Left panel: comparison between the observed X-ray luminosity (L_X, obs) and the distance from the mass-size relation of LTGs at z ∼ 0.7, for our six starbursts detected in X-rays. Upper limit on L_X, obs for six mid-IR AGNs undetected in X is shown with a black circle, where the horizontal segment represents the range of dist_LTG spanned by this subset. The intrinsic X-ray luminosity due to star-formation is highlighted with a gray line for the median SFR of the sample (±0.4 dex scatter from Mineo et al. 2014), and may dominate the total X-ray observed emission for the X-undetected starbursts. Center panel: X-ray attenuation L_X, obs/L_X, int as a function of the infrared-based attenuation A_V, tot (in a mixed model geometry and toward the center) for our sample of mid-IR detected AGNs. We assumed here a bolometric correction factor L_{X, intr, AGN} = 0.04 × L_BOL, AGN (Vasudevan & Fabian 2007). Stacks on the whole sample and on the X-undetected subset are displayed with hatching circles, while the violet shaded regions indicate the area of no obscuration, which incorporates a factor of two uncertainty in the conversion between intrinsic X-ray and bolometric AGN luminosity. Right panel: same diagram as before, but assuming an L_BOL, AGN- dependent bolometric correction (Lusso et al. 2012), as explained in the text.