Volume 546, October 2012
|Number of page(s)||4|
|Section||Interstellar and circumstellar matter|
|Published online||11 October 2012|
Observations of the post-shock break-out emission of SN 2011dh with XMM-Newton⋆
Institut für Astronomie und Astrophysik, Universität Tübingen,
Received: 10 August 2012
Accepted: 16 September 2012
Context. After the occurrence of the type cIIb SN 2011dh in the nearby spiral galaxy M 51 numerous observations were performed with different telescopes in various bands ranging from radio to γ-rays.
Aims. We analysed the XMM-Newton and Swift observations taken 3 to 30 days after the SN explosion to study the X-ray spectrum of SN 2011dh.
Methods. We extracted spectra from the XMM-Newton observations, which took place ~7 and 11 days after the SN. In addition, we created integrated Swift/XRT spectra of 3 to 10 days and 11 to 30 days.
Results. The spectra can be well-fitted with a power-law spectrum absorbed with Galactic foreground absorption. In addition, we find a harder spectral component in the first XMM-Newton spectrum taken at t ≈ 7 d. This component is also detected in the first Swift spectrum of t = 3–10 d.
Conclusions. While the persistent component can be explained as inverse Compton emission from radio synchrotron emitting electrons or emission of the reverse shock, the harder component is most likely bremsstrahlung emission from the shocked stellar wind. Therefore, the harder X-ray emission that fades away after t ≈ 10 d can be interpreted as emission from the shocked circumstellar wind of SN 2011dh.
Key words: shock waves / circumstellar matter / supernovae: individual: SN2011dh
© ESO, 2012
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