The nature of absorbers at high redshift

C. Fechner; P. Richter

doi:10.1051/0004-6361/200810421

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Volume 496 / No 1 (March II 2009)

A&A, 496 1 (2009) 31-44

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Issue		A&A Volume 496, Number 1, March II 2009


Page(s)		31 - 44
Section		Cosmology (including clusters of galaxies)
DOI		https://doi.org/10.1051/0004-6361/200810421
Published online		30 January 2009

Online Material

Appendix A: N V systems

$\begin{figure}\par\resizebox{9cm}{!}{\includegraphics[bb=33 485 373 780,clip=]{0421fga1.ps}}\par \end{figure}$	Figure A.1: Intervening system at z=1.5771 towards HE 0001-2340. Smooth lines indicate the profiles for the favorite HM01 model.
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$\begin{figure}\par\resizebox{9cm}{!}{\includegraphics[bb=33 220 373 780,clip=]{0421fga2.ps}} \end{figure}$	Figure A.2: Intervening system at z=1.5855 towards PKS 1448-232. Smooth lines indicate the profiles for the HM01 model. This system has a least two gas phases where the gas phase giving rise to features of low-ionization species is not included into the model.
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$\begin{figure}\par\resizebox{9cm}{!}{\includegraphics[bb=33 435 373 780,clip=]{0421fga3.ps}} \end{figure}$	Figure A.3: Intervening system at z=1.5966 towards PKS 0237-23. Smooth lines indicate the profiles for the favorite HM01 model.
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$\begin{figure}\par\resizebox{9cm}{!}{\includegraphics[bb=33 540 373 780,clip=]{0421fga4.ps}} \end{figure}$	Figure A.4: Intervening system at z=1.7236 towards PKS 1448-232. Smooth lines indicate the profiles for the favorite HM01 model.
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$\begin{figure}\par\resizebox{9cm}{!}{\includegraphics[bb=33 485 373 780,clip=]{0421fga5.ps}} \end{figure}$	Figure A.5: Intervening system at z=1.9656 towards HE 2217-2818. Smooth lines indicate the profiles for the favorite HM01 model.
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$\begin{figure}\par\resizebox{9cm}{!}{\includegraphics[bb=33 165 373 780,clip=]{0421fga6.ps}} \end{figure}$	Figure A.6: Intervening system at z=1.9744 towards Q 0122-380. Smooth lines indicate the profiles for the favorite HM01 model.
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$\begin{figure}\par\resizebox{9cm}{!}{\includegraphics[bb=33 485 373 780,clip=]{0421fga7.ps}} \end{figure}$	Figure A.7: Intervening system at z=2.0422 towards PKS 0237-23. Smooth lines indicate the profiles for the favorite HM01 model.
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$\begin{figure}\par\resizebox{9cm}{!}{\includegraphics[bb=33 542 373 780,clip=]{0421fga8.ps}} \end{figure}$	Figure A.8: Intervening system at z=2.0626 towards Q 0122-380. Smooth lines indicate the profiles for the favorite HM01 model.
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$\begin{figure}\par\resizebox{9cm}{!}{\includegraphics[bb=33 485 373 780,clip=]{0421fga9.ps}} \end{figure}$	Figure A.9: Intervening system at z=2.0764 towards Q 0329-385. Smooth lines indicate the profiles for the favorite HM01 model.
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$\begin{figure}\par\resizebox{9cm}{!}{\includegraphics[bb=33 542 373 780,clip=]{0421fa10.ps}} \end{figure}$	Figure A.10: Intervening system at z=2.1098 towards PKS 1448-232. Smooth lines indicate the profiles for the favorite HM01 model.
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$\begin{figure}\par\resizebox{9cm}{!}{\includegraphics[bb=33 542 373 780,clip=]{0421fa11.ps}} \end{figure}$	Figure A.11: Intervening system at z=2.1162 towards HE 1347-2457. Smooth lines indicate the profiles for the favorite HM01 model.
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$\begin{figure}\par\resizebox{9cm}{!}{\includegraphics[bb=33 435 373 780,clip=]{0421fa12.ps}} \end{figure}$	Figure A.12: Intervening system at z=2.2212 towards HE 0940-1050. Smooth lines indicate the profiles for the favorite HM01 model.
