The baryonic Tully-Fisher relation in the Simba simulation

M. Glowacki*, E. Elson, R. Davé

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review

Abstract / Description of output

We investigate the Baryonic Tully–Fisher relation (BTFR) in the (100h−1Mpc)3simba hydrodynamical galaxy formation simulation together with a higher resolution (25h−1Mpc)3simba run, for over 10 000 disc-dominated, H i-rich galaxies. We generate simulated galaxy rotation curves from the mass distribution, which we show yields similar results to using the gas rotational velocities. From this, we measure the galaxy rotation velocity Vcirc using four metrics: Vmax,Vflat,V2Re, and Vpolyex. We compare the predicted BTFR to the SPARC observational sample and find broad agreement. In detail, however, simba is biased towards higher Vcirc by up to 0.1 dex. We find evidence for the flattening of the BTFR in Vcirc > 300  km s−1 galaxies, in agreement with recent observational findings. simba’s rotation curves are more peaked for lower mass galaxies, in contrast with observations, suggesting overly bulge-dominated dwarf galaxies in our sample. We investigate for residuals around the BTFR versus H i mass, stellar mass, gas fraction, and specific star formation rate, which provide testable predictions for upcoming BTFR surveys. simba’s BTFR shows sub-optimal resolution mass convergence, with the higher resolution run lowering V in better agreement with data.
Original languageEnglish
Pages (from-to)3687-3702
Number of pages16
JournalMonthly Notices of the Royal Astronomical Society
Issue number3
Early online date27 Aug 2020
Publication statusPublished - 1 Nov 2020

Keywords / Materials (for Non-textual outputs)

  • astro-ph.GA


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