|Title||Observing the Highest Energy Emissions from Young Protostellar Jets|
|Author||Dr Eric Perlman|
|Description||A bipolar jet outflow, observed in optical-IR atomic and molecular emission lines, is a hallmark of the formation of a new star. Recently, XMM-Newton and Chandra have found X-ray emission from two protostellar jets, at least one of which originates in a class 0-1 protostar. This emission is believed to be produced within the leading edge of shocks, by interactions with the ambient medium. The X-ray emission is believed to excite the UV-optical-IR line emission. Our targets, HH211 and HH212, are class 0 systems. Class 0 protostars are believed to be at their most powerful stage, and are therefore also expected to have the most powerful X-ray emission. These observations are critical to understanding the evolution and physics of protostellar jets.|
|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, 2004-10-14T00:00:00Z, 014989, 17.56_20190403_1200. https://doi.org/10.5270/esa-xjgl9mx|