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arXiv 2023年

作者： Kilpatrick, Charles D. Foley, Ryan J. Jacobson-Galán, Wynn V. Piro, Anthony L. Smartt, Stephen J. Drout, Maria R. Gagliano, Alexander Gall, Christa Hjorth, Jens Jones, David O. Mandel, Kaisey S. Margutti, Raffaella Ramirez-Ruiz, Enrico Ransome, Conor L. Villar, V. Ashley Coulter, David A. Gao, Hua Matthews, David Jacob Taggart, Kirsty Zenati, Yossef Department of Physics and Astronomy Northwestern University EvanstonIL60208 United States Department of Astronomy and Astrophysics University of California Santa CruzCA95064 United States Department of Astronomy and Astrophysics University of California BerkeleyCA94720 United States The Observatories of the Carnegie Institution for Science 813 Santa Barbara St. PasadenaCA91101 United States Astrophysics Research Centre School of Mathematics and Physics Queen's University Belfast BelfastBT7 1NN United Kingdom Department of Physics University of Oxford Denys Wilkinson Building Keble Road OxfordOX1 3RH United Kingdom David A. Dunlap Department of Astronomy and Astrophysics University of Toronto 50 St. George Street TorontoONM5S 3H4 Canada Department of Astronomy University of Illinois 1002 W. Green St. Urbana-ChampaignIL61801 United States Center for Astrophysical Surveys National Center for Supercomputing Applications UrbanaIL61801 United States DARK Niels Bohr Institute University of Copenhagen Jagtvej 128 Copenhagen2200 Denmark Gemini Observatory NSF's NOIRLab 670 N. A'ohoku Place HiloHI96720 United States Institute of Astronomy Kavli Institute for Cosmology Madingley Road CambridgeCB3 0HA United Kingdom Department of Astronomy and Astrophysics The Pennsylvania State University Davey Lab State College PA16802 United States Institute for Computational & Data Sciences The Pennsylvania State University University ParkPA United States Institute for Gravitation and the Cosmos The Pennsylvania State University University ParkPA16802 United States Institute for Astronomy University of Hawaii 2680 Woodlawn Drive HonoluluHI96822 United States Department of Physics and Astronomy The Johns Hopkins University BaltimoreMD21218 United States ISEF International Fellowship

We present pre-explosion optical and infrared (IR) imaging at the site of the type II supernova (SN II) 2023ixf in Messier 101 at 6.9 Mpc. We astrometrically registered a ground-based image of SN 2023ixf to archival Hubble Space Telescope (HST), Spitzer Space Telescope (Spitzer), and ground-based near-IR images. A single point source is detected at a position consistent with the SN at wavelengths ranging from HST R-band to Spitzer 4.5 µm. Fitting to blackbody and red supergiant (RSG) spectral-energy distributions (SEDs), we find that the source is anomalously cool with a significant mid-IR excess. We interpret this SED as reprocessed emission in a 8600 R☉ circumstellar shell of dusty material with a mass ∼5×10−5 M☉ surrounding a log(L/L☉) = 4.74 ±0.07 and Teff = 3920+200−160 K RSG. This luminosity is consistent with RSG models of initial mass 11 M☉, depending on assumptions of rotation and overshooting. In addition, the counterpart was significantly variable in pre-explosion Spitzer 3.6 µm and 4.5 µm imaging, exhibiting ∼70% variability in both bands correlated across 9 yr and 29 epochs of imaging. The variations appear to have a timescale of 2.8 yr, which is consistent with κ-mechanism pulsations observed in RSGs, albeit with a much larger amplitude than RSGs such as α Orionis (Betelgeuse). © 2023, CC BY.

关键词： Supernovae

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A Next-Generation Liquid Xenon Observatory for Dark Matter and Neutrino physics

