|Title||Discovery of a QPO in the NGC55 ULX?|
|Author||Dr GULAB DEWANGAN|
|Description||We request a long (125ks) XMM-Newton observation of the ULX in the nearby galaxy NGC55. Previous short observations have revealed several unique aspects of this ULX. The temporal behavior of the ULX suggests a QPO at 1.5mHz and a power spectrum break. Such temporal features have been observed only for three other ULXs. Moreover, the source undergoes frequent spectral transitions making it a unique ULX where characteristic temporal behavior can be studied in conjunction with spectral transitions. Such studies are crucial to understanding the differences-similarities between ULX and Galactic X-ray binaries. Furthermore, the ULX exhibits a series of strange and unexplained X-ray dips of duration virgul200s, whose nature can be revealed in spectral analysis of co-added dip data.|
|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, 2011-06-16T00:00:00Z, 065505, 17.56_20190403_1200. https://doi.org/10.5270/esa-czkxp53|