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arXiv 2024年

作者： Prayag, V. Levin, L. Geyer, M. Stappers, B.W. Carli, E. Barr, E.D. Breton, R.P. Buchner, S. Burgay, M. Kramer, M. Possenti, A. Krishnan, V. Venkatraman Venter, C. Behrend, J. Chen, W. Horn, D.M. Padmanabh, P.V. Ridolfi, A. Department of Astronomy The University of Cape Town Private Bag X3 Rondebosch Cape Town7701 South Africa Group Department of Mathematics & Applied Mathematics University of Cape Town Cape Town7700 South Africa Jodrell Bank Centre for Astrophysics Department of Physics and Astronomy The University of Manchester ManchesterM13 9PL United Kingdom Max-Planck-Institut für Radioastronomie Auf Hügel 69 BonnD-53121 Germany 2 Fir Street Black River Park Observatory Cape Town7925 South Africa INAF-Osservatorio Astronomico di Cagliari via della Scienza 5 CA Selargius09047 Italy Centre for Space Research North-West University Private Bag X6001 Potchefstroom2520 South Africa National Institute for Theoretical and Computational Sciences South Africa Max-Planck-Institut für Gravitationsphysik Albert-Einstein-Institut HannoverD-30167 Germany Leibniz Universität Hannover HannoverD-30167 Germany

The Large Magellanic Cloud (LMC) presents a unique environment for pulsar population studies due to its distinct star formation characteristics and proximity to the Milky Way. As part of the TRAPUM (TRAnsients and PUlsars with MeerKAT) Large Survey Project, we are using the core array of the MeerKAT radio telescope (MeerKAT) to conduct a targeted search of the LMC for radio pulsars at L-band frequencies, 856–1712 MHz. The excellent sensitivity of MeerKAT, coupled with a 2-hour integration time, makes the survey 3 times more sensitive than previous LMC radio pulsar surveys. We report the results from the initial four survey pointings which has resulted in the discovery of seven new radio pulsars, increasing the LMC radio pulsar population by 30 per cent. The pulse periods of these new pulsars range from 278 to 1690 ms, and the highest dispersion measure is 254.20 pc cm–3. We searched for, but did not find any significant pulsed radio emission in a beam centred on the SN 1987A remnant, establishing an upper limit of 6.3 μJy on its minimum flux density at 1400 MHz. © 2024, CC BY.

关键词： Galaxies

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Open Hardware Solutions in Quantum Technology

arXiv

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arXiv 2023年

作者： Shammah, Nathan Roy, Anurag Saha Almudever, Carmen G. Bourdeauducq, Sébastien Butko, Anastasiia Cancelo, Gustavo Clark, Susan M. Heinsoo, Johannes Henriet, Loïc Huang, Gang Jurczak, Christophe Kotilahti, Janne Landra, Alessandro LaRose, Ryan Mari, Andrea Nowrouzi, Kasra Ockeloen-Korppi, Caspar Prawiroatmodjo, Guen Siddiqi, Irfan Zeng, William J. Unitary Fund San FranciscoCA94104 United States Qruise GmbH Saarbruecken66113 Germany Technical University of Valencia Spain M-Labs Limited North Point Hong Kong Applied Mathematics and Computational Research Division Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Fermi National Accelerator Laboratory BataviaIL60510 United States Sandia National Laboratories AlbuquerqueNM87123 United States IQM Quantum Computers Espoo02150 Finland PASQAL 7 rue Leonard de Vinci Massy91300 France Accelerator Technology and Applied Physics Division Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Quantonation Paris75010 France Center for Quantum Computing Science and Engineering Michigan State University East LansingMI48824 United States School of Science and Technology Università di Camerino Camerino62032 Italy Microsoft Quantum RedmondWA98052 United States Quantum Nanoelectronics Laboratory Department of Physics University of California at Berkeley BerkeleyCA94720 United States

Quantum technologies such as communications, computing, and sensing offer vast opportunities for advanced research and development. While an open-source ethos currently exists within some quantum technologies, especially in quantum computer programming, we argue that there are additional advantages in developing open quantum hardware (OQH). Open quantum hardware encompasses open-source software for the control of quantum devices in labs, blueprints and open-source toolkits for chip design and other hardware components, as well as openly-accessible testbeds and facilities that allow cloud-access to a wider scientific community. We provide an overview of current projects in the OQH ecosystem, identify gaps, and make recommendations on how to close them today. More open quantum hardware would accelerate technology transfer to and growth of the quantum industry and increase accessibility in science. © 2023, CC BY.