arXiv

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arXiv 2022年

作者： Aalbers, J. Abe, K. Aerne, V. Agostini, F. Ahmed Maouloud, S. Akerib, D.S. Akimov, D.Yu. Akshat, J. Al Musalhi, A.K. Alder, F. Alsum, S.K. Althueser, L. Amarasinghe, C.S. Amaro, F.D. Ames, A. Anderson, T.J. Andrieu, B. Angelides, N. Angelino, E. Angevaare, J. Antochi, V.C. Antón Martin, D. Antunovic, B. Aprile, E. Araújo, H.M. Armstrong, J.E. Arneodo, F. Arthurs, M. Asadi, P. Baek, S. Bai, X. Bajpai, D. Baker, A. Balajthy, J. Balashov, S. Balzer, M. Bandyopadhyay, A. Bang, J. Barberio, E. Bargemann, J.W. Baudis, L. Bauer, D. Baur, D. Baxter, A. Baxter, A.L. Bazyk, M. Beattie, K. Behrens, J. Bell, N.F. Bellagamba, L. Beltrame, P. Benabderrahmane, M. Bernard, E.P. Bertone, G.F. Bhattacharjee, P. Bhatti, A. Biekert, A. Biesiadzinski, T.P. Binau, A.R. Biondi, R. Biondi, Y. Birch, H.J. Bishara, F. Bismark, A. Blanco, C. Blockinger, G.M. Bodnia, E. Boehm, C. Bolozdynya, A.I. Bolton, P.D. Bottaro, S. Bourgeois, C. Boxer, B. Brás, P. Breskin, A. Breur, P.A. Brew, C.A.J. Brod, J. Brookes, E. Brown, A. Brown, E. Bruenner, S. Bruno, G. Budnik, R. Bui, T.K. Burdin, S. Buse, S. Busenitz, J.K. Buttazzo, D. Buuck, M. Buzulutskov, A. Cabrita, R. Cai, C. Cai, D. Capelli, C. Cardoso, J.M.R. Carmona-Benitez, M.C. Cascella, M. Catena, R. Chakraborty, S. Chan, C. Chang, S. Chauvin, A. Chawla, A. Chen, H. Chepel, V. Chott, N.I. Cichon, D. Cimental Chavez, A. Cimmino, B. Clark, M. Co, R.T. Colijn, A.P. Conrad, J. Converse, M.V. Costa, M. Cottle, A. Cox, G. Creaner, O. Cuenca Garcia, J.J. Cussonneau, J.P. Cutter, J.E. Dahl, C.E. D'Andrea, V. David, A. Decowski, M.P. Dent, J.B. Deppisch, F.F. de Viveiros, L. Di Gangi, P. Di Giovanni, A. Di Pede, S. Dierle, J. Diglio, S. Dobson, J.E.Y. Doerenkamp, M. Douillet, D. Drexlin, G. Druszkiewicz, E. Dunsky, D. Eitel, K. Elykov, A. Emken, T. Engel, R. Eriksen, S.R. Fairbairn, M. Fan, A. Fan, J.J. Farrell, S.J. Fayer, S. Fearon, N.M. Ferella, A. Ferrari, C. Fieguth, A. Fieguth, A. Fiorucci, S. SLAC National Accelerator Laboratory Menlo ParkCA94025 United States Kavli Institute for Particle Astrophysics and Cosmology Stanford University StanfordCA94305 United States Kamioka Observatory Institute for Cosmic Ray Research The University of Tokyo Higashi-Mozumi Kamioka Hida Gifu506-1205 Japan The University of Tokyo Kashiwa Chiba277-8582 Japan Physik-Institut University of Zurich Zurich8057 Switzerland Department of Physics and Astronomy University of Bologna INFN-Bologna Bologna40126 Italy LPNHE Sorbonne Université CNRS IN2P3 Paris75005 France Moscow115409 Russia Department of Physics and Astronomy Purdue University West LafayetteIN47907 United States Department of Physics University of Oxford Keble Rd OxfordOX1 3RH United Kingdom Department of Physics and Astronomy University College London LondonWC1E 6BT United Kingdom Department of Physics University of Wisconsin-Madison MadisonWI53706 United States Institut für Kernphysik Westfälische Wilhelms-Universität Münster Münster48149 Germany University of Michigan Randall Laboratory of Physics Ann ArborMI48109 United States LIBPhys Department of Physics University of Coimbra Coimbra3004-516 Portugal Department of Physics Blackett Laboratory Imperial College London LondonSW7 2BW United Kingdom INAF-Astrophysical Observatory of Torino Department of Physics University of Torino INFN-Torino Torino10125 Italy Nikhef The University of Amsterdam Science Park Amsterdam1098XG Netherlands Oskar Klein Centre Department of Physics Stockholm University AlbaNova StockholmSE-10691 Sweden Department of Physics Kavli Institute for Cosmological Physics The University of Chicago ChicagoIL60637 United States Vinca Institute of Nuclear Science University of Belgrade Mihajla Petrovica Alasa 12-14 Belgrade Serbia Faculty of Architecture Civil Engineering and Geodesy University of Banja Luka Bulevar vojvode Petra Bojovica 1a Banja Luka78000 Bosnia and Herzegovina Physics D

The nature of dark matter and properties of neutrinos are among the most pressing issues in contemporary particle physics. The dual-phase xenon time-projection chamber is the leading technology to cover the available parameter space for Weakly Interacting Massive Particles (WIMPs), while featuring extensive sensitivity to many alternative dark matter candidates. These detectors can also study neutrinos through neutrinoless double-beta decay and through a variety of astrophysical sources. A next-generation xenon-based detector will therefore be a true multi-purpose observatory to significantly advance particle physics, nuclear physics, astrophysics, solar physics, and cosmology. This review article presents the science cases for such a detector. © 2022, CC BY.

