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arXiv 2018年

作者： Skowron, J. Ryu, Y.-H. Hwang, K.-H. Udalski, A. Mroz, P. Kozlowski, S. Soszinski, I. Pietrukowicz, P. Szymánski, M.K. Poleski, R. Ulaczyk, K. Pawlak, M. Rybicki, K. Iwanek, P. Albrow, M.D. Chung, S.-J. Gould, A. Han, C. Jung, Y.K. Shin, I.-G. Shvartzvald, Y. Yee, J.C. Zang, W. Zhu, W. Cha, S.-M. Kim, D.-J. Kim, H.-W. Kim, S.-L. Lee, C.-U. Lee, D.-J. Lee, Y. Park, B.-G. Pogge, R.W. Warsaw University Observatory Al. Ujazdowskie 4 Warszawa00-478 Poland Korea Astronomy and Space Science Institute Daejon34055 Korea Republic of Department of Astronomy Ohio State University 140 W. 18th Ave. ColumbusOH43210 United States University of Canterbury Department of Physics and Astronomy Private Bag 4800 Christchurch8020 New Zealand Korea University of Science and Technology Daejeon34113 Korea Republic of Max-Planck-Institute for Astronomy Konigstuhl 17 Heidelberg69117 Germany Department of Physics Chungbuk National University Cheongju28644 Korea Republic of Harvard-Smithsonian CfA 60 Garden St. CambridgeMA02138 United States Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Drive PasadenaCA91109 United States Physics Department Tsinghua Centre for Astrophysics Tsinghua University Beijing100084 China Department of Physics Zhejiang University Hangzhou310058 China Canadian Institute for Theoretical Astrophysics University of Toronto 60 St George Street TorontoONM5S3H8 Canada School of Space Research Kyung Hee University Yongin Kyeonggi17104 Korea Republic of NASA Postdoctoral Program Fellow

We report the discovery of microlensing planet OGLE-2017-BLG-0373Lb. We show that while the planet-host system has an unambiguous microlens topology, there are two geometries within this topology that fit the data equally well, which leads to a factor 2.5 difference in planet-host mass ratio, i.e., q = 1.5 × 10-3vs. q = 0.6iÁ10.3. We show that this is an "accidental degeneracy" in the sense that it is due to a gap in the data. We dub it "the caustic-chirality degeneracy". We trace the mathematical origins of this degeneracy, which should enable similar degenerate solutions to be easily located in the future. A Bayesian estimate, based on a Galactic model, yields a host mass M = 0.25+0.30-0.15Mo at a distance DL = 5.9+1.3-1.95kpc. The lens-source relative proper motion is relatively fast, μ = 9 mas/yr, which implies that the host mass and distance can be determined by high-resolution imaging after about 10 years. The same observations could in principle resolve the discrete degeneracy in q, but this will be more challenging. Copyright © 2018, The Authors. All rights reserved.

关键词： Bayesian networks

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Ionized gas kinematics around an ultra-luminous x-ray source in ngc 5252 : Additional evidence for an off-nuclear agn

arXiv

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arXiv 2017年

作者： KIM, MINJIN HO, LUIS C. IM, MYUNGSHIN Korea Astronomy and Space Science Institute Daejeon305-348 Korea Republic of University of Science and Technology Daejeon305-350 Korea Republic of Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China Department of Astronomy School of Physics Peking University Beijing100871 China Astronomy Program Department of Physics and Astronomy Seoul National University 599 Gwanak-ro Gwanak-gu Seoul151-742 Korea Republic of

The Seyfert 2 galaxy NGC 5252 contains a recently identified ultra-luminous X-ray (ULX) source that has been suggested to be a possible candidate off-nuclear low-mass active galactic nucleus. We present follow-up optical integral-field unit observations obtained using GMOS on the Gemini-North telescope. In addition to confirming that the ionized gas in the vicinity of the ULX is kinematically associated with NGC 5252, the new observations reveal ordered motions consistent with rotation around the ULX. The close coincidence of the excitation source of the line-emitting gas with the position of the ULX further suggests that ULX itself is directly responsible for the ionization of the gas. The spatially resolved measurements of [N II] λ6584/Hα surrounding the ULX indicate a low gas-phase metallicity, consistent with those of other known low-mass active galaxies but not that of its more massive host galaxy. These findings strengthen the proposition that the ULX is not a background source, but rather that it is the nucleus of a small, low-mass galaxy accreted by NGC 5252. Copyright © 2017, The Authors. All rights reserved.

