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Aims. The brown dwarf (BD) formation process has not yet been completelyunderstood. To shed more light on the differences and similarities between starand BD formation processes, we study and compare the disk fraction among bothkinds of objects over a large angular region in the Taurus cloud. In addition,we examine the spatial distribution of stars and BD relative to the underlyingmolecular gas Methods. In this paper, we present new and updated photometrydata from the Infrared Array Camera (IRAC) aboard the Spitzer Space Telescopeon 43 BDs in the Taurus cloud, and recalculate of the BD disk fraction in thisregion. We also useed recently available CO mm data to study the spatialdistribution of stars and BDs relative to the cloud's molecular gas. Results.We find that the disk fraction among BDs in the Taurus cloud is 41 \pm 12%, avalue statistically consistent with the one among TTS (58 \pm 9%). We find thatBDs in transition from a state where they have a disk to a diskless state arerare, and we study one isolated example of a transitional disk with an innerradius of \approx 0.1 AU (CFHT BD Tau 12, found via its relatively small mid-IRexcess compared to most members of Taurus that have disks. We find that BDs arestatistically found in regions of similar molecular gas surface density tothose associated with stars. Furthermore, we find that the gas column densitydistribution is almost identical for stellar and substellar objects with andwithout disks.

The large-scale disk fraction of brown dwarfs in the Taurus cloud as measured with Spitzer