|Title||CONSTRAINING THE POPULATION OF HIGH-SPIN ERMASSIVE BLACK HOLES IN THE EARLY U|
|Author||Dr HONGJUN AN|
|Description||There are four massive quasars discovered at z>5. These sources present a puzzle; how black holes grow to 10^9 solar masses in the limited age of the universe. We would like to address this by estimating the population of such objects. The population estimation requires good constraints on their jet properties, in particular, the Doppler factor. We propose to observe the high-redshift blazar SDSSJ013127.34-032100.1 with XMM and NuSTAR for 40 ks and 100 ks, respectively, in order to model the broadband SED accurately. The broadband X-ray observation will allow us to measure the Doppler factor for the source, constraining the high-a supermassive BH population in the early universe. These measurements will be used to infer the number of similar BHs at high redshifts.|
|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, 2021-01-27T23:00:00Z, 085219, 18.00_20191217_1110. https://doi.org/10.5270/esa-[xxxxxxx]|