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

## TL;DR

This study refines the chemical abundance analysis of the 16 Cygni binary system, exploring the impact of planet formation and potential planet engulfment signatures using automated tools and spectral synthesis.

## Contribution

It provides an updated, precise abundance comparison of 16 Cyg A and B, including volatile and neutron capture elements, and demonstrates the effectiveness of automated tools for abundance determination.

## Key findings

- Abundance differences persist even with additional elements included.
- A positive T_c slope of 1.56e-5 dex K^{-1} consistent with previous studies.
- 16 Cyg A shows higher Li and Be levels, suggesting possible planet engulfment.

## Abstract

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