is the core radius of the density profile, we constrain the product of over-density and filament temperature to be $\delta_c \times (T_{\rm e}/10^7 \, {\rm K}) \times (r_c/0.5h^{-1} \, {\rm Mpc}) = 2.7 \pm 0.5$. To our knowledge, this is the first detection of filamentary gas at over-densities typical of cosmological large-scale structure. We compare our result to the BAHAMAS suite of cosmological hydrodynamic simulations (McCarthy et al. 2017) and find a slightly lower, but marginally consistent Comptonization excess, $\Delta y = (0.84 \pm 0.24) \times 10^{-8}$., Comment: 10 pages, 9 figures, accepted for publication in MNRAS (v4 and v5 to include funding acknowledgements. No other changes.)
Published: 2019

37. Energy band modulation of GaAs/Al0.26Ga0.74As quantum well in 3D self-assembled nanomembranes

Author: Honglou Zhen, Fei Zhang, GaoShang Huang, Zhe Ma, Xiaofei Nie, Fei Ding, Zengfeng Di, Yongfeng Mei, and Xin Cao
Subjects: Photoluminescence, Fabrication, Infrared, Stark effect, General Physics and Astronomy, 01 natural sciences, 010305 fluids & plasmas, Strain, symbols.namesake, Nanomembrane, 0103 physical sciences, ddc:530, Quantum well, 010306 general physics, Electronic band structure, Physics, business.industry, Modulation, symbols, Optoelectronics, Energy band, Light emission, Dewey Decimal Classification::500 | Naturwissenschaften::530 | Physik, business
Abstract: In this study, we investigate the modulation of energy band in 3D self-assembled nanomembranes containing GaAs/Al0.26Ga0.74As quantum wells (QWs). Photoluminescence (PL) characterizations demonstrate that the self-assembled structures have different optical transition properties and the modulation of the energy band is thus realized. Detailed spectral analyses disclose that the small strain change in structures with different curvatures cannot cause remarkable change in energy bands in Al0.26Ga0.74As layer. On the other hand, the optical transitions of GaAs QW layer is influenced by the strain evolution in term of light emission intensity. We also find the first order Stark effect in rolled-up nanomembrane with diameter of 150 μm, which is closely connected with the coupling effect between the deformation potential and the piezoelectric potential. Our work may pave a way for the fabrication of high performance rolled-QW infrared photo-detectors.
Published: 2019

38. Searching for HI imprints in cosmic web filaments with 21-cm intensity mapping

Author: Yi-Chao Li, Lister Staveley-Smith, Denis Tramonte, and Yin-Zhe Ma
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Omega, Redshift, Spectral line, Galaxy, Radio telescope, Space and Planetary Science, Brightness temperature, 0103 physical sciences, Intergalactic travel, Absorption (logic), 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We investigate the possible presence of neutral hydrogen (HI) in intergalactic filaments at very low redshift ($z\sim 0.08$), by stacking a set of 274,712 2dFGRS galaxy pairs over 21-cm maps obtained with dedicated observations conducted with the Parkes radio telescope, over a total sky area of approximately 1,300 square degrees covering two patches in the northern and in the southern Galactic hemispheres. The stacking is performed by combining local maps in which each pair is brought to a common reference frame; the resulting signal from the edge galaxies is then removed to extract the filament residual emission. We repeat the analysis on maps cleaned removing either 10 or 20 foreground modes in a principal component analysis. Our study does not reveal any clear HI excess in the considered filaments in either case; we determine upper limits on the total filament HI brightness temperature at $T_{\rm b} \lesssim 10.3 \,\mu\text{K}$ for the 10-mode and at $T_{\rm b} \lesssim 4.8 \,\mu\text{K}$ for the 20-mode removed maps at the 95% confidence level. These estimates translate into upper limits for the local filament HI density parameter, $\Omega_{\rm HI}^{\rm (f)} \lesssim 7.0\times10^{-5}$ and $\Omega_{\rm HI}^{\rm (f)} \lesssim 3.2\times10^{-5}$ respectively, and for the HI column density, $N_{\rm HI} \lesssim 4.6\times10^{15}\,\text{cm}^{-2}$ and $N_{\rm HI} \lesssim 2.1\times10^{15}\,\text{cm}^{-2}$ respectively. These column density constraints are consistent with previous detections of HI in the warm-hot intergalactic medium obtained observing broad Ly $\alpha$ absorption systems. The present work shows for the first time how such constraints can be achieved using the stacking of galaxy pairs on 21-cm maps., Comment: Accepted for publication by MNRAS. 18 pages, 11 figures
Published: 2019
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39. Probing hot gas around luminous red galaxies through the Sunyaev-Zel'dovich effect