关键词： Dark Matter

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Spatial variations in aromatic hydrocarbon emission in a dust-rich galaxy

arXiv

引用

arXiv 2023年

作者： Spilker, Justin S. Phadke, Kedar A. Aravena, Manuel Archipley, Melanie Bayliss, Matthew B. Birkin, Jack E. Béthermin, Matthieu Burgoyne, James Cathey, Jared Chapman, Scott C. Dahle, Håkon Gonzalez, Anthony H. Gururajan, Gayathri Hayward, Christopher C. Hezaveh, Yashar D. Hill, Ryley Hutchison, Taylor A. Kim, Keunho J. Kim, Seonwoo Law, David Legin, Ronan Malkan, Matthew A. Marrone, Daniel P. Murphy, Eric J. Narayanan, Desika Navarre, Alex Olivier, Grace M. Rich, Jeffrey A. Rigby, Jane R. Reuter, Cassie Rhoads, James E. Sharon, Keren Smith, J.D.T. Solimano, Manuel Sulzenauer, Nikolaus Vieira, Joaquin D. Weiß, Axel Whitaker, Katherine E. Department of Physics and Astronomy George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy Texas A&M University 4242 TAMU College StationTX77843-4242 United States Department of Astronomy University of Illinois 1002 West Green St. UrbanaIL61801 United States Center for AstroPhysical Surveys National Center for Supercomputing Applications 1205 West Clark St. UrbanaIL61801 United States Núcleo de Astronomía de la Facultad de Ingeniería y Ciencias Universidad Diego Portales Av. Ejército Libertador 441 Santiago Chile Department of Physics University of Cincinnati CincinnatiOH45221 United States Aix Marseille Univ. CNRS CNES LAM Marseille France Department of Physics and Astronomy University of British Columbia 6225 Agricultural Rd. VancouverV6T 1Z1 Canada Department of Astronomy University of Florida 211 Bryant Space Sciences Center GainesvilleFL32611 United States National Research Council Herzberg Astronomy and Astrophysics 5701 West Saanich Rd. VictoriaV9E 2E7 Canada Department of Physics and Atmospheric Science Dalhousie University HalifaxNS Canada Institute of Theoretical Astrophysics University of Oslo P.O. Box 1029 Blindern OsloNO-0315 Norway University of Bologna Via Gobetti 93/2 BolognaI-40129 Italy INAF - Osservatorio di Astrofisica e Scienza dello Spazio Via Gobetti 93/3 BolognaI-40129 Italy Center for Computational Astrophysics Flatiron Institute 162 Fifth Avenue New YorkNY10010 United States Département de Physique Université de Montréal MontréalQCH3T 1J4 Canada Ciela - Montreal Institute for Astrophysical Data Analysis and Machine Learning Montréal Canada Mila - Québec Artificial Intelligence Institute Montréal Canada Observational Cosmology Lab NASA Goddard Space Flight Center Code 665 8800 Greenbelt Rd. GreenbeltMD20771 United States Space Telescope Science Institute 3700 San Martin Dr. BaltimoreMD21218 United States Department of Physics and Astronomy University of California

Dust grains absorb half of the radiation emitted by stars throughout the history of the universe, re-emitting this energy at infrared wavelengths.1-3 Polycyclic aromatic hydrocarbons (PAHs) are large organic molecules that trace millimeter-size dust grains and regulate the cooling of the interstellar gas within galaxies.4,5 Observations of PAH features in very distant galaxies have been difficult due to the limited sensitivity and wavelength coverage of previous infrared telescopes.6,7 Here we present JWST observations that detect the 3.3μm PAH feature in a galaxy observed less than 1.5 billion years after the Big Bang. The high equivalent width of the PAH feature indicates that star formation, rather than black hole accretion, dominates the infrared emission throughout the galaxy. The light from PAH molecules, large dust grains, and stars and hot dust are spatially distinct from one another, leading to order-of-magnitude variations in the PAH equivalent width and the ratio of PAH to total infrared luminosity across the galaxy. The spatial variations we observe suggest either a physical offset between the PAHs and large dust grains or wide variations in the local ultraviolet radiation field. Our observations demonstrate that differences in the emission from PAH molecules and large dust grains are a complex result of localized processes within early galaxies. Copyright © 2023, The Authors. All rights reserved.

关键词： Polycyclic aromatic hydrocarbons

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Medium Bands, Mega Science: a JWST/NIRCam Medium-Band Imaging Survey of Abell 2744

