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Appendix A: Visual spectra of HR 1847A and HR 1847B

$\begin{figure} \par\includegraphics[width=17.6cm,clip]{13726fA1a.eps}\par\includ... ...3726fA1c.eps}\par\includegraphics[width=17.6cm,clip]{13726fA1d.eps} \end{figure}$

Figure A.1:

Line identification of the spectrum of HR 1847A obtained with the blue channel of the HEROS spectrograph (dots) and comparison with the synthetic spectrum calculated from the Kurucz (1993) LTE model atmosphere $\ensuremath{T_{\rm eff}} =12~500~\ensuremath{{\rm K}}$ , $\log g=3.5$ , rotationally broadened with $\ensuremath{(\varv \sin i)_{\rm A}} =40~\mbox{${\rm km}~{\rm s}^{-1}$ }$ (full line).

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$\begin{figure} \par\includegraphics[width=17.6cm,clip]{13726fA1e.eps}\par\includ... ...3726fA1g.eps}\par\includegraphics[width=17.6cm,clip]{13726fA1h.eps} \end{figure}$	Figure A.1: continued.
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$\begin{figure} \par\includegraphics[width=18cm,clip]{13726fA2a.eps}\par\includeg... ...{13726fA2c.eps}\par\includegraphics[width=18cm,clip]{13726fA2d.eps} \end{figure}$

Figure A.2:

Line identification of the spectrum of HR 1847A obtained with the red channel of the HEROS spectrograph (dots) and comparison with the synthetic spectrum calculated from the Kurucz (1993) LTE model atmosphere $\ensuremath{T_{\rm eff}} =12~500~\ensuremath{{\rm K}}$ , $\log g=3.5$ , rotationally broadened with $\ensuremath{(\varv \sin i)_{\rm A}} =40~\mbox{${\rm km}~{\rm s}^{-1}$ }$ (full line). Note the presence of telluric lines and bands near 6280 Å, $\ensuremath {{\rm H}\alpha }$ , 6870 Å, 7250 Å, and 7590 Å.

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$\begin{figure} \par\includegraphics[width=18cm,clip]{13726fA3a.eps}\par\includeg... ...{13726fA3c.eps}\par\includegraphics[width=18cm,clip]{13726fA3d.eps} \end{figure}$

Figure A.3:

Line identification of the spectrum of HR 1847B obtained with the blue channel of the HEROS spectrograph (dots) and comparison with a synthetic spectrum calculated from the Kurucz (1993) LTE model atmosphere $\ensuremath{T_{\rm eff}} =12~500~\ensuremath{{\rm K}}$ , $\log g=3.5$ , rotationally broadened with $\ensuremath{(\varv \sin i)_{\rm B}} =230~\mbox{${\rm km}~{\rm s}^{-1}$ }$ (full line).

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$\begin{figure} \par\includegraphics[width=18cm,clip]{13726fA3e.eps}\par\includeg... ...{13726fA3g.eps}\par\includegraphics[width=18cm,clip]{13726fA3h.eps} \end{figure}$	Figure A.3: continued.
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$\begin{figure} \par\includegraphics[width=18cm,clip]{13726fA4a.eps}\par\includeg... ...{13726fA4c.eps}\par\includegraphics[width=18cm,clip]{13726fA4d.eps} \end{figure}$

Figure A.4:

Line identification of the spectrum of HR 1847B obtained with the red channel of the HEROS spectrograph (dots), and comparison with a synthetic spectrum calculated from the Kurucz (1993) LTE model atmosphere $\ensuremath{T_{\rm eff}} =12~500~\ensuremath{{\rm K}}$ , $\log g=3.5$ , rotationally broadened with $\ensuremath{(\varv \sin i)_{\rm B}} =230~\mbox{${\rm km}~{\rm s}^{-1}$ }$ (full line). Note the presence of telluric lines and bands near 6280 Å, $\ensuremath {{\rm H}\alpha }$ , 6870 Å, 7250 Å, and 7590 Å.

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Table A.1: Heliocentric radial velocities (RV) of HR 1847A - spectra from Ondrejov Observatory, where $V_{\rm hel}$ is the heliocentric velocity.

Table A.2: Heliocentric radial velocities (RV) of HR 1847A - spectra from Rozhen Observatory.

Table A.3: Heliocentric radial velocities (RV) of HR 1847B - spectra from Ondrejov Observatory.

Table A.4: Heliocentric radial velocities (RV) of HR 1847B - spectra from Rozhen Observatory.