Author: Ian G. McCarthy, Ludovic Van Waerbeke, Yin-Zhe Ma, Alireza Hojjati, Hideki Tanimura, Nabila Aghanim, Tilman Tröster, Alexander Mead, Gary Hinshaw, Bruno Moraes, Institut d'astrophysique spatiale (IAS), and Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Active galactic nucleus, galaxies: clusters: intracluster medium, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Sunyaev–Zel'dovich effect, 01 natural sciences, galaxies: groups: general, 0103 physical sciences, 010303 astronomy & astrophysics, QC, Astrophysics::Galaxy Astrophysics, media_common, QB, Physics, 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, Redshift, Galaxy, galaxies: haloes, Gravitational lens, 13. Climate action, Space and Planetary Science, Sky, Halo, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We construct the mean thermal Sunyaev-Zel'dovich (tSZ) Comptonization y profile around Luminous Red Galaxies (LRGs) in the redshift range 0.16 < z < 0.47 from the Sloan Digital Sky Survey (SDSS) Data Release 7 (DR7) using the Planck y map. The mean central tSZ signal for the full sample is y ~ 1.8 * 10^(-7) and we detect tSZ emission out to ~30 arcmin, which is well beyond the 10 arcmin angular resolution of the y map and well beyond the virial radii of the LRGs. We compare the measured profile with predictions from the cosmo-OWLS suite of cosmological hydrodynamical simulations. This comparison agrees well for models that include feedback from active galactic nuclei (AGN), but not with hydrodynamic models without this energetic feedback mechanism. This suggests that an additional heating mechanism is required over SNe feedback and star formation to explain the y data profile. We also compare our results with predictions based on the halo model with a universal pressure profile (UPP) giving the y signal. The predicted profile is consistent with the data, but only if we account for the clustering of haloes via a two-halo term and if halo masses are estimated using the mean stellar-to-halo mass (SHM) relation of Coupon et al. (2015) or Wang et al.(2016) estimated from gravitational lensing measurements. We also discuss the importance of scatter in the SHM relation on the model predictions., 12 pages, 6 figures, accepted by MNRAS
Published: 2019
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40. Probing Diffuse Gas with Fast Radio Bursts

Author: A. Walters, Amanda Weltman, Jonathan Sievers, and Yin-Zhe Ma
Subjects: Physics, Current (mathematics), Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic microwave background, FOS: Physical sciences, Markov chain Monte Carlo, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Cosmology, Redshift, Baryon, symbols.namesake, Supernova, symbols, Baryon acoustic oscillations, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The dispersion measure -- redshift relation of Fast Radio Bursts, $\mathrm{DM}(z)$, has been proposed as a potential new probe of the cosmos, complementary to existing techniques. In practice, however, the effectiveness of this approach depends on a number of factors, including (but not limited to) the intrinsic scatter in the data caused by intervening matter inhomogeneities. Here, we simulate a number of catalogues of mock FRB observations, and use MCMC techniques to forecast constraints, and assess which parameters will likely be best constrained. In all cases we find that any potential improvement in cosmological constraints are limited by the current uncertainty on the the diffuse gas fraction, $f_{\rm d}(z)$. Instead, we find that the precision of current cosmological constraints allows one to constrain $f_{\rm d}(z)$, and possibly its redshift evolution. Combining CMB + BAO + SNe + $H_0$ constraints with just 100 FRBs (with redshifts), we find a typical constraint on the mean diffuse gas fraction of a few percent. A detection of this nature would alleviate the "missing baryon problem", and therefore highlights the value of localisation and spectroscopic followup of future FRB detections., Comment: 11 pages; 3 figues
Published: 2019
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41. Probing galaxy cluster and intra-cluster gas with luminous red galaxies

