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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{H4210F01.eps}\end{figure}$ Figure 1: The difference of the mean $E(B-V)_{\rm mean}$ values from nine external sources minus $E(B-V)_{\rm Fernie}$ , plotted against $E(B-V)_{\rm mean}$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{H4210F02.eps}\end{figure}$ Figure 2: The color residuals $\Delta (B-V)$ from the first-step P-C relation in function of the color excess $E(B-V)_{\rm Fernie}$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{H4210F03.eps}\end{figure}$ Figure 3: The adopted Galactic P-C relation in (B-V)⁰ as obtained from the corrected color excesses ${E(B-V)_{{\rm corr}}}$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{H4210F04.eps}\end{figure}$ Figure 4: The color residuals $\Delta (V-I)$ from a preliminary P-C relation plotted against the color excess $E(V-I) = 1.38 E(B-V)_{\rm corr}$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{H4210F05.eps}\end{figure}$ Figure 5: The final Galactic P-C relation in (V-I)⁰ as obtained from the corrected color excesses ${E(V-I)_{\rm corr}}$ .
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In the text

$\begin{figure} \par\includegraphics[width=14.2cm,clip]{H4210F06.eps}\end{figure}$ Figure 6a: The Period-Color relation in (B-V)⁰ for Cepheids in the Galaxy, LMC, and SMC. The Galaxy data are copied from Fig. 3. The solid line in each panel is the mean relation for the Galaxy from Eq. (3). Three theoretical models by Sandage et al. (1999; SBT), Baraffe & Alibert (2001; BA), and Caputo et al. (2000) are compared with the mean Galaxy line in panel (d). - The paucity of red LMC Cepheids is purely observational due to the few available B magnitudes and saturation effects for $\log P > 1.5$ .

In the text

$\begin{figure} \par\includegraphics[width=14.2cm,clip]{H4210F07.eps}\end{figure}$ Figure 6b: Same as Fig. 6a but for (V-I)⁰ colors. The Galaxy data are copied from Fig. 5. The Galaxy line in each panel is Eq. (5) of the text.

In the text

$\begin{figure} \par\includegraphics[width=13.8cm,clip]{H4210F08.eps}\end{figure}$ Figure 7a: Two color-diagrams in (B-V)⁰ vs. (V-I)⁰ for Cepheids in the Galaxy, LMC, and SMC in panels a), b), and c). The full line drawn in each panel is the linear least-squares line put through the Galaxy data in panel a). Panel d) shows calculated relations for four values of [Fe/H] from Table 6 of SBT for $\log g = 1.5$ and an atmospheric turbulent velocity of $1.7\nobreak\mbox{$\;$ km~s$^{-1}$ }$ . The model lines with the appropriate metallicities are repeated in panels a)- c) as dashed lines.

In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{H4210F09.eps}\end{figure}$ Figure 7b: A comparison of the mean position in the two-color diagram of Cepheids in the Galacty, LMC, and SMC. The loci of differentvalues of $\log P$ are indicated.

In the text

$\begin{figure} \par\includegraphics[width=15.3cm,clip]{H4210F10.eps}\end{figure}$ Figure 8: The provisional P-L relations in B, V, and I for Galactic Cepheids in open clusters ( left panels) and with BBW distances ( right panels). The Cepheids shown as triangles are not used for the solution; at short periods they are probable overtone pulsators (shown here with their inferred fundamental period), the three long period Cepheids with BBW distances have variable periods.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{H4210F11.eps}\end{figure}$ Figure 9: The magnitude residuals $\Delta M_{B,V,I}$ off the mean provisional P-L relations in function of the color excess ${E(B-V)_{{\rm corr}}}$ . Closed circles are data from Table 3 (left panel of Fig. 8), open circles are data from Table 4 (right panel of Fig. 8).
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{H4210F12.eps}\end{figure}$ Figure 10: The lack of correlation with Galactic longitude for the ratio of absolute magnitude residuals from the adopted P-L relations in Eqs. (15-17) to the corrected ${E(B-V)_{{\rm corr}}}$ color excess values for individual Cepheids in Tables 3 and 4. Closed circles are for Cepheids in Table 3. Open circles are Cepheids from Table 4.
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In the text

$\begin{figure} \par\includegraphics[width=11.7cm,clip]{H4210F13.eps}\end{figure}$ Figure 11: The combined P-L relations in B, V, and I from 25 Cepheids in open clusters (filled symbols) and 28 Cepheids with BBW distances (open symbols). Triangles are not used for the solution (cf. caption to Fig. 8). - The square in the M⁰_V and M⁰_I panels are from the HIPPARCOS calibration (Groenewegen & Oudmaijer 2000). - Upper and lower boundaries of the P-L relations are shown on the assumption that the constant-period lines have slopes of 3.52, 2.52, and 1.94 in B, V, and I, respectively, and that the instability strip has a width of $\pm0\hbox{$.\!\!^{\rm m}$ }13$ in (B-V)⁰ and $\pm0\hbox{$.\!\!^{\rm m}$ }10$ in (V-I)⁰ (cf. Fig. 15). The calculations use ${E(B-V)_{{\rm corr}}}$ values, $\alpha =0.44$ , and the ${{\cal R}_{B,V,I}}$ values, corrected for intrinsic color, as listed in Col. 11 of Tables 3 and 4.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{H4210F14.eps}\end{figure}$ Figure 12: Color residuals $\Delta (B-V)$ of the calibrating Galactic Cepheids with known metallicities in function of [Fe/H]. The red color of the metal-poor Cepheids must be due to systematic errors of the adopted color excesses ${E(B-V)_{{\rm corr}}}$ . Triangles stand for Cepheids with variable periods; they are not used for the solution.
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In the text

$\begin{figure} \par\includegraphics[width=14.7cm,clip]{H4210F15.eps}\end{figure}$ Figure 13: Comparison of the present Galactic P-L relations in B, V, and I with model calculations (see text). BA is Baraffe & Alibert (2001).
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In the text

$\begin{figure} \par\includegraphics[width=11cm,clip]{H4210F16.eps}\end{figure}$ Figure 14a: The position of 650 absorption-corrected fundamental-mode LMC Cepheids from Udalski et al. (1999b) in the P-L plane. The adopted LMC modulus is (m-M)⁰=18.54. Open symbols are Cepheids excluded by Udalski et al. (1999a). Overplotted are the mean Galactic P-L relations from Eqs. (15-17).