关键词： Technology transfer

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Exploring Modified Gravity: Constraints on the μ and Σ Parametrization with WMAP, ACT, and SPT

arXiv

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arXiv 2023年

作者： Andrade, Uendert Capistrano, Abraão J.S. Di Valentino, Eleonora Nunes, Rafael C. Leinweber Center for Theoretical Physics University of Michigan 450 Church Street Ann ArborMI48109-1040 United States Department of Physics College of Literature Science and the Arts University of Michigan 450 Church Street Ann ArborMI48109-1040 United States Observatório Nacional RJ Rio de Janeiro20921-400 Brazil Universidade Federal do Paraná PR Palotina85950-000 Brazil Applied physics graduation program UNILA PR Foz do Iguaçu85867-670 Brazil School of Mathematics and Statistics University of Sheffield United Kingdom Instituto de Física Universidade Federal do Rio Grande do Sul Porto Alegre RS 91501-970 Brazil Divisão de Astrofísica Instituto Nacional de Pesquisas Espaciais Avenida dos Astronautas 1758 SP São José dos Campos12227-010 Brazil

The cosmic acceleration problem remains one of the most significant challenges in cosmology. One of the proposed solutions to this problem is the modification of gravity on large scales. In this paper, we explore the well-known μ-Σ parametrization scenarios and confront them with observational data, including the cosmic microwave background (CMB) radiation from the Wilkinson Microwave Anisotropy Probe (WMAP), Atacama Cosmology Telescope (ACT), and South Pole Telescope (SPT), as well as large-scale structure data from the Sloan Digital Sky Survey (SDSS: BAO+RSD) and Pantheon Supernovae (SN) catalog. We employ a Bayesian framework to constrain the model parameters and discuss the implications of our results on the viability of modified gravity theories. Our analysis reveals the strengths and limitations of the μ-Σ parametrization and provides valuable insights into the nature of gravity on cosmological scales. From the joint analysis of the ACT + WMAP + SDSS + SN, we find μ0 − 1 = 0.02 ± 0.19 and Σ0 − 1 = 0.021 ± 0.068 at 68% CL. In light of the SPT + WMAP + SDSS + SN, we find μ0 − 1 = 0.07 ± 0.18 and Σ0 − 1 = −0.009+−0007811 at 68% CL. In all the analyses carried out, we do not find any deviations from the theory of general relativity. Our results represent an observational update on the well-known μ-Σ parameterization in view of current CMB data, independent and competitive with the constraints obtained with the Planck data. Copyright © 2023, The Authors. All rights reserved.

关键词： Telescopes

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A demonstration of improved constraints on primordial gravitational waves with delensing

