GRB 980425 host: [C II], [O I], and CO lines reveal recent enhancement of star formation due to atomic gas inflow

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Table A.1

Line and continuum fluxes and luminosities of each spaxel and the entire host.

[C ii]

[O i]

Reg

F_int

S/N

F_int

L′

F_int

S/N

F_int

L′

F_{100 μm}

L_FIR

(Jy km s^-1)

(10^-17 W m^-2)

(10⁵L_⊙)

(10⁶ Kkms^-1pc²)

(Jy km s^-1)

(10^-17 W m^-2)

(10⁵L_⊙)

(10⁶ Kkms^-1pc²)

(mJy)

(10⁶L_⊙)

(1)

(2)

(3)

(4)

(5)

(6)

(7)

(8)

(9)

(10)

(11)

(12)

(13)

Host

2073 ± 129

16.1

13.14 ± 0.82

55.9 ± 3.5

25.46 ± 1.58

262 ± 49

5.3

4.15 ± 0.78

17.7 ± 3.3

0.52 ± 0.10

327 ± 12

483.2 ± 5.6

37 ± 23

1.6

0.24 ± 0.15

1.0 ± 0.6

0.46 ± 0.29

8 ± 17

0.5

0.12 ± 0.27

0.5 ± 1.1

0.02 ± 0.03

9 ± 3

20.3 ± 6.6

115 ± 26

4.4

0.73 ± 0.17

3.1 ± 0.7

1.41 ± 0.32

13 ± 17

0.8

0.21 ± 0.28

0.9 ± 1.2

0.03 ± 0.03

20 ± 3

45.7 ± 6.6

73 ± 41

1.8

0.46 ± 0.26

2.0 ± 1.1

0.89 ± 0.50

−11 ± 11

−1.0

−0.17 ± 0.17

−0.7 ± 0.7

−0.02 ± 0.02

8 ± 3

17.4 ± 6.6

−110 ± 63

−1.7

−0.70 ± 0.40

−3.0 ± 1.7

−1.35 ± 0.78

−21 ± 14

−1.5

−0.33 ± 0.22

−1.4 ± 1.0

−0.04 ± 0.03

−3 ± 3

−7.2 ± 6.6

−66 ± 41

−1.6

−0.42 ± 0.26

−1.8 ± 1.1

−0.81 ± 0.51

6 ± 20

0.3

0.10 ± 0.32

0.4 ± 1.4

0.01 ± 0.04

−1 ± 3

−1.2 ± 6.6

94 ± 34

2.7

0.60 ± 0.22

2.5 ± 0.9

1.16 ± 0.42

−14 ± 32

−0.4

−0.22 ± 0.50

−0.9 ± 2.1

−0.03 ± 0.06

20 ± 3

45.8 ± 6.6

247 ± 34

7.2

1.57 ± 0.22

6.7 ± 0.9

3.04 ± 0.42

14 ± 17

0.9

0.23 ± 0.26

1.0 ± 1.1

0.03 ± 0.03

33 ± 3

75.4 ± 6.6

160 ± 30

5.4

1.02 ± 0.19

4.3 ± 0.8

1.97 ± 0.36

35 ± 15

2.3

0.55 ± 0.24

2.3 ± 1.0

0.07 ± 0.03

33 ± 3

74.7 ± 6.6

89 ± 30

3.0

0.57 ± 0.19

2.4 ± 0.8

1.10 ± 0.36

40 ± 14

2.9

0.63 ± 0.22

2.7 ± 0.9

0.08 ± 0.03

7 ± 3

16.5 ± 6.6

−28 ± 37

−0.8

−0.18 ± 0.23

−0.7 ± 1.0

−0.34 ± 0.45

14 ± 14

1.0

0.21 ± 0.21

0.9 ± 0.9

0.03 ± 0.03

3 ± 3

7.7 ± 6.6

96 ± 35

2.8

0.61 ± 0.22

2.6 ± 0.9

1.18 ± 0.43

32 ± 13

2.4

0.50 ± 0.21

2.1 ± 0.9

0.06 ± 0.03

24 ± 3

55.3 ± 6.6

197 ± 40

5.0

1.25 ± 0.25

5.3 ± 1.1

2.41 ± 0.49

27 ± 10

2.7

0.43 ± 0.16

1.8 ± 0.7

