**Table 2:** Photometric and derived properties of candidate clusters in NGC 6872. The complete list is available in electronic form at the CDS.
id	x	y	U^a	dU	B^a	dB	V^a	dV	I^a	dI	$\chi^{2}_{\nu}$ ^b	$A_{\rm V}$ ^c	log (Age/yr)^c	log Mass/ $M_{\odot}$ ^c	$M_{\rm V}$ ^d
2	120.6	164.0	23.25	0.17	23.05	0.04	22.27	0.03	21.37	0.04	2.00	0.00	9.48	6.89	-11.63
6	189.0	178.2	22.55	0.11	23.34	0.07	23.58	0.09	22.90	0.10	7.60	0.19	7.20	5.11	-10.51
10	215.5	197.7	22.05	0.09	22.58	0.05	22.73	0.07	22.50	0.09	1.80	0.06	6.64	4.59	-11.23
14	40.4	236.0	20.94	0.03	20.89	0.01	20.46	0.01	19.77	0.03	0.80	0.00	8.96	7.20	-13.44
16	71.0	240.8	21.83	0.07	22.21	0.03	22.28	0.04	21.96	0.06	6.80	0.25	6.62	4.79	-11.87
19	201.0	265.4	22.09	0.08	22.54	0.03	22.61	0.04	22.13	0.06	9.20	0.19	6.88	4.95	-11.48
20	159.4	273.8	22.75	0.17	23.14	0.08	23.07	0.09	22.15	0.07	3.10	0.74	7.30	5.52	-11.57

^a Magnitudes have only been corrected for foreground extinction.
^b The reduced $\chi^2$ value for the best fitting model.
^c Derived extinction, age, and mass using the 3DEF method. Sources with ages greater than 1 Gyr are most likely foreground stars.
^d Absolute magnitue of the source, correcting for the derived extinction.

Source LaTeX | All tables | In the text

	1 Introduction
	2 Observations, reduction and photometry
	3 The cluster population
	4 The youngest clusters
	5 Specific U-band luminosity
	6 A scenario for the formation and evolution of star clusters in tidal tails
	7 Conclusions
	References