Appendix B: Figures

The following five figures show the spectra for the H&K emission-line stars in the wavelength region around Ca II H and K (Fig. B1). A subsample of the stars with strong Ca II emission is plotted in the H$\alpha$ region (Fig. B2) and in the lithium region at 6708 Å (Fig. B3). The Strömgren y photometry is shown in Figs. B4 and B5 (Fig. B4 is for the stars with a photometric period and Fig. B5 for those without a detectable period).

Figure B1: Ca II spectra of stars with H and K emission. Shown are the 316 stars with an intensity level in the K line of $I_{\rm K}\geq 1$. The HD number (or HIP number or Variable Star designation if no HD number exists) is identified on top of each plot. Each plot covers a range of 50 Å centered at 3950 Å

Figure B1: continued

Figure B1: continued

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Figure B1: continued

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Figure B1: continued

Figure B2: Selected Balmer H$\alpha$ spectra of stars with strong Ca II H and K emission. The HD number (or HIP number if no HD number exists) is identified on top of each plot. The wavelength range shown is 30 Å

Figure B2: continued

Figure B2: continued

Figure B3: Lithium 6707.8-Å spectra of stars with Ca II H and K emission and $W_{\rm Li}\geq 10$ mÅ. The HD number (or HIP number if no HD number exists) is identified on top of each plot. The wavelength range shown is 25 Å. The dotted spectrum is a spectrum of the Sun vertically shifted by 0.01 for comparison purposes (the solar lithium equivalent width is $\approx$2 mÅ). The vertical line is the average rest wavelength of Li I at 6707.8 Å

Figure B3: continued

Figure B3: continued

Figure B3: continued

Figure B3: continued

Figure B4: Differential Strömgren-y light curves of stars with Ca II H and K emission. The HD number (or HIP number, or Variable Star designation, if no HD number exists) is identified on top of each plot. The left panel in each plot is the observations versus heliocentric Julian date. The right panel is the light curve phased with the best-fit photometric period from Table A3. Error bars for the observations indicate the variances from three individual readings between the variable and the comparison star

Figure B4: continued

Figure B4: continued

Figure B4: continued

Figure B4: continued

Figure B5: Differential Strömgren-y light curves of stars without a period determination. Note that many of these stars are likely photometric variable but the time coverage was just too short to cover a full cycle. Otherwise as in Fig. B4

Figure B5: continued