Abstract
We derive characteristic properties of the nonrandom spatial distribution of pre-main-sequence stars in the Taurus-Auriga molecular cloud by applying several different statistical techniques. We find that a power-law form for the two-point angular correlation function (with index −1.2) reproduces the overall shape of the actual pre-main-sequence distribution in Taurus at small angular scales (∼0.3°). This result is consistent with the existence of real clustering in the T Tauri distribution. With the aid of the nearest-neighbor distribution technique, we determine a median projected separation of −0.3 pc for young stars in this cloud, even after eliminating close pairs with separations less than 20″ (−3000 AU at the distance of Taurus) from our sample
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