Massive disc galaxies too dominated by dark matter in cosmological hydrodynamical simulations

Marasco, Antonino; Posti, Lorenzo; Oman, Kyle A.; Famaey, Benoît; Cresci, G.; Fraternali, Filippo

doi:10.1051/0004-6361/202038326

Cited by 30 publications

(28 citation statements)

References 70 publications

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“…However, our findings suggest that in order to reproduce the dynamics of barred galaxies, massive spirals must be baryon-dominated and should lie above the abundance matching relation. This is consistent with the recently reported findings (e.g., Posti et al 2019;Marasco et al 2020), which highlight the tension between the stellar-to-dark matter ratio of high-mass spirals obtained dynamically, and via methods such as abundance matching.…”

Section: Discussionsupporting

confidence: 92%

“…Recent work by Posti et al (2019) explored galaxies in the SPARC sample (Lelli et al 2016), finding that massive spirals lie above the relation for f derived from abundance matching, which implies that massive spirals are overly efficient at converting gas to stars (the so-called 'failed feedback problem'). A subsequent study by Marasco et al (2020) found that massive spirals in SPARC are more baryon-dominated than spiral galaxies in cosmological simulations, such as EAGLE and IllustrisTNG100. Interestingly, the Auriga galaxies follow a similar trend as the high-mass spiral galaxies in the SPARC sample, which are denoted by the grey symbols.…”

Section: Comparison With Previous Pattern Speed Estimations From Cosmological Simulationsmentioning

confidence: 96%

“…The mean and 1σ values for disc (barred) galaxies are shown with the circles/thick lines (squares/thin lines) and shaded region respectively. For comparison, we also show the high-mass disc galaxies from the SPARC sample explored in Marasco et al (2020), where the error bars denote 16th-84th percentile uncertainties. Right: baryon dominance, V /V tot , as a function of radius of Auriga, EAGLE, and Illustris disc galaxies in the mass range 3 × 10 10 < M /M < 10 11 .…”

Section: Comparison With Previous Pattern Speed Estimations From Cosmological Simulationsmentioning

confidence: 99%

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Revisiting the tension between fast bars and the ΛCDM paradigm

Fragkoudi

Grand

Pakmor

et al. 2021

A&A

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The pattern speed with which galactic bars rotate is intimately linked to the amount of dark matter in the inner regions of their host galaxies. In particular, dark matter haloes act to slow down bars via torques exerted through dynamical friction. Observational studies of barred galaxies tend to find that bars rotate fast, while hydrodynamical cosmological simulations of galaxy formation and evolution in the Lambda cold dark matter (ΛCDM) framework have previously found that bars slow down excessively. This has led to a growing tension between fast bars and the ΛCDM cosmological paradigm. In this study we revisit this issue, using the Auriga suite of high-resolution, magneto-hydrodynamical cosmological zoom-in simulations of galaxy formation and evolution in the ΛCDM framework, finding that bars remain fast down to z = 0. In Auriga, bars form in galaxies that have higher stellar-to-dark matter ratios and are more baryon-dominated than in previous cosmological simulations; this suggests that in order for bars to remain fast, massive spiral galaxies must lie above the commonly used abundance matching relation. While this reduces the aforementioned tension between the rotation speed of bars and ΛCDM, it accentuates the recently reported discrepancy between the dynamically inferred stellar-to-dark matter ratios of massive spirals and those inferred from abundance matching. Our results highlight the potential of using bar dynamics to constrain models of galaxy formation and evolution.

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Section: Discussionsupporting

confidence: 92%

Section: Comparison With Previous Pattern Speed Estimations From Cosmological Simulationsmentioning

confidence: 96%

Section: Comparison With Previous Pattern Speed Estimations From Cosmological Simulationsmentioning

confidence: 99%

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Revisiting the tension between fast bars and the ΛCDM paradigm

Fragkoudi

Grand

Pakmor

et al. 2021

A&A

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“…6.1 in Wechsler & Tinker 2018). Some recent hydrodynamical simulations also display the expected differences between the SHMRs of early-type and late-type galaxies (Grand et al 2019;Marasco et al 2020;Correa & Schaye 2020).…”

Section: Introductionmentioning

confidence: 73%

Dynamical evidence for a morphology-dependent relation between the stellar and halo masses of galaxies

