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Ultraluminous Star-Forming Galaxies and Extremely Luminous Warm Molecular Hydrogen Emission at z=2.16 in the PKS 1138-26 Radio Galaxy Protocluster

A deep Spitzer Infrared Spectrograph map of the PKS 1138-26 galaxy protocluster reveals ultraluminous PAH emission from obscured star formation in three protocluster galaxies, including Halpha-emitter (HAE) 229, HAE 131, and the central Spiderweb Galaxy. Star formation rates of 500-1100 Msun/yr are estimated from the 7.7 micron PAH feature. At such prodigious formation rates, the galaxy stellar masses will double in 0.6-1.1 Gyr. We are viewing the peak epoch of star formation for these protocluster galaxies. However, it appears that extinction of Halpha is much greater (factor of 40) in the two ULIRG HAEs compared to the Spiderweb. This may be attributed to different spatial distributions of star formation--nuclear star formation in the HAEs versus extended star formation in accreting satellite galaxies in the Spiderweb. We find extremely luminous mid-IR rotational line emission from warm molecular hydrogen in the Spiderweb Galaxy, with L(H2 0-0 S(3))= 1.4E44 erg/s (3.7E10 Lsun), 20 times more luminous than any previously known H2 emission galaxy (MOHEG). Depending on temperature, this corresponds to a very large mass of >9E6-2E9 Msun of T>300 K molecular gas, heated by the PKS 1138-26 radio jet, acting to quench nuclear star formation. There is >8 times more warm H2 at these temperatures in the Spiderweb than what has been seen in low-redshift (z<0.2) radio galaxies, indicating that the Spiderweb may have a larger reservoir of molecular gas than more evolved radio galaxies. This is the highest redshift galaxy yet in which warm molecular hydrogen has been directly detected.