We present neutron-capture element abundances for a homogeneous sample of 160 FGK-type planet-hosting stars (32 of them are multiplanetary systems). These stars host a total of 175 high-mass planets and 47 Neptunian and Super-Earth planets. Spectra were obtained with the Vilnius University Echelle Spectrograph (VUES) associated with a 1.65m telescope installed at Moletai Astronomical Observatory. The analysed elements include Sr, Y, Zr, Ba, La, Ce, Pr, Nd, and Eu. Abundances were derived using synthetic spectral fitting with the TURBOSPECTRUM code and MARCS model atmospheres under LTE, with NLTE corrections applied for Sr, Y, Ba and Eu. The dataset includes stellar parameters, and individual elemental abundances ([El/H]). We investigate the trends of [El/Fe] with [Fe/H] and planet mass, and examine condensation temperature (T_cond_) trends ({DELTA}[El/H]-T_cond_> slopes) for potential star-planet chemical signatures. The results show that most neutron-capture elements trace Galactic chemical evolution, but [Zr/Fe], [La/Fe], and [Ce/Fe] are enhanced in stars with planets compared to reference stars at a given [Fe/H]. Positive correlations between [El/Fe] and planet mass are observed towards higher-mass planets for most elements excluding strontium, yttrium, and barium, which exhibit insignificant correlations across all subsamples. The {DELTA}[El/H]-T_cond_ slopes suggest a possible enrichment of refractory elements in planet-hosting stars, especially in younger and less metal-rich systems. While strong correlations between {DELTA}[El/H]-T_cond_ slopes and stellar or planetary parameters are not observed, the data suggest some notable trends. Older dwarf stars hosting multiple planets tend to exhibit smaller or even negative {DELTA}[El/H]-T_cond_ slopes, whereas younger dwarfs show larger positive slopes, indicating a possible age-dependent chemical signature. Additionally, we find that multiplanetary systems are more frequently associated with metal-rich stars. This dataset supports ongoing efforts to understand the chemical signatures associated with planet formation.

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