|Title||ARK 564: A ''VERY HIGH STATE|
|Author||Dr IOSSIF PAPADAKIS|
|Description||Recent RXTE and XMM observations have revealed ..characteristic time scales" in the power spectra of AGN. The AGN PSDs appear to be similar to the power spectra of Galactic X-ray binaries, except from Ark 564. There are two ..break frequencies" in the power spectrum of this source, but none of them appears to scale linearly with central black hole mass when compared with the appropriate break frequencies found in the PSDs of Galactic sources at "low-hard" or ..high-soft" state. Here we propose a long (95 ksec) XMM observation of Ark 564 in order to detrmine accurately its high frequency PSD and investigate whether this source is "unique" among AGN with known PSDs, or its variability properties are similar to the properties of Galactic X-ray sources at the "very high state".|
|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, 2006-02-23T00:00:00Z, 020640, 17.56_20190403_1200. https://doi.org/10.5270/esa-befty95|