|Title||SEARCHING FOR RELATIVISTIC DISC REFLECTION IN THE HIGH MASS AGN PG1426+015|
|Author||Dr Dominic Walton|
|Description||Spin measurements for high-mass active galactic nuclei are currently very sparse, but are critical for testing correlations between mass and spin hinted at in the current sample of AGN with spin constraints, and testing theoretical models of supermassive black hole growth. We request a coordinated broadband X-ray observation of PG1426+015, which has the largest reverberation-mapped mass to date (log[Mbh-Msun] = 9.01 (+0.11,-0.16)), with XMM-Newton (100ks) and NuSTAR (100ks). The quality of the data will enable us to robustly search for relativistically broadened iron emission, an unambigous signature of reflection from the innermost accretion disc, and take an important first step towards constrining the spin for this key source.|
|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, 2021-02-17T23:00:00Z, 085221, 18.02_20200221_1200. https://doi.org/10.57780/esa-hoxibnm|