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Inferring the density, spin-temperature and neutral-fraction fields of HI from its 21-cm brightness temperature field using machine learning 利用机器学习从 21 厘米亮度温度场推断 HI 的密度场、自旋温度场和中性分数场
Pub Date : 2024-09-10 DOI: arxiv-2409.06769
Bohdan Bidenko, Léon V. E. Koopmans, P. Daniel Meerburg
The 21-cm brightness-temperature field of neutral hydrogen during the Epochof Reionization and Cosmic Dawn is a rich source of cosmological andastrophysical information, primarily due to its significant non-Gaussianfeatures. However, the complex, nonlinear nature of the underlying physicalprocesses makes analytical modelling of this signal challenging. Consequently,studies often resort to semi-numerical simulations. Traditional analysismethods, which rely on a limited set of summary statistics, may not adequatelycapture the non-Gaussian content of the data, as the most informativestatistics are not predetermined. This paper explores the application ofmachine learning (ML) to surpass the limitations of summary statistics byleveraging the inherent non-Gaussian characteristics of the 21-cm signal. Wedemonstrate that a well-trained neural network can independently reconstructthe hydrogen density, spin-temperature, and neutral-fraction fields withcross-coherence values exceeding 0.95 for $k$-modes below $0.5$ Mpc h$^{-1}$,based on a representative simulation at a redshift of $z approx 15$. Toachieve this, the neural network utilises the non-Gaussian information inbrightness temperature images over many scales. We discuss how thesereconstructed fields, which vary in their sensitivity to model parameters, canbe employed for parameter inference, offering more direct insights intounderlying cosmological and astrophysical processes only using limited summarystatistics of the brightness temperature field, such as its power spectrum.
再电离和宇宙黎明纪(Epochof Reionization and Cosmic Dawn)期间中性氢的 21 厘米亮度-温度场是宇宙学和天体物理学信息的丰富来源,这主要是由于它具有显著的非高斯特征。然而,由于基本物理过程的复杂性和非线性,对这一信号进行分析建模具有挑战性。因此,研究通常采用半数值模拟。传统的分析方法依赖于一组有限的汇总统计量,可能无法充分捕捉数据的非高斯内容,因为最有信息量的统计量并不是预先确定的。本文探讨了机器学习(ML)的应用,通过利用 21 厘米信号固有的非高斯特性来超越汇总统计的局限性。我们演示了一个训练有素的神经网络可以独立地重建氢密度场、自旋-温度场和中性分数场,对于低于0.5 Mpc h$^{-1}$的k$模式,交叉相干值超过0.95,这是基于红移为$z 约15$的代表性模拟。为了实现这一目标,神经网络利用了许多尺度的亮度温度图像中的非高斯信息。我们讨论了如何利用这些对模型参数敏感度不同的重建场来进行参数推断,从而仅利用亮度温度场的有限摘要统计(如其功率谱)就能更直接地洞察宇宙学和天体物理学的内在过程。
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引用次数: 0
Bayesian evidence for uncorrected gain factors in Galactic synchrotron template maps 银河系同步辐射模板图中未校正增益因子的贝叶斯证据
Pub Date : 2024-09-10 DOI: arxiv-2409.06770
Michael J. Wilensky, Melis O. Irfan, Philip Bull
The 408 MHz Haslam map is widely used as a low-frequency anchor for theintensity and morphology of Galactic synchrotron emission. Multi-frequency,multi-experiment fits show evidence of spatial variation and curvature in thesynchrotron frequency spectrum, but there are also poorly-understood gainfactors between experiments. We perform a Bayesian model comparison across arange of scenarios, using fits that include recent spectroscopic observationsat $sim 1$~GHz by MeerKAT. A large uncorrected gain factor of about 60% inthe Haslam data is strongly preferred, partly undermining its use as areference template.
