Revisiting the 16 Cygni planet host at unprecedented precision and exploring automated tools for precise abundances. (arXiv:1906.04195v1 [astro-ph.SR])

Revisiting the 16 Cygni planet host at unprecedented precision and exploring automated tools for precise abundances. (arXiv:1906.04195v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Maia_M/0/1/0/all/0/1">M. Tucci Maia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Melendez_J/0/1/0/all/0/1">J. Mel&#xe9;ndez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lorenzo_Oliveira_D/0/1/0/all/0/1">D. Lorenzo-Oliveira</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Spina_L/0/1/0/all/0/1">L. Spina</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jofre_P/0/1/0/all/0/1">P. Jofr&#xe9;</a>

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.

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.

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