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$\begin{figure}\par\resizebox{9cm}{!}{\includegraphics[bb=33 380 373 780,clip=]{0421fa13.ps}} \end{figure}$	Figure A.13: Intervening system at z=2.2354 towards HE 1158-1843. Smooth lines indicate the profiles for the favorite HM01 model.
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$\begin{figure}\par\resizebox{9cm}{!}{\includegraphics[bb=33 485 373 780,clip=]{0421fa14.ps}} \end{figure}$	Figure A.14: Intervening system at z=2.2464 towards Q 0420-388. Smooth lines indicate the profiles for the favorite HM01 model.
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$\begin{figure}\par\resizebox{9cm}{!}{\includegraphics[bb=33 328 373 780,clip=]{0421fa15.ps}} \end{figure}$	Figure A.15: Intervening system at z=2.2510 towards Q 0329-385. Smooth lines indicate the profiles for the favorite HM01 model.
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$\begin{figure}\par\resizebox{9cm}{!}{\includegraphics[bb=33 542 373 780,clip=]{0421fa16.ps}} \end{figure}$	Figure A.16: Intervening system at z=2.2753 towards HE 2347-4342. Smooth lines indicate the profiles for the favorite HM01 model.
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$\begin{figure}\par\resizebox{9cm}{!}{\includegraphics[bb=33 542 373 780,clip=]{0421fa17.ps}} \end{figure}$	Figure A.17: Intervening system at z=2.4686 towards HE 0151-4326. Smooth lines indicate the profiles for the favorite HM01 model.
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$\begin{figure}\par\resizebox{9cm}{!}{\includegraphics[bb=33 381 373 780,clip=]{0421fa18.ps}} \end{figure}$	Figure A.18: Associated system at z=2.1462 towards HE 1341-1020. Smooth lines indicate the profiles for the favorite HM01 model.
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$\begin{figure}\par\resizebox{9cm}{!}{\includegraphics[bb=33 58 373 780,clip=]{0421fa19.ps}} \end{figure}$	Figure A.19: Associated system at z=2.1475 towards HE 1341-1020. Smooth lines indicate the profiles for the favorite model with a HM01 background and an additional power law spectrum $\propto$ $\nu^{~-1.0}$ strongly dominating the ionizing radiation.
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$\begin{figure}\par\resizebox{9cm}{!}{\includegraphics[bb=33 485 373 780,clip=]{0421fa20.ps}} \end{figure}$	Figure A.20: Associated system at z=2.3520 towards Q 0329-385. Smooth lines indicate the profiles for the favorite HM01 model plus an additional small contribution of a power law spectrum $\propto$ $\nu^{~-0.37}$ .
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$\begin{figure}\par\resizebox{9cm}{!}{\includegraphics[bb=33 542 373 780,clip=]{0421fa21.ps}} \end{figure}$	Figure A.21: Associated system at z=2.4278 towards HE 1158-1843. Smooth lines indicate the profiles for the favorite model with a HM01 background and an additional power law spectrum $\propto$ $\nu^{~-1.0}$ strongly dominating the ionizing radiation.
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$\begin{figure}\par\resizebox{9cm}{!}{\includegraphics[bb=33 542 373 780,clip=]{0421fa22.ps}} \end{figure}$	Figure A.22: Associated system at z=2.4427 towards HE 1158-1843. Smooth lines indicate the profiles for the favorite model with a HM01 background and an additional power law spectrum $\propto$ $\nu^{~-1.0}$ strongly dominating the ionizing radiation.
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$\begin{figure}\par\resizebox{9cm}{!}{\includegraphics[bb=33 381 373 780,clip=]{0421fa23.ps}} \end{figure}$	Figure A.23: Associated system at z=2.6362 towards Q 0453-423. Smooth lines indicate the profiles for the favorite HM01 model plus an additional small contribution of a power law spectrum $\propto$ $\nu^{~-0.89}$ .
