  We report the serendipitous discovery of two objects close in projection with
fairly strong emission lines at long wavelength (~9190 A). One (A) seems not to
be hosted by any galaxy brighter than V(555)=27.5, or I(814)=26.7 (Vega-based
3-sigma limits in 1.0 arcsec diameter apertures), while the other line is
associated with a faint (I(814)~24.4) red galaxy (B) offset by 2.7 arcsec and 7
A spectrally. Both lines are broad (FWHM 700 km/s), extended spatially, and
have high equivalent widths (W(A,obs)>1225 A, 95% confidence limit;
W(B,obs)~150 A). No secondary spectral features are detected for galaxy A. Blue
continuum and the marginal detection of a second weak line in the spectrum of
galaxy B is consistent with [OII] (the strong line) and MgII (the weak line) at
z=1.466. By association, galaxy A is likely at z=1.464, implying a rest-frame
equivalent width of the [OII] emission line in excess of 600 A and a projected
separation of 30 kpc for the galaxy pair. Conventional wisdom states that
isolated emission lines with rest-frame equivalent widths larger than ~200 A
are almost exclusively Lyman-alpha. This moderate-redshift discovery therefore
compromises recent claims of high-redshift Lyman-alpha emitters for which other
criteria (i.e., line profile, associated continuum decrements) are not
reported. We discuss observational tests to distinguish Lyman-alpha emitters at
high redshift from foreground systems.
