Solar neighborhood activity scatter quantified with magnetic activity in co-eval wide binaries

The magnetic activity of stars in the unsaturated regime is connected to the stellar age, however, the scatter in variability in activity of cool stars in Gyr ages are not well understood. We estimate this scatter by using a sample of 34 same spectral type wide binaries. Archival X-ray data from Chandra and XMM-Newton is used to find the X-ray luminosity (L_X), an indicator of magnetic activity in the stellar Corona. The difference in L_X between the coeval components of the binary gives us the scatter observed in co-eval stars. In the solar neighborhood, we find the scatter in randomly paired same-spectral-type stars within 14pc deviate by more than one sigma when compared to co-eval stars in a wide binary. In addition, despite the low scatter, we also observe a bi-modality in the scatter for M dwarfs in the co-eval sample. As the activity-rotation relations and gyrochronology continue to be calibrated for field stars, volume limited X-ray surveys of stars can also help determine the degree of deviation from coeval behavior in the solar neighbourhood without the need to determine precise ages.