|Title||The Origin of the Fe-rich Knot in SN 1604|
|Author||Dr Toshiki Sato|
|Description||We propose a 200 ks XMM-Newton observation of the "Fe-rich" knot in the Type Ia supernova remnant of Kepler to confirm that the explosion originated from a near-Chandrasekhar-mass white dwarf (WD). Previous observations by Chandra have revealed an Fe-rich ejecta knot within the SNR moving at nearly the free expansion speed. The current spectrum of the knot shows strong emission lines from Fe-peak elements (Cr, Mn, Ni), pointing to an origin in the deepest layer of a near-Chandrasekhar-mass WD. However, due to high background in the Chandra data, it is difficult to claim a significant detection of the Ni line, which is key to determining the burning regime. Thanks to low background, high sensitivity in the Ni band, only the XMM-Newton can resolve this important issue in SN Ia physics.|
|Publication||No observations found associated with the current proposal|
|Instrument||EMOS1, EMOS2, EPN, OM, RGS1, RGS2|
|Mission Description||The European Space Agency's (ESA) X-ray Multi-Mirror Mission (XMM-Newton) was launched by an Ariane 504 on December 10th 1999. XMM-Newton is ESA's second cornerstone of the Horizon 2000 Science Programme. It carries 3 high throughput X-ray telescopes with an unprecedented effective area, and an optical monitor, the first flown on a X-ray observatory. The large collecting area and ability to make long uninterrupted exposures provide highly sensitive observations.
Since Earth's atmosphere blocks out all X-rays, only a telescope in space can detect and study celestial X-ray sources. The XMM-Newton mission is helping scientists to solve a number of cosmic mysteries, ranging from the enigmatic black holes to the origins of the Universe itself. Observing time on XMM-Newton is being made available to the scientific community, applying for observational periods on a competitive basis.
|Publisher And Registrant||European Space Agency|
|Credit Guidelines||European Space Agency, 2021-04-02T00:00:00Z, 084255, 18.02_20200221_1200. https://doi.org/esa-[xxxxxxx]|