1. The Compton hump and variable blue wing in the extreme low-flux NuSTAR observations of 1H0707-495
- Author
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Dominic J. Walton, S. E. Boggs, Erin Kara, Anne M. Lohfink, D. Stern, Michael Parker, Giorgio Matt, C. J. Hailey, Fiona A. Harrison, W. W. Zhang, A. C. Fabian, Finn Erland Christensen, Christopher S. Reynolds, Kara, E, Fabian, A. C., Lohfink, A. M., Parker, M. L., Walton, D. J., Boggs, S. E., Christensen, F. E., Hailey, C. J., Harrison, F. A., Matt, Giorgio, Reynolds, C. S., Stern, D., and Zhang, W. W.
- Subjects
individual: 1H0707-495 [Galaxies] ,galaxie [X-rays] ,active [Galaxies] ,Astrophysics::High Energy Astrophysical Phenomena ,Flux ,FOS: Physical sciences ,X-ray telescope ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,law.invention ,Telescope ,Black hole physic ,law ,0103 physical sciences ,Emission spectrum ,010303 astronomy & astrophysics ,Physics ,High Energy Astrophysical Phenomena (astro-ph.HE) ,X-ray astronomy ,010308 nuclear & particles physics ,Compton scattering ,Astronomy ,Astronomy and Astrophysics ,Black hole physics ,Redshift ,Galaxy ,galaxies [X-rays] ,Space and Planetary Science ,Astrophysics - High Energy Astrophysical Phenomena - Abstract
The Narrow-line Seyfert I galaxy, 1H0707-495, has been well observed in the 0.3-10 keV band, revealing a dramatic drop in flux in the iron K alpha band, a strong soft excess, and short timescale reverberation lags associated with these spectral features. In this paper, we present the first results of a deep 250 ks NuSTAR observation of 1H0707-495, which includes the first sensitive observations above 10 keV. Even though the NuSTAR observations caught the source in an extreme low-flux state, the Compton hump is still significantly detected. NuSTAR, with its high effective area above 7 keV, clearly detects the drop in flux in the iron K alpha band, and by comparing these observations with archival XMM-Newton observations, we find that the energy of this drop increases with increasing flux. We discuss possible explanations for this, the most likely of which is that the drop in flux is the blue wing of the relativistically broadened iron K alpha emission line. When the flux is low, the coronal source height is low, thus enhancing the most gravitationally redshifted emission., Submitted to MNRAS, comments are welcome. 9 pages, 5 figures
- Published
- 2015
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