Multiple methods for estimating the bispectrum of the cosmic microwave background with application to the MAXIMA data

被引：45

作者：

Santos, MG ^{[1
]}

Heavens, A

Balbi, A

Borrill, J

Ferreira, PG

Hanany, S

Jaffe, AH

Lee, AT

Rabii, B

Richards, PL

Smoot, GF

Stompor, R

Winant, CD

Wu, JHP

机构：

[1] Univ Oxford, Oxford OX1 3RH, England

[2] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA

[3] Univ Edinburgh, Astron Inst, Edinburgh EH9 3HJ, Midlothian, Scotland

[4] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy

[5] Univ Calif Berkeley, Ctr Particle Astrophys, Berkeley, CA 94720 USA

[6] Lawrence Berkeley Natl Lab, Natl Energy Res Sci Comp Ctr, Berkeley, CA 94720 USA

[7] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA

[8] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA

[9] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2BW, England

[10] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA

[11] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA

[12] Natl Taiwan Univ, Dept Phys, Taipei 106, Taiwan

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2003年 / 341卷 / 02期

基金：

美国国家科学基金会;

关键词：

methods : data analysis; methods : statistical; cosmic microwave background; early Universe;

D O I：

10.1046/j.1365-8711.2003.06438.x

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We describe different methods for estimating the bispectrum of cosmic microwave background data. In particular, we construct a minimum-variance estimator for the flat-sky limit and compare results with previously studied frequentist methods. Application to the MAXIMA data set shows consistency with primordial Gaussianity. Weak quadratic non-Gaussianity is characterized by a tunable parameter f (NL) , corresponding to non-Gaussianity at a level of similar to10(-5) f (NL) (the ratio of non-Gaussian to Gaussian terms), and we find limits of f (NL) = 1500 +/- 950 for the minimum-variance estimator and f (NL) = 2700 +/- 1650 for the usual frequentist estimator. These are the tightest limits on primordial non-Gaussianity, which include the full effects of the radiation transfer function.

引用

页码：623 / 643

页数：21

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