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Becherini, YvonneORCID iD iconorcid.org/0000-0002-2115-2930
Publications (10 of 218) Show all publications
Algaba, J. C., Balokovic, M., Chandra, S., Cheong, W.-Y. -., Cui, Y.-Z. -., D'Ammando, F., . . . Zhong, W. (2024). Broadband multi-wavelength properties of M87 during the 2018 EHT campaign including a very high energy flaring episode. Astronomy and Astrophysics, 692, Article ID A140.
Open this publication in new window or tab >>Broadband multi-wavelength properties of M87 during the 2018 EHT campaign including a very high energy flaring episode
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2024 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 692, article id A140Article in journal (Refereed) Published
Abstract [en]

Context. The nearby elliptical galaxy M87 contains one of only two supermassive black holes whose emission surrounding the event horizon has been imaged by the Event Horizon Telescope (EHT). In 2018, more than two dozen multi-wavelength (MWL) facilities (from radio to gamma-ray energies) took part in the second M87 EHT campaign. Aims. The goal of this extensive MWL campaign was to better understand the physics of the accreting black hole M87*, the relationship between the inflow and inner jets, and the high-energy particle acceleration. Understanding the complex astrophysics is also a necessary first step towards performing further tests of general relativity. Methods. The MWL campaign took place in April 2018, overlapping with the EHT M87* observations. We present a new, contemporaneous spectral energy distribution (SED) ranging from radio to very high-energy (VHE) gamma-rays as well as details of the individual observations and light curves. We also conducted phenomenological modelling to investigate the basic source properties. Results. We present the first VHE gamma-ray flare from M87 detected since 2010. The flux above 350 GeV more than doubled within a period of approximate to 36 hours. We find that the X-ray flux is enhanced by about a factor of two compared to 2017, while the radio and millimetre core fluxes are consistent between 2017 and 2018. We detect evidence for a monotonically increasing jet position angle that corresponds to variations in the bright spot of the EHT image. Conclusions. Our results show the value of continued MWL monitoring together with precision imaging for addressing the origins of high-energy particle acceleration. While we cannot currently pinpoint the precise location where such acceleration takes place, the new VHE gamma-ray flare already presents a challenge to simple one-zone leptonic emission model approaches, and it emphasises the need for combined image and spectral modelling.
Place, publisher, year, edition, pages
EDP Sciences, 2024
Keywords
galaxies: active, galaxies: individual: M 87, galaxies: jets, galaxies: nuclei
National Category
Astronomy, Astrophysics and Cosmology
Research subject
Physics, Astroparticle Physics
Identifiers
urn:nbn:se:lnu:diva-136893 (URN)10.1051/0004-6361/202450497 (DOI)001406602800001 ()2-s2.0-85216358290 (Scopus ID)
Available from: 2025-02-18 Created: 2025-02-18 Last updated: 2025-03-13Bibliographically approved
Aharonian, F., Benkhali, F. A., Aschersleben, J., Ashkar, H., Backes, M., Martins, V. B., . . . Zywucka, N. (2024). Curvature in the very-high energy gamma-ray spectrum of M 87. Astronomy and Astrophysics, 685, Article ID A96.
Open this publication in new window or tab >>Curvature in the very-high energy gamma-ray spectrum of M 87
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2024 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 685, article id A96Article in journal (Refereed) Published
Abstract [en]

