tokens: constraints and verification of the TeV emission mechanism in 30 Dor C. Hadronic and leptonic mechanisms predict different flux for the (10 GeV–1 TeV) band, both currently below Fermi -LAT ( Atwood et al. 2009 ; Ackermann et al. 2011 ) sensitivity and between Fermi and H.E.S.S. covered energy ranges, but within the capabilities of C.T.A. An example of the prospects of C.T.A. in this regard is shown by Acero et al. (2017b ) as applied to the SNR RX J1713.7–3946. The recent H.E.S.S. paper on RX J1713-3946 ( H.E.S.S. Collaboration 2018 ) demonstrates the possibilities for C.T.A. observations of LMC objects. H.E.S.S. revealed the TeV shell of RX J1713.7–3946 in unprecedented detail, and was found to extend further than the X-ray shell. This allowed the probing of particle escape, while the GeV and TeV spectra were covered to a level of accuracy that allowed a very detailed comparison of leptonic and hadronic emission mechanisms, including a magnetic field map for the leptonic case. 5 Conclusion We have presented an analysis of new Chandra observations of 30 Dor C in the Large Magellanic Cloud, the first superbubble detected in TeV γ -rays. These observations provided the sharpest view of the synchrotron X-ray shell of 30 Dor C, allowing us to perform a detailed morphological study and estimate the B -field in the superbubble, a key discriminator in assessing the dominant TeV γ -ray emission mechanism with a low B -field ~ 15 μ G required for a purely leptonic origin, a B -field of ≳ 50 μ G for a completely hadronic-dominated origin, or B -field of ~ 20 μ G for a 50–50 contribution of the leptonic and hadronic mechanisms to the TeV γ -rays. Using the new Chandra data, MCELS2 H α , and 6 cm radio continuum images we found an anti-correlation between the synchrotron X-ray and H α /6 cm shells. In addition, we discussed how long-slit spectroscopy of various regions of the 30 Dor C shell has shown no evidence of the high velocities necessary to explain the synchrotron X-rays (≳ 3000 km s −1 ). Rather the H α expansion velocities are more typical of an expanding superbubble ( 100 km s −1 ). We suggested that the SNR responsible for the synchrotron X-rays has reached the 30 Dor C supershell and has stalled in some regions, but continues through gaps in the shell in others. This is similar to the observed anti-correlation seen in RCW 86 ( Vink et al. 2006 ; Helder et al. 2013 ), which is attributed to the SNR evolving into a wind-blown cavity and encountering density gradients, though the velocity differences between synchrotron X-ray and H α shells are not as extreme. This may be a result of more pronounced density gradients and/or the fact that the shock radius is so much larger in 30 Dor C, meaning the shock energy has been distributed over a large area, making it more sensitive to these density gradients. We estimated the downstream B -field from the synchrotron X-ray shell. This was achieved by fitting the observed radial profile in sectors around 30
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