|Title||3C 234: a Compton-thick radio-loud Type 2 quasar in the backyard?|
|Author||Dr Enrico Piconcelli|
|Description||We propose a 30 ks XMM-Newton observation of the hidden radio-loud quasar 3C 234 (z = 0.1848). The F(2-10)-F(O[III]) ratio and a low signal-to-noise ASCA spectrum strongly suggest the possibility that the nuclear absorber is Compton-thick. The detection of a Fe Kalpha line with EW larger than 1 keV in the XMM-Newton spectrum would definitely confirm this suggestions. If so, 3C 234 would turn out to be the first Compton-thick radio-loud Type 2 QSO observed and, with an intrinsic 2-10 keV luminosity of 3 x 10e46 erg-s, one of the very most powerful object ever detected at z less than 0.2. The discovery of an AGN with such peculiar properties is strongly needed in the framework of Unified Models and, thereby, in the synthesis models of the X-ray cosmic background.|
|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, 2008-08-29T00:00:00Z, 040534, 17.56_20190403_1200. https://doi.org/10.5270/esa-dxipftw|