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Oblique Shocks at Supernova Remnants in Massive Star Clusters: A Model for the Cosmic-Ray Knee Observed by LHAASO

  • Authors: Luana N. Padilha, R. C. Dos Anjos

Luana N. Padilha and R. C. Dos Anjos 2026 The Astrophysical Journal 1002 .

  • Provider: AAS Journals

Caption: Figure 8.

Corner plots for Models A–D showing the local exploration of parameter space around the best-fit values, weighted by the χ 2 difference. The diagonal panels display 1D posteriors; vertical lines mark the median and the central 68% confidence interval. The off-diagonal panels show joint posteriors with contours at 68% and 95% credibility. Parameters include the wind power P w (in erg s−1), the transport index s, the characteristic shock radius r sh (in pc), the source index α, and, for Model A only, the supernova proximity factor ﹩{n}_{\mathrm{sn}}﹩. The numerical values printed in each panel correspond to the marginalized medians, and the number ﹩{\chi }_{\nu }^{2}﹩ beneath each set summarizes the fit quality for the corresponding model. Angular weights are not shown in this corner plot for clarity; they are presented in Table 3 and discussed in Section 3.2.

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