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arXiv 2024年

作者： Rowland, Lucie E. Hodge, Jacqueline Bouwens, Rychard Piña, Pavel Mancera Hygate, Alexander Algera, Hiddo Aravena, Manuel Bowler, Rebecca da Cunha, Elisabete Dayal, Pratika Ferrara, Andrea Herard-Demanche, Thomas Inami, Hanae van Leeuwen, Ivana de Looze, Ilse Oesch, Pascal Pallottini, Andrea Phillips, Siân Rybak, Matus Schouws, Sander Smit, Renske Sommovigo, Laura Stefanon, Mauro van der Werf, Paul Leiden Observatory Leiden University P.O. Box 9513 Leiden2300 RA Netherlands Hiroshima Astrophysical Science Center Hiroshima University 1-3-1 Kagamiyama Higashi-Hiroshima Hiroshima739-8526 Japan National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo Japan Núcleo de Astronomía Facultad de Ingeniería y Ciencias Universidad Diego Portales Av. Ejército Libertador 441 Santiago Chile Jodrell Bank Centre for Astrophysics Department of Physics and Astronomy School of Natural Sciences The University of Manchester ManchesterM13 9PL United Kingdom International Centre for Radio Astronomy Research University of Western Australia 35 Stirling Hwy CrawleyWA6009 Australia Australia Kapteyn Astronomical Institute University of Groningen Groningen9700 AV Netherlands Scuola Normale Superiore Piazza dei Cavalieri 7 Pisa56126 Italy Sterrenkundig Observatorium Ghent University Krijgslaan281-S9 GhentB-9000 Belgium Department of Astronomy University of Geneva Chemin Pegasi 51 Versoix1290 Switzerland Copenhagen Denmark Astrophysics Research Institute Liverpool John Moores University 146 Brownlow Hill LiverpoolL3 5RF United Kingdom Faculty of Electrical Engineering Mathematics and Computer Science Delft University of Technology Mekelweg 4 Delft2628 CD Netherlands SRON - Netherlands Institute for Space Research Niels Bohrweg 4 CA Leiden2333 Netherlands Center for Computational Astrophysics Flatiron Institute 162 5th Avenue New YorkNY10010 United States Departament d’Astronomia i Astrofísica Universitat de València C. Dr. Moliner 50 Burjassot ValènciaE-46100 Spain Unidad Asociada CSIC "Grupo de Astrofísica Extragaláctica y Cosmología" Instituto de Física de Cantabria Universitat de València Spain

We present high resolution (∼ 0.14" = 710 pc) ALMA [CII] 158μm and dust continuum follow-up observations of REBELS-25, a [CII]-luminous (L[CII] = (1.7 ± 0.2) × 109L☉) galaxy at redshift z = 7.3065 ± 0.0001. These high resolution, high signal-to-noise observations allow us to study the sub-kpc morphology and kinematics of this massive (M∗ = 8+−42 × 109M☉) star-forming (SFRUV+IR = 199+−10163 M☉yr−1) galaxy in the Epoch of Reionisation. By modelling the kinematics with 3DBAROLO, we find it has a low velocity dispersion (σ¯ = 33 ± 9 km s−1) and a high ratio of ordered-to-random motion (Vrot, max/σ¯ = 11+−84), indicating that REBELS-25 is a dynamically cold disc. Additionally, we find that the [CII] distribution is well fit by a near-exponential disc model, with a Sérsic index, n, of 1.3 ± 0.2, and we see tentative evidence of more complex non-axisymmetric structures suggestive of a bar in the [CII] and dust continuum emission. By comparing to other high spatial resolution cold gas kinematic studies, we find that dynamically cold discs seem to be more common in the high redshift Universe than expected based on prevailing galaxy formation theories, which typically predict more turbulent and dispersion-dominated galaxies in the early Universe as an outcome of merger activity, gas accretion and more intense feedback. This higher degree of rotational support seems instead to be consistent with recent cosmological simulations that have highlighted the contrast between cold and warm ionised gas tracers, particularly for massive galaxies. We therefore show that dynamically settled disc galaxies can form as early as 700 Myr after the Big Bang. Copyright © 2024, The Authors. All rights reserved.

