Early-type galaxy density profiles from IllustrisTNG: I. Galaxy correlations and the impact of baryons

Abstract

We explore the isothermal total density profiles of early-type galaxies (ETGs) in the IllustrisTNG simulation. For the selected 559 ETGs at $z=0$ with stellar mass $10^{10.7}{\mathrm{M}}_{\odot }⩽M_{\ast }⩽10^{11.9}{\mathrm{M}}_{\odot }$, the total power-law slope has a mean of $⟨{\gamma }^{\prime }⟩=2.011\pm 0.007$ and a scatter of ${\sigma }_{{\gamma }^{\prime }}=0.171$ over the radial range 0.4 to 4 times the stellar half mass radius. Several correlations between ${\gamma }^{\prime }$ and galactic properties including stellar mass, effective radius, stellar surface density, central velocity dispersion, central dark matter fraction and in-situ-formed stellar mass ratio are compared to observations and other simulations, revealing that IllustrisTNG reproduces many correlation trends, and in particular, ${\gamma }^{\prime }$ is almost constant with redshift below $z=2$. Through analyzing IllustrisTNG model variations we show that black hole kinetic winds are crucial to lowering ${\gamma }^{\prime }$ and matching observed galaxy correlations. The effects of stellar winds on ${\gamma }^{\prime }$ are subdominant compared to AGN feedback, and differ due to the presence of AGN feedback from previous works. The density profiles of the ETG dark matter halos are well-described by steeper-than-NFW profiles, and they are steeper in the full physics (FP) run than their counterparts in the dark matter only (DMO) run. Their inner density slopes anti-correlates (remain constant) with the halo mass in the FP (DMO) run, and anti-correlates with the halo concentration parameter $c_{200}$ in both types of runs. The dark matter halos of low-mass ETGs are contracted whereas high-mass ETGs are expanded, suggesting that variations in the total density profile occur through the different halo responses to baryons.

31 pages, 20 figures, 9 tables. Accepted for publication in MNRAS. Major revision, added the effects of feedback on the total density profile in Section 4. Pay attention to changes in Figures 7, 10, 12, and 16

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