Chapter 2 Galactic Gamma-ray Sources * *Supported by Key Research and Development Project (2018YFA0404204, 2016YFA0400804), the National Natural Science Foundation of China (11905043, 11803011, 12173018, 12121003, 11773014, 11633007, U1931204, U1731136), the Original Innovation Program of the Chinese Academy of Sciences (E085021002), Guangdong Major Project of Basic and Applied Basic Research (2019B030302001) and science research grant from the China Manned Space

Abstract

In the γ-ray sky, the highest fluxes come from Galactic sources: supernova remnants (SNRs), pulsars and pulsar wind nebulae, star forming regions, binaries and micro-quasars, giant molecular clouds, Galactic center, and the large extended area around the Galactic plane. The radiation mechanisms of γ-ray emission and the physics of the emitting particles, such as the origin, acceleration, and propagation, are of very high astrophysical significance. A variety of theoretical models have been suggested for the relevant physics, and emission with energies E≥1014 eV are expected to be crucial in testing them. In particular, this energy band is a direct window to test at which maximum energy a particle can be accelerated in the Galactic sources and whether the most probable source candidates such as Galactic center and SNRs are “PeVatrons”. Designed aiming at the very high energy (VHE, >100 GeV) observation, LHAASO will be a very powerful instrument in these astrophysical studies. Over the past decade, great advances have been made in the VHE γ-ray astronomy. More than 170 VHE γ-ray sources have been observed, and among them, 42 Galactic sources fall in the LHAASO field-of-view. With a sensitivity of 10 milli-Crab, LHAASO can not only provide accurate spectra for the known γ-ray sources, but also search for new TeV-PeV γ-ray sources. In the following sub-sections, the observation of all the Galactic sources with LHAASO will be discussed in details.