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AGN feedback in dwarf galaxies?

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Figure

Figure 1. Schematic view of the outflow structure. The accreting IMBH drives the wind with velocity v w
Figure 2. Ratio between the mechanical luminosity from the AGN and the mechanical luminosity from SNe, as a function of the halo mass, for different values of (a) the Eddington ratio χ , (b) the exponent α in the M BH – σ relation and (c) SNe wind efficien
Fig. 3 displays the propagation for different (χ , t AGN ) pairs. The critical mass is the halo mass (1) below which the shell velocity is above the escape velocity at the virial radius and (2) above which the shell slows down before reaching the virial ra
Figure 5. Critical black hole mass above which, for a given halo mass, AGN feedback is stronger than SN feedback for different values of (a) the duration of the AGN, t AGN , (b) the SN wind efficiency w and (c) the Eddington ratio χ

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