|Title||The Nature of the X-ray Emission in Sa Bulges|
|Author||Dr Jimmy Irwin|
|Description||The X-ray emission from the bulges of Sa galaxies consists of a hard 5-10 keV component, generally attributed to low mass X-ray binaries (LMXBs) and a soft 0.3 keV component of unknown origin. It is possible that the soft emission is from a warm ISM. However, we suggest that the soft emission also results from LMXBs. XMM will be able to resolve the soft emission into point sources, and determine the spectral properties of the brighter LMXBs. If Sa bulges are lacking an ISM, this implies that galactic winds have driven the gas lost from stars out of the galaxy. We propose an XMM observation of the bright, nearby Sa galaxy NGC3623. Since the L_X-L_B value of NGC3623 is a factor of 1.5 less than the Sa galaxy NGC1291, this would also imply there is not a universal stellar .|
|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, 2003-06-30T00:00:00Z, 008214, 17.56_20190403_1200. https://doi.org/10.5270/esa-9477pkb|