  As one of the series of papers reporting on a large reverberation mapping
campaign of super-Eddington accreting massive black holes (SEAMBHs) in active
galactic nuclei (AGNs), we present the results of 10 SEAMBHs monitored
spectroscopically during 2015-2017. Six of them are observed for the first
time, and have generally higher 5100 \AA\ luminosities than the SEAMBHs
monitored in our campaign from 2012 to 2015; the remaining four are repeat
observations to check if their previous lags change. Similar to the previous
SEAMBHs, the H$\beta$ time lags of the newly observed objects are shorter than
the values predicted by the canonical $R_{\mathrm{H\beta}}$-$L_{5100}$ relation
of sub-Eddington AGNs, by factors of $\sim2-6$, depending on the accretion
rate. The four previously observed objects have lags consistent with previous
measurements. We provide linear regressions for the
$R_{\mathrm{H\beta}}$-$L_{5100}$ relation, solely for the SEAMBH sample and for
low-accretion AGNs. We find that the relative strength of Fe II and the profile
of the H$\beta$ emission line can be used as proxies of accretion rate, showing
that the shortening of H$\beta$ lags depends on accretion rates. The recent
SDSS-RM discovery of shortened H$\beta$ lags in AGNs with low accretion rates
provides compelling evidence for retrograde accretion onto the black hole.
These evidences show that the canonical $R_{\mathrm{H\beta}}$-$L_{5100}$
relation holds only in AGNs with moderate accretion rates. At low accretion
rates, it should be revised to include the effects of black hole spin, whereas
the accretion rate itself becomes a key factor in the regime of high accretion
rates.
