Physical correlations of the scatter between galaxy mass, stellar content, and halo mass

Bradshaw, Christopher; Leauthaud, Alexie; Hearin, Andrew P.; Huang, Song; Behroozi, Peter

doi:10.1093/mnras/staa081

Cited by 38 publications

(28 citation statements)

References 115 publications

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“…well after transition, galaxies can still grow via merging and residual star formation. Although we do not explicitly separate the in-situ and ex-situ growth when computing the transition time, the fast growth phase is dominated by in-situ growth, while ex-situ growth only becomes important for massive quiescent galaxies 41,42 . To see what effect this has on the SHMR, Fig.…”

Section: The Evolution Of the Shmrmentioning

confidence: 99%

The Origin of the Colour Bimodality in the Scatter of the Stellar-to-Halo Mass Relation

Cui

Davé

Peacock

et al. 2020

Preprint

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Recent observations reveal that there is a strong bimodality in the scatter around the galaxy stellar-to-halo mass relation (SHMR): at a given halo mass, galaxies with a higher stellar mass tend to be blue indicating a higher specific star formation rate, while galaxies having a lower stellar mass tend to be red and quiescent; or at a given stellar mass, blue galaxies tend to live in halos with lower mass while red galaxies tend to have massive host halo. This has important implications for abundance matching and halo occupancy models commonly used in cosmological studies, but its physical origin remains debated. The SIMBA cosmological galaxy formation simulation successfully reproduces these observations, enabling us to investigate the physical driver behind this phenomenon. We show that the offset from the mean SHMR is strongly correlated with both halo formation time when half the halo mass assembled, as well as galaxy transition time defined as when the stellar doubling time becomes longer than 10 Gyr. Moreover, these two quantities are anti-correlated: early formed halos tend to host late transition galaxies corresponding to blue galaxies today, and vice versa, particularly for halo masses 11.5 ≲ log Mhalo ≲ 12.8M⊙ and galaxy stellar masses log M∗ ≥ 10M⊙. Prior to their transition time, galaxies lie on the SHMR for blue galaxies. Early transition galaxies, hosted by late formed halos, have their stellar mass growth almost ceased owing to AGN feedback even though their host halos continue to accrete mass, which moves these galaxies off the blue SHMR towards the red one creating the SHMR bimodality. We then investigate why early formed halos tend to host late transition galaxies. We find two key interconnected times: the gas-to-stellar domination time when the galaxy’s cold gas mass becomes smaller than its stellar mass, and the black hole (BH) jet ignition time governed by the BH Eddington ratio. Both show strong linear correlations with the galaxy transition time. Early formed halos have higher cold gas fractions (defined by cold gas mass in central galaxy with respect to the host halo mass) with a lower stellar-to-halo mass growth ratio before the transition time compared to the median or late forming halos; this allows them to sustain their stellar growth longer. Eventually, the continued growth fed by the cold gas reservoir allows them to surpass the galaxies with early transition times. Conversely, galaxies hosted by late formed halos have less cold gas with high stellar-to-halo mass growth ratios. Hence the Eddington rate be-comes low earlier on, which triggers AGN into an energetic jet mode that heats gas, rapidly truncates further accretion and also stops star formation. These processes thus conspire to create the SHMR bimodality. In SIMBA, the cold gas evolution occurs naturally owing to the interplay of accretion and star formation feedback, while the AGN feedback transitions from a radiative mode at high Eddington ratios that is ineffective at quenching, to a jet mode at low Eddington ratios that suppresses star formation. SIMBA further includes X-ray feedback that drives the last remaining cold gas out, completing the quenching and strengthening the SHMR bimodality.

