The interplay between accretion, galaxy downsizing and the formation of box/peanut bulges in TNG50

• Published in: arXiv.org
• Main Authors: Anderson, Stuart Robert, Gough-Kelly, Steven, Debattista, Victor P, Du, Min, Erwin, Peter, Cuomo, Virginia, Caruana, Joseph, Hernquist, Lars, Vogelsberger, Mark
• Format: Paper
• Language: English
• Published: Ithaca Cornell University Library, arXiv.org 25.11.2023
• Subjects: Barred galaxies; Deposition; Downsizing; Galactic bulge; Heating; Peanuts; Stars & galaxies; Stellar mass

From the TNG50 cosmological simulation we build a sample of 191 well-resolved barred galaxies with a stellar mass \(\log M_\star > 10\) at \(z=0\). We search for box/peanut bulges (BPs) in this sample, finding them in 55 per cent of cases. We compute \(f_\mathrm{BP}\), the BP probability for barred galaxies as a function of \(M_\star\), and find that this rises to a plateau, as found in observations of nearby galaxies. The transition mass where \(f_\mathrm{BP}\) reaches half the plateau value is \(\log M_\star = 10.14\), consistent with the observational value within measurement errors. We show that this transition in \(f_\mathrm{BP}\) can be attributed to the youth of the bars at low \(M_\star\), which is a consequence of downsizing of galaxies. Young bars, being generally shorter and weaker, have not yet had time to form BPs. At high mass, while we find a plateau, the value is at \(\sim 60\) per cent, whereas observations saturate at 100 per cent. We attribute this difference to excessive heating in TNG50, due to merger activity and to numerical resolution effects. BPs in TNG50 tend to occur in galaxies with more quiescent merger histories. As a result, the main driver of whether a bar hosts a BP in TNG50 is not the galaxy mass, but how long and strong the bar is. Separating the BP sample into those that have visibly buckled and those that have not, we find that fully half of BP galaxies show clear signs of buckling, despite the excessive heating and limited vertical resolution of TNG50.