Table 5: The magnitudes of the optical/NIR afterglow of GRB 040223 predicted by extrapolation of the X-ray afterglow, assuming that the host is similar to the Galaxy. The observed limits are reported for comparison.
  r J, $1{\rm st}$ epoch J, $2{\rm nd}$ epoch H, $1{\rm st}$ epoch H, $2{\rm nd}$ epoch $K_{\rm s}$, $1{\rm st}$ epoch $K_{\rm s}$, $2{\rm nd}$ epoch
Observed limits 18 20.9 21.1 19.8 20.4 19.9 20.2
Simple extrapolation              
z=0 $19.5\pm2$ $16.0\pm2$ $16.2\pm2$ $14.1\pm2$ $14.3\pm2$ $12.5\pm2$ $12.6\pm2$
z=0.9 $58\pm11$ $37\pm6$ $37\pm6$ $27\pm4$ $27\pm4$ $20.7\pm3$ $20.9\pm3$
Cooling break, fast cooling              
z=0, $\nu_ {\rm c}=7.5\times 10^{16}~\rm Hz$ $25.6\pm1$ $22.8\pm1$ $23.0\pm1$ $21.2\pm1$ $21.4\pm1$ $20.0\pm1$ $20.1\pm1$
z=0, $\nu_ {\rm c}=1.2\times 10^{17}~\rm Hz$ $26.2\pm1$ $23.4\pm0.5$ $23.6\pm0.5$ $21.9\pm0.4$ $22.0\pm0.4$ $20.6\pm0.3$ $20.7\pm0.3$
Cooling break, slow cooling              
z=0, $\nu_ {\rm c}=1.2\times 10^{17}~\rm Hz$ $22.5\pm2$ $19.3\pm2$ $19.5\pm2$ $17.6\pm2$ $17.8\pm2$ $16.1\pm2$ $16.3\pm2$
z=0.6, $\nu_ {\rm c}=1.2\times 10^{17}~\rm Hz$ $42\pm6$ $29\pm3$ $29\pm3$ $23.6\pm2$ $23.7\pm2$ $19.9\pm2$ $20.1\pm2$


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