|Title||Accretion states of the transient ULX in M83|
|Author||Dr Kip Kuntz|
|Description||In Dec 2010, Chandra revealed a previously unknown ULX in M83 where there had been no detectable X-ray source before. It has varied in flux and hardness but has remained bright for nearly two years. Our analysis shows that it is a black hole (BH) accreting from a low-mass secondary. The spectral evolution of a transient ULX as it fades is a critical test of the nature of these intriguing objects. Our goal is to determine whether it goes through the same canonical accretion states defined for Galactic BHs. We propose two 50-ks observations, separated by a few months, to identify the accretion state(s), accurately determine the physical parameters, and compare with stellar-mass BH states. This will constrain the mass of this ULX and help clarify the relation between ULXs and stellar-mass BHs.|
|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, 2015-01-23T23:00:00Z, 072345, 17.56_20190403_1200. https://doi.org/10.5270/esa-ogd6o85|