|Title||NGC 2264: a new dispersed population|
|Author||Dr Ettore Flaccomio|
|Description||An optical variability study of the "benchmark" star forming region NGC2264, observed with CoRoT, indicates that the cluster is more extended than currently believed. We propose to observe with EPIC two fields in the outskirts of NGC2264, each for 50ks. We want to: 1) confirm by means of X-ray detection the existence of a spatially extended population; 2) establish the star formation history of the region, e.g. whether the clustered and dispersed populations originated from the same or distinct formation events; 3) determine whether mass segregation affects NGC2264, thus compromising current determinations of the Initial Mass Function; 4) derive disk frequencies throughout the cluster and in sub-regions with different stellar densities and UV-radiation fields.|
|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, 2012-10-15T00:00:00Z, 067382, 17.56_20190403_1200. https://doi.org/10.5270/esa-1q626jt|