关键词： Ionization of gases

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New high-sensitivity searches for neutrons converting into antineutrons and/or sterile neutrons at the European Spallation Source

arXiv

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arXiv 2020年

作者： Addazi, A. Anderson, K. Ansell, S. Babu, K.S. Barrow, J. Baxter, D.V. Bentley, P.M. Berezhiani, Z. Bevilacqua, R. Biondi, R. Bohm, C. Brooijmans, G. Broussard, L.J. Dev, B. Crawford, C. Dolgov, A.D. Dunne, K. Fierlinger, P. Fitzsimmons, M.R. Fomin, A. Frost, M. Gardiner, S. Gardner, S. Galindo-Uribarri, A. Geltenbort, P. Girmohanta, S. Golubeva, E. Greene, G.L. Greenshaw, T. Gudkov, V. Hall-Wilton, R. Heilbronn, L. Herrero-Garcia, J. Ichikawa, G. Ito, T.M. Iverson, E. Johansson, T. Jönsson, L. Jwa, Y.-J. Kamyshkov, Y. Kanaki, K. Kearns, E. Kerbikov, B. Kitaguchi, M. Kittelmann, T. Klinkby, E. Kobakhidze, A. Koerner, L.W. Kopeliovich, B. Kozela, A. Kudryavtsev, V. Kupsc, A. Lee, Y. Lindroos, M. Makkinje, J. Marquez, J.I. Meirose, B. Miller, T.M. Milstead, D. Mohapatra, R.N. Morishima, T. Muhrer, G. Mumm, H.P. Nagamoto, K. Nesti, F. Nesvizhevsky, V.V. Nilsson, T. Oskarsson, A. Paryev, E. Pattie, R.W. Penttilä, S. Pokotilovski, Y.N. Potashnikova, I. Redding, C. Richard, J.-M. Ries, D. Rinaldi, E. Rossi, N. Ruggles, A. Rybolt, B. Santoro, V. Sarkar, U. Saunders, A. Senjanovic, G. Serebrov, A.P. Shimizu, H.M. Shrock, R. Silverstein, S. Silvermyr, D. Snow, W.M. Takibayev, A. Tkachev, I. Townsend, L. Tureanu, A. Varriano, L. Vainshtein, A. de Vries, J. Woracek, R. Yamagata, Y. Young, A.R. Zanini, L. Zhang, Z. Zimmer, O. Amherst Center for Fundamental Interactions Department of Physics University of Massachusetts AmherstMA United States INFN Laboratori Nazionali del Gran Sasso Assergi AQ67010 Italy Fermi National Accelerator Laboratory BataviaIL60510-5011 United States Department of Physics Indiana University 727 E. Third St. BloomingtonIN47405 United States Indiana University Center for Exploration of Energy & Matter BloomingtonIN47408 United States Indiana University Quantum Science and Engineering Center BloomingtonIN47408 United States Department of Physics Boston University BostonMA02215 United States Center for Theoretical Physics College of Physics Science and Technology Sichuan University Chengdu610065 China Department of Physics University of Chicago ChicagoIL60637 United States Department of Physics University of Maryland College ParkMD20742-4111 United States Department of Physics and Astronomy University of South Carolina ColumbiaSC29208 United States Dipartimento di Scienze Fisiche e Chimiche Università di L’Aquila Coppito AQ67100 Italy National Institute of Standards and Technology GaithersburgMD20899 United States NRC "Kurchatov Institute" - PNPI Gatchina Russia Physics Department Technical University Munich Garching85748 Germany Institut Laue-Langevin Grenoble38042 France Department of Physics University of Helsinki P.O.Box 64 HelsinkiFIN-00014 Finland Institutionen för Fysik Chalmers Tekniska Högskola Sweden Department of Physics University of Houston HoustonTX77204-5008 United States Department of Physics and Astronomy East Tennessee State University Johnson CityTN37614 United States Department of Physics Kennesaw State University KennesawGA30144 United States Physics Department Indian Institute of Technology Kharagpur721302 India Department of Physics and Astronomy University of Tennessee KnoxvilleTN37996 United States Department of Nuclear Engineering University of Tennessee KnoxvilleTN37996 United States H

The violation of Baryon Number, B, is an essential ingredient for the preferential creation of matter over antimatter needed to account for the observed baryon asymmetry in the universe. However, such a process has yet to be experimentally observed. The HIBEAM/NNBAR program is a proposed two-stage experiment at the European Spallation Source (ESS) to search for baryon number violation. The program will include high-sensitivity searches for processes that violate baryon number by one or two units: free neutron-antineutron oscillation (n → n¯) via mixing, neutron-antineutron oscillation via regeneration from a sterile neutron state (n → [n', n¯'] → n¯), and neutron disappearance (n → n');the effective ∆B = 0 process of neutron regeneration (n → [n', n¯'] → n) is also possible. The program can be used to discover and characterise mixing in the neutron, antineutron, and sterile neutron sectors. The experiment addresses topical open questions such as the origins of baryogenesis, the nature of dark matter, and is sensitive to scales of new physics substantially in excess of those available at colliders. A goal of the program is to open a discovery window to neutron conversion probabilities (sensitivities) by up to three orders of magnitude compared with previous searches. The opportunity to make such a leap in sensitivity tests should not be squandered. The experiment pulls together a diverse international team of physicists from the particle (collider and low energy) and nuclear physics communities, while also including specialists in neutronics and magnetics. Copyright © 2020, The Authors. All rights reserved.

