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Simulations have shown that bars are subject to a vertical bucklinginstability that transforms thin bars into boxy or peanut-shaped structures,but the physical conditions necessary for buckling to occur are not fullyunderstood. We use the large sample of local disk galaxies in theCarnegie-Irvine Galaxy Survey to examine the incidence of bars and buckled barsacross the Hubble sequence. Depending on the disk inclination angle ($i$), abuckled bar reveals itself as either a boxy/peanut-shaped bulge (at high $i$)or as a barlens structure (at low $i$). We visually identify bars,boxy/peanut-shaped bulges, and barlenses, and examine the dependence of bar andbuckled bar fractions on host galaxy properties, including Hubble type, stellarmass, color, and gas mass fraction. We find that the barred and unbarred disksshow similar distributions in these physical parameters. The bar fraction ishigher (70\%--80\%) in late-type disks with low stellar mass ($M_{*} <10^{10.5}\, M_{\odot}$) and high gas mass ratio. In contrast, the buckled barfraction increases to 80\% toward massive and early-type disks ($M_{*} >10^{10.5}\, M_{\odot}$), and decreases with higher gas mass ratio. Theseresults suggest that bars are more difficult to grow in massive disks that aredynamically hotter than low-mass disks. However, once a bar forms, it caneasily buckle in the massive disks, where a deeper potential can sustain thevertical resonant orbits. We also find a probable buckling bar candidate (ESO506$-$G004) that could provide further clues to understand the timescale of thebuckling process.

The Carnegie-Irvine Galaxy Survey. V. Statistical study of bars and buckled bars