**Table 1:** *UBV* photometry for stars in the fields of IC 2395 and BH 47.
Star	X	Y	$\alpha_{2000}$	$\delta_{2000}$	V	B-V	U-B	n	Name(s)	Spec. type	Membership
			( $^{\rm h m s}$ )	( $\hbox{$^\circ$ }$ $\hbox{$^\prime$ }$ )
1	464	542	8 42 15.9	-48 06.1	5.485	-0.179	-0.957	2	HD 74455, L 1	B2/3 IV-V	M, 96%
2	465	575	8 42 15.8	-48 04.4	11.696	0.291	0.144	3	L 18		M
3	472	584	8 42 17.9	-48 03.9	10.739	0.026	-0.121	3	L 15, CD -47 $\hbox{$^\circ$ }$ 4253		M
4	453	573	8 42 12.2	-48 04.5	11.698	1.687	1.814	3	L 42, CD -47 $\hbox{$^\circ$ }$ 4250		NM
5	450	532	8 42 11.7	-48 06.6	10.395	0.001	-0.186	4	L 43, CD -47 $\hbox{$^\circ$ }$ 4247		M
6	459	525	8 42 14.6	-48 06.9	11.281	0.089	0.034	4	L 44		M
7	459	517	8 42 14.6	-48 07.3	12.531	0.680	0.126	3	L 45		NM
8	444	497	8 42 10.3	-48 08.4	12.724	0.379	0.267	3	L 48		NM

Note: Stars Nos. 153, 156, 174 and 233 are double stars. Photometry refers to the combined light of both components. Stars Nos. 170, 217 and 222 were previously reported as variables (Lapasset & Clariá 1985). Star No. 82 was found to be variable, its individual $\Delta V$ variations being $\sim$ 0.3 mag. All the MK spectral types are from Houck (1978), except that of star No. 1, which is from Garrison et al. (1977).

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