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tokens: dust and PAH flux might be illumination of nearby cloud material by DoAr 21, rather than material associated with the system in a circumbinary disk distribution. Our results agree that heating of ambient local cloud material is a possible origin for the H 2 seen around DoAr 21. 4.4.4. GG Tau A GG Tau A is a subarcsecond triple system in the Taurus–Aurigae association (ensemble average distance of 140 pc; Table 7 ). It is composed of the M0 primary star GG Tau Aa and the nearly equal-mass Ab1+Ab2 binary (White et al. 1999 ; Di Folco et al. 2014 ). GG Tau A is famous for its spectacular and massive circumsystem ring of material that encompasses the three stars. A distribution of dust has been seen near the north of the stars in the scattered light maps of GG Tau A, revealing that material exists at locations that should be dynamically cleared in this complex multiple system (Krist et al. 2002 ; Duchêne et al. 2004 ). The GG Tau system also includes GG Tau Ba and Bb at a ∼10′′ projected separation to the south (White et al. 1999 ). Thus, GG Tau is a very young quintuple-star system. The GG Tau Bb component has a very late spectral type, making it a likely brown dwarf. The v = 1–0 S (1) line emission was measured in GG Tau A by Bary et al. ( 2003 ) with a flux of 6.9 × 10 −15 erg cm −2 s −1 . They interpreted the mission as arising from gas in the inner disks from one or more of the stars. Beck et al. ( 2012 ) presented the H 2 maps from Figure 4 of this study and showed that the extended H 2 emission is strongest from the northeastern region ∼40 au away from the stars. Since the time of that publication, improved maps of the dust and CO gas from ALMA have revealed that the region of brightest H 2 is colocated with the CO streamer connecting the outer circumsystem disk and the inner distribution of dust (Dutrey et al. 2016 ). This H 2 emission may be excited through stellar heating from the young stars, though the 1700 K LTE gas temperature measured from the H 2 line ratios is high for this distance from the stars. Beck et al. ( 2012 ) postulated that the streamers of gas in H 2 could be excited through shocks associated with infalling accreting material in this dynamically complex young triple. 4.4.5. GM Aur GM Aur is a spectral type K5 star at 158.9 pc distance in the Taurus–Aurigae association (Espaillat et al. 2011 ). It is a system in transition from the CTTS phase with a dense inner disk to the more evolved and X-ray-luminous WTTS phase. GM Aur has a ∼35 au cavity in the optically thick dust in the inner disk, though modeling of its SED and strong mass accretion suggest that gas and small particles persist within this cavity region. The hot inner H 2 disk gas was detected in the UV electronic transitions (France et al. 2012 ), with an emission profile showing an origin within the inner disk region. Our high-resolution spectrum presented in Figure 2 reveals the v = 1–0 S (1) H 2 line emission measured in GM Aur. This served as the basis