408 MHz Haslam 地图被广泛用作银河系同步辐射强度和形态的低频锚。多频率、多实验拟合结果显示了同步辐射频谱的空间变化和曲率,但实验之间的增益因子也不甚明了。我们使用贝叶斯模型对一系列情况进行了比较,拟合结果包括了最近由 MeerKAT 在 $sim 1$~GHz 进行的光谱观测。我们强烈倾向于使用哈斯拉姆数据中约60%的大的未校正增益因子,这在一定程度上削弱了其作为参考模板的作用。
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引用次数: 0
SCALE at Scale: Cosmological applications of small-scale CMB lensing 规模上的 SCALE:小尺度 CMB 透镜的宇宙学应用
Pub Date : 2024-09-09 DOI: arxiv-2409.05326
Victor C. Chan, Renée Hložek, Joel Meyers, Alexander van Engelen
The Small-Correlated-Against-Large Estimator (SCALE) for small-scale lensingof the cosmic microwave background (CMB) provides a novel method for measuringthe amplitude of CMB lensing power without the need for reconstruction of thelensing field. In our previous study, we showed that the SCALE method canoutperform existing reconstruction methods to detect the presence of lensing atsmall scales ($ell gg 3000$). Here we develop a procedure to includeinformation from SCALE in cosmological parameter inference. We construct aprecise neural network emulator to quickly map cosmological parameters todesired CMB observables such as temperature and lensing power spectra and SCALEcross spectra. We also outline a method to apply SCALE to full-sky maps of theCMB temperature field, and construct a likelihood for the application of SCALEin parameter estimation. SCALE supplements conventional observables such as theCMB power spectra and baryon acoustic oscillations in constraining parametersthat are sensitive to the small-scale lensing amplitude such as the neutrinomass $m_nu$. We show that including estimates of the small-scale lensingamplitude from SCALE in such an analysis provides enough constraininginformation to measure the minimum neutrino mass at $4sigma$ significance inthe scenario of minimal mass, and higher significance for higher mass. Finally,we show that SCALE will play a powerful role in constraining models ofclustering that generate scale-dependent modulation to the distribution ofmatter and the lensing power spectrum, as predicted by models of warm or fuzzydark matter.
针对宇宙微波背景(CMB)小尺度透镜的 "小相关-大相关估算器"(SCALE)提供了一种测量CMB透镜功率振幅的新方法,而无需重建透镜场。在我们之前的研究中,我们表明SCALE方法在探测小尺度($ell gg 3000$)上的透镜现象时可以优于现有的重建方法。在这里,我们开发了一个程序,把来自SCALE的信息纳入宇宙学参数推断中。我们构建了一个精确的神经网络模拟器,将宇宙学参数快速映射到所需的CMB观测数据上,如温度、透镜功率谱和SCALE交叉谱。我们还概述了将 SCALE 应用于 CMB 温度场全天空图的方法,并构建了将 SCALE 应用于参数估计的可能性。SCALE是对CMB功率谱和重子声振荡等传统观测指标的补充,用于约束对小尺度透镜振幅敏感的参数,如中微子质量(neutrinomass)$m_nu$。我们表明,在这样的分析中包括来自SCALE的小尺度透镜振幅的估计值,可以提供足够的约束信息,在最小质量的情况下以$4sigma$的显著性测量最小中微子质量,而在更大质量的情况下则以更高的显著性测量最小中微子质量。最后,我们展示了SCALE将在约束聚类模型中发挥强大的作用,这些聚类模型会对物质的分布和透镜功率谱产生规模依赖性调制,正如暖暗物质或模糊暗物质模型所预测的那样。
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引用次数: 0
ForestFlow: cosmological emulation of Lyman-$α$ forest clustering from linear to nonlinear scales ForestFlow:从线性到非线性尺度的莱曼-$α$森林聚类的宇宙学模拟
Pub Date : 2024-09-09 DOI: arxiv-2409.05682
J. Chaves-Montero, L. Cabayol-Garcia, M. Lokken, A. Font-Ribera, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, S. Cole, A. de la Macorra, S. Ferraro, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, K. Honscheid, R. Kehoe, D. Kirkby, A. Kremin, A. Lambert, M. Landriau, M. Manera, P. Martini, R. Miquel, A. Muñoz-Gutiérrez, G. Niz, I. Pérez-Ràfols, G. Rossi, E. Sanchez, M. Schubnell, D. Sprayberry, G. Tarlé, B. A. Weaver
On large scales, measurements of the Lyman-$alpha$ forest offer insightsinto the expansion history of the Universe, while on small scales, these imposestrict constraints on the growth history, the nature of dark matter, and thesum of neutrino masses. This work introduces ForestFlow, a cosmologicalemulator designed to bridge the gap between large- and small-scaleLyman-$alpha$ forest analyses. Using conditional normalizing flows, ForestFlowemulates the 2 Lyman-$alpha$ linear biases ($b_delta$ and $b_eta$) and 6parameters describing small-scale deviations of the 3D flux power spectrum($P_mathrm{3D}$) from linear theory. These 8 parameters are modeled as afunction of cosmology $unicode{x2013}$ the small-scale amplitude and slope ofthe linear