The spectrum of the evolved B8 III giant HR 62 exhibits weak He-lines and strong Mn and P lines .
HR 62 therefore resembles both a HgMn star ( CP3 ) and a He-weak PGa star ( CP4 ) .

This study is a companion project to a high resolution survey of slowly rotationg late-B type stars aiming at finding new chemically peculiar stars .
We have analysed the spectra of HR 62 ( B8 III ) and the dwarf comparison star HR 677 ( B8 V ) to derive their chemical abundances .
Both stars have similar effective temperatures ( 12500 K ) and projected rotational velocities ( \sim 25 km s ^ { -1 } ) .

The medium resolution ( R \sim 14000 ) spectra covering the wavelength range of 4380-7350 Å of HR 62 and HR 677 have been obtained with the échelle spectrograph attached to the 40 cm telescope in Ankara University Kreiken Observatory ( AUKR ) , Turkey .
We have used SYNSPEC49/SYNPLOT written by I. Hubeny , T. Lanz to compute grids of synthetic spectra and derive elemental abundances by modeling selected unblended lines .

We find that HR 62 exhibits underabundance of Si and remarkable overabundance of P and Mn with respect to the Sun .
In contrast , HR 677 does not have abundances departing by more than \pm 0.25 dex from solar abundances .
A mass of 5.4 M _ { \odot } and an age of 90 Myr have been estimated for HR 62 .

We discuss the origin of the chemical peculiarities of HR 62 and its status as a CP star .
The effective temperature of the star ( 12500 K ) agrees well with those of HgMn ( CP3 ) stars .
Furthermore , the main sequence end of its evolutionary track also intersects the domain of He-weak CP4 stars .
Hence these first results suggest that HR 62 may be a transition object between the CP4 to CP3 subgroup .
However , a more detailed analysis of higher resolution spectra at shorter wavelengths ( < 4380 Å ) is necessary to clearly address the nature of this interesting object .