引用

Physical Review D 2021年第2期103卷 022004-022004页

作者： P. A. R. Ade Z. Ahmed M. Amiri A. J. Anderson J. E. Austermann J. S. Avva D. Barkats R. Basu Thakur J. A. Beall A. N. Bender B. A. Benson F. Bianchini C. A. Bischoff L. E. Bleem J. J. Bock H. Boenish E. Bullock V. Buza J. E. Carlstrom C. L. Chang J. R. Cheshire, IV H. C. Chiang T-L. Chou R. Citron J. Connors C. Corbett Moran J. Cornelison T. M. Crawford A. T. Crites M. Crumrine A. Cukierman T. de Haan M. Dierickx M. A. Dobbs L. Duband W. Everett S. Fatigoni J. P. Filippini S. Fliescher J. Gallicchio E. M. George T. St. Germaine N. Goeckner-Wald D. C. Goldfinger J. Grayson N. Gupta G. Hall M. Halpern N. W. Halverson S. Harrison S. Henderson J. W. Henning S. R. Hildebrandt G. C. Hilton G. P. Holder W. L. Holzapfel J. D. Hrubes N. Huang J. Hubmayr H. Hui K. D. Irwin J. Kang K. S. Karkare E. Karpel S. Kefeli S. A. Kernasovskiy L. Knox J. M. Kovac C. L. Kuo K. Lau A. T. Lee E. M. Leitch D. Li A. Lowitz A. Manzotti J. J. McMahon K. G. Megerian S. S. Meyer M. Millea L. M. Mocanu L. Moncelsi J. Montgomery A. Nadolski T. Namikawa T. Natoli C. B. Netterfield H. T. Nguyen J. P. Nibarger G. Noble V. Novosad R. O’Brient R. W. Ogburn, IV Y. Omori S. Padin S. Palladino S. Patil T. Prouve C. Pryke B. Racine C. L. Reichardt C. D. Reintsema S. Richter J. E. Ruhl B. R. Saliwanchik K. K. Schaffer A. Schillaci B. L. Schmitt R. Schwarz C. D. Sheehy C. Sievers G. Smecher A. Soliman A. A. Stark B. Steinbach R. V. Sudiwala G. P. Teply K. L. Thompson J. E. Tolan C. Tucker A. D. Turner C. Umiltà T. Veach J. D. Vieira A. G. Vieregg A. Wandui G. Wang A. C. Weber N. Whitehorn D. V. Wiebe J. Willmert C. L. Wong W. L. K. Wu H. Yang V. Yefremenko K. W. Yoon E. Young C. Yu L. Zeng C. Zhang Cardiff University Cardiff CF10 3XQ United Kingdom SLAC National Accelerator Laboratory 2575 Sand Hill Road Menlo Park California 94025 USA Kavli Institute for Particle Astrophysics and Cosmology Stanford University 452 Lomita Mall Stanford California 94305 USA Department of Physics and Astronomy University of British Columbia Vancouver British Columbia V6T 1Z1 Canada Fermi National Accelerator Laboratory MS209 P.O. Box 500 Batavia Illinois 60510 USA NIST Quantum Devices Group 325 Broadway Mailcode 817.03 Boulder Colorado 80305 USA Department of Physics University of Colorado Boulder Colorado 80309 USA Department of Physics University of California Berkeley California 94720 USA Harvard-Smithsonian Center for Astrophysics 60 Garden Street Cambridge Massachusetts 02138 USA California Institute of Technology MS 249-17 1216 E. California Blvd. Pasadena California 91125 USA High Energy Physics Division Argonne National Laboratory 9700 S. Cass Avenue Argonne Illinois 60439 USA Kavli Institute for Cosmological Physics University of Chicago 5640 South Ellis Avenue Chicago Illinois 60637 USA Department of Astronomy and Astrophysics University of Chicago 5640 South Ellis Avenue Chicago Illinois 60637 USA School of Physics University of Melbourne Parkville Victoria 3010 Australia Department of Physics University of Cincinnati Cincinnati Ohio 45221 USA Jet Propulsion Laboratory Pasadena California 91109 USA Department of Physics Harvard University Cambridge Massachusetts 02138 USA Minnesota Institute for Astrophysics University of Minnesota Minneapolis Minnesota 55455 USA Department of Physics University of Chicago 5640 South Ellis Avenue Chicago Illinois 60637 USA Enrico Fermi Institute University of Chicago 5640 South Ellis Avenue Chicago Illinois 60637 USA Department of Physics McGill University 3600 Rue University Montreal Quebec H3A 2T8 Canada School of Mathematics Statistics and Computer Science University of KwaZulu-Natal Dur

We present a constraint on the tensor-to-scalar ratio, r, derived from measurements of cosmic microwave background (CMB) polarization B-modes with “delensing,” whereby the uncertainty on r contributed by the sample variance of the gravitational lensing B-modes is reduced by cross-correlating against a lensing B-mode template. This template is constructed by combining an estimate of the polarized CMB with a tracer of the projected large-scale structure. The large-scale-structure tracer used is a map of the cosmic infrared background derived from Planck satellite data, while the polarized CMB map comes from a combination of South Pole Telescope, bicep/Keck, and Planck data. We expand the bicep/Keck likelihood analysis framework to accept a lensing template and apply it to the bicep/Keck dataset collected through 2014 using the same parametric foreground modeling as in the previous analysis. From simulations, we find that the uncertainty on r is reduced by ∼10%, from σ(r)=0.024 to 0.022, which can be compared with a ∼26% reduction obtained when using a perfect lensing template or if there were zero lensing B-modes. Applying the technique to the real data, the constraint on r is improved from r0.05<0.090 to r0.05<0.082 (95% C.L.). This is the first demonstration of improvement in an r constraint through delensing.