arXiv

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arXiv 2024年

作者： Suess, Katherine A. Weaver, John R. Price, Sedona H. Pan, Richard Wang, Bingjie Bezanson, Rachel Brammer, Gabriel Cutler, Sam E. Labbé, Ivo Leja, Joel Williams, Christina C. Whitaker, Katherine E. Dayal, Pratika de Graaff, Anna Feldmann, Robert Franx, Marijn Fudamoto, Yoshinobu Fujimoto, Seiji Furtak, Lukas J. Goulding, Andy D. Greene, Jenny E. Khullar, Gourav Kokorev, Vasily Kriek, Mariska Lorenz, Brian Marchesini, Danilo Maseda, Michael V. Matthee, Jorryt Miller, Tim B. Mitsuhashi, Ikki Mowla, Lamiya A. Muzzin, Adam Naidu, Rohan P. Nanayakkara, Themiya Nelson, Erica J. Oesch, Pascal A. Setton, David J. Shipley, Heath Smit, Renske Spilker, Justin S. van Dokkum, Pieter Zitrin, Adi Kavli Institute for Particle Astrophysics and Cosmology Department of Physics Stanford University StanfordCA94305 United States Department of Astronomy University of Massachusetts AmherstMA01003 United States Department of Physics and Astronomy PITT PACC University of Pittsburgh PittsburghPA15260 United States Department of Physics and Astronomy Tufts University 574 Boston Ave. MedfordMA02155 United States Department of Astronomy & Astrophysics The Pennsylvania State University University ParkPA16802 United States Institute for Computational & Data Sciences The Pennsylvania State University University ParkPA16802 United States Institute for Gravitation and the Cosmos The Pennsylvania State University University ParkPA16802 United States Copenhagen Denmark Niels Bohr Institute University of Copenhagen Jagtvej 128 Copenhagen Denmark Centre for Astrophysics and Supercomputing Swinburne University of Technology MelbourneVIC3122 Australia NSF’s National Optical-Infrared Astronomy Research Laboratory 950 North Cherry Avenue TucsonAZ85719 United States Denmark Kapteyn Astronomical Institute University of Groningen Groningen9700 AV Netherlands Max-Planck-Institut für Astronomie Königstuhl 17 HeidelbergD-69117 Germany Department of Astrophysics University of Zurich ZurichCH-8057 Switzerland Leiden Observatory Leiden University P.O.Box 9513 LeidenNL-2300 AA Netherlands Center for Frontier Science Chiba University 1-33 Yayoi-cho Inage-ku Chiba263-8522 Japan Department of Astronomy The University of Texas at Austin AustinTX78712 United States Department of Physics Ben-Gurion University of the Negev P.O. Box 653 Be’er-Sheva84105 Israel Department of Astrophysical Sciences Princeton University 4 Ivy Lane PrincetonNJ08544 United States Department of Astronomy University of California BerkeleyCA94720 United States Department of Physics & Astronomy Tufts University MA02155 United States Department of Astronomy University of W

In this paper, we describe the "Medium Bands, Mega Science" JWST Cycle 2 survey (JWST-GO-4111) and demonstrate the power of these data to reveal both the spatially-integrated and spatially-resolved properties of galaxies from the local universe to the era of cosmic dawn. Executed in November 2023, MegaScience obtained ∼ 30arcmin2 of deep multiband NIRCam imaging centered on the z ∼ 0.3 Abell 2744 cluster, including eleven medium-band filters and the two shortest-wavelength broad-band filters, F070W and F090W. Together, MegaScience and the UNCOVER Cycle 1 treasury program provide a complete set of deep (∼ 28−30magAB) images in all NIRCam medium- and broad-band filters. This unique dataset allows us to precisely constrain photometric redshifts, map stellar populations and dust attenuation for large samples of distant galaxies, and examine the connection between galaxy structures and formation histories. MegaScience also includes ∼ 17 arcmin2 of NIRISS parallel imaging in two broad-band and four medium-band filters from 0.9 − 4.8µm, expanding the footprint where robust spectral energy distribution (SED) fitting is possible. We provide example SEDs and multiband cutouts at a variety of redshifts, and use a catalog of JWST spectroscopic redshifts to show that MegaScience improves both the scatter and catastrophic outlier rate of photometric redshifts by factors of 2-3. Additionally, we demonstrate the spatially-resolved science enabled by MegaScience by presenting maps of the [OIII] line emission and continuum emission in three spectroscopically-confirmed z > 6 galaxies. We show that line emission in reionization-era galaxies can be clumpy, extended, and spatially offset from continuum emission, implying that galaxy assembly histories are complex even at these early epochs. We publicly release fully reduced mosaics and photometric catalogs for both the NIRCam primary and NIRISS parallel fields (***/megascience). Copyright © 2024, The Authors. All right

关键词： Galaxies

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Harmonized-Multinational qEEG norms (HarMNqEEG)

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NEUROIMAGE 2022年 256卷 119190-119190页

