All Figures

$\begin{figure} {\includegraphics[width=13cm,clip]{5049f06.ps} }\end{figure}$ Figure 2: Main panel: flux-calibrated CAFOS spectra of HS 0417, HS 1016, HS 1340, HS 1857, and HS 2214. Fluxes are labelled alternatingly on the left and right side. HS 1340 was observed in quiescence and outburst, respectively. Right panel: close-up plots of the ${\rm H\alpha }$ and ${\rm H\beta }$ profiles.
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In the text

$\begin{figure} {\includegraphics[angle=-90,width=8cm,clip]{5049f07.ps} }\end{figure}$ Figure 3: Sample light curves of HS 0417 obtained at the Wendelstein observatory. Top panel: B-band data obtained during superoutburst on January 14, 2001. Bottom panel: filterless data obtained during quiescence.
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In the text

$\begin{figure} {\includegraphics[angle=-90,width=8cm,clip]{5049f08.ps} }\end{figure}$ Figure 4: Sample filterless light curves of HS 1016 obtained at the Kryoneri observatory.
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In the text

$\begin{figure} {\includegraphics[angle=-90,width=8cm,clip]{5049f09.ps} }\end{figure}$ Figure 5: Sample light curves of HS 1340. Top panel: R-band data obtained at the Kryoneri observatory. Bottom panel: filterless data obtained at the IAC80 telescope.
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In the text

$\begin{figure} {\includegraphics[angle=-90,width=8cm,clip]{5049f10.ps} }\end{figure}$ Figure 6: Sample R-band light curves of HS 2214 obtained at the Braeside observatory.
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In the text

$\begin{figure} {\includegraphics[width=8.2cm,clip]{5049f11.ps} }\end{figure}$ Figure 7: Sample R-band and filterless light curves of HS 1857 folded over the ephemeris in Eq. (1). See Sect. 6.2 for details.
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In the text

$\begin{figure} {\includegraphics[angle=-90,width=8cm,clip] {5049f12.ps} }\end{figure}$ Figure 8: Main panel: the Scargle periodogram of HS 0417 during quiescence computed from all photometric data except February 27, 2003. Top panel: the window function shifted to 13.7 ${\rm d^{-1}}$ .
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In the text

$\begin{figure} {\includegraphics[width=8.2cm,clip]{5049f13.ps} }\end{figure}$ Figure 9: The Scargle periodogram of the radial velocities of HS 1016, HS 1340, HS 1857, and HS 2214. The periodograms constructed from faked sets of data at the corresponding orbital frequency are shown in small windows.
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In the text

$\begin{figure} {\includegraphics[width=8.2cm,clip]{5049f14.ps} }\end{figure}$ Figure 10: ${\rm H\alpha }$ radial velocities of HS 1016, HS 1340, and HS 1857 and ${\rm H\alpha }$ plus ${\rm H\beta }$ radial velocities of HS 2214. The radial velocities of HS 1016 and HS 1340 are folded on their spectroscopic periods of 114.3 min and 92.66 min, respectively and those of HS 1857 and HS 2214 are folded on their photometric periods of 272.317 min and 258.02 min, respectively. The data on HS 1857 were folded using the eclipse ephemeris given in Eq. (1) while the other three systems were folded defining phase zero as the time of red-to-blue crossing of the radial velocities.
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In the text

$\begin{figure} {\includegraphics[angle=-90,width=8.2cm,clip]{5049f15.ps} }\end{figure}$ Figure 11: Main window: the mean magnitudes of HS1340 obtained from May 2001 to May 2005 in R-band (filled triangles), V-band (filled circles), and white light (open circles). The photometric error on the individual points is <0.05 mag. An additional systematic uncertainty arises from the combination of different band passes. Considering the apparent magnitudes of HS 1340 listed in the Sloan Digital Sky Survey which are g=17.3, r=17.1, and i=17.1, the errors due to colour terms are likely to be within $\pm 0.1$ mag. Small window: close up of the April 2003 CAFOS run. The first three points show the deep faint state with a mean magnitude of $V\simeq 18.5$ before the outburst on April 10, 2003.
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In the text

$\begin{figure} {\includegraphics[angle=-90,width=8.2cm,clip]{5049f16.ps} }\end{figure}$ Figure 12: The HST/STIS spectrum of HS 1857 taken on August 17, 2003 during an outburst.
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In the text