In the text

$\begin{figure} \par\includegraphics[width=11cm,clip]{H4210F17.eps}\end{figure}$ Figure 14b: The position of 489 absorption-corrected fundamental-mode SMC Cepheids from Udalski et al. (1999c) in the P-L plane. The adopted SMC modulus is (m-M)⁰=19.00. Symbols as in Fig. 14a.

In the text

$\begin{figure} \par\includegraphics[width=11.8cm,clip]{H4210F18.eps}\end{figure}$ Figure 15: The Galactic instability strip. Symbols are as in Fig. 11. The full lines correspond to Eqs. (21) and (22), respectively. Dashed lines indicate the adopted blue and red edges of the strip. Three outlying Cepheids are identified.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{H4210F19.eps}\end{figure}$ Figure 16: Comparison of the instability strip position in the Galaxy, LMC, and SMC. The dashed line is the ridge line of the instability strip of LMC and SMC from Eqs. (29-32) using the Cepheids adopted by Udalski et al. (1999a). The dotted lines are from all their fundamental-mode Cepheids. The full drawn lines are the Galactic ridge lines from Fig. 15.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{H4210F01.eps}\end{figure}$	Figure 1: The difference of the mean $E(B-V)_{\rm mean}$ values from nine external sources minus $E(B-V)_{\rm Fernie}$ , plotted against $E(B-V)_{\rm mean}$ .
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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{H4210F02.eps}\end{figure}$	Figure 2: The color residuals $\Delta (B-V)$ from the first-step P-C relation in function of the color excess $E(B-V)_{\rm Fernie}$ .
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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{H4210F03.eps}\end{figure}$	Figure 3: The adopted Galactic P-C relation in (B-V)⁰ as obtained from the corrected color excesses ${E(B-V)_{{\rm corr}}}$ .
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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{H4210F04.eps}\end{figure}$	Figure 4: The color residuals $\Delta (V-I)$ from a preliminary P-C relation plotted against the color excess $E(V-I) = 1.38 E(B-V)_{\rm corr}$ .
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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{H4210F05.eps}\end{figure}$	Figure 5: The final Galactic P-C relation in (V-I)⁰ as obtained from the corrected color excesses ${E(V-I)_{\rm corr}}$ .
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$\begin{figure} \par\includegraphics[width=15.3cm,clip]{H4210F10.eps}\end{figure}$	Figure 8: The provisional P-L relations in B, V, and I for Galactic Cepheids in open clusters ( left panels) and with BBW distances ( right panels). The Cepheids shown as triangles are not used for the solution; at short periods they are probable overtone pulsators (shown here with their inferred fundamental period), the three long period Cepheids with BBW distances have variable periods.
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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{H4210F11.eps}\end{figure}$	Figure 9: The magnitude residuals $\Delta M_{B,V,I}$ off the mean provisional P-L relations in function of the color excess ${E(B-V)_{{\rm corr}}}$ . Closed circles are data from Table 3 (left panel of Fig. 8), open circles are data from Table 4 (right panel of Fig. 8).
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{H4210F12.eps}\end{figure}$	Figure 10: The lack of correlation with Galactic longitude for the ratio of absolute magnitude residuals from the adopted P-L relations in Eqs. (15-17) to the corrected ${E(B-V)_{{\rm corr}}}$ color excess values for individual Cepheids in Tables 3 and 4. Closed circles are for Cepheids in Table 3. Open circles are Cepheids from Table 4.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{H4210F14.eps}\end{figure}$	Figure 12: Color residuals $\Delta (B-V)$ of the calibrating Galactic Cepheids with known metallicities in function of [Fe/H]. The red color of the metal-poor Cepheids must be due to systematic errors of the adopted color excesses ${E(B-V)_{{\rm corr}}}$ . Triangles stand for Cepheids with variable periods; they are not used for the solution.
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$\begin{figure} \par\includegraphics[width=14.7cm,clip]{H4210F15.eps}\end{figure}$	Figure 13: Comparison of the present Galactic P-L relations in B, V, and I with model calculations (see text). BA is Baraffe & Alibert (2001).
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$\begin{figure} \par\includegraphics[width=11.8cm,clip]{H4210F18.eps}\end{figure}$	Figure 15: The Galactic instability strip. Symbols are as in Fig. 11. The full lines correspond to Eqs. (21) and (22), respectively. Dashed lines indicate the adopted blue and red edges of the strip. Three outlying Cepheids are identified.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{H4210F19.eps}\end{figure}$	Figure 16: Comparison of the instability strip position in the Galaxy, LMC, and SMC. The dashed line is the ridge line of the instability strip of LMC and SMC from Eqs. (29-32) using the Cepheids adopted by Udalski et al. (1999a). The dotted lines are from all their fundamental-mode Cepheids. The full drawn lines are the Galactic ridge lines from Fig. 15.
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