|Title||Intensive Spectroscopic Monitoring of the Seyfert-1 Galaxy NGC 3516|
|Author||Dr Richard Mushotzky|
|Description||GT-NGC 3516 is well matched to the spectroscopic capabilities of XMM. The underlying continuum varies by factor virgul2 on a timescale of virgulfew hrs, contains deep absorption features due to ionized material along the line of sight as well as an asymmetric Fe Kalpha line arising from the innermost regions of the accretion disk. The ionization structure of both the absorber (using the RGS) and the profile of the Fe line will be well-determined in virgul5ks. We propose to observe NGC 3516 continuously for 1 orbit, allowing us to track the response of the absorber and of the Fe line to variations in the continuum. We propose a 5ks snapshot exposure prior to the main observations to check that the source is not in an usually low intensity state.|
|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, 2002-12-21T00:00:00Z, 010746, 17.56_20190403_1200. https://doi.org/10.5270/esa-4i52l36|