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Table 1

Physical properties of each spaxel and the entire host.

Reg SF RIR SF R[CII] SF R[OI] n G0 MH2, [CII]
(M⊙ yr-1) (M⊙ yr-1) (M⊙ yr-1) (cm-3) (106M⊙)
(1) (2) (3) (4) (5) (6) (7)
Host 0.260 ± 0.080 0.668 ± 0.040 0.287 ± 0.054 127.3 ± 7.9
44 0.008 ± 0.002 0.012 ± 0.007 0.009 ± 0.019 ··· ··· 2.3 ± 1.4
43 0.017 ± 0.002 0.036 ± 0.008 0.015 ± 0.019 7.1 ± 1.6
42 0.006 ± 0.002 0.023 ± 0.013 −0.012 ± 0.012 ··· ··· 4.5 ± 2.5
41 −0.003 ± 0.002 −0.034 ± 0.020 −0.023 ± 0.015 ··· ··· −6.8 ± 3.9
40 −0.000 ± 0.002 −0.021 ± 0.013 0.007 ± 0.022 ··· ··· −4.1 ± 2.5
34 0.017 ± 0.002 0.029 ± 0.011 −0.015 ± 0.035 ··· ··· 5.8 ± 2.1
33 0.028 ± 0.002 0.078 ± 0.011 0.016 ± 0.018 15.2 ± 2.1
32 0.028 ± 0.002 0.050 ± 0.009 0.038 ± 0.016 9.9 ± 1.8
31 0.006 ± 0.002 0.028 ± 0.009 0.044 ± 0.015 5.5 ± 1.8
30 0.003 ± 0.002 −0.009 ± 0.011 0.015 ± 0.015 ··· ··· −1.7 ± 2.2
24 0.021 ± 0.002 0.030 ± 0.011 0.035 ± 0.014 ··· ··· 5.9 ± 2.1
23 0.034 ± 0.002 0.062 ± 0.012 0.030 ± 0.011 12.1 ± 2.4
22 0.040 ± 0.002 0.079 ± 0.007 0.008 ± 0.008 15.3 ± 1.4
21 0.034 ± 0.002 0.070 ± 0.006 0.032 ± 0.007 13.6 ± 1.1
20 0.009 ± 0.002 −0.004 ± 0.010 −0.000 ± 0.010 ··· ··· −0.7 ± 2.1
14 0.016 ± 0.002 0.025 ± 0.010 −0.004 ± 0.015 ··· ··· 5.0 ± 2.0
13 0.019 ± 0.002 0.052 ± 0.011 −0.011 ± 0.014 10.1 ± 2.1
12 0.028 ± 0.002 0.050 ± 0.010 0.038 ± 0.012 9.7 ± 2.1
11 0.047 ± 0.002 0.028 ± 0.008 0.065 ± 0.011 5.6 ± 1.6
10 0.005 ± 0.002 −0.016 ± 0.007 0.009 ± 0.018 ··· ··· −3.1 ± 1.5
04 0.003 ± 0.002 0.020 ± 0.014 −0.022 ± 0.018 ··· ··· 3.9 ± 2.7
03 0.011 ± 0.002 0.025 ± 0.009 0.017 ± 0.018 ··· ··· 5.0 ± 1.8
02 0.009 ± 0.002 0.026 ± 0.013 0.007 ± 0.016 ··· ··· 5.1 ± 2.5
01 0.004 ± 0.002 0.012 ± 0.007 0.017 ± 0.014 ··· ··· 2.4 ± 1.4
00 0.000 ± 0.002 −0.016 ± 0.013 −0.052 ± 0.016 ··· ··· −3.2 ± 2.6

Notes. (1) The entire host or the spaxel number. (2) Star formation rates (SFRs) from the total (8–1000 μm) luminosity using SFR/M⊙ yr-1 = 10-10LIR/L⊙ assuming the Chabrier (2003) initial mass function. (3), (4) SFRs from the [C ii] and [O i] lines, respectively, using the calibration of De Looze et al. (2014). (5) Gas density. (6) Strength of the interstellar radiation field in Habing unit (solar neighbourhood value), both derived via the PDR modelling (Sect. 3). (7) Molecular gas mass estimated assuming (see Sect. 3) and the Galactic CO-to-H2 conversion factor αCO = 5 M⊙/ (K km s-1 pc2).

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