Context : Metal-rich globular clusters provide important tracers of the formation of our Galaxy .
Moreover , and not less important , they are very important calibrators for the derivation of properties of extra-galactic metal-rich stellar populations .
Nonetheless , only a few of the metal-rich globular clusters in the Milky Way have been studied using high-resolution stellar spectra to derive elemental abundances .
Additionally , Rosenberg et al .
identified a small group of metal-rich globular clusters that appeared to be about 2 billion years younger than the bulk of the Milky Way globular clusters .
However , it is unclear if like is compared with like in this dataset as we do not know the enhancement of \alpha -elements in the clusters and the amount of \alpha -elements is well known to influence the derivation of ages for globular clusters .

Aims : To derive elemental abundances for the metal-rich globular cluster NGC 6352 and to present our methods to be used in up-coming studies of other metal-rich globular clusters .

Methods : We present a study of elemental abundances for \alpha - and iron-peak elements for nine HB stars in the metal-rich globular cluster NGC 6352 .
The elemental abundances are based on high-resolution , high signal-to-noise spectra obtained with the UVES spectrograph on VLT .
The elemental abundances have been derived using standard LTE calculations and stellar parameters have been derived from the spectra themselves by requiring ionizational as well as excitational equilibrium .

Results : We find that NGC 6352 has [ Fe/H ] = -0.55 , is enhanced in the \alpha -elements to about +0.2 dex for Ca , Si , and Ti relative to Fe .
For the iron-peak elements we find solar values .
Based on the spectroscopically derived stellar parameters we find that an E ( B - V ) = 0.24 and ( m - M ) \simeq 14.05 better fits the data than the nominal values .
An investigation of \log gf -values for suitable Fe i lines lead us to the conclusion that the commonly used correction to the May et al .
( 1974 ) data should not be employed .

Conclusions :