Nonthermal x-rays from supernova remnant g330.2+1.0 and the characteristics of its central compact object

Sangwook Park, Oleg Kargaltsev, George G. Pavlov, Koji Mori, Patrick O. Slane, John P. Hughes, David N. Burrows, Gordon P. Garmire

Research output: Contribution to journalArticle

21 Scopus citations

Abstract

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, we find that the X-ray spectrum of J1601 can be described by neutron star atmosphere models (T ∞ ∼ 2.5-5.5MK). Assuming the distance of d ∼ 5 kpc for J1601 as estimated for SNR G330.2+1.0, a small emission region of R ∼ 0.4-2 km is implied. X-ray pulsations previously suggested by Chandra are not confirmed by the XMM-Newton data, and are likely not real. 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 less than 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 (Γ ∼ 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 ?rolloff ∼ 2-3 × 1017 Hz. For the measured widths of the X-ray filaments (D ∼ 0.3 pc) and the estimated shock velocity (vs ∼ a few × 103 km s-1), a downstream magnetic field B ∼ 10-50 μ G is derived. The estimated maximum electron energy Emax ∼ 27-38 TeV suggests that G330.2+1.0 is a candidate TeV γ -ray 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 γ -ray emission. Follow-up deep radio, X-ray, and γ -ray observations will be essential to reveal the details of the shock parameters and the nature of particle accelerations in this SNR.

Original languageEnglish (US)
Pages (from-to)431-441
Number of pages11
JournalAstrophysical Journal
Volume695
Issue number1
DOIs
StatePublished - Apr 10 2009

    Fingerprint

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this