Disentangling Weak AGN and Metallicity Gradients in High Redshift Star Forming Galaxies

Details Disentangling Weak AGN and Metallicity Gradients in High Redshift Star Forming Galaxies Disentangling Weak AGN and Metallicity Gradients in High Redshift Star Forming Galaxies

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21543511w&link_type=abstract

American Astronomical Society, AAS Meeting #215, #435.11; Bulletin of the American Astronomical Society, Vol. 42, p.381

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Optics

Scientific paper

We present diffraction-limited integral field spectrograph (IFS) observations of rest-frame Hβ, [O III], Hα, and [N II] emission from individual high redshift (1 < z < 3) star forming galaxies. These results are part of an on-going chemo-dynamical survey using 0.1" spatial resolution with OSIRIS coupled to the Keck Observatory Adaptive Optics (AO) system. In our previous work using OSIRIS, we found that metallicity indicators, like [N II] 658.4 nm and [O III] 500.7 nm, do not simply trace global star formation, but can be contaminated by weak AGN emission. These sources showed no other signs of AGN activity within their SEDs or rest-frame UV spectra. Our survey targets galaxies that have been used previously in metallicity studies at high-redshift. These observations allow us to disentangle any potential contamination from AGN activity, and to map two-dimensional chemical abundance gradients on sub-kiloparsec scales. We also investigate the internal rotation and velocity dispersion of these galaxies and discuss their implications for the growth of these early systems. We acknowledge funding support from NASA STScI HF-51265.01.

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