作者： Li, Min Wang, Ying Lopez-Naranjo, Carlos Hu, Shiang Reyes, Ronaldo Cesar Garcia Paz-Linares, Deirel Areces-Gonzalez, Ariosky Hamid, Aini Ismafairus Abd Evans, Alan C. Savostyanov, Alexander N. Calzada-Reyes, Ana Villringer, Arno Tobon-Quintero, Carlos A. Garcia-Agustin, Daysi Yao, Dezhong Dong, Li Aubert-Vazquez, Eduardo Reza, Faruque Razzaq, Fuleah Abdul Omar, Hazim Abdullah, Jafri Malin Galler, Janina R. Ochoa-Gomez, John F. Prichep, Leslie S. Galan-Garcia, Lidice Morales-Chacon, Lilia Valdes-Sosa, Mitchell J. Trondle, Marius Zulkifly, Mohd Faizal Mohd Rahman, Muhammad Riddha Bin Abdul Milakhina, Natalya S. Langer, Nicolas Rudych, Pavel Koenig, Thomas Virues-Alba, Trinidad A. Lei, Xu Bringas-Vega, Maria L. Bosch-Bayard, Jorge F. Valdes-Sosa, Pedro Antonio [a]The Clinical Hospital of Chengdu Brain Science Institute MOE Key Lab for Neuroinformation School of Life Science and Technology University of Electronic Science and Technology of China Chengdu China [b]Cuban Center for Neurocience La Habana Cuba [c]McGill Centre for Integrative Neuroscience Ludmer Centre for Neuroinformatics and Mental Health Montreal Neurological Institute Canada [d]Department of Neurosciences School of Medical Sciences Universiti Sains Malaysia Universiti Sains Malaysia Health Campus Kota Bharu Kelantan 16150 Malaysia [e]Brain and Behaviour Cluster School of Medical Sciences Universiti Sains Malaysia Health Campus Kota Bharu Kelantan 16150 Malaysia [f]Hospital Universiti Sains Malaysia Universiti Sains Malaysia Health Campus Kota Bharu Kelantan 16150 Malaysia [g]Humanitarian Institute Novosibirsk State University Novosibirsk 630090 Russia [h]Laboratory of Psychophysiology of Individual Differences Federal State Budgetary Scientific Institution Scientific Research Institute of Neurosciences and Medicine Novosibirsk 630117 Russia [i]Laboratory of Psychological Genetics at the Institute of Cytology and Genetics Siberian Branch of the Russian Academy of Sciences Novosibirsk 630090 Russia [j]University of Pinar del Río “Hermanos Saiz Montes de Oca” Pinar del Río Cuba [k]Department of Neurology Max Planck Institute for Human Cognitive and Brain Sciences Leipzig Germany [l]Department of Cognitive Neurology University Hospital Leipzig Leipzig Germany [m]Center for Stroke Research Charité-Universitätsmedizin Berlin Berlin Germany [n]Grupo Neuropsicología y Conducta - GRUNECO Faculty of Medicine Universidad de Antioquia Colombia [o]Research Department Institución Prestadora de Servicios de Salud IPS Universitaria Colombia [p]The Cuban center aging longevity and health Havana Cuba [q]Research Unit of NeuroInformation Chinese Academy of Medical Sciences Chengdu 2019RU035 China [r]School of Electrical Engineering Zhengzhou University Zhengzhou 4500

This paper extends frequency domain quantitative electroencephalography (qEEG) methods pursuing higher sensitivity to detect Brain Developmental Disorders. Prior qEEG work lacked integration of cross-spectral information omitting important functional connectivity descriptors. Lack of geographical diversity precluded accounting for site-specific variance, increasing qEEG nuisance variance. We ameliorate these weaknesses. (i) Create lifespan Riemannian multinational qEEG norms for cross-spectral tensors. These norms result from the HarMNqEEG project fostered by the Global Brain Consortium. We calculate the norms with data from 9 countries, 12 devices, and 14 studies, including 1564 subjects. Instead of raw data, only anonymized metadata and EEG cross spectral tensors were shared. After visual and automatic quality control, developmental equations for the mean and standard deviation of qEEG traditional and Riemannian DPs were calculated using additive mixed-effects models. We demonstrate qEEG "batch effects " and provide methods to calculate harmonized z-scores. (ii) We also show that harmonized Riemannian norms produce z-scores with increased diagnostic accuracy predicting brain dysfunction produced by malnutrition in the first year of life and detecting COVID induced brain dysfunction. (iii) We offer open code and data to calculate different individual z-scores from the HarMNqEEG dataset. These results contribute to developing bias-free, low-cost neuroimaging technologies applicable in various health settings.

关键词： Quantitative EEG EEG cross-spectrum Riemannian geometry Batch effects Z-score Harmonization Malnutrition Covid induced brain dysfunction Developmental Brain Chart

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Do cities have a unique magnetic pulse?

