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The observed stellar mass function (SMF) is very different to the halo mass function predicted by cold dark matter ( CDM), and it is widely accepted that this is due to energy feedback from supernovae and black holes. However, the strength and form of this feedback is not understood. In this paper, we use the phenomenological model GALFORM to explore how galaxy formation depends on the strength and halo mass dependence of feedback. We focus on 'expulsion' models in which the wind mass loading, , is proportional to 1/v n disc , with n = 0, 1, 2 and contrast these models with the successful Bower et al. model (B8W7), for which
Bower et al. (Tue,) studied this question.
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