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tokens: a low-order tunable filter will be described. We present Fabry–Perot data cubes for the large-diameter expanding structures around a giant H ii region, the centre of the 30 Doradus starburst (or 30 Doradus giant star-forming region), also called the Tarantula Nebula, in the Large Magellanic Cloud (LMC). The study of shells and bubbles, due to stellar winds and supernova explosions, within giant H ii regions is crucial for understanding the processes of mass and energy transfer from the stellar component to the interstellar medium and the processes of triggering of star formation. Although kinematic studies of supergiant shells and superbubbles in giant H ii regions are common in the literature, carried out both with long-slit and, more recently, with 3D spectroscopy, they have not had the necessary coverage and spatial resolution to answer a few key questions. Even the origin of the supersonic motions present in these regions is still a matter of debate (Melnick et al. 1999 ). Moreover, it is still not understood if the kinematics of giant H ii regions are due to an underlying diffuse component or to superposed multiple kinematic components. Having high spatial and spectral resolution velocity maps, as those delivered by SAM-FP, is crucial to tackle these problems. A few authors have studied the kinematics of the ionized gas in the 30 Doradus nebula, e.g. Chu Kennicutt ( 1994 ), Melnick et al. ( 1999 ), Redman et al. ( 2003 ), Torres-Flores et al. ( 2013 ), and references therein. All of these studies reported broad and possibly multiple components widespread in the nebula, which indicate a complex structure. These studies were either performed (i) with long-slit echelle spectroscopy (e.g. Chu Kennicutt 1994 ; Melnick et al. 1999 ), probing motions and physical conditions in small (parsec) and larger (tens of parsecs) scales but covering only a limited number of lines of sight; or (ii) with fibres, as the work of Torres-Flores et al. ( 2013 ), with a somewhat larger field of view, but probing the nebula in a sparse manner (every 5 × 5 pc 2 , with a filling factor of 0.0028). The advantage of this study is that it combines 3D spectroscopy information with continuous coverage of the field over a fairly large field of view, with a pixel size (binned 4 × 4) of 0.18 × 0.18 arcsec 2 (or 0.045 × 0.045 pc 2 ). These data show that the kinematic profiles change on scales of a tenth of a parsec over the whole field. The wealth of details seen in Hubble Space Telescope ( HST ) images of nearby giant H ii regions can now be investigated using similar-quality kinematic data taken with SAM-FP with a laser guide star. The main purpose of this paper is to highlight the potential of Fabry–Perot maps obtained with adaptive optics in the study of 30 Doradus and similar giant H ii regions. A high-order Fabry–Perot was used to observe the ionized gas within 30 Doradus, in its strongest optical line: Hα. In Section 2 , we first describe the new mode of SAM with a