Probing the IGMF with the Next Generation of Cherenkov Telescopes

Intergalactic space is believed to contain nonzero magnetic fields (the Intergalactic Magnetic Field: IGMF), which at scales of megaparsecs would have intensities below 10-9 G. Very high energy (VHE > 100 GeV) gamma-rays coming from blazars can produce e+e- pairs when interacting with the ext...

Descripción completa

Guardado en:
Detalles Bibliográficos
Publicado: 2018
Materias:
astroparticle physics
gamma rays: galaxies
magnetic fields
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v869_n1_p_Alonso
http://hdl.handle.net/20.500.12110/paper_0004637X_v869_n1_p_Alonso
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_0004637X_v869_n1_p_Alonso
record_format dspace
spelling paper:paper_0004637X_v869_n1_p_Alonso2023-06-08T14:29:21Z Probing the IGMF with the Next Generation of Cherenkov Telescopes astroparticle physics gamma rays: galaxies magnetic fields Intergalactic space is believed to contain nonzero magnetic fields (the Intergalactic Magnetic Field: IGMF), which at scales of megaparsecs would have intensities below 10-9 G. Very high energy (VHE > 100 GeV) gamma-rays coming from blazars can produce e+e- pairs when interacting with the extragalactic background light (EBL) and the cosmic microwave background, generating an electromagnetic cascade of megaparsec scale. The IGMF may produce a detectable broadening of the emission beam that could lead to important constrains both on the IGMF intensity and its coherence length. Using the Monte Carlo-based Elmag code, we simulate the electromagnetic cascade corresponding to two detected TeV sources: PKS 2155-304 visible from the south and H1426+428 visible from the north. Assuming an EBL model and intrinsic spectral properties of the sources, we obtain the spectral and angular distribution of photons when they arrive at Earth. We include the response of the next generation Cherenkov telescopes by using simplified models for Cherenkov Telescope Array (CTA)-south and CTA-north based on a full simulation of each array performance. Combining the instrument properties with the simulated source fluxes, we calculate the telescope point-spread function for null and non-null IGMF intensities and develop a method to test the statistical feasibility of detecting IGMF imprints by comparing the resulting angular distributions. Our results show that for the analyzed source PKS 2155-304 corresponding to the southern site, CTA should be able to detect IGMF with intensities stronger than 10-14.5 G within an observation time of ∼100 hr. © 2018. The American Astronomical Society. All rights reserved. 2018 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v869_n1_p_Alonso http://hdl.handle.net/20.500.12110/paper_0004637X_v869_n1_p_Alonso
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic astroparticle physics
gamma rays: galaxies
magnetic fields
spellingShingle astroparticle physics
gamma rays: galaxies
magnetic fields
Probing the IGMF with the Next Generation of Cherenkov Telescopes
topic_facet astroparticle physics
gamma rays: galaxies
magnetic fields
description Intergalactic space is believed to contain nonzero magnetic fields (the Intergalactic Magnetic Field: IGMF), which at scales of megaparsecs would have intensities below 10-9 G. Very high energy (VHE > 100 GeV) gamma-rays coming from blazars can produce e+e- pairs when interacting with the extragalactic background light (EBL) and the cosmic microwave background, generating an electromagnetic cascade of megaparsec scale. The IGMF may produce a detectable broadening of the emission beam that could lead to important constrains both on the IGMF intensity and its coherence length. Using the Monte Carlo-based Elmag code, we simulate the electromagnetic cascade corresponding to two detected TeV sources: PKS 2155-304 visible from the south and H1426+428 visible from the north. Assuming an EBL model and intrinsic spectral properties of the sources, we obtain the spectral and angular distribution of photons when they arrive at Earth. We include the response of the next generation Cherenkov telescopes by using simplified models for Cherenkov Telescope Array (CTA)-south and CTA-north based on a full simulation of each array performance. Combining the instrument properties with the simulated source fluxes, we calculate the telescope point-spread function for null and non-null IGMF intensities and develop a method to test the statistical feasibility of detecting IGMF imprints by comparing the resulting angular distributions. Our results show that for the analyzed source PKS 2155-304 corresponding to the southern site, CTA should be able to detect IGMF with intensities stronger than 10-14.5 G within an observation time of ∼100 hr. © 2018. The American Astronomical Society. All rights reserved.
title Probing the IGMF with the Next Generation of Cherenkov Telescopes
title_short Probing the IGMF with the Next Generation of Cherenkov Telescopes
title_full Probing the IGMF with the Next Generation of Cherenkov Telescopes
title_fullStr Probing the IGMF with the Next Generation of Cherenkov Telescopes
title_full_unstemmed Probing the IGMF with the Next Generation of Cherenkov Telescopes
title_sort probing the igmf with the next generation of cherenkov telescopes
publishDate 2018
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v869_n1_p_Alonso
http://hdl.handle.net/20.500.12110/paper_0004637X_v869_n1_p_Alonso
_version_ 1768544984016879616

Ejemplares similares