Image Details
Caption: Figure 2.
Wavefield solutions for three specific bands (of width 3.125 MHz) for both of our observations. The color scale corresponds to ﹩{\mathrm{log}}_{10}| W(\tau ,{f}_{D}){| }^{2}﹩ in arbitrary units. One sees that most power is contained within τ ≲ 0.8 ms but that the IRF extends to larger delays, with a faint structure at ∼2.5 ms.
© 2023. The Author(s). Published by the American Astronomical Society.