关键词： Neutrons

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Millimeter-wave point sources from the 2500-square-degree SPT-SZ survey: Catalog and population statistics

arXiv

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arXiv 2020年

作者： Everett, W.B. Zhang, L. Crawford, T.M. Vieira, J.D. Aravena, M. Archipley, M.A. Austermann, J.E. Benson, B.A. Bleem, L.E. Carlstrom, J.E. Chang, C.L. Chapman, S. Crites, A.T. de Haan, T. Dobbs, M.A. George, E.M. Halverson, N.W. Harrington, N. Holder, G.P. Holzapfel, W.L. Hrubes, J.D. Knox, L. Lee, A.T. Luong-Van, D. Mangian, A.C. Marrone, D.P. McMahon, J.J. Meyer, S.S. Mocanu, L.M. Mohr, J.J. Natoli, T. Padin, S. Pryke, C. Reichardt, C.L. Reuter, C.A. Ruhl, J.E. Sayre, J.T. Schaffer, K.K. Shirokoff, E. Spilker, J.S. Stalder, B. Staniszewski, Z. Stark, A.A. Story, K.T. Switzer, E.R. Vanderlinde, K. Weiß, A. Williamson, R. Center for Astrophysics and Space Astronomy Department of Astrophysical and Planetary Sciences University of Colorado BoulderCO80309 United States Department of Physics University of California Santa BarbaraCA93106 United States Department of Physics University of Illinois Urbana-Champaign UrbanaIL61801 United States Kavli Institute for Cosmological Physics University of Chicago ChicagoIL60637 United States Department of Astronomy and Astrophysics University of Chicago ChicagoIL60637 United States Astronomy Department University of Illinois Urbana-Champaign UrbanaIL61801 United States Núcleo de Astronomía Facultad de Ingeniería y Ciencias Universidad Diego Portales Av. Ejército 441 Santiago Chile NIST Quantum Devices Group BoulderCO80305 United States Department of Physics University of Colorado BoulderCO80309 United States Fermi National Accelerator Laboratory BataviaIL60510 United States High Energy Physics Division Argonne National Laboratory ArgonneIL60439 United States Department of Physics University of Chicago ChicagoIL60637 United States Enrico Fermi Institute University of Chicago ChicagoIL60637 United States Department of Physics and Atmospheric Science Dalhousie University HalifaxNSB3H 3J5 Canada Institute of Astronomy University of Cambridge Madingley Road CambridgeCB3 0HA United Kingdom California Institute of Technology PasadenaCA91125 United States Department of Physics University of California BerkeleyCA94720 United States Physics Division Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Department of Physics McGill University MontrealQCH3A 2T8 Canada Canadian Institute for Advanced Research CIFAR Program in Gravity and the Extreme Universe TorontoONM5G 1Z8 Canada European Southern Observatory Munich Germany University of Chicago ChicagoIL60637 United States Department of Physics University of California DavisCA95616 United States Steward Observatory University of Arizo

We present a catalog of emissive point sources detected in the SPT-SZ survey, a contiguous 2530-square-degree area surveyed with the South Pole Telescope (SPT) from 2008 - 2011 in three bands centered at 95, 150, and 220 GHz. The catalog contains 4845 sources measured at a significance of 4.5 σ or greater in at least one band, corresponding to detections above approximately 9.8, 5.8, and 20.4 mJy in 95, 150, and 220 GHz, respectively. Spectral behavior in the SPT bands is used for source classification into two populations based on the underlying physical mechanisms of compact, emissive sources that are bright at millimeter wavelengths: synchrotron radiation from active galactic nuclei and thermal emission from dust. The latter population includes a component of high-redshift sources often referred to as submillimeter galaxies (SMGs). In the relatively bright flux ranges probed by the survey, these sources are expected to be magnified by strong gravitational lensing. The survey also contains sources consistent with protoclusters, groups of dusty galaxies at high redshift undergoing collapse. We cross-match the SPT-SZ catalog with external catalogs at radio, infrared, and X-ray wavelengths and identify available redshift information. The catalog splits into 3980 synchrotron-dominated and 865 dust-dominated sources and we determine a list of 506 SMGs. Ten sources in the catalog are identified as stars. We calculate number counts for the full catalog, and synchrotron and dusty components, using a bootstrap method and compare our measured counts with models. This paper represents the third and final catalog of point sources in the SPT-SZ survey. Copyright © 2020, The Authors. All rights reserved.

