A spatially resolved study of ionized regions in galaxies at different ...
A spatially resolved study of ionized regions in galaxies at different ... A spatially resolved study of ionized regions in galaxies at different ...
160 Appendix A where c=0.434C. This value is the reddening constant, and is found in the literature as c(Hβ), the logarithmic extinction at Hβ (F Hβ = F Hβ0 10 −c ). We can rearrange equation A.2 as F λ = F λ0 10 −c(λ) = F λ0 10 −c(Hβ)(1+g(λ)) (A.3) where g(λ) = f(λ) - f(Hβ) and c(Hβ) the logarithmic extinction at Hβ, which can be written as c(Hβ) = 0.4A Hβ . Comparing equation A.3 with A.1 and taking into account the reddening curve ζ(λ), g(λ) = A λ A β − 1 = ζ(λ) ζ(λ Hβ ) − 1 (A.4) Finally, we can write the logarithmic extinction at any wavelength c(λ) as a function of the reddening curve c(λ) = c(Hβ)(1 + g(λ)) = c(Hβ) ζ(λ) ζ(λ Hβ ) (A.5) We can also write the constant of reddening in terms of the color excess c(Hβ) = 0.4A Hβ = 0.4ζ(λ Hβ )R V E(B − V ) (A.6) Taking into account the reddening law of Cardelli et al. (1989) and a value of R V = 3.1, we obtain A Hβ /A V = ζ(λ Hβ ) = 1.164, which allows to write the reddening constant as a function of the color excess as c(Hβ) = 1.443 E(B-V). Another way of estimating the extinction is by relating the visual extinction to the observed ratio of two lines. This method is useful when only Hα and Hβ are available. The relation is given by: and re-arranging it gives F Hα F Hβ = F Hα0 · 10 −0.4A Hα F Hβ0 · 10 −0.4A Hβ = F Hα0 F Hβ0 · 10 0.4 A Hβ −A Hα A V ·A V (A.7) A V = 2.5 · ( ) FHα /F log Hβ 10 F Hα0 /F Hβ0 A Hβ −A Hα A V (A.8)
Appendix B Physical conditions of the gas and abundances All equations employed in the calculation of the physical conditions of the gas and abundances are reproduced in this Appendix. Only the temperatures and elements involved in this work are listed. B.1 Physical conditions of the gas The electron density and temperatures of the ionized gas have been derived using the same procedures as in Pérez-Montero and Díaz (2003), based on the five-level statistical equilibrium atom approximation in the task temden, of the software package IRAF (De Robertis et al., 1987; Shaw and Dufour, 1995). The atomic coefficients used here are the same as in Pérez-Montero and Díaz (2003), except in the case of O + for which the transition probabilities from Zeippen (1982) and the collision strengths from Pradhan (1976) have been used, which offer more reliable nebular diagnostic results for this species (Wang et al., 2004). Adequate fitting functions have been derived from the temden task. They are given below. B.1.1 Density Sulphur The electron density can be derived from the [Sii] λλ 6717 / 6731 Å line ratio, through the R S2 parameter, which is defined as: 161
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- Page 210 and 211: 190 REFERENCES Bertelli, G., Bressa
- Page 212 and 213: 192 REFERENCES Girardi, L. & Bertel
- Page 214 and 215: 194 REFERENCES Kunth, D. & Sargent,
- Page 216 and 217: 196 REFERENCES Pérez-Montero, E.,
- Page 218 and 219: 198 REFERENCES Terlevich, R., Melni
Appendix<br />
B<br />
Physical conditions <strong>of</strong> the gas<br />
and abundances<br />
All equ<strong>at</strong>ions employed <strong>in</strong> the calcul<strong>at</strong>ion <strong>of</strong> the physical conditions <strong>of</strong> the gas and abundances<br />
are reproduced <strong>in</strong> this Appendix. Only the temper<strong>at</strong>ures and elements <strong>in</strong>volved <strong>in</strong><br />
this work are listed.<br />
B.1 Physical conditions <strong>of</strong> the gas<br />
The electron density and temper<strong>at</strong>ures <strong>of</strong> the <strong>ionized</strong> gas have been derived us<strong>in</strong>g the<br />
same procedures as <strong>in</strong> Pérez-Montero and Díaz (2003), based on the five-level st<strong>at</strong>istical<br />
equilibrium <strong>at</strong>om approxim<strong>at</strong>ion <strong>in</strong> the task temden, <strong>of</strong> the s<strong>of</strong>tware package IRAF (De<br />
Robertis et al., 1987; Shaw and Dufour, 1995). The <strong>at</strong>omic coefficients used here are the<br />
same as <strong>in</strong> Pérez-Montero and Díaz (2003), except <strong>in</strong> the case <strong>of</strong> O + for which the transition<br />
probabilities from Zeippen (1982) and the collision strengths from Pradhan (1976) have been<br />
used, which <strong>of</strong>fer more reliable nebular diagnostic results for this species (Wang et al., 2004).<br />
Adequ<strong>at</strong>e fitt<strong>in</strong>g functions have been derived from the temden task. They are given below.<br />
B.1.1 Density<br />
Sulphur<br />
The electron density can be derived from the [Sii] λλ 6717 / 6731 Å l<strong>in</strong>e r<strong>at</strong>io, through the<br />
R S2 parameter, which is def<strong>in</strong>ed as:<br />
161
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