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The disk around HD 141569 is one of a handful of systems whose weak infraredemission is consistent with a debris disk, but still has a significantreservoir of gas. Here we report spatially resolved mm observations of theCO(3-2) and CO(1-0) emission as seen with the SMA and CARMA. We find that theexcitation temperature for CO is lower than expected from cospatial blackbodygrains, similar to previous observations of analogous systems, and derive a gasmass that lies between that of gas-rich primordial disks and gas-poor debrisdisks. The data also indicate a large inner hole in the CO gas distribution andan outer radius that lies interior to the outer scattered light rings. Thisspatial distribution, with the dust rings just outside the gaseous disk, isconsistent with the expected interactions between gas and dust in an opticallythin disk. This indicates that gas can have a significant effect on thelocation of the dust within debris disks.

Resolved Gas Interior to the Dust Rings of the HD 141569 Disk