Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...21112305m&link_type=abstract
American Astronomical Society, AAS Meeting #211, #123.05; Bulletin of the American Astronomical Society, Vol. 39, p.953
Astronomy and Astrophysics
Astrophysics
Scientific paper
Highly obscured by dust, a population of high-redshift ultra-luminous infrared galaxies (ULIRGs; L > 1012 L&sun;) has been identified by their strong mm and submm emission. Deep follow-up radio observations enabled the determination of faint counterparts and rest-UV redshifts for a large number of these submm galaxies (SMGs). These radio-identified SMGs have been shown to be cold, massive, merging systems undergoing intense star-formation, yet harboring a rapidly growing SMBH. With Mdyn 1011M&sun; and SFRs 100-1000M&sun;/yr, SMGs are likely the progenitors of today's massive ellipticals. I have led a variety of projects to unveil the details of the astrophysics at work within SMGs. These include: (1) a mid-IR spectroscopic study with the state-of-the-art Spitzer InfraRed Spectrograph that has demonstrated that the bolometric luminosity of SMGs is dominated by intense starburst activity, even though X-ray data suggest that 28-50% (and maybe all) SMGs host an AGN; (2) a study with Keck's Near-InfraRed SPECtrograph of restframe optical line emission to obtain dynamical masses and SFRs of SMGs; and (3) a detailed near-IR 2D spectroscopic study using Keck's OSIRIS to resolve kpc-scale gas kinematics and with which we have spatially separated the compact, broad Hα AGN component (FWHM ≥ 1500 km/s) from the more extended, narrow-line Hα stellar component (FWHM ≤ 500 km/s) in select SMGs.
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