All Figures

	Figure 1: Spectra for the stars that have significant Li detections.
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In the text

Figure 2: The observed stars shown on the CO integrated intensity map (Dame et al. 2001) in Galactic coordinates. The equatorial gird is also drawn with dashed lines. Contours are from 3 K km s-1 with intervals of 6 K km s-1. The filled, gray and open circles denote observed X-ray point sources whose spectra are strong, weak, and without Li detection, respectively (see Sect. 3.3). The crosses are those with H lines in emission. The dotted ellipses show the nearby dark clouds of (A) LDN 1228, (B) LDN 1241, (C) LDN 1242, (D) LDN 1243, (E) LDN 1247, (F) LDN 1251, (G) LDN 1259-1262, (H) MBM 163-165, (I) LDN 1333, (J) LDN 1274, (K) Khavtassi 15, and (L) LDN 1221 around the CO void (see text).

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In the text

Figure 3: Li equivalent width versus effective temperature. The Li-rich stars detected in the Cep-Cas region are shown by the crosses, and those with H emission lines are by black dots. The small open circles and the large circles are Pleiades and IC 2602 stars, respectively, whose upper envelopes are drawn with the solid and the dashed lines (Neuhäuser 1997; Neuhäuser et al. 1997, and the references therein). The T Tauri stars in Taurus whose were measured by low-resolution and high-resolution spectrograph are also shown by open and filled diamonds, respectively.

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In the text

Figure 4: HR diagram for the PMS candidates. Tracks are for 0.1, 0.2, 0.4, 0.6, 0.8, 1, 1.2, 1.5 and 2 , and isochrones are for 0.1, 0.3, 1, 3, 10, 30 and 100 Myr, both taken from D'Antona & Mazzitelli (1994). Stars are assumed to be located in the Cep-Cas SFR at 200 pc. The error bars are drawn according to the spectral classification uncertainty of 1 subclass. The stars with the H emission lines are marked with black dots.

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In the text