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We investigated the presence of planetary companions around the nearby (7.6pc) and bright ($V=9$ mag) early-type M dwarf Gl 514, analysing 540 radialvelocities collected over nearly 25 years with the HIRES, HARPS, and CARMENESspectrographs. The data are affected by time-correlated signals at the level of2-3 ms$^{-1}$ due to stellar activity, that we filtered out testing threedifferent models based on Gaussian process regression. As a sanity cross-check,we repeated the analyses using HARPS radial velocities extracted with threedifferent algorithms. We used HIRES radial velocities and Hipparcos-Gaiaastrometry to put constraints on the presence of long-period companions, and weanalysed TESS photometric data. We found strong evidence that Gl 514 hosts asuper-Earth on a likely eccentric orbit, residing in the conservative habitablezone for nearly $34\%$ of its orbital period. The planet Gl 514 b has minimummass $m_b\sin i_b=5.2\pm0.9$ $M_{\rm Earth}$, orbital period$P_b=140.43\pm0.41$ days, and eccentricity $e_b=0.45^{+0.15}_{-0.14}$. Noevidence for transits is found in the TESS light curve. There is no evidencefor a longer period companion in the radial velocities and, based onastrometry, we can rule out a $\sim0.2$ $M_{\rm Jup}$ planet at a distance of$\sim3-10$ au, and massive giant planets/brown dwarfs out to several tens ofau. We discuss the possible presence of a second low-mass companion at ashorter distance from the host than Gl 514 b. Gl 514 b represents aninteresting science case to study the habitability of planets on eccentricorbits. We advocate for additional spectroscopic follow-up to get more accurateand precise planetary parameters. Further follow-up is also needed toinvestigate sub \ms and shorter period signals.

astronomy and astrophysics

A quarter century of spectroscopic monitoring of the nearby M dwarf Gl  514. A super-Earth on an eccentric orbit moving in and out of the habitable  zone