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We use the Spitzer Survey of Stellar Structure in Galaxies (S$^{4}$G) 3.6$\mu$m imaging to study the properties (length and strength) and fraction ofbars at $z=0$. We use the maximum of tangential-to-radial force ratio in thebar region ($Q_{\rm b}$) as a measure of the bar induced perturbation strengthfor a sample of $\sim 600$ barred galaxies. Bars are also characterized fromthe maximum of the normalized m=2 Fourier density amplitude ($A_{2}^{\rm max}$)and the bar maximum isophotal ellipticity ($\varepsilon$). Combining our forcecalculations with the HI kinematics from the literature we get an estimate ofthe halo-to-stellar mass ratios ($M_{\rm h}/M_{\ast}$) within the optical disk,which are in good agreement with studies based on weak lensing analysis,abundance matching and halo occupation distribution methods. By further usingthe Universal Rotation Curve models we obtain a first-order model of therotation curve decomposition of $1128$ disk galaxies. We find that the dilutionof $Q_{\rm b}$ by the halo becomes important for later types, implying $\sim20-25\%$ reduction for $T = 7-10$. Whether the halo correction is included ornot, the mean $Q_{\rm b}$ shows an increasing trend with $T$. Late-type barsare longer than previously found in the literature. We find possible evidencefor the growth of bars within a Hubble time, as (1) bars in early-type galaxiesshow larger density amplitudes and disk-relative sizes than theirintermediate-type counterparts, and (2) long bars are typically strong. We alsoobserve two clearly distinct types of bars, between early and intermediate-typegalaxies ($T<5$) on one side, and the late-type systems on the other, based onthe differences in the bar properties. Most likely this distinction isconnected to the larger halo-to-stellar ratio that we observe in later types,affecting the disk stability properties (Abridged).

Characterization of galactic bars from 3.6 $\mu$m S$^{4}$G imaging