English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Aims. We report the first detailed X-ray study of the supernova remnant (SNR)G304.6+0.1, achieved with the XMM-Newton mission. Methods. The powerful imagingcapability of XMM-Newton was used to study the X-ray characteristics of theremnant at different energy ranges. The X-ray morphology and spectralproperties were analyzed. In addittion, radio and mid-infrared data obtainedwith the Molonglo Observatory Synthesis Telescope and the Spitzer SpaceTelescope were used to study the association with the detected X-ray emissionand to understand the structure of the SNR at differents wavelengths. Results.The SNR shows an extended and arc-like internal structure in the X-ray bandwith out a compact point-like source inside the remnant. We find a high columndensity of NH in the range 2.5-3.5x1022 cm-2, which supports a relativelydistant location (d $\geq$ 9.7 kpc). The X-ray spectrum exhibits at least threeemission lines, indicating that the X-ray emission has a thin thermal plasmaorigin, although a non-thermal contribution cannot be discarded. The spectra ofthree different regions (north, center and south) are well represented by acombination of a non-equilibrium ionization (PSHOCK) and a power-law (PL)model. The mid-infrared observations show a bright filamentary structure alongthe north-south direction coincident with the NW radio shell. This suggeststhat Kes 17 is propagating in a non-uniform environment with high density andthat the shock front is interacting with several adjacent massive molecularclouds. The good correspondence of radio and mid-infrared emissions suggeststhat the filamentary features are caused by shock compression. The X-raycharacteristics and well-known radio parameters indicate that G304.6+0.1 is amiddle-aged SNR (2.8-6.4)x104 yr old and a new member of the recently proposedgroup of mixed-morphology SNRs.

XMM-Newton detection of the supernova remnant G304.6+0.1 (Kes 17)