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We use deep observations taken with the Photodetector Array Camera andSpectrometer (PACS), on board the Herschel satellite as part of the PACSevolutionary probe (PEP) guaranteed project along with submm ground-basedobservations to measure the dust mass of a sample of high-z submillimetergalaxies (SMGs). We investigate their dust content relative to their stellarand gas masses, and compare them with local star-forming galaxies. High-z SMGsare dust rich, i.e. they have higher dust-to-stellar mass ratios compared tolocal spiral galaxies (by a factor of 30) and also compared to localultraluminous infrared galaxies (ULIRGs, by a factor of 6). This indicates thatthe large masses of gas typically hosted in SMGs have already been highlyenriched with metals and dust. Indeed, for those SMGs whose gas mass ismeasured, we infer dust-to-gas ratios similar or higher than local spirals andULIRGs. However, similarly to other strongly star-forming galaxies in the localUniverse and at high-z, SMGs are characterized by gas metalicities lower (by afactor of a few) than local spirals, as inferred from their optical nebularlines, which are generally ascribed to infall of metal-poor gas. This is incontrast with the large dust content inferred from the far-IR and submm data.In short, the metalicity inferred from the dust mass is much higher (by morethan an order of magnitude) than that inferred from the optical nebular lines.We discuss the possible explanations of this discrepancy and the possibleimplications for the investigation of the metalicity evolution at high-z.

The dust content of high-z submillimeter galaxies revealed by Herschel