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We present SCExAO/CHARIS 1.1--2.4 micron integral field direct spectroscopyof the young HIP 79124 triple system. HIP 79124 is a member of theScorpius-Centaurus association, consisting of an A0V primary with two low-masscompanions at a projected separation of <1 arcsecond. Thanks to the highquality wavefront corrections provided by SCExAO, both companions aredecisively detected without the employment of any PSF-subtraction algorithm toeliminate quasi-static noise. The spectrum of the outer C object is very wellmatched by Upper Scorpius M4 pm 0.5 standard spectra, with a Teff = 2945 pm 100and a mass of 350 MJup. HIP 79124 B is detected at a separation of only 180 masin a highly-correlated noise regime, and it falls in the spectral range M6 pm0.5 with Teff = 2840 pm 190 and 100 MJup. Previous studies of stellarpopulations in Sco-Cen have highlighted a discrepancy in isochronal agesbetween the lower-mass and higher-mass populations. This could be explainedeither by an age spread in the region, or by conventional isochronal modelsfailing to reproduce the evolution of low-mass stars. The HIP 79124 systemshould be coeval, and therefore it provides an ideal laboratory to test thesescenarios. We place the three components in a color-magnitude diagram and findthat the models predict a younger age for the two low-mass companions (3 Myr)than for the primary star (6 Myr). These results imply that the omission ofmagnetic effects in conventional isochronal models inhibit them fromreproducing early low-mass stellar evolution, which is further supported by thefact that new models that include such effects provide more consistent ages inthe HIP 79124 system.

Isochronal age-mass discrepancy of young stars: SCExAO/CHARIS integral field spectroscopy of the HIP 79124 triple system