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arXiv 2022年

作者： Adams, C.B. Batista, P. Benbow, W. Brill, A. Brose, R. Buckley, J.H. Capasso, M. Christiansen, J.L. Errando, M. Feng, Qi Finley, J.P. Foote, G.M. Fortson, L. Furniss, A. Gallagher, G. Gent, A. Giuri, C. Hanlon, W.F. Hanna, D. Hassan, T. Hervet, O. Holder, J. Hona, B. Hughes, G. Humensky, T.B. Jin, W. Kaaret, P. Kertzman, M. Kieda, D. Kleiner, T.K. Krennrich, F. Kumar, S. Lang, M.J. Lundy, M. Maier, G. Millis, J. Moriarty, P. Mukherjee, R. Nievas-Rosillo, M. O'Brien, S. Ong, R.A. Otte, A.N. Patel, S. Patel, S.R. Pfrang, K. Pohl, M. Prado, R.R. Pueschel, E. Quinn, J. Ragan, K. Reynolds, P.T. Ribeiro, D. Roache, E. Ryan, J.L. Sadeh, I. Santander, M. Sembroski, G.H. Shang, R. Stevenson, B. Tucci, J.V. Vassiliev, V.V. Wakely, S.P. Weinstein, A. Wells, R.M. Williams, D.A. Williamson, And T.J. Acciari, V.A. Aniello, T. Ansoldi, S. Antonelli, L.A. Arbet Engels, A. Arcaro, C. Artero, M. Asano, K. Baack, D. Babić, A. Baquero, A. Barres de Almeida, U. Barrio, J.A. Batković, I. Becerra González, J. Bednarek, W. Bernardini, E. Bernardos, M. Berti, A. Besenrieder, J. Bhattacharyya, W. Bigongiari, C. Biland, A. Blanch, O. Bökenkamp, H. Bonnoli, G. Bošnjak, Ž. Burelli, I. Busetto, G. Carosi, R. Ceribella, G. Cerruti, M. Chai, Y. Chilingarian, A. Cikota, S. Colombo, E. Contreras, J.L. Cortina, J. Covino, S. D'Amico, G. D'Elia, V. Da Vela, P. Dazzi, F. De Angelis, A. De Lotto, B. Del Popolo, A. Delfino, M. Delgado, J. Delgado Mendez, C. Depaoli, D. Di Pierro, F. Di Venere, L. Do Souto Espiñeira, E. Dominis Prester, D. Donini, A. Dorner, D. Doro, M. Elsaesser, D. Fallah Ramazani, V. Fariña, L. Fattorini, A. Font, L. Fruck, C. Fukami, S. Fukazawa, Y. García López, R.J. Garczarczyk, M. Gasparyan, S. Gaug, M. Giglietto, N. Giordano, F. Gliwny, P. Godinović, N. Green, J.G. Green, D. Hadasch, D. Hahn, A. Heckmann, L. Herrera, J. Hrupec, D. Hütten, M. Inada, T. Iotov, R. Ishio, K. Iwamura, Y. Jiménez Martínez, I. Jormanainen, J. Physics Department Columbia University New YorkNY10027 United States DESY Platanenallee 6 Zeuthen 15738 Germany Center for Astrophysics | Harvard & Smithsonian CambridgeMA02138 United States N.A.S.A. Goddard Space-Flight Center Code 661 GreenbeltMD20771 United States Institute of Physics and Astronomy University of Potsdam Potsdam-Golm 14476 Germany Department of Physics Washington University St. LouisMO63130 United States Department of Physics and Astronomy Barnard College Columbia University NY10027 United States Physics Department California Polytechnic State University San Luis ObispoCA94307 United States Department of Physics and Astronomy Purdue University West LafayetteIN47907 United States Department of Physics and Astronomy The Bartol Research Institute University of Delaware NewarkDE19716 United States School of Physics and Astronomy University of Minnesota MinneapolisMN55455 United States Department of Physics California State University - East Bay HaywardCA94542 United States Department of Physics and Astrnomy Ball State University MuncieIN47306 United States School of Physics Center for Relativistic Astrophysics Georgia Institute of Technology 837 State Street NW AtlantaGA30332-0430 United States Physics Department McGill University MontrealQCH3A 2T8 Canada Santa Cruz Institute for Particle Physics Department of Physics University of California Santa CruzCA95064 United States Department of Physics and Astronomy University of Utah Salt Lake CityUT84112 United States Department of Physics and Astronomy University of Alabama TuscaloosaAL35487 United States Department of Physics and Astronomy University of Iowa Van Allen Hall Iowa CityIA52242 United States Department of Physics and Astronomy DePauw University GreencastleIN46135-0037 United States Department of Physics and Astronomy Iowa State University AmesIA50011 United States School of Physics National University of Ireland Galway University R

We report on a long-lasting, elevated gamma-ray flux state from VER J0521+211 observed by VERITAS, MAGIC, and Fermi-LAT in 2013 and 2014. The peak integral flux above 200 GeV measured with the nightly-binned light curve is (8.8 ± 0.4) × 10−7 ph m−2 s−1, or ∼37% of the Crab Nebula flux. Multiwavelength observations from X-ray, UV, and optical instruments are also presented. A moderate correlation between the X-ray and TeV gamma-ray fluxes was observed, and the X-ray spectrum appeared harder when the flux was higher. Using the gamma-ray spectrum and four models of the extragalactic background light (EBL), a conservative 95% confidence upper limit on the redshift of the source was found to be z ≤ 0.31. Unlike the gamma-ray and X-ray bands, the optical flux did not increase significantly during the studied period compared to the archival low-state flux. The spectral variability from optical to X-ray bands suggests that the synchrotron peak of the spectral energy distribution (SED) may become broader during flaring states, which can be adequately described with a one-zone synchrotron self-Compton model varying the high-energy end of the underlying particle spectrum. The synchrotron peak frequency of the SED, as well as the radio morphology of the jet from the MOJAVE program, are consistent with the source being an intermediate-frequency-peaked BL Lac object. © 2022, CC BY.

