6533b7d5fe1ef96bd12651d0

RESEARCH PRODUCT

XMM-Newton Large Program on SN1006 - I: Methods and Initial Results of Spatially-Resolved Spectroscopy

Jacco VinkAnne DecourchelleFabrizio BocchinoJiang-tao LiMarco MiceliMarco Miceli

subject

High Energy Astrophysical Phenomena (astro-ph.HE)PhysicsElectron densityAstrophysics::High Energy Astrophysical Phenomenadata analysis cosmic rays ISM: supernova remnants X-rays: ISM [acceleration of particles shock waves methods]FOS: Physical sciencesAstronomy and AstrophysicsAstrophysicsAstrophysics::Cosmology and Extragalactic Astrophysicsacceleration of particles shock waves methods: data analysis cosmic rays ISM: supernova remnants X-rays: ISMSpectral lineInterstellar mediumSupernovaSpace and Planetary ScienceIonizationAstrophysics::Solar and Stellar AstrophysicsSpectroscopySupernova remnantAstrophysics - High Energy Astrophysical PhenomenaAstrophysics - Instrumentation and Methods for AstrophysicsInstrumentation and Methods for Astrophysics (astro-ph.IM)Equivalent widthAstrophysics::Galaxy Astrophysics

description

Based on our newly developed methods and the XMM-Newton large program of SN1006, we extract and analyze the spectra from 3596 tessellated regions of this SNR each with 0.3-8 keV counts $>10^4$. For the first time, we map out multiple physical parameters, such as the temperature ($kT$), electron density ($n_e$), ionization parameter ($n_et$), ionization age ($t_{ion}$), metal abundances, as well as the radio-to-X-ray slope ($\alpha$) and cutoff frequency ($\nu_{cutoff}$) of the synchrotron emission. We construct probability distribution functions of $kT$ and $n_et$, 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 regions. We then compare the EW maps of OVII, OVIII, OVII K$\delta-\zeta$, Ne, Mg, SiXIII, SiXIV, 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 center. This "O Hole" has enhanced OVII K$\delta-\zeta$ and Fe emissions, indicating recently reverse shocked ejecta, but also has the highest $n_et$, indicating forward shocked ISM. Therefore, a multi-temperature model is needed to decompose these components. The asymmetric metal distributions suggest there is either an asymmetric explosion of the SN or an asymmetric distribution of the ISM.

10.1093/mnras/stv1882http://arxiv.org/abs/1508.02950