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$\begin{figure}\par\resizebox{9cm}{!}{\includegraphics[bb=33 485 373 780,clip=]{0421fa24.ps}} \end{figure}$	Figure A.24: Associated system at z=2.7091 towards PKS 0329-255. Smooth lines indicate the profiles for the favorite HM01 model.
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$\begin{figure}\par\resizebox{9cm}{!}{\includegraphics[bb=33 485 373 780,clip=]{0421fa25.ps}} \end{figure}$	Figure A.25: Associated system at z=2.8916 towards HE 2347-4342. Smooth lines indicate the profiles for the favorite HM01 model. Due to the marginal detection of C III is the blue components, which may lead to uncertain density estimates, we slightly overestimate the blue wing of the H I features in order to keep the metallicity constant in all 3 components.
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$\begin{figure}\par\resizebox{9cm}{!}{\includegraphics[bb=33 435 373 780,clip=]{0421fa26.ps}} \end{figure}$	Figure A.26: Associated system at z=2.8972 towards HE 2347-4342. Smooth lines indicate the profiles for the favorite HM01 model.
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$\begin{figure}\par\resizebox{9cm}{!}{\includegraphics[bb=33 435 373 780,clip=]{0421fa27.ps}} \end{figure}$	Figure A.27: Associated system at z=2.9027 towards HE 2347-4342. Smooth lines indicate the profiles for the favorite HM01 model plus an additional small contribution of a power law spectrum $\propto$ $\nu^{~+0.56}$ .
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$\begin{figure}\par\resizebox{9cm}{!}{\includegraphics[bb=33 650 373 780,clip=]{0421fa28.ps}} \end{figure}$	Figure A.28: Intervening system at z=1.5814 towards HE 0001-2340. Due to few detected species no photoionization model can be constructed. Smooth lines indicate Doppler profile fits.
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$\begin{figure}\par\resizebox{9cm}{!}{\includegraphics[bb=33 650 373 780,clip=]{0421fa29.ps}} \end{figure}$	Figure A.29: Intervening system at z=1.6109 towards PKS 0237-23. Due to few detected species no photoionization model can be constructed. Smooth lines indicate Doppler profile fits.
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$\begin{figure}\par\resizebox{9cm}{!}{\includegraphics[bb=33 650 373 780,clip=]{0421fa30.ps}} \end{figure}$	Figure A.30: Intervening system at z=1.8748 towards Q 0109-3518. Due to few detected species no photoionization model can be constructed. Smooth lines indicate Doppler profile fits.
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$\begin{figure}\par\resizebox{9cm}{!}{\includegraphics[bb=33 595 373 780,clip=]{0421fa31.ps}} \end{figure}$	Figure A.31: Intervening system at z=1.9144 towards HE 1158-1843. Due to few detected species no photoionization model can be constructed. Smooth lines indicate Doppler profile fits.
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$\begin{figure}\par\resizebox{9cm}{!}{\includegraphics[bb=33 595 373 780,clip=]{0421fa32.ps}} \end{figure}$	Figure A.32: Associated system at z=2.8780 towards HE 2347-4342. Due to few detected species no photoionization model can be constructed. Smooth lines indicate Doppler profile fits.
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Appendix B: Fitted line parameters

Table B.1: Line parameters of intervening N V absorption systems. The ionization parameter has been estimated adopting a Haardt & Madau (2001) UV background at the appropriate redshift normalized to $\log J(1~\textrm{Ryd}) = -21.15$ .

Table B.2: Line parameters of associated N V absorption systems. The ionization parameter has been estimated with an superposition of a Haardt & Madau (2001) UV background and a QSO power law spectrum with a slope $\alpha$ where the relative intensity of the QSO radiation is varied between $0.1 \le J_{{\rm QSO}}/J_{{\rm HM01}} \le 100$ . The quoted uncertainties of $\log U$ represent the resulting parameter range. If no $\alpha$ is given, a pure Haardt & Madau (2001) background has been adopted.

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