power spectrum $unicode{x2013}$ and the physics of theintergalactic medium. Thus, in combination with a Boltzmann solver, ForestFlowcan predict $P_mathrm{3D}$ on arbitrarily large (linear) scales and the 1Dflux power spectrum ($P_mathrm{1D}$) $unicode{x2013}$ the primary observablefor small-scale analyses $unicode{x2013}$ without the need for interpolationor extrapolation. Consequently, ForestFlow enables for the first timemultiscale analyses. Trained on a suite of 30 fixed-and-paired cosmologicalhydrodynamical simulations spanning redshifts from $z=2$ to $4.5$, ForestFlowachieves $3$ and $1.5%$ precision in describing $P_mathrm{3D}$ and$P_mathrm{1D}$ from linear scales to $k=5,mathrm{Mpc}^{-1}$ and$k_parallel=4,mathrm{Mpc}^{-1}$, respectively. Thanks to itsparameterization, the precision of the emulator is also similar for bothionization histories and two extensions to the $Lambda$CDM model$unicode{x2013}$ massive neutrinos and curvature $unicode{x2013}$ notincluded in the training set. ForestFlow will be crucial for the cosmologicalanalysis of Lyman-$alpha$ forest measurements from the DESI survey.
在大尺度上,对莱曼-$alpha$森林的测量提供了对宇宙膨胀历史的洞察,而在小尺度上,这些测量对宇宙的成长历史、暗物质的性质以及中微子质量的总和施加了严格的约束。这项工作介绍了ForestFlow,这是一个宇宙学模拟器,旨在弥合大尺度和小尺度莱曼-$alpha$森林分析之间的差距。利用条件归一化流,ForestFlow模拟了2个莱曼-$alpha$线性偏差($b_Δ$和$b_eta$)和6个描述三维通量功率谱($P_mathrm{3D}$)与线性理论的小尺度偏差的参数。这8个参数被建模为宇宙学($unicode{x2013}$)、线性功率谱的小尺度振幅和斜率($unicode{x2013}$)以及银河介质物理学的函数。因此,与波尔兹曼求解器相结合,ForestFlow可以预测任意大(线性)尺度的P_mathrm{3D}$和1D流功率谱(P_mathrm{1D}$)$unicode{x2013}$,这是小规模分析的主要观测指标$unicode{x2013}$,而不需要内插法或外推法。因此,ForestFlow首次实现了多尺度分析。ForestFlow在一套30个固定和配对的宇宙流体力学模拟上进行了训练,红移范围从$z=2$到$4.5$,ForestFlow达到了$3$和$1.5%的精度,分别描述了从线性尺度到k=5,mathrm{Mpc}^{-1}$和k_parallel=4,mathrm{Mpc}^{-1}$的P_mathrm{3D}$和P_mathrm{1D}$。得益于参数化,仿真器的精度对于两种离子化历史以及训练集中未包含的$Lambda$CDM模型的两个扩展$unicode{x2013}$大质量中微子和曲率$unicode{x2013}$也是相似的。ForestFlow对于从DESI巡天中得到的莱曼-$α$森林测量结果的宇宙学分析至关重要。
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引用次数: 0
The impact of feedback on the evolution of gas density profiles from galaxies to clusters: a universal fitting formula from the Simba suite of simulations 反馈对从星系到星团的气体密度剖面演变的影响:来自辛巴模拟套件的通用拟合公式
Pub Date : 2024-09-09 DOI: arxiv-2409.05815
Daniele Sorini, Sownak Bose, Romeel Davé, Daniel Anglés Alcázar
The radial distribution of gas within galactic haloes is connected to thestar formation rate and the nature of baryon-driven feedback processes. Usingsix variants of the hydrodynamic simulation Simba, we study the impact ofdifferent stellar/AGN feedback prescriptions on the gas density profiles ofhaloes in the total mass range $10^{11} , mathrm{M}_{odot} <M_{mathrm{200c}} < 10^{14} , mathrm{M}_{odot}$ and redshift interval$0
星系晕内气体的径向分布与恒星形成率和重子驱动反馈过程的性质有关。利用流体力学模拟Simba的六个变体,我们研究了不同的恒星/AGN反馈预设对总质量范围为$10^{11}, mathrm{M}_{odot_odot}的星系晕气体密度剖面的影响。mathrm{M}_{odot}
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引用次数: 0
Hitting the mark: Optimising Marked Power Spectra for Cosmology 击中目标为宇宙学优化标记功率谱
Pub Date : 2024-09-09 DOI: arxiv-2409.05695
Jessica A. Cowell, David Alonso, Jia Liu
Marked power spectra provide a computationally efficient way to extractnon-Gaussian information from the matter density field using the usual analysistools developed for the power spectrum without the need for explicitcalculation of higher-order correlators. In this work, we explore the optimalform of the mark function used for re-weighting the density field, to maximallyconstrain cosmology. We show that adding to the mark function or multiplying itby a constant leads to no additional information gain, which significantlyreduces our search space for optimal marks. We quantify the information gain ofthis optimal function and compare it against mark functions previously proposedin the literature. We find that we can gain around $sim2$ times smaller errorsin $sigma_8$ and $sim4$ times smaller errors in $Omega_m$ compared to usingthe traditional power spectrum alone, an improvement of $sim60%$ compared toother proposed marks when applied to the same dataset.
