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A density based hierarchical group-finding algorithm is used to identifystellar halo structures in a catalog of M-giants from the Two Micron All SkySurvey (2MASS). The intrinsic brightness of M-giant stars means that thiscatalog probes deep into the halo where substructures are expected to beabundant and easy to detect. Our analysis reveals 16 structures at highGalactic latitude (greater than 15 degree), of which 10 have been previouslyidentified. Among the six new structures two could plausibly be due to masksapplied to the data, one is associated with a strong extinction region and oneis probably a part of the Monoceros ring. Another one originates at lowlatitudes, suggesting some contamination from disk stars, but also showsprotrusions extending to high latitudes, implying that it could be a realfeature in the stellar halo. The last remaining structure is free from thedefects discussed above and hence is very likely a satellite remnant. Althoughthe extinction in the direction of the structure is very low, the structuredoes match a low temperature feature in the dust maps. While this casts somedoubt on its origin, the low temperature feature could plausibly be due to realdust in the structure itself. The angular position and distance of thisstructure encompass the Pisces overdensity traced by RR Lyraes in Stripe 82 ofthe Sloan Digital Sky Survey (SDSS). However, the 2MASS M-giants indicate thatthe structure is much more extended than what is visible with the SDSS, withthe point of peak density lying just outside Stripe 82. The morphology of thestructure is more like a cloud than a stream and reminiscent of that seen insimulations of satellites disrupting along highly eccentric orbits.

Group finding in the stellar halo using M-giants in 2MASS: An extended view of the Pisces Overdensity?