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arXiv 1603.04784astro-ph.IMastro-ph.CO
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可见光区射电弱透镜切变测量-- I.方法

Radio Weak Lensing Shear Measurement in the Visibility Domain - I. Methodology

Marzia Rivi, Lance Miller, Sphesihle Makhathini, Filipe Batoni Abdalla

摘要:

平方公里阵列(SKA)等新一代射电望远镜的高灵敏度将使宇宙学弱透镜测量在无线电波长上与光学测量竞争。我们提出了一个适应无线电数据的透镜拟合,星系形状测量的方法最初开发和用于光学弱透镜调查。这种可能性的方法使用分析星系模型,并使贝叶斯边缘化的可能性在不感兴趣的参数。它具有直接在可见度域工作的特点,这是采用射电干涉仪数据的自然方法,避免了成像过程引入的系统性。作为一个概念的证明,我们提供的结果,个别星系的可见度模拟与通量密度S >= 10 μ Jy在相位中心的建议SKA 1-MID基线配置,采用12个频率通道的频带950 - 1190 MHz。弱透镜剪切测量从人口的星系与现实的流量和scalelength分布后,获得自然网格的原始vitamins。剪切测量预计会受到“噪声偏差”的影响:我们估计的偏差的方法作为一个函数的信噪比(SNR)。我们获得的加性和乘性偏置值分别与SNR > 18和SNR > 30的SKA 1要求相当。SNR > 10的乘法偏差与CFHTLenS等地基光学勘测中发现的乘法偏差相当,我们预计,与用于光学勘测的剪切测量校准策略类似的剪切测量校准策略可以用于SKA无线电干涉仪数据的分析中,效果良好。

英文摘要:

The high sensitivity of the new generation of radio telescopes such as the Square Kilometre Array (SKA) will allow cosmological weak lensing measurements at radio wavelengths that are competitive with optical surveys. We present an adaptation to radio data of lensfit, a method for galaxy shape measurement originally developed and used for optical weak lensing surveys. This likelihood method uses an analytical galaxy model and makes a Bayesian marginalisation of the likelihood over uninteresting parameters. It has the feature of working directly in the visibility domain, which is the natural approach to adopt with radio interferometer data, avoiding systematics introduced by the imaging process. As a proof of concept, we provide results for visibility simulations of individual galaxies with flux density S >= 10 muJy at the phase centre of the proposed SKA1-MID baseline configuration, adopting 12 frequency channels in the band 950 - 1190 MHz. Weak lensing shear measurements from a population of galaxies with realistic flux and scalelength distributions are obtained after natural gridding of the raw visibilities. Shear measurements are expected to be affected by "noise bias": we estimate the bias in the method as a function of signal-to-noise ratio (SNR). We obtain additive and multiplicative bias values that are comparable to SKA1 requirements for SNR > 18 and SNR > 30, respectively. The multiplicative bias for SNR > 10 is comparable to that found in ground-based optical surveys such as CFHTLenS, and we anticipate that similar shear measurement calibration strategies to those used for optical surveys may be used to good effect in the analysis of SKA radio interferometer data.

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