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000596676 0247_ $$2doi$$a10.1093/mnras/stad1576
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000596676 0247_ $$2ISSN$$a0035-8711
000596676 0247_ $$2ISSN$$a1365-2966
000596676 0247_ $$2ISSN$$a1365-8711
000596676 0247_ $$2arXiv$$aarXiv:2305.16707
000596676 0247_ $$2altmetric$$aaltmetric:149068781
000596676 0247_ $$2WOS$$aWOS:001023895800033
000596676 0247_ $$2openalex$$aopenalex:W4378446371
000596676 037__ $$aPUBDB-2023-06222
000596676 041__ $$aEnglish
000596676 082__ $$a520
000596676 088__ $$2arXiv$$aarXiv:2305.16707
000596676 1001_ $$aAcharyya, A.$$b0
000596676 245__ $$aSensitivity of the Cherenkov Telescope Array to TeV photon emission from the Large Magellanic Cloud
000596676 260__ $$aOxford$$bOxford Univ. Press$$c2023
000596676 3367_ $$2DRIVER$$aarticle
000596676 3367_ $$2DataCite$$aOutput Types/Journal article
000596676 3367_ $$0PUB:(DE-HGF)16$$2PUB:(DE-HGF)$$aJournal Article$$bjournal$$mjournal$$s1697547636_3725953
000596676 3367_ $$2BibTeX$$aARTICLE
000596676 3367_ $$2ORCID$$aJOURNAL_ARTICLE
000596676 3367_ $$00$$2EndNote$$aJournal Article
000596676 500__ $$aAccepted for publication in MNRAS. Corresponding authors: Pierrick Martin, Maria Isabel Bernardos Martin, Fabio IoccoWaiting for fulltext 
000596676 520__ $$aA deep survey of the Large Magellanic Cloud at ~0.1-100TeV photon energies with the Cherenkov Telescope Array is planned. We assess the detection prospects based on a model for the emission of the galaxy, comprising the four known TeV emitters, mock populations of sources, and interstellar emission on galactic scales. We also assess the detectability of 30 Doradus and SN 1987A, and the constraints that can be derived on the nature of dark matter. The survey will allow for fine spectral studies of N157B, N132D, LMC P3, and 30 Doradus C, and half a dozen other sources should be revealed, mainly pulsar-powered objects. The remnant from SN 1987A could be detected if it produces cosmic-ray nuclei with a flat power-law spectrum at high energies, or with a steeper index 2.3-2.4 pending a flux increase by a factor >3-4 over ~2015-2035. Large-scale interstellar emission remains mostly out of reach of the survey if its >10GeV spectrum has a soft photon index ~2.7, but degree-scale 0.1-10TeV pion-decay emission could be detected if the cosmic-ray spectrum hardens above >100GeV. The 30 Doradus star-forming region is detectable if acceleration efficiency is on the order of 1-10% of the mechanical luminosity and diffusion is suppressed by two orders of magnitude within <100pc. Finally, the survey could probe the canonical velocity-averaged cross section for self-annihilation of weakly interacting massive particles for cuspy Navarro-Frenk-White profiles.
000596676 536__ $$0G:(DE-HGF)POF4-613$$a613 - Matter and Radiation from the Universe (POF4-613)$$cPOF4-613$$fPOF IV$$x0
000596676 588__ $$aDataset connected to CrossRef, INSPIRE, Journals: bib-pubdb1.desy.de
000596676 650_7 $$2INSPIRE$$aphoton: energy
000596676 650_7 $$2INSPIRE$$aacceleration: efficiency
000596676 650_7 $$2INSPIRE$$aenergy: high
000596676 650_7 $$2INSPIRE$$aphoton: emission
000596676 650_7 $$2INSPIRE$$anucleus: cosmic radiation
000596676 650_7 $$2INSPIRE$$acosmic radiation: spectrum
000596676 650_7 $$2INSPIRE$$aCherenkov Telescope Array
000596676 650_7 $$2INSPIRE$$agamma ray: emission
000596676 650_7 $$2INSPIRE$$agalaxy
000596676 650_7 $$2INSPIRE$$aTeV
000596676 650_7 $$2INSPIRE$$aspectral
000596676 650_7 $$2INSPIRE$$adiffusion
000596676 650_7 $$2INSPIRE$$adark matter: annihilation
000596676 650_7 $$2INSPIRE$$asensitivity
000596676 650_7 $$2INSPIRE$$aWIMP
000596676 650_7 $$2INSPIRE$$aflux
000596676 650_7 $$2INSPIRE$$asuppression
000596676 650_7 $$2INSPIRE$$aNavarro-Frenk-White profile
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000596676 7001_ $$0P:(DE-HGF)0$$aIocco, F.$$b152$$eCorresponding author
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000596676 773__ $$0PERI:(DE-600)2016084-7$$a10.1093/mnras/stad1576$$gVol. 523, no. 4, p. 5353 - 5387$$n4$$p5353 - 5387$$tMonthly notices of the Royal Astronomical Society$$v523$$x0035-8711$$y2023
000596676 7870_ $$0PUBDB-2023-03711$$aAcharyya, A. et.al.$$d2023$$iIsParent$$rarXiv:2305.16707$$tSensitivity of the Cherenkov Telescope Array to TeV photon emission from the Large Magellanic Cloud
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