用Sunyaev-Zel 'dovich成像探测星系团内介质湍流

IF 5.8 2区 物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS Astronomy & Astrophysics Pub Date : 2025-02-11 DOI:10.1051/0004-6361/202452342
R. Adam, T. Eynard-Machet, I. Bartalucci, D. Cherouvrier, N. Clerc, L. Di Mascolo, S. Dupourqué, C. Ferrari, J.-F. Macías-Pérez, E. Pointecouteau, G. W. Pratt
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引用次数: 0

摘要

紊流气体运动预计将主导簇内介质(ICM)的非热能收支。高角分辨率Sunyaev-Zel 'dovich成像的压力波动测量为研究ICM湍流开辟了一条新的途径,补充了x射线密度波动测量。我们开发了一个方法框架,旨在优化提取ICM压力波动功率谱统计信息,并公开发布了名为PITSZI(探测ICM湍流从Sunyaev-Zel 'dovich成像)的相关软件。我们将该工具应用于合并星团MACS J0717.5+3745的新IRAM KIDs阵列(NIKA)数据,测量了其压力波动功率谱的高显著性,并探讨了其非热含量的影响。根据径向压力模型的选择和应用方法的细节,我们测量了能量注入规模为Linj ~ 800kpc。功率谱归一化对应于特征幅值达到。这些结果是假设MACS J0717.5+3745的ICM可以描述为单个(光滑)晕上的压力波动,并且由于径向压力模型的选择而被系统控制。通过模拟,我们确定将径向模型拟合到数据中可以将观测到的波动抑制高达50%,而代表性差的径向模型可能会导致虚假波动,我们也对其进行了量化。假设压力波动和湍流之间存在标准标度关系,我们发现MACS J0717.5+3745具有湍流速度色散σv ~ 1200 km/s,动力学到动力学加热压分数Pkin/Pkin + th ~ 20%,我们估计流体静力质量偏差为bHSE ~ 0.3 ~ 0.4。我们的结果与从x射线表面亮度波动中获得的其他测量结果非常一致,并且与波动在本质上是绝热的一致。
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PITSZI: Probing intra-cluster medium turbulence with Sunyaev–Zel’dovich imaging
Turbulent gas motions are expected to dominate the non-thermal energy budget of the intracluster medium (ICM). The measurement of pressure fluctuations from high angular resolution Sunyaev–Zel’dovich imaging opens a new avenue to study ICM turbulence, complementary to X-ray density fluctuation measures. We developed a methodological framework designed to optimally extract information on the ICM pressure fluctuation power spectrum statistics, and publicly released the associated software named PITSZI (Probing ICM Turbulence from Sunyaev–Zel’dovich Imaging). We applied this tool to the New IRAM KIDs Array (NIKA) data of the merging cluster MACS J0717.5+3745 to measure its pressure fluctuation power spectrum at high significance, and to investigate the implications for its non-thermal content. Depending on the choice of the radial pressure model and the details of the applied methodology, we measured an energy injection scale Linj ∼ 800 kpc. The power spectrum normalization corresponds to a characteristic amplitude reaching . These results were obtained assuming that the ICM of MACS J0717.5+3745 can be described as pressure fluctuations on top of a single (smooth) halo, and were dominated by systematics due to the choice of the radial pressure model. Using simulations, we determined that fitting a radial model to the data can suppress the observed fluctuations by up to ∼50%, while a poorly representative radial model can induce spurious fluctuations, which we also quantified. Assuming standard scaling relations between the pressure fluctuations and turbulence, we find that MACS J0717.5+3745 presents a turbulent velocity dispersion σv ∼ 1200 km/s, a kinetic to kinetic plus thermal pressure fraction Pkin/Pkin + th ∼ 20%, and we estimate the hydrostatic mass bias to bHSE ∼ 0.3 − 0.4. Our results are in excellent agreement with alternative measurements obtained from X-ray surface brightness fluctuations, and in agreement with the fluctuations being adiabatic in nature.
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来源期刊
Astronomy & Astrophysics
Astronomy & Astrophysics 地学天文-天文与天体物理
CiteScore
10.20
自引率
27.70%
发文量
2105
审稿时长
1-2 weeks
期刊介绍: Astronomy & Astrophysics is an international Journal that publishes papers on all aspects of astronomy and astrophysics (theoretical, observational, and instrumental) independently of the techniques used to obtain the results.
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