Free Access
 Issue A&A Volume 496, Number 1, March II 2009 31 - 44 Cosmology (including clusters of galaxies) https://doi.org/10.1051/0004-6361/200810421 30 January 2009

## Appendix A: N V systems

 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

 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

 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

 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

 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

 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

 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

 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

 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

 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

 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

 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

 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

 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

 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

 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

 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

 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

 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 strongly dominating the ionizing radiation. Open with DEXTER

 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 . Open with DEXTER

 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 strongly dominating the ionizing radiation. Open with DEXTER

 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 strongly dominating the ionizing radiation. Open with DEXTER

 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 . Open with DEXTER

 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

 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

 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

 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 . Open with DEXTER

 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

 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

 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

 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

 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 .

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 where the relative intensity of the QSO radiation is varied between . The quoted uncertainties of represent the resulting parameter range. If no  is given, a pure Haardt & Madau (2001) background has been adopted.

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