Author: Yin-Zhe Ma, Yan Gong, Hideki Tanimura, Institut d'astrophysique spatiale (IAS), and Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic background radiation, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, cosmic background radiation, 01 natural sciences, Bin, symbols.namesake, 0103 physical sciences, Thermal, Cluster (physics), Planck, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Space and Planetary Science, galaxies: clusters: general, Astrophysics of Galaxies (astro-ph.GA), symbols, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We use the cross-correlation between the thermal Sunyaev-Zeldovich (tSZ) signal measured by the Planck satellite and the luminous red galaxy (LRG) samples provided by the SDSS DR7 to study the properties of galaxy cluster and intra-cluster gas. We separate the samples into three redshift bins z_1=(0.16, 0.26), z_2=(0.26, 0.36), z_3=(0.36, 0.47), and stack the Planck y-map against LRGs to derive the averaged y-profile for each redshift bin. We then fit the stacked profile with the theoretical prediction from the universal pressure profile (UPP) by using the Markov-Chain Monte-Carlo method. We find that the best-fit values of the UPP parameters for the three bins are generally consistent with the previous studies, except for the noticeable evolution of the parameters in the three redshift bins. We simultaneously fit the data in the three redshift bins together, and find that the original UPP model cannot fit the data at small angular scales very well in the first and third redshift bins. The joint fits can be improved by including an additional parameter eta to change the redshift-dependence of the model (i.e. E(z)^{8/3} -> E(z)^{8/3+eta}) with best-fit value as eta=-3.11^{+1.09}_{-1.13}. This suggests that the original UPP model with less redshift-dependence may provide a better fit to the stacked thermal Sunyaev-Zeldovich profile., 14 pages, 10 figures, 1 table, accepted for publication in MNRAS
Published: 2019

42. Resolving Hubble tension by self-interacting neutrinos with Dirac seesaw

Author: Jiaming Zheng, Hong-Jian He, and Yin-Zhe Ma
Subjects: Particle physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, General Relativity and Quantum Cosmology, Cosmology, symbols.namesake, High Energy Physics - Phenomenology (hep-ph), Seesaw molecular geometry, Nucleosynthesis, Gauge group, 0103 physical sciences, Physics, 010308 nuclear & particles physics, Horizon, Dirac (video compression format), High Energy Physics::Phenomenology, Astronomy and Astrophysics, High Energy Physics - Phenomenology, symbols, Neutrino, Astrophysics - Cosmology and Nongalactic Astrophysics, Hubble's law
Abstract: Self-interacting neutrinos that begin to free-stream at close to matter-radiation equality can reduce the physical size of photon sound horizon at last scattering surface. This mechanism can be the reason why standard $\Lambda$CDM cosmology sees a lower value of the Hubble constant than local measurements from distance ladder. We propose a new realization of self-interacting Dirac neutrinos (SID$\nu$) with light-dark-photon mediator for a viable interaction mechanism. Our model is UV completed by a Dirac seesaw with anomaly-free dark $U(1)_X^{}$ gauge group which charges the right-handed neutrinos. This model naturally generates small masses for Dirac neutrinos and induces self-scattering of right-handed neutrinos. The scattering with left-handed neutrinos is suppressed by a chirality-flip mass insertion when the neutrino energy is much larger than its mass. The resultant neutrino self-scattering is not operative for $E_{\nu}\gtrsim O(\text{keV})$, which avoids the cosmological and laboratory constraints. By evolving Boltzmann equations for left- and right-handed neutrino number densities, we show that about $2/3$ of the left-handed neutrinos are converted into right-handed neutrinos in a short epoch between the Big-Bang Nucleosynthesis and the recombination, and interact with each other efficiently afterwards. The resultant neutrino non-free-streaming is the crucial ingredient to shrink down the comoving sound horizon at drag epoch, which can reconcile the Hubble tension between early and late time measurements., Comment: 26 pages, JCAP in press. Only minor refinements, references added. (This update is much delayed due to pandemic situation.)
Published: 2020

