Table 1: IRS spectrum of NGC 3242. The measured line intensity is given in Col. 3. The last column gives the ratio of the line intensity to H$\beta $(=100).
Identification $\lambda $($\mu $m) Intensity $^{\dagger}$ I/H$\beta $
[Ar III] 8.992 904 $\pm$ 30 8.48
  10.511 8220 $\pm$ 160 70.3
H I(9-7) 11.306 38.4 $\pm$ 2.3 0.22
  11.760 70.8 $\pm$ 3.5 0.616
H I (7-6 + 11-8) 12.370 112.1 $\pm$ 4.6  
  12.810 150 $\pm$ 3.9 1.31
  13.099 81.5 $\pm$ 4.7 0.710
  14.319 35.6 $\pm$ 1.6 0.31
  15.553 13 320 $\pm$ 216 116.0
H I (10-8) 16.203 14.2 $\pm$ 3.4 0.15
H2 16.881 17.3 $\pm$ 9.7  
H2 16.976 5.2 $\pm$ 3.3  
  17.890 37.0 $\pm$ 2.0 0.322
  18.711 957 $\pm$ 22 8.33
H I (8-7) 19.065 43.0 $\pm$ 5.0 0.401
  20.312 57.0 $\pm$ 2.66 0.497
  21.818 39.6 $\pm$ 6.4 0.345
  25.884 15 724 $\pm$ 278 137
  33.473 363: $\pm$ 22 3.16:
  36.014 785: $\pm$ 98 6.84:
[O III] 51.8 34 700 $\pm$ 1400 162
  57.3 3100 $\pm$ 140 14.5
  88.4 15 500 $\pm$ 430 72.4
$^{\dagger}$ Intensities measured in units of 10-14 erg cm-2 s-1. The intensities below 19 $\mu $m have been increased by a factor of 3.96 to bring them on the same scale as the LH intensities measured through a larger diaphragm. The intensities below 10 $\mu $m are measured with the low resolution instrument.
: Indicates an uncertain value.
The last three measurements are taken from ISO.

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