关键词： Surveys

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Chromospheric plasma ejections in a light bridge of a sunspot

arXiv

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arXiv 2017年

作者： Song, Donguk Chae, Jongchul Yurchyshyn, Vasyl Lim, Eun-Kyung Cho, Kyung-Suk Yang, Heesu Cho, Kyuhyoun Kwak, Hannah Astronomy Program Department of Physics and Astronomy Seoul National University 1 Gwanak-ro Gwanak-gu Seoul08826 Korea Republic of Korea Astronomy and Space Science Institute 776 Daedeokdae-ro Yuseong-gu Daejeon34055 Korea Republic of Big Bear Solar Observatory New Jersey Institute of Technology 40386 North Shore Lane Big Bear CityCA92314-9672 United States

It is well-known that light bridges inside a sunspot produce small-scale plasma ejections and transient brightenings in the chromosphere, but the nature and origin of such phenomena are still unclear. Utilizing the high-spatial and high-temporal resolution spectral data taken with the Fast Imaging Solar Spectrograph and the TiO 7057 Å broadband filter images installed at the 1.6 meter New Solar Telescope of Big Bear Solar Observatory, we report arcsecond-scale chromospheric plasma ejections (1.′′7) inside a light bridge. Interestingly, the ejections are found to be a manifestation of upwardly propagating shock waves as evidenced by the sawtooth patterns seen in the temporal-spectral plots of the Ca ii 8542 Å and Hα intensities. We also found a fine-scale photospheric pattern (1′′) diverging with a speed of about 2 km s−1 two minutes before the plasma ejections, which seems to be a manifestation of magnetic flux emergence. As a response to the plasma ejections, the corona displayed small-scale transient brightenings. Based on our findings, we suggest that the shock waves can be excited by the local disturbance caused by magnetic reconnection between the emerging flux inside the light bridge and the adjacent umbral magnetic field. The disturbance generates slow-mode waves, which soon develop into shock waves, and manifest themselves as the arcsecond-scale plasma ejections. It also appears that the dissipation of mechanical energy in the shock waves can heat the local corona. Copyright © 2017, The Authors. All rights reserved.

关键词： Shock waves

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Full orbital solution for the binary system in the northern Galactic disc microlensing event Gaia16aye ⋆

arXiv

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arXiv 2019年

作者： Wyrzykowski, Lukasz Mróz, P. Rybicki, K.A. Gromadzki, M. Kolaczkowski, Z. Zielinski, M. Zielinski, P. Britavskiy, N. Gomboc, A. Sokolovsky, K. Hodgkin, S.T. Abe, L. Aldi, G.F. AlMannaei, A. Altavilla, G. Al Qasim, A. Anupama, G.C. Awiphan, S. Bachelet, E. Bakış, V. Baker, S. Bartlett, S. Bendjoya, P. Benson, K. Bikmaev, I.F. Birenbaum, G. Blagorodnova, N. Blanco-Cuaresma, S. Boeva, S. Bonanos, A.Z. Bozza, V. Bramich, D.M. Bruni, I. Burenin, R.A. Burgaz, U. Butterley, T. Caines, H.E. Caton, D.B. Calchi Novati, S. Carrasco, J.M. Cassan, A. Čepas, V. Cropper, M. Chruslińska, M. Clementini, G. Clerici, A. Conti, D. Conti, M. Cross, S. Cusano, F. Damljanovic, G. Dapergolas, A. D’Ago, G. de Bruijne, J.H.J. Dennefeld, M. Dhillon, V.S. Dominik, M. Dziedzic, J. Erece, O. Eselevich, M.V. Esenoglu, H. Eyer, L. Figuera Jaimes, R. Fossey, S.J. Galeev, A.I. Grebenev, S.A. Gupta, A.C. Gutaev, A.G. Hallakoun, N. Hamanowicz, A. Han, C. Handzlik, B. Haislip, J.B. Hanlon, L. Hardy, L.K. Harrison, D.L. van Heerden, H.J. Hoette, V.L. Horne, K. Hudec, R. Hundertmark, M. Ihanec, N. Irtuganov, E.N. Itoh, R. Iwanek, P. Jovanovic, M.D. Janulis, R. Jelínek, M. Jensen, E. Kaczmarek, Z. Katz, D. Khamitov, I.M. Kilic, Y. Klencki, J. Kolb, U. Kopacki, G. Kouprianov, V.V. Kruszynska, K. Kurowski, S. Latev, G. Lee, C.-H. Leonini, S. Leto, G. Lewis, F. Li, Z. Liakos, A. Littlefair, S.P. Lu, J. Manser, C.J. Mao, S. Maoz, D. Martin-Carrillo, A. Marais, J.P. Maskoliūnas, M. Maund, J.R. Meintjes, P.J. Melnikov, S.S. Ment, K. Mikolajczyk, P. Morrell, M. Mowlavi, N. Moździerski, D. Murphy, D. Nazarov, S. Netzel, H. Nesci, R. Ngeow, C.-C. Norton, A.J. Ofek, E.O. Pakštiene, E. Palaversa, L. Pandey, A. Paraskeva, E. Pawlak, M. Penny, M.T. Penprase, B.E. Piascik, A. Prieto, J.L. Qvam, J.K.T. Ranc, C. Rebassa-Mansergas, A. Reichart, D.E. Reig, P. Rhodes, L. Rivet, J.-P. Rixon, G. Roberts, D. Rosi, P. Russell, D.M. Zanmar Sanchez, R. Scarpetta, G. Seabroke, G. Shappee, B.J. Warsaw University Astronomical Observatory Al. Ujazdowskie 4 Warszawa00-478 Poland Department of Physics Chungbuk National University Cheongju28644 Korea Republic of Sternberg Astronomical Institute Moscow State University Universitetskii pr. 13 Moscow119992 Russia E-38205 La Laguna Tenerife Spain Universidad de La Laguna Dpto. Astrofísica La Laguna TenerifeE-38206 Spain Institute of Astronomy University of Cambridge Madingley Road CambridgeCB3 0HA United Kingdom 00078 Italy Indian Institute of Astrophysics II Block Koramangala Bengaluru560034 India National Astronomical Research Institute of Thailand 260 Moo 4 T. Donkaew A. Mae Rim Chiang Mai50180 Thailand Department of Space Sciences and Technologies Faculty of Science Akdeniz University Antalya07058 Turkey Université Côte d’Azur Observatoire de la Côte d’Azur CNRS Laboratoire Lagrange France School of Physics and Astronomy Tel-Aviv University tel-aviv6997801 Israel Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Drive PasadenaCA91109 United States NASA Postdoctoral Program Fellow Harvard-Smithsonian Center for Astrophysics 60 Garden Street CambridgeMA02138 United States Institute of Astronomy and NAO Rozhen BAS 72 Tsarighradsko Shousse Blvd. Sofia1784 Bulgaria National Optical Astronomy Observatory 950 N Cherry Avenue TucsonAZ85719 United States Subaru Telescope National Astronomical Observatory of Japan 650 N Aohoku Place HiloHI96720 United States IAASARS National Observatory of Athens Vas. Pavlou & I. Metaxa Penteli15236 Greece I-84084 Italy Department of Astronomy and Space Sciences Ege University Izmir35100 Turkey Centre for Advanced Instrumentation University of Durham South Road DurhamDH1 3LE United Kingdom c/ Martí i Franquès 1 Barcelona08028 Spain Department of Astrophysics IMAPP Radboud University Nijmegen P.O. Box 9010 Nijmegen6500 GL Netherlands INAF - Osservatorio di Astrofisica e Scienza dello Spazio di Bologna