Posti

Fall

2021

A&A

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We derive the stellar-to-halo mass relation (SHMR), namely f⋆ ∝ M⋆/Mh versus M⋆ and Mh, for early-type galaxies from their near-infrared luminosities (for M⋆) and the position-velocity distributions of their globular cluster systems (for Mh). Our individual estimates of Mh are based on fitting a flexible dynamical model with a distribution function expressed in terms of action-angle variables and imposing a prior on Mh from the correlation between halo concentration and mass in the standard Λ cold dark matter (ΛCDM) cosmology. We find that the SHMR for early-type galaxies declines with mass beyond a peak at M⋆ ∼ 5 × 1010 M⊙ and Mh ∼ 1 × 1012 M⊙ (near the mass of the Milky Way). This result is consistent with the standard SHMR derived by abundance matching for the general population of galaxies, and also with previous, less robust derivations of the SHMR for early-type galaxies. However, it contrasts sharply with the monotonically rising SHMR for late-type galaxies derived from extended HI rotation curves and the same ΛCDM prior on Mh that we adopt for early-type galaxies. We show that the SHMR for massive galaxies varies more or less continuously with disc fraction and Hubble type between these rising and falling branches. We also show that the different SHMRs for late-type and early-type galaxies are consistent with the similar scaling relations between their stellar velocities and masses (the Tully–Fisher and the Faber–Jackson relations). As we demonstrate explicitly, differences in the relations between the stellar and halo virial velocities account for the similarity of the scaling relations. We argue that all these empirical findings are natural consequences of a picture in which galactic discs are built mainly by relatively smooth and gradual inflow, regulated by feedback from young stars, while galactic spheroids are built by a combination of merging, black-hole fuelling, and feedback from active galactic nuclei.

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“…Finding a significantly different RAR at equal M would have interesting implications for galaxy formation models in the ΛCDM framework. In the ΛCDM framework it is expected that the galaxy-to-halo-mass relation, and therefore the RAR, can be different for different galaxy types through their galaxy formation history (Dutton et al 2010;Matthee et al 2017;Posti et al 2019;Marasco et al 2020). Two parameters that correlate heavily with galaxy formation history are Sérsic index and colour.…”

Section: The Rar For Early-and Late-type Kids Galaxiesmentioning

confidence: 99%

The weak lensing radial acceleration relation: Constraining modified gravity and cold dark matter theories with KiDS-1000

Brouwer

Oman²,

Valentijn³

et al. 2021

A&A

Self Cite

130

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We present measurements of the radial gravitational acceleration around isolated galaxies, comparing the expected gravitational acceleration given the baryonic matter (gbar) with the observed gravitational acceleration (gobs), using weak lensing measurements from the fourth data release of the Kilo-Degree Survey (KiDS-1000). These measurements extend the radial acceleration relation (RAR), traditionally measured using galaxy rotation curves, by 2 decades in gobs into the low-acceleration regime beyond the outskirts of the observable galaxy. We compare our RAR measurements to the predictions of two modified gravity (MG) theories: modified Newtonian dynamics and Verlinde’s emergent gravity (EG). We find that the measured relation between gobs and gbar agrees well with the MG predictions. In addition, we find a difference of at least 6σ between the RARs of early- and late-type galaxies (split by Sérsic index and u − r colour) with the same stellar mass. Current MG theories involve a gravity modification that is independent of other galaxy properties, which would be unable to explain this behaviour, although the EG theory is still limited to spherically symmetric static mass models. The difference might be explained if only the early-type galaxies have significant (Mgas ≈ M⋆) circumgalactic gaseous haloes. The observed behaviour is also expected in Λ-cold dark matter (ΛCDM) models where the galaxy-to-halo mass relation depends on the galaxy formation history. We find that MICE, a ΛCDM simulation with hybrid halo occupation distribution modelling and abundance matching, reproduces the observed RAR but significantly differs from BAHAMAS, a hydrodynamical cosmological galaxy formation simulation. Our results are sensitive to the amount of circumgalactic gas; current observational constraints indicate that the resulting corrections are likely moderate. Measurements of the lensing RAR with future cosmological surveys (such as Euclid) will be able to further distinguish between MG and ΛCDM models if systematic uncertainties in the baryonic mass distribution around galaxies are reduced.

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Massive disc galaxies too dominated by dark matter in cosmological hydrodynamical simulations

Cited by 30 publications

References 70 publications

Revisiting the tension between fast bars and the ΛCDM paradigm

Revisiting the tension between fast bars and the ΛCDM paradigm

Dynamical evidence for a morphology-dependent relation between the stellar and halo masses of galaxies

The weak lensing radial acceleration relation: Constraining modified gravity and cold dark matter theories with KiDS-1000

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