Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21723302m&link_type=abstract
American Astronomical Society, AAS Meeting #217, #233.02; Bulletin of the American Astronomical Society, Vol. 43, 2011
Astronomy and Astrophysics
Astronomy
Scientific paper
My Ph.D. research focuses on the role of star formation in galaxies. Star formation, a critical driver of galaxy evolution, responds both to external influences (local and global environment) and internal influences (e.g., dust). I show how common observables, in particular the star formation rate (SFR), is influenced when galaxies fall into clusters via large-scale filaments. I find that complex galaxy populations (e.g., blue passive galaxies) are a direct consequence of the impact of environment on the star formation of galaxies. For a sample of nearby (z 0.1) clusters I show that star formation in galaxies falling into clusters seems to be enhanced on the clusters' periphery. I argue that galaxy-galaxy interactions in intermediate density regions such as cluster outskirts play a critical role in galaxy evolution. I use the line-of-sight velocity information obtained from the integrated galaxy spectra together with dark matter simulations to show that statistically, a single passage through the cluster core reduces the SFR in a galaxy by 40%. Using the nearby (100 Mpc) Coma supercluster, I show that the star formation-density relation varies with galaxy type: while dwarfs are star-forming everywhere except in the core of clusters and groups, their massive counterparts are mostly evolving passively. Transitional populations (i.e., post-starburst or k+A galaxies) preferentially lie in the vicinity of richer structures.
I also present the first results from the Star Formation Reference Survey (SFRS), where I compare global SFR metrics for a FIR-selected sample of star-forming galaxies in the nearby Universe obtained from the ultra-violet, mid- and far-infrared to 1.4 GHz radio imaging to show how the SFRs based on these canonical indicators correlate with the total SFR expected from a galaxy's bolometric luminosity.
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