|Title||Constraining the nature of the companion star of the IMBH HLX-1|
|Author||Dr olivier godet|
|Description||We found in 2009 a strong virgul10^4 Msun IMBH candidate, the hyper luminous X-ray source HLX-1 in the outskirts of the ESO 243-49 galaxy. We proposed that the IMBH is fed by mass transfer episodes when a WD donor passes at periapsis and is tidally stripped, leading to X-ray outbursts. We detected in previous XMM observations of HLX-1 faint unresolved X-ray lines at 0.64, 0.88 & 0.98keV. We propose that they may be due to photo-ionization of nearby material by the central source. We request a 130ks XMM ToO to detect with a high significance soft X-ray lines when the source will be near its emission peak. Modeling of the RGS data with photo-ionization codes will help us put constraints on the physical and dynamical properties of the emitting material around the BH.|
|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, 2018-06-13T22:00:00Z, 080131, 17.56_20190403_1200. https://doi.org/10.5270/esa-b4qrm95|