000133383 001__ 133383 000133383 005__ 20250923084422.0 000133383 0247_ $$2doi$$a10.1051/0004-6361/202346794 000133383 0248_ $$2sideral$$a138078 000133383 037__ $$aART-2024-138078 000133383 041__ $$aeng 000133383 100__ $$aShan, Y. 000133383 245__ $$aCARMENES input catalog of M dwarfs 000133383 260__ $$c2024 000133383 5060_ $$aAccess copy available to the general public$$fUnrestricted 000133383 5203_ $$aAims: Knowledge of rotation periods (Prot) is important for understanding the magnetic activity and angular momentum evolution of late-type stars, as well as for evaluating radial velocity signals of potential exoplanets and identifying false positives. We measured photometric and spectroscopic Prot for a large sample of nearby bright M dwarfs with spectral types from M0 to M9, as part of our continual effort to fully characterize the Guaranteed Time Observation programme stars of the CARMENES survey. Methods: We analyse light curves chiefly from the SuperWASP survey and TESS data. We supplemented these with our own follow-up photometric monitoring programme from ground-based facilities, as well as spectroscopic indicator time series derived directly from the CARMENES spectra. Results: From our own analysis, we determined Prot for 129 stars. Combined with the literature, we tabulated Prot for 261 stars, or 75% of our sample. We developed a framework to evaluate the plausibility of all periods available for this sample by comparing them with activity signatures and checking for consistency between multiple measurements. We find that 166 of these stars have independent evidence that confirmed their Prot. There are inconsistencies in 27 periods, which we classify as debated. A further 68 periods are identified as provisional detections that could benefit from independent verification. We provide an empirical relation for the Prot uncertainty as a function of the Prot value, based on the dispersion of the measurements. We show that published formal errors seem to be often underestimated for periods longwards of ∼10 d. We examined rotation–activity relations with emission in X-rays, Hα, Ca II H&K, and surface magnetic field strengths for this sample of M dwarfs. We find overall agreement with previous works, as well as tentative differences in the partially versus fully convective subsamples. We show Prot as a function of stellar mass, age, and galactic kinematics. With the notable exception of three transiting planet systems and TZ Ari, all known planet hosts in this sample have Prot ≳ 15 d. Conclusions: Inherent challenges in determining accurate and precise stellar Prot means independent verification is important, especially for inactive M dwarfs. Evidence of potential mass dependence in activity–rotation relations would suggest physical changes in the magnetic dynamo that warrants further investigation using larger samples of M dwarfs on both sides of the fully convective boundary. Important limitations need to be overcome before the radial velocity technique can be routinely used to detect and study planets around young and active stars. 000133383 536__ $$9info:eu-repo/grantAgreement/ES/AEI/PID2019-107061GB-C64$$9info:eu-repo/grantAgreement/ES/AEI/PID2019-109522GB-C51$$9info:eu-repo/grantAgreement/ES/AEI/PID2019-109522GB-C52$$9info:eu-repo/grantAgreement/ES/AEI/PID2019-109522GB-C53$$9info:eu-repo/grantAgreement/ES/AEI/PID2019-109522GB-C54$$9info:eu-repo/grantAgreement/ES/AEI/PID2019-110689RB-I00$$9info:eu-repo/grantAgreement/ES/MINECO/SEV-2017-0709 000133383 540__ $$9info:eu-repo/semantics/openAccess$$aby$$uhttp://creativecommons.org/licenses/by/3.0/es/ 000133383 590__ $$a5.8$$b2024 000133383 592__ $$a1.968$$b2024 000133383 591__ $$aASTRONOMY & ASTROPHYSICS$$b16 / 84 = 0.19$$c2024$$dQ1$$eT1 000133383 593__ $$aSpace and Planetary Science$$c2024$$dQ1 000133383 593__ $$aAstronomy and Astrophysics$$c2024$$dQ1 000133383 655_4 $$ainfo:eu-repo/semantics/article$$vinfo:eu-repo/semantics/publishedVersion 000133383 700__ $$aRevilla, D. 000133383 700__ $$aSkrzypinski, S. L. 000133383 700__ $$aDreizler, S. 000133383 700__ $$aBéjar, V. J. S. 000133383 700__ $$aCaballero, J. A. 000133383 700__ $$aCardona Guillén, C. 000133383 700__ $$aCifuentes, C. 000133383 700__ $$aFuhrmeister, B. 000133383 700__ $$aReiners, A. 000133383 700__ $$aVanaverbeke, S. 000133383 700__ $$aRibas, I. 000133383 700__ $$aQuirrenbach, A. 000133383 700__ $$aAmado, P. J. 000133383 700__ $$aAceituno, F. J. 000133383 700__ $$aCasanova, V. 000133383 700__ $$aCortés-Contreras, M. 000133383 700__ $$aDubois, F. 000133383 700__ $$aGorrini, P. 000133383 700__ $$aHenning, Th. 000133383 700__ $$aHerrero, E. 000133383 700__ $$aJeffers, S. V. 000133383 700__ $$aKemmer, J. 000133383 700__ $$aLalitha, S. 000133383 700__ $$aLodieu, N. 000133383 700__ $$aLogie, L. 000133383 700__ $$aLópez González, M. J. 000133383 700__ $$aMartín-Ruiz, S. 000133383 700__ $$aMontes, D. 000133383 700__ $$aMorales, J. C. 000133383 700__ $$aNagel, E. 000133383 700__ $$aPallé, E. 000133383 700__ $$aPerdelwitz, V. 000133383 700__ $$0(orcid)0000-0001-5654-0266$$aPérez-Torres, M. 000133383 700__ $$aPollacco, D. 000133383 700__ $$aRau, S. 000133383 700__ $$aRodríguez-López, C. 000133383 700__ $$aRodríguez, E. 000133383 700__ $$aSchöfer, P. 000133383 700__ $$aSeifert, W. 000133383 700__ $$aSota, A. 000133383 700__ $$aZapatero Osorio, M. R. 000133383 700__ $$aZechmeister, M. 000133383 773__ $$g684 (2024), A9 [33 pp.]$$pAstron. astrophys.$$tAstronomy and Astrophysics$$x0004-6361 000133383 8564_ $$s7439423$$uhttps://zaguan.unizar.es/record/133383/files/texto_completo.pdf$$yVersión publicada 000133383 8564_ $$s3633208$$uhttps://zaguan.unizar.es/record/133383/files/texto_completo.jpg?subformat=icon$$xicon$$yVersión publicada 000133383 909CO $$ooai:zaguan.unizar.es:133383$$particulos$$pdriver 000133383 951__ $$a2025-09-22-14:36:30 000133383 980__ $$aARTICLE