Testing the class-dependent suppression hypothesis for YSO radio emission

Test whether the lower radio detectability of class II Taurus–Auriga young stellar objects relative to class III objects is caused by obscuration of non-thermal stellar emission by optically thick circumstellar material, by establishing the radio emission mechanisms operating across the full sample.

Background

The analysis shows class III YSOs have a significantly higher 3 GHz detection fraction than class II YSOs, consistent with prior VLA surveys. A proposed interpretation is that optically thick material in class II systems may suppress or obscure radio emission from stellar magnetic activity, while class III systems, being disk dispersed, allow emission to emerge unimpeded.

However, without multi-frequency or polarization data to diagnose mechanisms, this hypothesis cannot be tested with current VLASS Quick Look data.