Is there structure in the velocity dispersion maps of turbulent disks?
Abstract
Galaxies at z > 1 have shown to be different from galaxies at local redshifts. They have irregular morphologies with prominent star-forming clumps. However, due to the limited resolution of high-redshift observations, it is difficult to disentangle the physical processes that create and destroy star-forming clumps. Leaving many open questions in the study of galaxy evolution. The DYnamics of Newly Assembled Massive Objects (DYNAMO) survey aims to observe local galaxies (z < 0.25) with properties similar to those at high redshift (z∼2). This poster presents the near infrared spectra of 3 DYNAMO objects taken with the OSIRIS integral-field spectrograph on the Keck telescope. The high spatial and spectral resolution of OSIRIS allows us to obtain detailed kinematic maps. We are able to resolve the velocity dispersion of individual star-forming clumps down to sizes of ~300 pc. We find that after removing the systematics there is a significant structure in the velocity dispersion. However, whether there is a correlation between velocity dispersion and star formation, remains an open question. This work aims to disentangle the role of turbulence in the life and dead of star-forming clumps.
- Publication:
-
The Interplay between Local and Global Processes in Galaxies,
- Pub Date:
- June 2016
- Bibcode:
- 2016ilgp.confE..23O
- Keywords:
-
- galaxies: general;
- galaxies: structures