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Section: The Evolution Of the Shmrmentioning

confidence: 99%

The Origin of the Colour Bimodality in the Scatter of the Stellar-to-Halo Mass Relation

Cui

Davé

Peacock

et al. 2020

Preprint

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“…Another possibility resides in the use of different mass proxies. A stellar mass based mass proxy, such as the one presented in [92] is expected to be less impacted by projection effects [93]. In future work, we plan on comparing results from these different mass proxies, which could help with shedding light on the unknown systematics found in this work.…”

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confidence: 98%

Dark Energy Survey Year 1 Results: Cosmological constraints from cluster abundances and weak lensing

Abbott¹,

Aguena²,

Alarcón³

et al. 2020

Phys. Rev. D

243

152

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We perform a joint analysis of the counts and weak lensing signal of redMaPPer clusters selected from the Dark Energy Survey (DES) Year 1 dataset. Our analysis uses the same shear and source photometric redshifts estimates as were used in the DES combined probes analysis. Our analysis results in surprisingly low values for S 8 ¼ σ 8 ðΩ m =0.3Þ 0.5 ¼ 0.65 AE 0.04, driven by a low matter density parameter, Ω m ¼ 0.179 þ0.031 −0.038 , with σ 8 − Ω m posteriors in 2.4σ tension with the DES Y1 3x2pt results, and in 5.6σ with the Planck CMB analysis. These results include the impact of post-unblinding changes to the analysis, which did not improve the level of consistency with other data sets compared to the results obtained at the unblinding. The fact that multiple cosmological probes (supernovae, baryon acoustic oscillations, cosmic shear, galaxy clustering and CMB anisotropies), and other galaxy cluster analyses all favor significantly higher matter densities suggests the presence of systematic errors in the data or an incomplete modeling of the relevant physics. Cross checks with x-ray and microwave data, as well as independent constraints on the observable-mass relation from Sunyaev-Zeldovich selected clusters, suggest that the discrepancy resides in our modeling of the weak lensing signal rather than the cluster abundance. Repeating our analysis using a higher richness threshold (λ ≥ 30) significantly reduces the tension with other probes, and points to one or more richness-dependent effects not captured by our model.

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“…Nevertheless, the reconstruction performance also depends on the accuracy of the inferred halo masses in the observations, thus the impacts of realistic halo mass scatters on our results were also investigated in this work. A better understanding of the relation between observables and underlying halos in the galaxy-halo connection and observable-mass relation studies (see Wechsler & Tinker 2018;Bradshaw et al 2020 and references therein) should be essential and critical to decreasing the mass scatters and consequently to maximizing the gains of biased tracer reconstruction.…”

Section: Discussionmentioning

confidence: 99%

Biased Tracer Reconstruction with Halo Mass Information

Liu

2021

ApJS

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Plenty of crucial information about our universe is encoded in the cosmic large-scale structure (LSS). However, extractions of this information are usually hindered by the nonlinearities of the LSS, which can be largely alleviated by various techniques known as reconstruction. In realistic applications, the efficiencies of these methods are always degraded by many limiting factors, a quite important one being the shot noise induced by the finite number density of biased matter tracers (i.e., luminous galaxies or dark matter halos) in observations. In this work, we explore the gains of biased tracer reconstruction achieved from halo mass information, which can suppress the shot-noise component and dramatically improves the cross-correlation between tracer field and dark matter. To this end, we first closely study the clustering biases and the stochasticity properties of halo fields with various number densities under different weighting schemes, i.e., the uniform, mass, and optimal weightings. Then, we apply the biased tracer reconstruction method to these different weighted halo fields and investigate how linear bias and observational mass scatter affect the reconstruction performance. Our results demonstrate that halo masses are critical information for significantly improving the performance of biased tracer reconstruction, indicating great application potential for substantially promoting the precision of cosmological measurements (especially for baryon acoustic oscillations) in ambitious ongoing and future galaxy surveys.

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Physical correlations of the scatter between galaxy mass, stellar content, and halo mass

Cited by 38 publications

References 115 publications

The Origin of the Colour Bimodality in the Scatter of the Stellar-to-Halo Mass Relation

The Origin of the Colour Bimodality in the Scatter of the Stellar-to-Halo Mass Relation

Dark Energy Survey Year 1 Results: Cosmological constraints from cluster abundances and weak lensing

Biased Tracer Reconstruction with Halo Mass Information

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