  We present SCExAO/CHARIS 1.1--2.4 micron integral field direct spectroscopy
of the young HIP 79124 triple system. HIP 79124 is a member of the
Scorpius-Centaurus association, consisting of an A0V primary with two low-mass
companions at a projected separation of <1 arcsecond. Thanks to the high
quality wavefront corrections provided by SCExAO, both companions are
decisively detected without the employment of any PSF-subtraction algorithm to
eliminate quasi-static noise. The spectrum of the outer C object is very well
matched by Upper Scorpius M4 pm 0.5 standard spectra, with a Teff = 2945 pm 100
and a mass of 350 MJup. HIP 79124 B is detected at a separation of only 180 mas
in a highly-correlated noise regime, and it falls in the spectral range M6 pm
0.5 with Teff = 2840 pm 190 and 100 MJup. Previous studies of stellar
populations in Sco-Cen have highlighted a discrepancy in isochronal ages
between the lower-mass and higher-mass populations. This could be explained
either by an age spread in the region, or by conventional isochronal models
failing to reproduce the evolution of low-mass stars. The HIP 79124 system
should be coeval, and therefore it provides an ideal laboratory to test these
scenarios. We place the three components in a color-magnitude diagram and find
that 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 of
magnetic effects in conventional isochronal models inhibit them from
reproducing early low-mass stellar evolution, which is further supported by the
fact that new models that include such effects provide more consistent ages in
the HIP 79124 system.
