|Title||USING X-RAYS TO PROBE THE STELLAR POPULATION IN CHA II|
|Author||Dr BEATE STELZER|
|Description||We propose for XMM-Newton observations of two highly extincted fields in the ChaII star forming region. Our aim is to complete the census of cloud members using X-ray emission as a means to discover young stars. A clear assessment of the full stellar population is essential to establish the evolutionary state of a star forming cloud. ChaII seems to represent a comparatively young phase where many stars retain their disks. But a large number of low-mass members may still be hidden in the dark parts of the cloud. In contrast to earlier X-ray instrumentation XMM-Newton provides enough sensitivity and an extended spectral range allowing to penetrate the highly absorbed parts of ChaII, and study the stellar population across regions of high and varying extinction.|
|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, 2005-02-07T00:00:00Z, 020003, 17.56_20190403_1200. https://doi.org/10.5270/esa-h2bip26|