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Table 1:

IRS spectrum of NGC 6210.
Identification $\lambda$($\mu$m) Intensity $^{\dagger}$ I/H$\beta$
H I(9-6)+[K IV] 5.94 79.6 $\pm$ 28 0.72
H I (12-7) 6.77 17 $\pm$ 0.4  
  6.98 83 $\pm$ 4.5 0.76
  7.31 53 $\pm$ 2.9 0.47
H I(6-5) 7.47 301 $\pm$ 17  
  8.99 1610 $\pm$ 52 14.7
  10.506 16700 $\pm$ 250 152
H I(9-7) 11.305 48.2 $\pm$ 1.2  
  11.757 90.1 $\pm$ 3.7 0.82
H I (7-6+11-8) 12.368 114 $\pm$ 4  
  12.808 498 $\pm$ 40 4.55
H 1 (13-9) 14.180 7.1 $\pm$ 0.9  
  14.359 4.74 $\pm$ 0.6 0.043
  15.548 18500 $\pm$ 1500 169
H I (10-8) 16.210 12.4 $\pm$ 2.4  
  17.885 22.7 $\pm$ 2.2 0.21
  18.707 2820 $\pm$ 120 25.7
  20.310 48.7: $\pm$ 6.6 0.45:
  21.814 79.5 $\pm$ 10.5 0.72
  22.924 31.9 $\pm$ 3.9 0.29
  25.884 777 $\pm$ 21 7.10
  33.014 34.5: $\pm$ 2.7 0.31
  33.470 890 $\pm$ 10.7 8.14
  34.809 33.6 $\pm$ 6.3 0.30
  36.001 1590 $\pm$ 24 14.5
$^{\dagger}$ 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 1.77 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 and are brought to the same scale by matching the [S IV] and [Ne II] lines.
: Indicates an uncertain value.
The measured line intensity is given in Col. 3. The last column gives the ratio of the line intensity to H$\beta$(=100).

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