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Observations at 14.2 to 17.9 GHz made with the Arcminute Microkelvin Imager (AMI) Small Array towards 14 Lynds dark nebulae with a resolution of ≈2 arcmin are reported. These sources are selected from the Submillimetre Common‐User Bolometre Array (SCUBA) observations of Visser, Richer &amp; Chandler as small angular diameter clouds well matched to the synthesized beam of the AMI Small Array. Comparison of the AMI observations with radio observations at lower frequencies with matched  uv ‐plane coverage is made, in order to search for any anomalous excess emission which can be attributed to spinning dust. Possible emission from spinning dust is identified as a source within a 2‐arcmin radius of the SCUBA position of the Lynds dark nebula, exhibiting an excess with respect to lower frequency radio emission. We find five sources which show a possible spinning dust component in their spectra. These sources have rising spectral indices in the frequency range 14.2–17.9 GHz with  α 17.9  14.2 =−0.7 ± 0.7  to  −2.9 ± 0.4 , where   S ∝ν −α  . Of these five one has already been reported, L1111, we report one new definite detection, L675 (16σ), and three new probable detections (L944, L1103 and L1246). The relative certainty of these detections is assessed on the basis of three criteria: the extent of the emission, the coincidence of the emission with the SCUBA position and the likelihood of alternative explanations for the excess. Extended microwave emission makes the likelihood of the anomalous emission arising as a consequence of a radio counterpart to a protostar or a protoplanetary disc unlikely. We use a 2‐arcmin radius in order to be consistent with the  IRAS  identifications of dark nebulae, and our third criterion is used in the case of L1103 where a high flux density at 850 μm relative to the far‐infrared data suggests a more complicated emission spectrum.

AMI observations of Lynds dark nebulae: further evidence for anomalous cm‐wave emission ★