Surface Photometry and Metallicity of the Polar Ring Galaxy A0136-0801
  We present a photometric and spectroscopic study of the polar ring galaxy
A0136-0801 in order to constrain its formation history. Near-Infrared (NIR) and
optical imaging data are used to extract surface brightness and color profiles
of the host galaxy and the wide polar structure in A0136-0801. The host galaxy
dominates the light emission in all bands; the polar structure is more luminous
in the optical bands and is three times more extended than the main spheroid.
The average stellar population in the spheroid is redder than in the polar
structure and we use their (B-K) vs. (J-K) colors to constraint the ages of
these populations using stellar population synthesis models. The inferred ages
are 3-5 Gyrs for the spheroid and 1-3 Gyrs for the polar structure. We then use
long slit spectra along the major axis of the polar structure to derive the
emission line ratios and constrain the oxygen abundance, metallicity and star
formation rate in this component. We find 12+log(O/H) = 8.33 +- 0.43 and Z ~
0.32 Zsun, using emission line ratios. These values are used, together with the
ratio of the baryonic masses of the host galaxy and polar structure, to
constraint the possible models for the formation scenario. We conclude that the
tidal accretion of gas from a gas rich donor or the disruption of a gas-rich
satellite are formation mechanisms that may lead to systems with physical
parameters in agreement with those measured for A0136-0801.
