tokens: be coincidental. The small number of galaxies in our sample and the substantial uncertainties on the measurements of the dust mass and gas metallicity preclude us from drawing any solid conclusion regarding a possible physical link between metallicity and circumgalactic dust mass fraction. Our data do not allow us to determine unambiguously the origin of the circumgalactic dust. The best case in our sample for dust entrained in a galactic wind is NGC 1569, but we cannot rule out the possibility that cold dust features that appear to lie in the zone of influence of the galactic wind are instead dust features of external (e.g. tidal) origin in front or behind the wind. Future studies that not only consider the distribution of the circumgalactic dust with respect to the wind and tidal features but also the kinematics of dust tracers such H 2 , CO, Na I D, and H i will help shed light on the origin of this far-flung dust in NGC 1569 and other dwarf galaxies. APPENDIX A: NOTES ON INDIVIDUAL GALAXIES For the discussion in these notes, please refer to Figs 1 (a)–(f) and Figs 2 (a)–(f). He 2-10 : broad cold dust emission regions surround He 2–10 out to ∼1.5 kpc in all SPIRE bands as well as the 160 m PACS map. The 160 m emission map appears similar in extent and morphology to the H i distribution observed by Kobulnicky et al. ( 1995 ). The 70 m PACS map exhibits a bit more anisotropy in its distribution of circumgalactic emission with tapering features extending to the north–northeast, southwest, and east-southeast. The north–northeast feature extends furthest to ∼2.6 kpc. The orientation of these tapering features appears similar to the smaller 0.5 kpc-scale Hα bubbles (Méndez et al. 1999 ; Zastrow et al. 2013 ), but appears less correlated with the shape of the X-ray emission (Kobulnicky Martin 2010 ). Several knots of emission separated from He 2–10 by ∼3–4 kpc to the north-west and southwest in the PACS maps cannot be definitively ruled out as background sources given the signal-to-noise levels or foreground Milky Way dust clouds, but coincident emission in the SPIRE maps seems connected to the disc via colder streams bridging their separation. The most prominent emission in the SPIRE maps towards the knots north-west of the disc seems similarly oriented to an X-ray feature observed by Kobulnicky Martin ( 2010 ). NGC 1569 : a dense complex of filamentary and broad circumgalactic cold dust features stretch out from all along the disc of NGC 1569. The prominent Hα, 8.0, and 24 m filament (Waller 1991 ; Hunter et al. 1993 ; Westmoquette et al. 2008 ; McCormick et al. 2013 ) extending southwest from the western edge of the disc also shows up in the PACS maps, but becomes fainter and disappears in the SPIRE bands. A clump of cold dust directly south of the galactic nucleus resides ∼1.8 kpc from the disc mid-plane and appears to have made a clean break with the other circumgalactic cold dust emission in the PACS maps. Some faint 8.0 m emission
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