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We present Atacama Large Millimeter/submillimeter Array (ALMA) Cycle 0 Band 7observations of an extremely metal-poor dwarf starburst galaxy in the LocalUniverse, SBS0335-052 (12+log(O/H)~7.2). With these observations, dust isdetected at 870micron (ALMA Band 7), but 87% of the flux in this band is due tofree-free emission from the starburst. We have compiled a spectral energydistribution (SED) of SBS0335-052 that spans almost 6 orders of magnitude inwavelength and fit it with a spherical dust shell heated by a single-agestellar population; the best-fit model gives a dust mass of (3.8+/-0.6)x10^4Msun. We have also constructed a SED including Herschel archival data forIZw18, another low-metallicity dwarf starburst (12+log(O/H)=7.17), and fit itwith a similar model to obtain a dust mass of (3.4+/-1.0)x10^2 Msun. Comparedwith their atomic gas mass, the dust mass of SBS0335-052 far exceeds theprediction of a linear trend of dust-to-gas mass ratio with metallicity, whileIZw18 falls far below. We use gas scaling relations to assess a putativemissing gas component in both galaxies and find that the missing, possiblymolecular, gas in SBS0335-052 is a factor of 6 times higher than the valueinferred from the observed HI column density; in IZw18 the missing component is4 times smaller. Ultimately, despite their similarly low metallicity, thedifferences in gas and dust column densities in SBS0335-052 and IZw18 suggestthat metal abundance does not uniquely define star-formation processes. At somelevel, self-shielding and the survival of molecules may depend just as much ongas and dust column density as on metallicity. The effects of low metallicitymay at least be partially compensated for by large column densities in theinterstellar medium.

ALMA observations of cool dust in a low-metallicity starburst, SBS0335-052