The spatial distribution deviation and the power suppression of baryons from dark matter

Yang, Hua-Yu; Wang, Yun; He, Pinjia; Zhu, Weishan; Feng, Long-Long

doi:10.1093/mnras/stab3062

Cited by 4 publications

(3 citation statements)

References 41 publications

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“…Moreover, by measuring the env-WCC in TNG100-1, we find that the dark matter and the gas in both the extreme dense (Δ  200) and underdense (Δ  0.1) environments always maintain very high correlation at all redshifts over a wide scale range, which qualitatively agrees with the findings in Farahi et al (2022) and Yang et al (2021). Particularly at the present epoch, the env-WCC is greater than 0.9 in densities of Δ  200 and Δ  0.1 at scales of k  10 h Mpc −1 .…”

Section: Discussionsupporting

confidence: 85%

“…On the simulation side, many studies have confirmed that the baryonic gas follows the underlying dark matter distribution on large scales quite well. For example, the power spectrum of the gas density field is very close to that of dark matter (e.g., Cui & Zhang 2017;Springel et al 2018), the spatial distributions of the dark matter and the baryonic gas are highly correlated with each other over a wide range of scales (e.g., Yang et al 2020Yang et al , 2021, and the gas alone can be used to classify the cosmic web in an unbiased manner (e.g., Cui et al 2018). Additionally, the intergalactic gas distribution is receiving increasing attention in observations.…”

Section: Introductionmentioning

confidence: 99%

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Simultaneous Dependence of Matter Clustering on Scale and Environment

Wang

2022

ApJ

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In this work, we propose new statistical tools that are capable of characterizing the simultaneous dependence of dark matter and gas clustering on the scale and the density environment, and these are the environment-dependent wavelet power spectrum (env-WPS), the environment-dependent bias function (env-bias), and the environment-dependent wavelet cross-correlation function (env-WCC). These statistics are applied to the dark matter and baryonic gas density fields of the TNG100-1 simulation at redshifts of z=3.0-0.0, and to Illustris-1 and SIMBA at z = 0. The measurements of the env-WPSs suggest that the clustering strengths of both the dark matter and the gas increase with increasing density, while that of a Gaussian field shows no density dependence. By measuring the env-bias and env-WCC, we find that they vary significantly with the environment, scale, and redshift. A noteworthy feature is that at z = 0.0, the gas is less biased in denser environments of Δ ≳ 10 around 3 h Mpc−1, due to the gas reaccretion caused by the decreased AGN feedback strength at lower redshifts. We also find that the gas correlates more tightly with the dark matter in both the most dense and underdense environments than in other environments at all epochs. Even at z = 0, the env-WCC is greater than 0.9 in Δ ≳ 200 and Δ ≲ 0.1 at scales of k ≲ 10 h Mpc−1. In summary, our results support the local density environment having a non-negligible impact on the deviations between dark matter and gas distributions up to large scales.

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Section: Discussionsupporting

confidence: 85%

Section: Introductionmentioning

confidence: 99%

Simultaneous Dependence of Matter Clustering on Scale and Environment

Wang

2022

ApJ

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“…Cui & Zhang 2017;Springel et al 2018), the spatial distributions of the dark matter and bary-onic gas are highly correlated with each other over a wide range of scales (e.g. Yang et al 2020Yang et al , 2021, and the gas alone can be used to classify the cosmic web un-biased (e.g. Cui et al 2018).…”

Section: Introductionmentioning

confidence: 99%

Simultaneous Dependence of Matter Clustering on Scale and Environment

Wang¹,

He²

2022

Preprint

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In this work, we propose new statistical tools that are capable of characterizing the simultaneous dependence of the matter clustering on the scale and density environment, which are the environment-dependent wavelet power spectrum (env-WPS) and environment-dependent wavelet cross-correlation (env-WCC). We apply these statistics to the projected 2D dark matter and baryonic gas density fields of the IllustrisTNG simulation at redshifts from z = 3.0 to z = 0.0. Measurement of the env-WPSs indicates that the clustering strengths of both the dark matter and gas increase with density. At all redshifts, we observe that the env-WPS of the gas is suppressed on intermediate and small scales, which is caused by baryonic processes. Furthermore, by computing the environmental bias function, we find that this suppression varies with the environment, scale and redshift. A noteworthy feature is that at z = 0.0, the bias value increases with density on scales 2 k 10 hMpc −1 , which is the reversal of that in earlier times. On the other hand, the env-WCC also shows strong environmental dependence on scales k 2 hMpc −1 and is sensitive to the redshift. We find that at z = 3.0, the coherence of the dark matter and gas decreases with density. At lower redshifts, the coherence in denser environments becomes much higher than that in less dense environments. These results suggest that baryonic processes have less effect on the matter clustering in high-density environments at later times. Obviously, these statistics provide us rich information and hence could improve our understanding of the matter clustering.

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How do baryonic effects on the cosmic matter distribution vary with scale and local density environment?

Wang,

2024

Monthly Notices of the Royal Astronomical Society

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In this study, we investigate how the baryonic effects vary with scale and local density environment mainly by utilizing a novel statistic, the environment-dependent wavelet power spectrum (env-WPS). With four state-of-the-art cosmological simulation suites, EAGLE, SIMBA, Illustris, and IllustrisTNG, we compare the env-WPS of the total matter density field between the hydrodynamic and dark matter-only (DMO) runs at z = 0. We find that the clustering is most strongly suppressed in the emptiest environment of $\rho _\mathrm{m}/\bar{\rho }_\mathrm{m}<0.1$ with maximum amplitudes ∼67 − 89 per cent on scales ∼1.86 − 10.96 hMpc−1, and less suppressed in higher density environments on small scales (except Illustris). In the environments of $\rho _\mathrm{m}/\bar{\rho }_\mathrm{m}\geqslant 0.316$ (≥10 in EAGLE), the feedbacks also lead to enhancement features at intermediate and large scales, which is most pronounced in the densest environment of $\rho _\mathrm{m}/\bar{\rho }_\mathrm{m}\geqslant 100$ and reaches a maximum ∼7 − 15 per cent on scales ∼0.87 − 2.62 hMpc−1 (except Illustris). The baryon fraction of the local environment decreases with increasing density, denoting the feedback strength, and potentially explaining some differences between simulations. We also measure the volume and mass fractions of local environments, which are affected by ≳ 1 per cent due to baryon physics. In conclusion, our results show that the baryonic processes can strongly modify the overall cosmic structure on the scales of k > 0.1 hMpc−1, which encourages further research in this direction.

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The spatial distribution deviation and the power suppression of baryons from dark matter

Cited by 4 publications

References 41 publications

Simultaneous Dependence of Matter Clustering on Scale and Environment

Simultaneous Dependence of Matter Clustering on Scale and Environment

Simultaneous Dependence of Matter Clustering on Scale and Environment

How do baryonic effects on the cosmic matter distribution vary with scale and local density environment?

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