|Title||Post-Merger Galaxies and the Generation of Hot Halos in Ellipticals|
|Author||Dr Trevor Ponman|
|Description||Previous studies of merging spiral galaxies reveal that the hot ISM is expelled from the system at the point of nuclear merger. After 1 Gyr the merger remnant appears to have little or no hot gas halo. Yet normal, old ellipticals clearly have extensive hot halos. This proposal aims to solve this mystery. In parti- cular, do merger remnants become more X-ray luminous over time or do mergers create a low Lx elliptical. There is very little X-ray data for post merger rem- nants with ages of 1-3 Gyrs. This timescale appears to be the crucial .turning point. in their X-ray properties. We propose to image such a sample with the PN. This will provide a key consistency check of the merger hypothesis and will con- strain the different possible mechanisms for hot halo regeneration.|
|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, 2003-05-24T00:00:00Z, 004934, 17.56_20190403_1200. https://doi.org/10.5270/esa-khii2lt|