The central black hole in active galactic nuclei (AGNs) and their surrounding structures are of interest to astronomers. AGNs have been intensively monitored since the first time they been identified at the 1960s. Many methods and models have been raised in the past years, which are continuing to detect the intrinsic nature of AGNs. Super-Eddington accreting massive black holes (SEAMBHs) are a special subclass of AGNs, as they can serve as a new type of cosmological candles, and are also the objects we are interested in.Since the fall of 2012, we have monitored a large sample of high accretion rate AGNs, aiming at better understanding the role of accretion rates on BLRs and the physics of accretion onto black holes. Our results reveal that SEAMBHs reach saturated luminosities due to the photon trapping caused by Super-Eddington accretion. These results build a solid foundation for the cosmological candle theory. We have used the velocity-resolved analysis to offer a glimpse into the geometry and kinematics of the BLRs. This paper focuses on applying the maximum entropy method (MEM) to our SEAMBH sample for the velocity-delay maps of \hb and \hr emission lines. The maps of six objects are reliably reconstructed using MEM. The maps of H$\beta$ and H$\gamma$ emission lines of Mrk 335 indicate that the gas of its broad-line region (BLR) is infalling. For Mrk 142, its H$\beta$ and H$\gamma$ lines show signatures of outflow. The H$\beta$ and H$\gamma$ maps of Mrk 1044 demonstrate complex kinematics -- a virialized motion accompanied by an outflow signature, and the H$\beta$ map of IRAS F12397+3333 is consistent with a disk or a spherical shell. The \hb\ maps of Mrk~486 and MCG~+06-26-012 suggest the presence of an inflow and outflow, respectively. These super-Eddington accretors show diverse geometry and kinematics.NGC 5548 has been well spectroscopically monitored for reverberation mapping of the central kinematics by 19 campaigns. Using the maximum entropy method in this Letter, we build up a high-quality velocity-delay map of the \hb\ emission line in the light curves of the continuum and the line variations observed between 2015-2016. The map shows the response strength and lags of the velocity fields of the \hb\ emitting regions. The velocity-delay structure of the map is generally symmetric, with strong red and blue wings at time lag $\tau \lesssim 15$ days, a narrower velocity distribution at $\tau \gtrsim 15$ days, and a deficit of response in the core. This is suggestive of a disk geometry of the broad-line region (BLR).The relatively weaker \hb\ response at the longer lags in the red side indicates anisotropic emission from the outer part of the BLR. We also recover the velocity-delay maps of NGC~5548 from the historical data of 13 years to investigate the long-term variability of its BLR. In general, the BLR of NGC 5548 was switching between the inflow and virialized phases in the past years. The resultant maps of seven years reveal inflow signatures and show decreasing lags, indicating that the changes in the BLR size are related to the infalling BLR gas. The other four maps show potential disk signatures which are similar to our map.
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