$\begin{figure} {\includegraphics[angle=-90,width=8.2cm,clip]{5049f17.ps} }\end{figure}$ Figure 13: The periodogram of HS 1857 computed from nine eclipses obtained during the 2002 to 2004 runs.
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In the text

$\begin{figure} {\includegraphics[angle=-90,width=8.5cm,clip]{5049f18.ps} }\end{figure}$ Figure 14: The average CAFOS spectrum of HS 2214 (black line) along with the best-matching M-dwarf template of spectral type M 2.5, scaled to fit the strength of the molecular bands in HS 2214. The 2MASS $JHK_{\rm s}$ infrared fluxes of HS 2214 are represented by filled triangles; the JHK spectrum of the M-dwarf template is shown as gray dots.
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In the text

$\begin{figure} {\includegraphics[angle=-90,width=8.3cm,clip]{5049f19.ps} }\end{figure}$ Figure 15: Main panel: the analysis-of-variance (AOV) periodogram of HS 2214 calculated from the two longest light curves obtained at the Braeside Observatory, which show a double-humped pattern. Top panel: the AOV periodogram created from a sine wave with the orbital period of 258.02 min.
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In the text

$\begin{figure} {\includegraphics[width=8.5cm,clip]{5049f20.ps} }\end{figure}$ Figure 16: The spectroscopic and photometric data of HS 2214 are folded on the photometric period of 258.02 min using the spectroscopic zero-point $T_{0}={\rm HJD}~2~451~812.3309$ defined by the red-to-blue crossing of the ${\rm H\alpha }$ and ${\rm H\beta }$ radial velocities. In that phase convention, the inferior conjunction of the secondary star is expected at orbital phase zero. Top panel: the radial velocity variation of the ${\rm H\alpha }$ and ${\rm H\beta }$ emission lines, as already shown in Fig. 10. A whole cycle has been repeated for clarity. Middle panel: the photometric data obtained from the Braeside Observatory. Bottom panel: the photometric data binned into 25 phase slots, along with a two-frequency sine fit (dashed line).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{5049f21.ps} \end{figure}$ Figure 17: Top panel: the orbital period distribution of known CVs and dwarf novae from Ritter & Kolb (2003, 7th edition, rev. 7.5, July 2005) are shown in gray and shade, respectively. Bottom panel: the period distribution of known dwarf novae according to their subtype, U Gem (UG), Z Cam (ZC), SU UMa (SU), WZ Sge (WZ), ER UMa (ER), and unclassified subtype (XX). The dashed lines are the conventional 2-3 h period gap.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{5049f22.ps} \end{figure}$ Figure 18: Top panel: the orbital period distribution of 41 new CVs and 14 dwarf novae identified in HQS are shown in gray and shade, respectively. Bottom panel: the period distribution of HQS dwarf novae according to their subtype, U Gem (UG), Z Cam (ZC), SU UMa (SU), WZ Sge (WZ), and unclassified subtype (XX). The dashed lines are the conventional 2-3 h period gap.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=5.8cm]{5049f01.eps}\hfill \inclu... ...04.eps}\hspace{5.8cm} \includegraphics[width=5.8cm]{5049f05.eps} }\end{figure}$ Figure 1: $10\hbox {$^\prime $ }\times 10\hbox {$^\prime $ }$ finding charts for HS 0417, HS 1016, HS 1340, HS 1857, and HS 2214 obtained from the Digitized Sky Survey. HS 2214 is the northern component of a close visual binary. See Table 3 for details on the comparison stars C1-C11.
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In the text

