|Title||High-redshift quasars: Cosmology and Physics|
|Author||Dr Elisabeta Lusso|
|Description||The non-linear X-ray-UV relation in quasars can be used to build a Hubble diagram and test cosmological models at high redshift. To this aim, we were awarded an XMM LP to observe 30 bright quasars at zvirgul3. We found a tighter-than- expected X-ray-UV relation, implying that pointed observations can greatly reduce the uncertainties in the determination of quasar distances, and a new population of X-ray weak quasars that represents virgul30% of the zvirgul3 sample. We propose an extensive survey of bright, radio-quiet, SDSS quasars at zvirgul4 with the goals of (1) detecting a 4sigma deviation from the LambdaCDM model using this zvirgul4 sample alone, (2) measuring the X-ray weak fraction of quasars for the first time at zvirgul4 and its evolution with time.|
|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, 2021-04-16T00:00:00Z, 084497, 18.02_20200221_1200. https://doi.org/esa-[xxxxxxx]|