关键词： Galaxies

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Identification of Antiferromagnetic Domains Via the Optical Magnetoelectric Effect

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physical Review Letters 2018年第5期121卷 057601-057601页

作者： Vilmos Kocsis Karlo Penc Toomas Rõõm Urmas Nagel Jakub Vít Judit Romhányi Yusuke Tokunaga Yasujiro Taguchi Yoshinori Tokura István Kézsmárki Sándor Bordács RIKEN Center for Emergent Matter Science (CEMS) Wako Saitama 351-0198 Japan Department of Physics Budapest University of Technology and Economics and MTA-BME Lendület Magneto-optical Spectroscopy Research Group 1111 Budapest Hungary Institute for Solid State Physics and Optics Wigner Research Centre for Physics Hungarian Academy of Sciences H-1525 Budapest P.O.B. 49 Hungary National Institute of Chemical Physics and Biophysics 12618 Tallinn Estonia Institute of Physics ASCR Na Slovance 2 182 21 Prague 8 Czech Republic Faculty of Nuclear Science and Physical Engineering Czech Technical University Břehová 7 115 19 Prague 1 Czech Republic Okinawa Institute of Science and Technology Graduate University Onna-son Okinawa 904-0395 Japan Department of Advanced Materials Science University of Tokyo Kashiwa 277-8561 Japan Quantum-Phase Electronics Center Department of Applied Physics University of Tokyo Tokyo 113-8656 Japan Department of Applied Physics University of Tokyo Hongo Tokyo 113-8656 Japan Experimental Physics 5 Center for Electronic Correlations and Magnetism Institute of Physics University of Augsburg 86159 Augsburg Germany Hungarian Academy of Sciences Premium Postdoctor Program 1051 Budapest Hungary

The ultimate goal of multiferroic research is the development of a new-generation nonvolatile memory devices, where magnetic bits are controlled via electric fields with low energy consumption. Here, we demonstrate the optical identification of magnetoelectric (ME) antiferromagnetic (AFM) domains in the LiCoPO4 exploiting the strong absorption difference between the domains. This unusual contrast, also present in zero magnetic field, is attributed to the dynamic ME effect of the spin-wave excitations, as confirmed by our microscopic model, which also captures the characteristics of the observed static ME effect. The control and the optical readout of AFM/ME domains, demonstrated here, will likely promote the development of ME and spintronic devices based on AFM insulators.

关键词： Magnetoelectric effect Optical & microwave phenomena Multiferroics Single crystal materials Terahertz spectroscopy

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Correction to: Dissociating motor learning from recovery in exoskeleton training post-stroke

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Journal of neuroengineering and rehabilitation 2018年第1期15卷 120页

作者： Nicolas Schweighofer Chunji Wang Denis Mottet Isabelle Laffont Karima Bakhti David J Reinkensmeyer Olivier Rémy-Néris Biokinesiology and Physical Therapy University of Southern California Los Angeles USA. schweigh@usc.edu. Neuroscience graduate Program University of Southern California Los Angeles USA. STAPS Université de Montpellier Euromov Montpellier France. Montpellier University Hospital Euromov IFRH Montpellier University Montpellier France. Departments of Mechanical and Aerospace Engineering Anatomy and Neurobiology University of California Irvine USA. Université de Bretagne Occidentale Centre hospitalier universitaire LaTIM-INSERM UMR1101 Brest France.

The original article [1] contained an error whereby the co-author, Karima Bakhti's name was displayed incorrectly.

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Early Release Science of the exoplanet WASP-39b with JWST NIRCam

arXiv

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arXiv 2022年

作者： Ahrer, Eva-Maria Stevenson, Kevin B. Mansfield, Megan Moran, Sarah E. Brande, Jonathan Morello, Giuseppe Murray, Catriona A. Nikolov, Nikolay K. Petit dit de la Roche, Dominique J.M. Schlawin, Everett Wheatley, Peter J. Zieba, Sebastian Batalha, Natasha E. Damiano, Mario Goyal, Jayesh M. Lendl, Monika Lothringer, Joshua D. Mukherjee, Sagnick Ohno, Kazumasa Batalha, Natalie M. Battley, Matthew P. Bean, Jacob L. Beatty, Thomas G. Benneke, Björn Berta-Thompson, Zachory K. Carter, Aarynn L. Cubillos, Patricio E. Daylan, Tansu Espinoza, Néstor Gao, Peter Gibson, Neale P. Gill, Samuel Harrington, Joseph Hu, Renyu Kreidberg, Laura Lewis, Nikole K. Line, Michael R. López-Morales, Mercedes Parmentier, Vivien Powell, Diana K. Sing, David K. Tsai, Shang-Min Wakeford, Hannah R. Welbanks, Luis Alam, Munazza K. Alderson, Lili Allen, Natalie H. Anderson, David R. Barstow, Joanna K. Bayliss, Daniel Bell, Taylor J. Blecic, Jasmina Bryant, Edward M. Burleigh, Matthew R. Carone, Ludmila Casewell, S.L. Changeat, Quentin Chubb, Katy L. Crossfield, Ian J.M. Crouzet, Nicolas Decin, Leen Désert, Jean-Michel Feinstein, Adina D. Flagg, Laura Fortney, Jonathan J. Gizis, John E. Heng, Kevin Iro, Nicolas Kempton, Eliza M.-R. Kendrew, Sarah Kirk, James Knutson, Heather A. Komacek, Thaddeus D. Lagage, Pierre-Olivier Leconte, Jérémy Lustig-Yaeger, Jacob MacDonald, Ryan J. Mancini, Luigi May, E.M. Mayne, N.J. Miguel, Yamila Mikal-Evans, Thomas Molaverdikhani, Karan Palle, Enric Piaulet, Caroline Rackham, Benjamin V. Redfield, Seth Rogers, Laura K. Roy, Pierre-Alexis Rustamkulov, Zafar Shkolnik, Evgenya L. Sotzen, Kristin S. Taylor, Jake Tremblin, P. Tucker, Gregory S. Turner, Jake D. de Val-Borro, Miguel Venot, Olivia Zhang, Xi Centre for Exoplanets and Habitability University of Warwick Coventry United Kingdom Department of Physics University of Warwick Coventry United Kingdom Johns Hopkins APL LaurelMD United States Steward Observatory University of Arizona TucsonAZ United States NHFP Sagan Fellow United States Lunar and Planetary Laboratory University of Arizona TucsonAZ United States Department of Physics & Astronomy University of Kansas LawrenceKS United States Tenerife Spain Tenerife Spain INAF- Palermo Astronomical Observatory Piazza del Parlamento Palermo Italy Department of Astrophysical and Planetary Sciences University of Colorado BoulderCO United States Space Telescope Science Institute BaltimoreMD United States Département d'Astronomie Université de Genève Sauverny Switzerland Max Planck Institute for Astronomy Heidelberg Germany Leiden Observatory University of Leiden Leiden Netherlands NASA Ames Research Center Moffett Field CA United States Jet Propulsion Laboratory PasadenaCA United States HBNI Odisha India Department of Physics Utah Valley University OremUT United States Department of Astronomy & Astrophysics University of California Santa Cruz Santa CruzCA United States Astrobiology Program UC Santa Cruz Santa CruzCA United States Department of Astronomy & Astrophysics University of Chicago ChicagoIL United States Department of Astronomy University of Wisconsin-Madison MadisonWI United States Department of Physics Institute for Research on Exoplanets Université de Montréal MontrealQC Canada Space Research Institute Austrian Academy of Sciences Graz Austria INAF Osservatorio Astrofisico di Torino Pino Torinese Italy Department of Astrophysical Sciences Princeton University PrincetonNJ United States LSSTC Catalyst Fellow Department of Physics & Astronomy Johns Hopkins University BaltimoreMD United States Earth and Planets Laboratory Carnegie Institution for Science WashingtonDC United States School of Physics Trinity Col