标记功率谱提供了一种计算高效的方法,利用为功率谱开发的常规分析工具,从物质密度场中提取非高斯信息,而无需明确计算高阶相关因子。在这项工作中,我们探索了用于重新加权密度场的标记函数的最优形式,以最大限度地约束宇宙学。我们证明,增加标记函数或乘以一个常数不会带来额外的信息增益,这大大缩小了我们寻找最优标记的空间。我们量化了这个最优函数的信息增益,并将其与之前文献中提出的标记函数进行了比较。我们发现,与单独使用传统的功率谱相比,我们可以在 $sigma_8$ 和 $Omega_m$ 中分别获得约 $sim2$ 倍和 $sim4$ 倍的较小误差,与其他提出的标记相比,在应用于相同数据集时提高了 $sim60%$ 。
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引用次数: 0
Cosmological constraints from angular homogeneity scale measurements 角均匀性尺度测量的宇宙学约束
Pub Date : 2024-09-09 DOI: arxiv-2409.06009
Xiaoyun Shao, Carlos A. P. Bengaly, Rodrigo S. Gonçalves, Gabriela C. Carvalho, Jailson Alcaniz
In this paper, we obtain new measurements of the angular homogeneity scale($theta_H$) from the BOSS DR12 and eBOSS DR16 catalogs of Luminous RedGalaxies of the Sloan Digital Sky Survey. Considering the flat $Lambda$CDMmodel, we use the $theta_H(z)$ data to constrain the matter density parameter($Omega_{m0}$) and the Hubble constant ($H_{0}$). We find $H_0 = 65.7 pm 7.0$km s$^{-1}$ Mpc$^{-1}$ and $Omega_{m0}>0.293$. By combining the $theta_H$measurements with current Baryon Acoustic Oscillations (BAO) and Type IaSupernova (SN) data, we obtain $H_{0}= 69.9^{+4.9}_{-4.5}$ km s$^{-1}$Mpc$^{-1}$ and $Omega_{m0} = 0.294^{+0.013}_{-0.015}$ ($theta_H$ + BAO) and$H_{0}=70.7^{+5.2}_{-4.1}$ km s$^{-1}$ Mpc$^{-1}$ and $Omega_{m0}=0.299 pm0.022$ ($theta_H$ + SN). We show that $theta_H$ measurements help break theBAO and SN degeneracies concerning $H_0$, as they do not depend on the soundhorizon scale at the drag epoch or the SN absolute magnitude value obtainedfrom the distance ladder method. Hence, despite those constraints being loosecompared to other probes, $theta_H$ data may provide an independentcosmological probe of $H_0$ in light of the Hubble tension. For completeness,we also forecast the constraining power of future $theta_H$ data via MonteCarlo simulations. Considering a relative error of the order of 1$%$, weobtain competitive constraints on $Omega_{m0}$ and $H_0$ ($approx 5%$ error)from the joint analysis with current SN and BAO measurements.
