Home > Publications database > Constraining the cosmic-ray pressure in the inner Virgo Cluster using H.E.S.S. observations of M 87 > print

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024 7 _ |a arXiv:2305.09607
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037 _ _ |a PUBDB-2023-03519
041 _ _ |a English
088 _ _ |a arXiv:2305.09607
|2 arXiv
100 1 _ |a Aharonian, F.
|b 0
245 _ _ |a Constraining the cosmic-ray pressure in the inner Virgo Cluster using H.E.S.S. observations of M 87
260 _ _ |c 2023
336 7 _ |a Preprint
|b preprint
|m preprint
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336 7 _ |a Electronic Article
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336 7 _ |a preprint
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336 7 _ |a ARTICLE
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336 7 _ |a Output Types/Working Paper
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500 _ _ |a 15 pages, 7 figures. Accepted for publication in A&A. Corresponding authors: Victor Barbosa Martins, Stefan Ohm, Cornelia Arcaro, Natalia Żywucka, Mathieu de Naurois
520 _ _ |a The origin of the gamma-ray emission from M87 is currently a matter of debate. This work aims to localize the VHE (100 GeV-100 TeV) gamma-ray emission from M87 and probe a potential extended hadronic emission component in the inner Virgo Cluster. The search for a steady and extended gamma-ray signal around M87 can constrain the cosmic-ray energy density and the pressure exerted by the cosmic rays onto the intra-cluster medium, and allow us to investigate the role of the cosmic rays in the active galactic nucleus feedback as a heating mechanism in the Virgo Cluster. H.E.S.S. telescopes are sensitive to VHE gamma rays and have been utilized to observe M87 since 2004. We utilized a Bayesian block analysis to identify M87 emission states with H.E.S.S. observations from 2004 until 2021, dividing them into low, intermediate, and high states. Because of the causality argument, an extended ($\gtrsim$kpc) signal is allowed only in steady emission states. Hence, we fitted the morphology of the 120h low state data and found no significant gamma-ray extension. Therefore, we derived for the low state an upper limit of 58'(corresponding to $\approx$4.6kpc) in the extension of a single-component morphological model described by a rotationally symmetric 2D Gaussian model at 99.7% confidence level. Our results exclude the radio lobes ($\approx$30 kpc) as the principal component of the VHE gamma-ray emission from the low state of M87. The gamma-ray emission is compatible with a single emission region at the radio core of M87. These results, with the help of two multiple-component models, constrain the maximum cosmic-ray to thermal pressure ratio $X_{{CR,max.}}$$\lesssim$$0.32$ and the total energy in cosmic-ray protons (CRp) to $U_{CR}$$\lesssim$5$\times10^{58}$ erg in the inner 20kpc of the Virgo Cluster for an assumed CRp power-law distribution in momentum with spectral index $\alpha_{p}$=2.1.
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588 _ _ |a Dataset connected to INSPIRE
650 _ 7 |a gamma ray, emission
|2 INSPIRE
650 _ 7 |a gamma ray, VHE
|2 INSPIRE
650 _ 7 |a p, cosmic radiation
|2 INSPIRE
650 _ 7 |a cosmic radiation, energy
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650 _ 7 |a cosmic radiation, pressure
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650 _ 7 |a energy, density
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650 _ 7 |a VIRGO
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650 _ 7 |a cluster
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650 _ 7 |a HESS
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650 _ 7 |a AGN
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650 _ 7 |a power spectrum
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650 _ 7 |a causality
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650 _ 7 |a feedback
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650 _ 7 |a thermal
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650 _ 7 |a Bayesian
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650 _ 7 |a rotation
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650 _ 7 |a TeV
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700 1 _ |a Benkhali, F. Ait
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700 1 _ |a Arcaro, C.
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700 1 _ |a Aschersleben, J.
|b 3
700 1 _ |a Backes, M.
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700 1 _ |a Barbosa Martins, V.
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700 1 _ |a Batzofin, R.
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700 1 _ |a Becherini, Y.
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700 1 _ |a Berge, D.
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700 1 _ |a Bernlöhr, K.
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700 1 _ |a Burger-Scheidlin, C.
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700 1 _ |a Caroff, S.
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700 1 _ |a Chandra, S.
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700 1 _ |a Lang, R. G.
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700 1 _ |a Le Stum, S.
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700 1 _ |a Moulin, E.
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700 1 _ |a Muller, J.
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700 1 _ |a Nakashima, K.
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700 1 _ |a de Naurois, M.
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700 1 _ |a Niemiec, J.
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700 1 _ |a Noel, A. Priyana
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700 1 _ |a O'Brien, P.
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700 1 _ |a Ohm, S.
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700 1 _ |a Olivera-Nieto, L.
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700 1 _ |a de Ona Wilhelmi, E.
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700 1 _ |a Panny, S.
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700 1 _ |a Panter, M.
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700 1 _ |a Sasaki, M.
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700 1 _ |a Schwanke, U.
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700 1 _ |a Sol, H.
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700 1 _ |a Suzuki, H.
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700 1 _ |a Terrier, R.
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700 1 _ |a Uchiyama, Y.
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700 1 _ |a van Eldik, C.
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700 1 _ |a Wong, Yu Wun
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700 1 _ |a H. E. S. S. Collaboration
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914 1 _ |y 2023
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