关键词： Galaxies

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Precision orbital dynamics from interstellar scintillation arcs for PSR J0437−4715

arXiv

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arXiv 2020年

作者： Reardon, Daniel J. Coles, William A. Bailes, Matthew Bhat, N.D. Ramesh Dai, Shi Hobbs, George B. Kerr, Matthew Manchester, Richard N. Oslowski, Stefan Parthasarathy, Aditya Russell, Christopher J. Shannon, Ryan M. Spiewak, Renée Toomey, Lawrence Tuntsov, Artem V. van Straten, Willem Walker, Mark A. Wang, Jingbo Zhang, Lei Zhu, Xing-Jiang Centre for Astrophysics and Supercomputing Swinburne University of Technology P.O. Box 218 HawthornVIC3122 Australia Australia Electrical and Computer Engineering University of California at San Diego La Jolla CA United States International Centre for Radio Astronomy Research Curtin University BentleyWA6102 Australia Australia Telescope National Facility CSIRO Astronomy & Space Science P.O. Box 76 EppingNSW1710 Australia Space Science Division Naval Research Laboratory WashingtonDC20375-5352 United States CSIRO Scientific Computing Services Australian Technology Park Locked Bag 9013 AlexandriaNSW1435 Australia Manly Astrophysics 15/41-42 East Esplanade ManlyNSW2095 Australia Institute for Radio Astronomy & Space Research Auckland University of Technology Private Bag 92006 Auckland1142 New Zealand Xinjiang Astronomical Observatory Chinese Academy of Sciences 150 Science 1-Street Xinjiang Urumqi830011 China National Astronomical Observatories Chinese Academy of Sciences A20 Datun Road Chaoyang District Beijing100101 China University of Chinese Academy of Sciences Beijing100049 China School of Physics and Astronomy Monash University VIC3800 Australia

Intensity scintillations of radio pulsars are known to originate from interference between waves scattered by the electron density irregularities of interstellar plasma, often leading to parabolic arcs in the two-dimensional power spectrum of the recorded dynamic spectrum. The degree of arc curvature depends on the distance to the scattering plasma and its transverse velocity with respect to the line-of-sight. We report the observation of annual and orbital variations in the curvature of scintillation arcs over a period of 16 years for the bright millisecond pulsar, PSR J0437−4715. These variations are the signature of the relative transverse motions of the Earth, pulsar, and scattering medium, which we model to obtain precise measurements of parameters of the pulsar’s binary orbit and the scattering medium itself. We observe two clear scintillation arcs in most of our >5000 observations and we show that they originate from scattering by thin screens located at distances D1 = 89.8 ± 0.4 pc and D2 = 124 ± 3 pc from Earth. The best-fit scattering model we derive for the brightest arc yields the pulsar’s orbital inclination angle i = 137.1 ± 0.3◦, and longitude of ascending node, Ω = 206.3 ± 0.4◦. Using scintillation arcs for precise astrometry and orbital dynamics can be superior to modelling variations in the diffractive scintillation timescale, because the arc curvature is independent of variations in the level of turbulence of interstellar plasma. This technique can be used in combination with pulsar timing to determine the full three-dimensional orbital geometries of binary pulsars, and provides parameters essential for testing theories of gravity and constraining neutron star masses. Copyright © 2020, The Authors. All rights reserved.

关键词： Pulsars

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A Conflict in the radio Frequency Spectrum of LEO-HTS and HEO-HTS Systems

A Conflict in the Radio Frequency Spectrum of LEO-HTS and HE...

引用

engineering and Telecommunication (EnT-MIPT)

作者： Valentin R. Anpilogov Andrey A. Gritsenko Yury N. Chekushkin Igor V. Zimin JSC “VSAT-TEL” Moscow Russia JSC Information Space Center “Severnaya Corona” Saint Petersburg Russia PhysTech-School of Radio Engineering and Computer Technologies Moscow Institute of Physics and Technology (State University) Dolgoprudny Russia