在本文中,我们从斯隆数字巡天的BOSS DR12和eBOSS DR16的发光红星系表中获得了新的角均匀性尺度($theta_H$)的测量结果。考虑到平坦的$Lambda$CDM模型,我们使用$theta_H(z)$数据来约束物质密度参数($Omega_{m0}$)和哈勃常数($H_{0}$)。我们发现 $H_0 = 65.7 pm 7.0$km s$^{-1}$ Mpc$^{-1}$ 和 $Omega_{m0}>0.293$ 。将$theta_H$测量结果与当前的重子声学振荡(BAO)和Ia型超新星(SN)数据相结合,我们得到了$H_{0}= 69.9^{+4.9}_{-4.5}$ km s$^{-1}$ Mpc$^{-1}$ 和 $Omega_{m0} = 0.294^{+0.013}_{-0.015}$ ($theta_H$ + BAO)和$H_{0}= 70.7^{+5.2}_{-4.1}$ km s$^{-1}$ Mpc$^{-1}$ 和 $Omega_{m0}=0.299 pm0.022$ ($theta_H$ + SN)。我们的研究表明,$theta_H$的测量结果有助于打破关于$H_0$的BAO和SN退行性,因为它们并不依赖于拖曳纪元的声水平尺度,也不依赖于从距离阶梯法中得到的SN绝对震级值。因此,尽管与其他探测相比,这些约束比较宽松,但是$theta_H$数据可能会根据哈勃张力为$H_0$提供一个独立的宇宙学探测。为了完整起见,我们还通过蒙特卡洛模拟预测了未来$theta_H$数据的约束能力。考虑到1%的相对误差,我们通过与目前的SN和BAO测量联合分析,获得了对$Omega_{m0}$和$H_0$的有竞争力的约束(误差约为5%)。
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引用次数: 0
CMB polarization non-Gaussianity from accreting primordial black holes 来自吸积原始黑洞的CMB偏振非高斯性
Pub Date : 2024-09-09 DOI: arxiv-2409.06028
Trey W. JensenNYU, Yacine Ali-HaïmoudNYU
Primordial black holes (PBHs) would induce non-Gaussianity in the cosmicmicrowave background (CMB) by sourcing recombination perturbations spatiallymodulated by relative velocities between PBHs and the baryons they accrete. Theleading non-Gaussian signatures are non-vanishing connected 4-point correlationfunctions, or trispectra. Earlier, we computed the CMB temperature trispectrum,and forecasted Planck to be more sensitive to it than to changes in the CMBtemperature power spectrum for light enough PBHs. Excitingly, accreting PBHswould also induce non-Gaussianity in CMB polarization, and source both E and Bmodes, which we compute in this paper. We first calculate linear-responseperturbations to the tensor-valued photon distribution function sourced by ageneral spatially-varying ionization history, and apply our results toaccreting PBHs. We then compute linear-order perturbations to the temperatureand polarization 2-point functions sourced by inhomogeneities in recombinationdue to accreting PBHs; we find them to be negligible relative to theircounterparts sourced by homogeneous perturbations to the ionization history.Lastly, we compute all CMB trispectra including temperature, E- and B-modepolarization at linear order in the PBH abundance. We forecast that includingpolarization data in a 4-point-function analysis would only increase Planck'ssensitivity to accreting PBHs by a factor ~2 relative to using temperaturealone. As a consequence, we find that a search for PBHs using all temperatureand polarization trispectra with Planck data would mostly not be competitivewith current bounds from temperature and polarization power spectra. Incontrast, we forecast that a CMB Stage-4 experiment would gain significantsensitivity to accreting PBHs through a 4-point-function search, in particularthrough the contributions of parity-odd trispectra including one B-mode field.