Measuring the metallicity and carbon-to-oxygen (C/O) ratio in exoplanet atmospheres is a fundamental step towards constraining the dominant chemical processes at work and, if in equilibrium, revealing planet formation histories. Transmission spectroscopye.g., 1,2 provides the necessary means by constraining the abundances of oxygen- and carbon-bearing species;however, this requires broad wavelength coverage, moderate spectral resolution, and high precision that, together, are not achievable with previous observatories. Now that JWST has commenced science operations, we are able to observe exoplanets at previously uncharted wavelengths and spectral resolutions. Here we report time-series observations of the transiting exoplanet WASP-39b using JWST’s Near InfraRed Camera (NIRCam). The long-wavelength spectroscopic and short-wavelength photometric light curves span 2.0 – 4.0 µm, exhibit minimal systematics, and reveal well-defined molecular absorption features in the planet’s spectrum. Specifically, we detect gaseous H2O in the atmosphere and place an upper limit on the abundance of CH4. The otherwise prominent CO2 feature at 2.8 µm is largely masked by H2O. The best-fit chemical equilibrium models favour an atmospheric metallicity of 1–100× solar (i.e., an enrichment of elements heavier than helium relative to the Sun) and a sub-stellar carbon-to-oxygen (C/O) ratio. The inferred high metallicity and low C/O ratio may indicate significant accretion of solid materials during planet formatione.g., 3,4 or disequilibrium processes in the upper atmospheree.g., 5,6 © 2022, CC BY.

关键词： Spectral resolution

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Early Release Science of the exoplanet WASP-39b with JWST NIRISS

arXiv

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arXiv 2022年

作者： Feinstein, Adina D. Radica, Michael Welbanks, Luis Murray, Catriona Anne Ohno, Kazumasa Coulombe, Louis-Philippe Espinoza, Néstor Bean, Jacob L. Teske, Johanna K. Benneke, Björn Line, Michael R. Rustamkulov, Zafar Saba, Arianna Tsiaras, Angelos Barstow, Joanna K. Fortney, Jonathan J. Gao, Peter Knutson, Heather A. MacDonald, Ryan J. Mikal-Evans, Thomas Rackham, Benjamin V. Taylor, Jake Parmentier, Vivien Batalha, Natalie M. Berta-Thompson, Zachory K. Carter, Aarynn L. Changeat, Quentin Dos Santos, Leonardo A. Gibson, Neale P. Goyal, Jayesh M. Kreidberg, Laura López-Morales, Mercedes Lothringer, Joshua D. Miguel, Yamila Molaverdikhani, Karan Moran, Sarah E. Morello, Giuseppe Mukherjee, Sagnick Sing, David K. Stevenson, Kevin B. Wakeford, Hannah R. Ahrer, Eva-Maria Alam, Munazza K. Alderson, Lili Allen, Natalie H. Batalha, Natasha E. Bell, Taylor J. Blecic, Jasmina Brande, Jonathan Caceres, Claudio Casewell, S.L. Chubb, Katy L. Crossfield, Ian J.M. Crouzet, Nicolas Cubillos, Patricio E. Decin, Leen Désert, Jean-Michel Harrington, Joseph Heng, Kevin Henning, Thomas Iro, Nicolas Kempton, Eliza M.-R. Kendrew, Sarah Kirk, James Krick, Jessica Lagage, Pierre-Olivier Lendl, Monika Mancini, Luigi Mansfield, Megan May, E.M. Mayne, N.J. Nikolov, Nikolay K. Palle, Enric Petit dit de la Roche, Dominique J.M. Piaulet, Caroline Powell, Diana Redfield, Seth Rogers, Laura K. Roman, Michael T. Roy, Pierre-Alexis Nixon, Matthew C. Schlawin, Everett Tan, Xianyu Tremblin, P. Turner, Jake D. Venot, Olivia Waalkes, William C. Wheatley, Peter J. Zhang, Xi Department of Astronomy & Astrophysics University of Chicago ChicagoIL United States NSF Graduate Research Fellow Department of Physics Institute for Research on Exoplanets Université de Montréal MontrealQC Canada School of Earth and Space Exploration Arizona State University TempeAZ United States NHFP Sagan Fellow Department of Astrophysical and Planetary Sciences University of Colorado BoulderCO United States Department of Astronomy & Astrophysics University of California Santa Cruz Santa CruzCA United States Space Telescope Science Institute BaltimoreMD United States Department of Physics & Astronomy Johns Hopkins University BaltimoreMD United States Earth and Planets Laboratory Carnegie Institution for Science WashingtonDC United States Department of Earth and Planetary Sciences Johns Hopkins University BaltimoreMD United States Department of Physics and Astronomy University College London United Kingdom INAF - Osservatorio Astrofisico di Arcetri Largo E. Fermi 5 Firenze Italy School of Physical Sciences The Open University Milton Keynes United Kingdom Division of Geological and Planetary Sciences California Institute of Technology PasadenaCA United States Department of Astronomy University of Michigan Ann ArborMI United States Department of Astronomy Carl Sagan Institute Cornell University IthacaNY United States Max Planck Institute for Astronomy Heidelberg Germany Department of Earth Atmospheric and Planetary Sciences Massachusetts Institute of Technology CambridgeMA United States Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology CambridgeMA United States 51 Pegasi b Fellow Atmospheric Oceanic and Planetary Physics Department of Physics University of Oxford Oxford United Kingdom Université Côte d'Azur Observatoire de la Côte d'Azur CNRS Laboratoire Lagrange France Astrobiology Program UC Santa Cruz Santa CruzCA United States European Space Agency Space Telescope Science Institute Balti

Transmission spectroscopy provides insight into the atmospheric properties and consequently the formation history, physics, and chemistry of transiting exoplanets1. However, obtaining precise inferences of atmospheric properties from transmission spectra requires simultaneously measuring the strength and shape of multiple spectral absorption features from a wide range of chemical species2–4. This has been challenging given the precision and wavelength coverage of previous observatories5. Here, we present the transmission spectrum of the Saturn-mass exoplanet WASP-39 b obtained using the SOSS mode of the NIRISS instrument on the JWST. This spectrum spans 0.6–2.8 µm in wavelength and reveals multiple water absorption bands, the potassium resonance doublet, as well as signatures of clouds. The precision and broad wavelength coverage of NIRISS-SOSS allows us to break model degeneracies between cloud properties and the atmospheric composition of WASP-39 b, favouring a heavy element enhancement ("metallicity") of ~10 – 30× the solar value, a sub-solar carbon-to-oxygen (C/O) ratio, and a solar-to-super-solar potassium-to-oxygen (K/O) ratio. The observations are also best explained by wavelength-dependent, non-gray clouds with inhomogeneous coverage of the planet’s terminator. © 2022, CC BY.

