Science With The Cherenkov Telescope Array

• Autore: The Cta Consortium
• Pubblicazione: Singapore : , : World Scientific Publishing Company, , 2018; ©2019
• Descrizione fisica: 1 electronic resource (364 p.)
• Disciplina: 522/.6862
• Soggetto topico: Gamma ray astronomy; Astronomy
• Soggetto non controllato: Gamma Rays; Astrophysics; Cherenkov Telescope Array (CTA); Cherenkov Telescopes; Astroparticle Physics; Multiwavelength; Multimessenger; Astronomy; Dark Matter
• Altri autori: OngRene A The Cta Consortium
• Nota di contenuto: Intro -- Contents -- Executive Summary -- Authors -- Acknowledgements -- Chapters and Corresponding Authors -- Chapter 1. Introduction to CTA Science -- 1.1 Key Characteristics and Capabilities -- 1.1.1 Surveying Capabilities -- 1.1.2 Short Timescale Capabilities -- 1.1.3 Capabilities Beyond Gamma Rays -- 1.2 Overview of CTA Science Themes -- 1.2.1 Understanding the Origin and Role of Relativistic Cosmic Particles -- 1.2.1.1 Cosmic accelerators -- 1.2.1.2 Propagation and influence of accelerated particles -- 1.2.2 Probing Extreme Environments -- 1.2.2.1 Black holes and jets -- 1.2.2.2 Neutron stars and relativistic outflows -- 1.2.2.3 Cosmic voids -- 1.2.3 Exploring Frontiers in Physics -- 1.2.3.1 Dark matter -- 1.2.3.2 Quantum gravity and axion-like particle search -- 1.3 Community Input to the Science Case -- Chapter 2. Synergies -- 2.1 Radio to (Sub)Millimetre -- 2.2 Infrared/Optical through Ultraviolet and Transient Factories -- 2.3 X-ray -- 2.4 Sub-VHE Gamma-ray Energies -- 2.5 Complementary VHE Gamma-ray Instruments -- 2.6 VHE and UHE Neutrinos -- 2.7 Gravitational Waves -- Chapter 3. Core Programme Overview -- Chapter 4. Dark Matter Programme -- 4.1 Science Targeted -- 4.1.1 Existence of Dark Matter -- 4.1.2 Distribution of Dark Matter -- 4.1.3 The Nature of Dark Matter -- 4.1.4 Search Methods for Dark Matter -- 4.1.5 Annihilation of Dark Matter Particles -- 4.1.6 Parameters Expected for WIMP Dark Matter -- 4.1.7 Rate of Gamma Rays in Detector -- 4.2 Strategy -- 4.2.1 Milky Way -- 4.2.1.1 Description -- 4.2.1.2 Evolution of knowledge -- 4.2.1.3 Observational strategy -- 4.2.1.4 Performance -- 4.2.2 Dwarf Spheroidal Galaxies and Dark Clumps -- 4.2.2.1 Description -- 4.2.2.2 Evolution of knowledge -- 4.2.2.3 Observational strategy -- 4.2.2.4 Performance -- 4.2.3 Large Magellanic Cloud -- 4.2.3.1 Description -- 4.2.3.2 Evolution of knowledge. ; 4.2.3.3 Observational strategy -- 4.2.3.4 Performance -- 4.2.4 Clusters of Galaxies -- 4.2.5 Summary of Targets -- 4.3 Data Products -- Chapter 5. KSP: Galactic Centre -- 5.1 Science Targeted -- 5.1.1 Scientific Objectives -- 5.1.1.1 Revealing the nature of the central gamma-ray source -- 5.1.1.2 Diffuse VHE emission: Particle acceleration in the vicinity of the Galactic Centre -- 5.1.1.3 Exploring large-scale outflows -- 5.1.1.4 Supernova remnants, pulsar-wind nebulae, and molecular clouds -- 5.1.2 Context/Advance beyond State of the Art -- 5.1.2.1 Central engine -- 5.1.2.2 Advances in the study of diffuse emission -- 5.2 Strategy -- 5.2.1 Timeline and Sub-array Choice -- 5.2.2 Relation to other KSPs -- 5.2.3 Analysis Strategy -- 5.3 Data Products -- 5.4 Expected Performance/Return -- 5.4.1 Determination of the Nature of the Central Source -- 5.4.2 A Detailed View of the Diffuse VHE Emission -- 5.4.3 Resolving New, Previously Undetectable Sources -- 5.4.4 Search for Variability in the VHE Source Near Sgr A* -- 5.4.5 Studying the Interaction of the Central Source with Neighbouring Clouds -- 5.4.6 Science Impact -- Chapter 6. KSP: Galactic Plane Survey -- 6.1 Science Targeted -- 6.1.1 Scientific Objectives -- 6.1.2 Context/Advance beyond State of the Art -- 6.1.3 Multi-wavelength/Multi-messenger Context -- 6.1.3.1 Synergy with HAWC -- 6.1.3.2 Synergies with other instruments -- 6.2 Strategy -- 6.2.1 Observation Requirements -- 6.2.2 Targets, Observation Strategy, and Follow-ups -- 6.2.3 Relation/Importance to other KSPs -- 6.3 Data Products -- 6.4 Expected Performance/Return -- 6.4.1 Performance of the CTA GPS -- 6.4.2 Source Confusion -- 6.4.3 Summary -- Chapter 7. KSP: Large Magellanic Cloud Survey -- 7.1 Science Targeted -- 7.1.1 Scientific Objectives -- 7.1.2 Context/Advance beyond State of the Art -- 7.2 Strategy -- 7.3 Data Products. ; 7.4 Expected Performance/Return -- Chapter 8. KSP: Extragalactic Survey -- 8.1 Science Targeted -- 8.1.1 Scientific Objectives -- 8.1.2 