The radio galaxy M 87 is a variable very-high energy (VHE) gamma-ray source, exhibiting three major flares, which were reported in 2005, 2008, and 2010. Despite extensive studies, the origin of the VHE gamma-ray emission is not yet fully understood. In this study, we investigate the VHE gamma-ray spectrum of M 87 during states of high gamma-ray activity, utilizing 20.2 h of H.E.S.S. observations. Our findings indicate a preference for a curved spectrum, characterized by a log-parabola model with extra-galactic background light (EBL) model above 0.3 TeV at the 4σ level, compared to a power-law spectrum with EBL. We investigate the degeneracy between the absorption feature and the EBL normalization and derive upper limits on EBL models that are mainly sensitive in the wavelength range of 12.4 μm–40 μm.
Place, publisher, year, edition, pages
EDP Sciences, 2024
Keywords
astroparticle physics, galaxies: active, galaxies: jets, gamma rays: galaxies, infrared: general
National Category
Astronomy, Astrophysics and Cosmology
Research subject
Physics, Astroparticle Physics
Identifiers
urn:nbn:se:lnu:diva-133061 (URN)10.1051/0004-6361/202348913 (DOI)001279369300001 ()2-s2.0-85193454856 (Scopus ID)
Available from: 2024-10-28 Created: 2024-10-28 Last updated: 2024-11-21Bibliographically approved
Aharonian, F., Ait Benkhali, F., Aschersleben, J., Ashkar, H., Backes, M., Barbosa Martins, V., . . . Zywucka, N. (2024). HESS observations of the 2021 periastron passage of PSR B1259-63/LS 2883. Astronomy and Astrophysics, 687, Article ID A219.
Open this publication in new window or tab >>HESS observations of the 2021 periastron passage of PSR B1259-63/LS 2883
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2024 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 687, article id A219Article in journal (Refereed) Published
Abstract [en]

PSR B1259-63/LS 2883 is a gamma-ray binary system that hosts a pulsar in an eccentric orbit, with a 3.4 yr period, around an O9.5Ve star (LS 2883). At orbital phases close to periastron passages, the system radiates bright and variable non-thermal emission, for which the temporal and spectral properties of this emission are, for now, poorly understood. In this regard, very high-energy (VHE) emission is especially useful to study and constrain radiation processes and particle acceleration in the system. We report on an extensive VHE observation campaign conducted with the High Energy Stereoscopic System, comprised of approximately 100 h of data taken over five months, from t(p) - 24 days to t(p) + 127 days around the system's 2021 periastron passage (where t(p) is the time of periastron). We also present the timing and spectral analyses of the source. The VHE light curve in 2021 is consistent overall with the stacked light curve of all previous observations. Within the light curve, we report a VHE maximum at times coincident with the third X-ray peak first detected in the 2021 X-ray light curve. In the light curve - although sparsely sampled in this time period - we see no VHE enhancement during the second disc crossing. In addition, we see no correspondence to the 2021 GeV flare in the VHE light curve. The VHE spectrum obtained from the analysis of the 2021 dataset is best described by a power law of spectral index Gamma = 2.65 +/- 0.04(stat) +/- 0.04(sys), a value consistent with the spectral index obtained from the analysis of data collected with H.E.S.S. during the previous observations of the source. We report spectral variability with a difference of Delta Gamma = 0.56 +/- 0.18(stat) +/- 0.10(sys) at 95% confidence intervals, between sub-periods of the 2021 dataset. We also detail our investigation into X-ray/TeV and GeV/TeV flux correlations in the 2021 periastron passage. We find a linear correlation between contemporaneous flux values of X-ray and TeV datasets, detected mainly after t(p) + 25 days, suggesting a change in the available energy for non-thermal radiation processes. We detect no significant correlation between GeV and TeV flux points, within the uncertainties of the measurements, from similar to t(p) - 23 days to similar to t(p) + 126 days. This suggests that the GeV and TeV emission originate from different electron populations.
Place, publisher, year, edition, pages
EDP Sciences, 2024
Keywords
radiation mechanisms: non-thermal, binaries: general, pulsars: individual: PSR B1259-63/LS 2883
National Category
Astronomy, Astrophysics and Cosmology
Research subject
Physics, Astroparticle Physics
Identifiers
urn:nbn:se:lnu:diva-131891 (URN)10.1051/0004-6361/202449612 (DOI)001272307300006 ()2-s2.0-85199425347 (Scopus ID)
Available from: 2024-08-21 Created: 2024-08-21 Last updated: 2024-09-03Bibliographically approved
Aharonian, F., Benkhali, F. A., Aschersleben, J., Ashkar, H., Backes, M., Martins, V. B., . . . Zywucka, N. (2024). High-Statistics Measurement of the Cosmic-Ray Electron Spectrum with HESS. Physical Review Letters, 133(22), Article ID 221001.
Open this publication in new window or tab >>High-Statistics Measurement of the Cosmic-Ray Electron Spectrum with HESS
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2024 (English)In: Physical Review Letters, ISSN 0031-9007, E-ISSN 1079-7114, Vol. 133, no 22, article id 221001Article in journal (Refereed) Published
Abstract [en]

