|Title||Connection between the Accretion Disk and Relativistic Jet in the Blazar 3C 279|
|Author||Prof Alan Marscher|
|Description||We request a 126ks .stare. of 3C279 to combine with our 15yr RXTE light curve in order to measure the power spectral density (PSD) of the X-ray flux variations over timescales from virgul1E4 to 1E8 s. The data will determine whether the PSD has a break at virgul5E-7 Hz from a slope of -1 at low variational frequencies to virgul -2.4 at high frequencies. This is expected if, like the radio galaxies 3C111 and 3C120, the blazar follows the break timescale-mass-accretion rate scaling relationship found for non-beamed Seyfert galaxies and X-ray binaries. Since the X-rays observed in 3C279 arise from the highly relativistic jet, a positive result will demonstrate that even the fastest jets are driven from the accretion disk-corona rather than from the ergosphere of the black hole.|
|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, 2012-02-03T00:00:00Z, 065161, 17.56_20190403_1200. https://doi.org/10.5270/esa-fm68luo|