|Title||The First High-Resolution Grating Spectrum of a High-Redshift Quasar|
|Author||Prof Ehud Behar|
|Description||High-redshift (z) quasars are the farthest persistently bright X-ray point sources in the universe. Although the high column densities towards high-z quasars were observed in the early days of ROSAT, we still do not know whether this absorption is intrinsic to the quasar, or is due to intervening material, or whether the continuum is simply curved as to mimic absorption. So far, observations of such sources were limited to the moderate resolution of CCD spectra. We propose to obtain a high S-N 180 ks RGS spectrum of a highly absorbed - yet extremely bright - quasar RBS 315 (z = 2.69) in order to finally reveal the nature of its absorber: An outflow with absorption lines, the diffuse phase of the intergalactic medium, or just curved continuum.|
|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, 2014-02-13T00:00:00Z, 069090, 17.56_20190403_1200. https://doi.org/10.5270/esa-f4xpfwf|