arXiv

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arXiv 2022年

作者： Dumont, Vincent Bowen, Trevor A. Roglans, Roger Dobler, Gregory Sharma, Mohit S. Karpf, Andy Bale, Stuart D. Wickenbrock, Arne Zhivun, Elena Kornack, Tom Wurtele, Jonathan S. Budker, Dmitry Computational Research Division Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Department Of Physics University Of California BerkeleyCA94720-7300 United States Space Sciences Laboratory University Of California BerkeleyCA94720-7300 United States Biden School Of Public Policy And Administration University Of Delaware NewarkDE19716 United States Department Of Physics And Astronomy University Of Delaware NewarkDE19716 United States Data Science Institute University Of Delaware NewarkDE19713 United States Center For Urban Science And Progress New York University BrooklynNY11201 United States Civil And Urban Engineering Tandon School Of Engineering New York University BrooklynNY11201 United States Institut Für Physik Universität Mainz Staudingerweg 7 Mainz55128 Germany Helmholtz Institut Mainz Staudingerweg 18 Mainz55128 Germany Twinleaf LLC 300 Deer Creek Drive PlainsboroNJ08536 United States Johannes Gutenberg-Universität Mainz Mainz55128 Germany Helmholtz Institut Mainz Mainz55128 Germany

We present a comparative analysis of urban magnetic fields between two American cities: Berkeley (California) and Brooklyn Borough of New York City (New York). Our analysis uses data taken over a four-week period during which magnetic field data were continuously recorded using a fluxgate magnetometer of 70 pT/√ Hz sensitivity. We identified significant differences in the magnetic signatures. In particular, we noticed that Berkeley reaches a near-zero magnetic field activity at night whereas magnetic activity in Brooklyn continues during nighttime. We also present auxiliary measurements acquired using magnetoresistive vector magnetometers (VMR), with sensitivity of 300 pT/√ Hz, and demonstrate how cross-correlation, and frequency-domain analysis, combined with data filtering can be used to extract urban magnetometry signals and study local anthropogenic activities. Finally, we discuss the potential of using magnetometer networks to characterize the global magnetic field of cities and give directions for future development. Copyright © 2022, The Authors. All rights reserved.

关键词： Magnetometers

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NGDEEP: The Star Formation and Ionization Properties of Galaxies at 1.7 < z < 3.4

arXiv

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arXiv 2024年

作者： Shen, Lu Papovich, Casey Matharu, Jasleen Pirzkal, Nor Hu, Weida Berg, Danielle A. Bagley, Micaela B. Backhaus, Bren E. Cleri, Nikko J. Dickinson, Mark Finkelstein, Steven L. Hathi, Nimish P. Huertas-Company, Marc Hutchison, Taylor A. Giavalisco, Mauro Grogin, Norman A. Jaskot, Anne E. Jung, Intae Kartaltepe, Jeyhan S. Koekemoer, Anton M. Lotz, Jennifer M. Pérez-González, Pablo G. Rothberg, Barry Simons, Raymond C. Vanderhoof, Brittany N. Yung, L.Y. Aaron Department of Physics and Astronomy Texas A&M University College StationTX77843-4242 United States George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy Texas A&M University College StationTX77843-4242 United States Denmark Niels Bohr Institute University of Copenhagen Jagtvej 128 N CopenhagenDK-2200 Denmark ESA AURA Space Telescope Science Institute United States Department of Astronomy The University of Texas at Austin AustinTX United States Department of Physics and Astronomy University of Kansas LawrenceKS66045 United States Department of Astronomy and Astrophysics The Pennsylvania State University University ParkPA16802 United States Institute for Computational and Data Sciences The Pennsylvania State University University ParkPA16802 United States Institute for Gravitation and the Cosmos The Pennsylvania State University University ParkPA16802 United States NSF’s National Optical-Infrared Astronomy Research Laboratory 950 N. Cherry Ave. TucsonAZ85719 United States Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States Instituto de Astrofísica de Canarias Tenerife La Laguna Spain Universidad de la Laguna Tenerife La Laguna Spain Université Paris-Cité LERMA Observatoire de Paris PSL Paris France Astrophysics Science Division NASA Goddard Space Flight Center 8800 Greenbelt Rd GreenbeltMD20771 United States University of Massachusetts Amherst 710 North Pleasant Street AmherstMA01003-9305 United States Space Telescope Science Institute BaltimoreMD United States Department of Physics and Astronomy Williams College WilliamstownMA01267 United States Space Telescope Science Institute BaltimoreMD21218 United States Laboratory for Multiwavelength Astrophysics School of Physics and Astronomy Rochester Institute of Technology 84 Lomb Memorial Drive RochesterNY14623 United States Space Telescope Science Institute 3700 San Martin Dr. BaltimoreMD21218 United Sta

We use JWST/NIRISS slitless spectroscopy from the Next Generation Deep Extragalactic Exploratory Public (NGDEEP) Survey to investigate the physical condition of 178 star-forming galaxies at 1.7 ∗/M☉) 7, nearly a factor of a hundred lower than previous studies. We focus on the [O ii]/[O iii] (O32) ratio which is primarily sensitive to the ionization state and with a secondary dependence on the gas-phase metallicity of the interstellar medium. We find significant ( 5σ) correlations between the O32 ratio and galaxy properties as O32 increases with decreasing stellar mass, decreasing star formation rate (SFR), increasing specific SFR (sSFR≡ SFR/M∗), and increasing equivalent width (EW) of Hα and Hβ. These trends suggest a tight connection between the ionization parameter and these galaxy properties. Galaxies at z ∼ 2 − 3 exhibit a higher O32 than local normal galaxies with the same stellar masses and SFRs, indicating that they have a higher ionization parameter and lower metallicity than local normal galaxies. In addition, we observe a mild evolutionary trend in the O32–EW(Hβ) relation from z ∼ 0 to z 5, where higher redshift galaxies show increased O32 and EW, with possibly higher O32 at fixed EW. We argue that both the enhanced recent star formation activity and the higher star formation surface density may contribute to the increase in O32 and the ionization parameter. Copyright © 2024, The Authors. All rights reserved.

