|Title||Constraining the SED of potentially dust deficient AGN in nearby dwarf galaxies|
|Author||Prof Kevin Schawinski|
|Description||We have identified four Active Galactic Nuclei (AGN) in nearby dwarf galaxies (z<0.1, M <1E9.5M_sun) with an unexpected deficit of mid-IR (3.4-22 micron) emission. The extremely low mid-IR luminosity could be due to a dust deficit and absence of a torus. If confirmed this may lead to new insights into the AGN central engine structure in the regime of low black hole mass, AGN luminosity and-or Eddington ratio. The Chandra data available for one of the galaxies seem to confirm the deficit. We therefore propose to use XMM-Newton to obtain X-Ray data for the remaining three objects. This data will allow us to constrain the whole Spectral Energy Distribution (SED) of the hosted AGN and confirm the mid-IR deficit in a statistical sample.|
|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, 2016-03-23T23:00:00Z, 074062, 17.56_20190403_1200. https://doi.org/10.5270/esa-pej7h6p|