Owing to their rapid cooling rate and hence loss-limited propagation distance, cosmic-ray electrons and positrons (CRe) at very high energies probe local cosmic-ray accelerators and provide constraints on exotic production mechanisms such as annihilation of dark matter particles. We present a high-statistics measurement of the spectrum of CRe candidate events from 0.3 to 40 TeV with the High Energy Stereoscopic System, covering 2 orders of magnitude in energy and reaching a proton rejection power of better than 10(4). The measured spectrum is well described by a broken power law, with a break around 1 TeV, where the spectral index increases from Gamma(1) = 3.25 +/- 0.02(stat) +/- 0.2(sys) to Gamma(2) = 4.49 +/- 0.04(stat) +/- 0.2(sys). Apart from the break, the spectrum is featureless. The absence of distinct signatures at multi-TeV energies imposes constraints on the presence of nearby CRe accelerators and the local CRe propagation mechanisms.
Place, publisher, year, edition, pages
American Physical Society, 2024
National Category
Astronomy, Astrophysics and Cosmology
Research subject
Physics, Astroparticle Physics
Identifiers
urn:nbn:se:lnu:diva-134822 (URN)10.1103/PhysRevLett.133.221001 (DOI)001382592900001 ()39672149 (PubMedID)2-s2.0-85210773226 (Scopus ID)
Available from: 2025-01-23 Created: 2025-01-23 Last updated: 2025-01-23Bibliographically approved
Aharonian, F., Benkhali, F. A., Aschersleben, J., Ashkar, H., Backes, M., Baktash, A., . . . Harding, A. (2024). Spectrum and extension of the inverse-Compton emission of the Crab Nebula from a combined Fermi-LAT and HESS analysis. Astronomy and Astrophysics, 686, Article ID A308.
Open this publication in new window or tab >>Spectrum and extension of the inverse-Compton emission of the Crab Nebula from a combined Fermi-LAT and HESS analysis
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2024 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 686, article id A308Article in journal (Refereed) Published
Abstract [en]

The Crab Nebula is a unique laboratory for studying the acceleration of electrons and positrons through their non-thermal radiation. Observations of very-high-energy γ rays from the Crab Nebula have provided important constraints for modelling its broadband emission. We present the first fully self-consistent analysis of the Crab Nebula's γ-ray emission between 1 GeV and ~100 TeV, that is, over five orders of magnitude in energy. Using the open-source software package Gammapy, we combined 11.4 yr of data from the Fermi Large Area Telescope and 80 h of High Energy Stereoscopic System (H.E.S.S.) data at the event level and provide a measurement of the spatial extension of the nebula and its energy spectrum. We find evidence for a shrinking of the nebula with increasing γ-ray energy. Furthermore, we fitted several phenomenological models to the measured data, finding that none of them can fully describe the spatial extension and the spectral energy distribution at the same time. Especially the extension measured at TeV energies appears too large when compared to the X-ray emission. Our measurements probe the structure of the magnetic field between the pulsar wind termination shock and the dust torus, and we conclude that the magnetic field strength decreases with increasing distance from the pulsar. We complement our study with a careful assessment of systematic uncertainties.
Place, publisher, year, edition, pages
EDP Sciences, 2024
Keywords
acceleration of particles, radiation mechanisms: non-thermal, gamma rays: general, ISM: individual objects: Crab Nebula
National Category
Astronomy, Astrophysics and Cosmology
Research subject
Physics, Astroparticle Physics
Identifiers
urn:nbn:se:lnu:diva-133062 (URN)10.1051/0004-6361/202348651 (DOI)001271691900001 ()2-s2.0-85201046243 (Scopus ID)
Available from: 2024-10-28 Created: 2024-10-28 Last updated: 2024-11-11Bibliographically approved
Aharonian, F., Benkhali, F. A., Aschersleben, J., Ashkar, H., Backes, M., Baktash, A., . . . Zywucka, N. (2024). TeV flaring activity of the AGN PKS 0625-354 in November 2018. Astronomy and Astrophysics, 683, Article ID A70.
Open this publication in new window or tab >>TeV flaring activity of the AGN PKS 0625-354 in November 2018
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2024 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 683, article id A70Article in journal (Refereed) Published
Abstract [en]