关键词： Water absorption

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All-sky, all-frequency directional search for persistent gravitational waves from Advanced LIGO’s and Advanced Virgo’s first three observing runs

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physical Review D 2022年第12期105卷 122001-122001页

作者： R. Abbott T. D. Abbott F. Acernese K. Ackley C. Adams N. Adhikari R. X. Adhikari V. B. Adya C. Affeldt D. Agarwal M. Agathos K. Agatsuma N. Aggarwal O. D. Aguiar L. Aiello A. Ain P. Ajith T. Akutsu S. Albanesi A. Allocca P. A. Altin A. Amato C. Anand S. Anand A. Ananyeva S. B. Anderson W. G. Anderson M. Ando T. Andrade N. Andres T. Andrić S. V. Angelova S. Ansoldi J. M. Antelis S. Antier S. Appert Koji Arai Koya Arai Y. Arai S. Araki A. Araya M. C. Araya J. S. Areeda M. Arène N. Aritomi N. Arnaud S. M. Aronson K. G. Arun H. Asada Y. Asali G. Ashton Y. Aso M. Assiduo S. M. Aston P. Astone F. Aubin C. Austin S. Babak F. Badaracco M. K. M. Bader C. Badger S. Bae Y. Bae A. M. Baer S. Bagnasco Y. Bai L. Baiotti J. Baird R. Bajpai M. Ball G. Ballardin S. W. Ballmer A. Balsamo G. Baltus S. Banagiri D. Bankar J. C. Barayoga C. Barbieri B. C. Barish D. Barker P. Barneo F. Barone B. Barr L. Barsotti M. Barsuglia D. Barta J. Bartlett M. A. Barton I. Bartos R. Bassiri A. Basti M. Bawaj J. C. Bayley A. C. Baylor M. Bazzan B. Bécsy V. M. Bedakihale M. Bejger I. Belahcene V. Benedetto D. Beniwal T. F. Bennett J. D. Bentley M. BenYaala F. Bergamin B. K. Berger S. Bernuzzi D. Bersanetti A. Bertolini J. Betzwieser D. Beveridge R. Bhandare U. Bhardwaj D. Bhattacharjee S. Bhaumik I. A. Bilenko G. Billingsley S. Bini R. Birney O. Birnholtz S. Biscans M. Bischi S. Biscoveanu A. Bisht B. Biswas M. Bitossi M.-A. Bizouard J. K. Blackburn C. D. Blair D. G. Blair R. M. Blair F. Bobba N. Bode M. Boer G. Bogaert M. Boldrini L. D. Bonavena F. Bondu E. Bonilla R. Bonnand P. Booker B. A. Boom R. Bork V. Boschi N. Bose S. Bose V. Bossilkov V. Boudart Y. Bouffanais A. Bozzi C. Bradaschia P. R. Brady A. Bramley A. Branch M. Branchesi J. E. Brau M. Breschi T. Briant J. H. Briggs A. Brillet M. Brinkmann P. Brockill A. F. Brooks J. Brooks D. D. Brown S. Brunett G. Bruno R. Bruntz J. Bryant T. Bulik H. J. Bulten A. Buonanno R. Buscicchio D. Buskulic C. Buy R. L. Byer L. Cadonati G. Cagnoli C. Cahillane J. Calderón Bustillo J. D. Callaghan T. A. Callis LIGO Laboratory California Institute of Technology Pasadena California 91125 USA Louisiana State University Baton Rouge Louisiana 70803 USA Dipartimento di Farmacia Università di Salerno I-84084 Fisciano Salerno Italy INFN Sezione di Napoli Complesso Universitario di Monte S. Angelo I-80126 Napoli Italy OzGrav School of Physics & Astronomy Monash University Clayton 3800 Victoria Australia LIGO Livingston Observatory Livingston Louisiana 70754 USA University of Wisconsin-Milwaukee Milwaukee Wisconsin 53201 USA OzGrav Australian National University Canberra Australian Capital Territory 0200 Australia Max Planck Institute for Gravitational Physics (Albert Einstein Institute) D-30167 Hannover Germany Leibniz Universität Hannover D-30167 Hannover Germany Inter-University Centre for Astronomy and Astrophysics Pune 411007 India University of Cambridge Cambridge CB2 1TN United Kingdom Theoretisch-Physikalisches Institut Friedrich-Schiller-Universität Jena D-07743 Jena Germany University of Birmingham Birmingham B15 2TT United Kingdom Center for Interdisciplinary Exploration & Research in Astrophysics (CIERA) Northwestern University Evanston Illinois 60208 USA Instituto Nacional de Pesquisas Espaciais 12227-010 São José dos Campos São Paulo Brazil Gravity Exploration Institute Cardiff University Cardiff CF24 3AA United Kingdom INFN Sezione di Pisa I-56127 Pisa Italy International Centre for Theoretical Sciences Tata Institute of Fundamental Research Bengaluru 560089 India Gravitational Wave Science Project National Astronomical Observatory of Japan (NAOJ) Mitaka City Tokyo 181-8588 Japan Advanced Technology Center National Astronomical Observatory of Japan (NAOJ) Mitaka City Tokyo 181-8588 Japan INFN Sezione di Torino I-10125 Torino Italy Università di Napoli “Federico II” Complesso Universitario di Monte S. Angelo I-80126 Napoli Italy Université de Lyon Université Claude Bernard Lyon 1 CNRS Institut Lumière Matière F-69622 Villeurbanne France De

We present the first results from an all-sky all-frequency (ASAF) search for an anisotropic stochastic gravitational-wave background using the data from the first three observing runs of the Advanced LIGO and Advanced Virgo detectors. Upper limit maps on broadband anisotropies of a persistent stochastic background were published for all observing runs of the LIGO-Virgo detectors. However, a broadband analysis is likely to miss narrowband signals as the signal-to-noise ratio of a narrowband signal can be significantly reduced when combined with detector output from other frequencies. Data folding and the computationally efficient analysis pipeline, PyStoch, enable us to perform the radiometer map-making at every frequency bin. We perform the search at 3072 HEALPix equal area pixels uniformly tiling the sky and in every frequency bin of width 1/32 Hz in the range 20–1726 Hz, except for bins that are likely to contain instrumental artefacts and hence are notched. We do not find any statistically significant evidence for the existence of narrowband gravitational-wave signals in the analyzed frequency bins. Therefore, we place 95% confidence upper limits on the gravitational-wave strain for each pixel-frequency pair, the limits are in the range (0.030−9.6)×10−24. In addition, we outline a method to identify candidate pixel-frequency pairs that could be followed up by a more sensitive (and potentially computationally expensive) search, e.g., a matched-filtering-based analysis, to look for fainter nearly monochromatic coherent signals. The ASAF analysis is inherently independent of models describing any spectral or spatial distribution of power. We demonstrate that the ASAF results can be appropriately combined over frequencies and sky directions to successfully recover the broadband directional and isotropic results.

