|Title||The X-ray source populations of different stellar generations in the LMC|
|Author||Dr Vallia Antoniou|
|Description||We propose XMM-Newton observations of 8 regions of the LMC with the strongest "clean" star-formation episodes in the virgul6-50 Myr age range. These observations will probe the X-ray source populations in regions of different stellar content, down to a luminosity of virgul10^33 erg-s in our nearest star-forming galaxy. From their optical counterparts we will classify the X-ray sources as supergiants or Be-X-ray binaries (SG- or Be-XRBs), while based on X-ray spectra and timing analysis we will identify X-ray binary pulsars. These results will address the connection between stellar and different XRB sub-populations. The proposed observations will complement previous X-ray studies of the LMC as well as investigations in other galaxies where these faint XRB populations cannot be observed.|
|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, 2013-02-18T00:00:00Z, 067109, 17.56_20190403_1200. https://doi.org/10.5270/esa-62hc8np|