Fig. 10.
Comparison of stellar masses, radii, and mean densities (in solar units) determined via the seismic scaling relations (Eqs. (1)–(3)) against those from stellar modeling using the SPI pipeline. The biases in the residuals are all consistent with zero (0.09 ± 0.11 M⊙, 0.035 ± 0.045 R⊙, and 0.005 ± 0.042 ρ⊙).
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