Home > Publications database > Prospects for γ-ray observations of the Perseus galaxy cluster with the Cherenkov Telescope Array > print

001     625886
005     20250625124614.0
024 7 _ |a 10.1088/1475-7516/2024/10/004
|2 doi
024 7 _ |a 1475-7508
|2 ISSN
024 7 _ |a 1475-7516
|2 ISSN
024 7 _ |a 10.3204/PUBDB-2025-01211
|2 datacite_doi
024 7 _ |a altmetric:153925338
|2 altmetric
024 7 _ |a arXiv:2309.03712
|2 arXiv
024 7 _ |a WOS:001375578500001
|2 WOS
037 _ _ |a PUBDB-2025-01211
041 _ _ |a English
082 _ _ |a 530
088 _ _ |a arXiv:2309.03712
|2 arXiv
100 1 _ |a Abe, K.
|b 0
245 _ _ |a Prospects for γ-ray observations of the Perseus galaxy cluster with the Cherenkov Telescope Array
260 _ _ |a London
|c 2024
|b IOP
336 7 _ |a article
|2 DRIVER
336 7 _ |a Output Types/Journal article
|2 DataCite
336 7 _ |a Journal Article
|b journal
|m journal
|0 PUB:(DE-HGF)16
|s 1749546789_2074669
|2 PUB:(DE-HGF)
336 7 _ |a ARTICLE
|2 BibTeX
336 7 _ |a JOURNAL_ARTICLE
|2 ORCID
336 7 _ |a Journal Article
|0 0
|2 EndNote
500 _ _ |a 93 pages (including author list, appendix and references), 143 figures. Submitted to JCAP
520 _ _ |a Galaxy clusters are expected to be both dark matter (DM) reservoirs and storage rooms for the cosmic-ray protons (CRp) that accumulate along the cluster's formation history. Accordingly, they are excellent targets to search for signals of DM annihilation and decay at γ-ray energies and are predicted to be sources of large-scale γ-ray emission due to hadronic interactions in the intracluster medium (ICM).In this paper, we estimate the sensitivity of the Cherenkov Telescope Array (CTA) to detect diffuse γ-ray emission from the Perseus galaxy cluster.We first perform a detailed spatial and spectral modelling of the expected signal for both the DM and the CRp components. For each case, we compute the expected CTA sensitivity accounting for the CTA instrument response functions. The CTA observing strategy of the Perseus cluster is also discussed.In the absence of a diffuse signal (non-detection), CTA should constrain the CRp to thermal energy ratio X$_{500}$ within the characteristic radius R$_{500}$ down to about X$_{500}$ < 3 × 10$^{-3}$, for a spatial CRp distribution that follows the thermal gas and a CRp spectral index α$_{CRp}$ = 2.3. Under the optimistic assumption of a pure hadronic origin of the Perseus radio mini-halo and depending on the assumed magnetic field profile, CTA should measure α$_{CRp}$ down to about Δα$_{CRp}$ ≃ 0.1 and the CRp spatial distribution with 10% precision, respectively. Regarding DM, CTA should improve the current ground-based γ-ray DM limits from clusters observations on the velocity-averaged annihilation cross-section by a factor of up to ∼ 5, depending on the modelling of DM halo substructure. In the case of decay of DM particles, CTA will explore a new region of the parameter space, reaching models with τ$_{χ}$ > 10$^{27}$ s for DM masses above 1 TeV.These constraints will provide unprecedented sensitivity to the physics of both CRp acceleration and transport at cluster scale and to TeV DM particle models, especially in the decay scenario.
536 _ _ |a 613 - Matter and Radiation from the Universe (POF4-613)
|0 G:(DE-HGF)POF4-613
|c POF4-613
|f POF IV
|x 0
536 _ _ |a DFG project G:(GEPRIS)445052434 - SFB 1491: Das Wechselspiel der kosmischen Materie - von der Quelle bis zum Signal (445052434)
|0 G:(GEPRIS)445052434
|c 445052434
|x 1
588 _ _ |a Dataset connected to CrossRef, Journals: bib-pubdb1.desy.de
650 _ 7 |a galaxy: cluster
|2 INSPIRE
650 _ 7 |a gamma ray: emission
|2 INSPIRE
650 _ 7 |a dark matter: annihilation
|2 INSPIRE
650 _ 7 |a p: cosmic radiation
|2 INSPIRE
650 _ 7 |a dark matter: halo
|2 INSPIRE
650 _ 7 |a energy: thermal
|2 INSPIRE
650 _ 7 |a dark matter: mass
|2 INSPIRE
650 _ 7 |a dark matter: decay
|2 INSPIRE
650 _ 7 |a cross section: annihilation
|2 INSPIRE
650 _ 7 |a energy: ratio
|2 INSPIRE
650 _ 7 |a gamma ray: energy
|2 INSPIRE
650 _ 7 |a particle: model
|2 INSPIRE
650 _ 7 |a Cherenkov Telescope Array
|2 INSPIRE
650 _ 7 |a sensitivity
|2 INSPIRE
650 _ 7 |a TeV
|2 INSPIRE
650 _ 7 |a acceleration
|2 INSPIRE
650 _ 7 |a spectral
|2 INSPIRE
650 _ 7 |a power spectrum
|2 INSPIRE
650 _ 7 |a gas
|2 INSPIRE
650 _ 7 |a magnetic field
|2 INSPIRE
650 _ 7 |a spatial distribution
|2 INSPIRE
650 _ 7 |a formation
|2 INSPIRE
650 _ 7 |a structure
|2 INSPIRE
650 _ 7 |a history
|2 INSPIRE
650 _ 7 |a cosmic ray experiments
|2 autogen
650 _ 7 |a dark matter experiments
|2 autogen
650 _ 7 |a galaxy clusters
|2 autogen
650 _ 7 |a gamma ray experiments
|2 autogen
693 _ _ |0 EXP:(DE-H253)CTA-20150101
|5 EXP:(DE-H253)CTA-20150101
|e Cherenkov Telescope Array
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700 1 _ |a Abe, S.
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700 1 _ |a Acero, F.
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700 1 _ |a Acharyya, A.
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700 1 _ |a Adam, R.
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