关键词： Cosmic microwave background Inflation Large scale structure of the Universe

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LtU-ILI: AN ALL-IN-ONE FRAMEWORK FOR IMPLICIT INFERENCE IN ASTROphysics AND COSMOLOGY

arXiv

引用

arXiv 2024年

作者： Ho, Matthew Bartlett, Deaglan J. Chartier, Nicolas Cuesta-Lazaro, Carolina Ding, Simon Lapel, Axel Lemos, Pablo Lovell, Christopher C. Makinen, T. Lucas Modi, Chirag Pandya, Viraj Pandey, Shivam Perez, Lucia A. Wandelt, Benjamin Bryan, Greg L. UMR 7095 98 bis bd Arago ParisF-75014 France Center for the Gravitational-Wave Universe Astronomy Program Department of Physics and Astronomy Seoul National University Seoul08826 Korea Republic of Center for Astrophysics Harvard & Smithsonian 60 Garden St CambridgeMA02138 United States The NSF AI Institute for Artificial Intelligence and Fundamental Interactions United States Department of Physics Massachusetts Institute of Technology CambridgeMA02139 United States Department of Physics Université de Montréal Montréal Canada Mila - Quebec Artificial Intelligence Institute Montréal Canada Ciela - Montreal Institute for Astrophysical Data Analysis and Machine Learning Montréal Canada Center for Computational Astrophysics Flatiron Institute 162 5th Avenue New YorkNY10010 United States Institute of Cosmology and Gravitation University of Portsmouth Burnaby Road PortsmouthPO1 3FX United Kingdom & Astrophysics Group Imperial College London Blackett Laboratory Prince Consort Road LondonSW7 2AZ United Kingdom Center for Computational Mathematics Flatiron Institute 162 5th Avenue New YorkNY10010 United States Columbia Astrophysics Laboratory Columbia University 550 West 120th Street New YorkNY10027 United States 4 place Jussieu ParisF-75252 Cedex 5 France

This paper presents the Learning the Universe Implicit Likelihood Inference (LtU-ILI) pipeline, a codebase for rapid, user-friendly, and cutting-edge machine learning (ML) inference in astrophysics and cosmology. The pipeline includes software for implementing various neural architectures, training schemata, priors, and density estimators in a manner easily adaptable to any research workflow. It includes comprehensive validation metrics to assess posterior estimate coverage, enhancing the reliability of inferred results. Additionally, the pipeline is easily parallelizable and is designed for efficient exploration of modeling hyperparameters. To demonstrate its capabilities, we present real applications across a range of astrophysics and cosmology problems, such as: estimating galaxy cluster masses from X-ray photometry;inferring cosmology from matter power spectra and halo point clouds;characterizing progenitors in gravitational wave signals;capturing physical dust parameters from galaxy colors and luminosities;and establishing properties of semi-analytic models of galaxy formation. We also include exhaustive benchmarking and comparisons of all implemented methods as well as discussions about the challenges and pitfalls of ML inference in astronomical sciences. All code and examples are made publicly available at https://***/maho3/ltu-ili. © 2024, CC BY.

关键词： Cosmology

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Bridging HPC Communities through the Julia programming Language

arXiv

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arXiv 2022年

作者： Churavy, Valentin Godoy, William F. Bauer, Carsten Ranocha, Hendrik Schlottke-Lakemper, Michael Räss, Ludovic Blaschke, Johannes Giordano, Mosè Schnetter, Erik Omlin, Samuel Vetter, Jeffrey S. Edelman, Alan Massachussetts Institute of Technology United States Oak Ridge National Laboratory United States Paderborn Center for Parallel Computing Paderborn University Germany Department of Mathematics University of Hamburg Germany Applied and Computational Mathematics RWTH Aachen University Germany University of Stuttgart Germany ETH Zurich Switzerland Birmensdorf Switzerland National Energy Research Scientific Computing Center Lawrence Berkeley National Laboratory 1 Cyclotron Road BerkeleyCA94720 United States Centre for Advanced Research Computing University College London Gower Street LondonWC1E 6BT United Kingdom Perimeter Institute 31 Caroline St. N. WaterlooONN2L 2Y5 Canada Department of Physics and Astronomy University of Waterloo 200 University Avenue West WaterlooONN2L 3G1 Canada Center for Computation & Technology Louisiana State University Baton RougeLA70803 United States ETH Zurich Switzerland

