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Aims. We use the recently published database (Trifonov et al. 2020) of radialvelocities (RVs) that were derived from fifteen years of HARPS/ESO observationsto search for planet candidates. Methods. For targets with sufficient RV data,we apply an automated algorithm to identify significant periodic signals andfit a Keplerian model for orbital estimates. We also search the auxiliary dataof stellar-activity indices and compare our findings with existing literature,to detect periodic RV signals that have no counterpart in the activitytimeseries. The most convincing signals are then manually inspected todesignate additional false planet detection, focusing the search on long-period(P > 1 000 d) massive candidates around FGK dwarf stars. Results. We identifytwo Jupiter analogs, in orbit around the slightly evolved F8V star HD 103891and the Solar-like star HD 105779. We use nested sampling to derive theirorbital parameters, and find their orbital periods to be 1919 +/- 16 d and 2412+/- 54 d, while their minimum masses are 1.44 +/- 0.02 M Jup and 0.64 +/- 0.06M Jup , respectively. While the orbit of HD 103891 b is slightly eccentric (e =0.31 +/- 0.03), that of HD 105779 b is likely circular (e < 0.16). Conclusions.With minimum astrometric signatures of 59 and 42 $\mu$as, HD 103891 b and HD105779 b join the growing sample of planets whose exact masses may soon bederived with Gaia astrometry. This finding also highlights the importance oflong-term RV surveys to study planetary occurrence beyond the snow line ofSolar-like stars.

Analysis of the public HARPS/ESO spectroscopic archive -- Jupiter-like planets around HD 103891 and HD 105779