Kinematics of the Broad-line Region of 3C 273 from a Ten-year Reverberation Mapping Campaign. (arXiv:1811.03812v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_Z/0/1/0/all/0/1">Zhi-Xiang Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Du_P/0/1/0/all/0/1">Pu Du</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smith_P/0/1/0/all/0/1">Paul S. Smith</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhao_Y/0/1/0/all/0/1">Yulin Zhao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hu_C/0/1/0/all/0/1">Chen Hu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xiao_M/0/1/0/all/0/1">Ming Xiao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_Y/0/1/0/all/0/1">Yan-Rong Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Huang_Y/0/1/0/all/0/1">Ying-Ke Huang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_K/0/1/0/all/0/1">Kai Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bai_J/0/1/0/all/0/1">Jin-Ming Bai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ho_L/0/1/0/all/0/1">Luis C. Ho</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_J/0/1/0/all/0/1">Jian-Min Wang</a>

Despite many decades of study, the kinematics of the broad-line region of 3C
273 are still poorly understood. We report a new, high signal-to-noise,
reverberation mapping campaign carried out from Nov 2008 to Mar 2018 that
allows the determination of time lags between emission lines and the variable
continuum with high precision. The time lag of variations in Hbeta relative
to those of the 5100AA continuum is $146.8_{-12.1}^{+8.3}$ days in the rest
frame. The time lag of the Hgamma emission line is found to be nearly the
same as for Hbeta. The lag of the Fe II emission is $322.0_{-57.9}^{+55.5}$
days, longer by a factor of $sim$2 than for the Balmer lines. The
velocity-resolved lag measurements of the Hbeta line show a complex structure
which can be possibly explained by a Keplerian disk or virialized motion with
some inflowing radial velocity in the Hbeta-emitting region. The decomposition
of its HST images yields a host stellar mass of $M_* = 10^{11.3 pm 0.7}
M_{odot}$. Taking the virial factor of $f_{rm BLR} = 1.3$, we derive a BH
mass of $M_{bullet} = 4.1_{-0.4}^{+0.3} times 10^8 M_{odot}$ and an
accretion rate of $9.3,L_{rm Edd},c^{-2}$ from the Hbeta line.

Despite many decades of study, the kinematics of the broad-line region of 3C
273 are still poorly understood. We report a new, high signal-to-noise,
reverberation mapping campaign carried out from Nov 2008 to Mar 2018 that
allows the determination of time lags between emission lines and the variable
continuum with high precision. The time lag of variations in Hbeta relative
to those of the 5100AA continuum is $146.8_{-12.1}^{+8.3}$ days in the rest
frame. The time lag of the Hgamma emission line is found to be nearly the
same as for Hbeta. The lag of the Fe II emission is $322.0_{-57.9}^{+55.5}$
days, longer by a factor of $sim$2 than for the Balmer lines. The
velocity-resolved lag measurements of the Hbeta line show a complex structure
which can be possibly explained by a Keplerian disk or virialized motion with
some inflowing radial velocity in the Hbeta-emitting region. The decomposition
of its HST images yields a host stellar mass of $M_* = 10^{11.3 pm 0.7}
M_{odot}$. Taking the virial factor of $f_{rm BLR} = 1.3$, we derive a BH
mass of $M_{bullet} = 4.1_{-0.4}^{+0.3} times 10^8 M_{odot}$ and an
accretion rate of $9.3,L_{rm Edd},c^{-2}$ from the Hbeta line.

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