Gaia16aye was a binary microlensing event discovered in the direction towards the northern Galactic disc and was one of the first microlensing events detected and alerted to by the Gaia space mission. Its light curve exhibited five distinct brightening episodes, reaching up to I=12 mag, and it was covered in great detail with almost 25,000 data points gathered by a network of telescopes. We present the photometric and spectroscopic follow-up covering 500 days of the event evolution. We employed a full Keplerian binary orbit microlensing model combined with the motion of Earth and Gaia around the Sun to reproduce the complex light curve. The photometric data allowed us to solve the microlensing event entirely and to derive the complete and unique set of orbital parameters of the binary lensing system. We also report on the detection of the first-ever microlensing space-parallax between the Earth and Gaia located at L2. The properties of the binary system were derived from microlensing parameters, and we found that the system is composed of two main-sequence stars with masses 0.57±0.05 M and 0.36±0.03 M at 780 pc, with an orbital period of 2.88 years and an eccentricity of 0.30. We also predict the astrometric microlensing signal for this binary lens as it will be seen by Gaia as well as the radial velocity curve for the binary system. Events such as Gaia16aye indicate the potential for the microlensing method of probing the mass function of dark objects, including black holes, in directions other than that of the Galactic bulge. This case also emphasises the importance of long-term time-domain coordinated observations that can be made with a network of heterogeneous telescopes. Copyright © 2019, The Authors. All rights reserved.

关键词： Geometrical optics

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Optimal CMB lensing reconstruction and parameter estimation with SPTpol data