43. The Aero-elastic-wake Coupling Behavior for a Two-wind-turbines Case with Power Control Process

Author: Pan Zeng, LiPing Lei, and Zhe Ma
Subjects: Physics, Coupling, Wind power, business.industry, Process (computing), Mechanics, Wake, business, Power control
Abstract: This study focuses on the aero-elastic-wake coupling behavior of wind turbines. A newly developed code called FALM (Flexible Actuator Line Model), which combines the wake simulation ability of the actuator line mothed (ALM) and the structural simulation ability of the flexible multibody dynamics method, was employed to achieve these simulations. The power output and thrust, the natural frequency and deformation and the wake characteristics of a single NREL 5MW wind turbine were studied to validate this code. It shows that nonlinear effects such as spin softening and stress stiffening were fully considered by FALM and it can also guarantee a reliable prediction of power and thrust of wind turbines. Furthermore, a case of two-wind-turbines with the inlet wind speed of 14m/s (exceeding the rated wind speed) were carried out to study the aero-elastic-wake coupling behavior in a wind farm. It shows that FALM is able to simulate multiple wind turbines with power control system involved. The pitch control process of the upstream wind turbine was predicted and the dynamic loads of the downstream wind turbine caused by the wake effect were studied. These results will contribute to the study of reducing the fatigue load caused by wake effect.
Published: 2020

44. High performance distributed acoustic sensor based on digital LFM pulse coherent-optical time domain reflectometer for intrapulse event

Author: Shuanghao Wang, Junfeng Jiang, Yongning Zhang, Shuang Wang, Zhe Ma, Tiegen Liu, Panpan Niu, Wenjie Chen, and Kun Liu
Subjects: Physics, Acoustics, Event (relativity), General Engineering, Acoustic sensor, General Physics and Astronomy, Optical time-domain reflectometer, Pulse (physics)
Published: 2020

45. Self-copy-shift-based differential phase extracting method for fiber distributed acoustic sensing

Author: Guanhua Liang, Zhenyang Ding, Shuang Wang, Tiegen Liu, Junfeng Jiang, Kun Liu, Zhe Ma, Wenjie Chen, and Tianhua Xu
Subjects: Physics, business.industry, Distributed acoustic sensing, 01 natural sciences, Signal, Atomic and Molecular Physics, and Optics, Differential phase, Electronic, Optical and Magnetic Materials, 010309 optics, Amplitude modulation, Optics, Modulation, 0103 physical sciences, Demodulation, Waveform, Heterodyne detection, Electrical and Electronic Engineering, business
Abstract: A differential phase extracting method based on self-copy-shift for distributed acoustic sensing is proposed. Heterodyne and optical hybrids are used to realize high signal-to-noise ratio in-phase and quadrature-phase (IQ) signal measurement. The measured signals are self-copied and shifted for certain data points, and then they are digitally mixed with the original signals to construct the differential phase. The four produced signals are then combined to carry out IQ demodulation. An experiment with strain having an amplitude modulation waveform is carried out. The results showed that waveform information can be recovered well, and the signal-to-noise ratio achieves 32.8 dB.
Published: 2020