Most gamma-ray detected active galactic nuclei are blazars with one of their relativistic jets pointing towards the Earth. Only a few objects belong to the class of radio galaxies or misaligned blazars. Here, we investigate the nature of the object PKS 0625-354, its gamma-ray flux and spectral variability and its broad-band spectral emission with observations from H.E.S.S., Fermi-LAT, Swift-XRT, and UVOT taken in November 2018. The H.E.S.S. light curve above 200 GeV shows an outburst in the first night of observations followed by a declining flux with a halving time scale of 5.9 h. The gamma gamma-opacity constrains the upper limit of the angle between the jet and the line of sight to similar to 10 degrees. The broad-band spectral energy distribution shows two humps and can be well fitted with a single-zone synchrotron self Compton emission model. We conclude that PKS 0625-354, as an object showing clear features of both blazars and radio galaxies, can be classified as an intermediate active galactic nuclei. Multi-wavelength studies of such intermediate objects exhibiting features of both blazars and radio galaxies are sparse but crucial for the understanding of the broad-band emission of gamma-ray detected active galactic nuclei in general.
Place, publisher, year, edition, pages
EDP Sciences, 2024
Keywords
galaxies: active, galaxies: individual: PKS 0625-354, galaxies: jets, gamma rays: galaxies
National Category
Astronomy, Astrophysics and Cosmology
Research subject
Physics, Astroparticle Physics
Identifiers
urn:nbn:se:lnu:diva-128813 (URN)10.1051/0004-6361/202348063 (DOI)001185071900015 ()2-s2.0-85187160658 (Scopus ID)
Available from: 2024-04-12 Created: 2024-04-12 Last updated: 2024-04-23Bibliographically approved
Aharonian, F., Benkhali, F. A., Aschersleben, J., Ashkar, H., Backes, M., Baktash, A., . . . Zywucka, N. (2024). Unveiling extended gamma-ray emission around HESS J1813-178. Astronomy and Astrophysics, 686, Article ID A149.
Open this publication in new window or tab >>Unveiling extended gamma-ray emission around HESS J1813-178
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2024 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 686, article id A149Article in journal (Refereed) Published
Abstract [en]

Context. HESS J1813-178 is a very-high-energy gamma-ray source spatially coincident with the young and energetic pulsar PSR J1813-1749 and thought to be associated with its pulsar wind nebula (PWN). Recently, evidence for extended high-energy emission in the vicinity of the pulsar has been revealed in the Fermi Large Area Telescope (LAT) data. This motivates revisiting the HESS J1813-178 region, taking advantage of improved analysis methods and an extended dataset. Aims. Using data taken by the High Energy Stereoscopic System (H.E.S.S.) experiment and the Fermi-LAT, we aim to describe the gamma-ray emission in the region with a consistent model, to provide insights into its origin. Methods. We performed a likelihood-based analysis on 32 hours of H.E.S.S. data and 12 yr of Fermi-LAT data and we fitted a spectromorphological model to the combined datasets. These results allowed us to develop a physical model for the origin of the observed.-ray emission in the region. Results. In addition to the compact very-high-energy gamma-ray emission centred on the pulsar, we find a significant yet previously undetected component along the Galactic plane. With Fermi-LAT data, we confirm extended high-energy emission consistent with the position and elongation of the extended emission observed with H.E.S.S. These results establish a consistent description of the emission in the region from GeV energies to several tens of TeV. Conclusions. This study suggests that HESS J1813-178 is associated with a gamma-ray PWN powered by PSR J1813-1749. A possible origin of the extended emission component is inverse Compton emission from electrons and positrons that have escaped the confines of the pulsar and form a halo around the PWN.
Place, publisher, year, edition, pages
EDP Sciences, 2024
Keywords
pulsars: individual: PSR J1813-1749, gamma rays: general, gamma rays: ISM
National Category
Astronomy, Astrophysics and Cosmology
Research subject
Physics, Astroparticle Physics
Identifiers
urn:nbn:se:lnu:diva-131855 (URN)10.1051/0004-6361/202348374 (DOI)001253345700001 ()2-s2.0-85195817727 (Scopus ID)
Available from: 2024-08-16 Created: 2024-08-16 Last updated: 2024-10-22Bibliographically approved
Aharonian, F., Benkhali, F. A., Aschersleben, J., Ashkar, H., Backes, M., Martins, V. B., . . . Zywucka, N. (2024). Very-high-energy γ-Ray Emission from Young Massive Star Clusters in the Large Magellanic Cloud. Astrophysical Journal Letters, 970(1), Article ID L21.
Open this publication in new window or tab >>Very-high-energy γ-Ray Emission from Young Massive Star Clusters in the Large Magellanic Cloud
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2024 (English)In: Astrophysical Journal Letters, ISSN 2041-8205, E-ISSN 2041-8213, Vol. 970, no 1, article id L21Article in journal (Refereed) Published
Abstract [en]

