Table 2
Photometric properties and dust extinction of each ISM region shown in Fig. 5.
| Region | SB(Lyα) | SB(UV) | Lyα contribution | UV contribution | Hα/Hβ |
|
| 10-14 erg s-1 cm-2 | 10-15 erg s-1 cm-2 Å-1 | |||||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) |
|
|
||||||
| Galaxy disk | −7.96 |
5.05 |
0%a | 76 % |
3.62 |
0.34 |
| Halo 1 | 4.40 |
0.76 |
56 % |
11 % |
3.09 |
0.11 |
| Halo 2 | 3.49 |
0.83 |
44 % |
12 % |
3.26 |
0.18 |
Notes.While the contribution in Lyα emission is shown in Col. 4, the UV contribution is shown in Col. 5 (both are derived from the analysis of the Lyα and UV maps of Mrk 1486; see Fig. 2). The nebular color excess (7) is measured from the Balmer decrement Hα/Hβ (6), assuming an intrinsic ratio of 2.86 for a 10 000 K gas (Case B, Osterbrock 1989) and the ratio determined using the SMC extinction law.
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