All Figures

	Figure 1: Light curves of six Scuti type pulsating stars whose classification is re-confirmed in the present study. In each panel, the used data are as follows: ROTSE (ROTSE-I), SOAO_V (our V-magnitude), SOAO_I (our I-magnitude), and SOAO_VI (our (V-I) color). Mean magnitudes of each data set are expressed in an arbitrary scale.
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In the text

	Figure 2: Light curves re-classified as W UMa type eclipsing binary stars. The data symbols are the same as Fig. 1.
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In the text

	Figure 2: continued.
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In the text

	Figure 2: continued.
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In the text

	Figure 3: Peculiar light curves of two variable stars. (Left) ROTSE J181613.28+495205.0 is a AM Her, strongly magnetic cataclysmic variable. (Right) ROTSE J191516.94+475914.5 does not show any noticeable light variations in our observations.
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In the text

	Figure 4: versus amplitudes difference diagram. Filled circles represent thirteen W UMa type eclipsing binaries and open circles denote six  Scuti type pulsating stars. The slopes of against , are much different between two variable types.
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In the text

	Figure 5: V-amplitudes versus periods diagram of Scuti stars. Open circles represent six Scuti stars observed in this study. Dots denote known Scuti stars, which were catalogued by Rodríguez et al. (2000).
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In the text

Figure 6: Difference of color distributions between pulsating and eclipsing stars. (Left) (B-R) versus R diagram using the observational data of Everett et al. (2002). Filled circles are EA/EW stars, open circles are SX Phe/ Scuti stars, and small crosses are un-classified variable stars. (Right) (B-R) versus R diagram of ROTSE-I Scuti stars. B and R magnitude obtained from the USNO catalogue. Filled circles are eclipsing variables and open circles are pulsating variables observed in this study. Small crosses are un-observed stars.

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In the text