Supernova Remnants and Molecular Clouds as Gamma-ray Sources
Tulun ErginCenter for Astrophysics, Harvard
detection of TeV and GeV gamma rays from galactic and extragalactic
sources is an important step forward in understanding the sites of
production and acceleration of cosmic rays (CRs) including what types
of CRs are produced and how they are accelerated to very high energies.
Gamma rays are not deflected by the interstellar and intergalactic
magnetic fields nor absorbed by the interstellar gas and dust.
Therefore, gamma rays can be detected, both at GeV energies by
space-borne instruments, such as NASA's Fermi Gamma-ray Space
Telescope, and at TeV energies by ground-based instruments, like the
imaging atmospheric Cherenkov telescopes (IACTs). In the Galaxy, a wide
range of gamma-ray sources, such as supernova remnants, pulsars and
pulsar wind nebulae, gamma-ray binaries, and star-forming regions are
candidate sites of production and acceleration of cosmic rays.
Additionally, the angular and spectral distribution of the diffuse
galactic gamma-ray emission caused by the CRs interacting with
molecular clouds can provide unique information about the character of
propagation of CRs in galactic magnetic fields. In this presentation, I
want to talk about the gamma-ray and radio detection of the supernova
remnants and molecular clouds, and finding their associated
counterparts in other wavelengths to better understand the nature of
the CR accelerators and their interactions with the surrounding
Wednesday, 31 March 2010, FENS L035, 13:40