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Table 2.

Properties of the sample computed for this work.

Object PA e RUV μ0, inner μ0, outer Rs, inner Rs, outer LR25 LRUV di (outer)
name [degrees] [arcsec] [mag] [mag] [arcsec] [arcsec] [mag abs] [mag abs]
NGC 0300 4.93 0.069 1325 22.46 24.81 159.51 242.27 –18.17 –18.26 25.89
NGC 0991 68.0 0.11 152 21.97 19.38 28.06 13.5 –18.67 –19.29 19.2
NGC 1042 71.0 0.17 263 22.22 19.78 52.06 26.87 –19.81 –20.11 20.86
NGC 1051 137.5 0.43 120 22.33 22.78 18.76 24.16 –18.32 –18.65 23.51
NGC 1140 106.69 0.3 182 20.03 25.07 9.41 45.62 –19 –19.12 27.31
NGC 1512 176.74 0.41 504 21.47 24.22 46.02 112.14 –19.84 –20.05 27.21
NGC 1672 29.34 0.06 330 20.64 19.75 44.41 41.15 –20.89 –20.98 21.37
NGC 2090 109.0 0.47 332 21.87 22.19 27.01 42.1 –19.53 –19.85 23.23
NGC 6902 56.86 0.32 344 21.63 23.95 25.04 61.14 –21.33 –21.72 28.41

Notes. The position angle and the ellipticity are chosen as described in Section 2.2; the RUV is chosen as described in Section 3.3.1. The PA is defined in this work from W to N. The central surface brightness and the scale length are computed as in Section 3. Typical uncertainties on μ0, g are a few tenths of the magnitude while the uncertainties for the rs are lower than 10%. The luminosity is calculated from the g-band profile within R25 and RUV. The diffuseness di is calculated from Equation (3), following Sprayberry et al. (1995).

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