Table 2: For each nova, the year, magnitude, and amplitude of the outburst, the slope $F = \lambda ^{\alpha }$ of the continuum, and the FWHM, equivalent widths, and line fluxes of the main emission lines in the observed spectra are given. No de-reddening has been applied. Note that the uncertainty of the line flux describes the uncertainty of the relative flux in the line and does not include the photometric error. Outburst magnitudes and amplitudes are taken/calculated from the references as given in the text.

Nova		 Date $m_{\rm max}$ $\Delta m$ $\alpha $ Transition FWHM [nm] -W [nm] F [10-18 W m-2]

V630 Sgr		 1936 ${\rm vis}=4.0^{\rm m}$ 13.9$^{\rm m}$ $-1.21 \pm 0.02^{1}$ H$\alpha $ $2.36\pm 0.04$ $2.70 \pm 0.06$ $4.09\pm 0.09$
        $-2.55 \pm 0.02^{1}$ H$\beta $ $1.90\pm 0.04$ $1.35 \pm 0.07$ $3.32\pm 0.15$
          H$\gamma$ $1.59\pm 0.04$ $0.73 \pm 0.04$ $2.15\pm 0.07$
          He II $\lambda$541 $2.00\pm 0.09$ $0.51\pm 0.03$ $1.15\pm 0.06$
          He II $\lambda$469 $1.93\pm 0.06$ $2.8\pm 0.2$ $7.0\pm 0.2$

XX Tau		 1927 $p=5.9^{\rm m}$ $>13.1^{\rm m}$ $-2.66\pm 0.03$ H$\alpha $ $3.36 \pm 0.03$ $5.2\pm 0.1$ $1.56\pm 0.05$
          H$\beta $ $2.30 \pm 0.04$ $1.92\pm 0.06$ $1.29\pm 0.05$
          H$\gamma$ $2.21 \pm 0.05$ $1.36\pm 0.03$ $1.17\pm 0.01$
          H$\delta$ $2.56 \pm 0.04$ $1.38\pm 0.1$ $1.3\pm 0.1$
          H$\epsilon$ $2.29 \pm 0.04$ $1.11\pm 0.05$ $1.12\pm 0.04$
          H8 $2.05 \pm 0.07$ $0.85\pm 0.05$ $0.88\pm 0.04$
          H9 $1.91 \pm 0.12$ $0.53\pm 0.05$ $0.58\pm 0.04$
          He I $\lambda$668 $1.9 \pm 1.5$ $0.39\pm 0.1$ $0.11\pm 0.04$
          He I $\lambda$588 $2.8\pm 0.2$ $0.50\pm 0.1$ $0.22\pm 0.04$
          He I $\lambda$447 $2.3 \pm 0.2$ $0.35\pm 0.1$ $0.31\pm 0.06$

V529 Ori		 1678 ${\rm vis}=7^{\rm m}$   $+4.87\pm 0.07^{2}$ H$\alpha $ $1.43\pm 0.05$ $2.95\pm 0.06$ $3.75\pm 0.07$

CQ Vel		 1940 $p=9.0^{\rm m}$ $>12.1^{\rm m}$ $-1.15 \pm 0.03$ H$\alpha $ $2.88 \pm 0.04$ $1.80\pm0.05$ $0.52\pm 0.01$
          H$\beta $ $2.1\pm 0.1$ $0.45\pm0.05$ $0.18\pm 0.01$

V842 Cen		 1986 ${\rm vis}=4.6^{\rm m}$ $>13.4^{\rm m}$ $-4.32\pm 0.05 ^{3}$ H$\alpha $ $5.08\pm 0.03$ $7.31\pm 0.04$ $0.0719\pm 0.0004$
        $-1.59\pm 0.02 ^{3}$ H$\beta $ $1.79\pm 0.02$ $1.56\pm 0.03$ $0.0248\pm 0.0003$
          H$\gamma$ $1.5 \pm 0.05$ $0.86\pm 0.02$ $0.0208\pm 0.0003$
          H$\delta$ $1.9 \pm 0.1$ $0.8\pm 0.2$ $0.027\pm 0.03$
          H$\epsilon$ $1.42\pm 0.02$ $0.67\pm 0.03$ $0.0264\pm 0.0003$
          H8 $1.41\pm 0.03$ $0.38\pm 0.05$ $0.016\pm 0.001$
          He I $\lambda$706? $1.95\pm 0.05$ $0.12\pm 0.02$ $0.00105\pm 0.0003$
          He I $\lambda$668 $1.86\pm 0.02$ $0.33\pm 0.02$ 0.00314
          He I $\lambda$588 $1.72\pm 0.02$ >0.38 >0.0044
          He I $\lambda$447 $1.35\pm 0.2$ $0.22\pm 0.02$ $0.0045 \pm 0.0004$
          C IV $\lambda$580 $2.3 \pm 0.2$ $0.30\pm 0.02$ $0.0035 \pm 0.0004$
1 The continuum of V630 Sgr shows two slopes; the first for $\lambda < 582$ nm, the second for $\lambda \ge 582$ nm.
2 V529 Ori shows no straight line in the double-logarithmic plot; thus only a formal value for a linear fit to the data is given.
3 The continuum of V842 Cen shows two slopes; the first for $\lambda < 500$ nm, the second for $\lambda \ge 500$ nm.

Source LaTeX | All tables | In the text

Article Contents
1 Introduction
2 Observation and data reduction
3 V630 Sagittarii
4 XX Tauri
5 V529 Orionis
6 CQ Velorum
7 V842 Centauri
8 Discussion and conclusion
References
List of tables
List of figures