|Title||A DEEP LOOK AT THE (RELATIVELY) X-RAY BRIGHT BALQSO FIRST 1556+3517|
|Author||Prof MICHAEL BROTHERTON|
|Description||We propose a 40 ks EPIC observation of the low-ionization broad absorption line (LoBAL) quasar FIRST 1556+3517. BAL quasars are X-ray faint and only since the advent of XMM and Chandra have they been routinely detected. Initial surveys reveal that the high-ionzation BAL (HiBAL) quasars are the X-ray brightest of the class and are apparently normal quasars with moderate to high line-of-sight absorbing column densities. LoBAL quasars are significantly fainter in the X-rays. The red, radio-loud BALQSO FIRST 1556+3517, a short-exposure target of both Chandra and XMM, is the X-ray brightest LoBAL quasar known at high redshifts and luminosities. The spectrum is too soft and faint to result from simple absorption, and is probably relfected as in Seyfert 2 galaxies.|
|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, 2006-08-05T00:00:00Z, 020405, 17.56_20190403_1200. https://doi.org/10.5270/esa-wytbpei|