The Evolution and Growth of Nearby Galaxy Groups
DOI :
https://doi.org/10.17307/wsc.v1i1.326Mots-clés :
Galaxy groups, Galaxy Evolution, Magnitude Gap, BGG, Group Richness, Galaxy, MergersRésumé
This project strives to study the relationship between the group environment and individual galaxy properties. Group richness is used as a proxy for different environmental conditions and mass to form a sample of 40 low mass (3N<10), 40 medium mass (10N<20), and 40 high mass (20N) groups from the Berlind et al. 2006 volume-limited Mr18 catalog and Tempel et al. 2014 flux-limited catalog. Unique Color-Magnitude-Position and Color-Stellar Mass-Position diagrams are produced for each sample group. I identified dynamically active and inactive groups using the magnitude gap through a crude version of methodology described in Raouf et al. 2019. Project figures are used to analyze how BGG properties, dynamic activity, and group appearance depend on group richness. Analysis focuses on BGGs to understand how one evolutionary mechanism, mergers, is impacted by basic differences in a group’s environment.
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Fichiers supplémentaires
- Berlind et al 2006 High Mass Mr Diagrams (English)
- Berlind et al. 2006 Low Mass color-magnitude-position Diagrams (English)
- Berlind et al. 2006 Medium Mass color-magnitude-position (English)
- Berlind et al. 2006 High Mass color-mass-position (English)
- Berlind et al. 2006 Low Mass color-mass-position (English)
- Berlind et al. 2006 Medium Mass color-mass-position (English)
- Tempel et al. 2014 High Mass color-magnitude-position (English)
- Tempel et al. 2014 Low Mass color-magnitude-position (English)
- Tempel et al. 2014 Medium Mass color-magnitude-position (English)
- Tempel et al. 2014 High Mass color-mass-position (English)
- Tempel et al. 2014 Low Mass color-mass-position.pdf (English)
- Tempel et al. 2014 Medium Mass color-mass-position (English)
- Sample Information Table (English)
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