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arXiv 2025年

作者： Shiraogawa, Takafumi Krug, Simon León Ehara, Masahiro von Lilienfeld, O. Anatole Institute for Molecular Science National Institutes of Natural Sciences 38 Nishigonaka Myodaiji Okazaki444-8585 Japan Research Center for Computational Science National Institutes of Natural Sciences 38 Nishigonaka Myodaiji Okazaki444-8585 Japan The Graduate University for Advanced Studies 38 Nishigonaka Myodaiji Okazaki444-8585 Japan Machine Learning Group Technische Universität Berlin Berlin10587 Germany Chemical Physics Theory Group Department of Chemistry University of Toronto St. George Campus TorontoM5S3H6 Ontario Canada Department of Materials Science and Engineering University of Toronto St. George Campus TorontoM5S 3E4 Ontario Canada Vector Institute for Artificial Intelligence TorontoM5S 1M1 Ontario Canada Berlin Institute for the Foundations of Learning and Data Berlin10587 Germany Department of Physics University of Toronto St. George Campus TorontoM5S 1A7 Ontario Canada Acceleration Consortium University of Toronto TorontoM5R 0A3 Ontario Canada

Understanding chemical compound space (CCS), a set of molecules and materials, is crucial for the rational discovery of molecules and materials. Concepts of symmetry have recently been introduced into CCS to account for near degeneracies and differences in electronic energies between iso-electronic materials. In this work, we present approximate relationships of response properties based on a first-principles view of CCS. They have been derived from perturbation theory and antisymmetry considerations involving nuclear charges. These rules allow approximate predictions of relative response properties of pairs of distinct compounds with opposite nuclear charge variations from a highly symmetric reference material, without the need for experiments or quantum chemical calculations of each compound. We numerically and statistically verified these rules for electric and magnetic response properties (electric dipole moment, polarizabilities, hyperpolarizabilities, and magnetizabilities) among charge-neutral and iso-electronic BN-doped polycyclic aromatic hydrocarbon derivatives of naphthalene, anthracene, and pyrene. Our analysis indicates that, despite their simplicity, antisymmetry rule-based predictions are remarkably accurate, enabling dimensionality reduction of CCS. Response properties in alchemical perturbation density functional theory were investigated to clarify the origin of this predictive power. © 2025, CC BY.

关键词： Naphthalene

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Multiple Peaks and a Long Precursor in the Type IIn Supernova 2021qqp: An Energetic Explosion in a Complex Circumstellar Environment

arXiv

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arXiv 2023年

作者： Hiramatsu, Daichi Matsumoto, Tatsuya Berger, Edo Ransome, Conor Villar, V. Ashley Gomez, Sebastian Cendes, Yvette De, Kishalay Bostroem, K. Azalee Farah, Joseph Howell, D. Andrew McCully, Curtis Newsome, Megan Gonzalez, Estefania Padilla Pellegrino, Craig Suzuki, Akihiro Terreran, Giacomo Center for Astrophysics Harvard & Smithsonian 60 Garden Street CambridgeMA02138-1516 United States The NSF AI Institute for Artificial Intelligence and Fundamental Interactions United States Department of Physics Columbia Astrophysics Laboratory Columbia University 538 West 120th Street New YorkNY10027 United States Department of Astronomy & Astrophysics The Pennsylvania State University 525 Davey Laboratory 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 Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States MIT-Kavli Institute for Astrophysics and Space Research 77 Massachusetts Avenue CambridgeMA02139 United States Steward Observatory University of Arizona 933 North Cherry Avenue TucsonAZ85721-0065 United States Las Cumbres Observatory 6740 Cortona Drive Suite 102 GoletaCA93117-5575 United States Department of Physics University of California Santa BarbaraCA93106-9530 United States Research Center for the Early Universe Graduate School of Science The University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo113-0033 Japan

We present optical photometry and spectroscopy of the Type IIn supernova (SN) 2021qqp. Its unusual light curve is marked by a long precursor for ≈ 300 days, a rapid increase in brightness for ≈ 60 days, and then a sharp increase of ≈ 1.6 mag in only a few days to a first peak of Mr ≈ −19.5 mag. The light curve then declines rapidly until it re-brightens to a second distinct peak of Mr ≈ −17.3 mag centered at ≈ 335 days after the first peak. The spectra are dominated by Balmer lines with a complex morphology, including a narrow component with a width of ≈ 1300 km s−1 (first peak) and ≈ 2500 km s−1 (second peak) that we associate with the circumstellar medium (CSM) and a P Cygni component with an absorption velocity of ≈ 8500 km s−1 (first peak) and ≈ 5600 km s−1 (second peak) that we associate with the SN–CSM interaction shell. Using the luminosity and velocity evolution, we construct a flexible analytical model, finding two significant mass-loss episodes with peak mass loss rates of ≈ 10 and ≈ 5 M☉ yr−1 about 0.8 and 2 yr before explosion, respectively, with a total CSM mass of ≈ 2 − 4 M☉. We show that the most recent mass-loss episode could explain the precursor for the year preceding the explosion. The SN ejecta mass is constrained to be ≈ 5 − 30 M☉ for an explosion energy of ≈ (3−10)×1051 erg. We discuss eruptive massive stars (luminous blue variable, pulsational pair instability) and an extreme stellar merger with a compact object as possible progenitor channels. © 2023, CC BY.

