Spectroscopic and photometric observations of the peculiar object AM 2049-691 are presented here .
Its systemic velocity is V _ { GSR } = ( 10956 \pm 30 ) km s ^ { -1 } , and the derived distance ( H _ { 0 } = 75 km s ^ { -1 } Mpc ^ { -1 } ) results 146 Mpc .
A bridge is observed between two very distinct nuclei whose separation is about 10 kpc , as well as two tails that emerge from the extremes SW and NE of the main body and extend up to 41 and 58 kpc respectively .
The spectral characteristics of the all observed zones are typical of H II regions of low excitation .
The internal reddening is quit high , particularly in the NE nucleus .
All the derived equivalent widths of the H \alpha + [ N II ] lines indicate enhanced star formation compared with isolated galaxies , specially in the NE nucleus ; the equivalent width corresponding to the integrated spectrum reflects starburst activity in the whole object , and is compatible with a merger of two disk galaxies .
The observed characteristics of AM 2049-691 indicate it is a merger , where a overabundance of nitrogen is detected in one of the nuclei , which has the most evolved population and would be the most massive one .
The detected total IR emission is not very high .
The integrated total color B - V corresponds to a Sc-Scd galaxy and its average integrated population is about F7 type .
Indicative B - V colors of the nuclei , corrected for internal absorption , are in agreement with the spectroscopic results .
The central radial velocity dispersions at the nuclei suggest that the most massive galaxy would be the progenitor of the SW component .
The observed radial velocity curve shows the presence of two subsystems , each one associated with a different nucleus .