关键词： Gravitational wave detection Gravitational waves

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Constraints on dark photon dark matter using data from LIGO’s and Virgo’s third observing run

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physical Review D 2022年第6期105卷 063030-063030页

作者： R. Abbott T. D. Abbott F. Acernese K. Ackley C. Adams N. Adhikari R. X. Adhikari V. B. Adya C. Affeldt D. Agarwal M. Agathos K. Agatsuma N. Aggarwal O. D. Aguiar L. Aiello A. Ain P. Ajith T. Akutsu S. Albanesi A. Allocca P. A. Altin A. Amato C. Anand S. Anand A. Ananyeva S. B. Anderson W. G. Anderson M. Ando T. Andrade N. Andres T. Andrić S. V. Angelova S. Ansoldi J. M. Antelis S. Antier S. Appert Koji Arai Koya Arai Y. Arai S. Araki A. Araya M. C. Araya J. S. Areeda M. Arène N. Aritomi N. Arnaud S. M. Aronson K. G. Arun H. Asada Y. Asali G. Ashton Y. Aso M. Assiduo S. M. Aston P. Astone F. Aubin C. Austin S. Babak F. Badaracco M. K. M. Bader C. Badger S. Bae Y. Bae A. M. Baer S. Bagnasco Y. Bai L. Baiotti J. Baird R. Bajpai M. Ball G. Ballardin S. W. Ballmer A. Balsamo G. Baltus S. Banagiri D. Bankar J. C. Barayoga C. Barbieri B. C. Barish D. Barker P. Barneo F. Barone B. Barr L. Barsotti M. Barsuglia D. Barta J. Bartlett M. A. Barton I. Bartos R. Bassiri A. Basti M. Bawaj J. C. Bayley A. C. Baylor M. Bazzan B. Bécsy V. M. Bedakihale M. Bejger I. Belahcene V. Benedetto D. Beniwal T. F. Bennett J. D. Bentley M. BenYaala F. Bergamin B. K. Berger S. Bernuzzi D. Bersanetti A. Bertolini J. Betzwieser D. Beveridge R. Bhandare U. Bhardwaj D. Bhattacharjee S. Bhaumik I. A. Bilenko G. Billingsley S. Bini R. Birney O. Birnholtz S. Biscans M. Bischi S. Biscoveanu A. Bisht B. Biswas M. Bitossi M.-A. Bizouard J. K. Blackburn C. D. Blair D. G. Blair R. M. Blair F. Bobba N. Bode M. Boer G. Bogaert M. Boldrini L. D. Bonavena F. Bondu E. Bonilla R. Bonnand P. Booker B. A. Boom R. Bork V. Boschi N. Bose S. Bose V. Bossilkov V. Boudart Y. Bouffanais A. Bozzi C. Bradaschia P. R. Brady A. Bramley A. Branch M. Branchesi J. E. Brau M. Breschi T. Briant J. H. Briggs A. Brillet M. Brinkmann P. Brockill A. F. Brooks J. Brooks D. D. Brown S. Brunett G. Bruno R. Bruntz J. Bryant T. Bulik H. J. Bulten A. Buonanno R. Buscicchio D. Buskulic C. Buy R. L. Byer L. Cadonati G. Cagnoli C. Cahillane J. Calderón Bustillo J. D. Callaghan T. A. Callis LIGO Laboratory California Institute of Technology Pasadena California 91125 USA Louisiana State University Baton Rouge Louisiana 70803 USA Dipartimento di Farmacia Università di Salerno I-84084 Fisciano Salerno Italy INFN Sezione di Napoli Complesso Universitario di Monte S. Angelo I-80126 Napoli Italy OzGrav School of Physics and Astronomy Monash University Clayton 3800 Victoria Australia LIGO Livingston Observatory Livingston Louisiana 70754 USA University of Wisconsin-Milwaukee Milwaukee Wisconsin 53201 USA OzGrav Australian National University Canberra Australian Capital Territory 0200 Australia Max Planck Institute for Gravitational Physics (Albert Einstein Institute) D-30167 Hannover Germany Leibniz Universität Hannover D-30167 Hannover Germany Inter-University Centre for Astronomy and Astrophysics Pune 411007 India University of Cambridge Cambridge CB2 1TN United Kingdom Theoretisch-Physikalisches Institut Friedrich-Schiller-Universität Jena D-07743 Jena Germany University of Birmingham Birmingham B15 2TT United Kingdom Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA) Northwestern University Evanston Illinois 60208 USA Instituto Nacional de Pesquisas Espaciais 12227-010 São José dos Campos São Paulo Brazil Gravity Exploration Institute Cardiff University Cardiff CF24 3AA United Kingdom INFN Sezione di Pisa I-56127 Pisa Italy International Centre for Theoretical Sciences Tata Institute of Fundamental Research Bengaluru 560089 India Gravitational Wave Science Project National Astronomical Observatory of Japan (NAOJ) Mitaka City Tokyo 181-8588 Japan Advanced Technology Center National Astronomical Observatory of Japan (NAOJ) Mitaka City Tokyo 181-8588 Japan INFN Sezione di Torino I-10125 Torino Italy Università di Napoli “Federico II” Complesso Universitario di Monte S. Angelo I-80126 Napoli Italy Université de Lyon Université Claude Bernard Lyon 1 CNRS Institut Lumière Matière F-69622 Villeurbanne Franc

We present a search for dark photon dark matter that could couple to gravitational-wave interferometers using data from Advanced LIGO and Virgo’s third observing run. To perform this analysis, we use two methods, one based on cross-correlation of the strain channels in the two nearly aligned LIGO detectors, and one that looks for excess power in the strain channels of the LIGO and Virgo detectors. The excess power method optimizes the Fourier transform coherence time as a function of frequency, to account for the expected signal width due to Doppler modulations. We do not find any evidence of dark photon dark matter with a mass between mA∼10−14–10−11 eV/c2, which corresponds to frequencies between 10–2000 Hz, and therefore provide upper limits on the square of the minimum coupling of dark photons to baryons, i.e., U(1)B dark matter. For the cross-correlation method, the best median constraint on the squared coupling is ∼1.31×10−47 at mA∼4.2×10−13 eV/c2; for the other analysis, the best constraint is ∼2.4×10−47 at mA∼5.7×10−13 eV/c2. These limits improve upon those obtained in direct dark matter detection experiments by a factor of ∼100 for mA∼[2–4]×10−13 eV/c2, and are, in absolute terms, the most stringent constraint so far in a large mass range mA∼2×10−13–8×10−12 eV/c2.

