Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21714242e&link_type=abstract
American Astronomical Society, AAS Meeting #217, #142.42; Bulletin of the American Astronomical Society, Vol. 43, 2011
Astronomy and Astrophysics
Astronomy
Scientific paper
The inner structure of AGNs has a standard model, but the model is poorly tested. The model is that of an accretion disk surrounded by a hot corona. The disk produces the primary optical and UV emission, the corona upscatters these photons to X-rays, and a fraction of those X-rays are re-processed in the disk, which fluoresces to produce the Compton Hump (E>10keV) and an Fe-K emission line that is broadened by disk rotation and general relativity. Since few corona temperatures have been measaured, we cannot separate the Compton y-parameter into its temperature (kt) and optical depth (Tau) components. As we lack high signal-to-noise >10keV spectra the parameters of the red wing to the 6.4keV Fe-K line are poorly determined in all but a few cases, limiting our knowledge of the disk inner radius and black hole spin - or our ability to test alternative, e.g. multi-Nh screens.
NuSTAR will provide the first high S/N spectra of AGNs above 10keV. We present detailed simulations that demonstrate that the kT-Tau degeneracy can be very cleanly broken. In conjunction with Suzaku or XMM-Newton spectra we show that the red wing Fe-K profile can be exquisitely determined, giving the black hole spin parameter with small uncertainties. We also show that NuSTAR can span wide ranges of black hole mass and Eddington ratio with a reasonable observing program.
Brenneman Laura
Civano Francesca
Elvis Martin
Harrison Fiona
NuSTAR Team
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