关键词： Supernovae

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The XLZD Design Book: Towards the Next-Generation Liquid Xenon Observatory for Dark Matter and Neutrino physics

arXiv

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arXiv 2024年

作者： Aalbers, J. Abe, K. Adrover, M. Maouloud, S. Ahmed Akerib, D.S. Al Musalhi, A.K. Alder, F. Althueser, L. Amaral, D.W.P. Amarasinghe, C.S. Ames, A. Andrieu, B. Angelides, N. Angelino, E. Antunovic, B. Aprile, E. Araújo, H.M. Armstrong, J.E. Arthurs, M. Babicz, M. Bajpai, D. Baker, A. Balzer, M. Bang, J. Barberio, E. Bargemann, J.W. Barillier, E. Basharina-Freshville, A. Baudis, L. Bauer, D. Bazyk, M. Beattie, K. Beaupere, N. Bell, N.F. Bellagamba, L. Benson, T. Bhatti, A. Biesiadzinski, T.P. Biondi, R. Biondi, Y. Birch, H.J. Bishop, E. Bismark, A. Boehm, C. Boese, K. Bolotnikov, A. Brás, P. Braun, R. Breskin, A. Brew, C.A.J. Brommer, S. Brown, A. Bruni, G. Budnik, R. Burdin, S. Cai, C. Capelli, C. Carini, G. Carmona-Benitez, M.C. Carter, M. Chauvin, A. Chawla, A. Chen, H. Cherwinka, J.J. Chin, Y.T. Chott, N.I. Chavez, A.P. Cimental Clark, K. Colijn, A.P. Colling, D.J. Conrad, J. Converse, M.V. Coronel, R. Costanzo, D. Cottle, A. Cox, G. Cuenca-García, J.J. Curran, D. Cussans, D. D’Andrea, V. Garcia, L.C. Daniel Darlington, I. Dave, S. David, A. Davies, G.J. Decowski, M.P. Deisting, A. Delgaudio, J. Dey, S. Di Donato, C. Di Felice, L. Di Gangi, P. Diglio, S. Ding, C. Dobson, J.E.Y. Doerenkamp, M. Drexlin, G. Druszkiewicz, E. Dunbar, C.L. Eitel, K. Elykov, A. Engel, R. Eriksen, S.R. Fayer, S. Fearon, N.M. Ferella, A.D. Ferrari, C. Fieldhouse, N. Fischer, H. Flaecher, H. Flehmke, T. Flierman, M. Fraser, E.D. Fruth, T.M.A. Fujikawa, K. Fulgione, W. Fuselli, C. Gaemers, P. Gaior, R. Gaitskell, R.J. Gallice, N. Galloway, M. Gao, F. Garroum, N. Geffre, A. Genovesi, J. Ghag, C. Ghosh, S. Giacomobono, R. Gibbons, R. Girard, F. Glade-Beucke, R. Glück, F. Gokhale, S. Grandi, L. Green, J. Grigat, J. van der Grinten, M.G.D. Größle, R. Guan, H. Guida, M. Gyorgy, P. Haiston, J.J. Hall, C.R. Hall, T. Hammann, R. Hannen, V. Hansmann-Menzemer, S. Hargittai, N. Hartigan-O’Connor, E. Haselschwardt, S.J. Hernandez, M. Hertel, S.A. Higuera, A. Hils, C. Nikhef the University of Groningen Van Swinderen Institute Groningen9747AG Netherlands University of Tokyo Higashi-Mozumi Kamioka Hida Gifu506-1205 Japan Physik-Institut University of Zürich Zürich8057 Switzerland LPNHE Sorbonne Université CNRS IN2P3 Paris75005 France SLAC National Accelerator Laboratory Menlo ParkCA94025-7015 United States Kavli Institute for Particle Astrophysics and Cosmology Stanford University StanfordCA94305-4085 United States LondonWC1E 6BT United Kingdom Institute for Nuclear Physics University of Münster Münster48149 Germany Department of Physics and Astronomy Rice University HoustonTX77005 United States Department of Physics University of California Santa Barbara Santa BarbaraCA93106-9530 United States Department of Physics Imperial College London Blackett Laboratory LondonSW7 2AZ United Kingdom INAF-Astrophysical Observatory of Torino Department of Physics University of Torino INFN-Torino Torino10125 Italy INFN-Laboratori Nazionali del Gran Sasso Gran Sasso Science Institute L’Aquila67100 Italy Vinca Institute of Nuclear Science University of Belgrade Mihajla Petrovica Alasa 12-14 Belgrade Serbia Physics Department Columbia University New YorkNY10027 United States Department of Physics University of Maryland College ParkMD20742-4111 United States Department of Physics & Astronomy University of Alabama TuscaloosaAL34587-0324 United States Department of Physics King’s College London LondonWC2R 2LS United Kingdom Institute for Data Processing and Electronics Karlsruhe Institute of Technology Karlsruhe76021 Germany Department of Physics Brown University ProvidenceRI02912-9037 United States ARC Centre of Excellence for Dark Matter Particle Physics School of Physics The University of Melbourne VIC3010 Australia SUBATECH IMT Atlantique CNRS IN2P3 Nantes Université Nantes44307 France BerkeleyCA94720-8099 United States Department of Physics and Astronomy University of Bologna INF

