$m^2/K$).

This paper presents the first results of SETI at FAST. The FAST SETI instrument was installed by the UC Berkeley SETI group in September 2018, and we have conducted preliminary commensal and targetted observations over the past year. This paper is organized as follows: Section \[sec:2\] describes the commensal observations at FAST and an overview of the SETI analysis pipeline. SERENDIP data acquisition, reduction, and analysis are described in Section \[sec:3\]. Radio frequency interference (RFI) removal is discussed in Section \[sec:4\], and Machine Learning for radio frequency interference (RFI) removal and candidate selection are provided in Section \[sec:5\]. Results is presented in Section \[sec:6\]. Conclusion and Future Plans are in Section \[sec:7\].

Commensal observation for SETI at FAST {#sec:2}
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Radio astronomy is a discipline that relies on observation. However, observing time on large telescopes is typically oversubscribed and often only one source can be observed at a time. To increase sky coverage, commensal observation [@BOWYER1983147] is being increasingly employed. During commensal observation, although the direction of the telescope is determined by the primary observer, secondary observers can receive a copy of the raw data in real time. This is the technique used for SETI at FAST.

The Chinese 