Context/advance beyond state of the art -- 8.2 Strategy -- 8.2.1 Possibility of Several Pointings for a given Field of View -- 8.2.2 Shallow survey versus deep survey -- 8.2.3 Targets -- 8.3 Data Products -- 8.4 Expected Performance/Return -- 8.4.1 Method -- 8.4.2 Serendipitous Discoveries during the Construction Phase -- 8.4.3 Results after the Completion of the Survey -- 8.4.4 Participation of LSTs -- 8.4.5 Prospects for Divergent Pointing -- Chapter 9. KSP: Transients -- 9.1 Science Targeted -- 9.1.1 Scientific Objectives -- 9.1.2 Context/Advance beyond State of the Art -- 9.2 Strategy -- 9.3 Data Products -- 9.4 Expected Performance/Return -- Chapter 10. KSP: Cosmic Ray PeVatrons -- 10.1 Science Targeted -- 10.1.1 Scientific Objectives -- 10.1.2 Context/Advance beyond State of the Art -- 10.1.2.1 Hadronic mechanisms and the connection with cosmic-ray origin -- 10.2 Strategy -- 10.2.1 Targets -- 10.3 Data Products -- 10.4 Expected Performance/Return -- Chapter 11. KSP: Star Forming Systems -- 11.1 Science Targeted -- 11.1.1 Scientific Objectives -- 11.1.2 Context/Advance beyond State of the Art -- 11.1.2.1 Star-forming regions -- 11.1.2.2 Star-forming galaxies -- 11.1.2.3 Starburst galaxies -- 11.1.2.4 ULIRGs -- 11.2 Strategy -- 11.3 Data Products -- 11.4 Expected Performance/Return -- 11.4.1 Star-forming Regions -- 11.4.2 Star-forming Galaxies -- 11.4.3 Starburst Galaxies -- 11.4.4 ULIRGs -- Chapter 12. KSP: Active Galactic Nuclei -- 12.1 Science Targeted -- 12.1.1 Relativistic Jets from Supermassive Black Holes -- 12.1.1.1 What are the relevant particle acceleration and emission processes in VHE blazars? How are different blazar types related?. ; 12.1.1.2 What causes the observed variability in AGN from time scales of a few years down to a few minutes? -- 12.1.1.3 From where does the VHE emission of radio galaxies originate? -- 12.1.1.4 Do other classes of AGN emit VHE gamma rays? -- 12.1.2 Blazars as Probes of the Universe -- 12.1.2.1 What is the spectrum of the EBL at redshift z ∼ 0 and how does it evolve at higher redshifts? -- 12.1.2.2 What is the strength of the IGMF? -- 12.1.3 UHECRs and Fundamental Physics -- 12.1.3.1 AGN as potential sources of UHECRs -- 12.1.3.2 Can we find signatures for the existence of axion-like particles? -- 12.1.3.3 Can we rule out Lorentz Invariance Violation? -- 12.1.4 Advance beyond State of the Art -- 12.2 Strategy -- 12.2.1 Target Selection -- 12.2.1.1 Long-term monitoring -- 12.2.1.2 AGN flare programme -- 12.2.1.3 High-quality spectra -- 12.2.1.4 Time distribution model for the AGN KSP -- 12.2.2 Multi-wavelength and Multi-messenger Coverage -- 12.3 Data Products -- 12.4 Expected Performance/Return -- 12.4.1 Guaranteed Science Return -- 12.4.2 Discovery Potential -- Chapter 13. KSP: Clusters of Galaxies -- 13.1 Science Targeted -- 13.1.1 Scientific Objectives -- 13.1.2 Context/Advance beyond State of the Art -- 13.2 Strategy -- 13.2.1 Targets -- 13.3 Data Products -- 13.4 Expected Performance/Return -- Chapter 14. Capabilities beyond Gamma Rays -- 14.1 Cosmic-Ray Nuclei -- 14.2 Cosmic-Ray Electrons -- 14.3 Optical Measurements with CTA -- Chapter 15. Appendix: Simulating CTA -- References -- Glossary.
• Sommario/riassunto: This book summarizes the science to be carried out by the upcoming Cherenkov Telescope Array, a major ground-based gamma-ray observatory that will be constructed over the next six to eight years. The major scientific themes, as well as core program of key science projects, have been developed by the CTA Consortium, a collaboration of scientists from many institutions worldwide. CTA will be the major facility in high-energy and very high-energy photon astronomy over the next decade and beyond. CTA will have capabilities well beyond past and present observatories. Thus, CTA's science program is expected to be rich and broad and will complement other major multiwavelength and multimessenger facilities. This book is intended to be the primary resource for the science case for CTA and it thus will be of great interest to the broader physics and astronomy communities. The electronic version (e-book) is available in open access.
• Titolo autorizzato: Science With The Cherenkov Telescope Array
• ISBN: 981-327-010-1; 981-327-009-8
• Formato: Materiale a stampa
• Livello bibliografico: Monografia
• Lingua di pubblicazione: Inglese
• Record Nr.: 9910346694803321
• Lo trovi qui: Univ. Federico II