Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{4214fig1.eps}\end{figure}$ Figure 1: Number density distribution of RR Lyrae stars in the LMC. The unit for the number density, d is stars/sq. degree. The colour code is explained in the figure, where magenta denotes locations of highest density and blue denotes locations of lowest density.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{4214fig2.eps}\end{figure}$ Figure 2: The normalised number density distribution of RRLS along (filled circles) the PA = 120 $^\circ$ (along the bar, filled circle), 30 $^\circ$ (across the bar, open square), 75 $^\circ$ (asterix) and 165 $^\circ$ (open circle). The errors include statistical error and a 20% more due to any improper incompleteness correction.
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In the text

$\begin{figure} \par\includegraphics[width=8.05cm,clip]{4214fig3.eps}\end{figure}$ Figure 3: The locations used to estimate the number density distribution of RRLS as shown in Fig. 2, where PA = 120 $^\circ$ (along the bar, filled circle), 75 $^\circ$ (asterix), 165 $^\circ$ (open circle) and 210 $^\circ$ (across the bar, open square). The small dots indicate spatial coverage of the OGLE II survey.
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In the text

$\begin{figure} \par\includegraphics[width=8.15cm,clip]{4214fig4.eps}\end{figure}$ Figure 4: The normalised maximum number density of RRLS (filled circle), giant stars (crosses) and RC stars (open circle). The peak value of the distribution are 4300 (RRLS), 1.5 $\times$ 10⁸ (RC stars) and 2.5 $\times$ 10⁴ (red giants) stars/sq.degree.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4214fig5.eps}\end{figure}$ Figure 5: The variation in the extinction corrected magnitude as a function of RA. Note that the distribution is symmetric with respect to a concentration near I₀ = 18.45 mag, which can be considered as the disk of the LMC.
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In the text

$\begin{figure} \par\includegraphics[width=8.25cm,clip]{4214fig6.eps}\end{figure}$ Figure 6: 2D plot of the estimated value of dispersion ( $\sigma _{({\rm dep})}$ ) in the mean magnitude of the ab type RRLS. The colour code is indicated in the figure. The open circles indicate locations which have average mean magnitude less than 18.3 and crosses denote location which have values greater than 18.5 (see Fig. 7).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4214fig7.eps}\end{figure}$ Figure 7: The variation of $\sigma _{({\rm dep})}$ ( upper panel) and scale-height ( lower panel) as a function of RA. Locations with number of stars more than 10 are shown as dots and those with more than 30 stars are shown with circles around them.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4214fig8.eps}\end{figure}$ Figure 8: The distribution of the scale-height. The solid line is for locations with more than 10 stars and dotted line is for locations with more than 30 stars. Single Gaussian fit is indicated by dashed curve and double Gaussian fit is indicated by solid curve.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4214fig1.eps}\end{figure}$	Figure 1: Number density distribution of RR Lyrae stars in the LMC. The unit for the number density, d is stars/sq. degree. The colour code is explained in the figure, where magenta denotes locations of highest density and blue denotes locations of lowest density.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{4214fig2.eps}\end{figure}$	Figure 2: The normalised number density distribution of RRLS along (filled circles) the PA = 120 $^\circ$ (along the bar, filled circle), 30 $^\circ$ (across the bar, open square), 75 $^\circ$ (asterix) and 165 $^\circ$ (open circle). The errors include statistical error and a 20% more due to any improper incompleteness correction.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.05cm,clip]{4214fig3.eps}\end{figure}$	Figure 3: The locations used to estimate the number density distribution of RRLS as shown in Fig. 2, where PA = 120 $^\circ$ (along the bar, filled circle), 75 $^\circ$ (asterix), 165 $^\circ$ (open circle) and 210 $^\circ$ (across the bar, open square). The small dots indicate spatial coverage of the OGLE II survey.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.15cm,clip]{4214fig4.eps}\end{figure}$	Figure 4: The normalised maximum number density of RRLS (filled circle), giant stars (crosses) and RC stars (open circle). The peak value of the distribution are 4300 (RRLS), 1.5 $\times$ 10⁸ (RC stars) and 2.5 $\times$ 10⁴ (red giants) stars/sq.degree.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm,clip]{4214fig5.eps}\end{figure}$	Figure 5: The variation in the extinction corrected magnitude as a function of RA. Note that the distribution is symmetric with respect to a concentration near I₀ = 18.45 mag, which can be considered as the disk of the LMC.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.25cm,clip]{4214fig6.eps}\end{figure}$	Figure 6: 2D plot of the estimated value of dispersion ( $\sigma _{({\rm dep})}$ ) in the mean magnitude of the ab type RRLS. The colour code is indicated in the figure. The open circles indicate locations which have average mean magnitude less than 18.3 and crosses denote location which have values greater than 18.5 (see Fig. 7).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4214fig7.eps}\end{figure}$	Figure 7: The variation of $\sigma _{({\rm dep})}$ ( upper panel) and scale-height ( lower panel) as a function of RA. Locations with number of stars more than 10 are shown as dots and those with more than 30 stars are shown with circles around them.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm,clip]{4214fig8.eps}\end{figure}$	Figure 8: The distribution of the scale-height. The solid line is for locations with more than 10 stars and dotted line is for locations with more than 30 stars. Single Gaussian fit is indicated by dashed curve and double Gaussian fit is indicated by solid curve.
Open with DEXTER