The Julia programming language has evolved into a modern alternative to fill existing gaps in scientific computing and data science applications. Julia leverages a unified and coordinated single-language and ecosystem paradigm and has a proven track record of achieving high performance without sacrificing user productivity. These aspects make Julia a viable alternative to high-performance computing's (HPC's) existing and increasingly costly many-body workflow composition strategy in which traditional HPC languages (e.g., Fortran, C, C++) are used for simulations, and higher-level languages (e.g., Python, R, MATLAB) are used for data analysis and interactive computing. Julia's rapid growth in language capabilities, package ecosystem, and community make it a promising universal language for HPC. This paper presents the views of a multidisciplinary group of researchers from academia, government, and industry that advocate for an HPC software development paradigm that emphasizes developer productivity, workflow portability, and low barriers for entry. We believe that the Julia programming language, its ecosystem, and its community provide modern and powerful capabilities that enable this group's objectives. Crucially, we believe that Julia can provide a feasible and less costly approach to programming scientific applications and workflows that target HPC facilities. In this work, we examine the current practice and role of Julia as a common, end-to-end programming model to address major challenges in scientific reproducibility, data-driven AI/machine learning, co-design and workflows, scalability and performance portability in heterogeneous computing, network communication, data management, and community education. As a result, the diversification of current investments to fulfill the needs of the upcoming decade is crucial as more supercomputing centers prepare for the exascale era. © 2022, CC BY.

关键词： Productivity

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Estimation of Shear Wave Velocity of Darul Imarah District, Aceh Besar, Indonesia by Using 1D HVSR Inversion

引用

IOP Conference Series: Materials Science and Engineering 2020年第1期846卷

作者： Y Yusran Aulia Khalqillah Umar Muksin Muhammad Syukri Syamsul Rizal Nazli Ismail Doctoral Program of Mathematics and Applied Sciences Universitas Syiah Kuala Banda Aceh Indonesia Education of Physics Universitas Islam Negeri Ar-Raniry Banda Aceh Indonesia Department of Physics Universitas Syiah Kuala Banda Aceh Indonesia Tsunami and Disaster Mitigation Research Center (TDMRC) Universitas Syiah Kuala Banda Aceh Indonesia Department of Marine Sciences Universitas Syiah Kuala Banda Aceh Indonesia

A total of 19 locations of Horizontal to Vertical Spectral Ratio (HVSR) measurements was conducted in Darul Imarah District, Aceh Besar, Indonesia. The objective of the research is to investigate the shear wave velocity (Vs) structure. This survey is important to analyze a structural characteristic through a Vs, considering the measurement points intersect to Aceh Segment Fault. One of the methods to obtain Vs is 1D HVSR inversion. In this paper, we analyzed only four of 19 measurement points of HVSR data to estimate Vs, they are AB03, AB08, AB09 and AB19 points. The inversion results show that the four points have four layers with different Vs. The average of Vs30 of AB03, AB08, AB09 and AB19 were calculated, they are 150.90 m/s, 197.16 m/s, 150.45 m/s and 316.80 m/s, respectively. The AB09 has the lowest average of Vs30 (highest amplification) than the other points and has soft soil composition. Furthermore, based on the average of Vs30 and amplification, the subsurface of AB03, AB08 and AB19 may have combination soft soil and stiff soil in 30 m depth. The complete analysis of average of Vs30 structure will be conducted at all sites including a 3D velocity structure will be derived from the interpolation of 1D velocity.

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Corrigendum: Hyperuniformity variation with quasicrystal local isomorphism class

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Journal of physics. Condensed matter : an Institute of physics journal 2017年第47期29卷 2017 Aug 8页

作者： C Lin P J Steinhardt S Torquato Department of Physics Princeton University Princeton NJ 08544 United States of America. Princeton Center for Theoretical Science Princeton University Princeton NJ 08544 United States of America. Department of Chemistry Princeton University Princeton NJ 08544 United States of America. Program of Applied and Computational Mathematics Princeton University Princeton NJ 08544 United States of America. Princeton Institute for the Science and Technology of Materials Princeton University Princeton NJ 08544 United States of America.

