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tokens: panels include ellipses representing the 2 fitted disk components to guide the eye. These are drawn at the radial location corresponding to the inner and outer disk radius for disk #1 (thick line) and disk #2 (thin line), as summarized in Table 2 . The right panel ( top ) shows the real part of the visibilities as function of the deprojected baseline for the data (black dots) and the model (red line). The bottom panel shows the residuals. The visibilities are binned in sets of 200. The radial brightness profile for the continuum emission rises monotonically until it peaks at 0.44. After that it decreases and shows a change in slope around 1.15 until it becomes indistinguishable from the background around 1.35, as shown in the bottom left panel of Fig. 5 . The radial brightness distribution of the dust continuum emission between the peak at 0.44 and the outer disk radius at 1.35 can be fitted by two power laws separated at 1.15 with exponents of 6 and 16, respectively. The azimuthal brightness profile for the continuum emission peaks at an azimuth of 135 with a maximum 25% above the median value for the disk and 18 away from the major axis of the disk. To further study the azimuthal structure of the disk we subtract a median radial Gaussian profile from each azimuthal row in the polar projection. We create this average Gaussian by selecting only those radial slices with an integrated value within 1% of the median integrated value over all azimuths (Fig. 6 ). The remaining structure peaks close to the major axis of the disk and is best fit with a 2D Gaussian centered on (radius, azimuth) =(0.43, 18) with a FWHM of 0.15 in radius and 52 in azimuth. This feature is discussed in Sect. 4 . 3.2. CO and HCO<inline-formula specific-use="simple-math"><sup>+</sup></inline-formula> emission We detect spatially and spectrally resolved emission from the 12 CO and HCO + emission lines from the HD 34282 disk. We show the moment maps and line profiles in Figs. 2 and 3 respectively. Fig. 5 ALMA band 7 image reconstructed using superuniform weighting, deprojected using the disk inclination and rotated with the position angle listed in Table 2 to put the major axis of the disk at 0 (north; bottom right panel ), converted to polar coordinates ( top left panel ). This polar map is collapsed along the radial and azimuthal axes to yield the azimuthal intensity distribution ( top right ) and the radial intensity distribution ( bottom left ). In this last panel we also show the size of the beam minor and major axis for reference. Fig. 6 Surface brightness of the disk after subtracting a Gaussian fit to the median radial profile, shown in polar coordinates with the position angle relative to the major axis of the disk on the -axis and the radial distance from the center on the -axis. Contours of the best-fit 2D Gaussian are show at values of [0.25, 0.5 and 0.75] times its peak value. We estimate the systemic velocity from the 12 CO emission line at km s, based on the