XMM-NEWTONANDCHANDRAOBSERVATIONS OF THE EJECTA-DOMINATED MIXED-MORPHOLOGY GALACTIC SUPERNOVA REMNANT G352.7–0.1

Abstract

We present a spatial and spectral X-ray analysis of the Galactic supernova remnant (SNR) G352.7−0.1 using archival data from observations made with the XMM-Newton X-ray Observatory and the Chandra X-ray Observatory. Prior X-ray observations of this SNR had revealed a thermal center-filled morphology that contrasts with a shell-like radio morphology, thus establishing G352.7−0.1 as a member of the class of Galactic SNRs known as mixedmorphology SNRs (MMSNRs). Our study confirms that the X-ray emission comes from the SNR interior and must be ejecta dominated. Spectra obtained with XMM-Newton may be fit satisfactorily with a single thermal component (namely a non-equilibrium ionization component with enhanced abundances of silicon and sulfur). In contrast, spectra extracted by Chandra from certain regions of the SNR cannot always be fit by a single thermal component. For those regions, a second thermal component with solar abundances or two thermal components with different temperatures and thawed silicon and sulfur abundances (respectively) can generate a statistically acceptable fit. We argue that the former scenario is more physically plausible: on the basis of parameters of our spectral fits, we calculate physical parameters including X-ray emitting mass (∼45 M for solar abundances). We find no evidence for overionization in the X-ray emitting plasma associated with the SNR: this phenomenon has been seen in other MMSNRs. We have conducted a search for a neutron star within the SNR by using a hard (2-10 keV) Chandra image but could not identify a firm candidate. We also present (for the first time) the detection of infrared emission from this SNR as detected at 24 μm by the MIPS on board Spitzer. Finally, we discuss the properties of G352.7−0.1 in the context of other ejecta-dominated MMSNRs.

Fe-RICH EJECTA IN THE SUPERNOVA REMNANT G352.7–0.1 WITHSUZAKU

“…However, XMM-Newton image of the SNR showed that the X-ray emission completely fills the interior of the radio remnant; therefore, Giacani et al (2009) concluded that this remnant belonged to the MM class. Pannuti et al (2014) confirmed that this SNR is MM by using XMM-Newton and Chandra data. MM SNRs (Rho & Petre 1998), also known as thermal composites, are identified with shell emission in the radio band and centrally brightened thermal emission in the X-ray band with little or no limb brightening.…”

“…Recently, Pannuti et al (2014) presented X-ray study of the remnant by using data from XMM-Newton and Chandra. Their XMM-Newton spectra gave the bestfit with a single thermal component (kT e ∼ 1.2 keV) in NEI condition with enhanced abundances of Si and S. On the other hand, their Chandra spectra has been best described with two thermal components (VNEI+VNEI) with temperatures of ∼2.14 keV for hard and ∼0.39 keV for soft component for the whole remnant, although the spectra of some regions can be fit with single VNEI model.…”

“…G352.7−0.1 is one of Fe-rich SNRs in our Galaxy. Although it has been previously argued to be a core-collapse (CC) SN origin by Giacani et al (2009) and Pannuti et al (2014), its progenitor has not been well identified yet. Since Suzaku (Mitsuda et al 2007) has better sensitivity to Fe K-shell lines than other satellites (Yamaguchi et al 2014), our main aim is to identify the origin of G352.7−0.1 by determining Fe abundance based on a deep observation (∼201.6 ks) with the X-ray Imaging Spectrometer (XIS; Koyama et al 2007) onboard Suzaku.…”

Fe K and ejecta emission in SNR G15.9+0.2 withXMM-Newton

“…Symmetrically, it can not excluded that some CC SNRs are found at the low ionisation end. Part of SNR G15.9+0.2, for instance, still has emission at 6.4 keV, while SNR G352.7−0.1 has an Fe K centroid at 6.44 keV and is also of uncertain type; some studies suggest that it is the remnant a CC SNR (Giacani et al 2009;Pannuti et al 2014). Another caveat is that the current sample of Fe K emitting objects inherently contains some age bias, the youngest objects being preeminently of type Ia.…”

The Metal-Enriched Thermal Composite Supernova Remnant Kesteven 41 (G337.8-0.1) in a Molecular Environment

“…In Kes 41, the dust destruction scenario may not be favorable because argon, obviously enriched, is an inert element and cannot be easily depleted into dust. In the most recent X-ray studies of G352.7−0.1 and W51C, metal enrichment is explained to come from supernova ejecta (Pannuti et al 2014a;Sasaki et al 2014).…”