XMM-Newton observation of the TeV-discovered supernova remnant HESS J1534-571

• Published in: Astronomy and astrophysics (Berlin) Vol. 679; p. A48
• Main Authors: Nguyen-Dang, N. T., Pühlhofer, G., Sasaki, M., Bamba, A., Doroshenko, V., Santangelo, A.
• Format: Journal Article
• Language: English
• Published: Heidelberg EDP Sciences 01.11.2023
• Subjects: Cosmic rays; Energy bands; Gamma emission; Supernova remnants; Synchrotrons; XMM (spacecraft)
• ISSN: 0004-6361; 1432-0746
• DOI: 10.1051/0004-6361/202346448

We report the results obtained from XMM-Newton observations of the TeV-detected supernova remnant (SNR) HESS J1534-571. We focus on the nature of the cosmic-ray particle content in the SNR, which is revealed by its γ -ray emission. No signatures of X-ray synchrotron emission were detected from the SNR. This is consistent with earlier results obtained with Suzaku from other regions of the object. A joint modeling of the XMM-Newton and Suzaku spectra yields an upper limit for the total X-ray flux from the SNR area of ~5.62 × 10 −13 erg cm −2 s −1 (95% C.I.) in the energy band of 2.0–10.0 keV for an assumed photon index of 2.0. On the other hand, we do find evidence in the XMM-Newton data for a line-like emission feature at 6.4 keV from localized regions, again confirming earlier Suzaku measurements. We discuss the findings in the context of the origin of the observed γ -ray emission. Although neither hadronic nor leptonic scenarios can be fully ruled out, the observed line emission can be interpreted as the result of interactions between lower-energy (~ MeV) cosmic-ray protons with high gas-density regions in and around HESS J1534-571, and thus potentially be associated with particles accelerated in the SNR.