This report describes the experimental strategy and technologies for a next-generation xenon observatory sensitive to dark matter and neutrino physics. The detector will have an active liquid xenon target mass of 60–80 tonnes and is proposed by the XENON-LUX-ZEPLIN-DARWIN (XLZD) collaboration. The design is based on the mature liquid xenon time projection chamber technology of the current-generation experiments, LZ and XENONnT. A baseline design and opportunities for further optimization of the individual detector components are discussed. The experiment envisaged here has the capability to explore parameter space for Weakly Interacting Massive Particle (WIMP) dark matter down to the neutrino fog, with a 3σ evidence potential for spin-independent WIMP-nucleon cross sections as low as 3 × 10−49 cm2 (at 40 GeV/c2 WIMP mass). The observatory is also projected to have a 3σ observation potential of neutrinoless double-beta decay of 136Xe at a half-life of up to 5.7 × 1027 years. Additionally, it is sensitive to astrophysical neutrinos from the atmosphere, sun, and galactic supernovae. Copyright © 2024, The Authors. All rights reserved.

关键词： Dark Matter

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Neutrinoless Double Beta Decay Sensitivity of the XLZD Rare Event Observatory

arXiv

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arXiv 2024年

作者： Aalbers, J. Abe, K. Adrover, M. Maouloud, S. Ahmed Akerib, D.S. Musalhi, A.K. Al Alder, F. Althueser, L. Amaral, D.W.P. Amarasinghe, C.S. Ames, A. Andrieu, B. Angelides, N. Angelino, E. Antunovic, B. Aprile, E. Araújo, H.M. Armstrong, J.E. Arthurs, M. Babicz, M. Bajpai, D. Baker, A. Balzer, M. Bang, J. Barberio, E. Bargemann, J.W. Barillier, E. Basharina-Freshville, A. Baudis, L. Bauer, D. Bazyk, M. Beattie, K. Beaupere, N. Bell, N.F. Bellagamba, L. Benson, T. Bhatti, A. Biesiadzinski, T.P. Biondi, R. Biondi, Y. Birch, H.J. Bishop, E. Bismark, A. Boehm, C. Boese, K. Bolotnikov, A. Brás, P. Braun, R. Breskin, A. Brew, C.A.J. Brommer, S. Brown, A. Bruni, G. Budnik, R. Burdin, S. Cai, C. Capelli, C. Carini, G. Carmona-Benitez, M.C. Carter, M. Chauvin, A. Chawla, A. Chen, H. Cherwinka, J.J. Chin, Y.T. Chott, N.I. Chavez, A.P. Cimental Clark, K. Colijn, A.P. Colling, D.J. Conrad, J. Converse, M.V. Coronel, R. Costanzo, D. Cottle, A. Cox, G. Cuenca-García, J.J. Curran, D. Cussans, D. D’Andrea, V. Garcia, L.C. Daniel Darlington, I. Dave, S. David, A. Davies, G.J. Decowski, M.P. Deisting, A. Delgaudio, J. Dey, S. Di Donato, C. Di Felice, L. Di Gangi, P. Diglio, S. Ding, C. Dobson, J.E.Y. Doerenkamp, M. Drexlin, G. Druszkiewicz, E. Dunbar, C.L. Eitel, K. Elykov, A. Engel, R. Eriksen, S.R. Fayer, S. Fearon, N.M. Ferella, A.D. Ferrari, C. Fieldhouse, N. Fischer, H. Flaecher, H. Flehmke, T. Flierman, M. Fraser, E.D. Fruth, T.M.A. Fujikawa, K. Fulgione, W. Fuselli, C. Gaemers, P. Gaior, R. Gaitskell, R.J. Gallice, N. Galloway, M. Gao, F. Garroum, N. Geffre, A. Genovesi, J. Ghag, C. Ghosh, S. Giacomobono, R. Gibbons, R. Girard, F. Glade-Beucke, R. Glück, F. Gokhale, S. Grandi, L. Green, J. Grigat, J. van der