VizieR Online Data Catalog: Low-mass pre-main-sequence stars in Taurus-Auriga (Nofi+, 2021)

The infrared spectral observations used to measure the Teff and the vsini were obtained using the Immersion GRating INfrared Spectrometer (IGRINS) at both the 2.7m Harlan J. Smith Telescope at McDonald Observatory, and the 4.3m Lowell Discovery Telescope between 2014 October and 2018 March. IGRINS is a high-resolution (R~45000) near-infrared spectrograph with no moving parts that simultaneously records the H and K bands (1.4-2.5um). See Section 2.2.1.

In addition to the infrared spectroscopy, we also obtained optical high-resolution (R~60000) spectra at McDonald Observatory as part of the ongoing search for substellar companions to young stars. Starting in 2004 and continuing to the present time, spectra have been obtained primarily with the McDonald Observatory 2.7m Harlan J. Smith telescope coupled to the Robert G. Tull cross-dispersed coude echelle spectrograph. A smaller number of stars have been observed with the 2.1m Otto Struve telescope coupled to the Sandiford echelle cassegrain spectrometer. See Section 2.2.2.

We obtained ground-based photometry for many of our targets, to determine stellar rotation periods. Our ground-based photometry comes from seasonal V-band monitoring of the sample stars using the Lowell 0.7m robotic telescope. The stars have generally been observed for about ten nights per month from September through March each year since 2012, using CCD differential aperture photometry. Additionally, we obtained rotation periods for several of our sample targets from the K2 long-cadence time-series photometry observed during Campaign 13 between 2017 March 8 and 2017 May 27 UTC. See Section 2.2.3.

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