Table 7: Number of spectra in different magnitude sub-samples. Bright and faint galaxies correspond to objects with $M_{R_{\rm AB}}<-20$ and $M_{R_{\rm AB}}>-20$ respectively. Bright objects correspond to the same sampling in absolute magnitude as in the MORPHS spectroscopic catalogue (Dressler et al. 1999).
Sample ${N}_{\rm\rm tot}$ k k+a k+a? Emission line

Bright 52 44 (84.6%) 1 (1.9%) 3 (5.8%) 4 (7.7%)

Faint 31 15 (48.4%) 5 (16.1%) 4 (12.9%) 7 (22.6%)

Total 83 59 (71.1%) 6 (7.2%) 7 (8.4%) 11 (13.3%)

**Table 7:** Number of spectra in different magnitude sub-samples. Bright and faint galaxies correspond to objects with $M_{R_{\rm AB}}<-20$ and $M_{R_{\rm AB}}>-20$ respectively. Bright objects correspond to the same sampling in absolute magnitude as in the MORPHS spectroscopic catalogue (Dressler et al. 1999).
Sample	${N}_{\rm\rm tot}$	k	k+a	k+a?	Emission line
Bright	52	44 (84.6%)	1 (1.9%)	3 (5.8%)	4 (7.7%)
Faint	31	15 (48.4%)	5 (16.1%)	4 (12.9%)	7 (22.6%)
Total	83	59 (71.1%)	6 (7.2%)	7 (8.4%)	11 (13.3%)

Source LaTeX | All tables | In the text

	1 Introduction
	2 The data
	3 Cluster membership
	4 Colour properties and spatial morphology of A3921
	5 Cluster kinematics
	6 Dynamical study of the system
	7 Spectral properties of the cluster members
	8 Discussion and conclusions
	Appendix A: Red sequence identification
	References