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 ...
164 Appendix B Sulphur As in the case of [Oii], the temperature of [Sii] depends on density (np 3 ions). The ratio used to estimate t([Sii]) is R ′ S2 = I(6717Å) + I(6731Å) I(4068Å) + I(4076Å) If one of the [Sii] auroral lines cannot be measured, the theoretical ratio can be used, I(4068Å) ≈ 3 · I(4067Å). Then, the temperature is calculated where t([Sii]) = a 0 (n) + a 1 (n) · R ′ S2 + a 2(n) R ′ S2 + a 3(n) R ′ S2 a 0 (n) = 1.92 − 0.0017 · n − 0.848 n a 1 (n) = −0.0375 − 0.0185 n a 2 (n) = −14.15 + 0.019 · n − 10.4 n a 3 (n) = −105.64 + 0.019 · n − 58.52 n Direct measurements of the [Siii] temperature have been possible with the availability of the collisional lines in the near IR. The ratio is: R S3 = I(9069Å) + I(9532Å) I(6312Å) This expression can be simplified in case of lacking one of the near IR lines, using the theoretical ratio I(9532Å) ≈ 2.44 · I(9069Å). The temperature can be calculated by the fit: t([Siii]) = R S3 + 36.4 1.8 · R S3 − 3.01 B.2 Ionic abundances The derived fittings to the ionic task results following the functional form given by Pagel et al. (1992) for each element are listed below. In all relations t denotes the appropriate line electron temperature, in units of 10 4 K, corresponding to the assumed ionization structure, and n the electron density.
B • Physical conditions of the gas and abundances 165 Oxygen The chemical abundance of O + can be determined from the intensity of the [Oii] λλ 3727, 3729 Å lines: ( ) I(3727 + 3729) 12+log(O + /H + ) = log +5.992+ 1.583 −0.681·log t+log(1+0.00023·n) I(Hβ) t For the O 2+ abundance, [Oiii] λλ 4959,5007 Å lines are used: ( ) I(4959 + 5007) 12 + log(O 2+ /H + ) = log + 6.144 + 1.251 − 0.55 · log t I(Hβ) t Sulphur The abundance of the S + is obtained from the 6717,6731 Å lines: ( ) I(6717 + 6731) 12 + log(S + /H + ) = log + 5.423 + 0.929 − 0.28 · log t + 0.0001 · n I(Hβ) t When the [Sii] auroral lines are not available, it is usually assumed that t[Sii] ≈ t[Oii], although there is evidence suggesting a somewhat lower value. The abundance is obtained from the 9069,9532 Å lines for S 2+ : ( ) I(9069 + 9532) 12 + log(S 2+ /H + ) = log + 5.8 + 0.771 − 0.22 · log t I(Hβ) t Nitrogen The N + abundance can be calculated from the 6548 and 6584 Å lines: ( ) I(6548 + 6584) 12 + log(N + /H + ) = log + 6.273 + + 0.894 − 0.592 · log t I(Hβ) t Given the proximity to Hα, if one of them cannot be measured the theoretical relation I(6584Å) ≈ 2.9 · I(6548Å) can be used. Neon The [Neiii] line at 3868 Å is used for neon: 12 + log(Ne 2+ /H + ) = log ( ) I(3868) + 6.486 + 1.558 − 0.504 · log t I(Hβ) t For this ion, the assumption t([Neiii]) ≈ t([Oiii]) is usually adopted.
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- Page 180 and 181: 160 Appendix A where c=0.434C. This
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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
B • Physical conditions <strong>of</strong> the gas and abundances 165<br />
Oxygen<br />
The chemical abundance <strong>of</strong> O + can be determ<strong>in</strong>ed from the <strong>in</strong>tensity <strong>of</strong> the [Oii] λλ 3727,<br />
3729 Å l<strong>in</strong>es:<br />
( )<br />
I(3727 + 3729)<br />
12+log(O + /H + ) = log<br />
+5.992+ 1.583 −0.681·log t+log(1+0.00023·n)<br />
I(Hβ)<br />
t<br />
For the O 2+ abundance, [Oiii] λλ 4959,5007 Å l<strong>in</strong>es are used:<br />
( )<br />
I(4959 + 5007)<br />
12 + log(O 2+ /H + ) = log<br />
+ 6.144 + 1.251 − 0.55 · log t<br />
I(Hβ)<br />
t<br />
Sulphur<br />
The abundance <strong>of</strong> the S + is obta<strong>in</strong>ed from the 6717,6731 Å l<strong>in</strong>es:<br />
( )<br />
I(6717 + 6731)<br />
12 + log(S + /H + ) = log<br />
+ 5.423 + 0.929 − 0.28 · log t + 0.0001 · n<br />
I(Hβ)<br />
t<br />
When the [Sii] auroral l<strong>in</strong>es are not available, it is usually assumed th<strong>at</strong> t[Sii] ≈ t[Oii],<br />
although there is evidence suggest<strong>in</strong>g a somewh<strong>at</strong> lower value.<br />
The abundance is obta<strong>in</strong>ed from the 9069,9532 Å l<strong>in</strong>es for S 2+ :<br />
( )<br />
I(9069 + 9532)<br />
12 + log(S 2+ /H + ) = log<br />
+ 5.8 + 0.771 − 0.22 · log t<br />
I(Hβ)<br />
t<br />
Nitrogen<br />
The N + abundance can be calcul<strong>at</strong>ed from the 6548 and 6584 Å l<strong>in</strong>es:<br />
( )<br />
I(6548 + 6584)<br />
12 + log(N + /H + ) = log<br />
+ 6.273 + + 0.894 − 0.592 · log t<br />
I(Hβ)<br />
t<br />
Given the proximity to Hα, if one <strong>of</strong> them cannot be measured the theoretical rel<strong>at</strong>ion<br />
I(6584Å) ≈ 2.9 · I(6548Å) can be used.<br />
Neon<br />
The [Neiii] l<strong>in</strong>e <strong>at</strong> 3868 Å is used for neon:<br />
12 + log(Ne 2+ /H + ) = log<br />
( ) I(3868)<br />
+ 6.486 + 1.558 − 0.504 · log t<br />
I(Hβ)<br />
t<br />
For this ion, the assumption t([Neiii]) ≈ t([Oiii]) is usually adopted.
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