SUZAKU STUDIES OF THE CENTRAL ENGINE IN THE TYPICAL TYPE I SEYFERT NGC 3227: DETECTION OF MULTIPLE PRIMARY X-RAY CONTINUA WITH DISTINCT PROPERTIES

The type I Seyfert galaxy NGC 3227 was observed by Suzaku six times in 2008, with intervals of similar to 1 week and net exposures of similar to 50 ks each. Among the six observations, the source varied by nearly an order of magnitude; it was brightest in the first observation with a 2-10 keV luminosity of 1.2 x 10(42) erg s(-1), while faintest in the fourth observation with 2.9 x 10(41) erg s(-1). As it became fainter, the continuum in the 2-45 keV band became harder, while the narrow Fe-Ka emission line, detected on all occasions at 6.4 keV of the source rest frame, remained approximately constant in the photon flux. Through a method of variability-assisted broadband spectroscopy, the 2-45 keV spectrum of NGC 3227 was decomposed into three distinct components. One is a relatively soft powerlaw continuum with a photon index of similar to 2.3, weakly absorbed and highly variable on timescales of similar to 5 ks; it was observed only when the source was above a threshold luminosity of similar to 6.6 x 10(41) erg s(-1) (in 2-10 keV), and was responsible for further source brightening beyond. Another is a harder and more absorbed continuum with a photon index of similar to 1.6, which persisted through the six observations and varied slowly on timescales of a few weeks by a factor of similar to 2. This component, carrying a major fraction of the broadband emission when the source is below the threshold luminosity, is considered as an additional primary emission. The last one is a reflection component with the narrow iron line, produced at large distances from the central black hole.