Photo-chemo-dynamical analysis and the origin of the bulge globular
  cluster Palomar 6
  Palomar 6 (Pal~6) is a moderately metal-poor globular cluster projected
towards the Galactic bulge. A full analysis of the cluster can give hints on
the early chemical enrichment of the Galaxy and a plausible origin of the
cluster. The aim of this study is threefold: a detailed analysis of
high-resolution spectroscopic data obtained with the UVES spectrograph at the
Very Large Telescope (VLT) at ESO, the derivation of the age and distance of
Pal~6 from Hubble Space Telescope (HST) photometric data, and an orbital
analysis to determine the probable origin of the cluster. High-resolution
spectra of six red giant stars in the direction of Palomar 6 were obtained at
the $8$m VLT UT2-Kueyen telescope equipped with the UVES spectrograph in
FLAMES$+$UVES configuration. Spectroscopic parameters were derived through
excitation and ionisation equilibrium of \ion{Fe}{I} and \ion{Fe}{II} lines,
and the abundances were obtained from spectrum synthesis. From HST photometric
data, the age and distance were derived through a statistical isochrone
fitting. Finally, a dynamical analysis was carried out for the cluster assuming
two different Galactic potentials. Four stars that are members of Pal~6 were
identified in the sample, which gives a mean radial velocity of $174.3\pm1.6$
km\,s$^{-1}$ and a mean metallicity of [Fe/H]$\,=-1.10\pm0.09$ for the cluster.
We found an enhancement of $\alpha$-elements (O, Mg, Si, and Ca)
$0.29<\,$[X/Fe]$\,<0.38$ and the iron-peak element Ti of [Ti/Fe]$\,\sim+0.3$.
The odd-Z elements (Na and Al) show a mild enhancement of [X/Fe]$\,\sim +0.25$.
The abundances of both first- (Y and Zr) and second-peak (Ba and La) heavy
elements are relatively high, with $+0.4<\,$[X/Fe]$\,<+0.60$ and
$+0.4<\,$[X/Fe]$\,<+0.5$, respectively. The r-element Eu is also relatively
high with [Eu/Fe]$\,\sim +0.6$. $\mathbf{\left[Truncated\right]}$
