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tokens: et al. 2014 )—have positions on the IR CMD consistent with the field locus (e.g., Figure 14 ). Finally, the AB Dor member SDSS J1110+0116 (T5.5; Gagné et al. 2015a ) also coincides with the field locus. Thus, for L/T objects as young as ≈100 Myr, while the temperatures for a given spectral type may be age dependent, the IR absolute magnitudes across the L/T transition do not seem to strongly depend on age. Figure 25. Absolute magnitudes vs. spectral type for our sample with an expanded range of spectral types, in order to highlight the latest-type objects. The L/T objects are shown as green squares, with the measurement errors comparable to the symbol size. Normal field objects (small gray triangles) are the same as in Figure 12 . The thick black lines are the polynomial fits from Dupuy Liu ( 2012 ), and the gray region shows the rms about the fits. See Figure 6 caption for further details. The two latest-type red objects in our sample, WISE J0206+2640 (L9 (red)) and WISE J0754+7909 (T2p (red)), may be illuminating landmarks for the transition. Their spectra are unusual compared to most field objects of similar type, especially WISE J0754+7909 (see details in Appendix ). And yet their absolute magnitudes are largely consistent with field objects, with the largest discrepancy being WISE J0206+2640 having ≈0.5 mag fainter magnitudes at Y and J bands compared to the field. Even given its very peculiar spectrum, WISE J0754+7909 has absolute magnitudes and color–magnitude positions in accord with the field. Thus, while the spectral peculiarities of these two objects may not be due to low gravity (indeed both have old field kinematics; Table 15 ), their consistency with field objects may be circumstantial evidence that the IR magnitudes of the L/T transition are robust over a range of physical properties. One interesting question that we can address is whether the J -band flux reversal that is a hallmark of L/T transition binaries in the field population (e.g., Liu et al. 2006 ) would appear different at lower gravities. The most extreme such flux-reversal binaries known are 2MASS J1404−3159AB (Δ J = −0.54 ± 0.08 mag, Δ K = 1.33 ± 0.05 mag; Looper et al. 2008a ) and SDSS J1052+4422AB (Δ J = −0.45 ± 0.09 mag, Δ K = 0.52 ± 0.05 mag; Dupuy et al. 2015 ). SDSS J1052+4422AB has a very precise evolutionary-model-based age derived from its dynamical masses and luminosities, clearly demonstrating that it is field age and gravity ( Gyr and = 5.0–5.2 dex; Dupuy et al. 2015 ). Now that we have parallaxes for members of YMGs that span the L/T transition, we can imagine hypothetical L/T transition binaries composed of these coeval objects. For example, if the AB Dor members WISEP J0047+6803 (L7 int-g ) and SDSS J1110+0116 (T5.5) were paired together in a binary, they would have Δ J = −0.37 ± 0.11 mag, Δ K = 2.04 ± 0.09 mag. If the primary were instead 2MASS J2244+2043 (L6 vl-g ), the flux ratios would be Δ J = −0.47 ± 0.09 mag, Δ K = 1.89 ±0.09 mag. Thus, it