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Dense aperture arrays provide key benefits in modern astrophysical research.They are flexible, employing cheap receivers, while relying on the ever moresophisticated compute back-end to deal with the complexities of signalprocessing required for optimal use. Their advantage is that they offer verylarge fields of view and are readily scalable to any size, all other thingsbeing equal. Since they represent "software telescopes", the science casesthese arrays can be applied to are quite broad. Here, we describe thecalibration and performance of the AARTFAAC-12 instrument, which is composed ofthe twelve centrally located stations of the LOFAR array. We go into thedetails of the data acquisition and pre-processing, we describe the newlydeveloped calibration pipeline as well as the noise properties of the resultingimages and present radio source counts at 41.7 MHz and 61 MHz. We find thatAARTFAAC-12 is confusion limited at 0.9 Jy/PSF at 61 MHz with a PSF size of17'x11' and that the normalized source counts agree with the scaled VLSSr and6C survey counts. The median spectral index of the sources between the twofrequencies we observed at is -0.78. Further, we have used the derived sourcecounts to estimate any excess cosmic radio background, and we do not findevidence for it at our observing frequencies compared to published literaturevalues.

Characterization of the AARTFAAC-12 aperture array: radio source counts at 42 and 61 MHz