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The binary system 16 Cygni is key in studies of the planet-star chemicalcomposition connection, as only one of the stars is known to host a planet.This allows us to better assess the possible influence of planet interactionson the chemical composition of stars that are born from the same cloud andthus, should have a similar abundance pattern. In our previous work, we foundclear abundance differences for elements with Z$\leq30$ between both componentsof this system, and a trend of these abundances as a function of thecondensation temperature (T$_{c}$), which suggests a spectral chemicalsignature related to planet formation. In this work we show that our previousfindings are still consistent even if we include more species, like thevolatile N and neutron capture elements (Z $>$ 30). We report a slope withT$_{c}$ of $1.56 \pm 0.24 \times 10^{-5}$ dex K$^{-1}$, that is good agreementwith both our previous work and recent results by Nissen and collaborators. Wealso performed some tests using ARES and iSpec to automatic measure theequivalent width and found T$_c$ slopes in reasonable agreement with ourresults as well. In addition, we determine abundances for Li and Be by spectralsynthesis, finding that 16 Cyg A is richer not only in Li but also in Be, whencompared to its companion. This may be evidence of planet engulfment,indicating that the T$_{c}$ trend found in this binary system may be a chemicalsignature of planet accretion in the A component, rather than a imprint of thegiant planet rocky core formation on 16 Cyg B.

Revisiting the 16 Cygni planet host at unprecedented precision and exploring automated tools for precise abundances