Table 1.
Basic properties of FCC 47 and its nuclear star cluster.
FCC 47 | Notes | |
---|---|---|
Morphological type | S0 | 1 |
Distance [Mpc] | 18.3 ± 0.6 | 2 |
Physical scale [pc arcsec−1] | 88.7 | |
Inclination [°] | 47 ± 4 | 3 |
Effective radius [kpc] | 2.60 | 4 |
σe, star [km s−1] | 95 ± 5 | 5 |
σ0, star [km s−1] | 106 ± 5 | 5 |
Galaxy stellar mass [M⊙] | (1.0 ± 0.1)×1010 | 6 |
NSC | ||
Effective radius [pc] | 66.5 ± 11.1 | 7 |
NSC mass [M⊙] | (7 ± 1.4)×108 | 8 |
Notes. 1: de Vaucouleurs et al. (1991). 2: Blakeslee et al. (2009) using surface-brightness fluctuation measurements. 3: the inclination corresponds to the θ viewing angle of our triaxial Schwarzschild orbit-superposition models. 4: derived by applying the routine mge_half_light_isophote of the Jeans Anisotropic Modelling package (Cappellari 2008) on our surface brightness model (Sect. 3.1). For comparison, Ferguson (1989) found 2.66 kpc. 5: effective velocity dispersion and central velocity dispersion derived by co-adding the spectra of the large-scale optical IFU data in elliptical annuli of the size of the effective radius and 1 arcsec, respectively. 6: The galaxy stellar mass (M*, gal) was derived using the dynamical Schwarzschild orbit-superposition model with varying stellar populations and varying IMF. The mass does not change significantly for the other mass models. For comparison, Liu et al. (2019) derived M*, gal = 9.3 × 109 M⊙ using a colour-based stellar M*/L and Fahrion et al. (2019b) derived M*, gal = 1.6 × 1010 M⊙ using triaxial Schwarzschild models. 7: Turner et al. (2012) fitted a double Sersić profile fit to the HST F475W filter image. 8: Fahrion et al. (2019b) using stellar population models.
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