We report on the deepest X-ray observation of the narrow-line Seyfert 1 galaxy Mrk 335 in the low-flux state obtained with Suzaku .
The data are compared to a 2006 high-flux Suzaku observation when the source was \sim 10 \times brighter .
Describing the two flux levels self-consistently with partial covering models would require extreme circumstances , as the source would be subject to negligible absorption during the bright state and ninety-five per cent covering with near Compton-thick material when dim .
Blurred reflection from an accretion disc around a nearly maximum spinning black hole ( a > 0.91 , with preference for a spin parameter as high as \sim 0.995 ) appears more likely and is consistent with the long-term and rapid variability .
Measurements of the emissivity profile and spectral modelling indicate the high-flux Suzaku observation of Mrk 335 is consistent with continuum-dominated , jet-like emission ( i.e .
beamed away from the disc ) .
It can be argued that the ejecta must be confined to within \sim 25 { \thinspace r _ { g } } if it does not escape the system .
During the low-flux state the corona becomes compact and only extends to about 5 { \thinspace r _ { g } } from the black hole , and the spectrum becomes reflection-dominated .
The low-frequency lags measured at both epochs are comparable indicating that the accretion mechanism is not changing between the two flux levels .
Various techniques to study the spectral variability ( e.g .
principal component analysis , fractional variability , difference spectra , and hardness ratio analysis ) indicate that the low-state variability is dominated by changes in the power law flux and photon index , but that changes in the ionisation state of the reflector are also required .
Most notably , the ionisation parameter becomes inversely correlated with the reflected flux after a long-duration flare-like event during the observation .