Table 1.

Parameter dependence of the mass–metallicity relation. For each parameter and stellar mass bin, the median values are listed.

IDlog(M/M)12+log(O/H) [N2] ([N2+R23])SFR (M yr−1)|$D_{\rm n}(4000)$|E(BV)Gas fractionNa
18.96 ± 0.038.06 ± 0.12 (8.15 ± 0.14)8.3 ± 2.20.69 ± 0.040.08 ± 0.040.61 ± 0.0525 (24)
29.12 ± 0.058.14 ± 0.07 (8.23 ± 0.10)9.7 ± 2.40.77 ± 0.070.08 ± 0.050.55 ± 0.0668 (61)
39.28 ± 0.058.24 ± 0.07 (8.39 ± 0.10)13.2 ± 3.40.85 ± 0.060.11 ± 0.040.52 ± 0.0798 (90)
49.48 ± 0.048.31 ± 0.06 (8.47 ± 0.08)15.0 ± 5.40.91 ± 0.060.13 ± 0.040.46 ± 0.0892 (86)
59.70 ± 0.048.40 ± 0.05 (8.60 ± 0.07)15.6 ± 4.20.98 ± 0.040.17 ± 0.040.36 ± 0.0699 (97)
69.90 ± 0.058.47 ± 0.04 (8.69 ± 0.06)16.5 ± 4.91.02 ± 0.030.20 ± 0.050.29 ± 0.07117 (115)
710.09 ± 0.068.53 ± 0.05 (8.77 ± 0.08)19.3 ± 5.11.05 ± 0.030.23 ± 0.050.22 ± 0.0582 (80)
810.28 ± 0.058.55 ± 0.04 (8.80 ± 0.05)27.9 ± 9.71.05 ± 0.030.27 ± 0.040.20 ± 0.0559 (59)
910.48 ± 0.058.59 ± 0.02 (8.85 ± 0.05)34.0 ± 7.81.07 ± 0.020.30 ± 0.050.16 ± 0.0334 (33)
IDlog(M/M)12+log(O/H) [N2] ([N2+R23])SFR (M yr−1)|$D_{\rm n}(4000)$|E(BV)Gas fractionNa
18.96 ± 0.038.06 ± 0.12 (8.15 ± 0.14)8.3 ± 2.20.69 ± 0.040.08 ± 0.040.61 ± 0.0525 (24)
29.12 ± 0.058.14 ± 0.07 (8.23 ± 0.10)9.7 ± 2.40.77 ± 0.070.08 ± 0.050.55 ± 0.0668 (61)
39.28 ± 0.058.24 ± 0.07 (8.39 ± 0.10)13.2 ± 3.40.85 ± 0.060.11 ± 0.040.52 ± 0.0798 (90)
49.48 ± 0.048.31 ± 0.06 (8.47 ± 0.08)15.0 ± 5.40.91 ± 0.060.13 ± 0.040.46 ± 0.0892 (86)
59.70 ± 0.048.40 ± 0.05 (8.60 ± 0.07)15.6 ± 4.20.98 ± 0.040.17 ± 0.040.36 ± 0.0699 (97)
69.90 ± 0.058.47 ± 0.04 (8.69 ± 0.06)16.5 ± 4.91.02 ± 0.030.20 ± 0.050.29 ± 0.07117 (115)
710.09 ± 0.068.53 ± 0.05 (8.77 ± 0.08)19.3 ± 5.11.05 ± 0.030.23 ± 0.050.22 ± 0.0582 (80)
810.28 ± 0.058.55 ± 0.04 (8.80 ± 0.05)27.9 ± 9.71.05 ± 0.030.27 ± 0.040.20 ± 0.0559 (59)
910.48 ± 0.058.59 ± 0.02 (8.85 ± 0.05)34.0 ± 7.81.07 ± 0.020.30 ± 0.050.16 ± 0.0334 (33)

Note.aNumber of galaxies in each stellar mass bin. The value in parentheses is presented for LBAs which have metallicity determined by using the N2+R23 calibration method.

