The effects of X-ray background on the X-ray emission from the Galactic supernova remnants

Nergis Cesur,Aytap Sezer,Murat Hüdaverdi̇

doi:10.3906/fiz-1802-19

Nergis Cesur, Aytap Sezer + Show 1 more

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https://doi.org/10.3906/fiz-1802-19

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Abstract

We present the results of an X-ray background emission study of the well-known Galactic supernova remnants (SNRs) Cas A, RCW 86, RX J1713.7-3946, and SN 1006 by using the archival Chandra and XMM-Newton X-ray Observatories data. With the advent of detector technologies and increased capability of the spectral resolutions, accurate background modelling for the extended sources, such as SNRs, is getting crucial at the modelling step since it might be effective on estimating the physical parameters of the plasma. For this purpose, we concentrate on the background emission spectral modelling by investigating its spectral parameters and components. Hence, the results of the modelled background spectra of these four SNRs are presented by using the combination of thermal and nonthermal emission models properly to the background components.

Highlights

Analysing the extended and faint sources, such as the Galactic supernova remnants (SNRs), with accurately modelled background emission is important since it might affect the spectral results (e.g., [1,2,3])
According to a previous study [5], the Galactic ridge X-ray emission (GRXE) spectrum requires the following components: the high-temperature plasma (HP; responsible for the 6.7 keV line), which probably originates from cataclysmic variables; the low-temperature plasma (LP; responsible for the 2.45 keV line), which may originate from multiple supernovae (SNe) within the past 10 5 yr or point sources like dM stars; the cold matter (CM; might be responsible for the 6.4 keV line), which possibly originates from the bombardment of X-rays or particles in cold interstellar gas; plus, the foreground emission (FE)
Despite the effect of the cosmic X-ray background (CXB) is valid for the background emission of all the SNRs as seen in the first lines of all the tables, its contribution differs for each SNR

Summary

Introduction

Analysing the extended and faint sources, such as the Galactic supernova remnants (SNRs), with accurately modelled background emission is important since it might affect the spectral results (e.g., [1,2,3]). In recent years, the importance of background modelling before performing detailed spectral analysis has been emphasised in plenty of studies (e.g., [3,4,5,6]) Under these circumstances, all spectral parameters can be examined reliably with the background modelling method, which is suitable for determining the thermal or nonthermal characteristics of SNRs. In this paper, we aimed to investigate the X-ray background emission of the well-known Galactic SNRs Cas A, RCW 86, RX J1713.7 −3946, and SN 1006 with various approaches according to their X-ray background conditions. While estimating the GRXE background, in some cases, the separating to the component method is not always adhered to according to some sources (e.g., [6,14,15])

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Conclusion