A SAMI and MaNGA view on the kinematics of star-forming galaxies
We investigate the physical connection between the growth of dispersionsupported stellar structures (e.g. classical bulges) and position of galaxies on the star forming main sequence (SFMS) at z~0. Combining the might of the SAMI and MaNGA galaxy IFS surveys, we measure the λRe spin parameter for 37...
| Main Authors: | , , |
|---|---|
| Format: | Conference Object |
| Language: | unknown |
| Published: |
2021
|
| Subjects: | |
| Online Access: | https://zenodo.org/record/4721522 https://doi.org/10.5281/zenodo.4721522 |
| Summary: | We investigate the physical connection between the growth of dispersionsupported stellar structures (e.g. classical bulges) and position of galaxies on the star forming main sequence (SFMS) at z~0. Combining the might of the SAMI and MaNGA galaxy IFS surveys, we measure the λRe spin parameter for 3781 galaxies with reliable stellar kinematics. After first confirming the importance of PSF corrections for seeing-dominated IFS data, we present the kinematic properties of galaxies above, below, and on the SFMS. Above log M*~10.5, we find tantalising evidence for an increase in the number of galaxies with dispersion-supported structures, suggesting a connection between bulge growth and the bending of the main sequence. Our results suggest that while a population of galaxies possessing some dispersion-supported structure is already present on the SFMS, further growth would be required after the galaxy has quenched to match the kinematic properties observed in passive galaxies at z~0. |
|---|