46. Planck 2018 results. VIII. Gravitational lensing

Author: Charles R. Lawrence, L. Pagano, Andrea Zacchei, J. B. Kim, K. Benabed, E. Martínez-González, Francesco Forastieri, M. Migliaccio, Martin White, M. Bucher, J. R. Bond, B. Ruiz-Granados, Andrea Zonca, N. Mauri, J. J. Bock, Douglas Scott, Davide Maino, H. C. Chiang, Yashar Akrami, Anthony Challinor, M. Tenti, Michele Maris, J. A. Tauber, M. Savelainen, O. Doré, K. Ganga, P. Bielewicz, Tiziana Trombetti, Jose M. Diego, Jean-François Cardoso, Francesca Perrotta, J. Aumont, Torsten A. Enßlin, M. Ashdown, H. K. Eriksen, X. Dupac, P. B. Lilje, Krzysztof M. Gorski, A. Marcos-Caballero, M. Reinecke, A. Mennella, Nabila Aghanim, R. A. Sunyaev, Julien Carron, Paolo Natoli, Franz Elsner, L. Montier, A. Mangilli, F. Cuttaia, Martin Kunz, Mathieu Remazeilles, R. B. Barreiro, F. Piacentini, G. Roudier, J.-L. Puget, K. Kiiveri, Guilaine Lagache, M.-A. Miville-Deschênes, L. Salvati, J. F. Macías-Pérez, Jon E. Gudmundsson, Yin-Zhe Ma, Jason D. McEwen, Zhiqi Huang, M. López-Caniego, Jose Alberto Rubino-Martin, L. P. L. Colombo, Martina Gerbino, G. Polenta, A. Moneti, F. K. Hansen, S. Galli, Soumen Basak, Mario Ballardini, Graca Rocha, J.-P. Bernard, Carlo Burigana, Nicoletta Krachmalnicoff, Chiara Sirignano, Sabino Matarrese, G. de Zotti, A. Renzi, C. Combet, Benjamin D. Wandelt, Julian Borrill, George Efstathiou, M. Frailis, Carlo Baccigalupi, Andrei V. Frolov, Jörg P. Rachen, Antony Lewis, Valeria Pettorino, François Levrier, E. Hivon, Will Handley, E. Di Valentino, Jacques Delabrouille, N. Mandolesi, Gianluca Morgante, Andrew H. Jaffe, Philip Lubin, Ingunn Kathrine Wehus, Diego Molinari, L. Toffolatti, A. J. Banday, Fabio Finelli, Massimiliano Lattanzi, Tuhin Ghosh, P. de Bernardis, R. Fernandez-Cobos, Aurelien A. Fraisse, B. P. Crill, B. Van Tent, P. Vielva, Erminia Calabrese, C. Rosset, Michele Liguori, Fabrizio Villa, Anthony Lasenby, Adam Moss, Ricardo Genova-Santos, E. Keihänen, E. Franceschi, Yabebal Fantaye, D. Tavagnacco, Nicola Bartolo, Marian Douspis, Nicola Vittorio, A. Karakci, W. C. Jones, A.-S. Suur-Uski, V. Lindholm, J. Valiviita, Peter G. Martin, S. Galeotta, Alessandro Gruppuso, J. González-Nuevo, J.-M. Lamarre, B. Partridge, A. Ducout, D. Paoletti, Hannu Kurki-Suonio, Steven Gratton, Lloyd Knox, L. Polastri, Alessandro Melchiorri, Reijo Keskitalo, M. Tomasi, Marco Bersanelli, Jan Hamann, Simon D. M. White, M. Sandri, Gianmarco Maggio, G. Patanchon, D. Herranz, M. Le Jeune, F. Boulanger, François R. Bouchet, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), 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), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Planck, Ministerio de Economía y Competitividad (España), Consejo Superior de Investigaciones Científicas (España), European Commission, European Research Council, European Space Agency, Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), Sorbonne Université (SU)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2020-....] (UGA [2020-....])-Institut polytechnique de Grenoble - Grenoble Institute of Technology [2020-....] (Grenoble INP [2020-....]), Université Grenoble Alpes [2020-....] (UGA [2020-....]), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centre 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), Universidad de Cantabria, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Astrophysique, Laboratoire de physique de l'ENS - ENS Paris (LPENS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), 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), Università degli studi