|Title||The Explosion Geometries of Short GRBs: Implications for Energetics and Rates|
|Author||Ms Wen-fai Fong|
|Description||The jet angle distribution for short GRBs is sparsely determined yet essential to constrain due to its direct implications for the true energy scale and event rate. Our current knowledge of the distribution comes from late-time X-ray observations (>1 day after the burst). Here, we propose XMM-Newton TOO observations to monitor a short GRB afterglow and constrain its collimation from the detection or non-detection of a jet break, to constrain >10-20 deg. A precise calculation of the angle additionally requires broad-band afterglow observations to constrain the GRB energy and circumburst density. With our ongoing broad-band short GRB TOO programs, our group is uniquly poised to provide the tightest constraints on these angles.|
|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, 2014-08-31T00:00:00Z, 072257, 17.56_20190403_1200. https://doi.org/10.5270/esa-g0ls2m9|