ISBN: (纸本)9781728104331

Many analytical companies associate the development of the satellite communications market with new LEO/MEO/HEO-HTS systems with the target function of broadband access. The basis of these systems is the use of multisatellite constellations. Their practical realization requires solving numerous scientific and technical problems. One of the most painful problems is the problem of electromagnetic compatibility (EMC) between projected systems as well as between projected and operating satellite networks. The article shows that the realization of any of LEO-HTS systems results in a conflict situation in the radio frequency spectrum of the fixed-satellite and broadcasting-satellite services (Ku, Ka, Q/V bands). It is shown by the example of the analysis of EMC of LEO-HTS OneWeb and HEO-HTS Express-RV systems, the latter being oriented to servicing the Arctic regions in the Ku band, that to parry this conflict situation, a decrease in the capacity of subscriber radio links of the Express-RV system and/or an increase in the size of its subscriber antennas are required. The results of the analysis are presented for several geographical locations of subscriber terminals (from 60° N and more) and show that time intervals of interference action and C/I values depend considerably on their location in the Express-RV coverage area.

关键词： Satellite broadcasting Interference Orbits Structural beams Receiving antennas Satellites

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Detecting bases of maximal cliques in a graph 12th

Detecting bases of maximal cliques in a graph

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12th International Conference on Future Information technology, FutureTech 2017

作者： Hao, Fei Park, Doo-Soon Pei, Zheng School of Computer Science Shaanxi Normal University Xi’an China Department of Computer Software Engineering Soonchunhyang University Asan Korea Republic of Center for Radio Administration and Technology Development Xihua University Chengdu China

ISBN: (纸本)9789811050404

Maximal Cliques Enumeration (MCE), as a fundamental problem, has been extensively investigated in many fields, such as social networks, and biological science and so forth. However, the existing research works usually ignore the formation principle of maximal cliques which can help us to speed up the detection of maximal cliques in a graph. This paper pioneers a novel problem on detection of bases of maximal cliques in a graph. We propose a formal concept analysis based approach for detecting the bases of maximal cliques and detection theorem. It is believed that our work can provide a new research solution and direction for future topological structure analysis in various complex networking systems. © Springer Nature Singapore Pte Ltd. 2017.

关键词： Formal concept analysis

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Galaxy clusters at z∼1 imaged by ALMA with the Sunyaev-Zel’dovich effect

arXiv

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arXiv 2022年

作者： Kitayama, Tetsu Ueda, Shutaro Okabe, Nobuhiro Akahori, Takuya Hilton, Matt Hughes, John P. Ichinohe, Yuto Kohno, Kotaro Komatsu, Eiichiro Lin, Yen-Ting Miyatake, Hironao Oguri, Masamune Sifón, Cristóbal Takakuwa, Shigehisa Takizawa, Motokazu Tsutsumi, Takahiro van Marrewijk, Joshiwa Wollack, Edward J. Department of Physics Toho University Chiba Funabashi274-8510 Japan No. 1 Section 4 Roosevelt Road Taipei10617 Taiwan Institute of Astronomy National Tsing Hua University Hsinchu30013 Taiwan Department of Physics Hiroshima University 1-3-1 Kagamiyama Higashi-Hiroshima Hiroshima739-8526 Japan Astrophysical Science Center Hiroshima University 1-3-1 Kagamiyama Higashi-Hiroshima Hiroshima739-8526 Japan Core Research for Energetic Universe Hiroshima University Department of Physics Hiroshima University 1-3-1 1-3-1 Kagamiyama Higashi-Hiroshima Hiroshima739-8526 Japan Physics Program Graduate School of Advanced Science and Engineering Hiroshima University 1-3-1 Kagamiyama Higashi-Hiroshima Hiroshima739-8526 Japan Mizusawa VLBI observatory National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Operation Division SKA Observatory Jodrell Bank Lower Withington MacclesfieldSK11 9DL United Kingdom Astrophysics Research Centre University of KwaZulu-Natal Westville Campus Durban4041 South Africa School of Mathematics Statistics & Computer Science University of KwaZulu-Natal Westville Campus Durban4041 South Africa Wits Centre for Astrophysics School of Physics University of the Witwatersrand Private Bag 3 Johannesburg2050 South Africa Department of Physics and Astronomy Rutgers The State University of New Jersey PiscatawayNJ08854-8019 United States Department of Physics Rikkyo University 3-34-1 Nishi-Ikebukuro Toshima-ku Tokyo171-8501 Japan Institute of Astronomy School of Science The University of Tokyo 2-21-1 Osawa Mitaka Tokyo181-0015 Japan Research Center for the Early Universe School of Science The University of Tokyo 7-3-1 Hongo Bunkyo Tokyo113-0033 Japan Max-Planck-Institut für Astrophysik Karl-Schwarzschild Str. 1 GarchingD-85741 Germany The University of Tokyo Institutes for Advanced Study The University of Tokyo 5-1-5 Kashiwanoha Chiba277-8583 Japan Nagoya University Nagoya464-8

