This dataset describes candidate signal detections obtained at the Green Bank Telescope in 2016 and reprocessed with the 2020 UCLA SETI Group data processing pipeline. Analysis of Kepler mission data suggests that the Milky Way includes billions of Earth-sized planets in the habitable zone of their host stars. Current technology enables the detection of technosignatures emitted from a large fraction of the Galaxy. We describe a search for technosignatures that is sensitive to Arecibo-class transmitters located within ∼420 ly of Earth and transmitters that are 1000 times more effective than Arecibo within ∼13000 ly of Earth. Our observations focused on 14 planetary systems in the Kepler field and used the L-band receiver (1.15–1.73 GHz) of the 100 m diameter Green Bank Telescope. Each source was observed for a total integration time of 5 minutes. We obtained power spectra at a frequency resolution of 3 Hz and examined narrowband signals with Doppler drift rates between ±9 Hz s −1 . We flagged any detection with a signal-to-noise ratio in excess of 10 as a candidate signal and identified approximately 850,000 candidates. Most (99%) of these candidate signals were automatically classified as human-generated radio-frequency interference (RFI). A large fraction (>99%) of the remaining candidate signals were also flagged as anthropogenic RFI because they have frequencies that overlap those used by global navigation satellite systems, satellite downlinks, or other interferers detected in heavily polluted regions of the spectrum. All 19 remaining candidate signals were scrutinized and none were attributable to an extraterrestrial source.

The field descriptions are as follows: ID: a unique integer identifier for the signal NAME: the name of the source SCAN: the scan index number (1, 2) for the source MJD: the Modified Julian Date at the start of the scan FREQ: the frequency (Hz) at the start of the scan DFDT: the rate of change in frequency (Hz/s) Z: the signal power integrated over the scan duration aka Z score (standard deviations of the noise) BW: an estimate of the bandwidth (FWHM) of the signal (Hz) FSNR: a flag set to Y if signal power exceeds detection threshold FDOP: a flag set to Y if DFDT is not zero FBTH: a flag set to Y if signal is detected in both scans of this source FOTH: a flag set to Y if signal is not detected in scans of other sources FAND: a flag set to Y if FSNR=FDOP=FBTH=FOTH=Y PARTNER: the ID of the signal in a subsequent scan of this source, if known RFICODE: an identifier for the probable source of RFI NOTES: additional notes The field names and types are as follows: +---------+--------------+ | Field | Type | +---------+--------------+ | ID | int(11) | | NAME | varchar(50) | | SCAN | int(4) | | MJD | double(16,8) | | FREQ | double(20,6) | | DFDT | double(14,8) | | Z | double(15,3) | | BW | double(8,1) | | FSNR | char(1) | | FDOP | char(1) | | FBTH | char(1) | | FOTH | char(1) | | FAND | char(1) | | PARTNER | int(11) | | RFICODE | char(5) | | NOTES | text | +---------+--------------+

Please see journal article for methods.