  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 \AA{} of HR 62 and HR 677 have been obtained with the \'{e}chelle
spectrograph attached to the 40 cm telescope in Ankara University Kreiken
Observatory (AUKR), Turkey. We have used SYNSPEC49/SYNPLOT written by I. Hubeny
and 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 \AA{}) is necessary to clearly address the nature
of this interesting object.