Grinten, M.G.D. Größle, R. Guan, H. Guida, M. Gyorgy, P. Haiston, J.J. Hall, C.R. Hall, T. Hammann, R. Hannen, V. Hansmann-Menzemer, S. Hargittai, N. Hartigan-O’Connor, E. Haselschwardt, S.J. Hernandez, M. Hertel, S.A. Higuera, A. Hils, C. Nikhef The University of Groningen Van Swinderen Institute Groningen9747AG Netherlands University of Tokyo Higashi-Mozumi Kamioka Gifu Hida506-1205 Japan Physik-Institut University of Zürich Zürich8057 Switzerland LPNHE Sorbonne Université CNRS IN2P3 Paris75005 France SLAC National Accelerator Laboratory Menlo ParkCA94025-7015 United States Kavli Institute for Particle Astrophysics and Cosmology Stanford University StanfordCA94305-4085 United States LondonWC1E 6BT United Kingdom Institute for Nuclear Physics University of Münster Münster48149 Germany Department of Physics and Astronomy Rice University HoustonTX77005 United States Department of Physics University of California Santa Barbara Santa BarbaraCA93106-9530 United States Department of Physics Imperial College London Blackett Laboratory LondonSW7 2AZ United Kingdom INAF-Astrophysical Observatory of Torino Department of Physics University of Torino INFN-Torino Torino10125 Italy INFN-Laboratori Nazionali del Gran Sasso Gran Sasso Science Institute L’Aquila67100 Italy Vinca Institute of Nuclear Science University of Belgrade Mihajla Petrovica Alasa 12-14 Belgrade Serbia Physics Department Columbia University New YorkNY10027 United States Department of Physics University of Maryland College ParkMD20742-4111 United States Department of Physics & Astronomy University of Alabama TuscaloosaAL34587-0324 United States Department of Physics King’s College London LondonWC2R 2LS United Kingdom Institute for Data Processing and Electronics Karlsruhe Institute of Technology Karlsruhe76021 Germany Department of Physics Brown University ProvidenceRI02912-9037 United States ARC Centre of Excellence for Dark Matter Particle Physics School of Physics The University ofMelbourne VIC3010 Australia SUBATECH IMT Atlantique CNRS IN2P3 Nantes Université Nantes44307 France BerkeleyCA94720-8099 United States Department of Physics and Astronomy University of Bologna INFN

The XLZD collaboration is developing a two-phase xenon time projection chamber with an active mass of 60 to 80 t capable of probing the remaining WIMP-nucleon interaction parameter space down to the so-called neutrino fog. In this work we show that, based on the performance of currently operating detectors using the same technology and a realistic reduction of radioactivity in detector materials, such an experiment will also be able to competitively search for neutrinoless double beta decay in 136Xe using a natural-abundance xenon target. XLZD can reach a 3σ discovery potential half-life of 5.7×1027 yr (and a 90% CL exclusion of 1.3×1028 yr) with 10 years of data taking, corresponding to a Majorana mass range of 7.3–31.3 meV (4.8–20.5 meV). XLZD will thus exclude the inverted neutrino mass ordering parameter space and will start to probe the normal ordering region for most of the nuclear matrix elements commonly considered by the community. © 2024, CC BY-NC-SA.

