ChandraObservations of Galactic Supernova Remnant Vela Jr.: A New Sample of Thin Filaments Emitting Synchrotron X‐Rays

Abstract

The Galactic supernova remnant (SNR) Vela Jr. (RX J0852.0À4622, G266.6-1.2) shows sharp filamentary structures on its northwestern edge in the hard X-ray band. The filaments are very smooth and located on the extreme outside edge of the remnant. We measured the averaged scale width of the filaments (w u and w d ) with excellent spatial resolution with Chandra, and they are on the order of the size of the point-spread function of Chandra on the upstream side and 49B5 (36B0-88B8) on the downstream side. The spectra of the filaments are very hard and have no linelike structure; they were well reproduced with an absorbed power-law model with À ¼ 2:67 (2.55-2.77) or a SRCUT model with roll ¼ 4:3 (3:4 5:3) ; 10 16 Hz under the assumption of p ¼ 0:3. These results imply that the hard X-rays are synchrotron radiation emitted by accelerated electrons, as mentioned previously. Using a correlation between the function B roll /w 2 d and the SNR age, we estimated the distance and the age of Vela Jr.: the estimated distance and age are 0.33 (0.26-0.50) kpc and 660 (420-1400) yr, respectively. These results are consistent with previous reports, implying that the B-age relation may be a useful tool for estimating the distance and the age of synchrotron X-ray-emitting SNRs. Subject headingg s: acceleration of particles -ISM: individual (G266.6-1.2, RX J0852.0À4622) -supernova remnants -X-rays: ISM

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

“…This can lead to strong modifications of the shock structure and a nonlinear coupling between the shock flow and CR acceleration. Some observational results are consistent with the predictions of such nonlinear DSA (NLDSA) models (Bamba et al 2003(Bamba et al , 2005a2005b, Vink & Laming 2003Warren et al 2005;Uchiyama et al 2007;Helder et al 2009). However, whether these models can fully explain all aspects revealed by the accumulating multiwavelength observations still remains in doubt.…”

The structure of TeV-bright shell-type supernova remnants

“…The X-ray and gamma-ray images of this remnant are consistent with a very thin shell of 1 • in radius and ∼0.2 • in thickness. The radius of SNR RX J0852.0-4622 is 5−10 pc (Aharonian et al 2005 for a distance of 0.26−0.50 kpc, and its age is about 420−1400 yrs (Bamba et al 2005). The young shell-type SNR RCW 86 (also known as G315.4-2.3 and MSH 14-63) has been observed in radio (Kesteven & Caswell 1987), optical (Smith 1997), X-ray (Pisarskietal et al 1984, and gamma-ray Aharonian et al 2009) with a nearly circular shape of 40 in diameter.…”

Probing the effects of hadronic acceleration at the SN 1006 shock front

“…X-ray synchrotron emission from high energy electrons accelerated at the shock front up to TeV energies has been first observed in SN 1006 (Koyama et al 1995) and then in other young SNRs as, for example, G1.9+0.3 (Reynolds et al 2009), Vela Jr. (Slane et al 2001, Bamba et al 2005, and G353.6-0.7 (Tian et al 2010). Recently, TeV emission has been detected in SN 1006 (Acero et al 2010).…”