arXiv

引用

arXiv 2020年

作者： Millea, Marius Daley, C.M. Chou, T.-L. Anderes, E. Ade, P.A.R. Anderson, A.J. Austermann, J.E. Avva, J.S. Beall, J.A. Bender, A.N. Benson, B.A. Bianchini, F. Bleem, L.E. Carlstrom, J.E. Chang, C.L. Chaubal, P. Chiang, H.C. Citron, R. Corbett Moran, C. Crawford, T.M. Crites, A.T. de Haan, T. Dobbs, M.A. Everett, W. Gallicchio, J. George, E.M. Goeckner-Wald, N. Guns, S. Gupta, N. Halverson, N.W. Henning, J.W. Hilton, G.C. Holder, G.P. Holzapfel, W.L. Hrubes, J.D. Huang, N. Hubmayr, J. Irwin, K.D. Knox, L. Lee, A.T. Li, D. Lowitz, A. McMahon, J.J. Meyer, S.S. Mocanu, L.M. Montgomery, J. Natoli, T. Nibarger, J.P. Noble, G. Novosad, V. Omori, Y. Padin, S. Patil, S. Pryke, C. Reichardt, C.L. Ruhl, J.E. Saliwanchik, B.R. Schaffer, K.K. Sievers, C. Smecher, G. Stark, A.A. Thorne, B. Tucker, C. Veach, T. Vieira, J.D. Wang, G. Whitehorn, N. Wu, W.L.K. Yefremenko, V. Department of Physics University of California BerkeleyCA94720 United States Astronomy Department University of Illinois at Urbana-Champaign 1002 W. Green Street UrbanaIL61801 United States Kavli Institute for Cosmological Physics University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States Department of Physics University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States Department of Statistics University of California One Shields Avenue DavisCA95616 United States Cardiff University CardiffCF10 3XQ United Kingdom Fermi National Accelerator Laboratory MS209 P.O. Box 500 BataviaIL60510 United States NIST Quantum Devices Group 325 Broadway Mailcode 817.03 BoulderCO80305 United States Department of Physics University of Colorado BoulderCO80309 United States High Energy Physics Division Argonne National Laboratory 9700 S. Cass Avenue ArgonneIL60439 United States Department of Astronomy and Astrophysics University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States School of Physics University of Melbourne ParkvilleVIC3010 Australia Enrico Fermi Institute University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States Department of Physics McGill University 3600 Rue University MontrealQCH3A 2T8 Canada School of Mathematics Statistics & Computer Science University of KwaZulu-Natal Durban South Africa University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States Jet Propulsion Laboratory PasadenaCA91109 United States Dunlap Institute for Astronomy & Astrophysics University of Toronto 50 St George St TorontoONM5S 3H4 Canada Department of Astronomy & Astrophysics University of Toronto 50 St George St TorontoONM5S 3H4 Canada Physics Division Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Canadian Institute for Advanced Research CIFAR Program in Gravity Extreme Universe TorontoONM5G 1Z8 Canada Department of Astrophysical and Pla

We perform the first simultaneous Bayesian parameter inference and optimal reconstruction of the gravitational lensing of the cosmic microwave background (CMB), using 100 deg2 of polarization observations from the SPTpol receiver on the South Pole Telescope. These data reach noise levels as low as 5.8 µK-arcmin in polarization, which are low enough that the typically used quadratic estimator (QE) technique for analyzing CMB lensing is significantly sub-optimal. Conversely, the Bayesian procedure extracts all lensing information from the data and is optimal at any noise level. We infer the amplitude of the gravitational lensing potential to be Aφ = 0.949 ±0.122 using the Bayesian pipeline, consistent with our QE pipeline result, but with 17% smaller error bars. The Bayesian analysis also provides a simple way to account for systematic uncertainties, performing a similar job as frequentist "bias hardening," and reducing the systematic uncertainty on Aφ due to polarization calibration from almost half of the statistical error to effectively zero. Finally, we jointly constrain Aφ along with AL, the amplitude of lensing-like effects on the CMB power spectra, demonstrating that the Bayesian method can be used to easily infer parameters both from an optimal lensing reconstruction and from the delensed CMB, while exactly accounting for the correlation between the two. These results demonstrate the feasibility of the Bayesian approach on real data, and pave the way for future analysis of deep CMB polarization measurements with SPT-3G, Simons Observatory, and CMB-S4, where improvements relative to the QE can reach 1.5 times tighter constraints on Aφ and 7 times lower effective lensing reconstruction noise. Copyright © 2020, The Authors. All rights reserved.

关键词： Cosmology

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OGLE-2017-BLG-1130: The first binary gravitational microlens detected from spitzer only

