Buckling bars in nearly face-on galaxies observed with MaNGA

TL;DR

This study identifies and analyzes buckling bars in nearly face-on galaxies using stellar kinematics from MaNGA data, confirming a specific velocity pattern and estimating the frequency of buckling events.

Contribution

It introduces a novel kinematic signature for detecting buckling bars and reports five new candidates, doubling previous known instances.

Findings

Detected a quadrupolar velocity pattern associated with buckling.

Identified five buckling bar candidates in MaNGA data.

Observed buckling frequency consistent with simulation predictions.

Abstract

Over half of disk galaxies are barred, yet the mechanisms for bar formation and the life-time of bar buckling remain poorly understood. In simulations, a thin bar undergoes a rapid (<1 Gyr) event called "buckling," during which the inner part of the bar is asymmetrically bent out of the galaxy plane and eventually thickens, developing a peanut/X-shaped profile when viewed side-on. Through analyzing stellar kinematics of N-body model snapshots of a galaxy before, during, and after the buckling phase, we confirm a distinct quadrupolar pattern of out-of-plane stellar velocities in nearly face-on galaxies. This kinematic signature of buckling allows us to identify five candidates of currently buckling bars among 434 barred galaxies in the Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) Survey, an integral field unit (IFU) spectroscopic survey that measures the composition and kinematic structure of nearby galaxies. The frequency of buckling events detected is consistent with the 0.5-1 Gyr timescale predicted by simulations. The five candidates we present more than double the total number of candidate buckling bars, and are the only ones found using the kinematic signature.