High-resolution spectra of Late-type stars

We performed spectroscopic observations with echelle spectrographs to cover the entirety of the optical spectral range simultaneously. Standard data reduction was performed with the IRAF echelle package. We applied the spectral subtraction technique to reveal chromospheric emission in the stars of the sample.

The equivalent width of chromospheric emission lines was measured in the subtracted spectra and then converted to fluxes using equivalent width--flux relationships. Radial and rotational velocities were determined by the cross-correlation technique. Kinematics, equivalent widths of the lithium line 6707.8{AA} and spectral types were also determined.

• Results: A catalog of spectroscopic data is compiled: radial and rotational velocities, space motion, equivalent widths of optical chromospheric activity indicators from Ca II H & K to the calcium infrared triplet and the lithium line in 6708{AA}. Fluxes in the chromospheric emission lines and R'_HK are also determined for each observation of star in the sample. We used these data to investigate the emission levels of our stars. The study of the H{alpha} emission line revealed the presence of two different populations of chromospheric emitters in the sample, clearly separated in the log(F_H{alpha}_/F_bol_)-(V-J) diagram. The dichotomy may be associated with the age of the stars.