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Palomar 6 (Pal~6) is a moderately metal-poor globular cluster projectedtowards the Galactic bulge. A full analysis of the cluster can give hints onthe early chemical enrichment of the Galaxy and a plausible origin of thecluster. The aim of this study is threefold: a detailed analysis ofhigh-resolution spectroscopic data obtained with the UVES spectrograph at theVery Large Telescope (VLT) at ESO, the derivation of the age and distance ofPal~6 from Hubble Space Telescope (HST) photometric data, and an orbitalanalysis to determine the probable origin of the cluster. High-resolutionspectra of six red giant stars in the direction of Palomar 6 were obtained atthe $8$m VLT UT2-Kueyen telescope equipped with the UVES spectrograph inFLAMES$+$UVES configuration. Spectroscopic parameters were derived throughexcitation and ionisation equilibrium of \ion{Fe}{I} and \ion{Fe}{II} lines,and the abundances were obtained from spectrum synthesis. From HST photometricdata, the age and distance were derived through a statistical isochronefitting. Finally, a dynamical analysis was carried out for the cluster assumingtwo different Galactic potentials. Four stars that are members of Pal~6 wereidentified 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) heavyelements are relatively high, with $+0.4<\,$[X/Fe]$\,<+0.60$ and$+0.4<\,$[X/Fe]$\,<+0.5$, respectively. The r-element Eu is also relativelyhigh with [Eu/Fe]$\,\sim +0.6$. $\mathbf{\left[Truncated\right]}$

Photo-chemo-dynamical analysis and the origin of the bulge globular cluster Palomar 6