原始黑洞(PBHs)会在宇宙微波背景(CMB)中引起非高斯性,因为它们会产生重组扰动,而重组扰动是由原始黑洞和它们吸积的重子之间的相对速度在空间上调节的。主要的非高斯特征是非幂相关的四点相关函数,或称三谱。早些时候,我们计算了 CMB 温度三谱,并预测普朗克对它比对足够轻的 PBH 的 CMB 温度功率谱变化更敏感。令人兴奋的是,增殖的PBH也会引起CMB极化的非高斯性,并同时产生E和B模式,我们在本文中计算了这两种模式。我们首先计算了由一般空间变化电离历史引起的张量光子分布函数的线性响应扰动,并将我们的结果应用于正在增生的 PBH。然后,我们计算了由于增殖 PBHs 引起的重组不均匀性对温度和偏振 2 点函数的线性阶扰动;我们发现,相对于电离历史的同质扰动,这些扰动可以忽略不计。最后,我们以 PBH 丰度的线性阶计算了包括温度、E 和 B 模偏振在内的所有 CMB 三谱图。我们预测,在四点函数分析中加入极化数据,只会使普朗克对增生PBHs的灵敏度比单纯使用温度提高约2倍。因此,我们发现,利用普朗克数据的所有温度和偏振三谱图来搜索PBHs,在大多数情况下都无法与当前温度和偏振功率谱图的边界相竞争。与此相反,我们预测 CMB 第四阶段实验将通过四点函数搜索,特别是通过包括一个 B 模式场在内的奇偶三谱的贡献,获得对增生 PBH 的显著灵敏度。
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引用次数: 0
Implications of feedback solutions to the $S_8$ tension for the baryon fractions of galaxy groups and clusters S_8$张力的反馈解对星系群和星系团重子分数的影响
Pub Date : 2024-09-09 DOI: arxiv-2409.05716
Jaime Salcido, Ian G. McCarthy
Recent large-scale structure (LSS) surveys have revealed a persistent tensionin the value of $S_8$ compared to predictions from the standard cosmologicalmodel. This tension may suggest the need for new physics beyond the standardmodel, but an accurate characterisation of baryonic effects is essential toavoid biases. Although some studies indicate that baryonic effects are toosmall to resolve this tension, others propose that more aggressive feedbackmechanisms could reconcile differences between cosmic microwave background(CMB) measurements and low-redshift LSS observations. In this paper, weinvestigate the role of baryonic effects in alleviating the $S_8$ tension. Weextend the SP(k) model (Salcido et al. 2023), which was trained on hundreds ofcosmological hydrodynamical simulations to map the suppression of the matterpower spectrum to the baryon fraction in groups and clusters, to predict therequired baryon fraction for a given $P(k)$ suppression. We then comparepredictions from recent cosmic shear (weak lensing) analyses with the latestbaryon budget measurements from X-ray and weak gravitational lensing studies.Our findings show that studies marginalising over baryonic effects while fixingcosmological parameters to a Planck-like cosmology predict strong $P(k)$suppression and baryon fractions that are much lower than existing low-redshiftbaryon budget estimates of galaxy groups and clusters. Conversely, most studiesthat marginalise over both cosmological parameters and baryonic effects implybaryon fractions that are consistent with observations but lower values of$S_8$ than inferred from the CMB. Unless the observed baryon fractions arebiased high by a factor of several, these results suggest that a mechanismbeyond baryonic physics alone is required to modify or slow down the growth ofstructure in the universe in order to resolve the $S_8$ tension.
最近的大尺度结构(LSS)探测发现,与标准宇宙学模型的预测值相比,$S_8$的值持续存在紧张关系。这种张力可能表明需要标准模型之外的新物理,但要避免偏差,就必须准确描述重子效应的特征。尽管一些研究表明重子效应太小,不足以解决这一矛盾,但另一些研究提出,更积极的反馈机制可以调和宇宙微波背景(CMB)测量与低红移 LSS 观测之间的差异。在本文中,我们研究了重子效应在缓解 $S_8$ 张力中的作用。我们扩展了SP(k)模型(Salcido等人,2023年),该模型是在数百次宇宙学流体力学模拟中训练出来的,用于将物质能量谱的压制映射到星团和星簇中的重子分数上,从而预测在给定的$P(k)$压制下所需的重子分数。我们的研究结果表明,在将宇宙学参数固定为普朗克类宇宙学的同时,将重子效应边际化的研究预测出了强烈的$P(k)$抑制和重子分数,而这些预测值远远低于现有的星系群和星系团的低重子预算估计值。与此相反,大多数对宇宙学参数和重子效应进行边际化的研究意味着重子分数与观测结果一致,但S_8$的值低于从CMB推断的值。除非观测到的重子分数偏高了几倍,否则这些结果表明,为了解决S_8$张力问题,需要一种超越重子物理学的机制来改变或减缓宇宙中结构的增长。
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引用次数: 0
