0.065    0.05    0.060    0.02    0.803    1.93      
           4860    $0.14\pm0.06$     -       -        -       -      0.383    1.68      
           5007    $0.20\pm0.15$     -       -        -       -      0.342    1.41      
           6548    $1.00\pm0.00$     -       -        -       -      0.027    0.01      
           6583    $0.43\pm0.16$     -       -        -       -      0.021    0.01      
  ------ -------- --------------- ------- -------- ------- -------- ------- -------- -- --

@Cowie97 and @Gallego95 provide number density counts for star forming galaxies at a range of redshifts. Both adopt a , $\Omega_{\Lambda} = 0$, $\Omega_{\mathrm{M}} =
1$ cosmology, which we converted to match that used in this work (Section \[sec:intro\]). In addition, @Gallego95 assume a @Scalo86 IMF; @Cowie97 provide a conversion to a @Salpeter55 IMF, and it is these results we adopt in this work. Based on these, we can estimate the number density of star forming galaxies along our line of sight: see Fig. \[fig:sfgs\].

@Kennicutt98 provides a conversion between star formation rate in a galaxy and luminosity; the ratios given in Table \[tab:interlopers\] make it possible to convert that into expected luminiosities for the other lines. After applying a correction for instrumental effects and galactic extinction [@Schlegel98], a locus of points in the magnitude-wavelength completeness diagrams (Fig. \[fig:simresults\]) on which each line at a given redshift might be detected is 