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Table 6

Comparison of the observed and predicted intensities of some strong emission lines in Haro 11B and C.

Ion CLOUDY Observationsa
Bb Cb Bb Cb
I/I(Hβ) I/I(Hβ) I/I(Hβ) I/I(Hβ)
3727 [O ii]c 2.058 1.927 2.186 2.336
3869 [Ne iii] 0.283 0.321 0.299 0.314
4101 Hδ 0.264 0.267 0.277 0.269
4340 Hγ 0.472 0.475 0.499 0.461
4861 Hβ 1.000 1.000 1.000 1.000
4959 [O iii] 1.208 1.070 1.194 0.990
5007 [O iii] 3.635 3.220 3.716 3.172
6563 Hα 2.917 2.891 2.907 2.864
6583 [N ii] 0.342 0.381 0.488 0.576
6716 [S ii] 0.072 0.078 0.156 0.291
6731 [S ii] 0.051 0.055 0.102 0.134
9069 [S iii] 0.172 0.154 0.156 0.144
9532 [S iii] 0.426 0.382 0.432 0.385
10 829 He i 0.286 0.254 0.326 0.283
12 570 [Fe ii] 0.021 0.030 0.014 0.028
12 821 Paβ 0.164 0.161 0.144 0.176
16 436 [Fe ii] 0.018 0.025 0.012 0.017
19 450 Brδ 0.018 0.018 0.019 0.014
21 661 Brγ 0.028 0.027 0.031 0.028
MIR data for Haro 11
Ion Fd I/I(Hβ)e I/I(Hβ)f CLOUDY
10.51 μm [S iv] 4.395 0.122 0.365 0.224
12.81 μm [Ne ii] 3.123 0.087 0.259 0.097
15.55 μm [Ne iii] 9.814 0.273 0.814 0.466
18.71 μm [S iii] 4.524 0.126 0.376 0.206

Notes. 

(a)

Extinction-corrected fluxes.

(b)

B and C mean Haro 11B and Haro 11C, respectively.

(c)

Sum of the 3726 and 3728 [O ii] lines.

(d)

Observed flux in units of 10-13 erg s-1 cm-2 (Wu et al. 2008).

(e)

Extinction-corrected flux ratios with C(Hβ) = 0.745.

(f)

Extinction-corrected flux ratios with C(Hβ) = 0.27.

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