Table 3: Details of the globular cluster luminosity function (GCLF) fitting for the Hydra galaxies NGC 3309 and NGC 3311 and the Centaurus galaxies NGC 4696 and NGC 4709, performed in the rings where SBF were measured. A Gaussian with width $\sigma =1.3$ mag (Kundu & Whitmore 2001) with an error allowance for $\sigma$ of $\pm$ 0.15 mag is fit to the incompleteness corrected number counts in Fig. 3. The error of the turnover magnitude (TOM) is the maximum of the fitting error and the difference in TOM when changing $\sigma$ to its lower and upper limit of 1.15 and 1.45 mag. $I_{\rm cut}$ is the limiting magnitude for the GCLF fitting, identical to the 50% completeness limit for GC detection. An absolute turn-over magnitude of $M_I=-8.46 \pm 0.2$ mag is assumed (Kundu & Whitmore 2001). The GCLF-TOMs of the two Hydra galaxies are poorly constrained both because of a brighter cutoff magnitude and lower number of GCs compared to NGC 4696.
Gal-Nr. TOM [mag] $\sigma$ $I_{\rm cut}$ [mag] $(m-M)_{\rm GC}$ (m-M)_SBF $N_{\rm GC, rings}$ $M_{\rm V, rings}$ $S_{\rm N, rings}$

NGC 3309 25.49 $\pm$ 0.70 1.30 (fixed) 24.70 33.95 $\pm$ 0.73 32.81 $\pm$ 0.13 430 $\pm$ 140 -20.30 $\pm$ 0.2 3.5 $\pm$ 1.3

NGC 3311 25.09 $\pm$ 0.59 1.30 (fixed) 24.70 33.55 $\pm$ 0.63 33.09 $\pm$ 0.14 810 $\pm$ 300 -20.60 $\pm$ 0.2 4.6 $\pm$ 1.9

NGC 4696 24.49 $\pm$ 0.27 1.30 (fixed) 25.05 32.95 $\pm$ 0.34 33.14 $\pm$ 0.16 2390 $\pm$ 300 -21.25 $\pm$ 0.2 7.3 $\pm$ 1.5

NGC 4709 23.86 $\pm$ 0.26 1.30 (fixed) 25.00 32.32 $\pm$ 0.33 32.50 $\pm$ 0.15 360 $\pm$ 60 -19.60 $\pm$ 0.2 5.0 $\pm$ 1.3

**Table 3:** Details of the globular cluster luminosity function (GCLF) fitting for the Hydra galaxies NGC 3309 and NGC 3311 and the Centaurus galaxies NGC 4696 and NGC 4709, performed in the rings where SBF were measured. A Gaussian with width $\sigma =1.3$ mag (Kundu & Whitmore 2001) with an error allowance for $\sigma$ of $\pm$ 0.15 mag is fit to the incompleteness corrected number counts in Fig. 3. The error of the turnover magnitude (TOM) is the maximum of the fitting error and the difference in TOM when changing $\sigma$ to its lower and upper limit of 1.15 and 1.45 mag. $I_{\rm cut}$ is the limiting magnitude for the GCLF fitting, identical to the 50% completeness limit for GC detection. An absolute turn-over magnitude of $M_I=-8.46 \pm 0.2$ mag is assumed (Kundu & Whitmore 2001). The GCLF-TOMs of the two Hydra galaxies are poorly constrained both because of a brighter cutoff magnitude and lower number of GCs compared to NGC 4696.
Gal-Nr.	TOM [mag]	$\sigma$	$I_{\rm cut}$ [mag]	$(m-M)_{\rm GC}$	(m-M)_SBF	$N_{\rm GC, rings}$	$M_{\rm V, rings}$	$S_{\rm N, rings}$
NGC 3309	25.49 $\pm$ 0.70	1.30 (fixed)	24.70	33.95 $\pm$ 0.73	32.81 $\pm$ 0.13	430 $\pm$ 140	-20.30 $\pm$ 0.2	3.5 $\pm$ 1.3
NGC 3311	25.09 $\pm$ 0.59	1.30 (fixed)	24.70	33.55 $\pm$ 0.63	33.09 $\pm$ 0.14	810 $\pm$ 300	-20.60 $\pm$ 0.2	4.6 $\pm$ 1.9
NGC 4696	24.49 $\pm$ 0.27	1.30 (fixed)	25.05	32.95 $\pm$ 0.34	33.14 $\pm$ 0.16	2390 $\pm$ 300	-21.25 $\pm$ 0.2	7.3 $\pm$ 1.5
NGC 4709	23.86 $\pm$ 0.26	1.30 (fixed)	25.00	32.32 $\pm$ 0.33	32.50 $\pm$ 0.15	360 $\pm$ 60	-19.60 $\pm$ 0.2	5.0 $\pm$ 1.3

Source LaTeX | All tables | In the text

	1 Introduction
	2 The data
	3 Results
	4 Discussion
	5 Summary and conclusions
	References