|Title||EMISSION FROM THE MISSING BARYONS IN THE LOCAL GROUP|
|Author||Dr JOEL BREGMAN|
|Description||The detection of X-ray absorption and emission lines at z = 0 has been interpreted as an extensive isothermal Local Group medium with a gaseous mass exceeding the baryonic mass of all Local Group galaxies. A large gaseous mass helps to solve the missing baryon problem , a leading cosmological issue. However, the gas mass is highly model dependent, and in an alternative model, the gas lies in a Galactic halo of size 50 kpc and with a gas mass orders of magnitude lower. We can discriminate between the Galactic Halo and Local Group models by determining whether most of the diffuse X-ray emission (0.5-1 keV) lies in front or behind a Magellanic Stream cloud at a distance of 50 kpc. For the Local Group model, the MS cloud will absorb the emission beyond it, casting an X-ray shadow .|
|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, 2005-01-30T00:00:00Z, 020467, 17.56_20190403_1200. https://doi.org/10.5270/esa-p1h43r9|