Table 1.

Parameter dependence of the mass–metallicity relation. For each parameter and stellar mass bin, the median values are listed.

IDlog(M/M)12+log(O/H) [N2] ([N2+R23])SFR (M yr−1)|$D_{\rm n}(4000)$|E(BV)Gas fractionNa
18.96 ± 0.038.06 ± 0.12 (8.15 ± 0.14)8.3 ± 2.20.69 ± 0.040.08 ± 0.040.61 ± 0.0525 (24)
29.12 ± 0.058.14 ± 0.07 (8.23 ± 0.10)9.7 ± 2.40.77 ± 0.070.08 ± 0.050.55 ± 0.0668 (61)
39.28 ± 0.058.24 ± 0.07 (8.39 ± 0.10)13.2 ± 3.40.85 ± 0.060.11 ± 0.040.52 ± 0.0798 (90)
49.48 ± 0.048.31 ± 0.06 (8.47 ± 0.08)15.0 ± 5.40.91 ± 0.060.13 ± 0.040.46 ± 0.0892 (86)
59.70 ± 0.048.40 ± 0.05 (8.60 ± 0.07)15.6 ± 4.20.98 ± 0.040.17 ± 0.040.36 ± 0.0699 (97)
69.90 ± 0.058.47 ± 0.04 (8.69 ± 0.06)16.5 ± 4.91.02 ± 0.030.20 ± 0.050.29 ± 0.07117 (115)
710.09 ± 0.068.53 ± 0.05 (8.77 ± 0.08)19.3 ± 5.11.05 ± 0.030.23 ± 0.050.22 ± 0.0582 (80)
810.28 ± 0.058.55 ± 0.04 (8.80 ± 0.05)27.9 ± 9.71.05 ± 0.030.27 ± 0.040.20 ± 0.0559 (59)
910.48 ± 0.058.59 ± 0.02 (8.85 ± 0.05)34.0 ± 7.81.07 ± 0.020.30 ± 0.050.16 ± 0.0334 (33)
IDlog(M/M)12+log(O/H) [N2] ([N2+R23])SFR (M yr−1)|$D_{\rm n}(4000)$|E(BV)Gas fractionNa
18.96 ± 0.038.06 ± 0.12 (8.15 ± 0.14)8.3 ± 2.20.69 ± 0.040.08 ± 0.040.61 ± 0.0525 (24)
29.12 ± 0.058.14 ± 0.07 (8.23 ± 0.10)9.7 ± 2.40.77 ± 0.070.08 ± 0.050.55 ± 0.0668 (61)
39.28 ± 0.058.24 ± 0.07 (8.39 ± 0.10)13.2 ± 3.40.85 ± 0.060.11 ± 0.040.52 ± 0.0798 (90)
49.48 ± 0.048.31 ± 0.06 (8.47 ± 0.08)15.0 ± 5.40.91 ± 0.060.13 ± 0.040.46 ± 0.0892 (86)
59.70 ± 0.048.40 ± 0.05 (8.60 ± 0.07)15.6 ± 4.20.98 ± 0.040.17 ± 0.040.36 ± 0.0699 (97)
69.90 ± 0.058.47 ± 0.04 (8.69 ± 0.06)16.5 ± 4.91.02 ± 0.030.20 ± 0.050.29 ± 0.07117 (115)
710.09 ± 0.068.53 ± 0.05 (8.77 ± 0.08)19.3 ± 5.11.05 ± 0.030.23 ± 0.050.22 ± 0.0582 (80)
810.28 ± 0.058.55 ± 0.04 (8.80 ± 0.05)27.9 ± 9.71.05 ± 0.030.27 ± 0.040.20 ± 0.0559 (59)
910.48 ± 0.058.59 ± 0.02 (8.85 ± 0.05)34.0 ± 7.81.07 ± 0.020.30 ± 0.050.16 ± 0.0334 (33)

Note.aNumber of galaxies in each stellar mass bin. The value in parentheses is presented for LBAs which have metallicity determined by using the N2+R23 calibration method.

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