  The scaling of the turbulent spectra provides a key measurement that allows
to discriminate between different theoretical predictions of turbulence. In the
solar wind, this has driven a large number of studies dedicated to this issue
using in-situ data from various orbiting spacecraft. While a semblance of
consensus exists regarding the scaling in the MHD and dispersive ranges, the
precise scaling in the transition range and the actual physical mechanisms that
control it remain open questions. Using the high-resolution data in the inner
heliosphere from Parker Solar Probe (PSP) mission, we find that the sub-ion
scales (i.e., at the frequency f ~ [2, 9] Hz) follow a power-law spectrum f^a
with a spectral index a varying between -3 and -5.7. Our results also show that
there is a trend toward and anti-correlation between the spectral slopes and
the power amplitudes at the MHD scales, in agreement with previous studies: the
higher the power amplitude the steeper the spectrum at sub-ion scales. A
similar trend toward an anti-correlation between steep spectra and increasing
normalized cross helicity is found, in agreement with previous theoretical
predictions about the imbalanced solar wind. We discuss the ubiquitous nature
of the ion transition range in solar wind turbulence in the inner heliosphere.