关键词： Stars

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General relativistic Poynting-Robertson effect to diagnose wormholes existence: Static and spherically symmetric case

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Physical Review D 2020年第10期101卷 104037-104037页

作者： Vittorio De Falco Emmanuele Battista Salvatore Capozziello Mariafelicia De Laurentis Research Centre for Computational Physics and Data Processing Faculty of Philosophy and Science Silesian University in Opava Bezručovo nám. 13 CZ-746 01 Opava Czech Republic Institute for Theoretical Physics Karlsruhe Institute of Technology (KIT) 76128 Karlsruhe Germany Institute for Nuclear Physics Karlsruhe Institute of Technology (KIT) Hermann-von-Helmholtz-Platz 1 76344 Eggenstein-Leopoldshafen Germany Università degli studi di Napoli “Federico II ” Dipartimento di Fisica “Ettore Pancini” Complesso Universitario di Monte S. Angelo Via Cintia Edificio 6 80126 Napoli Italy Istituto Nazionale di Fisica Nucleare Sezione di Napoli Complesso Universitario di Monte S. Angelo Via Cintia Edificio 6 80126 Napoli Italy

We derive the equations of motion of a test particle in the equatorial plane around a static and spherically symmetric wormhole influenced by a radiation field including the general relativistic Poynting-Robertson effect. From the analysis of this dynamical system, we develop a diagnostic to distinguish a black hole from a wormhole, which can be timely supported by several and different observational data. This procedure is based on the possibility of having some wormhole metrics, which smoothly connect to the Schwarzschild metric in a small transition surface layer very close to the black hole event horizon. To detect such a metric change, we analyze the emission proprieties from the critical hypersurface (stable region where radiation and gravitational fields balance) together with those from an accretion disk in the Schwarzschild spacetime toward a distant observer. Indeed, if the observational data are well fitted within such a model, it immediately implies the existence of a black hole; while in the case of strong departures from such a description it means that a wormhole could be present. Finally, we discuss our results and draw conclusions.

关键词： Classical black holes General relativity General relativity equations & solutions General relativity formalism Gravitation Singularities In general relativity Accretion disk & black-hole plasma Astronomical black holes Astrophysical electromagnetic fields Numerical simulations in gravitation & astrophysics

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The effect of pre-impact spin on the Moon-forming collision

arXiv

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arXiv 2020年

作者： Ruiz-Bonilla, S. Eke, V.R. Kegerreis, J.A. Massey, R.J. Teodoro, L.F.A. Institute for Computational Cosmology Durham University South Road DurhamDH1 3LE United Kingdom Institute for Data Science Durham University South Road DurhamDH1 3LE United Kingdom BAERI/NASA Ames Research Center Moffett FieldCA United States School of Physics and Astronomy University of Glasgow ScotlandG12 8QQ United Kingdom

We simulate the hypothesised collision between the proto-Earth and a Mars-sized impactor that created the Moon. Amongst the resulting debris disk in some impacts, we find a self-gravitating clump of material. It is roughly the mass of the Moon, contains ∼ 1% iron like the Moon, and has its internal composition resolved for the first time. The clump contains mainly impactor material near its core but becomes increasingly enriched in proto-Earth material near its surface. A graduated composition has recently been measured in the oxygen isotope ratios of Apollo samples, suggesting incomplete mixing between proto-Earth and impactor material that formed the Moon. However, the formation of the Moon-sized clump depends sensitively on the spin of the impactor. To explore this, we develop a fast method to construct models of multi-layered, rotating bodies and their conversion into initial conditions for smoothed particle hydrodynamical (SPH) simulations. We use our publicly available code to calculate density and pressure profiles in hydrostatic equilibrium, then generate configurations of over a billion particles with SPH densities within 1% of the desired values. This algorithm runs in a few minutes on a desktop computer, for 107 particles, and allows direct control over the properties of the spinning body. In comparison, relaxation or spin-up techniques that take hours on a supercomputer before the structure of the rotating body is even known. Collisions that differ only in the impactor’s initial spin reveal a wide variety of outcomes: a merger, a grazing hit-and-run, or the creation of an orbiting proto-Moon. Copyright © 2020, The Authors. All rights reserved.

