A Misaligned Debris Disk relative to the Host Star CPD-72 2713 from JWST/NIRCam Imaging

Observations of debris disks provide a valuable window to investigate the formation and evolution of planetary systems. We present high-contrast JWST/NIRCam observations of CPD-72 2713, a 24 Myr-old star that belongs to the $\beta$ Pic moving group. We obtained the first scattered-light images of the disk in both F210M and F444W filters, revealing a nearly face-on orientation. Forward modeling yields disk radii of $55.4_{-3.2}^{+3.0}\mathrm{A}\mathrm{U}$ (F210M) and $39.1_{-2.6}^{+4.6}\mathrm{A}\mathrm{U}$ (F444W), both significantly smaller than the thermal emission radii measured with ALMA and Herschel/PACS. This discrepancy suggests that scattered light traces the inner region of the disk while thermal emission probes the outer regions. Combining the stellar rotation period ($4.47\pm 0.67$ days) from TESS light curves and spectroscopic $v\sin i_{\ast }$, we constrained the stellar inclination to ${47}^{\circ }\mathrm{.}{2}_{-7.7}^{+11.1}$ ($1\sigma$). The minimum star-disk mutual inclinations are ${27}^{\circ }\mathrm{.}{6}_{-8.2}^{+11.5}(1\sigma )$ from F210M data and ${27}^{\circ }\mathrm{.}{3}_{-10.9}^{+12.5}(1\sigma )$ in F444W data. We find that the minimum star–disk mutual inclination exceeds ${10}^{\circ }$ at the $95\mathrm{\%}$ credible level in both F210M and F444W, suggesting a misalignment between the scattered-light disk and the stellar equatorial plane. We note that variation among published disk inclination measurements and potential systematic uncertainties may affect this probability. With JWST high-contrast imaging, we rule out planets down to $0.3{\mathrm{M}}_{\mathrm{J}}$ at ${0.5}^{\mathrm{\prime }\mathrm{\prime }}$ and beyond, disfavoring a planet as the driver of the star-disk misalignment.