Table 2: Characteristics of the multi-sinusoidal fit of individual runs of observations of BG CMi. The flux is expressed in units of 10^-15 erg s^-1 cm^-2 Å^-1. The calibration in Vhas been made using the magnitude of the comparison star. For R, the standard magnitude is unknown and has been arbitrarily set to zero. This makes values of intensity to be apparently large. They may be calibrated after further determination of the R magnitude of the comparison star. For bad phase distribution caused by an incomplete coverage of the period in the first two runs, the values are highly biased and should not be taken for further analysis. Such biased or statistically insignificant values are marked by a semi-column ":''.
Date I₀ R₁ R₂ R₃ R₄ R₅ R₆

V 52635 -759: $\pm$ 129 1381: $\pm$ 2318 1018: $\pm$ 1670 599: $\pm$ 945 270: $\pm$ 400 85: $\pm$ 115 14: $\pm$ 17

V 52638 46: $\pm$ 49 77: $\pm$ 89 60: $\pm$ 67 39: $\pm$ 41 20: $\pm$ 20 7.17: $\pm$ 6.67 1.39: $\pm$ 1.29

V 53035 3.527 $\pm$ 0.042 0.294 $\pm$ 0.055 0.337 $\pm$ 0.054 0.273 $\pm$ 0.055 0.071: $\pm$ 0.059 0.050: $\pm$ 0.059 0.092: $\pm$ 0.056

V 53036 3.796 $\pm$ 0.035 0.362 $\pm$ 0.050 0.343 $\pm$ 0.049 0.167 $\pm$ 0.050 0.040: $\pm$ 0.049 0.075: $\pm$ 0.049 0.062: $\pm$ 0.049

V 53052 3.578 $\pm$ 0.035 0.442 $\pm$ 0.051 0.179 $\pm$ 0.050 0.048: $\pm$ 0.051 0.068: $\pm$ 0.049 0.054: $\pm$ 0.047 0.097: $\pm$ 0.048

V 53385 3.467 $\pm$ 0.100 0.257: $\pm$ 0.158 0.296: $\pm$ 0.158 0.296: $\pm$ 0.153 0.131: $\pm$ 0.152 0.059: $\pm$ 0.136 0.011: $\pm$ 0.143

R 53385 272816 $\pm$ 6747 31239 $\pm$ 10432 17926: $\pm$ 10145 20531: $\pm$ 9874 4393: $\pm$ 9968 6942: $\pm$ 9139 1100: $\pm$ 9558

V 53404 3.494 $\pm$ 0.086 0.406 $\pm$ 0.124 0.421 $\pm$ 0.120 0.072: $\pm$ 0.121 0.135: $\pm$ 0.121 0.100: $\pm$ 0.120 0.075: $\pm$ 0.120

R 53404 272413 $\pm$ 6526 31228 $\pm$ 9288 32071 $\pm$ 9066 7256: $\pm$ 9077 6246: $\pm$ 9273 5251: $\pm$ 9189 3509: $\pm$ 9264

**Table 2:** Characteristics of the multi-sinusoidal fit of individual runs of observations of BG CMi. The flux is expressed in units of 10^-15 erg s^-1 cm^-2 Å^-1. The calibration in Vhas been made using the magnitude of the comparison star. For R, the standard magnitude is unknown and has been arbitrarily set to zero. This makes values of intensity to be apparently large. They may be calibrated after further determination of the R magnitude of the comparison star. For bad phase distribution caused by an incomplete coverage of the period in the first two runs, the values are highly biased and should not be taken for further analysis. Such biased or statistically insignificant values are marked by a semi-column ":''.
Date	I₀	R₁	R₂	R₃	R₄	R₅	R₆
V 52635	-759: $\pm$ 129	1381: $\pm$ 2318	1018: $\pm$ 1670	599: $\pm$ 945	270: $\pm$ 400	85: $\pm$ 115	14: $\pm$ 17
V 52638	46: $\pm$ 49	77: $\pm$ 89	60: $\pm$ 67	39: $\pm$ 41	20: $\pm$ 20	7.17: $\pm$ 6.67	1.39: $\pm$ 1.29
V 53035	3.527 $\pm$ 0.042	0.294 $\pm$ 0.055	0.337 $\pm$ 0.054	0.273 $\pm$ 0.055	0.071: $\pm$ 0.059	0.050: $\pm$ 0.059	0.092: $\pm$ 0.056
V 53036	3.796 $\pm$ 0.035	0.362 $\pm$ 0.050	0.343 $\pm$ 0.049	0.167 $\pm$ 0.050	0.040: $\pm$ 0.049	0.075: $\pm$ 0.049	0.062: $\pm$ 0.049
V 53052	3.578 $\pm$ 0.035	0.442 $\pm$ 0.051	0.179 $\pm$ 0.050	0.048: $\pm$ 0.051	0.068: $\pm$ 0.049	0.054: $\pm$ 0.047	0.097: $\pm$ 0.048
V 53385	3.467 $\pm$ 0.100	0.257: $\pm$ 0.158	0.296: $\pm$ 0.158	0.296: $\pm$ 0.153	0.131: $\pm$ 0.152	0.059: $\pm$ 0.136	0.011: $\pm$ 0.143
R 53385	272816 $\pm$ 6747	31239 $\pm$ 10432	17926: $\pm$ 10145	20531: $\pm$ 9874	4393: $\pm$ 9968	6942: $\pm$ 9139	1100: $\pm$ 9558
V 53404	3.494 $\pm$ 0.086	0.406 $\pm$ 0.124	0.421 $\pm$ 0.120	0.072: $\pm$ 0.121	0.135: $\pm$ 0.121	0.100: $\pm$ 0.120	0.075: $\pm$ 0.120
R 53404	272413 $\pm$ 6526	31228 $\pm$ 9288	32071 $\pm$ 9066	7256: $\pm$ 9077	6246: $\pm$ 9273	5251: $\pm$ 9189	3509: $\pm$ 9264

Source LaTeX | All tables | In the text

	1 Introduction
	2 Observations and comparison stars
	3 Separation of spin and orbital variability
	4 Color variability with the phase of orbital and spin period
	5 194-minute orbital period
	6 Variability of the spin period
	7 Conclusions
	References