GAS AND DUST IN THE PRE-MAIN-SEQUENCE MULTIPLE SYSTEM GG-TAURI

We present 1.4 and 2.7 mm aperture synthesis maps of the gas and dust continuum emission around GG Tauri, a very young component of a pre-ma in-sequence multiple star system; both GG Tau and its apparent compani on, GG Tau/c, at 1500 AU separation, are themselves binaries. At 1.4 m m, dust continuum emission approximately 750 AU in extent is associate d with GG Tau, and a secondary peak is near GG Tau/c. Spectral line im ages in the (1 --> 0) and (2 --> 1) transitions of (CO)-C-13 reveal ga seous structure around GG Tau, elongated along the GG Tau-GG Tau/c axi s (P.A. almost-equal-to 184-degrees). There is some suggestion that th e gas associated with GG Tau/c alone is extended in a different direct ion (P.A. approximately 90-degrees-135-degrees). Marked changes in the morphology and velocity structure of the molecular emission near GG T au/c also indicate that this system is differently oriented. Clumps be tween the two systems may be vestiges of a connecting bar. GG Tau and GG Tau/c appear to have originated in a common cloud; their different systemic orientations suggest that they formed from an initially prola te cloud rather than from an extensive (greater-than-or-equal-to 1500 AU), highly flattened disk.