We present high angular-resolution measurements of the thermal Sunyaev-Zel’dovich effect (SZE) toward two galaxy clusters, RCS J2319+0038 at z = 0.9 and HSC J0947−0119 at z = 1.1, by the Atacama Large Millimeter/submillimeter Array (ALMA) in Band 3. They are supplemented with available Chandra X-ray data, optical data taken by Hyper Suprime-Cam on Subaru, and millimeter-wave SZE data from the Atacama Cosmology Telescope. Taking into account departures from spherical symmetry, we have reconstructed non-parametrically the inner pressure profile of two clusters as well as electron temperature and density profiles for RCS J2319+0038. This is one of the first such measurements for an individual cluster at z >∼ 0.9. We find that the inner pressure profile of both clusters is much shallower than that of local cool-core clusters. Our results consistently suggest that RCS J2319+0038 hosts a weak cool core, where radiative cooling is less significant than in local cool cores. On the other hand, HSC J0947−0119 exhibits an even shallower pressure profile than RCS J2319+0038 and is more likely a non-cool-core cluster. The SZE centroid position is offset by more than 140 h−170kpc from the peaks of galaxy distribution in HSC J0947−0119, suggesting a stronger influence of mergers in this cluster. We conclude that these distant clusters are at a very early stage of developing the cool cores typically found in clusters at lower redshifts. Copyright © 2022, The Authors. All rights reserved.

关键词： Millimeter waves

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Wavelet-Based Video Coding: Modem Implementations and Prospects of Coding Efficiency Increase 4

Wavelet-Based Video Coding: Modem Implementations and Prospe...

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4th International Conference on engineering and Telecommunication, En and T 2017

作者： Bystrov, Kirill S. Gryzov, Gennady Yu. Dvorkovich, Alexander V. Dvorkovich, Viktor P. Multimedia Systems and Technology Lab. Moscow Institute of Physics and Technology Moscow Russia Fiztech-School of Radio Engineering and Computer Technology Moscow Institute of Physics and Technology Moscow Russia Multimedia Technology and Telecommunication Dep. Moscow Institute of Physics and Technology Moscow Russia

ISBN: (纸本)9781538645475

Discrete wavelet transform (DWT) have found a practical use in multiple applications of digital signal processing including image compression. Despite a set of advantages, DWT is still weakly used in modern video compression technique and systems. Here an observation of DWT usage prospects is presented for video coding in terms of multichannel wavelet video codec implementation. © 2017 IEEE.

关键词： Discrete wavelet transforms

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A New Algorithm for Attitude Detemination Based on Chicken Swarm Optimization

A New Algorithm for Attitude Detemination Based on Chicken S...

引用

International Conference on Digital Home (ICDH)

作者： Yuanfa Ji Yue Wu Xiyan Sun Suqing Yan Qidong Chen Baoqiang Du Guangxi Experiment Center of Information Science Guilin University of Electronic Technology Guilin China Guangxi Key Laboratory of Precision Navigation Technology and Application Guilin University of Electronic Technology Guilin China Key laboratory of radio wave environment and modeling technology Qingdao China School of Computer and Communication Engineering Zhengzhou University of Light Industry Zhengzhou China

In this paper a new algorithm for global navigation satellite system attitude determination based on CSO (Chicken Swarm Optimization) was developed. A distinct feature of this algorithm is the new optimization. The traditional LAMBDA algorithm for integer ambiguity resolution is time-consuming due to the large search space and complex calculation, so the attitude determination time is longer correspondingly. The optimization algorithm without search space based on least squares proposed in this paper improves the efficiency of fixing the integer ambiguity and applied to solve attitude problems. In conclusion, it is proven to work, offering a very efficient method of attitude determination.

