Astronomy & Astrophysics

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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3741.f1.eps}\end{figure}$ Figure 1: Number distributions of morphological types, B-band corrected absolute magnitudes and SBs, and corrected (B-K) colors for the recompiled sample of 78 normal HSB and LSB disk galaxies. The contribution of the HSB galaxies is shaded.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3741.f2.eps}\end{figure}$ Figure 2: a). Correlation between $(V_{\rm d,m}/V_{\rm t,m})$ and $\Sigma _{\rm d,0}$ for disks in centrifugal equilibrium inside a pseudo-isothermal (upper curves) and a NFW (lower curves) halo of $\mbox{$M_{\rm v}$ }= 3.5\times 10^{11}~\mbox{$M_\odot$ }$ . See details about the model parameters in the text. Solid lines are for $f_{\rm d} = 0.05$ , while upper and lower dashed lines around the solid curves are for $f_{\rm d} =0.08$ and 0.03, respectively. The approximate region of maximum disk (see text) is bounded by the dot-dashed lines. b) Same as in panel a), but for the NFW model, taking into account the disk gravitational dragging over the halo. The shaded region encompasses the $\pm 1\sigma$ scatter in concentrations around the central model. The solid upper and lower curves are for $\mbox{$M_{\rm v}$ }= 3.5\times 10^{12}~\mbox{$M_\odot$ }$ and $3.5\times 10^{10}~\mbox{$M_\odot$ }$ with the corresponding average concentration parameters and $f_{\rm d} = 0.05$ . c) and d). Relation between $(V_{\rm d,m}/V_{\rm t,m})$ and the disk(baryon)-to-dynamical mass ratios inside 2.2 $h_{\rm d}$ and 5 $h_{\rm d}$ for the same models shown in the left panels. In panel c) thick and thin lines are for the NFW and pseudo-isothermal halos, respectively. In panel d) the linear fittings (in Log-Log) are given.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3741.f3.eps}\end{figure}$ Figure 3: a) Same as in Fig. 2 but for observations (empty circles) and evolutionary model results (solid triangles, squares, and circles corresponding to $\mbox{$M_{\rm v}$ }= 3.5\times 10^{10}~\mbox{$M_\odot$ }, 3.5\times 10^{11}~\mbox{$M_\odot$ }$ , and $3.5\times 10^{12}~\mbox{$M_\odot$ }$ , respectively). The models are for $f_{\rm d} = 0.05$ . Four galaxies, which are outliers in this plot, as well as the Milky Way and Andromeda galaxies are indicated by their names. For indication, the composite mass models presented in Fig. 2 for the pseudo-isothermal halo (upper curves) and the NFW halo with gravitational drag (lower curves) are also shown. The solid lines are for $\mbox{$M_{\rm v}$ }= 3.5\times 10^{11}~\mbox{$M_\odot$ }$ while the dashed ones are for $3.5\times 10^{10}~\mbox{$M_\odot$ }$ (upper curves) and $3.5\times 10^{12}~\mbox{$M_\odot$ }$ (lower curves). b) Means per $\Sigma _{\rm d,0}$ bins and their corresponding standard deviations for the observational data (thick dashed line and shaded area) and the model results (thick solid line and empty frame) showed in panel a). The arrows from the thick curve are an estimate of how much the models would decrease if $f_{\rm d}$ is decreased to 0.03.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3741.f4.eps}\end{figure}$ Figure 4: a) Dynamical-to-baryonic mass ratio vs. the baryonic surface density for observations (empty circles) and models (same symbols as in Fig. 3). The left axis is the quantity inferred directly from the observational data, while the right axis is this quantity multiplied by 5; in the assumption that the rotation curve remains constant up to 5 $h_{\rm d}$ , this corresponds to $M_{\rm dyn}/M_{\rm bar}$ at 5 $h_{\rm d}$ . Solid and dotted lines are the linear regressions for models and observations, respectively. For observations, the fitting (at 5 $h_{\rm d}$ ) is showed in the upper right. b) Same as in panel a) but for the stellar mass and surface density. c) Same as in panel a) but for the K-band luminosity and SB. Only observations are showed in this panel.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3741.f5.eps} \end{figure}$ Figure 5: a) Same as Fig. 4, but for B-band luminosity and SB, and only for observational data. b) Same as panel a) but using the definitions of Graham (2002; see text) and including some LSB galaxies with large bulges also considered by Graham (circles with crosses). Notice how the scatter in the correlation seen in panel a) increases in panel b).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3741.f6.eps} \end{figure}$ Figure 6: a) Same as in Fig. 5a but for h_B instead of $\Sigma _{B,0}$ in thex-axis. The data are sorted into three groups according to their B-band magnitudes. The corresponding ranges are: $4.0\times 10^{8}{-}2.5\times 10^{9}L_{B_{\odot }}$ (open symbols), $2.5\times 10^{9}{-}1.6\times 10^{10}L_{B\odot }$ (targeted symbols), and $1.6\times 10^{10}-1.0\times 10^{11}L_{B_{\odot }}$ (solid symbols). Although for all the data is not significant, for the data sorted in luminosity ranges, a correlation between the mass-to-light ratio and h_B appears. b) Same as in Fig. 5b but for h_B instead of $\Sigma _{B,0}$ in the x-axis. A correlation appears for all the data in this panel (calculated according to Graham 2002).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3741.f7.eps}\par\includegraphics[width=8.5cm,clip]{3741a.f7.eps} \end{figure}$ Figure 7: a) Approximate dynamical-to-baryonic mass ratio at 5 $h_{\rm d}$ vs. integral (B-K) color for observational data. No correlation, if any, an anti-correlation, is seen. However, for limited ranges of surface density, a correlation appears as this density is lower. The data in the plot were sorted into three groups according to their disk central surface densities: open, targeted and solid symbols are for low, intermedium and high surface densities, respectively (we use surface densities instead of L_K luminosity in order to have the same ranges for the model data presented in panel b). The solid line is an eye-fit to the low surface density group. b) Same as in panel a) but for the model data and for (B-V)instead of (B-K). See text for explanations of this figure.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3741.f1.eps}\end{figure}$	Figure 1: Number distributions of morphological types, B-band corrected absolute magnitudes and SBs, and corrected (B-K) colors for the recompiled sample of 78 normal HSB and LSB disk galaxies. The contribution of the HSB galaxies is shaded.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3741.f5.eps} \end{figure}$	Figure 5: a) Same as Fig. 4, but for B-band luminosity and SB, and only for observational data. b) Same as panel a) but using the definitions of Graham (2002; see text) and including some LSB galaxies with large bulges also considered by Graham (circles with crosses). Notice how the scatter in the correlation seen in panel a) increases in panel b).
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