English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

Abridged: We measured photometric and spectroscopic $P_{\rm rot}$ for a largesample of nearby bright M dwarfs with spectral types from M0 to M9, as part ofour continual effort to fully characterize the Guaranteed Time Observationprogramme stars of the CARMENES survey. We determine $P_{\rm rot}$ for 129stars. Combined with the literature, we tabulate $P_{\rm rot}$ for 261 stars,or 75% of our sample. We evaluate the plausibility of all periods available forthis sample by comparing them with activity signatures and checking forconsistency between multiple measurements. We find that 166 of these stars haveindependent evidence that confirmed their $P_{\rm rot}$. There areinconsistencies in 27 periods, which we classify as debated. A further 68periods are identified as provisional detections that could benefit fromindependent verification. We provide an empirical relation for the $P_{\rmrot}$ uncertainty as a function of the $P_{\rm rot}$ value, based on thedispersion of the measurements. We show that published formal errors seem to beoften underestimated for periods $\gtrsim 10$ d. We highlight the importance ofindependent verification on $P_{\rm rot}$ measurements, especially for inactiveM dwarfs. We examine rotation-activity relations with emission in X-rays,H$\alpha$, Ca II H & K, and surface magnetic field strengths. We find overallagreement with previous works, as well as tentative differences in thepartially versus fully convective subsamples. We show $P_{\rm rot}$ as afunction of stellar mass, age, and galactic kinematics. With the notableexception of three transiting planet systems and TZ Ari, all known planet hostsin this sample have $P_{\rm rot} \gtrsim 15$ d. This indicates that importantlimitations need to be overcome before the radial velocity technique can beroutinely used to detect and study planets around young and active stars.

CARMENES input catalog of M dwarfs: VII. New rotation periods for the survey stars and their correlations with stellar activity