Studying star forming regions in all scales with the Cherenkov Telescope Array

• Grant number: 25/20917-3
• Support Opportunities: Scholarships in Brazil - Scientific Initiation
• Start date: November 01, 2025
• End date: October 31, 2026
• Field of knowledge: Physical Sciences and Mathematics - Astronomy
• Principal Investigator: Elisabete Maria de Gouveia Dal Pino
• Grantee: Gabriel Almeida Moraes
• Host Institution: Instituto de Astronomia, Geofísica e Ciências Atmosféricas (IAG). Universidade de São Paulo (USP). São Paulo , SP, Brazil
• Associated research grant: 21/02120-0 - Investigation of high energy and plasma astrophysics phenomena, installation of the ASTRI-Mini Array & construction of the Cherenkov Telescope Array Small Size Telescopes (CTA-SSTs), AP.ESP

Abstract

Star formation (SF) is a fundamental process in the cosmic cycle of matter, spanning a wide range of spatial scales and involving complex interactions between gas, radiation, magnetic fields, and cosmic rays (CRs). CRs are closely linked to the life cycle of massive stars and are believed to be produced in several astrophysical environments, including massive star clusters (MSCs), supernova remnants (SNRs), and superbubbles. These regions often exhibit non-thermal emission signatures, including in the gamma-ray regime, hinting at efficient CR acceleration processes up to very high energies. However, the exact mechanisms driving CR acceleration across these environments-such as diffusive shock acceleration (DSA), and stochastic acceleration via turbulence-driven magnetic reconnection-remain actively debated.This scientific initiation project explores the connection between CR acceleration and gamma-ray emission in star-forming regions across multiple scales, with a particular focus on TeV gamma-ray observations using the upcoming Cherenkov Telescope Array Observatory (CTAO). The project employs 3D magnetohydrodynamic (MHD) simulations to study the dynamical evolution of molecular clouds and star-forming galaxies. Using test-particle methods embedded in MHD frameworks developed by the research group, the study investigates how compact sources embedded within star-forming environments contribute to CR acceleration and associated emission processes.One core objective is to generate realistic density and magnetic field templates of star-forming regions from MHD simulations. These templates are then used to model gamma-ray emission from CR interactions, both in localized halos and in diffuse backgrounds. The resulting physical models are coupled with CTAO simulation tools (e.g., ctools and CTAO instrument response functions) to create synthetic gamma-ray observations, which predict how CTAO will observe these regions once operational.This approach allows for a detailed assessment of the observational signatures of different CR acceleration mechanisms and their spatial correlations with the structure of the interstellar medium. It also addresses challenges in distinguishing source emission from diffuse gamma-ray backgrounds, an essential step for interpreting extended gamma-ray sources in the CTAO era.Through this multi-faceted methodology combining numerical simulations and observational modeling, the project aims to deepen our understanding of the interplay between star formation, turbulence, magnetic fields, and CR-driven gamma-ray emission. The outcomes are expected to contribute to the interpretation of future CTAO data and to broader efforts in high-energy astrophysics and galactic evolution.