vs $J-K'$ diagrams to perform the diagnostics for distinguishing dusty star-forming EROs from passively evolved ones, as suggested by Pozzetti and Mannucci (2000) for identifying more plausible counterpart of the SCUBA source among those EROs in figure 5, in case they are at $1 < z < 2$. We also plotted the color tracks of elliptical and dusty starburst galaxies based on the GISSEL 99 model (Buruzal, Charlot 1993) for calculating the SEDs of each track. The ellipticals are represented by a simple stellar population with solar metallicity with Salpeter IMF with an age of 15 Gyrs. For dusty starbursts, we used a model with a constant star formation rate over 1Gyr reddened to $E(B-V) =$ 0.8 using the dust-extinction law by Calzetti et al.(2000). We used the criteria suggested by Pozzetti and Mannucci (2000) for distinguishing two populations of EROs, which is $(J-K) = 0.34(R-K)+0.19$ with $R_{\rm{c}}-K > 5.3$, and found that more than half of the EROs near the SCUBA source (“A1”, “A4”, “E” and “F”) can be categorized as dusty starburst populations. They may consist of groups of dusty EROs or some blends of lensed objects, because “A1” to “A4” are well aligned along another arc, which 