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

arXiv

引用

arXiv 2019年

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

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

关键词： Cosmology

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Weak-lensing mass calibration of ACTPOL sunyaev-zel’dovich clusters with the hyper suprime-cam survey

arXiv

引用

arXiv 2018年

作者： Miyatake, Hironao Battaglia, Nicholas Hilton, Matt Medezinski, Elinor Nishizawa, Atsushi J. More, Surhud Aiola, Simone Bahcall, Neta Bond, J. Richard Calabrese, Erminia Choi, Steve K. Devlin, Mark J. Dunkley, Joanna Dunner, Rolando Fuzia, Brittany Gallardo, Patricio Gralla, Megan Hasselfield, Matthew Halpern, Mark Hikage, Chiaki Hill, J. Colin Hincks, Adam D. Hložek, Renée Huffenberger, Kevin Hughes, John P. Koopman, Brian Kosowsky, Arthur Louis, Thibaut Madhavacheril, Mathew S. McMahon, Jeff Mandelbaum, Rachel Marriage, Tobias A. Maurin, Loïc Miyazaki, Satoshi Moodley, Kavilan Murata, Ryoma Naess, Sigurd Newburgh, Laura Niemack, Michael D. Nishimichi, Takahiro Okabe, Nobuhiro Oguri, Masamune Osato, Ken Page, Lyman Partridge, Bruce Robertson, Naomi Sehgal, Neelima Sherwin, Blake Shirasaki, Masato Sievers, Jonathan Sifón, Cristóbal Simon, Sara Spergel, David N. Staggs, Suzanne T. Stein, George Takada, Masahiro Trac, Hy Umetsu, Keiichi van Engelen, Alex Wollack, Edward J. Institute for Advanced Research Nagoya University Nagoya464-8601 Japan Division of Physics and Astrophysical Science Graduate School of Science Nagoya University Nagoya464-8602 Japan Jet Propulsion Laboratory California Institute of Technology PasadenaCA91109 United States UTIAS University of Tokyo Chiba277-8583 Japan Center for Computational Astrophysics Flatiron Institute New YorkNY10010 United States Department of Astronomy Cornell University IthacaNY14853 United States Department of Astrophysical Sciences Princeton University PrincetonNJ08544 United States Astrophysics & Cosmology Research Unit School of Mathematics Statistics & Computer Science University of KwaZulu-Natal Westville Campus Durban4041 South Africa Department of Physics Princeton University PrincetonNJ08544 United States Canadian Institute for Theoretical Astrophysics University of Toronto TorontoONM5S 3H8 Canada School of Physics and Astronomy Cardiff University The Parade CardiffCF24 3AA United Kingdom Department of Physics and Astronomy University of Pennsylvania PhiladelphiaPA19104 United States Instituto de Astrofísica Centro de Astro-Ingeniería Facultad de Física Pontificia Universidad Católica de Chile Av. Vicuña Mackenna 4860 Macul Santiago7820436 Chile Department of Physics Florida State University TallahasseeFL32306 United States Department of Physics Cornell University IthacaNY14853 United States Department of Astronomy/Steward Observatory University of Arizona 933 N. Cherry Ave. TucsonAZ85721 United States Institute for Gravitation and the Cosmos Pennsylvania State University University ParkPA16802 United States Department of Astronomy and Astrophysics Pennsylvania State University University ParkPA16802 United States Department of Physics and Astronomy University of British Columbia VancouverBCV6T 1Z4 Canada School of Natural Sciences Institute for Advanced Study PrincetonNJ08540 United States Department of Physics University

We present weak-lensing measurements using the first-year data from the Hyper Suprime-Cam Strategic Survey program on the Subaru telescope for eight galaxy clusters selected through their thermal Sunyaev-Zel’dovich (SZ) signal measured at 148 GHz with the Atacama Cosmology Telescope Polarimeter experiment. The overlap between the two surveys in this work is 33.8 square degrees, before masking bright stars. The signal-to-noise ratio of individual cluster lensing measurements ranges from 2.2 to 8.7, with a total of 11.1 for the stacked cluster weak-lensing signal. We fit for an average weak-lensing mass distribution using three different profiles, a Navarro-Frenk-White profile, a dark-matter-only emulated profile, and a full cosmological hydrodynamic emulated profile. We interpret the differences among the masses inferred by these models as a systematic error of 10%, which is currently smaller than the statistical error. We obtain the ratio of the SZ-estimated mass to the lensing-estimated mass (the so-called hydrostatic mass bias (Formula presented), which is comparable to previous SZ-selected clusters from the Atacama Cosmology Telescope and from the Planck Satellite. We conclude with a discussion of the implications for cosmological parameters inferred from cluster abundances compared to cosmic microwave background primary anisotropy measurements. Subject headings: galaxies: clusters: general;gravitational lensing: weak;cosmology: observations Copyright © 2018, The Authors. All rights reserved.

关键词： Cams

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