ALMA Detection of Extended Millimeter Halos in the HD 32297 and HD 61005 Debris Disks

We present Atacama Large Millimeter/submillimeter Array (ALMA) 1.3 mm (230 GHz) observations of the HD 32297 and HD 61005 debris disks, two of the most iconic debris disks because of their dramatic swept-back wings seen in scattered light images. These observations achieve sensitivities of 14 and 13 mu Jy beam(-1) for HD. 32297 and HD. 61005, respectively, and provide the highest resolution images of these two systems at millimeter wavelengths to date. By adopting a Markov Chain Monte Carlo modeling approach, we determine that both disks are best described by a two-component model consisting of a broad (Delta R/R > 0.4) planetesimal belt with a rising surface density gradient and a steeply falling outer halo aligned with the scattered light disk. The inner and outer edges of the planetesimal belt are located at 78.5 +/- 8.1 au and 122 +/- 3 au for HD 32297, and 41.9 +/- 0.9 au and 67.0 +/- 0.5 au for HD 61005. The halos extend to 440 +/- 32 au and 188 +/- 8 au, respectively. We also detect (CO)-C-12 J = 2-1 gas emission from HD 32297 co-located with the dust continuum. These new ALMA images provide observational evidence that larger, millimeter-sized grains may also populate the extended halos of these two disks previously thought to only be composed of small, micron-sized grains. We discuss the implications of these results for potential shaping and sculpting mechanisms of asymmetric debris disks.