Investigating Sub-structures Of Galaxies At z=2 With CANDELS

Details Investigating Sub-structures Of Galaxies At z=2 With CANDELS Investigating Sub-structures Of Galaxies At z=2 With CANDELS

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21942903g&link_type=abstract

American Astronomical Society, AAS Meeting #219, #429.03

Astronomy and Astrophysics

Astronomy

Scientific paper

We use the deep and high-resolution optical (HST/ACS) and near--IR (HST/WFC3 IR) imaging data in the Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey (CANDELS) to study the sub-structure of galaxies at z 2. The CANDELS images enable us to resolve structures of z 2 galaxies down to kiloparsec scale in the rest-frame UV and optical bands. In this work, we study the properties of giant kpc-scale clumps in star-forming galaxies (SFGs) at z 2 through multi-wavelength broad band photometry. The physical properties of clumps are measured through fitting spatially resolved seven-band (BVizYJH) spectral energy distribution (SED) to models. On average, our clumps are blue and have similar median rest-frame UV--optical color as the diffuse components of their host galaxies, but the clumps have large scatter in their colors. Although the SFR--stellar mass relation of galaxies is dominated by the diffuse components, clumps emerge as regions with enhanced specific star formation rates (SSFRs), contributing individually 10% and together 50% of the star formation rate (SFR) of the host galaxies. However, the contributions of clumps to the rest-frame UV/optical luminosity and stellar mass are smaller, typically a few percent individually and 20% together. Clump properties have radial variations in the sense that central clumps are redder, older, more extincted, denser, and less active on forming stars than outskirts clumps. Our results provide constraints on current theoretical models of clump formation and evolution.

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