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tokens: either because the source istoo faint or, for example, because of non-ideal weather. The flux density scale is set by observations of DR 21. Sources NGC 7027, 3C 274, and 3C 84 are used as secondary calibrators. A detailed description of the data reduction and analysis is given in Teräsranta et al. (1998) . The error estimate in the flux density includes the contribution from the measurement rms and theuncertainty of the absolute calibration. Observation statistics are available in Table A.1 . Columns 1 – 3 give the name and the coordinates of the sources (in J2000). The number of detections and observations at 37 GHz isshown in Col. 4. and the detection percentage in Col. 5. Cols. 6 and 7 give the maximum flux density at 37 GHz and the 1.4 GHz flux density from FIRST. A table containing 37 GHz flux densities and their errors is available at the CDS. Table A.1 Basic data and statistics of the 37 GHz observations. Notes. ( a ) This source has been detected also by LOFAR at a very low frequency of 150 MHz with a flux density of 3.6 mJy. We also performed test observations of a source with a descrepancy in its classification. In Järvelä et al. (2015) J090113.23+465734.7 is listed as radio loud. A search radius of 1 arcmin was used to obtain the radio data, and while there is no detected radio source at the source coordinates (the mean epoch of the FIRST observations is 1997.2), there is a radio source in its close proximity at coordinates RA 09h01m09.225s, Dec +46d57m21.19s. This is MJV 09737, which has no listed redshift or observationsat other wavelengths. Their separation is 0.72 arcmin and it is therefore probable that the radio data in Järvelä et al. (2015) originate in this source, and J090113.23+465734.7 is apparently radio silent. The source has been detected at 37 GHz only once, and the detection raised concern about the possible contamination by MJV 09737 since it also lies within our antenna beam (2.4 arcmin at 37 GHz). The flux density of MJV 09373 at 1.4 GHz is 1.55 mJy and it has not been detected at higher radio frequencies; thus it is likely to be faint at 37 GHz. To ensure this we ran a set of simple tests to check how another radio source lying in the antenna beam might affect our observations, by observing the sources in pairs several times. All observations of MJV 09737 were non-detections so its contributionto 37 GHz observations seems negligible, but this test is not precise enough to certainly rule out possible contamination. Appendix B <italic>Fermi</italic>–LAT data reduction Since the 37 GHz detections suggest the presence of jets, it is possible that these sources are also gamma-ray emitters. Therefore we obtained their Fermi gamma-ray fluxes in the energy range 0.1–300 GeV by analysing the Fermi –LAT data from 2008 August 04 to 2017 August 10 using the Fermi Science Tools 1 version v10r0p5. We applied the data selection recommendation 2 for the Pass 8 data to select events in the source class, while excluding those