CHIPS: THE COSMOLOGICAL H i POWER SPECTRUM ESTIMATOR

CHIPS: THE COSMOLOGICAL H i POWER SPECTRUM ESTIMATOR
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DOI：
10.3847/0004-637x/818/2/139
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发表时间：
2016-01
期刊：
The Astrophysical Journal
影响因子：
--
通讯作者：
C. Trott;B. Pindor;P. Procopio;R. Wayth;D. Mitchell;B. McKinley;S. Tingay;N. Barry;A. Beardsley;G. Bernardi;J. Bowman;F. Briggs;R. Cappallo;P. Carroll;A. D. Oliveira-Costa;J. Dillon;A. Ewall-Wice;L. Feng;L. Greenhill;B. Hazelton;J. Hewitt;N. Hurley-Walker;M. Johnston-Hollitt;D. Jacobs;D. Kaplan;Hs. Kim;E. Lenc;J. Line;A. Loeb;C. Lonsdale;M. Morales;E. Morgan;A. Neben;N. Thyagarajan;D. Oberoi;A. Offringa;S. Ord;S. Paul;J. Pober;T. Prabu;J. Riding;N. Shankar;S. Sethi;K. Srivani;R. Subrahmanyan;I. Sullivan;Max Tegmark;R. Webster;A. Williams;C. Williams;C. Wu;J. Wyithe
C. Trott;B. Pindor;P. Procopio;R. Wayth;D. Mitchell;B. McKinley;S. Tingay;N. Barry;A. Beardsley;G. Bernardi;J. Bowman;F. Briggs;R. Cappallo;P. Carroll;A. D. Oliveira-Costa;J. Dillon;A. Ewall-Wice;L. Feng;L. Greenhill;B. Hazelton;J. Hewitt;N. Hurley-Walker;M. Johnston-Hollitt;D. Jacobs;D. Kaplan;Hs. Kim;E. Lenc;J. Line;A. Loeb;C. Lonsdale;M. Morales;E. Morgan;A. Neben;N. Thyagarajan;D. Oberoi;A. Offringa;S. Ord;S. Paul;J. Pober;T. Prabu;J. Riding;N. Shankar;S. Sethi;K. Srivani;R. Subrahmanyan;I. Sullivan;Max Tegmark;R. Webster;A. Williams;C. Williams;C. Wu;J. Wyithe
中科院分区：
其他
文献类型：
--
作者：
C. Trott;B. Pindor;P. Procopio;R. Wayth;D. Mitchell;B. McKinley;S. Tingay;N. Barry;A. Beardsley;G. Bernardi;J. Bowman;F. Briggs;R. Cappallo;P. Carroll;A. D. Oliveira-Costa;J. Dillon;A. Ewall-Wice;L. Feng;L. Greenhill;B. Hazelton;J. Hewitt;N. Hurley-Walker;M. Johnston-Hollitt;D. Jacobs;D. Kaplan;Hs. Kim;E. Lenc;J. Line;A. Loeb;C. Lonsdale;M. Morales;E. Morgan;A. Neben;N. Thyagarajan;D. Oberoi;A. Offringa;S. Ord;S. Paul;J. Pober;T. Prabu;J. Riding;N. Shankar;S. Sethi;K. Srivani;R. Subrahmanyan;I. Sullivan;Max Tegmark;R. Webster;A. Williams;C. Williams;C. Wu;J. Wyithe

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探测再电离时代（EoR）的宇宙学中性氢信号并估算其基本物理参数是当前许多低频射电望远镜的主要科学目标。在这里，我们描述的宇宙H i功率谱估计（CHIPS），一种算法开发和实施的数据从默奇森宽场阵列，计算的二维和球平均的亮度温度波动的功率谱。CHIPS的主要动机是应用现实的工具和前景模型来形成最佳估计，从而最大限度地提高无偏信号估计的可能性，并允许对输出进行全面的协变理解。CHIPS通过最大似然估计器采用数据的逆协方差加权，从而允许使用完整的参数空间进行信号估计（“前景抑制”）。我们描述的动机的算法，实施，应用到真实的和模拟数据，和早期的输出。在应用于一组3小时的数据时，我们在k = 0.05小时时对EoR无量纲功率设定2σ上限？在红移范围z = [6.2-6.6]内Δ k 2 mK2的Mpc−1，与之前的估计一致。
Detection of the cosmological neutral hydrogen signal from the Epoch of Reionization (EoR) and estimation of its basic physical parameters are principal scientific aims of many current low-frequency radio telescopes. Here we describe the Cosmological H i Power Spectrum Estimator (CHIPS), an algorithm developed and implemented with data from the Murchison Widefield Array, to compute the two-dimensional and spherically-averaged power spectrum of brightness temperature fluctuations. The principal motivations for CHIPS are the application of realistic instrumental and foreground models to form the optimal estimator, thereby maximizing the likelihood of unbiased signal estimation, and allowing a full covariant understanding of the outputs. CHIPS employs an inverse-covariance weighting of the data through the maximum likelihood estimator, thereby allowing use of the full parameter space for signal estimation (“foreground suppression”). We describe the motivation for the algorithm, implementation, application to real and simulated data, and early outputs. Upon application to a set of 3 hr of data, we set a 2σ upper limit on the EoR dimensionless power at k = 0.05 h ?> Mpc−1 of Δ k 2 mK2 in the redshift range z = [6.2–6.6], consistent with previous estimates.