di Parma = University of Parma (UNIPR), Computing and Mathematical Sciences [Pasadena]], California Institute of Technology (CALTECH), Canadian Institute for Theoretical Astrophysics (CITA), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Centre National d'Études Spatiales [Toulouse] (CNES), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Dipartimento di Fisica [Roma La Sapienza], Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Laboratory for Phytosanitary Diagnostics and Forecasts, All-Russian Institute for Plant Protection, Russian Academy of Sciences [Moscow] (RAS), Institut National Polytechnique (Toulouse) (Toulouse INP), Université de Toulouse (UT), ICRA and Physics Department, Dipartimento di Fisica 'G. Galilei', Università degli Studi di Padova = University of Padua (Unipd), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), University of Manchester [Manchester], Venetian Institute Molecular Medicine (VIMM), University of British Columbia (UBC), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Planck Collaboration, European Project: 616170,EC:FP7:ERC,ERC-2013-CoG,COSMOPARS(2014), 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), Aghanim N., 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., Bock J.J., Bond J.R., Borrill J., Bouchet F.R., Boulanger F., Bucher M., Burigana C., Calabrese E., Cardoso J.-F., Carron J., Challinor A., Chiang H.C., Colombo L.P.L., Combet C., Crill B.P., Cuttaia F., De Bernardis P., De Zotti G., Delabrouille J., Di Valentino E., Diego J.M., Dore O., Douspis M., Ducout A., Dupac X., Efstathiou G., Elsner F., Ensslin T.A., Eriksen H.K., Fantaye Y., Fernandez-Cobos R., Finelli F., Forastieri F., Frailis M., Fraisse A.A., Franceschi E., Frolov A., Galeotta S., Galli S., Ganga K., Genova-Santos R.T., Gerbino M., Ghosh T., Gonzalez-Nuevo J., Gorski K.M., Gratton S., Gruppuso A., Gudmundsson J.E., Hamann J., Handley W., Hansen F.K., Herranz D., Hivon E., Huang Z., Jaffe A.H., Jones W.C., Karakci A., Keihanen E., Keskitalo R., Kiiveri K., Kim J., Knox L., Krachmalnicoff N., Kunz M., Kurki-Suonio H., Lagache G., Lamarre J.-M., Lasenby A., Lattanzi M., Lawrence C.R., Le Jeune M., Levrier F., Lewis A., Liguori M., Lilje P.B., Lindholm V., Lopez-Caniego M., Lubin P.M., Ma Y.-Z., Macias-Perez J.F., Maggio G., Maino D., Mandolesi N., Mangilli A., Marcos-Caballero A., Maris M., Martin P.G., Martinez-Gonzalez E., Matarrese S., Mauri N., McEwen J.D., Melchiorri A., Mennella A., Migliaccio M., Miville-Deschenes M.-A., Molinari D., Moneti A., Montier L., Morgante G., Moss A., Natoli P., Pagano L., Paoletti D., Partridge B., Patanchon G., Perrotta F., Pettorino V., Piacentini F., Polastri L., Polenta G., Puget J.-L., Rachen J.P., Reinecke M., Remazeilles M., Renzi A., Rocha G., Rosset C., Roudier G., Rubino-Martin J.A., Ruiz-Granados B., Salvati L., Sandri M., Savelainen M., Scott D., Sirignano C., Sunyaev R., 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., Vittorio N., Wandelt B.D., Wehus I.K., White M., White S.D.M., Zacchei A., Zonca A., Department of Physics, Helsinki Institute of Physics, Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), University of Parma = Università degli studi di Parma [Parme, Italie], Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Université Fédérale Toulouse Midi-Pyrénées, Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Universita degli Studi di Padova, Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-École normale supérieure - Paris (ENS Paris), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)
