Galaxy Merge

Simulation

• 'Identikit' software (Barnes & Hibbard 2009) : merge的状态

• 星系的次并合对spin的影响不大，主并合又分两种情况[1]、

fast rotator : 质量较小的merge，气体较多，merge之后可以重新获得气体和恒星，从而获得spin

slow rotator: 质量较大的merge，气体少，并合消耗spin，因而最终是slow rotator

galaxy pair

• 大星系周围的非常close的satellite计数 [2]

If the satellites eventually infall into the host galaxies, the merger channel will be largely dominated by satellites with a mass ratio down to 1:10,(as these objects have 68 per cent of the total mass in satellites).