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This work presents a homogeneous derivation of atmospheric parameters andiron abundances for a sample of giant and subgiant stars which host giantplanets, as well as a control sample of subgiant stars not known to host giantplanets. The analysis is done using the same technique as for our previousanalysis of a large sample of planet-hosting and control sample dwarf stars. Acomparison between the distributions of [Fe/H] in planet-hosting main-sequencestars, subgiants, and giants within these samples finds that the main-sequencestars and subgiants have the same mean metallicity of <[Fe/H]> \simeq +0.11dex, while the giant sample is typically more metal poor, having an averagemetallicity of <[Fe/H]> = -0.06 dex. The fact that the subgiants have the sameaverage metallicities as the dwarfs indicates that significant accretion ofsolid metal-rich material onto the planet-hosting stars has not taken place, assuch material would be diluted in the evolution from dwarf to subgiant. Thelower metallicity found for the planet-hosting giant stars in comparison withthe planet-hosting dwarfs and subgiants is interpreted as being related to theunderlying stellar mass, with giants having larger masses and thus, on averagelarger-mass protoplanetary disks. In core accretion models of planet formation,larger disk masses can contain the critical amount of metals necessary to formgiant planets even at lower metallicities.

Metallicities of Planet Hosting Stars: A Sample of Giants and Subgiants