Subjects: Cosmological parameter, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of Universe, Astronomy, Cosmic microwave background, Cosmological parameters, Cosmic background radiation, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Cosmology: observation, 01 natural sciences, 7. Clean energy, NO, symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, HALO-MODEL, Cosmic background radiation, Cosmological parameters, Cosmology: observations, Gravitational lensing: weak, Large-scale structure of Universe, Gravitational lensing: weak, Cosmic infrared background, 0103 physical sciences, Cosmology: observations, Planck, observations [Cosmology], 010303 astronomy & astrophysics, QB, Physics, Settore FIS/05, 010308 nuclear & particles physics, POWER SPECTRA, Spectral density, Astronomy and Astrophysics, 115 Astronomy, Space science, Redshift, GALAXIES, Gravitational lens, Space and Planetary Science, CROSS-CORRELATION, Dark energy, symbols, astro-ph.CO, DARK ENERGY, weak [Gravitational lensing], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Planck Collaboration: et al., arXiv:1807.06210v2, We present measurements of the cosmic microwave background (CMB) lensing potential using the final Planck 2018 temperature and polarization data. Using polarization maps filtered to account for the noise anisotropy, we increase the significance of the detection of lensing in the polarization maps from 5σ to 9σ. Combined with temperature, lensing is detected at 40σ. We present an extensive set of tests of the robustness of the lensing-potential power spectrum, and construct a minimum-variance estimator likelihood over lensing multipoles 8 ≤ L ≤ 400 (extending the range to lower L compared to 2015), which we use to constrain cosmological parameters. We find good consistency between lensing constraints and the results from the Planck CMB power spectra within the ΛCDM model. Combined with baryon density and other weak priors, the lensing analysis alone constrains σ8Ωm0.25 = 0.589 ± 0.020 (1σ errors). Also combining with baryon acoustic oscillation data, we find tight individual parameter constraints, σ8 = 0.811 ± 0.019, H0 = 67.9−1.3+1.2 km s−1 Mpc−1, and Ωm = 0.303−0.018+0.016. Combining with Planck CMB power spectrum data, we measure σ8 to better than 1% precision, finding σ8 = 0.811 ± 0.006. CMB lensing reconstruction data are complementary to galaxy lensing data at lower redshift, having a different degeneracy direction in σ8 − Ωm space; we find consistency with the lensing results from the Dark Energy Survey, and give combined lensing-only parameter constraints that are tighter than joint results using galaxy clustering. Using the Planck cosmic infrared background (CIB) maps as an additional tracer of high-redshift matter, we make a combined Planck-only estimate of the lensing potential over 60% of the sky with considerably more small-scale signal. We additionally demonstrate delensing of the Planck power spectra using the joint and individual lensing potential estimates, detecting a maximum removal of 40% of the lensing-induced power in all spectra. The improvement in the sharpening of the acoustic peaks by including both CIB and the quadratic lensing reconstruction is detected at high significance., Support is acknowledged from the European Research Council under the European Union’s Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement No. [616170], and from the Science and Technology Facilities Council [grant numbers ST/L000652/1 and ST/N000927/1, respectively]. The Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU).
Published: 2018

