Zoom-in on the star-forming region of SpARCS1049+56, labeled as S2 in Figure 3. Left (a): composite HST image (F105W in blue and green; F160W in red), highlighting the BCG and the star-forming tidal-like tail. Overlaid yellow contours represent the Spitzer 24 μm emission from T. Webb et al. (2015a) at 2σ_rms, 3σ_rms, 4σ_rms, and 5σ_rms. The centroid of the MIPS emission is highlighted, and the emission appears slightly extended along the star-forming tail. Middle left (b): 144 MHz LOFAR 6″ image with a beam of 6﹩\mathop{.}\limits^{\unicode{x02033}}﹩0 × 6﹩\mathop{.}\limits^{\unicode{x02033}}﹩0. Contours are 4σ_rms, 6σ_rms, 8σ_rms, and 10σ_rms, where σ_rms = 33 μJy beam⁻¹. The centroid of the MIPS emission coincides with the peak of the radio emission (labeled S2 in Figure 3). Middle right (c): 144 MHz LOFAR image obtained with the International LOFAR Telescope, with a beam of 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩39 × 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩22, using the same low-resolution contours as in the middle-left panel. No source is detected, indicating that the LOFAR emission in the middle-left panel is of diffuse origin. Right (d): JVLA 1.5 GHz image from A. Trudeau et al. (2019), with contours at 3σ_rms, 4σ_rms, and 5σ_rms, where σ_rms = 10.5 μJy beam⁻¹. Color bars are included; radio image units are Jy beam⁻¹.