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tokens: use for power beaming are in the millimeter band, so are outside the microwave range the Allen Telescope Array observed. Similarly, power beaming using near-IR frequencies would be undetectable by the Boquete observatory. Therefore, the Harp et al. ( 2016 ) and Schuetz et al. ( 2016 ) limited observation times and wavelength coverage are not sufficient to produce firm conclusions on power beaming from KIC 8462852. Most applications would be seen in the radio—if transmissions were oriented in our direction at the proper time and at the frequencies observed—but are not. More extensive observations should be made in more systematic studies of power beaming leakage, including observing at higher radio frequencies and for longer times at visible wavelengths. 5. CONCLUSIONS AND IMPLICATIONS We have listed several classes of power beaming applications/missions, quantifying the principal observable parameters. Applying this reasoning to the recent observations of KIC 8462852, we conclude that if power beaming were in use at the time observed, generally pointed in our direction, and at frequencies between 1 and 10 GHz, that most power beaming applications would have been detectable. The non-detection provides a weak (owing to the caveat of the probabilities listed) rejection of the popular hypothesis that the system is inhabited by an advanced spacefaring extraterrestrial civilization. As discussed above, the beaming power levels are high and transient and easily dwarf any ETI civilization’s diffuse leakage to space (Sullivan et al. 1978 ). Power beaming described here is larger than that necessary for beaming systems for communication: for a 1000 ly range beacon (Benford et al. 2010 ). SETI programs could explore a different part of parameter space by observations suitable to finding leakage from power beams. Such beams would be visible over large interstellar distances. This implies a new approach to the SETI search: instead of focusing on narrowband beacon transmissions generated by another civilization, look for more powerful beams with much wider bandwidth. This requires a new approach for their discovery by telescopes on Earth. Past SETI observations have been in the 1–10 GHz microwave band. For our atmosphere, future observations should look in bands where with lower oxygen and water vapor allow transmission: windows at 35 GHz, 70–115 GHz, 130–170 GHz, and 200–320 GHz. And, of course, such transient sources require longer observing times. A promising avenue is to revisit past observations of transient events, of which there are many, to look for patterns and identify as possible regions of the sky to emphasize. ETIs would know their power beams could be observed. They could put a message on the power beam and broadcast it for our receipt at little additional energy or cost. By observing leakage from power beams, we may well find a message embedded on the beam. That message may use optimized power-efficient designs such as spread spectrum and