Infrared images through the filter K (9#9=2.10 10#10, width=0.34 10#10) were taken with the MAGIC camera attached to the Cassegrain focus of the 3.5m telescope at the German-Spanish Observatory in Calar Alto on 1996 September 26. The detector was a Rockwell 25611#11pixel NICMOS3 array, and the camera was set up in the high resolution mode of the f/10 focus, giving a sampling of 0.32 arcsec/pixel and a field of view of 827#782. The observation procedure consisted in 312#12 mosaic patterns of the object and nearby sky, alternating the exposures. The mosaic on the galaxy has a 90% overlap between the component tiles. During the observations, the seeing was 1.0 arcsec and the conditions photometric. Each galaxy frame was subtracted from a median sky frame and divided by the flat field. The nine frames were recentered using two or three field point sources and the nucleus, and subsequently they were median averaged. The flux calibration was performed with observations of the Kitt Peak faint standard stars numbers 30, 31 and 32. NGC 6951 was observed on 1996 September 30, as one of the targets of the BARS collaboration, through the filters J and Kshort ( Ks) with the ARcetry Near-Infrared CAmera, ARNICA, attached to the 2.56m Nordic Optical Telescope in La Palma. ARNICA uses a NICMOS3 array that gives a pixel scale of 0.51 arcsec/pixel and a field of view of 1307#7130. We integrated 40 seconds on the object (dithered in 11 positions) and the same time on the sky, for a total integration time on the object of 440 s in J and 880 s in Ks (with a 10 shift between the different images to facilitate bad pixel removal). Since the size of the galaxy is much larger than the field of view, we repeated the process four times, with the central region of NGC 6951 in common, placed in one of the corners. This allowed us to obtain a final mosaic image with a total integration time of 1760 s in J (3520 s in Ks) in the central 2 and 440 s in J (880 s in Ks) in the rest. Flat-field frames were obtained from the median of the sky frames taken along the night. Sky-subtracted and flat-fielded images were then aligned by using a number of foreground stars. We observed 4 standard stars for the flux calibration, leading to a photometric accuracy of 10%. For all the reduction and calibration steps we used the package sqiid within IRAF. We measure a FWHM for the stars in the final mosaic of 1.3. The 38#8 limiting magnitudes are 18.8 in J and 19.5 in Ks.