关键词： Neutrons

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Astrometry and Precise Radial Velocities Yield a Complete Orbital Solution for the Nearby Eccentric Brown Dwarf LHS 1610 b

arXiv

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arXiv 2023年

作者： Fitzmaurice, Evan Stefánsson, Guðmundur Kavanagh, Robert D. Mahadevan, Suvrath Cañas, Caleb I. Winn, Joshua N. Robertson, Paul Ninan, Joe P. Albrecht, Simon Callingham, J.R. Cochran, William D. Delamer, Megan Kanodia, Shubham Lin, Andrea S.J. Marcussen, Marcus L. Pope, Benjamin J.S. Ramsey, Lawrence W. Roy, Arpita Vedantham, Harish Wright, Jason T. Department of Astronomy & Astrophysics Pennsylvania State University University ParkPA16802 United States Center for Exoplanets and Habitable Worlds Pennsylvania State University University ParkPA16802 United States Institute for Computational and Data Sciences The Pennsylvania State University University ParkPA16802 United States Institute for Computational and Data Sciences Scholar NASA Sagan Fellow United States Department of Astrophysical Sciences Princeton University 4 Ivy Lane PrincetonNJ08540 United States ASTRON Netherlands Institute for Radio Astronomy Oude Hoogeveensedijk 4 Dwingeloo7991 PD Netherlands NASA Postdoctoral Fellow United States NASA Goddard Space Flight Center 8800 Greenbelt Road GreenbeltMD20771 United States Department of Physics & Astronomy The University of California Irvine IrvineCA92697 United States Department of Astronomy and Astrophysics Tata Institute of Fundamental Research Homi Bhabha Road Colaba Mumbai400005 India Stellar Astrophysics Centre Department of Physics and Astronomy Aarhus University Ny Munkegade 120 Aarhus C8000 Denmark Leiden Observatory Leiden University PO Box 9513 Leiden2300 RA Netherlands McDonald Observatory Department of Astronomy The University of Texas at Austin 2515 Speedway AustinTX78712 United States Center for Planetary Systems Habitability The University of Texas at Austin 2515 Speedway AustinTX78712 United States Earth and Planets Laboratory Carnegie Institution for Science 5241 Broad Branch Road NW WashingtonDC20015 United States School of Mathematics & Physics University of Queensland St LuciaQLD4072 Australia Centre for Astrophysics University of Southern Queensland West Street ToowoombaQLD4350 Australia Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States Department of Physics and Astronomy Johns Hopkins University 3400 N Charles St BaltimoreMD21218 United States Kapteyn Astronomical Institute University of Groningen

We characterize the LHS 1610 system, a nearby (d = 9.7 pc) M5 dwarf hosting a brown dwarf in a 10.6 day, eccentric (e ∼ 0.37) orbit. A joint fit of the available Gaia two-body solution, discovery radial velocities (RVs) from TRES, and new RVs obtained with the Habitable-zone Planet Finder, yields an orbital inclination of 117.2 ±0.9◦ and a mass constraint of 50.9 ±0.9 MJ. This gives LHS 1610 b the second most precise mass of brown dwarfs orbiting M stars within 25pc. We highlight a discrepancy between the Gaia two-body solution eccentricity (e = 0.52±0.03) and that from the RVs (e = 0.3702± 0.0003), which requires the astrometric time-series release (Gaia DR4) for further diagnostics. With a flare rate of 0.28 ±0.07 flares/day from TESS photometry, and a rotation period of 84 ±8 days, LHS 1610 joins other mid M stars—including Proxima Centauri and YZ Ceti—as nearby mid M dwarfs with flare rates on the higher end for their long rotation periods. These stars are promising candidates for searching for sub-Alfvénic star-companion interactions, raising the question whether LHS 1610 b could be driving the flares on its host star. However, the available TESS photometry is insufficient to confirm or rule out any orbital phase-dependence of the flares. We show that the LHS 1610 system, as a nearby mid M star with a large, short-period companion, is a promising target to look for evidence of star-companion interactions or aural emission from the brown dwarf at radio wavelengths. Copyright © 2023, The Authors. All rights reserved.

关键词： Stars

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PKS J0805−0111: A Second Owens Valley Radio Observatory Blazar Showing Highly Significant Sinusoidal Radio Variability - The Tip of the Iceberg

