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Probing Dark Matter and Fundamental Physics with the Cherenkov Telescope Array

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Probing Dark Matter and Fundamental Physics with the Cherenkov Telescope Array cherenkov telescope array Probing Dark Matter and Fundamental Physics with the Cherenkov Telescope Array Authors: F. Iocco (Università “Federico II”& INFN sezione di Napoli, Italy), M. Meyer (University of Hamburg, Germany), M. Doro (University of Padova), W. Hofmann (Max Planck Institute for Nuclear Physics, Heidelberg, Germany), J. Pérez-Romero (Instituto de Física Téorica UAM-CSIC, Universidad Autónoma de Madrid, Spain), G. Zaharijas (University of Nova Gorica), (continues on next page) Contact points: [email protected], [email protected] https://www.cta-observatory.org/about/cta-consortium/ Credit: Gabriel Pérez Diaz (IAC)/Marc-André Besel (CTAO)/ESO/ N. Risinger (skysurvey.org) arXiv:2106.03582v2 [astro-ph.HE] 9 Jun 2021 Astrophysical observations provide strong evidence that more than 80% of all matter in the Universe is in the form of dark matter (DM). Two leading candidates of particles beyond the Standard Model that could constitute all or a fraction of the DM content are the so-called Weakly Interacting Massive Particles (WIMPs) and Axion-Like Particles (ALPs). The upcoming Cherenkov Telescope Array, which will observe gamma rays between 20 GeV and 300 TeV with unprecedented sensitivity, will have unique capabilities to search for these DM candidates. A particularly promising target for WIMP searches is the Galactic Center. WIMPs with annihilation cross sections correctly producing the DM relic density will be detectable with CTA, assuming an Einasto-like density profile and WIMP masses between 200 GeV and 10 TeV. Regarding new physics beyond DM, CTA observations will also enable tests of fundamental symmetries of nature such as Lorentz invariance. 1. Introduction A. Aguirre-Santaella (Instituto de F´ısica Teorica´ UAM-CSIC, Universidad Autonoma´ de Madrid, Spain), E. Amato (INAF-Osservatorio Astrofisico di Arcetri, Italy), E.O. Anguner (Centre de Physique des Par- ticules de Marseille, France), L.A. Antonelli (INAF-Osservatorio Astronomico di Roma, Italy), Y. Asca- sibar (Universidad Autonoma´ de Madrid, Spain), C. Balazs´ (Monash University, Melbourne, Australia), G. Beck (University of the Witwatersrand, South Africa), C. Bigongiari (INAF-Osservatorio Astronomico di Roma, Italy), J. Bolmont (LPNHE, CNRS/IN2P3, Sorbonne University, France), T. Bringmann (Univer- sity of Oslo), A.M. Brown (Durham University, U.K.), M.G. Burton (Armagh Observatory & Planetarium, UK), M. Cardillo (INAF - IAPS, Roma, Italy) S. Chaty (University of Paris & CEA, France), G. Cotter (University of Oxford, UK), D. della Volpe (Universite´ de Geneve),` A. Djannati-Ata¨ı (Universite´ de Paris, CNRS/IN2P3, APC, France), C. Eckner (University of Nova Gorica), G. Emery, (Universite´ de Geneve),` E. Fedorova (Taras Shevchenko National University of Kyiv), M. D. Filipovic (Western Sydney University, Australia), G. Galanti (INAF - IASF Milano, Italy), V. Gammaldi (Instituto de F´ısica Teorica´ UAM-CSIC, Universidad Autonoma´ de Madrid), E. M. de Gouveia Dal Pino (IAG-USP - Universidade de Sao˜ Paulo, Brazil), J. Granot (Open University of Israel, Israel), J.G. Green (INAF - Osservatorio Astronomico di Roma, Italy), K. Hayashi (National Institute of Technology, Ichinoseki College, Japan), S. Hernandez-´ Cadena (Instituto de F´ısica, Universidad Nacional Autonoma´ de Mexico),´ N. Hiroshima (RIKEN, In- stitute of Physical and Chemical Research, Japan), B. Hnatyk (Taras Shevchenko National University of Kyiv), D. Horan (LLR/Ecole Polytechnique, CNRS/IN2P3, France), M. Hutten¨ (Max Planck Institute for Physics, Germany), M. Jamrozy (Jagiellonian University, Poland), A. Lamastra (INAF - Osservatorio Astronomico di Roma, Italy), J.-P.Lenain (LPNHE, CNRS/IN2P3, Sorbonne Universite,´ France), E. Lind- fors (FINCA, University of Turku, Finland), I. Liodakis (FINCA, University of Turku, Finland), S. Lombardi (INAF-Osservatorio Astronomico di Roma, Italy), F. Longo (University and INFN, Trieste, Italy), F. Lu- carelli (INAF - Oss. Astr. di Roma and ASI-SSDC, Italy), K. Kohri (Institute of Particle and Nuclear Studies, KEK, Japan), M. Martinez (Institut de F´ısica d’Altes Energies, IFAE-BIST, Barcelona, Spain), H. Mart´ınez-Huerta (Departamento de F´ısica y Matematicas,´ Universidad de Monterrey, Mexico),´ D. Mazin (ICRR, University of Tokyo, Japan and MPI for physics, Germany), A. Moralejo (Institut de F´ısica d’Altes Energies, IFAE-BIST, Barcelona, Spain), A. Morselli (INFN Roma Tor Vergata, Italy), C.G. Mundell (University of Bath, UK), R.A. Ong, (University of California, Los Angeles, USA), V. Poireau (LAPP, CNRS/IN2P3, Univ. Savoie Mont Blanc, France), O. Reimer (Innsbruck University, Institute for Astro- and Particle Physics, Austria), J. Rico (Institut de Fisica d’Altes Energies, Barcelona, Spain), G. Romeo (INAF - Osservatorio Astrofisico di Catania, Italy), P.Romano (INAF, Osservatorio Astronomico di Brera), G. Rowell (University of Adelaide, Australia), I. Sadeh (DESY-Zeuthen, Germany), M.A. Sanchez-Conde´ (Instituto de F´ısica Teorica´ UAM-CSIC, Universidad Autonoma´ de Madrid, Spain), F.G. Saturni (INAF - Osservatorio Astronomico di Roma, Italy), O. Sergijenko (Taras Shevchenko National University of Kyiv), H. Sol (LUTH, Observatoire de Paris, CNRS, France), A. Stamerra (INAF, Osservatorio Astronomico di Roma, Italy), Th. Stolarczyk (AIM, CEA, CNRS, Universite´ Paris-Saclay, Universite´ de Paris, France), F. Tavecchio (INAF, Osservatorio Astronomico di Brera), S. Vercellone (INAF, Osservatorio Astronomico di Brera), V. Testa (INAF - Osservatorio Astronomico di Roma, Italy), L. Tibaldo (IRAP - Universite´ de Toulouse, CNRS, UPS, CNES, France), M. Vecchi (Kapteyn Astronomical Institute, University of Groningen), A. Viana (IFSC - Universidade de Sao˜ Paulo, Brazil), V. Vitale (INFN - Roma Tor Vergata), V. Zhdanov (Taras Shevchenko National University of Kyiv) on behalf of the CTA consortium 1 Introduction Astrophysical observations of different objects such as spiral galaxies, galaxy clusters, elliptical galax- ies, galaxies with low surface brightness and dwarf spheroidal galaxies all indicate the existence of a non-baryonic dark component of matter [1]. Together with independent observations of the Early Universe this is interpreted in the self-consistent paradigm of a Λ cold dark matter Universe [2]. No mundane astrophysical population, and no particle predicted by the Standard Model, can provide a “standard physics” candidate for the dark matter (DM), since they do not fulfill the requirements of the above-mentioned observations [3]. Thus, evidence for physics beyond the Standard Model of particles intriguingly arises from astrophysical observations. Many well-motivated extensions of the Standard Model have been devised, which provide new particle candidates that, on the one hand, comply with the observational requirements for DM, and, on the other hand, provide a minimal coupling to the visible sector, offering a window for potential observations. Interestingly, for many of the potential candidates the coupling with Standard Model particles would CTA Consortium Page 2 of7 j Issue j Rev. 2. WIMP searches produce radiation at energies above the GeV scale, thus making gamma-ray observatories ideal tools in the search for the dark matter. Such radiation would be visible “in excess” on the top of the standard astrophysical sources, thus requiring a rigorous characterization of the fore and background signals, and a strategic choice of target objects. Weakly interacting Massive Particles (WIMPs) and Axion Like Particles (ALPs) are recognized to be particularly promising class of candidates [3,4]. With a factor 5-20 higher sensitivity, better spectral and angular resolution than current Imaging Atmo- spheric Cherenkov Telescopes [5], the Cherenkov Telescope Array (CTA) will be the prime instrument for gamma-ray astronomy and DM searches over the coming decades. CTA will be a unique tool for the astrophysics community to delve into the exploration of physics beyond the Standard Model. 2 WIMP searches 2.1 Rationale of WIMP annihilation / mechanism Weakly Interacting Massive Particles are promising particle candidates for the DM: the same process of self-annihilation into Standard Model particles, which dictates their relic abundance in the Early Universe would allow them today to produce prompt or secondary gamma-ray emission in environments rich in DM. Such particles with masses and couplings at the electroweak scale would be a compelling solution to the DM puzzle because their existence would explain the presently measured DM abundance as a result of the thermal history of the Universe and, at the same time, it might address the naturalness problems in the Standard Model of particle physics. CTA is expected to reach the benchmark value of the (velocity weighted) annihilation cross-section of roughly (3 10−26 cm3 s−1) for WIMPs produced thermally in the early Universe, thus being the only gamma-ray× instrument –planned or existing– capable of testing physics beyond the Standard Model at the TeV scale in astrophysical environments. This complements direct DM searches in underground laboratories or WIMP searches at colliders (see, e.g., Ref. [6]). 2.2 Targets CTA will observe different targets in the search for DM, which are selected on the rationale that the signal produced by DM annihilation is larger in close-by regions with high DM density. Galactic center (GC). The GC region has the largest DM signal (albeit large uncertainties), of all known targets and will be an essential DM target for CTA. However, the GC hosts a rich environment of astrophysical
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