The Nature of Compact Galaxies in the Hubble Deep Field (II): Spectroscopic Properties and Implications for the Evolution of the Star Formation Rate Density of the Universe

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Abstract
We present a spectroscopic study of 51 compact field galaxies with redshifts z < 1.4 and apparent magnitudes I < 23.74 in the flanking fields of the Hubble Deep Field. These galaxies are compact in the sense that they have small apparent half-light radii (r_e < 0.5 arcsec) and high surface brightnesses (SB_e < 22.2 mag arcsec^-2). The spectra, taken at the Keck telescope, show emission lines in 88% of our sample, and only absorption lines in the remaining 12%. Emission-line profiles are roughly Gaussian with velocity widths that range from the measurement limit of sigma = 35 km s^-1 to 150 km s^-1. Rest-frame [OII]3727 equivalent widths range from 5A to 94A , yielding star formation rates (SFR) of 0.1 to 14 M yr^-1. The analysis of various line diagnostic diagrams reveals that 60% of compact emission-line galaxies have velocity widths, excitations, Hbeta luminosities, SFRs, and mass-to-light ratios characteristic of young star-forming HII galaxies. The remaining 40% form a more heterogeneous class of evolved starbursts, similar to local starburst disk galaxies. We find that, although the compact galaxies at z>0.7 have similar SFRs per unit mass to those at z<0.7, they are on average 10 times more massive. Our sample implies a lower limit for the global comoving SFR density of 0.004 M yr^-1 Mpc^-3 at z = 0.55, and 0.008 M yr^-1 Mpc^-3 at z = 0.85 (assuming Salpeter IMF, Ho = 50 km s^-1 Mpc^-1, and qo = 0.5). These values, when compared to estimates for a sample of local compact galaxies selected in a similar fashion, support a history of the universe in which the SFR density declines by a factor 10 from z = 1 to today.