claim a detection, since instrumental artifacts lead to non-Gaussian and/or non-stationary noise in many narrow frequency bands. A variety of veto techniques were used to trim down the initial list of candidates and arrive at a final list of outliers.

Six 0.1 Hz sub-bands (see Table (\[t:BadBands\])) had to be manually aborted in both searches, with a seventh aborted in the July-August search, as even with the threshold in place, they produced an excessive number of candidates. Each of these subbands was compared to records of known noise artifacts and disturbances in the detector, and in each case a known instrumental line was confirmed. These sub-bands were later rerun with the record of candidates disabled in order to produce histograms and loudest-outlier files for upper limit validation.

To protect against spurious noise lines, a second veto based on the $\mathcal{F}$-statistic consistency veto introduced in [@S5Einstein2] was used. This uses the fact that an astrophysical signal should have a higher joint value of $2\mathcal{F}$ (combining data from the two interferometers) than in either interferometer alone. Recorded candidates that violate this inequality were vetoed. This is a simpler version of the more recent line veto [@Keitel2014].

Finally, to enforce coincidence between detectors, 