0.05 ± 0.02

39 ± 3

90.3 ± 6.6

249 ± 22

11.3

1.58 ± 0.14

6.7 ± 0.6

3.06 ± 0.27

8 ± 7

1.0

0.12 ± 0.12

0.5 ± 0.5

0.01 ± 0.01

47 ± 3

108.3 ± 6.6

221 ± 18

12.3

1.40 ± 0.11

6.0 ± 0.5

2.71 ± 0.22

29 ± 7

4.4

0.46 ± 0.10

1.9 ± 0.4

0.06 ± 0.01

40 ± 3

90.9 ± 6.6

−12 ± 34

−0.3

−0.07 ± 0.21

−0.3 ± 0.9

−0.14 ± 0.41

−0 ± 9

−0.1

−0.01 ± 0.14

−0.0 ± 0.6

−0.00 ± 0.02

11 ± 3

24.4 ± 6.6

81 ± 32

2.5

0.51 ± 0.20

2.2 ± 0.9

0.99 ± 0.39

−3 ± 14

−0.2

−0.05 ± 0.22

−0.2 ± 0.9

−0.01 ± 0.03

18 ± 3

42.2 ± 6.6

165 ± 34

4.8

1.04 ± 0.22

4.4 ± 0.9

2.02 ± 0.42

−10 ± 13

−0.8

−0.16 ± 0.20

−0.7 ± 0.9

−0.02 ± 0.03

22 ± 3

50.4 ± 6.6

158 ± 34

4.7

1.00 ± 0.21

4.3 ± 0.9

1.94 ± 0.41

35 ± 11

3.1

0.56 ± 0.18

2.4 ± 0.8

0.07 ± 0.02

33 ± 3

76.5 ± 6.6

91 ± 26

3.6

0.58 ± 0.16

2.4 ± 0.7

1.11 ± 0.31

59 ± 10

6.1

0.94 ± 0.16

4.0 ± 0.7

0.12 ± 0.02

56 ± 3

127.1 ± 6.6

−51 ± 24

−2.1

−0.32 ± 0.15

−1.4 ± 0.7

−0.62 ± 0.30

9 ± 16

0.5

0.14 ± 0.26

0.6 ± 1.1

0.02 ± 0.03

6 ± 3

13.3 ± 6.6

64 ± 44

1.4

0.40 ± 0.28

1.7 ± 1.2

0.78 ± 0.54

−20 ± 17

−1.2

−0.32 ± 0.26

−1.4 ± 1.1

−0.04 ± 0.03

4 ± 3

8.7 ± 6.6

81 ± 29

2.8

0.52 ± 0.19

2.2 ± 0.8

1.00 ± 0.36

16 ± 16

0.9

0.25 ± 0.26

1.0 ± 1.1

0.03 ± 0.03

12 ± 3

28.6 ± 6.6

83 ± 41

2.0

0.53 ± 0.26

2.2 ± 1.1

1.02 ± 0.50

7 ± 15

0.5

0.11 ± 0.23

0.4 ± 1.0

0.01 ± 0.03

10 ± 3

23.8 ± 6.6

38 ± 23

1.7

0.24 ± 0.15

1.0 ± 0.6

0.47 ± 0.28

16 ± 13

1.3

0.25 ± 0.20

1.1 ± 0.9

0.03 ± 0.03

5 ± 3

10.3 ± 6.6

−52 ± 43

−1.2

−0.33 ± 0.27

−1.4 ± 1.2

−0.64 ± 0.53

−48 ± 15

−3.2

−0.75 ± 0.24

−3.2 ± 1.0

−0.09 ± 0.03

1 ± 3

1.2 ± 6.6

Notes. (1) The entire host or the spaxel number. Columns (2)–(6) concern the [C ii] and (7)–(11) concern the [O i] line. (2, 7) Integrated flux within dotted lines in Figs. 2 and 3. (3, 8) Signal-to-noise ratio of the line. (4, 9) Integrated flux in W m^-2. (5, 10) Line luminosity in solar luminosity. (6, 11) Line luminosity using Eq. (3) in Solomon et al. (1997). (12) Flux at 100 μm. (13) Far-infrared (40–120 μm) luminosity.

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