Dark Matter distinguished by skewed microlensing in the "Dragon Arc"

Microlensed stars recently discovered by JWST & HST follow closely the winding critical curve of A370 along all sections of the ``Dragon Arc" traversed by the critical curve. These transients are fainter than mAB>26.5, corresponding to the Asymptotic Giant Branch (AGB) and microlensed by diffuse cluster stars observed with 18M_/pc², or about 1% of the projected dark matter density. Most microlensed stars appear along the inner edge of the critical curve, following an asymmetric band of width 4kpc that is skewed by -0.7±0.2kpc. Some skewness is expected as the most magnified images should form along the inner edge of the critical curve with negative parity, but the predicted shift is small -0.04kpc and the band of predicted detections is narrow, 1.4kpc. Adding CDM-like dark halos of 10⁶⁻⁸M_ broadens the band as desired but favours detections along the outer edge of the critical curve, in the wrong direction, where sub-halos generate local Einstein rings. Instead, the interference inherent to ``Wave Dark Matter" as a Bose-Einstein condensate (ψDM) forms a symmetric band of critical curves that favours negative parity detections. A de Broglie wavelength of 10pc matches well the observed $4$kpc band of microlenses and predicts negative skewness -0.6kpc, similar to the data. The implied corresponding boson mass is 10⁻²²eV, in good agreement with estimates from dwarf galaxy cores when scaled by momentum. Further JWST imaging may reveal the pattern of critical curves by simply ``joining the dots" between microlensed stars, allowing wave corrugations of ψDM to be distinguished from CDM sub-halos