47. Hybrid demodulation method for distributed acoustic sensing based on coherent detection and pulse pair

Author: Guanhua Liang, Panpan Niu, Zhenyang Ding, Tiegen Liu, Zhe Ma, Kun Liu, Wenjie Chen, Shuang Wang, Yongning Zhang, and Junfeng Jiang
Subjects: 010302 applied physics, Physics, Acoustics, General Engineering, Phase (waves), General Physics and Astronomy, Beat (acoustics), 02 engineering and technology, Distributed acoustic sensing, 021001 nanoscience & nanotechnology, 01 natural sciences, Fiber coupler, Vibration, Pulse pair, 0103 physical sciences, Demodulation, Waveform, 0210 nano-technology
Abstract: A hybrid demodulation method based on coherent detection and pulse pair for distributed acoustic sensing is proposed. The Rayleigh backscattering light of pulse pair is coherent amplified by local reference light. A 3 × 3 fiber coupler is utilized to produce stable 2π/3 phase shift for phase extraction. The digital mixing of the beat signals of two pulses suppress the noise caused by phase drift and vibration on the local reference fiber. Several simulated acoustic waveforms are detected and retrieved. Experimental results show that the system has good linear response. And the equivalent strain of noise is as low as 0.4n ε.
Published: 2019

48. Forecasts of cosmological constraints from HI intensity mapping with FAST, BINGO and SKA-I

Author: Elimboto Yohana, Yin-Zhe Ma, and Yi-Chao Li
Subjects: Physics, Space and Planetary Science, Astrophysics::Instrumentation and Methods for Astrophysics, Intensity mapping, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We forecast the cosmological constraints of the neutral hydrogen (HI) intensity mapping (IM) technique with radio telescopes by assuming 1-year of observational time. The current and future radio telescopes we consider here are FAST (Five hundred meter Aperture Spherical Telescope), BINGO (Baryon acoustic oscillations In Neutral Gas Observations), and SKA-I (Square Kilometre Array phase I) single-dish experiment. We also forecast the combined constraints of the three radio telescopes with Planck. We find that, the $1 \sigma$ errors of $(w_{0}, w_{a})$ for BINGO, FAST and SKA-I with respect to the fiducial values are respectively, $(0.9293, 3.5792), (0.4083, 1.5878), (0.3158, 0.4622)$. This is equivalent to $(56.04\%, 55.64\%)$ and $(66.02\%, 87.09\%)$ improvements in constraining $(w_{0}, w_{a})$ for FAST and SKA-I relative to BINGO. Simulations further show that SKA-I will put more stringent constraints than both FAST and BINGO when each of the experiment is combined with Planck measurement. For the $9$ cosmological parameters in consideration, we find that, there is a trade-off between SKA-I and FAST in constraining cosmological parameters, with each experiment being more superior in constraining a particular set of parameters., Comment: Accepted for publication by RAA. 33 pages, 16 figures
Published: 2019

49. 21 cm limits on decaying dark matter and primordial black holes

Author: Louis E. Strigari, Bhaskar Dutta, Steven J. Clark, Yin-Zhe Ma, and Yu Gao
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Particle physics, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, FOS: Physical sciences, Primordial black hole, Astrophysics::Cosmology and Extragalactic Astrophysics, Radiation temperature, 01 natural sciences, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), Intergalactic medium, 0103 physical sciences, Strong coupling, Absorption (logic), Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Reionization, Energy (signal processing)
Abstract: Recently the Experiment to Detect the Global Epoch of Reionization Signature (EDGES) reported the detection of a 21cm absorption signal stronger than astrophysical expectations. In this paper we study the impact of radiation from dark matter (DM) decay and primordial black holes (PBH) on the 21cm radiation temperature in the reionization epoch, and impose a constraint on the decaying dark matter and PBH energy injection in the intergalactic medium, which can heat up neutral hydrogen gas and weaken the 21cm absorption signal. We consider decay channels DM$\rightarrow e^+e^-, \gamma\gamma$, $\mu^+\mu^-$, $b\bar{b}$ and the $10^{15-17}$g mass range for primordial black holes, and require the heating of the neutral hydrogen does not negate the 21cm absorption signal. For $e^+e^-$, $\gamma\gamma$ final states and PBH cases we find strong 21cm bounds that can be more stringent than the current extragalactic diffuse photon bounds. For the DM$\rightarrow e^+e^-$ channel, the lifetime bound is $\tau_{\rm DM}> 10^{27}$s for sub-GeV dark matter. The bound is $\tau_{\rm DM}\ge 10^{26}$s for sub-GeV DM$\rightarrow \gamma\gamma$ channel and reaches $10^{27}$s at MeV DM mass. For $b\bar{b}$ and $\mu^+\mu^-$ cases, the 21 cm constraint is better than all the existing constraints for $m_{\rm DM}, Comment: 7 pages, 4 figures
Published: 2018

50. Constraining the interaction between dark sectors with future HI intensity mapping observations

Author: Amanda Weltman, Yin-Zhe Ma, and Xiao-Dong Xu
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Intensity mapping, FOS: Physical sciences, Astronomy, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, Spectral line, Coupling (physics), 0103 physical sciences, Dark energy, Range (statistics), Sensitivity (control systems), 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We study a model of interacting dark matter and dark energy, in which the two components are coupled. We calculate the predictions for the 21-cm intensity mapping power spectra, and forecast the detectability with future single-dish intensity mapping surveys (BINGO, FAST and SKA-I). Since dark energy is turned on at $z\sim 1$, which falls into the sensitivity range of these radio surveys, the HI intensity mapping technique is an efficient tool to constrain the interaction. By comparing with current constraints on dark sector interactions, we find that future radio surveys will produce tight and reliable constraints on the coupling parameters., Comment: 12 pages, 7 figures
Published: 2018

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