raw visibility data were calibrated with the MIR reduction package $^{4}$. The passband was flattened using ∼ 1 hour scans of 3c454.3 and the solutions for the antenna-based complex gains were obtained using the primary calibrator 1625-254. These gains, applied to our secondary calibrator, 1626-298, served as a consistency check for the solutions. 

The absolute flux scale was determined through observations of either Callisto or Ceres and is estimated to be accurate to 15%. The flux densities of detected sources were measured by fitting a point source model to the visibility data, while upper limits were derived from the rms of the visibility amplitudes. The rms noise of our SMA observations range from 1.5 to 5 mJy per beam. We detected, at the 3– σ level or better, 5 of our 24 SMA targets: #3, 15, 18, 21, and 32. The 1.3 mm fluxes (and 3-sigma upper limits) for our entire SMA sample are listed in Table 2. 

## 3.1.2. CSO-Bolocam Observations 

Millimeter wavelength observations of 5 of our targets were made with Bolocam 5 at the CSO on Mauna Kea, Hawaii, during June 25 $^{th}$-30$^{th}$, 2009. The observations were performed in the 1.1 mm mode, which has a bandwidth of 45 GHz centered at 268 GHz. Our sources were scanned using a Lissajous pattern providing 10 min of integration time per scan. Between 16 and 40 scans per source were obtained. The weather was clear for the run, with τ$_{225 GHz}$ ranging from 0.05 to 0.1. Several quasars close to the science fields were used as poniting calibrators, while Uranus and Neptune were used as flux calibrators. The data were reduced and the maps from individual scans were coadded using the Bolocam analysis 

