The ALMA Discovery of the Rotating Disk and Fast Outflow of Cold Molecular Gas in NGC~1275. (arXiv:1905.06017v1 [astro-ph.GA])

The ALMA Discovery of the Rotating Disk and Fast Outflow of Cold Molecular Gas in NGC~1275. (arXiv:1905.06017v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Nagai_H/0/1/0/all/0/1">H. Nagai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Onishi_K/0/1/0/all/0/1">K. Onishi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kawakatu_N/0/1/0/all/0/1">N. Kawakatu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fujita_Y/0/1/0/all/0/1">Y. Fujita</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kino_M/0/1/0/all/0/1">M. Kino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fukazawa_Y/0/1/0/all/0/1">Y. Fukazawa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lim_J/0/1/0/all/0/1">J. Lim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Forman_W/0/1/0/all/0/1">W. Forman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vrtilek_J/0/1/0/all/0/1">J. Vrtilek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nakanishi_K/0/1/0/all/0/1">K. Nakanishi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Noda_H/0/1/0/all/0/1">H. Noda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Asada_K/0/1/0/all/0/1">K. Asada</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wajima_K/0/1/0/all/0/1">K. Wajima</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ohyama_Y/0/1/0/all/0/1">Y. Ohyama</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+David_L/0/1/0/all/0/1">L. David</a>

We present ALMA Band 6 observations of the CO(2-1), HCN(3-2), and
HCO$^{+}$(3-2) lines in the nearby radio galaxy / brightest cluster galaxy
(BCG) of NGC~1275 with the spatial resolution of $sim20$~pc. In the previous
observations, CO(2-1) emission was detected as radial filaments lying in the
east-west direction. We resolved the inner filament and found that the filament
cannot be represented by a simple infalling stream both morphologically and
kinematically. The observed complex nature of the filament resembles the cold
gas structure predicted by recent numerical simulations of cold chaotic
accretion. A crude estimate suggests that the accretion rate of the cold gas
can be higher than that of hot gas. Within the central 100~pc, we detected a
rotational disk of the molecular gas whose mass is $sim10^{8}~M_{sun}$. This
is the first evidence of the presence of massive cold gas disk on this spatial
scale for BCGs. The disk rotation axis is approximately consistent with the
axis of the radio jet on subpc scales. This probably suggests that the cold gas
disk is physically connected to the innermost accretion disk which is
responsible for jet launching. We also detected absorption features in the
HCN(3-2) and HCO$^{+}$(3-2) spectra against the radio continuum emission mostly
radiated by $sim1.2$-pc size jet. The absorption features are blue-shifted
from the systemic velocity by $sim$300-600~km~s$^{-1}$, which suggests the
presence of outflowing gas from the active galactic nucleus (AGN). We discuss
the relation of the AGN feeding with cold accretion, the origin of blue-shifted
absorption, and estimate of black hole mass using the molecular gas dynamics.

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