Is there a UV/X-ray connection in IRAS 13224-3809?
Abstract
We present results from the optical, ultraviolet, and X-ray monitoring of the NLS1 galaxy IRAS 13224-3809 taken with Swift and XMM-Newton during 2016. IRAS 13224-3809 is the most variable bright AGN in the X-ray sky and shows strong X-ray reflection, implying that the X-rays strongly illuminate the inner disc. Therefore, it is a good candidate to study the relationship between coronal X-ray and disc UV emission. However, we find no correlation between the X-ray and UV flux over the available ∼40 d monitoring, despite the presence of strong X-ray variability and the variable part of the UV spectrum being consistent with irradiation of a standard thin disc. This means either that the X-ray flux which irradiates the UV emitting outer disc does not correlate with the X-ray flux in our line of sight and/or that another process drives the majority of the UV variability. The former case may be due to changes in coronal geometry, absorption or scattering between the corona and the disc.
- Publication:
-
Monthly Notices of the Royal Astronomical Society
- Pub Date:
- April 2018
- DOI:
- 10.1093/mnras/sty008
- arXiv:
- arXiv:1712.06606
- Bibcode:
- 2018MNRAS.475.2306B
- Keywords:
-
- accretion;
- accretion discs;
- black hole physics;
- galaxies: individual: IRAS13224-3809;
- galaxies: Seyfert;
- Astrophysics - High Energy Astrophysical Phenomena;
- Astrophysics - Astrophysics of Galaxies
- E-Print:
- 9 pages, 8 figures, MNRAS submitted: this version in response to reviewers comments