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We present a kinematic analysis of the dense molecular gas in the central 200parsecs of the nearby galaxy NGC1097, based on Cycle 0 observations with theAtacama Large Millimeter/sub-millimeter Array (ALMA). We use the HCN(4-3) lineto trace the densest interstellar molecular gas, and quantify its kinematics,and estimate an inflow rate for the molecular gas. We find a strikingsimilarity between the ALMA kinematic data and the analytic spiral inflow modelthat we have previously constructed based on ionized gas velocity fields onlarger scales. We are able to follow dense gas streaming down to 40 pc distancefrom the supermassive black hole in this Seyfert 1 galaxy. In order to fulfillmarginal stability, we deduce that the dense gas is confined to a very thindisc, and we derive a dense gas inflow rate of 0.09 Msun/yr at 40 pc radius.Combined with previous values from the Ha and CO gas, we calculate a combinedmolecular and ionized gas inflow rate of 0.2 Msun/yr at 40 pc distance from thecentral supermassive black hole of NGC1097.

ALMA follows streaming of dense gas down to 40 pc from the supermassive black hole in NGC1097