tokens: part of the GAMA survey. This provides the substantial advantage of deep and complete spectroscopic coverage to select targets and define environment. The GAMA regions also contain excellent photometric data across 21 bands from ultraviolet to far-infrared (Driver et al. 2016 ). Bryant et al. ( 2015 ) describe the selection of targets in the GAMA regions in detail, but for completeness we outline the selection here. The SAMI Galaxy Survey targets in the GAMA regions were selected within three 4 × 12° regions along the equator (Dec. ≃0°), centred at approximate right RA of 9, 12, and 15 h (see Table 1 ). Galaxies were targeted based on cuts in the redshift-stellar mass plane, with a stellar mass proxy that used i -band magnitude and g − i colour (Taylor et al. 2011 ; Bryant et al. 2015 ). Galaxies were selected within a series of four stepped volumes, with higher stellar mass limits at higher redshift (see fig. 4 of Bryant et al. 2015 ). The primary sample is limited to redshift z 0.095. Observations aimed to have high and uniform completeness for this primary sample. A secondary sample was also defined that included high mass galaxies to higher redshift ( z 0.115) and used fainter stellar mass limits. As the secondary targets were observed at lower priority, these are less complete (see Table 1 ). Fig. 1 shows the distribution of primary (observed: red, unobserved: blue) and secondary targets (observed: magenta, unobserved: cyan) in redshift and RA. A set of filler galaxies, at lower priority that the secondary targets, was also defined. These are discussed in Section 2.1.3 . Figure 1. The distribution of SAMI galaxies within the three GAMA regions. We show the original GAMA redshift survey (small grey points), observed (red), and unobserved (blue) primary SAMI galaxies, observed (magenta) and unobserved (cyan) secondary SAMI galaxies. Table 1. The coordinates and number of objects in the GAMA regions. For each region, we list the RA and declination (Dec.). For both the primary and secondary samples, we list the number of observed galaxies N obs , the number of good targets N good (i.e. those not flagged as bad for photometric reasons such as a bright star in the field of view) and the number of all targets N all (including objects with bad flags). The listed completeness for the primary sample is N obs / N good . Each potential target was visually checked to identify problems, such as bright nearby stars or sources being a sub-component of a larger galaxy. These were flagged within the input catalogue and their priority set so that they were not observed. The column named BAD_CLASS in the input catalogue (named InputCatGAMADR3) contains flags for different types of problem sources. A full description of the flags is given by Bryant et al. ( 2015 ). A small subset of the sources required adjustment of the coordinates for targeting (0.6 per cent of the input catalogue). This was typically in order to place an asymmetric galaxy or a close pair
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