The Galaxy Activity, Torus, and Outflow Survey (GATOS). V: Unveiling PAH survival and resilience in the circumnuclear regions of AGN with JWST 星系活动、环和外流巡天(GATOS)。V:利用 JWST 揭开多环芳香烃在 AGN 环核区的生存和恢复能力的面纱
Pub Date : 2024-09-09 DOI: arxiv-2409.05686
I. García-Bernete, D. Rigopoulou, F. R. Donnan, A. Alonso-Herrero, M. Pereira-Santella, T. Shimizu, R. Davies, P. F. Roche, S. García-Burillo, A. Labiano, L. Hermosa Muñoz, L. Zhang, A. Audibert, E. Bellocchi, A. Bunker, F. Combes, D. Delaney, D. Esparza-Arredondo, P. Gandhi, O. González-Martín, S. F. Hönig, M. Imanishi, E. K. S. Hicks, L. Fuller, M. Leist, N. A. Levenson, E. Lopez-Rodriguez, C. Packham, C. Ramos Almeida, C. Ricci, M. Stalevski, M. Villar Martín, M. J. Ward
We analyze JWST MIRI/MRS observations of the infrared PAH bands in thenuclear and circumnuclear regions of local AGN from the GATOS Survey. In thiswork, we examine the PAH properties in the circumnuclear regions of AGN andAGN-outflows, and compare them to those in star-forming regions and theinnermost regions of AGN. This study employs 4.9-28.1 micron sub-arcsecondangular resolution data to investigate the properties of PAH in three nearbysources (DL~30-40 Mpc). Our findings align with previous JWST studies, showingthat the central regions of AGN show a larger fraction of neutral PAH molecules(i.e. elevated 11.3/6.2 and 11.3/7.7 PAH ratios) compared to star-forminggalaxies. We find that the AGN might affect not only the PAH population in theinnermost region but also in the extended regions up to ~kpc scales. Bycomparing our observations to PAH diagnostic diagrams, we find that, ingeneral, regions located in the projected direction of the AGN-outflow occupysimilar positions on the PAH diagnostic diagrams as those of the innermostregions of AGN. Star-forming regions that are not affected by the AGN in thesegalaxies share the same part of the diagram as Star-forming galaxies. Weexamine the potential of the PAH-H2 diagram to disentangle AGN versusstar-forming activity. Our results suggest that in Sy-like AGN, illuminationand feedback from the AGN might affect the PAH population at nuclear and kpcscales, in particular, the ionization state of the PAH grains. However, PAHsizes are rather similar. The carriers of the ionized PAH bands (6.2 and 7.7micron) are less resilience than those of neutral PAH bands (11.3 micron),which might be particularly important for strongly AGN-host coupled systems.Therefore, caution must be applied when using PAH bands as star-formation rateindicators in these systems even at kpc scales, with the ionized ones beingmore affected by the AGN.
我们分析了 JWST MIRI/MRS 从 GATOS 巡天观测中观测到的局地 AGN 核区和环核区的红外 PAH 波段。在这项工作中,我们研究了AGN环核区和AGN外流的PAH特性,并将其与恒星形成区和AGN最内层区的PAH特性进行了比较。这项研究利用 4.9-28.1 微米亚弧秒分辨率数据,研究了三个近邻源(DL~30-40 Mpc)中 PAH 的性质。我们的研究结果与 JWST 之前的研究结果一致,表明与恒星形成星系相比,AGN 的中心区域显示出更大比例的中性 PAH 分子(即 11.3/6.2 和 11.3/7.7 PAH 比值升高)。我们发现,AGN可能不仅会影响最内层区域的PAH种群,也会影响延伸区域的PAH种群,其影响范围可达~kpc尺度。通过将我们的观测结果与PAH诊断图进行比较,我们发现,一般来说,位于AGN外流投影方向的区域在PAH诊断图上的位置与AGN最内层区域的位置相似。在这些星系中,没有受到AGN影响的恒星形成区域与恒星形成星系在图中的位置相同。我们研究了 PAH-H2 图在区分 AGN 与恒星形成活动方面的潜力。我们的研究结果表明,在Sy-like AGN中,AGN的光照和反馈可能会影响核尺度和kpc尺度的PAH种群,特别是PAH晶粒的电离状态。然而,多环芳香烃的大小相当相似。因此,在这些系统中使用 PAH 波段作为恒星形成率指标时必须谨慎,即使在 kpc 尺度上也是如此,电离的 PAH 波段受 AGN 的影响更大。
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引用次数: 0
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arXiv - PHYS - Cosmology and Nongalactic Astrophysics
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