1 / 7

Who is ESO511-G030?

Who is ESO511-G030?. Nearby Seyfert 1 galaxy 97.5 Mpc away from XMM-Newton (z=0.0224) XMM-Newton observation of approximately 100 ks performed on 5 th August 2007 in the framework of the FERO project. Aladin RGB composite image. ESO511-G030 remarkable properties.

ziva
Download Presentation

Who is ESO511-G030?

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Who is ESO511-G030? Nearby Seyfert 1 galaxy 97.5 Mpc away from XMM-Newton (z=0.0224) XMM-Newton observation of approximately 100 ks performed on 5th August 2007 in the framework of the FERO project Aladin RGB composite image

  2. ESO511-G030 remarkable properties About 30% increase in Hardness Ratio F(2.0-10 keV)/F(0.2-2.0 keV) in 100 ks

  3. ESO511-G030 remarkable properties Particular hysteresis cycle in the countrate-hardness ratio space

  4. ESO511-G030 remarkable properties Variability studies allow us to constrain timescales and distances in the system to understand better the structure of Seyferts and processes acting therein

  5. Our fit: phabs×(powerlaw+pexrav+zgauss+kdblurreflion) OVII triplet

  6. Our fit: phabs×(powerlaw+pexrav+zgauss+kdblurreflion) OVII triplet

  7. Comparison with light bending model Miniutti & Fabian (2004) • Miniutti & Fabian (2004) propose a model in which the connection between primary emission and disc reflection fluxes can be explained assuming a change in height of the primary X-ray emission source over the disc, thus modifying the geodesics photons follow: • Higher height  less photons will be captured by the BH  lower powerlaw observed flux • Lower height  more photons will follow blackhole-influenced metrics geodesics  accretion disc gets more illuminated and the observed powerlaw flux is lower

More Related