Table 2
Unextinction corrected Brγ, Paβ, [FeII]1.26, and [FeII]1.64 fluxes with the AV derived by the Paβ/Brγ intrinsic line ratio.
| Galaxy | Paβ | Brγ | [FeII]1.26 | [FeII]1.64 | AvBrγa |
| 10-14 (erg s-1 cm-2) | 10-14 (erg s-1 cm-2) | 10-14 (erg s-1 cm-2) | 10-14 (erg s-1 cm-2) | (mag) | |
|
|
|||||
| NGC 3628 | 0.7 | 1.4 | 1.4 | 0.6 | 20.3 |
| NGC 4536 | 12.7 | 3.5 | 3.4 | 4.5 | 3.9 |
| NGC 1792 | 1.3 | 0.3 | 0.1 | – | 2.9 |
| NGC 1084 | 1.0 | 0.3 | 0.3 | 0.5 | 3.0 |
| NGC 1808 | 18.3 | 4.4 | 9.2 | 8.0 | 2.7 |
| NGC 520 | 1.2 | 1.3 | 1.2 | 0.3 | 15.3 |
| NGC 7552 | 20.7 | 6.8 | 6.3 | 8.1 | 5.3 |
| NGC 7632 | 1.8 | 0.5 | 0.5 | 0.8 | 3.9 |
| NGC 1614 | 13.8 | 3.5 | 3.1 | 3.7 | 3.3 |
| NGC 6240 | 3.3 | 0.6 | 8.5 | 8.7 | 15.6 |
| Arp 220 | 0.4 | 0.5 | 0.7 | – | 15.4 |
Notes. All measurements have a 10% error, which is the estimated calibration uncertainty. NGC 1792 has a 20% error due to the low signal to noise of this observation.
AV is determined assuming using the near-infrared extinction law Aλ ∝ λ-1.8 (Martin & Whittet 1990). Although the measured AV is very high in some galaxies, the extinction measured in the NIR wavelength range is significantly less.
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