关键词： Dark matter Gravitational wave detectors

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Search for continuous gravitational waves from 20 accreting millisecond x-ray pulsars in O3 LIGO data

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physical Review D 2022年第2期105卷 022002-022002页

作者： R. Abbott T. D. Abbott F. Acernese K. Ackley C. Adams N. Adhikari R. X. Adhikari V. B. Adya C. Affeldt D. Agarwal M. Agathos K. Agatsuma N. Aggarwal O. D. Aguiar L. Aiello A. Ain T. Akutsu S. Albanesi A. Allocca P. A. Altin A. Amato C. Anand S. Anand A. Ananyeva S. B. Anderson W. G. Anderson M. Ando T. Andrade N. Andres T. Andrić S. V. Angelova S. Ansoldi J. M. Antelis S. Antier S. Appert Koji Arai Koya Arai Y. Arai S. Araki A. Araya M. C. Araya J. S. Areeda M. Arène N. Aritomi N. Arnaud S. M. Aronson K. G. Arun H. Asada Y. Asali G. Ashton Y. Aso M. Assiduo S. M. Aston P. Astone F. Aubin C. Austin S. Babak F. Badaracco M. K. M. Bader C. Badger S. Bae Y. Bae A. M. Baer S. Bagnasco Y. Bai L. Baiotti J. Baird R. Bajpai M. Ball G. Ballardin S. W. Ballmer A. Balsamo G. Baltus S. Banagiri D. Bankar J. C. Barayoga C. Barbieri B. C. Barish D. Barker P. Barneo F. Barone B. Barr L. Barsotti M. Barsuglia D. Barta J. Bartlett M. A. Barton I. Bartos R. Bassiri A. Basti M. Bawaj J. C. Bayley A. C. Baylor M. Bazzan B. Bécsy V. M. Bedakihale M. Bejger I. Belahcene V. Benedetto D. Beniwal T. F. Bennett J. D. Bentley M. BenYaala F. Bergamin B. K. Berger S. Bernuzzi D. Bersanetti A. Bertolini J. Betzwieser D. Beveridge R. Bhandare U. Bhardwaj D. Bhattacharjee S. Bhaumik I. A. Bilenko G. Billingsley S. Bini R. Birney O. Birnholtz S. Biscans M. Bischi S. Biscoveanu A. Bisht B. Biswas M. Bitossi M.-A. Bizouard J. K. Blackburn C. D. Blair D. G. Blair R. M. Blair F. Bobba N. Bode M. Boer G. Bogaert M. Boldrini L. D. Bonavena F. Bondu E. Bonilla R. Bonnand P. Booker B. A. Boom R. Bork V. Boschi N. Bose S. Bose V. Bossilkov V. Boudart Y. Bouffanais A. Bozzi C. Bradaschia P. R. Brady A. Bramley A. Branch M. Branchesi J. E. Brau M. Breschi T. Briant J. H. Briggs A. Brillet M. Brinkmann P. Brockill A. F. Brooks J. Brooks D. D. Brown S. Brunett G. Bruno R. Bruntz J. Bryant T. Bulik H. J. Bulten A. Buonanno R. Buscicchio D. Buskulic C. Buy R. L. Byer L. Cadonati G. Cagnoli C. Cahillane J. Calderón Bustillo J. D. Callaghan T. A. Callister E. Ca LIGO Laboratory California Institute of Technology Pasadena California 91125 USA Louisiana State University Baton Rouge Louisiana 70803 USA Dipartimento di Farmacia Università di Salerno I-84084 Fisciano Salerno Italy INFN Sezione di Napoli Complesso Universitario di Monte S. Angelo I-80126 Napoli Italy OzGrav School of Physics & Astronomy Monash University Clayton 3800 Victoria Australia LIGO Livingston Observatory Livingston Louisiana 70754 USA University of Wisconsin-Milwaukee Milwaukee Wisconsin 53201 USA OzGrav Australian National University Canberra Australian Capital Territory 0200 Australia Max Planck Institute for Gravitational Physics (Albert Einstein Institute) D-30167 Hannover Germany Leibniz Universität Hannover D-30167 Hannover Germany Inter-University Centre for Astronomy and Astrophysics Pune 411007 India University of Cambridge Cambridge CB2 1TN United Kingdom Theoretisch-Physikalisches Institut Friedrich-Schiller-Universität Jena D-07743 Jena Germany University of Birmingham Birmingham B15 2TT United Kingdom Center for Interdisciplinary Exploration & Research in Astrophysics (CIERA) Northwestern University Evanston Illinois 60208 USA Instituto Nacional de Pesquisas Espaciais 12227-010 São José dos Campos São Paulo Brazil Gravity Exploration Institute Cardiff University Cardiff CF24 3AA United Kingdom INFN Sezione di Pisa I-56127 Pisa Italy Gravitational Wave Science Project National Astronomical Observatory of Japan (NAOJ) Mitaka City Tokyo 181-8588 Japan Advanced Technology Center National Astronomical Observatory of Japan (NAOJ) Mitaka City Tokyo 181-8588 Japan INFN Sezione di Torino I-10125 Torino Italy Università di Napoli “Federico II” Complesso Universitario di Monte S. Angelo I-80126 Napoli Italy Université de Lyon Université Claude Bernard Lyon 1 CNRS Institut Lumière Matière F-69622 Villeurbanne France Department of Physics The University of Tokyo Bunkyo-ku Tokyo 113-0033 Japan Research Center for the Early Un

Results are presented of searches for continuous gravitational waves from 20 accreting millisecond x-ray pulsars with accurately measured spin frequencies and orbital parameters, using data from the third observing run of the Advanced LIGO and Advanced Virgo detectors. The search algorithm uses a hidden Markov model, where the transition probabilities allow the frequency to wander according to an unbiased random walk, while the J-statistic maximum-likelihood matched filter tracks the binary orbital phase. Three narrow subbands are searched for each target, centered on harmonics of the measured spin frequency. The search yields 16 candidates, consistent with a false alarm probability of 30% per subband and target searched. These candidates, along with one candidate from an additional target-of-opportunity search done for SAX J1808.4−3658, which was in outburst during one month of the observing run, cannot be confidently associated with a known noise source. Additional follow-up does not provide convincing evidence that any are a true astrophysical signal. When all candidates are assumed nonastrophysical, upper limits are set on the maximum wave strain detectable at 95% confidence, h095%. The strictest constraint is h095%=4.7×10−26 from IGR J17062−6143. Constraints on the detectable wave strain from each target lead to constraints on neutron star ellipticity and r-mode amplitude, the strictest of which are ε95%=3.1×10−7 and α95%=1.8×10−5 respectively. This analysis is the most comprehensive and sensitive search of continuous gravitational waves from accreting millisecond x-ray pulsars to date.

