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 language | English |
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Pages (from-to) | 3687-3702 |
Number of pages | 16 |
Journal | Monthly Notices of the Royal Astronomical Society |
Volume | 498 |
Issue number | 3 |
Early online date | 27 Aug 2020 |
DOIs | |
Publication status | Published - 1 Nov 2020 |
Keywords / Materials (for Non-textual outputs)
- astro-ph.GA