XMM-Newton large program on SN1006 - I. Methods and initial results of spatially resolved spectroscopy
Date Issued
2015
Author(s)
Description
The authors would like to acknowledge Dyer Kristy and Reynolds Stephen for providing their radio images of SN1006 and for helpful discussions. We also acknowledge Ballet Jean and Acero Fabio for helpful discussions and the anonymous referee for helpful comments and suggestions. LJ-T acknowledges the financial support from CNES and the travel support from NSFC through the grant 11233001.
Abstract
Based on our newly developed methods and the XMM-Newton large program of SN1006, we extract and analyse the spectra from 3596 tessellated regions of this supernova remnant (SNR) each with 0.3-8 keV counts >104. For the first time, we map out multiple physical parameters, such as the temperature (kT), electron density (ne), ionization parameter (net), ionization age (tion), metal abundances, as well as the radio-to-X-ray slope (α) and cutoff frequency (νcutoff) of the synchrotron emission. We construct probability distribution functions of kT and net, and model them with several Gaussians, in order to characterize the average thermal and ionization states of such an extended source. We construct equivalent width (EW) maps based on continuum interpolation with the spectral model of each region. We then compare the EW maps of O VII, O VIII, O VII Kδ - ζ, Ne, Mg, Si XIII, Si XIV, and S lines constructed with this method to those constructed with linear interpolation. We further extract spectra from larger regions to confirm the features revealed by parameter and EW maps, which are often not directly detectable on X-ray intensity images. For example, O abundance is consistent with solar across the SNR, except for a low-abundance hole in the centre. This `O hole' has enhanced O VII Kδ - ζ and Fe emissions, indicating recently reverse shocked ejecta, but also has the highest net, indicating forward shocked interstellar medium (ISM). Therefore, a multitemperature model is needed to decompose these components. The asymmetric metal distributions suggest there is either an asymmetric explosion of the supernova or an asymmetric distribution of the ISM.
Volume
453
Issue
4
Start page
3953
Issn Identifier
0035-8711
Ads BibCode
2015MNRAS.453.3953L
Rights
open.access
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