ERRATUM 2: "A SENSITIVE IDENTIFICATION OF WARM DEBRIS DISKS IN THE SOLAR NEIGHBORHOOD THROUGH PRECISE CALIBRATION OF SATURATED WISE PHOTOMETRY" (2014, ApJS, 212, 10)

Five stars were erroneously identified as infrared excess sources at $12\;\mu {\rm{m}}$ and $22\;\mu {\rm{m}}$. The new excess associated with HIP 85523 was overestimated because its ${B}_{T}-{V}_{T}$ color was corrected according to empirical tables based on its Hipparcos spectral type of K7. Multiple references however have confirmed its spectral type to be M2.5/3 V (e.g., Riaz et al. 2006; Cushing et al. 2006; Torres et al. 2006). Therefore our photospheric color was underestimated, and the excess was overestimated. The W4 photometry for HIP 69281 is likely contaminated by nearby projected companions with a similar assessment provided by Wu et al. (2013). HIP 32435 is likely contaminated by a star ∼15'' away and a galaxy that is 25'' away, as noted by Donaldson et al. (2012). HIP 106914 might be a false-positive star based on MIPS 24 μm measurements reported in Moór et al. (2011), and the presence of a bright nearby source seen in MIPS 70 μm images. HIP 69682 was reported to have an excess at 60 μm by Rhee et al. (2007), and identified by us as a W4 excess. However, the presence of a red companion 214 from the primary is likely responsible for the 60 μm excess, as the two would be blended in the 60'' IRAS beam. We remove HIP 69682 from our list of excesses as the PSF tail of the red companion is also most likely responsible for the W4 excess flux of HIP 69682.

The above reduction brings the total number of detected excesses to 209 instead of 214, and the total number of new 10–30 μm excesses to 113 instead of 116. Our tally of new excesses constitutes a 25% increase in the census of debris disks within 75 pc and a 35% increase of debris disks with 10–30 μm excesses within this volume.

In Section 4.4, we discuss the state of circumbinary dust in 26 binary systems. Several of these systems were erroneously identified as binary systems. We have removed HIP 544, HIP 1481, HIP 2472, HIP 61960, HIP 95261, and HIP 115738 from our list of binaries. In addition, we have revised Table 8, the entries in which were inadvertently scrambled during submission. The new Table 8 reflects the true characteristics of these binary excess hosts.

The overall scientific conclusions in the original manuscript are unaffected by the changes reported here.