TY - JOUR
T1 - The multi-wavelength Tully-Fisher relation in the TNG50 cosmological simulation
AU - Baes, M
AU - Gebek, A
AU - Kunene, S
AU - Leeuw, L
AU - Nelson, D
AU - Ponomareva, Anastasia A.
AU - Andreadis, N
AU - Bianchetti, A.
AU - de Blok, W.J.G.
AU - Rajohnson, S.H.A.
AU - Sorgho, A
N1 - © The Authors 2025. This is an Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0).
PY - 2025/4/2
Y1 - 2025/4/2
N2 - Context. The Tully-Fisher relation (TFR) is one of the most important and widely used empirical correlations in extragalactic astronomy. Apart from its importance as a secondary distance indicator, the TFR relation serves as a test for galaxy evolution models, because it connects the baryonic and dark matter components of galaxies. Aims. We aimed at simulating the multi-wavelength TFR relation from UV to mid-infrared (MIR) wavelengths for the TNG50 cosmological simulation at z = 0, and at comparing the results with observational TFR studies. Our goal was to compare the wavelength dependence of the slope and scatter with the observed values, and to search for secondary parameters that reduce the scatter in the TFR. Methods. We selected a large sample of simulated late-type, disc-dominated galaxies from the TNG50 simulation. For each galaxy, we used the SKIRT radiative transfer code to generate realistic synthetic global fluxes in 12 UV to MIR broadbands and synthetic integrated H I line profiles. We used bivariate linear regression to determine the TFR in each band, and we searched for a second TFR parameter by correlating the residuals with different physical parameters. Results. Our TNG50 TFR reproduces the characteristic behaviour of the observed TFR in many studies: the TFR becomes steeper and tighter as we move from UV/optical to infrared wavelengths. The slope changes from ‑7.46 ± 0.14 mag dex‑1 in the NUV band to ‑9.66 ± 0.09 mag dex‑1 in the IRAC [4.5] band. Quantitatively, our slopes are well within the spread of different observational results. The u ‑ r colour or the sSFR can significantly reduce the scatter in the UV and optical bands. Using u ‑ r colour as second parameter, the modified TFR has a roughly constant intrinsic tightness of over the entire UV to MIR range. Conclusions. The combination of the TNG50 cosmological simulation and the SKIRT radiative transfer postprocessing is capable of broadly reproducing the multi-wavelength TFR. A better matched sample selection, the use of different characteristic velocity scales, and more advanced internal dust attenuation correction are steps towards a more stringent comparison of the simulated and observed multi-wavelength TFR.
AB - Context. The Tully-Fisher relation (TFR) is one of the most important and widely used empirical correlations in extragalactic astronomy. Apart from its importance as a secondary distance indicator, the TFR relation serves as a test for galaxy evolution models, because it connects the baryonic and dark matter components of galaxies. Aims. We aimed at simulating the multi-wavelength TFR relation from UV to mid-infrared (MIR) wavelengths for the TNG50 cosmological simulation at z = 0, and at comparing the results with observational TFR studies. Our goal was to compare the wavelength dependence of the slope and scatter with the observed values, and to search for secondary parameters that reduce the scatter in the TFR. Methods. We selected a large sample of simulated late-type, disc-dominated galaxies from the TNG50 simulation. For each galaxy, we used the SKIRT radiative transfer code to generate realistic synthetic global fluxes in 12 UV to MIR broadbands and synthetic integrated H I line profiles. We used bivariate linear regression to determine the TFR in each band, and we searched for a second TFR parameter by correlating the residuals with different physical parameters. Results. Our TNG50 TFR reproduces the characteristic behaviour of the observed TFR in many studies: the TFR becomes steeper and tighter as we move from UV/optical to infrared wavelengths. The slope changes from ‑7.46 ± 0.14 mag dex‑1 in the NUV band to ‑9.66 ± 0.09 mag dex‑1 in the IRAC [4.5] band. Quantitatively, our slopes are well within the spread of different observational results. The u ‑ r colour or the sSFR can significantly reduce the scatter in the UV and optical bands. Using u ‑ r colour as second parameter, the modified TFR has a roughly constant intrinsic tightness of over the entire UV to MIR range. Conclusions. The combination of the TNG50 cosmological simulation and the SKIRT radiative transfer postprocessing is capable of broadly reproducing the multi-wavelength TFR. A better matched sample selection, the use of different characteristic velocity scales, and more advanced internal dust attenuation correction are steps towards a more stringent comparison of the simulated and observed multi-wavelength TFR.
KW - radiative transfer / galaxies: formation / galaxies: fundamental parameters / galaxies: kinematics and dynamics / galaxies: photometry
U2 - 10.1051/0004-6361/202453417
DO - 10.1051/0004-6361/202453417
M3 - Article
SN - 0004-6361
VL - 696
JO - Astronomy & Astrophysics
JF - Astronomy & Astrophysics
M1 - A52
ER -