Black hole mass measurement using ALMA observations of [CI] and CO emissions in the Seyfert 1 galaxy NGC 7469

We present a supermassive black hole (SMBH) mass measurement in the Seyfert 1 galaxy NGC7469 using Atacama Large Millimeter/submillimeter Array (ALMA) observations of atomic-${\rm [CI]}$(1-0) and molecular-$^{12}$CO(1-0) emission lines at spatial resolution $\approx0.3$" (or $\approx$ 100 pc). These emissions reveal that hosts circumnuclear gas disc (CND) with ring-like structure two-arm/bi-symmetric spiral pattern within it, surrounded by starbursting ring. The CND has relatively low $\sigma/V\approx0.35$ ($r\sim0.5$") $\sim0.19$ ($r>0.5"$), suggesting is dynamically settled suitable for deriving its central source. As expected from X-ray dominated region (XDR) effects dramatically increase an atomic carbon abundance dissociating CO molecules, we suggest [CI](1-0) better probe SMBH masses than AGNs. Our dynamical model ${\rm kinematics yields $M_{\rm BH}=1.78^{+2.69}_{-1.10}\times10^7$M$_\odot$ $M/L_{\rm F547M}=2.25^{+0.40}_{-0.43}$ (M$_\odot$/L$_\odot$). CO(1-0) also gives consistent BH}$ larger uncertainty, up to order magnitude, i.e.\ BH}=1.60^{+11.52}_{-1.45}\times10^7$M$_\odot$. This newly 2 times higher determined reverberation mapped (RM) method arising unresolved broad-line (BLR). Given this new BH}$, are able constrain specific RM dimensionless scaling factor $f=7.2^{+4.2}_{-3.4}$ AGN BLR NGC7469. thus Keplerian virial velocity component inclination $i\approx11.0^\circ$$_{-2.5}^{+2.2}$, confirming face-on orientation assuming geometrically thin model.