Low-mass pre-main-sequence stars in Taurus-Auriga

We present vsini measurements of high-resolution infrared and optical spectroscopy for 70 pre-main-sequence stars in the Taurus-Auriga star-forming region, in addition to effective temperatures measured from line-depth ratios, as well as stellar rotation periods determined from optical photometry.

From the literature, we identified the stars in our sample that show evidence of residing in circumstellar disks or multiple systems. The comparison of infrared vsini measurements calculated using two techniques shows a residual scatter of ~1.8km/s, defining a typical error floor for the vsini of pre-main-sequence stars from infrared spectra. A comparison of the vsini distributions of stars with and without companions shows that binaries/multiples typically have a higher measured vsini, which may be caused by contamination by companion lines, shorter disk lifetimes in binary systems, or tidal interactions in hierarchical triples.