arXiv

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arXiv 2024年

作者： de la Parra, P.V. Kiehlmann, S. Mróz, P. Readhead, A.C.S. Synani, A. Begelman, M.C. Blandford, R.D. Ding, Y. Harrison, F. Liodakis, I. Max-Moerbeck, W. Pavlidou, V. Reeves, R. Vallisneri, M. Aller, M.F. Graham, M.J. Hovatta, T. Lawrence, C.R. Lazio, T.J.W. Mahabal, A.A. Molina, B. O’Neill, S. Pearson, T.J. Ravi, V. Tassis, K. Zensus, J.A. CePIA Astronomy Department Universidad de Concepción Casilla 160-C Concepción Chile Department of Physics Institute of Theoretical and Computational Physics University of Crete Heraklion71003 Greece Astronomical Observatory University of Warsaw Al. Ujazdowskie 4 Warszawa00-478 Poland Owens Valley Radio Observatory California Institute of Technology PasadenaCA91125 United States Institute of Astrophysics Foundation for Research and Technology-Hellas HeraklionGR-70013 Greece JILA University of Colorado National Institute of Standards and Technology 440 UCB BoulderCO80309-0440 United States Department of Astrophysical and Planetary Sciences University of Colorado 391 UCB BoulderCO80309-0391 United States Kavli Institute for Particle Astrophysics and Cosmology Department of Physics 20 Stanford University StanfordCA94305 United States Cahill Center for Astronomy and Astrophysics California Institute of Technology PasadenaCA91125 United States NASA Marshall Space Flight Center HuntsvilleAL35812 United States Finnish Center for Astronomy with ESO University of Turku Vesilinnantie 5 FI-20014 Finland Departamento de Astronomía Universidad de Chile Camino El Observatorio 1515 Las Condes Santiago Chile Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Drive PasadenaCA91109 United States Department of Astronomy University of Michigan 323 West Hall 1085 S. University Avenue Ann ArborMI48109 United States Division of Physics Mathematics and Astronomy California Institute of Technology PasadenaCA91125 United States University of Turku University of Turku FI-20014 Finland Aalto University Metsähovi Radio Observatory Metsähovintie 114 Kylmälä02540 Finland Center for Data Driven Discovery California Institute of Technology PasadenaCA91125 United States Department of Physics Princeton University Jadwin Hall PrincetonNJ08540 United States Max-Planck-Institut für Radioastronomie Auf dem Hügel 69 BonnD-5312

Owens Valley Radio Observatory (OVRO) observations of supermassive black hole binary (SMBHB) candidate PKS 2131−021 revealed, for the first time, six likely characteristics of the phenomenology exhibited by SMBHB in blazars, of which the most unexpected and critical is sinusoidal flux density variations. We have now identified a second blazar, PKS J0805−0111, showing significant sinusoidal variations, with an observed period that translates to 1.422 ± 0.005 yr in the rest frame of the z = 1.388 object. We generate 106 simulated light curves to reproduce the radio variability characteristics of PKS J0805−0111, and show that the global probability, considering the look-elsewhere effect, indicates that the observed periodicity can be attributed to the red noise tail of the power spectral density, with a p0 value of 7.8 × 10−5 (i.e. 3.78σ). PKS J0805−0111 displays all six characteristics observed in PKS 2131−021. Taking into account the well-defined OVRO sample size, the false positive probability ∼ 0.22, but the rare behavior makes this a strong SMBHB candidate. The discovery of a second SMBHB candidate exhibiting these rare characteristics reveals that PKS 2131−021 is not a unique, isolated case. With these two strong cases we are clearly seeing only the tip of the iceberg. We estimate that the number of SMBHB candidates amongst blazars ∼ 1 in 100. © 2024, CC BY.

关键词： Landforms

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Beyond UVJ: Color Selection of Galaxies in the JWST Era

arXiv

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arXiv 2022年

作者： Antwi-Danso, Jacqueline Papovich, Casey Leja, Joel Marchesini, Danilo Marsan, Z. Cemile Martis, Nicholas S. Labbé, Ivo Muzzin, Adam Glazebrook, Karl Straatman, Caroline M.S. Tran, Kim-Vy H. George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy Texas A&m University College StationTX United States Department of Physics and Astronomy Texas A&m University 4242 TAMU College StationTX United States Department of Astronomy & Astrophysics The Pennsylvania State University University ParkPA16802 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 Department of Physics and Astronomy Tufts University MedfordMA United States Department of Physics and Astronomy York University TorontoON Canada Department of Astronomy and Physics St. Mary's University HalifaxNS Canada National Research Council of Canada Herzberg Astronomy & Astrophysics Research Centre 5071 West Saanich Road VictoriaBCV9E 2E7 Canada Center for Astrophysics & Supercomputing Swinburne University HawthornVIC Australia Department of Physics and Astronomy Ghent University Krijgslaan 281 S9 GentB-9000 Belgium Max-Planck Institut für Astronomie Königstuhl 17 HeidelbergD-69117 Germany School of Physics University of New South Wales Kensington Australia Arc Centre for Excellence in All-Sky Astrophysics in 3D Australia

