Kavli Affiliate: Claudio Ricci
| First 5 Authors: Zachary Stone, Yue Shen, Scott F. Anderson, Franz Bauer, W. N. Brandt
| Summary:
We present dynamical modeling of the broad-line region (BLR) for the highly
variable AGN SDSS J141041.25+531849.0 ($z = 0.359$) using photometric and
spectroscopic monitoring data from the Sloan Digital Sky Survey Reverberation
Mapping project and the SDSS-V Black Hole Mapper program, spanning from early
2013 to early 2023. We model the geometry and kinematics of the BLR in the
H$beta$, H$alpha$, and MgII, emission lines for three different time periods
to measure the potential change of structure within the BLR across time and
line species. We consistently find a moderately edge-on $(i_{rm full-state} =
53.29^{circ} ,{}^{+7.29}_{-6.55})$ thick-disk $(theta_{rm opn, ;
full-state} = 54.86^{circ} ,{}^{+5.83}_{-4.74})$ geometry for all BLRs, with
a joint estimate for the mass of the supermassive black hole (SMBH) for each of
three time periods, yielding $log_{10}(M_{rm BH} / M_{odot}) =
7.66^{+0.12}_{-0.13}$ when using the full dataset. The inferred individual
virial factor $f$ $sim 1$ is significantly smaller than the average factor for
a local sample of dynamically modeled AGNs. There is strong evidence for
non-virial motion, with over $80%$ of clouds on inflowing/outflowing orbits.
We analyze the change in model parameters across emission lines, finding the
radii of BLRs for the emission lines are consistent with the following relative
sizes $R_{rm Hbeta} lesssim R_{rm MgII } lesssim R_{rm Halpha}$.
Comparing results across time, we find $R_{rm low-state} lesssim R_{rm
high-state}$, with the change in BLR size for H$beta$, being more significant
than for the other two lines. The data also reveal complex, time-evolving, and
potentially transient dynamics of the BLR gas over decade-long timescales,
encouraging for future dynamical modeling of fine-scale BLR kinematics.
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