Small Scatter and Nearly Isothermal Mass Profiles to Four Half-Light Radii From Two-Dimensional Stellar Dynamics of Early-Type Galaxies

Cappellari, Michele; Romanowsky, Aaron J.; Brodie, Jean P.; Forbes, Duncan A.; Strader, Jay; Foster, Caroline; Kartha, Sreeja S.; Pastorello, Nicola; Pota, Vincenzo; Spitler, Lee R.; Usher, Christopher; Arnold, Jacob A.

doi:10.1088/2041-8205/804/1/l21

Cited by 116 publications

(214 citation statements)

References 47 publications

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“…First, in galaxies dominated by baryons there is no systematic evidence for large cores or lowered DM density profiles (e.g., Cappellari et al 2015). Second, in galaxy clusters the stars dominate the total mass budget within their half-light radii, yet the DM tends to be under-dense compared to predictions.…”

Section: Motivation: Contraction Of Sidm Halosmentioning

confidence: 98%

A Testable Conspiracy: Simulating Baryonic Effects on Self-interacting Dark Matter Halos

Elbert

Bullock

Kaplinghat

et al. 2018

ApJ

111

116

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We investigate the response of self-interacting dark matter (SIDM) halos to the growth of galaxy potentials using idealized simulations, with each run in tandem with collisionless cold dark matter (CDM). We find that if the stellar potential strongly dominates in the central parts of a galaxy, then SIDM halos can be as dense as CDM halos on observable scales. For extreme cases, core collapse can occur, leading to SIDM halos that are denser and cuspier than their CDM counterparts. If the stellar potential is not dominant, then SIDM halos retain isothermal cores with densities far below CDM predictions. When a disk is present, the inner SIDM halo becomes more flattened in the disk plane than the CDM halo.  s -is disfavored for DM collision velocities above about 1500 km s −1 . More generally, the interaction between baryonic potentials and SIDM densities offers new directions for constraining SIDM cross-sections in galaxies where baryons are dynamically important.

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Section: Motivation: Contraction Of Sidm Halosmentioning

confidence: 98%

A Testable Conspiracy: Simulating Baryonic Effects on Self-interacting Dark Matter Halos

Elbert

Bullock

Kaplinghat

et al. 2018

ApJ

111

116

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“…Therefore, the circular velocity of a typical ETG decreases between 0 and 10 percent when going from 0.5−1 R eff , where it is traced by CO, to the outer regions, where it is traced by H i. Cappellari et al (2015) recently found that the mass profiles of a sample of 14 ETGs can be well described by a nearly isothermal power law ρ tot ∝ r −γ with an average logarithmic slope γ = 2.19 with remarkable small scatter in γ. The small decrease in circular velocity we observe is consistent with such mass profiles.…”

Section: Comparison To the Co K-band Tfrmentioning

confidence: 95%

The H I Tully-Fisher relation of early-type galaxies

Heijer

Oosterloo

Serra

et al. 2015

A&A

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We study the H i K-band Tully-Fisher relation and the baryonic Tully-Fisher relation for a sample of 16 early-type galaxies, taken from the ATLAS 3D sample, which all have very regular H i disks extending well beyond the optical body ( > ∼ 5 R eff ). We use the kinematics of these disks to estimate the circular velocity at large radii for these galaxies. We find that the Tully-Fisher relation for our early-type galaxies is offset by about 0.5−0.7 mag from the relation for spiral galaxies, in the sense that early-type galaxies are dimmer for a given circular velocity. The residuals with respect to the spiral Tully-Fisher relation correlate with estimates of the stellar mass-tolight ratio, suggesting that the offset between the relations is mainly driven by differences in stellar populations. We also observe a small offset between our Tully-Fisher relation with the relation derived for the ATLAS 3D sample based on CO data representing the galaxies' inner regions ( < ∼ 1 R eff ). This indicates that the circular velocities at large radii are systematically 10% lower than those near 0.5−1 R eff , in line with recent determinations of the shape of the mass profile of early-type galaxies. The baryonic Tully-Fisher relation of our sample is distinctly tighter than the standard one, in particular when using mass-to-light ratios based on dynamical models of the stellar kinematics. We find that the early-type galaxies fall on the spiral baryonic Tully-Fisher relation if one assumes M/L K = 0.54 M /L for the stellar populations of the spirals, a value similar to that found by recent studies of the dynamics of spiral galaxies. Such a mass-to-light ratio for spiral galaxies would imply that their disks are 60−70% of maximal. Our analysis increases the range of galaxy morphologies for which the baryonic Tully-Fisher relations holds, strengthening previous claims that it is a more fundamental scaling relation than the classical Tully-Fisher relation.

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“…We use the parameter k to take into account different galaxy mass profiles: k ∼ 4 for the Hernquist profiles assumed by the model (see Barausse 2012, for details), but k ∼ 10 (or even larger) is possible if a core is present. On the other hand, strong lensing and accurate dynamical modelling have shown that the mass profiles of intermediate-mass, early-type galaxies are consistent with nearly isothermal profiles down to (at least) tenths of the effective radius (e.g., Cappellari et al 2015, and references therein). These have k ∼ 1.…”

Section: The Normalisation Of the Scaling Relations And The Role Of Smentioning

confidence: 99%

Selection bias in dynamically measured supermassive black hole samples: scaling relations and correlations between residuals in semi-analytic galaxy formation models

Barausse

Shankar

Bernardi

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Recent work has confirmed that the scaling relations between the masses of supermassive black holes and host-galaxy properties such as stellar masses and velocity dispersions may be biased high. Much of this may be caused by the requirement that the black-hole sphere of influence must be resolved for the black-hole mass to be reliably estimated. We revisit this issue with a comprehensive galaxy evolution semi-analytic model. Once tuned to reproduce the (mean) correlation of black-hole mass with velocity dispersion, the model cannot account for the correlation with stellar mass. This is independent of the model's parameters, thus suggesting an internal inconsistency in the data. The predicted distributions, especially at the low-mass end, are also much broader than observed. However, if selection effects are included, the model's predictions tend to align with the observations. We also demonstrate that the correlations between the residuals of the scaling relations are more effective than the relations themselves at constraining AGN feedback models. In fact, we find that our model, while in apparent broad agreement with the scaling relations when accounting for selection biases, yields very weak correlations between their residuals at fixed stellar mass, in stark contrast with observations. This problem persists when changing the AGN feedback strength, and is also present in the hydrodynamic cosmological simulation Horizon-AGN, which includes state-of-the-art treatments of AGN feedback. This suggests that current AGN feedback models are too weak or simply not capturing the effect of the black hole on the stellar velocity dispersion.

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Small Scatter and Nearly Isothermal Mass Profiles to Four Half-Light Radii From Two-Dimensional Stellar Dynamics of Early-Type Galaxies

Cited by 116 publications

References 47 publications

A Testable Conspiracy: Simulating Baryonic Effects on Self-interacting Dark Matter Halos

A Testable Conspiracy: Simulating Baryonic Effects on Self-interacting Dark Matter Halos

The H I Tully-Fisher relation of early-type galaxies

Selection bias in dynamically measured supermassive black hole samples: scaling relations and correlations between residuals in semi-analytic galaxy formation models

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