The Tarantula Nebula in the Large Magellanic Cloud is known for its high star formation activity. At its center lies the young massive star cluster R136, providing a significant amount of the energy that makes the nebula shine so brightly at many wavelengths. Recently, young massive star clusters have been suggested to also efficiently produce very high-energy cosmic rays, potentially beyond PeV energies. Here, we report the detection of very-high-energy γ-ray emission from the direction of R136 with the High Energy Stereoscopic System, achieved through a multicomponent, likelihood-based modeling of the data. This supports the hypothesis that R136 is indeed a very powerful cosmic-ray accelerator. Moreover, from the same analysis, we provide an updated measurement of the γ-ray emission from 30 Dor C, the only superbubble detected at TeV energies presently. The γ-ray luminosity above 0.5 TeV of both sources is (2-3) x 1035 erg s-1. This exceeds by more than a factor of 2 the luminosity of HESS J1646-458, which is associated with the most massive young star cluster in the Milky Way, Westerlund 1. Furthermore, the γ-ray emission from each source is extended with a significance of >3σ and a Gaussian width of about 30 pc. For 30 Dor C, a connection between the γ-ray emission and the nonthermal X-ray emission appears likely. Different interpretations of the γ-ray signal from R136 are discussed.
Place, publisher, year, edition, pages
Institute of Physics Publishing (IOPP), 2024
National Category
Astronomy, Astrophysics and Cosmology
Research subject
Physics, Astroparticle Physics
Identifiers
urn:nbn:se:lnu:diva-133146 (URN)10.3847/2041-8213/ad5e67 (DOI)001290659200001 ()2-s2.0-85199364571 (Scopus ID)
Available from: 2024-10-28 Created: 2024-10-28 Last updated: 2024-11-11Bibliographically approved
Aharonian, F., Ait Benkhali, F., Arcaro, C., Aschersleben, J., Backes, M., Barbosa, V. M., . . . Zywucka, N. (2023). Constraining the cosmic-ray pressure in the inner Virgo Cluster using HESS observations of M 87. Astronomy and Astrophysics, 675, Article ID A138.
Open this publication in new window or tab >>Constraining the cosmic-ray pressure in the inner Virgo Cluster using HESS observations of M 87
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2023 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 675, article id A138Article in journal (Refereed) Published
Abstract [en]

