查看“Galaxy Merge”的源代码

==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[https://arxiv.org/abs/1703.00545]、
: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

*streams are a strong indication of nearly circular infall of a satellite (with a large angular momentum), whereas the appearance of shells clearly points to (nearly) radial satellite infall. [https://arxiv.org/pdf/1808.10454.pdf]
==mini-merge==
*质量比小于1:10
*mini mergers can increase the size of the host disc significantly without changing the global shape of the galaxy, if the impact occurs along the disk plane, providing a possible explanation for extended low-surface brightness disks reported from observations [https://arxiv.org/pdf/1808.10454.pdf]

==galaxy pair==
*大星系周围的非常close的satellite计数 [http://adsabs.harvard.edu/abs/2014MNRAS.442..347R]
: 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).
*HI轮廓的非对称性 arXiv:1907.09877
*运动学上的非对称性，CALIFA的数据 [https://www.aanda.org/10.1051/0004-6361/201424935]