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Appendix A: Notes on individual QSOs

We usually find an extra UV-flux drop in the spectra. However, the u-band photometry is consistent with the reddened QSO template. This drop might be caused by the inaccurate flux calibration at the blue end of the spectrum. The QSO SEDs and extinction curves are presented in Fig. A.1.

	Fig. A.1 Same as caption of Fig. 1.
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Appendix A.1: HAQ J0015+1129

This is a reddened QSO from the HAQ survey of Paper II at redshift z = 0.87. The spectrum was obtained with the NOT/ALFOSC. The redshift was based on the detection of the Mg ii emission line. The data are well fit with a steeper extinction curve with A_V = 0.58 ± 0.13 and R_V = 2.66 ± 0.31. Previously, Paper II reported A_V = 0.78.

Appendix A.2: HAQ J0129−0059

This is a reddened QSO from the HAQ survey of Paper I at redshift z = 0.71. The spectrum was obtained with the NTT/EFOSC2. The redshift was estimated from the Mg ii emission line. We modelled the QSO SED, and the data are well fit with A_V = 0.74 ± 0.17 and R_V = 2.41 ± 0.28. Previously, Paper I derived A_V = 1.5.

Appendix A.3: HAQ J0130+1439

This is a reddened QSO from the HAQ survey of Paper II at redshift z = 0.93. The spectrum was obtained with the NOT/ALFOSC, and the redshift was derived from the Mg ii emission line. We modelled the QSO SED, and the data are well fit with A_V = 0.46 ± 0.12 and R_V = 2.23 ± 0.35. Paper II reported A_V = 0.4 from their SED analysis.

Appendix A.4: HAQ J0151+0618

This is a reddened QSO from the HAQ survey of Paper II at redshift z = 0.95. The spectrum was obtained with the NOT/ALFOSC. The redshift was based on the detection of the Mg ii emission line. The SED is nicely reproduced with a steep extinction curve with A_V = 0.51 ± 0.14 and R_V = 2.29 ± 0.23. Previously, Paper II reported A_V = 0.72.

Appendix A.5: HAQ J0247−0052

This is a reddened QSO from the HAQ survey of Paper I at redshift z = 0.825. The spectrum was obtained with the NTT/EFOSC2. The redshift was estimated from the Mg ii and O ii emission lines. The SED can be modelled with R_V = 2.52 ± 0.19 and a very high extinction value of A_V = 1.00 ± 0.11. Previously, Paper I inferred A_V = 1.5 from their SED analysis.

Appendix A.6: HAQ J0312+0035

This is a reddened QSO from the HAQ survey of Paper I at redshift z = 1.28. The spectrum was obtained with the NTT/EFOSC2. The redshift was derived from the Mg ii and C iii emission lines. The SED can be modelled with a steep extinction curve with A_V = 0.50 ± 0.12 and R_V = 2.29 ± 0.23. Previously, Paper I derived A_V = 0.8.

Appendix A.7: HAQ J0319+0623

This is a reddened QSO from the HAQ survey of Paper II at redshift z = 2.10. The spectrum was obtained with the NOT/ALFOSC, and the redshift was derived from the Si iv + O iv, C iv, and C iii emission lines. The SED can be modelled with a steep extinction curve with A_V = 0.20 ± 0.06 and R_V = 2.38 ± 0.365. Paper II reported A_V = 0.13 from the SED analysis.

Appendix A.8: HAQ J0347+0115

This is a reddened QSO from the HAQ survey of Paper II at redshift z = 0.98. The spectrum was obtained with the NOT/ALFOSC. The redshift was estimated from the Mg ii emission line. The SED is modelled well with a steep extinction curve and A_V = 0.29 ± 0.12 together with R_V = 2.23 ± 0.39. Previously, Paper II inferred A_V = 0.4 from the SED analysis.

Appendix A.9: HAQ J1400+0219

This is a reddened QSO from the HAQ survey of Paper II at redshift z = 0.86. The spectrum was obtained with the NOT/ALFOSC. The redshift was based on the detection of Mg ii emission line. We found the observed data fit very well with a steep extinction curve and relatively high A_V with A_V = 0.56 ± 0.09 and R_V = 2.16 ± 0.36. Previously, Paper II reported A_V = 0.85.

Appendix A.10: HAQ J1409+0940

This is a reddened QSO from the HAQ survey of Paper II at redshift z = 0.92. The spectrum was obtained with the NOT/ALFOSC, and the redshift was derived from the relatively weak Mg ii emission line. The SED can be modelled with a steep extinction curve with A_V = 0.54 ± 0.10 and R_V = 2.27 ± 0.26. Paper II derived A_V = 0.93 from SED analysis.

Appendix A.11: HAQ J1527+0250

This is a reddened BAL QSO from the HAQ survey of Paper II at redshift z = 2.13. The spectrum was obtained with the NOT/ALFOSC. The redshift was estimated from the C iv and C iii emission lines. We found that the observed data fit very well with a steep extinction curve with A_V = 0.21 ± 0.07 and R_V = 2.33 ± 0.36. Previously, Paper II reported A_V = 0.2.

Appendix A.12: HAQ J1606+2902

This is a reddened BAL QSO from the HAQ survey of Paper II at redshift z = 1.82. The spectrum was obtained with the NOT/ALFOSC, and the redshift was based on the detection of C iv, Fe ii, and Mg ii emission lines. The data are nicely reproduced with a low extinction value of A_V = 0.26 ± 0.08 and R_V = 2.44 ± 0.24. Paper II inferred A_V = 0.25 from their SED analysis.

Appendix A.13: HAQ J1639+3157

This is a reddened QSO from the HAQ survey of Paper II at redshift z = 0.82. The spectrum was obtained with the NOT/ALFOSC, and the redshift was based on the detection of Mg ii emission line. The data are well described with a steep extinction curve and relatively high extinction value of A_V = 0.73 ± 0.11 and R_V = 2.48 ± 0.18. Previously, Paper II derived A_V = 0.79.

Appendix A.14: HAQ J1643+2944

This is a reddened QSO from the HAQ survey of Paper II at redshift z = 1.08. The spectrum was obtained with the NOT/ALFOSC. The redshift was derived from the relatively weak Mg ii emission line. The SED of the QSO fits well with A_V = 0.39 ± 0.13 and R_V = 2.56 ± 0.27. Paper II previously reported A_V = 0.44 from the SED analysis.

Appendix A.15: HAQ J2310+1117

This is a reddened QSO from the HAQ survey of Paper II at redshift z = 0.82. The spectrum was obtained with the NOT/ALFOSC, and the redshift was estimated from the weak Mg ii emission line. We found that the observed data fit very well with a steep extinction curve with A_V = 0.57 ± 0.13 and R_V = 2.44 ± 0.28. Previously, Paper II reported A_V = 0.92 from the SED analysis.

Appendix A.16: HAQ J2355−0041

This is a reddened QSO from the HAQ survey of Paper I at redshift z = 1.01. The spectrum was obtained with the NOT/ALFOSC. The redshift was inferred from the Mg ii emission line. The SED is fit very well with a steep extinction curve with A_V = 0.65 ± 0.13 and R_V = 2.54 ± 0.24. Paper I derived A_V = 1.0−1.6 from the SED analysis.

© ESO, 2015