关键词： Gravitational waves Binary stars Neutron stars & pulsars

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Galactic transient sources with the Cherenkov Telescope Array Observatory

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Monthly Notices of the Royal Astronomical Society 2025年第1期540卷 205–238页

作者： Abe, K Abe, S Abhir, J Abhishek, A Acero, F Acharyya, A Adam, R Aguasca-Cabot, A Agudo, I Aguirre-Santaella, A Alfaro, J Alfaro, R Alvarez-Crespo, N Alves Batista, R Amans, J-P Amato, E Ambrosi, G Ambrosino, F Angüner, E O Antonelli, L A Aramo, C Arcaro, C Arnesen, T T H Asano, K Ascasibar, Y Aschersleben, J Ashkar, H Augusto Stuani, L Baack, D Backes, M Balazs, C Balbo, M Baquero Larriva, A Barbosa Martins, V Barres de Almeida, U Barrio, J A Barrios-Jiménez, L Batković, I Batzofin, R Baxter, J Becerra González, J Becker Tjus, J Belmont, R Benbow, W Bernete, J Bernlöhr, K Berti, A Bertucci, B Beshley, V Bhattacharjee, P Bhattacharyya, S Bigongiari, C Bissaldi, E Blanch, O Blazek, J Bocchino, F Boisson, C Bolmont, J Bonnoli, G Bonollo, A Bordas, P Bosnjak, Z Bottacini, E Böttcher, M Bradascio, F Bronzini, E Brown, A M Brunelli, G Bulgarelli, A Burelli, I Burger-Scheidlin, C Burmistrov, L Burton, M Buscemi, M Cailleux, J Campoy-Ordaz, A Cantlay, B K Capasso, G Caproni, A Capuzzo-Dolcetta, R Caraveo, P Caroff, S Carosi, A Carosi, R Carquin, E Carrasco, M-S Cascone, E Cassol, F Castaldini, L Castrejon, N Castro-Tirado, A J Cerasole, D Ceribella, G Cerruti, M Chadwick, P M Chaty, S Chen, A W Chernyakova, M Chiavassa, A Chudoba, J Chytka, L Cicciari, G M Cifuentes, A Coimbra Araujo, C H Colapietro, M Conforti, V Contreras, J L Cortina, J Costa, A Costantini, H Cotter, G Cristofari, P Cuevas, O Curtis-Ginsberg, Z D’Aì, A D’Amico, G D’Ammando, F Dai, S Dazzi, F de Bony de Lavergne, M De Caprio, V De Cesare, G De Frondat Laadim, F de Gouveia Dal Pino, E M De Lotto, B De Lucia, M de Martino, D de Menezes, R de Naurois, M de Ona Wilhelmi, E de Souza, V del Peral, L del Valle, M V Delgado, C Dell’aiera, M Della Valle, M della Volpe, D Depaoli, D Devin, J Di Girolamo, T Di Piano, A Di Pierro, F Di Tria, R Di Venere, L Diebold, S Dignam, C Dima, R Dinesh, A Djuvsland, J Dominik, R M Dominis Prester, D Donini, A Dorner, D Dörner, J Doro, M Dubos, C Ducci, L Dwarkadas, V V Ebr, J Eckner, C Egberts, K Einecke, S Elsässer, D Emery Department of Physics Tokai University 4-1-1 Kita-Kaname Hiratsuka Kanagawa 259-1292 Japan Institute for Cosmic Ray Research University of Tokyo 5-1-5 Kashiwa-no-ha Kashiwa Chiba 277-8582 Japan ETH Zürich Institute for Particle Physics and Astrophysics Otto-Stern-Weg 5 CH-8093 Zürich Switzerland INFN and Università degli Studi di Siena Dipartimento di Scienze Fisiche della Terra e dell’Ambiente (DSFTA) Sezione di Fisica Via Roma 56 I-53100 Siena Italy Université Paris-Saclay Université Paris Cité CEA CNRS AIM F-91191 Gif-sur-Yvette Cedex France FSLAC IRL 2009 CNRS/IAC E-38205 La Laguna Tenerife Spain University of Alabama Tuscaloosa Department of Physics and Astronomy Gallalee Hall Box 870324 Tuscaloosa AL 35487-0324 USA Université Côte d’Azur Observatoire de la Côte d’Azur CNRS Laboratoire Lagrange UF 06304 Nice France Laboratoire Leprince-Ringuet CNRS/IN2P3 École Polytechnique Institut Polytechnique de Paris F-91120 Palaiseau France Departament de Física Quàntica i Astrofísica Institut de Ciències del Cosmos Universitat de Barcelona IEEC-UB Martí i Franquès 1 E-08028 Barcelona Spain Instituto de Astrofísica de Andalucía-CSIC Glorieta de la Astronomía s/n E-18008 Granada Spain Institute for Computational Cosmology and Department of Physics Durham University South Road Durham DH1 3LE UK Pontificia Universidad Católica de Chile Av. Libertador Bernardo O’Higgins 340 8331150 Santiago Chile Universidad Nacional Autónoma de México Delegación Coyoacán 04510 Ciudad de México Mexico IPARCOS-UCM Instituto de Física de Partículas y del Cosmos and EMFTEL Department Universidad Complutense de Madrid E-28040 Madrid Spain Instituto de Física Teórica UAM/CSIC and Departamento de Física Teórica Universidad Autónoma de Madrid c/ Nicolás Cabrera 13-15 Campus de Cantoblanco UAM E-28049 Madrid Spain LUTH GEPI and LERMA Observatoire de Paris Université PSL Université Paris Cité CNRS 5 place Jules Janssen F-92190 Meudon France INAF – Osservatorio

A wide variety of Galactic sources show transient emission at soft and hard X-ray energies: low- and high-mass X-ray binaries containing compact objects, isolated neutron stars exhibiting extreme variability as magnetars as well as pulsar-wind nebulae. Although most of them can show emission up to MeV and/or GeV energies, many have not yet been detected in the TeV domain by Imaging Atmospheric Cherenkov Telescopes. In this paper, we explore the feasibility of detecting new Galactic transients with the Cherenkov Telescope Array Observatory (CTAO) and the prospects for studying them with Target of Opportunity observations. We show that CTAO will likely detect new sources in the TeV regime, such as the massive microquasars in the Cygnus region, low-mass X-ray binaries with low-viewing angle, flaring emission from the Crab pulsar-wind nebula or other novae explosions, among others. Since some of these sources could also exhibit emission at larger time-scales, we additionally test their detectability at longer exposures. We finally discuss the multiwavelength synergies with other instruments and large astronomical facilities.

