The interaction of a supernova (SN) with circumstellar gas gives radiationpredominantly in the X-ray range. We propose to make spectral and imagingobservations of a small number of young SNe. By comparing the spectra withmodels for the shock emission, developed by the group, the temperature of theemitting gas, and hence the shock velocity, can be determined. From the lowenergy cutoff it can be decided whether the shock is radiative or adiabatic.The abundances in the shocked gas reflect whether the reverse shock is in thehydrogen, helium or oxygen rich regions of the SN ejecta. The requestedobservations, together with our optical, radio and UV data, are henceindispensable to get a detailed picture of both the SN ejecta, shock wave,and
Instrument
EMOS1, EMOS2, EPN, OM, RGS1, RGS2
Temporal Coverage
2001-06-17T04:47:34Z/2001-06-17T15:02:39Z
Version
17.56_20190403_1200
Mission Description
The European Space Agencys (ESA) X-ray Multi-Mirror Mission (XMM-Newton) was launched by an Ariane 504 on December 10th 1999. XMM-Newton is ESAs 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 Earths 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.
European Space Agency, Mr Stefan Immler, 2002, 'XMM Observations of X-Ray Emission from Supernovae', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-vbyy1um
