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We have obtained high-resolution data of the z 2 ring-like, clumpystar-forming galaxy (SFG) ZC406690 using the VLT/SINFONI with AO (in K-band)and in seeing-limited mode (in H- and J-band). Our data includes all of themain strong optical emission lines: [OII], [OIII], Ha, Hb, [NII] and [SII]. Wefind broad, blueshifted Ha and [OIII] emission line wings in the spectra of thegalaxy's massive, star-forming clumps (sigma \sim 85 km s^-1) and even broaderwings (up to 70% of the total Ha flux, with sigma \sim 290 km s^-1) in regionsspatially offset from the clumps by \sim 2 kpc. The broad emission likelyoriginates from large-scale outflows with mass outflow rates from individualclumps that are 1-8x the SFR of the clumps. Based on emission line ratiodiagnostics ([NII]/Ha and [SII]/Ha) and photoionization and shock models, wefind that the emission from the clumps is due to a combination ofphotoionization from the star-forming regions and shocks generated in theoutflowing component, with 5-30% of the emission deriving from shocks. In termsof the ionization parameter (6x10^7-10^8 cm/s, based on both the SFR and theO32 ratio), density (local electron densities of 300-1800 cm^-3 in and aroundthe clumps, and ionized gas column densities of 1200-8000 Msol/pc^2), and SFR(10-40 Msol/yr), these clumps more closely resemble nuclear starburst regionsof local ULIRGs and dwarf irregulars than HII regions in local galaxies.However, the star-forming clumps are not located in the nucleus as in localstarburst galaxies but instead are situated in a ring several kpc from thecenter of their high-redshift host galaxy, and have an overall disk-likemorphology. The two brightest clumps are quite different in terms of theirinternal properties, energetics and relative ages, and thus we are given aglimpse at two different stages in the formation and evolution of rapidlystar-forming giant clumps at high-z.

Shocked Superwinds from the z~2 Clumpy Star-forming Galaxy, ZC406690