We present a new rest-frame color-color selection method using "synthetic us- gsand gs- is", (ugi)scolors to identify star-forming and quiescent galaxies. Our method is similar to the widely-used U - V versus V - J (UVJ) diagram. However, UVJ suffers known systematics. Spectroscopic campaigns have shown that UVJ-selected quiescent samples at z 3 include ∼ 10 - 30% contamination from galaxies with dust-obscured star formation and strong emission lines. Moreover, at z > 3, UV J colors are extrapolated because the rest-frame J-band shifts beyond the coverage of the deepest bandpasses at soffers improvements to UVJ at z > 3, and can be applied to galaxies in the JWST era. We apply (ugi)sselection to galaxies at 0.5 0color by up to 1 magnitude, but changes (gs- is)0color by ≤ 0.2 mag, even at z ≅ 6. While (ugi)s-selected quiescent samples are comparable to UV J in completeness (both achieve ∼85-90% at z = 3-3.5), (ugi)sreduces contamination in quiescent samples by nearly a factor of two, from ≅35% to ≅17% at z = 3, and from ≅60% to ≅33% at z = 6. This leads to improvements in the true-to-false-positive ratio (TP/FP), where we find TP/FP 2.2 for (ugi)sat z ≅ 3.5 - 6, compared to TP/FP swill provide higher-fidelity samples. © 2022, CC BY.

关键词： Galaxies

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Analytical Rayleigh potential for the general relativistic Poynting-Robertson effect

arXiv

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arXiv 2019年

作者： de Falco, Vittorio Battista, Emmanuele Research Centre for Computational Physics and Data Processing Faculty of Philosophy & Science Silesian University in Opava Bezručovo nám. 13 OpavaCZ-746 01 Czech Republic

–We determine the analytic expression of the Rayleigh potential associated to the general relativistic Poynting-Robertson effect. This constitutes the first example of a physical dissipative system treated analytically in General Relativity. The employed approach and further implications are discussed. Copyright © 2019, The Authors. All rights reserved.

关键词： Relativity

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The need to implement FAIR principles in biomolecular simulations

arXiv

引用

arXiv 2024年

作者： Amaro, R. Åqvist, J. Bahar, I. Battistini, F. Bellaiche, A. Beltran, D. Biggin, P.C. Bonomi, M. Bowman, G.R. Bryce, R. Bussi, G. Carloni, P. Case, D. Cavalli, A. Chang, C.A. Cheatham, T.E. Cheung, M.S. Chipot, C. Chong, L.T. Choudhary, P. Cisneros, G.A. Clementi, C. Collepardo-Guevara, R. Coveney, P. Covino, R. Crawford, T.D. Dal Peraro, M. de Groot, B. Delemotte, L. De Vivo, M. Essex, J. Fraternali, F. Gao, J. Gelpí, J.L. Gervasio, F.L. Gonzalez-Nilo, F.D. Grubmüller, H. Guenza, M.G. Guzman, H.V. Harris, S. Head-Gordon, T. Hernandez, R. Hospital, A. Huang, N. Huang, X. Hummer, G. Iglesias-Fernández, J. Jensen, J.H. Jha, S. Jiao, W. Jorgensen, W.L. Kamerlin, S.C.L. Khalid, S. Laughton, C. Levitt, M. Limongelli, V. Lindahl, E. Lindorff-Larsen, K. Loverde, S. Lundborg, M. Luo, Y.L. Luque, F.J. Lynch, C.I. MacKerell, A. Magistrato, A. Marrink, S.J. Martin, H. McCammon, J.A. Merz, K. Moliner, V. Mulholland, A. Murad, S. Naganathan, A.N. Nangia, S. Noe, F. Noy, A. Oláh, J. O'Mara, M. Ondrechen, M.J. Onuchic, J.N. Onufriev, A. Osuna, S. Palermo, G. Panchenko, A.R. Pantano, S. Parish, C. Parrinello, M. Perez, A. Perez-Acle, T. Perilla, J.R. Pettitt, B.M. Pietropaolo, A. Piquemal, J.-P. Poma, A. Praprotnik, M. Ramos, M.J. Ren, P. Reuter, N. Roitberg, A. Rosta, E. Rovira, C. Roux, B. Röthlisberger, U. Sanbonmatsu, K. Schlick, T. Shaytan, A.K. Simmerling, C. Smith, J.C. Sugita, Y. Świderek, K. Taiji, M. Tao, P. Tikhonova, I.G. Tirado-Rives, J. Tuñón, I. Van Der Kamp, M.W. Van der Spoel, D. Velankar, S. Voth, G.A. Wade, R. Warshel, A. Welborn, V.V. Wetmore, S. Wong, C.F. Yang, L.-W. Zacharias, M. Orozco, M. Department of Molecular Biology University of California San DiegoCA United States Department of Cell and Molecular Biology Uppsala University Uppsala Sweden Laufer Center for Physical and Quantitative Biology Renaissance School of Medicine Stony Brook University Stony BrookNY United States Department of Biochemistry and Cell Biology Renaissance School of Medicine Stony Brook University Stony BrookNY United States Barcelona Spain European Molecular Biology Laboratory European Bioinformatics Institute Hinxton United Kingdom Structural Bioinformatics and Computational Biochemistry Department of Biochemistry University of Oxford Oxford United Kingdom Institut Pasteur Université Paris Cité CNRS UMR 3528 Computational Structural Biology Unit Paris France Department of Biochemistry and Biophysics University of Pennsylvania PhiladelphiaPA United States Division of Pharmacy and Optometry University of Manchester Manchester United Kingdom Scuola Internazionale Superiore di Studi Avanzati-SISSA Trieste Italy Computational Biomedicine Institute of Advanced Simulations IAS-5 Institute for Neuroscience and Medicine INM-9 Forschungszentrum Jülich GmbH Jülich Germany Department of Physics and Universitätsklinikum RWTH Aachen University Aachen Germany Department of Chemistry & Chemical Biology Rutgers University PiscatawayNJ United States Istituto Italiano di Tecnologia Drug Discovery and Development Bologna Italy Lausanne Switzerland Department of Chemistry University of California RiversideCA United States Department of Medicinal Chemistry College of Pharmacy University of Utah Salt Lake CityUT United States Department of Physics University of Washington SeattleWA United States Pacific Northwest National Laboratory RichlandWA United States LIA CNRS-UIUC UMR n°7019 Université de Lorraine Vandœuvre-lès-Nancy France Department of Physics University of Illinois at Urbana-Champaign UrbanaIL United States Department of Biochemistry and Molecular Biol