$\begin{figure} {\includegraphics[width=13cm,clip]{5049f06.ps} }\end{figure}$	Figure 2: Main panel: flux-calibrated CAFOS spectra of HS 0417, HS 1016, HS 1340, HS 1857, and HS 2214. Fluxes are labelled alternatingly on the left and right side. HS 1340 was observed in quiescence and outburst, respectively. Right panel: close-up plots of the ${\rm H\alpha }$ and ${\rm H\beta }$ profiles.
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$\begin{figure} {\includegraphics[angle=-90,width=8cm,clip]{5049f07.ps} }\end{figure}$	Figure 3: Sample light curves of HS 0417 obtained at the Wendelstein observatory. Top panel: B-band data obtained during superoutburst on January 14, 2001. Bottom panel: filterless data obtained during quiescence.
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$\begin{figure} {\includegraphics[angle=-90,width=8cm,clip]{5049f08.ps} }\end{figure}$	Figure 4: Sample filterless light curves of HS 1016 obtained at the Kryoneri observatory.
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$\begin{figure} {\includegraphics[angle=-90,width=8cm,clip]{5049f09.ps} }\end{figure}$	Figure 5: Sample light curves of HS 1340. Top panel: R-band data obtained at the Kryoneri observatory. Bottom panel: filterless data obtained at the IAC80 telescope.
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$\begin{figure} {\includegraphics[angle=-90,width=8cm,clip]{5049f10.ps} }\end{figure}$	Figure 6: Sample R-band light curves of HS 2214 obtained at the Braeside observatory.
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$\begin{figure} {\includegraphics[width=8.2cm,clip]{5049f11.ps} }\end{figure}$	Figure 7: Sample R-band and filterless light curves of HS 1857 folded over the ephemeris in Eq. (1). See Sect. 6.2 for details.
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$\begin{figure} {\includegraphics[angle=-90,width=8cm,clip] {5049f12.ps} }\end{figure}$	Figure 8: Main panel: the Scargle periodogram of HS 0417 during quiescence computed from all photometric data except February 27, 2003. Top panel: the window function shifted to 13.7 ${\rm d^{-1}}$ .
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$\begin{figure} {\includegraphics[width=8.2cm,clip]{5049f13.ps} }\end{figure}$	Figure 9: The Scargle periodogram of the radial velocities of HS 1016, HS 1340, HS 1857, and HS 2214. The periodograms constructed from faked sets of data at the corresponding orbital frequency are shown in small windows.
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$\begin{figure} {\includegraphics[angle=-90,width=8.2cm,clip]{5049f16.ps} }\end{figure}$	Figure 12: The HST/STIS spectrum of HS 1857 taken on August 17, 2003 during an outburst.
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$\begin{figure} {\includegraphics[angle=-90,width=8.2cm,clip]{5049f17.ps} }\end{figure}$	Figure 13: The periodogram of HS 1857 computed from nine eclipses obtained during the 2002 to 2004 runs.
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$\begin{figure} {\includegraphics[angle=-90,width=8.5cm,clip]{5049f18.ps} }\end{figure}$	Figure 14: The average CAFOS spectrum of HS 2214 (black line) along with the best-matching M-dwarf template of spectral type M 2.5, scaled to fit the strength of the molecular bands in HS 2214. The 2MASS $JHK_{\rm s}$ infrared fluxes of HS 2214 are represented by filled triangles; the JHK spectrum of the M-dwarf template is shown as gray dots.
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$\begin{figure} {\includegraphics[angle=-90,width=8.3cm,clip]{5049f19.ps} }\end{figure}$	Figure 15: Main panel: the analysis-of-variance (AOV) periodogram of HS 2214 calculated from the two longest light curves obtained at the Braeside Observatory, which show a double-humped pattern. Top panel: the AOV periodogram created from a sine wave with the orbital period of 258.02 min.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{5049f22.ps} \end{figure}$	Figure 18: Top panel: the orbital period distribution of 41 new CVs and 14 dwarf novae identified in HQS are shown in gray and shade, respectively. Bottom panel: the period distribution of HQS dwarf novae according to their subtype, U Gem (UG), Z Cam (ZC), SU UMa (SU), WZ Sge (WZ), and unclassified subtype (XX). The dashed lines are the conventional 2-3 h period gap.
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$\begin{figure} \par\mbox{\includegraphics[width=5.8cm]{5049f01.eps}\hfill \inclu... ...04.eps}\hspace{5.8cm} \includegraphics[width=5.8cm]{5049f05.eps} }\end{figure}$	Figure 1: $10\hbox {$^\prime $ }\times 10\hbox {$^\prime $ }$ finding charts for HS 0417, HS 1016, HS 1340, HS 1857, and HS 2214 obtained from the Digitized Sky Survey. HS 2214 is the northern component of a close visual binary. See Table 3 for details on the comparison stars C1-C11.
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