EDP Sciences
Free Access
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.

Open with DEXTER

 \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.

Open with DEXTER

 \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.

Open with DEXTER

 \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.

Open with DEXTER

 \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.

Open with DEXTER

 \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.

Open with DEXTER

 \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.

Open with DEXTER

 \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.

Open with DEXTER

 \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.

Open with DEXTER

 \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.

Open with DEXTER

 \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.

Open with DEXTER

 \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.

Open with DEXTER

 \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.

Open with DEXTER

 \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.

Open with DEXTER

 \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.

Open with DEXTER

 \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.

Open with DEXTER

 \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.

Open with DEXTER

 \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.

Open with DEXTER

 \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.

Open with DEXTER

 \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 $ $\nu^{~-0.37}$.

Open with DEXTER

 \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.

Open with DEXTER

 \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.

Open with DEXTER

 \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 $ $\nu^{~-0.89}$.

Open with DEXTER

 \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.

Open with DEXTER

 \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.

Open with DEXTER

 \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.

Open with DEXTER

 \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}$.

Open with DEXTER

 \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.

Open with DEXTER

 \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.

Open with DEXTER

 \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.

Open with DEXTER

 \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.

Open with DEXTER

 \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.

Open with DEXTER

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.


Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.