|Title||Broadband X-ray Spectroscopy of the Unique ULX P13 in NGC7793|
|Author||Dr Dominic Walton|
|Description||We request an XMM (50 ks) + NuSTAR (100 ks) ToO observation of the ULX P13 in NGC7793 during its ultraluminous regime (Lx > 2e39 erg-s). The dynamical mass constraint available for this source requires it to be super-Eddington at these luminosities, making it a key laboratory for understanding this exotic mode of accretion. These observations will provide the first hard X-ray detection of this source, and provide a vital point of comparison with a known super-Eddington accretor for the rest of the ULX population with broadband X-ray observations, which is currently missing. P13 is currently the only source that can provide this link. Our ToO will be triggered by the 12x1 ks Swift monitoring additionally requested as part of this proposal.|
|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, 2017-06-13T22:00:00Z, 078180, 17.56_20190403_1200. https://doi.org/10.5270/esa-6uyp7jo|