关键词： Antennas Antenna measurements Position measurement Mathematical model Covariance matrices Global navigation satellite system Optimization

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Kinetic electrostatic waves and their association with current structures in the solar wind

arXiv

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arXiv 2021年

作者： Graham, Daniel B. Khotyaintsev, Yu.V. Vaivads, A. Edberg, N.J.T. Eriksson, A.I. Johansson, E. Sorriso-Valvo, L. Maksimovic, M. Souček, J. Píša, D. Bale, S.D. Chust, T. Kretzschmar, M. Krasnoselskikh, V. Lorfèvre, E. Plettemeier, D. Steller, M. Štverák, Š. Trávníček, P. Vecchio, A. Horbury, T.S. O'Brien, H. Evans, V. Angelini, V. Uppsala75121 Sweden Division of Space and Plasma Physics School of Electrical Engineering and Computer Science KTH Royal Institute of Technology Stockholm11428 Sweden LESIA Observatoire de Paris Université PSL CNRS Sorbonne Université Univ. Paris Diderot Sorbonne Paris Cité 5 place Jules Janssen Meudon92195 France Institute of Atmospheric Physics The Czech Academy of Sciences Prague Czech Republic Space Sciences Laboratory University of California BerkeleyCA United States Physics Department University of California BerkeleyCA United States LPP CNRS Ecole Polytechnique Sorbonne Université Observatoire de Paris Université Paris-Saclay Palaiseau Paris France LPC2E CNRS 3A avenue de la Recherche Scientifique Orléans France Université d'Orléans Orléans France CNES 18 Avenue Edouard Belin Toulouse31400 France Technische Universität Dresden Helmholtz Str. 10 DresdenD-01187 Germany Space Research Institute Austrian Academy of Sciences Graz Austria Astronomical Institute The Czech Academy of Sciences Prague Czech Republic Radboud Radio Lab Department of Astrophysics Radboud University Nijmegen Netherlands Imperial College London South Kensington Campus LondonSW7 2AZ United Kingdom

Context. A variety of kinetic electrostatic and electromagnetic waves develop in the solar wind. The relationship between these waves and larger-scale structures, such as current sheets and ongoing turbulence remain a topic of investigation. Similarly, the instabilities producing ion-acoustic waves in the solar wind remains an open question. Aims. The goals of this paper are to investigate kinetic electrostatic Langmuir and ion-acoustic waves in the solar wind at 0.5 AU and determine whether current sheets and associated streaming instabilities can produce the observed waves. The relationship between these waves and currents observed in the solar wind is investigated statistically. Methods. Solar Orbiter's radio and Plasma Waves (RPW) instrument suite provides high-resolution snapshots of the fluctuating electric field. The Low Frequency Receiver (LFR) resolves the waveforms of ion-acoustic waves and the Time Domain Sampler (TDS) resolves the waveforms of both ion-acoustic and Langmuir waves. Using these waveform data we determine when these waves are observed in relation to current structures in the solar wind, estimated from the background magnetic field. Results. Langmuir and ion-acoustic waves are frequently observed in the solar wind. Ion-acoustic waves are observed about 1% of the time at 0.5 AU. The waves are more likely to be observed in regions of enhanced currents. However, the waves typically do not occur at current structures themselves. The observed currents in the solar wind are too small to drive instability by the relative drift between single ion and electron populations. When multi-component ion and/or electron distributions are present the observed currents may be sufficient for instability. Ion beams are the most plausible source of ion-acoustic waves in the solar wind. The spacecraft potential is confirmed to be a reliable probe of the background electron density by comparing the peak frequencies of Langmuir waves with the plasma frequency calcu