关键词： Hydrodynamics

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Accretion in strong field gravity with eXTP

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Science China(physics,Mechanics & Astronomy) 2019年第2期62卷 45-73页

作者： Alessandra De Rosa Phil Uttley LiJun Gou Yuan Liu Cosimo Bambi Didier Barret Tomaso Belloni Emanuele Berti Stefano Bianchi Ilaria Caiazzo Piergiorgio Casella Marco Feroci Valeria Ferrari Leonardo Gualtieri Jeremy Heyl Adam Ingram Vladimir Karas FangJun Lu Bin Luo Giorgio Matt Sara Motta Joseph Neilsen Paolo Pani Andrea Santangelo XinWen Shu JunFeng Wang Jian-Min Wang YongQuan Xue YuPeng Xu WeiMin Yuan YeFei Yuan Shuang-Nan Zhang Shu Zhang Ivan Agudo Lorenzo Amati Nils Andersson Cristina Baglio Pavel Bakala Altan Baykal Sudip Bhattacharyya Ignazio Bombaci NiccolóBucciantini Fiamma Capitanio Riccardo Ciolfi Wei K.Cui Filippo D'Ammando Thomas Dauser Melania Del Santo Barbara De Marco Tiziana Di Salvo Chris Done Michal Dovciak Andrew C.Fabian Maurizio Falanga Angelo Francesco Gambino Bruce Gendre Victoria Grinberg Alexander Heger Jeroen Homan Rosario Iaria JiaChen Jiang ChiChuan Jin Elmar Koerding Manu Linares Zhu Liu Thomas J.Maccarone Julien Malzac Antonios Manousakis Frédéric Marin Andea Marinucci Missagh Mehdipour Mariano Méndez Simone Migliari Cole Miller Giovanni Miniutti Emanuele Nardini Paul T.O'Brien Julian P.Osborne Pierre Olivier Petrucci Andrea Possenti Alessandro Riggio Jerome Rodriguez Andrea Sanna LiJing Shao Malgosia Sobolewska Eva Sramkova Abigail L.Stevens Holger Stiele Giulia Stratta Zdenek Stuchlik Jiri Svoboda Fabrizio Tamburini Thomas M.Tauris Francesco Tombesi Gabriel Torok Martin Urbanec Frederic Vincent QingWen Wu Feng Yuan Jean J.M.in't Zand Andrzej A.Zdziarski XinLin Zhou INAF-Istituto di Astrofisica e Planetologie Spaziali Via Fosso del Cavaliere Anton Pannekoek Institute for Astronomy University of Amsterdam National Astronomical Observatories Chinese Academy of Science Institute of High Energy Physics Chinese Academy of Science Center for Field Theory and Particle Physics and Department of Physics Fudan University IRAP Universitéde ToulouseCNRSUPSCNES INAF-Osservatorio Astronomico di Brera Department of Physics and Astronomy The University of MississippiUniversity Dipartimento di Matematica e Fisica Universitàdegli studi Roma Tre University of British Columbia INAF-Osservatorio Astronomico di Roma INFN-Roma 2 c/o Dipartimento di Fisica II Universit?di Roma"Tor Vergata" Dipartimento di Fisica Universitàdegli Studi di Roma"La Sapienza"&Sezione INFN Roma1 Department of Physics University of OxfordClarendon Laboratory Astronomical Institute Academy of Sciences School of Astronomy and Space Science Nanjing University MIT Kavli Institute for Astrophysics and Space Research Institut für Astronomie und Astrophysik Eberhard Karls Universität Department of Physics Anhui Normal University Department of Astronomy and Institute of Theoretical Physics and Astrophysics Xiamen University CAS Key Laboratory for Research in Galaxies and Cosmology Department of AstronomyUniversity of Science and Technology of China Instituto de Astrofísica de Andalucia(CSIC) Glorieta de la Astronomía s/n INAF-Istituto di Astrofisica Spaziale e Fisica cosmica di Bologna Mathematical Sciences and STAG Research Centre University of Southampton New York University Abu Dhabi Institute of Physics and Research Centre for Computational Physics and Data Processing Faculty of Philosophy&ScienceSilesian University in OpavaíBezru?ovo nám. Department of Physics Middle East Technical University Department of Astronomy and Astrophysics Tata Institute of Fundamental Research Dipartimento di Fisica Universit?di Pisa&INFN INAF-Osservatorio Astrofisico di Arcetri INAF-Osservatorio Astronomico di Padova INFN-TIFPA Trento Ins

In this paper we describe the potential of the enhanced X-ray Timing and Polarimetry(eXTP) mission for studies related to accretion flows in the strong field gravity regime around both stellar-mass and supermassive black-holes. eXTP has the unique capability of using advanced "spectral-timing-polarimetry" techniques to analyze the rapid variations with three orthogonal diagnostics of the flow and its geometry, yielding unprecedented insight into the inner accreting regions, the effects of strong field gravity on the material within them and the powerful outflows which are driven by the accretion process.

关键词： X-ray black holes physics accretion

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