A new method to derive age differences between the various super star clusters observed in starburst galaxies using the two color diagram (B−H) vs (H−K) is presented. This method offers a quick and easy way to differentiate very young and intermediate age stellar populations even if data on extinction are unavailable. In this case, discrimination of regions younger and older than 4 Myr is feasi...

We report on the local environment, radial velocity, and star formation history of [O II]-selected emissionline objects in the z ≈ 0.4 galaxy cluster Abell 851, using optical spectra obtained with Keck I/LRIS and Keck II/DEIMOS. A large fraction (≈ 55%) of cluster [O II] emitters show strong Balmer absorption lines (& 4 Å in equivalent width at Hδ). These e(a)-type spectra have been attributed ...

The fate of ionizing radiation in starburst galaxies is key to understanding cosmic reionization. However, the galactic parameters on which the escape fraction of ionizing radiation depend are not well understood. Ionizationparameter mapping provides a simple, yet effective, way to study the radiative transfer in starburst galaxies. We obtain emission-line ratio maps of [S iii]/[S ii] for six, ...

We present the star formation rate (SFR) and starburst fraction (SBF) for a sample of field galaxies from the ICBS intermediate-redshift cluster survey. We use [O II] and Spitzer 24 μm fluxes to measure SFRs, and 24 μm fluxes and Hδ absorption to measure of SBFs, for both our sample and a present-epoch field sample from the Sloan Digital Sky Survey (SDSS) and Spitzer Wide-area Infrared Extragal...

The collision of gas-rich galaxies is believed to produce strong shocks between their gas clouds which cause the onset of the observed bursts of extended star formation. However, the so far observed shock signatures in colliding galaxies can be explained essentially by winds from already existing massive stars and supernovae and thus do not give any evidence for an outstanding pre-starburst pha...

We report the detection of CO(3→2) emission from the submillimeter–selected luminous galaxy SMMJ14011+0252. The optical counterpart of the submillimeter source has been identified as a merger system with spectral characteristics consistent with a starburst at z = 2.565. The CO emission confirms the optical identification of the submillimeter source and implies a molecular gas mass of 5×1010h 75...

Some of the basic properties of star formation in starburst galaxies are reviewed. I discuss triggering and termination mechanisms in starbursts and provide estimates of star-formation rates. Galaxies with ongoing star formation at low and high redshift are compared.

We compare high-resolution optical and radio imaging of 12 luminous submillimeter (submm) galaxies at a median z = 2.2 ± 0.2 observed with Hubble Space Telescope (HST) and the MERLIN and VLA radio interferometers at comparable spatial resolution, ∼ 0.3 (∼ 2 kpc). The radio emission is used as a tracer of the likely far-infrared morphology of these dusty, luminous galaxies. In ∼30% of the sample...