In this contribution, a search for neutrino emission from the Central Molecular Zone (CMZ) and Cygnus OB2 with the KM3NeT/ARCA detector is presented. The CMZ extends for a few hundred parsecs around the Galactic center, containing the massive molecular clouds Sgr A, Sgr B, and Sgr C. Cygnus OB2 is a massive star-forming region of a few parsecs in the constellation of Cygnus. It contains regions with high gas densities and a rich stellar population. The high energy gamma-ray emission from these regions could be dominated by the interactions of cosmic-rays with the molecular gas, resulting in the production of gamma-rays and neutrinos. Here we present a search for neutrino emission from these two regions. The corresponding sensitivities of the current KM3NeT/ARCA geometry as well as the case of the complete future detector are explored. No significant excess was observed, therefore we set upper limits.

Prospects of neutrino observations of the Central Molecular Zone and Cygnus OB2 with KM3NeT/ARCA

Benhassi M.;Buompane R.;De Benedittis A.;Gialanella L.;Idrissi Ibnsalih W.;Mitsou M. L.;Morales-Gallegos L.;Musone M. R.;Vivolo D.;
2025

Abstract

In this contribution, a search for neutrino emission from the Central Molecular Zone (CMZ) and Cygnus OB2 with the KM3NeT/ARCA detector is presented. The CMZ extends for a few hundred parsecs around the Galactic center, containing the massive molecular clouds Sgr A, Sgr B, and Sgr C. Cygnus OB2 is a massive star-forming region of a few parsecs in the constellation of Cygnus. It contains regions with high gas densities and a rich stellar population. The high energy gamma-ray emission from these regions could be dominated by the interactions of cosmic-rays with the molecular gas, resulting in the production of gamma-rays and neutrinos. Here we present a search for neutrino emission from these two regions. The corresponding sensitivities of the current KM3NeT/ARCA geometry as well as the case of the complete future detector are explored. No significant excess was observed, therefore we set upper limits.
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11591/587167
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