Detection of Gamma Rays around 1 TeV from RX J0852.0-4622 by CANGAROO-II

Abstract

We have detected gamma-ray emission at the 6 σ level at energies greater than 500 GeV from the supernova remnant RX J0852.0−4622 (G266.2−1.2) using the

Neutrino signal from extended Galactic sources in IceCube

“…The distance to Vela Jr. has been estimated to be on the order of 200 pc (Aschenbach et al 1999), which is closer than the Cygnus region. The CANGAROO-II imaging atmospheric Cerenkov telescope detected the source at the 6σ level in 100 h (Katagiri et al 2005). This source has been also detected by the H.E.S.S.…”

“…It is one of the most luminous Galactic sources in the VHE energy band. The flux was reported to be of about 10% of Crab at 1 TeV by Katagiri et al (2005). It was discovered in 1998 using X-ray images performed by ROSAT (Aschenbach 1998).…”

Modeling supernova remnants: effects of diffusive cosmic-ray acceleration on the evolution and application to observations

“…(Aharonian et al 2005(Aharonian et al , 2006, CANGAROO-II (Katagiri et al 2005), MAGIC (Albert et al 2007), SHALON (Sinitsyna et al 2009), and VERITAS (Acciari et al 2009(Acciari et al , 2010. In addition, discoveries of non-thermal X-ray emission from SNRs (see a review by Reynolds 2008) imply that electrons are accelerated to TeV energies in supernova remnants (SNR).…”

Prospects for Cherenkov Telescope Array Observations of the Young Supernova Remnant RX J1713.7−3946

“…Another radio observation of CS also confirmed the existence of a very dense (>10 5 cm −3 ) ISM core toward the SNR (Maxted et al 2012). We are also aware that some of these characteristics are common among several other young SNRs, including RXJ0852.0−4622 (Aharonian et al 2005(Aharonian et al , 2007bKatagiri et al 2005), RCW86 ), and HESSJ1731−347 (Abramowski et al 2011). It is noteworthy that no thermal X-ray emission has been firmly detected in these SNRs (e.g., Koyama et al 1997;Tsunemi et al 2000;Bamba et al 2012).…”

“…So far, VHE gamma-ray observations have revealed the existence of high-energy particles at the shock of young SNRs (e.g., Enomoto et al 2002;Aharonian et al 2004Aharonian et al , 2005Aharonian et al , 2006Aharonian et al , 2007aAharonian et al , 2007bAharonian et al , 2009Katagiri et al 2005;Albert et al 2007;Acero et al 2010;Abramowski et al 2011;Acciari et al 2011;see also Ferrand & Safi-Harb 2012). Although the gamma rays are suggested to originate from either leptonic (low-energy photons upscattered by high-energy electrons) or hadronic (π 0 -decay photons generated by accelerated protons colliding with surrounding gas) processes, it is generally a nontrivial task to distinguish these processes despite abundant multiwavelength studies.…”