Existing observations indicate most of the X-ray emission from hot CGM or the galactic corona can be attributed to stellar feedback, while the accretion induced hot halo gas, as predicted by galaxy formation models, is not detected. We propose an XMM-Newton survey of the M31 halo, in order to search for the accreted hot halo. We will study the spatial distribution of hot gas density, temperature, and metallicity. We will estimate the strength of collisional ionization to better model the UV absorption lines from the HST observed background AGN. These analyses will help us to explore if the accreted CGM is previously not detected because they have low density and distribute at large radii, or they have too low temperature to emit X-ray, or they have too low metallicity so X-ray emissivity.
Publication
No observations found associated with the current proposal
Instrument
EPN, RGS1, OM, RGS2, EMOS1, EMOS2
Temporal Coverage
2017-06-28T03:21:11Z/2018-01-19T13:05:16Z
Version
17.56_20190403_1200
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.