关键词： Turbulence

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Solar Orbiter/RPW antenna calibration in the radio domain and its application to type III burst observations

arXiv

引用

arXiv 2021年

作者： Vecchio, A. Maksimovic, M. Krupar, V. Bonnin, X. Zaslavsky, A. Astier, P.L. Dekkali, M. Cecconi, B. Bale, S.D. Chust, T. Guilhem, E. Khotyaintsev, Yu.V. Krasnoselskikh, V. Kretzschmar, M. Lorfèvre, E. Plettemeier, D. Souček, J. Steller, M. Štverák, S. Trávníček, P. Vaivads, A. Radboud Radio Lab Department of Astrophysics Radboud University Nijmegen Netherlands Lesia Observatoire de Paris Université Psl Cnrs Sorbonne Université Université de Paris France Goddard Planetary Heliophysics Institute University of Maryland Baltimore County BaltimoreMD United States Heliophysics Science Division Nasa Goddard Space Flight Center GreenbeltMD United States Space Sciences Laboratory University of California BerkeleyCA United States Physics Department University of California BerkeleyCA United States Lpp Cnrs Ecole Polytechnique Sorbonne Université Observatoire de Paris Université Paris-Saclay Palaiseau Paris France Cnes 18 Avenue Edouard Belin Toulouse31400 France Uppsala Sweden LPC2E Cnrs 3A avenue de la Recherche Scientifique Orléans France Technische Universität Dresden Würzburger Str. 35 DresdenD-01187 Germany Institute of Atmospheric Physics of the Czech Academy of Sciences Prague Czech Republic Space Research Institute Austrian Academy of Sciences Graz Austria Astronomical Institute of the Czech Academy of Sciences Ondvrejov Czech Republic Space and Plasma Physics School of Electrical Engineering and Computer Science Kth Royal Institute of Technology Stockholm Sweden

Context. In order to allow for a comparison with the measurements from other antenna systems, the voltage power spectral density measured by the radio and Plasma waves receiver (RPW) on board Solar Orbiter needs to be converted into physical quantities that depend on the intrinsic properties of the radiation itself (e.g., the brightness of the source). Aims. The main goal of this study is to perform a calibration of the RPW dipole antenna system that allows for the conversion of the voltage power spectral density measured at the receiver's input into the incoming flux density. Methods. We used space observations from the Thermal Noise Receiver (TNR) and the High Frequency Receiver (HFR) to perform the calibration of the RPW dipole antenna system. Observations of type III bursts by theWind spacecraft are used to obtain a reference radio flux density for cross-calibrating the RPW dipole antennas. The analysis of a large sample of HFR observations (over about ten months), carried out jointly with an analysis of TNR-HFR data and prior to the antennas' deployment, allowed us to estimate the reference system noise of the TNR-HFR receivers. Results. We obtained the effective length, leff, of the RPW dipoles and the reference system noise of TNR-HFR in space, where the antennas and pre-amplifiers are embedded in the solar wind plasma. The obtained leffvalues are in agreement with the simulation and measurements performed on the ground. By investigating the radio flux intensities of 35 type III bursts simultaneously observed by Solar Orbiter and Wind, we found that while the scaling of the decay time as a function of the frequency is the same for the Waves and RPW instruments, their median values are higher for the former. This provides the first observational evidence that Type III radio waves still undergo density scattering, even when they propagate from the source, in a medium with a plasma frequency that is well below their own emission frequency. © 2021, CC BY.

关键词： Calibration

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ENERGY-EFFICIENT MICROWAVE COMPONENTS FOR MOBILE COMMUNICATION

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China Communications 2017年第2期14卷 19-20页

作者： Yuanan Liu Quanyuan Feng Fadhel M. Ghannouchi the electronic institute of china the school of information science and technology in southwest jiaotong university(swjtu) ChengduChina the institute of microelectronics of swjtu the electrical and computer engineering department schulich school of engineeringuniversity of calgaryCalgaryABCanada the intelligent rf radio laboratory(iradio lab) university of calgary royal society of canada the canadian academy of engineering-canadian academy of engineering the engineering institute of canada-engineering institute of canada ieee microwave theory and techniques society(ieee mtt-s)

In the coexisted world of 3G,4G,5G and many other specialized wireless communication systems,billions of connections could be existing for various information transmission ***,data show that the increase of network capacity is heavily more than the increase of the network energy efficiency in recent years,which could lead to more energy consumption per transmitted bit in the future *** basic units in mobile communication systems,microwave/RF components and modules play key roles

关键词： high data ENERGY-EFFICIENT MICROWAVE COMPONENTS FOR MOBILE COMMUNICATION PAPR show DPA

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