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tokens: beam = 058 × 050, PA = 81°; shown in the lower left corner). Contour levels are −3, 3, 5, 7, 9, 11, 13, 15, 17, 19, and 21 times the rms of the map, 19.3 μ Jy beam −1 . (b) Naturally weighted VLA image of the 3.0 cm emission obtained by combining data from A and B configurations (synthesized beam = 039 × 036, PA = 58°; shown in the lower left corner). Contour levels are −3, 3, 5, 7, 9, 11, 13 and 15 times the rms of the map, 2.1 μ Jy beam −1 . An image of the 3.0 cm emission is presented in Figure 2 (b). The emission shows a tripolar structure, suggesting a combination of dust emission from a disk and free–free emission from a monopolar (one-sided) radio jet perpendicular to it. This kind of morphology, with two perpendicular structures, has already been observed in other sources, such as HH 111 (Rodríguez et al. 2014 ) and HH 80–81 (Carrasco-González et al. 2012 ). In both cases, the emission was separated into two components by fitting two Gaussians to it. In the case of GM Aur, we estimate from the SED fit a dust contribution at 3.0 cm of ∼11 μ Jy, which represents only one-eighth of the detected emission at 3.0 cm. In order to check whether this flux density can account for the disk emission of GM Aur at 3.0 cm, we obtained an image of the estimated dust emission at 3.0 cm by scaling the 7 mm image with the dust spectral index obtained from the SED fit. We then subtracted this scaled image to the 3.0 cm image, which was previously convolved to have the same angular resolution as the 7 mm observations. The resulting image still showed significant emission from the disk. By fitting two Gaussians to the remaining 3.0 cm emission, we separated the source into a component with the same PA as the GM Aur disk ( S ν = 31 ± 3 μ Jy), and another one perpendicular to it ( S ν = 45 ± 3 μ Jy) 9 9 We note that none of the fit parameters were fixed and yet two perpendicular components were obtained. (Figure 3 ). We interpret these two components to be tracing the free–free emission from a photoevaporating disk and a radio jet, respectively (see Section 4 ). Figure 3. Superposition of the two components of the free–free emission at 3.0 cm obtained from our two-Gaussian fit (black and white contours) over the 7 mm emission of the transitional disk of GM Aur shown in Figure 2 (a) (color scale). We propose that the disk component (black contours) is produced by the photoevaporative winds arising from the disk, while the perpendicular component (white contours) is tracing the free–free emission from an accretion-driven radio jet. The 3.0 cm image was previously convolved to the same angular resolution (058 × 050, PA = 81°; shown in the lower left corner) as the 7 mm image. Contour levels are −3, 3, 4, 5, 6, 7, and 9 times the rms of the convolved 3.0 cm image, 2.8 μ Jy beam −1 . We also combined our new 5 cm observations with archival data (Table 1 ) to get a sensitive image (rms ≃ 2.5 μ Jy; beam = 053 × 036, PA = −74°). The image shows a compact