  This study presents elemental abundances of the early A-type supergiant HD
80057 and the late A-type supergiant HD80404. High resolution and high
signal-to-noise ratio spectra published by the UVES Paranal Observatory Project
(Bagnulo et al., 2003) were analysed to compute their elemental abundances
using ATLAS9 (Kurucz, 1993, 2005; Sbordone et al., 2004). In our analysis we
assumed local thermodynamic equilibrium. The atmospheric parameters of HD 80057
used in this study are from Firnstein & Przybilla (2012), and that of HD80404
are derived from spectral energy distribution, ionization equilibria of Cr I/II
and Fe I/II, and the fits to the wings of Balmer lines and Paschen lines as
Teff = 7700 +/- 150 K and log g=1.60 +/- 0.15 (in cgs). The microturbulent
velocities of HD 80057 and HD 80404 have been determined as 4.3 +/- 0.1 and 2.2
+/- 0.7 km s^-1 . The rotational velocities are 15 +/-1 and 7 +/- 2 km s^-1 and
their macroturbulence velocities are 24 +/-2 and 2+/-1 km s^-1 . We have given
the abundances of 27 ions of 20 elements for HD 80057 and 39 ions of 25
elements for HD80404. The abundances are close to solar values, except for some
elements (Na, Sc, Ti, V, Ba, and Sr). We have found the metallicities [M/H] for
HD 80057 and HD 80404 as -0.15 +/- 0.24 and -0.02 +/- 0.20 dex, respectively.
The evolutionary status of these stars are discussed and their
nitrogen-to-carbon (N/C) and nitrogen-to-oxygen (N/O) ratios show that they are
in their blue supergiant phase before the red supergiant region.
