|Title||X-RAY EMISSION FROM LOW-MASS PROTOSTARS IN THE L1251 DARK CLOUD|
|Author||Dr THEODORE SIMON|
|Description||Until recently no Class 0 object had ever been detected as an X ray source. I am proposing a 35 ks observation of L1251, a small dark cloud which is a site of active star formation. L1251 harbors a number of high-velocity molecular outflows, long chains of HH emission knots, and low-luminosity IRAS sources. Two of the IRAS sources appear to be young (10^5 yr) Class 0 objects of about solar mass. A goal of this observation is to determine whether the X ray properties of these objects, including their surrounding environments, are different from those of embedded protostars that form in much more massive clouds. Because of its lower density and mass, the L1251 cloud may be more transparent to X rays and more easily probed than a dense cloud like Orion.|
|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, 2005-01-29T00:00:00Z, 020154, 17.56_20190403_1200. https://doi.org/10.5270/esa-ma73k5f|