The origin of the gamma-ray emission from M 87 is currently a matter of debate. This work aims to localize the very high-energy (VHE; 100 GeV - 100 TeV) gamma-ray emission from M 87 and probe a potential extended hadronic emission component in the inner Virgo Cluster. The search for a steady and extended gamma-ray signal around M 87 can constrain the cosmic-ray energy density and the pressure exerted by the cosmic rays onto the intracluster medium and allow us to investigate the role of cosmic rays in the active galactic nucleus feedback as a heating mechanism in the Virgo Cluster. The High Energy Stereoscopic System (H.E.S.S.) telescopes are sensitive to VHE gamma rays and have been used to observe M 87 since 2004. We utilized a Bayesian block analysis to identify M 87 emission states with H.E.S.S. observations from 2004 to 2021, dividing them into low, intermediate, and high states. Because of the causality argument, an extended (≳1 kpc) signal is allowed only in steady emission states. Hence, we fitted the morphology of the 120 h low-state data and find no significant gamma-ray extension. Therefore, we derive for the low state an upper limit of 58″(corresponding to ≈4.6 kpc) in the extension of a single-component morphological model described by a rotationally symmetric 2D Gaussian model at the 99.7% confidence level. Our results exclude the radio lobes (≈30 kpc) as the principal component of the VHE gamma-ray emission from the low state of M 87. The gamma-ray emission is compatible with a single emission region at the radio core of M 87. These results, with the help of two multiple-component models, constrain the maximum cosmic-ray to thermal pressure ratio to XCR, max. ≲ 0.32 and the total energy in cosmic-ray protons to UCR  ≲  5  ×  1058 erg in the inner 20 kpc of the Virgo Cluster for an assumed cosmic-ray proton power-law distribution in momentum with spectral index αp = 2.1
Place, publisher, year, edition, pages
EDP Sciences, 2023
Keywords
astroparticle physics, gamma rays, galaxies, clusters, intracluster medium, radio continuum
National Category
Astronomy, Astrophysics and Cosmology
Research subject
Physics, Astroparticle Physics
Identifiers
urn:nbn:se:lnu:diva-123893 (URN)10.1051/0004-6361/202346056 (DOI)001033560900005 ()2-s2.0-85165532261 (Scopus ID)
Available from: 2023-08-25 Created: 2023-08-25 Last updated: 2024-10-22Bibliographically approved
Aharonian, F., Aschersleben, J., Backes, M., Martins, V. B., Batzofin, R., Becherini, Y., . . . Zywucka, N. (2023). Constraints on the Intergalactic Magnetic Field Using Fermi-LAT and HESS Blazar Observations. Astrophysical Journal Letters, 950(2), Article ID L16.
Open this publication in new window or tab >>Constraints on the Intergalactic Magnetic Field Using Fermi-LAT and HESS Blazar Observations
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2023 (English)In: Astrophysical Journal Letters, ISSN 2041-8205, E-ISSN 2041-8213, Vol. 950, no 2, article id L16Article in journal (Refereed) Published
Abstract [en]

Magnetic fields in galaxies and galaxy clusters are believed to be the result of the amplification of intergalactic seed fields during the formation of large-scale structures in the universe. However, the origin, strength, and morphology of this intergalactic magnetic field (IGMF) remain unknown. Lower limits on (or indirect detection of) the IGMF can be obtained from observations of high-energy gamma rays from distant blazars. Gamma rays interact with the extragalactic background light to produce electron-positron pairs, which can subsequently initiate electromagnetic cascades. The gamma-ray signature of the cascade depends on the IGMF since it deflects the pairs. Here we report on a new search for this cascade emission using a combined data set from the Fermi Large Area Telescope and the High Energy Stereoscopic System. Using state-of-the-art Monte Carlo predictions for the cascade signal, our results place a lower limit on the IGMF of B > 7.1 x 10(-16) G for a coherence length of 1 Mpc even when blazar duty cycles as short as 10 yr are assumed. This improves on previous lower limits by a factor of 2. For longer duty cycles of 10(4) (10(7)) yr, IGMF strengths below 1.8 x 10(-14) G (3.9 x 10(-14) G) are excluded, which rules out specific models for IGMF generation in the early universe.
Place, publisher, year, edition, pages
Institute of Physics Publishing (IOPP), 2023
National Category
Astronomy, Astrophysics and Cosmology
Research subject
Physics, Astroparticle Physics
Identifiers
urn:nbn:se:lnu:diva-124085 (URN)10.3847/2041-8213/acd777 (DOI)001021638900001 ()2-s2.0-85164482030 (Scopus ID)
Available from: 2023-09-05 Created: 2023-09-05 Last updated: 2024-10-23Bibliographically approved
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Identifiers
ORCID iD: ORCID iD iconorcid.org/0000-0002-2115-2930

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