Combined Long and Short Timescale X-ray Variability of NGC4051 with RXTE and XMM-Newton

Details Combined Long and Short Timescale X-ray Variability of NGC4051 with RXTE and XMM-Newton Combined Long and Short Timescale X-ray Variability of NGC4051 with RXTE and XMM-Newton

2003-11-10

arxiv.org/abs/astro-ph/0311220v1

Mon.Not.Roy.Astron.Soc.348:783,2004

Astronomy and Astrophysics

Astrophysics

Accepted for publication in MNRAS; 22 pages, 19 figures

Scientific paper

10.1111/j.1365-2966.2004.07376.x

We present over 6.5 years of frequent X-ray observations of the NLS1 galaxy NGC4051 by RXTE together with a >100ks observation by XMM-Newton and so derive a 2-10 keV PSD covering an unprecedent frequency range of over 6.5 decades from <10^-8 to >10^-2 Hz. This PSD is a very good match to the PSD of the galactic black hole binary system (GBH) Cyg X-1 when in a `high', rather than `low', state providing the first definite confirmation of an AGN in a `high' state. A bending, rather than sharply broken, powerlaw is a better description of the PSDs of Cyg X-1 in the high state and of NGC4051. At low frequencies the PSD of NGC4051 has a slope of -1.1 bending, at nu_B = 8 x 10^-4 Hz, to a slope of alpha_H ~ -2 (steeper at lower energies). If nu_B scales with mass, we imply a black hole mass of 3 x 10^5 Msolar in NGC4051, consistent with the 5 x 10^5 Msolar reverberation value. Hence NGC4051 is emitting at ~30% L_Edd. NGC4051 follows the same rms-flux relationship as GBHs. Phase lags and coherence between bands are also the same as in GBHs. The lag of soft by hard photons increases, and coherence decreases, as band separation increases. The lag, and coherence, are greater for variations of longer Fourier period. This behaviour suggests that higher photon energies and shorter variability timescales are associated with smaller radii. Using also data from the literature, we cannot fit all AGN to the same linear scaling of break timescale with black hole mass. However broad line AGN are consistent with a linear scaling from Cyg X-1 in its low state and NLS1 galaxies scale better with Cyg X-1 in its high state. We suggest that the relationship between black hole mass and break timescale is a function of at least one other underlying parameter, which may be accretion rate or black hole spin.

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