arXiv

引用

arXiv 2018年

作者： Wang, Tianshu Novati, S. Calchi Udalski, A. Gould, A. Mao, Shude Zang, W. Beichman, C. Bryden, G. Carey, S. Gaudi, B.S. Henderson, C.B. Shvartzvald, Y. Yee, J.C. Mroz, P. Poleski, R. Skowron, J. Szymanski, M.K. Soszynski, I. Kozlowski, S. Pietrukowicz, P. Ulaczyk, K. Pawlak, M. Albrow, M.D. Chung, S.-J. Han, C. Hwang, K.-H. Jung, Y.K. Ryu, Y.-H. Shin, I.-G. Zhu, W. Cha, S.-M. Kim, D.-J. Kim, H.-W. Kim, S.-L. Lee, C.-U. Lee, D.-J. Lee, Y. Park, B.-G. Pogge, R.W. Physics Department and Tsinghua Centre for Astrophysics Tsinghua University Beijing100084 China IPAC Caltech Mail Code 100-22 1200 E. California Blvd. PasadenaCA91125 United States Spitzer Team Warsaw University Observatory Al. Ujazdowskie 4 Warszawa00-478 Poland OGLE collaboration Korea Astronomy and Space Science Institute Daejon34055 Korea Republic of Department of Astronomy Ohio State University 140 W. 18th Ave. ColumbusOH43210 United States Max-Planck-Institute for Astronomy Konigstuhl 17 Heidelberg69117 Germany KMTnet National Astronomical Observatories Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China Jodrell Bank Centre for Astrophysics School of Physics and Astronomy University of Manchester Oxford Road ManchesterM139PL United Kingdom Department of Physics Zhejiang University Hangzhou310058 China NASA Exoplanet Science Institute California Institute of Technology MS 100-22 PasadenaCA91125 United States Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Drive PasadenaCA91109 United States Spitzer Science Center California Institute of Technology MS 220-6 PasadenaCA United States NASA Postdoctoral Program Fellow Harvard-Smithsonian Center for Astrophysics 60 Garden St. CambridgeMA02138 United States Department of Astronomy Ohio State University 140 W.18th Ave. ColumbusOH43210 United States Warsaw University Observatory Al. Ujazdowskie 4 Warszawa00-478 Poland University of Canterbury Department of Physics and Astronomy Private Bag 4800 Christchurch8020 New Zealand Korea University of Science and Technology Daejeon34113 Korea Republic of Department of Physics Chungbuk National University Cheongju28644 Korea Republic of Canadian Institute for Theoretical Astrophysics University of Toronto 60 St George Street TorontoONM5S3H8 Canada School of Space Research Kyung Hee University Yongin Kyeonggi17104 Korea Republic of

We analyze the binary gravitational microlensing event OGLE-2017-BLG-1130 (mass ratio q ∼ 0.45), the first published case in which the binary anomaly was only detected by the Spitzer space Telescope. This event provides strong evidence that some binary signals can be missed by observations from the ground alone but detected by Spitzer. We therefore invert the normal procedure, first finding the lens parameters by fitting the space-based data and then measuring the microlensing parallax using ground-based observations. We also show that the normal four-fold spacebased degeneracy in the single-lens case can become a weak eight-fold degeneracy in binary-lens events. Although this degeneracy is resolved in event OGLE-2017-BLG-1130, it might persist in other events. Copyright © 2018, The Authors. All rights reserved.

关键词： Geometrical optics

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Author Correction: Aplp1 interacts with Lag3 to facilitate transmission of pathologic α-synuclein

引用

Nature communications 2024年第1期15卷 6413页

作者： Xiaobo Mao Hao Gu Donghoon Kim Yasuyoshi Kimura Ning Wang Enquan Xu Ramhari Kumbhar Xiaotian Ming Haibo Wang Chan Chen Shengnan Zhang Chunyu Jia Yuqing Liu Hetao Bian Senthilkumar S Karuppagounder Fatih Akkentli Qi Chen Longgang Jia Heehong Hwang Su Hyun Lee Xiyu Ke Michael Chang Amanda Li Jun Yang Cyrus Rastegar Manjari Sriparna Preston Ge Saurav Brahmachari Sangjune Kim Shu Zhang Yasushi Shimoda Martina Saar Haiqing Liu Sin Ho Kweon Mingyao Ying Creg J Workman Dario A A Vignali Ulrike C Muller Cong Liu Han Seok Ko Valina L Dawson Ted M Dawson Neuroregeneration and Stem Cell Programs Institute for Cell Engineering Johns Hopkins University School of Medicine Baltimore MD 21205 USA. xmao4@jhmi.edu. Department of Neurology Johns Hopkins University School of Medicine Baltimore MD 21205 USA. xmao4@jhmi.edu. Adrienne Helis Malvin Medical Research Foundation New Orleans LA 70130-2685 USA. xmao4@jhmi.edu. Neuroregeneration and Stem Cell Programs Institute for Cell Engineering Johns Hopkins University School of Medicine Baltimore MD 21205 USA. Department of Neurology Johns Hopkins University School of Medicine Baltimore MD 21205 USA. Department of Neurology Nanjing Brain Hospital Nanjing Jiangsu 210029 PR China. Medical College Yangzhou University Yangzhou Jiangsu 225001 PR China. Department of Pharmacology College of Medicine Dong-A University 32 Daesin Gongwwon-ro Seo-gu Busan 49201 Republic of Korea. Adrienne Helis Malvin Medical Research Foundation New Orleans LA 70130-2685 USA. Department of Anesthesiology West China Hospital Sichuan University. The Research Units of West China (2018RU012)-Chinese Academy of Medical Sciences West China Hospital Sichuan University Chengdu Sichuan 610041 PR China. Interdisciplinary Research Center on Biology and Chemistry Shanghai Institute of Organic Chemistry Chinese Academy of Sciences 26 Qiuyue Road Shanghai 201210 China. University of the Chinese Academy of Sciences 19 A Yuquan Road Shijingshan District Beijing 100049 China. Institute for NanoBioTechnology Johns Hopkins University Baltimore MD 21218 USA. Department of Materials Science and Engineering Whiting School of Engineering Johns Hopkins University Baltimore MD 21218 USA. Department of Brain and Cognitive Sciences Massachusetts Institute of Technology Cambridge MA 02139 USA. Picower Institute for Learning and Memory Cambridge MA 02139 USA. Harvard-MIT MD/PhD Program Harvard Medical School Boston MA 02115 USA. Department of Biological Science and Biotechnology Chungbuk Nati

