“Photometry of overlapping galaxy pairs”的版本间差异
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'''Collaborator: Shuai Feng (postgraduate student)''' |
'''Collaborator: Shuai Feng (postgraduate student)''' |
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== Question == |
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[[File:overlapping_pair.png|150px|right]] |
[[File:overlapping_pair.png|150px|right]] |
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Galaxy pair is a kind of self-gravitational system, which contains two member galaxies. Because of simplest configuration, galaxy pairs are very useful to study the interaction effect, such as merge, tidal force, dynamic fiction. However, projected effect often causes overlapping in galaxy pairs, especially in compact pairs. That seriously biases photometric parameters due to comtamination of each star light. How to get rid of overlapping influence has become a very important task. |
Galaxy pair is a kind of self-gravitational system, which contains two member galaxies. Because of simplest configuration, galaxy pairs are very useful to study the interaction effect, such as merge, tidal force, dynamic fiction. However, projected effect often causes overlapping in galaxy pairs, especially in compact pairs. That seriously biases photometric parameters due to comtamination of each star light. How to get rid of overlapping influence has become a very important task. |
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2015年4月21日 (二) 11:10的版本
Advisor: Shiyin Shen[1]
Collaborator: Shuai Feng (postgraduate student)
Galaxy pair is a kind of self-gravitational system, which contains two member galaxies. Because of simplest configuration, galaxy pairs are very useful to study the interaction effect, such as merge, tidal force, dynamic fiction. However, projected effect often causes overlapping in galaxy pairs, especially in compact pairs. That seriously biases photometric parameters due to comtamination of each star light. How to get rid of overlapping influence has become a very important task.