Open Access

Table C.5.

Metallicity measurements using multiple calibrations for individual regions within the galaxy.

Name catID C(H β) PG16S PG16Sedown PG16Seup PG16R PG16Redown PG16Reup N2 N2edown N2eup O3N2 O3N2edown O3N2eup
ESO097-013 ESO097-013-247 0.43 8.64 0.04 0.03 8.85 0.06 0.06 8.77 0.03 0.03
NGC 0628a 266 0.2 8.61 0.28 0.42
NGC 3381 14 0.22 8.47 0.01 0.02 8.55 0.01 0.02 8.67 0.02 0.02 8.72 0.02 0.02
NGC 4038 NGC 4038-3-62 0.21 8.559 0.006 0.006 8.77 0.01 0.01 8.728 0.005 0.005
NGC 4651 NGC 4651-89 0.46 8.5 0.06 0.07 8.55 0.1 0.11 8.49 0.07 0.06
NGC 5236 NGC 5236-19 0.32 8.61 0.02 0.02 8.77 0.03 0.03 8.77 0.01 0.01
NGC 5457 1323-52797-0052 0.26 8.37 0.03 0.03 8.5 0.03 0.03 8.43 0.02 0.02
NGC 5480 50 0.3 8.48 0.01 0.01 8.57 0.02 0.02 8.68 0.01 0.01 8.79 0.02 0.02
NGC 7320 10 0.06 8.26 0.05 0.06 8.21 0.08 0.09 8.37 0.05 0.05 8.41 0.05 0.04
UGC 09299 1886 1.97 8.21 8.39 8.51

Name IZI IZIedown IZIeup IZIchi2 KK04 KK04edown KK04eup T04 T04edown T04eup ONPG16 ONPG16edown ONPG16eup r/r25 r/rapp Sample

ESO097-013 8.83 0.18 0.06 0.23 9.05 0.03 0.03 0.07 0.04 MUSE
NGC 0628 8.8 0.74 0.16 0.02 0.46 0.23 Sanchez12
NGC 3381 8.64 0.21 0.15 0.03 9.03 0.02 0.02 8.99 0.02 0.02 −0.88 0.03 0.03 0.73 0.35 CALIFA
NGC 4038 8.69 0.18 0.1 0.16 9.002 0.005 0.005 0.06 0.04 MUSE
NGC 4651 8.59 0.23 0.15 0.13 8.73 0.07 0.06 0.49 0.19 MUSE
NGC 5236 8.86 0.15 0.05 0.12 9.06 0.01 0.01 0.32 0.18 MUSE
NGC 5457 8.44 0.06 0.06 2.72 8.65 0.02 0.02 0.63 0.43 SDSS
NGC 5480 8.78 0.31 0.1 0.04 9.09 0.03 0.02 9.07 0.02 0.02 −0.79 0.05 0.07 0.56 0.18 CALIFA
NGC 7320 8.38 0.11 0.18 0.49 8.57 0.29 0.2 8.64 0.05 0.04 −1.36 0.08 0.08 0.58 0.71 Rodr14
UGC 09299 8.75 0.25 0.06 SAMI

Notes. The same ten randomly selected regions are shown as in Table C.3. Each of the metallicity columns are labeled by the abbreviation of their calibration (see Sect. 3), and are given in 12+log(O/H) together with their asymmetric uncertainties. rr25 and rrapp give the deprojected radius of the regiondivided by r25 and rapp (photometry aperture radius) respectively.

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