Fig. 1
Images of the CO(2 − 1) line emission (from Schinnerer et al. 2000) and HCN(1 − 0) line emission from NGC 3227. Superimposed is the ellipse tracing the circumnuclear ring (Davies et al. 2006). While the CO emission originates mostly from the ring, the HCN intensity is far higher in the central region. There is an order-of-magnitude change in the flux ratio between these regions.
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