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Research and development for HI intensity mapping

arXiv

引用

arXiv 2019年

作者： Timbie, Peter Ahmed, Zeeshan Alonso, David Amin, Mustafa A. Ansari, Réza Arena, Evan J. Bandura, Kevin Beardsley, Adam Bull, Philip Castorina, Emanuele Chang, Tzu-Ching Davé, Romeel van Engelen, Alexander Ewall-Wice, Aaron Ferraro, Simone Foreman, Simon Frisch, Josef Green, Daniel Holder, Gilbert Jacobs, Daniel Dillon, Joshua S. Karagiannis, Dionysios Kaurov, Alexander A. Knox, Lloyd Kuhn, Emily Liu, Adrian Ma, Yin-Zhe Masui, Kiyoshi W. McClintock, Thomas Moodley, Kavilan Münchmeyer, Moritz Newburgh, Laura B. Nomerotski, Andrei O'Connor, Paul Obuljen, Andrej Padmanabhan, Hamsa Parkinson, David Perdereau, Olivier Rapetti, David Saliwanchik, Benjamin Sehgal, Neelima Shaw, J. Richard Sheehy, Chris Sheldon, Erin Shirley, Raphael Silverstein, Eva Slatyer, Tracy Slosar, Anže Stankus, Paul Stebbins, Albert Timbie, Peter T. Tucker, Gregory S. Tyndall, William Villaescusa-Navarro, Francisco Wulf, Dallas UW-Madison SLAC National Accelerator Laboratory Menlo ParkCA94025 United States University of Oxford OxfordOX1 3RH United Kingdom Department of Physics & Astronomy Rice University HoustonTX77005 United States Université Paris-Sud LAL UMR 8607 Orsay CedexF-91898 France CNRS/IN2P3 OrsayF-91405 France Brookhaven National Laboratory UptonNY11973 United States Drexel University PhiladelphiaPA19104 United States CSEE West Virginia University MorgantownWV26505 United States Center for Gravitational Waves and Cosmology West Virginia University MorgantownWV26505 United States Arizona State University TempeAZ85287 United States Queen Mary University of London Mile End Road LondonE1 4NS United Kingdom Department of Physics & Astronomy University of the Western Cape Cape Town7535 South Africa Department of Physics University of California Berkeley BerkeleyCA94720 United States Jet Propulsion Laboratory California Institute of Technology PasadenaCA United States University of Edinburgh EdinburghEH8 9YL United Kingdom Canadian Institute for Theoretical Astrophysics University of Toronto TorontoONM5S 3H8 Canada Lawrence Berkeley National Laboratory BerkeleyCA94720 United States University of California San Diego La JollaCA92093 United States Department of Physics University of Illinois at Urbana-Champaign UrbanaIL61801 United States Department of Astronomy University of California Berkeley BerkeleyCA94720 United States Dipartimento di Fisica e Astronomia "G. Galilei" Università degli Studi di Padova via Marzolo 8 PadovaI-35131 Italy Istituto Nazionale di Fisica Nucleare Sezione di Padova via Marzolo 8 PadovaI-35131 Italy Institute for Advanced Study PrincetonNJ08540 United States University of California at Davis DavisCA95616 United States Department of Physics Yale University New HavenCT06520 United States McGill University MontrealQCH3A 2T8 Canada Astrophysics and Cosmology Research Unit School of Chemistry and Phy

Development of the hardware, data analysis, and simulation techniques for large compact radio arrays dedicated to mapping the 21 cm line of neutral hydrogen gas has proven to be more difficult than imagined twenty years ago when such telescopes were first proposed. Despite tremendous technical and methodological advances, there are several outstanding questions on how to optimally calibrate and analyze such data. On the positive side, it has become clear that the outstanding issues are purely technical in nature and can be solved with sufficient development activity. Such activity will enable science across redshifts, from early galaxy evolution in the pre-reionization era to dark energy evolution at low redshift. Copyright © 2019, The Authors. All rights reserved.

关键词： Mapping

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