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We present an overview of recent key results from the SAMI Galaxy Survey on the build-up of mass and angular momentum in galaxies across morphology and environment. The SAMI Galaxy survey is a multi-object integral field spectroscopic survey and provides a wealth of spatially-resolved, two-dimensional stellar and gas measurements for galaxies of all morphological types, with high-precision due the stable spectral resolution of the AAOmega spectrograph. The sample size of ~3000 galaxies allows for dividing the sample in bins of stellar mass, environment, and star-formation or morphology, whilst maintaining a statistical significant number of galaxies in each bin. By combining imaging, spatially resolved dynamics, and stellar population measurements, our result demonstrate the power of utilising integral field spectroscopy on a large sample of galaxies to further our understanding of physical processes involved in the build-up of stellar mass and angular momentum in galaxies. [ABSTRACT FROM AUTHOR]

We present the second major release of data from the Sydney – Australian Astronomical Observatory Multi-Object Integral Field Spectrograph (SAMI) Galaxy Survey. Data Release Two includes data for 1559 galaxies, about 50 per cent of the full survey. Galaxies included have a redshift range 0.004 < |$z$| < 0.113 and a large stellar mass range 7.5 < log (M ⋆/M⊙) < 11.6. The core data for each galaxy consist of two primary spectral cubes covering the blue and red optical wavelength ranges. For each primary cube, we also provide three spatially binned spectral cubes and a set of standardized aperture spectra. For each core data product, we provide a set of value-added data products. This includes all emission line value-added products from Data Release One, expanded to the larger sample. In addition, we include stellar kinematic and stellar population value-added products derived from absorption line measurements. The data are provided online through Australian Astronomical Optics' Data Central. We illustrate the potential of this release by presenting the distribution of |${\sim } 350\, 000$| stellar velocity dispersion measurements from individual spaxels as a function of R / R e, divided in four galaxy mass bins. In the highest stellar mass bin [log (M ⋆/M⊙) > 11], the velocity dispersion strongly increases towards the centre, whereas below log (M ⋆/M⊙) < 10 we find no evidence for a clear increase in the central velocity dispersion. This suggests a transition mass around log (M ⋆/M⊙) ∼ 10 for galaxies with or without a dispersion-dominated bulge. [ABSTRACT FROM AUTHOR]