The communities that embraced data archiving efforts decades ago are now, in the era of data-driven biology, those gaining the most from the AI revolution. The structural biology community was a pioneer in this regard by establishing the Protein data Bank (PDB) in 1971 and making data accessible using the FAIR (Findable, Accessible, Interoperable and Reusable) principles even before these were articulated [1, 2]. The genomics/bioinformatics community has followed the example, establishing many widely used databases [3, 4]. By contrast, molecular simulation has been anchored in usage paradigms dating back to the seventies, when molecular dynamics (MD) simulation was first applied to study biomacromolecules [5]. At that time, MD was used by theoretical physicists and chemists in "proof of concept" simulations. Still, fifty years later, MD has evolved into a cornerstone molecular biology technique that can provide accurate quantitative analysis and property prediction. MD is now employed by tens of thousands of researchers worldwide, accounting for roughly 15% of global supercomputer usage. Unfortunately, these rich and costly data are not systematically maintained, and when further analyses are required, simulations have to be rerun-an unacceptable situation from scientific, environmental and sustainability standpoints. In this letter, we argue for a collaborative endeavor to archive MD simulation data and describe ongoing efforts to establish cost-effective and sustainable data archiving strategies. © 2024, CC BY-NC-SA.

关键词： Biotic

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Habitable zones around almost extremely spinning black holes (black sun revisited)

arXiv

引用

arXiv 2020年

作者： Bakala, Pavel Dočekal, Jan Turoňová, Zuzana Research Centre for Computational Physics and Data Processing Faculty of Philosophy and Science Bezrucovonam. 13 OpavaCZ-746 01 Czech Republic M. R. Stefánik Observatory and Planetarium Sládkovicova 41 Hlohovec920 01 Slovakia INAF - Osservatorio Astronomico di Roma Via Frascati 33 Monteporzio Catone Roma00078 Italy

We analyzed the thermodynamics of hypothetical exoplanets at very low Keplerian circular orbits in close vicinity of rapidly spinning supermassive black holes. Such black hole exoplanets are heated by strongly blueshifted and focused flux of the incoming cosmic microwave background (CMB) and cooled by the cold part of the local sky containing the black hole shadow. This gives rise to a temperature difference, which can drive processes far from thermodynamic equilibrium in a hypothetical life form inhabiting black hole exoplanets, similar to the case of a planet heated by the radiation of the parent star and cooled by the night sky. We found that for a narrow range of radii of very low Keplerian circular orbits and for very high spin of a supermassive black hole, the temperature regime of the black hole exoplanets corresponds to the habitable zone around standard stars. The thermodynamics of black hole exoplanets therefore, in principle, does not exclude the existence of life based on known biology. The peak of the multiblackbody spectral profile of the CMB heating the exoplanet is located in the ultraviolet band, but a significant fraction of the flux comes also in the visible and infrared bands. The minimum mass of a black hole ensuring the resistance to tidal disruption of an Earth-like exoplanet orbiting in the habitable zone is estimated to 1.63 108mo. Copyright © 2020, The Authors. All rights reserved.

关键词： Extrasolar planets

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