|Title||The connection of X-ray tails and HI tails of late-type cluster galaxies|
|Author||Dr Ming Sun|
|Description||X-ray tails of late-type cluster galaxies were only detected recently with Chandra and XMM. Detailed studies of these systems allow us to better understand ram-pressure stripping, galaxy transformation in clusters, mixing of the stripped cold ISM with the hot ICM, r^ant micro-physics and intracluster SF. However, X-ray tails are rare in blind searches, often submerged in strong cluster background. We propose a targeted search for X-ray tails for six late-type galaxies with known HI tails in the Virgo cluster. The combination of Virgo.s proximity, the low cluster background around these galaxies and XMM.s power in the soft X-ray band will put strong constraints on the properties of X-ray tails even if none are detected, which will also be compared with our simulations.|
|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, 2011-07-03T00:00:00Z, 065179, 17.56_20190403_1200. https://doi.org/10.5270/esa-9224b70|