Nonthermal X-Rays from Supernova Remnant G330.2+1.0 and the Characteristics of its Central Compact Object

Details Nonthermal X-Rays from Supernova Remnant G330.2+1.0 and the Characteristics of its Central Compact Object Nonthermal X-Rays from Supernova Remnant G330.2+1.0 and the Characteristics of its Central Compact Object

Jan 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21335907p&link_type=abstract

American Astronomical Society, AAS Meeting #213, #359.07; Bulletin of the American Astronomical Society, Vol. 41, p.503

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We present results from our X-ray data analysis of the supernova remnant (SNR) G330.2+1.0 and its central compact object (CCO), CXOU J160103.1-513353 (J1601 hereafter). Using our XMM-Newton and Chandra observations, the X-ray spectrum of J1601 is described by neutron star (NS) atmosphere models, indicating a small hot region(s) (R 1-2 km, Th 2.5-3.7 MK) and the cool NS surface (R = 10 km, Ts < 1.5 MK). X-ray pulsations are not detected. However, our timing analysis of the XMM-Newton data is limited by poor photon statistics, and thus pulsations with a relatively low amplitude (i.e., an intrinsic pulsed-fraction < 40%) cannot be ruled out. Our results indicate that J1601 is a CCO similar to that in the Cassiopeia A SNR. X-ray emission from SNR G330.2+1.0 is dominated by power law continuum (photon index 2.1-2.5) which primarily originates from thin filaments along the boundary shell. This X-ray spectrum implies synchrotron radiation from shock-accelerated electrons with an exponential roll-off frequency 2-3 x 1017 Hz. For the measured widths of the X-ray filaments (D 0.3 pc) and the estimated shock velocity (vs a few x 103 km/s), a downstream magnetic field B 10-50 uG is derived. The estimated maximum electron energy Emax 27-38 TeV suggests that G330.2+1.0 is a candidate TeV source. We detect faint thermal X-ray emission in G330.2+1.0. We estimate a low preshock density n0 0.1 cm-3, which suggests a dominant contribution from an inverse Compton mechanism (than the proton-proton collision) to the prospective gamma-ray emission. Follow-up deep radio, X-ray, and gamma-ray observations will be essential to reveal the details of the shock parameters and the nature of particle accelerations in this SNR.

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