关键词： binaries: general stars: magnetars novae cataclysmic variables pulsars: general gamma-rays: general

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Effect of climate on traits of dominant and rare tree species in the world’s forests

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Nature Communications 2025年第1期16卷 1-15页

作者： Hordijk, Iris Poorter, Lourens Liang, Jingjing Reich, Peter B. de-Miguel, Sergio Nabuurs, Gert-Jan Gamarra, Javier G. P. Chen, Han Y. H. Zhou, Mo Wiser, Susan K. Pretzsch, Hans Paquette, Alain Picard, Nicolas Hérault, Bruno Bastin, Jean-Francois Alberti, Giorgio Abegg, Meinrad Adou Yao, Yves C. Almeyda Zambrano, Angelica M. Alvarado, Braulio V. Alvarez-Davila, Esteban Alvarez-Loayza, Patricia Alves, Luciana F. Amaral, Iêda Ammer, Christian Antón-Fernández, Clara Araujo-Murakami, Alejandro Arroyo, Luzmila Avitabile, Valerio Aymard C, Gerardo A. Baker, Timothy Banki, Olaf Barroso, Jorcely Bastian, Meredith L. Birigazzi, Luca Birnbaum, Philippe Bitariho, Robert Boeckx, Pascal Bongers, Frans Bouriaud, Olivier Brancalion, Pedro H. S. Brandl, Susanne Brearley, Francis Q. Brienen, Roel Broadbent, Eben N. Bruelheide, Helge Cazzolla Gatti, Roberto Cesar, Ricardo G. Cesljar, Goran Chazdon, Robin L. Chisholm, Chelsea Cienciala, Emil Clark, Connie J. Clark, David B. Colletta, Gabriel Coomes, David Cornejo Valverde, Fernando Corral-Rivas, Jose J. Crim, Philip Cumming, Jonathan Dayanandan, Selvadurai de Gasper, André L. Decuyper, Mathieu Derroire, Géraldine DeVries, Ben Djordjevic, Ilija Dourdain, Aurélie Dolezal, Jiri Engone Obiang, Nestor Laurier Enquist, Brian Eyre, Teresa Fandohan, Adandé Belarmain Fayle, Tom M. Ferreira, Leandro V. Feldpausch, Ted R. Finér, Leena Fischer, Markus Fletcher, Christine Frizzera, Lorenzo Gianelle, Damiano Glick, Henry B. Harris, David Hector, Andrew Hemp, Andreas Herbohn, John Hillers, Annika Honorio Coronado, Eurídice N. Hui, Cang Cho, Hyunkook Ibanez, Thomas Jung, Ilbin Imai, Nobuo Jagodzinski, Andrzej M. Jaroszewicz, Bogdan Johannsen, Vivian Joly, Carlos A. Jucker, Tommaso Karminov, Viktor Kartawinata, Kuswata Kearsley, Elizabeth Kenfack, David Kennard, Deborah Kepfer-Rojas, Sebastian Keppel, Gunnar Khan, Mohammed Latif Killeen, Timothy Kim, Hyun Seok Kitayama, Kanehiro Köhl, Michael Korjus, Henn Kraxner, Florian Laarmann, Diana Lang, Mait Lewis, Simon Lu, Huicui Lukina, Natalia Maitner, Br Institute of Integrative Biology ETH Zurich (Swiss Federal Institute of Technology) Zurich Switzerland Wageningen University and Research Wageningen Netherlands Department of Forestry and Natural Resources Purdue University West Lafayette IN United States Department of Forest Resources University of Minnesota St Paul MN United States Hawkesbury Institute for the Environment Western Sydney University Penrith NSW Australia Department of Agricultural and Forest Sciences and Engineering University of Lleida Lleida Spain Forest Science and Technology Centre of Catalonia (CTFC) Solsona Spain Forestry Division Food and Agriculture Organization of the United Nations Rome Italy Faculty of Natural Resources Management Lakehead University Thunder Bay ON Canada Manaaki Whenua–Landcare Research Lincoln New Zealand Chair for Forest Growth and Yield Science TUM School for Life Sciences Technical University of Munich Munich Germany Centre for Forest Research Université du Québec à Montréal Montréal QC Canada GIP ECOFOR Paris France CIRAD Forêts et Sociétés Montpellier France Forêts et Sociétés Univ Montpellier CIRAD Montpellier France Gembloux Agro Bio-Tech University of Liege Liege Belgium Faculty of Science and Technology Free University of Bolzano Bolzano Italy Department of Agricultural Food Environmental and Animal Sciences University of Udine Udine Italy Swiss Federal Institute for Forest Snow and Landscape Research WSL Birmensdorf Switzerland UFR Biosciences University Félix Houphouët-Boigny Abidjan Cote d'Ivoire Spatial Ecology and Conservation Laboratory Center for Latin American Studies University of Florida Gainesville FL United States Forestry School Tecnológico de Costa Rica TEC Cartago Costa Rica Fundacion ConVida Universidad Nacional Abierta y a Distancia UNAD Medellin Colombia Field Museum of Natural History Chicago IL United States Center for Tropical Research Institute of the Environment and Sustainability UCLA Los Angeles CA

Species’ traits and environmental conditions determine the abundance of tree species across the globe. The extent to which traits of dominant and rare tree species differ remains untested across a broad environmental range, limiting our understanding of how species traits and the environment shape forest functional composition. We use a global dataset of tree composition of >22,000 forest plots and 11 traits of 1663 tree species to ask how locally dominant and rare species differ in their trait values, and how these differences are driven by climatic gradients in temperature and water availability in forest biomes across the globe. We find three consistent trait differences between locally dominant and rare species across all biomes;dominant species are taller, have softer wood and higher loading on the multivariate stem strategy axis (related to narrow tracheids and thick bark). The difference between traits of dominant and rare species is more strongly driven by temperature compared to water availability, as temperature might affect a larger number of traits. Therefore, climate change driven global temperature rise may have a strong effect on trait differences between dominant and rare tree species and may lead to changes in species abundances and therefore strong community reassembly. © The Author(s) 2025.

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