CNKD in NGC 2179

By Michele Cappellari, Padova, April 16, 1998

Comparing the model with the observations

Observed Halpha emission line at the center of the Sa galaxy NGC2179

Model of the above emission line (on the same scale). The best fit is obtained with a Black Hole of 1.8*10^8 Msolar. This value is in good agreement with the Kormendy & Richstone (1995) relationship (Mbh=0.003*Mbulge).

Effect of a variation in the surface brightness profile

In the four pictures below the model has been computed with four different choiches of the radial profile of the gaseous disk. The surface brightness I(r)=r^n, with n=-1.5, -1.0, -0.5, 0.0.

Effect of a variation of the Black Hole mass

In the four figures below the Black Hole mass is given a mass Mbh=0.0, 9*10^7, 1.8*10^8, 3.6*10^8. The best mass estimate is Mbh=1.8*10^8 Msolar.

Effect of the intrinsic gas dispersion

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