|Title||X-ray Spectrometry of SN1987A|
|Author||Dr Frank Haberl|
|Description||From our last XMM-Newton observation of SN 1987A performed in Jan. 2008 (100 ks, AO6) we obtained EPIC and RGS spectra of unprecedented quality. The soft X-ray light curve shows a significant flattening after 2005, while at higher energies the light curve seems to steepen. To further monitor the turn-over we propose to continue our yearly XMM-Newton observations of SN 1987A. Together with our accepted AO7 observation this will allow us to study the time evolution of the shock conditions and abundance profiles of, e.g., N, O, Fe, Ne (with RGS). At high energies EPIC-pn can help to clarify the extremely low Fe abundance observed so far. Is the Fe completely swallowed by the central compact object or is the emission from the inner sections of the progenitor star still absorbed?|
|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, 2011-01-13T00:00:00Z, 060120, 17.56_20190403_1200. https://doi.org/10.5270/esa-43b8lol|