We have studied the fast timing and spectral behavior of the black hole candidate (BHC) GX 339-4 using all 1-20 keV EXOSAT ME data: the 1983 July, 1984 March, 1984 May, and 1985 April observations. In 1985 April, GX 339-4 was in a weak low state (0.03 x 10(-9) ergs cm(-2) s(-1), 2-10 keV). The X-ray spectrum was a hard power law with a photon index alpha of 1.82, and the power spectrum, though ill-constrained by the data, was consistent with a typical BHC low-state spectrum. During the other three pointings the system was brighter (1.5 x 10(-9) ergs cm(-2) s(-1), 2-10 keV), an ultrasoft component was present in the spectrum, and the power law was steeper (alpha similar to 3.5 in 1984; in 1983 it was not well measured); the power spectrum showed a hat-topped band-limited noise component with a break frequency of similar to 4.5 Hz and a fractional rms amplitude of similar to 7%. Comparing flux levels, X-ray spectra, and power spectra, we conclude that in these observations GX 339-4 was in a state intermediate between the usual BHC low and high states. The system was similar to 4 times brighter than in its usual low state, 4 times fainter than in its usual high state, and an order of magnitude fainter than in its very high state. We compare these results to those recently obtained on other BHCs, and conclude that this ''intermediate-state'' behavior is a common characteristic of BHCs, which occurs at (M) over dot levels intermediate between the high and the low state. We argue that this result can be used to resolve the longstanding issue of the dependence of the power spectral break frequency in the low state on mass accretion rate, and strengthens the idea that low-state noise and very high state noise may have a common origin. We briefly discuss a possible interpretation for the changes in break frequency in the low state and between low state and intermediate state.
