This adds SNR G15.9+0.2 to the short list of seven SNRs hosting a confirmed CCO and as many hosting bona fide candidates ( Lazendic et al. (2016) to confirm that the central object is indeed a young cooling low-magnetized neutron star. Recently, deeper Chandra observations allowed Klochkov et al. Second, a compact source, identified as CXOU J181852.0−150213, was discovered in the central region of the SNR ( R06) with X-ray properties typical of central compact objects (CCOs, e.g.
This could add SNR G15.9+0.2 to the small sample (about 15) of SNRs confirmed to be ≲ 2000 yr old (using the compilation 1 of Ferrand & Safi-Harb 2012) and thus reduces the discrepancy between the observed and expected numbers of young SNRs. First, it is likely young, ~ 10 3 yr according to R06, as suggested by its small angular diameter and Chandra X-ray analysis. (2011), who measured a dust temperature and mass of 60 K and 8.1 × 10 -2 M ⊙, respectively.Īlthough 300 SNRs are now known in the Milky Way, SNR G15.9+0.2 is an interesting target for an in-depth analysis for several reasons. The SNR was detected in infrared with Spitzer/MIPS by Pinheiro Gonçalves et al. Its X-ray morphology favours a core-collapse (CC) origin according to Lopez et al. The source is relatively bright in X-rays, as found in Chandra data by Reynolds et al. Higher spatial resolution radio observations with VLA revealed the elongated shell-like structure of the SNR with a bright enhancement on the eastern border ( Dubner et al. SNR G15.9+0.2 was discovered as a supernova remnant (SNR) at radio wavelengths in Molonglo-Parkes observations by Clark et al. Key words: ISM: supernova remnants / X-rays: individuals: SNR G15.9+0.2 / X-rays: ISM Only a lower limit of 5 kpc is placed on the distance to SNR G15.9+0.2, constraining its age to t SNR ≳ 2 kyr. We also present some caveats regarding the use of Fe K line centroid energy as a typing tool for SNRs. We discuss how the source fits within the sample of SNRs with detected Fe K emission and find that it is the core-collapse SNR with the lowest Fe K centroid energy. We measure the line properties and find evidence for spatial variations. Using EPIC’s collective power, Fe K line emission from SNR G15.9+0.2 is detected for the first time. Abundance ratios of Mg, Si, S, Ar, and Ca strongly suggest that the progenitor of SNR G15.9+0.2 was a massive star with a main sequence mass likely in the range 20–25 M ⊙, strengthening the physical association with a candidate central compact object detected with Chandra. Prominent line features reveal the presence of ejecta. By comparing the SNR’s X-ray absorption column density with the atomic and molecular gas distribution along the line of sight, we attempt to constrain the distance to the SNR. EPIC data are used to investigate the morphological and spectral properties of the remnant, searching in particular for supernova ejecta and Fe K line emission. We present a study of the Galactic supernova remnant SNR G15.9+0.2 with archival XMM- Newton observations. 709, CEA-Saclay, 91191 Gif-sur-Yvette Cedex, FranceĪims. Laboratoire AIM, IRFU/Service d’Astrophysique – CEA/DRF – CNRS – Université Paris Diderot, Bât. Astronomical objects: linking to databases.Including author names using non-Roman alphabets.Suggested resources for more tips on language editing in the sciences Punctuation and style concerns regarding equations, figures, tables, and footnotes The cookie is set by the GDPR Cookie Consent plugin and is used to store whether or not user has consented to the use of cookies. The cookie is used to store the user consent for the cookies in the category "Performance". This cookie is set by GDPR Cookie Consent plugin. The cookie is used to store the user consent for the cookies in the category "Other. The cookies is used to store the user consent for the cookies in the category "Necessary". The cookie is set by GDPR cookie consent to record the user consent for the cookies in the category "Functional". The cookie is used to store the user consent for the cookies in the category "Analytics". These cookies ensure basic functionalities and security features of the website, anonymously. Necessary cookies are absolutely essential for the website to function properly.
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