We present new observations of the XZ Tau system made at high angular resolution ( 55 milliarcsec ) with the Karl G. Jansky Very Large Array ( VLA ) at a wavelength of 7 mm . Observations of XZ Tau made with the VLA in 2004 appeared to show a triple-star system , with XZ Tau A resolved into two sources , XZ Tau A and XZ Tau C. The angular separation of XZ Tau A and C ( 0.09 arcsec ) suggested a projected orbital separation of around 13 AU with a possible orbital period of around 40 yr. Our follow-up observations were obtained approximately 8 yr later , a fifth of this putative orbital period , and should therefore allow us to constrain the orbital parameters of XZ Tau C , and evaluate the possibility that a recent periastron passage of C coincided with the launch of extended optical outflows from XZ Tau A . Despite improved sensitivity and resolution , as compared with the 2004 observations , we find no evidence of XZ Tau C in our data . Components A and B are detected with a signal-to-noise ratio greater than ten ; their orbital motions are consistent with previous studies of the system , although the emission from XZ Tau A appears to be weaker . Three possible interpretations are offered : either XZ Tau C is transiting XZ Tau A , which is broadly consistent with the periastron passage hypothesis , or the emission seen in 2004 was that of a transient , or XZ Tau C does not exist . A fourth interpretation , that XZ Tau C was ejected from the system , is dismissed due to the lack of angular momentum redistribution in the orbits of XZ Tau A and XZ Tau B that would result from such an event . Transients are rare but can not be ruled out in a T Tauri system known to exhibit variable behaviour . Our observations are insufficient to distinguish between the remaining possibilities , at least not until we obtain further VLA observations at a sufficiently later time . A further non-detection would allow us to reject the transit hypothesis , and the periastron passage of XZ Tau C as agent of XZ Tau A ’ s outflows .