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We present a new catalogue of EROs from the Groth Strip and study the relation between their morphology and mass. With a selection criterion F814W−  K  s ≥ 4  and   K  s ≤ 21.0  we find 102 EROs, over a survey area of 155 arcmin 2 , leading to a surface density of 0.66 arcmin −2 . The photometric data include   U ,  B ,  F 606 W ,  F 814 W ,  J ,  K  s   bands. Morphologies are based on a by eye classification and we distinguish between three basic classes: compact objects, targets with a disc and/or a bulge component and irregular or merger candidates. An additional group consists of the few objects which could not be classified.  The majority of our targets has either a very compact morphology (34 ± 6 per cent), or show more or less distinct disc components (43 ± 6 per cent). 14 ± 4 per cent are merger or irregulars and seven objects (approximately 9 per cent) could not be classified.  We also study the dependence of structural parameters (effective radius:  r  eff , Sérsic index:  n ) on morphological appearance. As expected, EROs that are either compact or show a distinct bulge component have smaller median effective radii (1.22 ± 0.14 kpc and 3.31 ± 0.53 kpc) than disc dominated (5.50 ± 0.51 kpc) or possible irregular galaxies or merger candidates (4.92 ± 0.14 kpc). More importantly, the Sérsic index changes from 2.30 ± 0.34 and 3.24 ± 0.55, to 1.03 ± 0.24 and 1.54 ± 0.40, respectively.  As found in previous studies, most the EROs in our sample have redshifts between  z = 1 and 2; however, compact EROs in our sample are found at redshifts as low as  z = 0.4 and as high as  z = 2.8; the latter qualify as well as distant red galaxies (DRGs). Disc‐like EROs are also found up to  z = 2.8; however, those with a bulge‐disc structure are only seen at  z  &lt; 1.5.  For each of these EROs we determined the stellar mass and mean population age by fitting synthetic Bruzual (2007) spectra to the photometric spectral energy distributions, via χ 2  minimization. Mass estimates were obtained by assuming an exponentially declining star formation rate with a wide set of parameters, e.g. decay time, redshift of last star formation, metallicity and optical depth. Total stellar masses for our sample are in the range 9.1 &lt; log( M /M ⊙ ) &lt; 11.6. We cannot detect significant differences between the stellar mass distribution of the morphological classes. EROs with masses of log( M /M ⊙ ) &gt; 11.0 dominantly show compact morphologies, but also include a significant number of sources with a disc morphology.

The morphologies and masses of extremely red galaxies in the Groth Strip