1 INTRODUCTION

2 THE UPGRADED SAMI INSTRUMENT
2.1 New hexabundle connectors
2.2 Improved throughput

3 SCIENCE DRIVERS INFLUENCING THE TARGET SELECTION

4 SCIENCE CONSTRAINTS ON THE TARGET SELECTION TO MEET THE SCIENCE DRIVERS
4.1 Redshift range
4.2 Stellar mass or absolute magnitude selection

5 FINAL SELECTION OF NON-CLUSTER GALAXIES
5.1 The GAMA survey
5.2 Limits for the stellar mass selection
5.3 Selection of SAMI targets from the GAMA-I survey
5.4 Galaxy sizes and surface brightness distributions
5.5 Data quality at the extremes of our selection
5.6 Comparison to previous IFU surveys

6 FINAL SELECTION: CLUSTER GALAXIES
6.1 Selection of clusters and cluster galaxies

7 COMBINED FIELD AND CLUSTER SAMPLE PROPERTIES
7.1 Sky coverage
7.2 Group and cluster masses
7.3 Galaxy stellar masses
7.4 Colours and magnitudes

8 ANCILLARY DATA FROM OTHER SURVEYS
8.1 UV, optical and infrared
8.2 Radio data

9 SAMI GALAXY SURVEY OBSERVING PROGRAM
9.1 Flux calibrators and guide stars
9.2 Optimal tiling of the SAMI fields, and plate production

10 SUMMARY