The Atacama Cosmology Telescope: reionization kSZ trispectrum methodology and limits

Author:

MacCrann Niall12,Qu Frank J12,Namikawa Toshiya3,Bolliet Boris24ORCID,Cai Hongbo5,Calabrese Erminia6,Choi Steve K7,Coulton William12ORCID,Darwish Omar8,Ferraro Simone9,Guan Yilun10,Hill J Colin11,Hilton Matt1213,Hložek Renée1415,Kramer Darby16,Madhavacheril Mathew S17,Moodley Kavilan1819,Sehgal Neelima20,Sherwin Blake D12,Sifón Cristóbal21,Staggs Suzanne T22,Trac Hy23,Van Engelen Alexander16,Vavagiakis Eve M24

Affiliation:

1. DAMTP, Centre for Mathematical Sciences, University of Cambridge , Wilberforce Road, Cambridge CB3 OWA , UK

2. Kavli Institute for Cosmology, University of Cambridge , Madingley Road, Cambridge CB3 0HA , UK

3. Center for Data-Driven Discovery , Kavli IPMU (WPI), UTIAS, The University of Tokyo, Kashiwa, 277-8583 , Japan

4. Astrophysics Group, Cavendish Laboratory , J. J. Thomson Avenue, Cambridge CB3 0HE , UK

5. Department of Physics and Astronomy, University of Pittsburgh , Pittsburgh, PA 15260 USA

6. School of Physics and Astronomy, Cardiff University , The Parade, Cardiff, Wales CF24 3AA , UK

7. Department of Physics and Astronomy, University of California , Riverside, CA 92521 , USA

8. D’epartement de Physique Th’eorique et CAP, Universit’e de Genève, , 24 Quai Ansermet, CH-1211 Genève 4 , Switzerland

9. Lawrence Berkeley National Laboratory , One Cyclotron Road, Berkeley, CA 94720 , USA

10. Dunlap Institute for Astronomy and Astrophysics, University of Toronto , Toronto, ON M5S 3H4 , Canada

11. Department of Physics, Columbia University , New York, NY 10027 , USA

12. Wits Centre for Astrophysics, School of Physics, University of the Witwatersrand , Private Bag 3, Johannesburg 2050 , South Africa

13. Astrophysics Research Centre, School of Mathematics, Statistics, and Computer Science, University of KwaZulu-Natal , Westville Campus, Durban 4041 , South Africa

14. Dunlap Institute of Astronomy & Astrophysics , 50 St. George St., Toronto, ON M5S 3H4 , Canada

15. David A. Dunlap Department of Astronomy & Astrophysics, University of Toronto , 50 St. George St., Toronto, ON M5S 3H4 , Canada

16. School of Earth and Space Exploration, Arizona State University , Tempe, AZ 85287 , USA

17. Department of Physics and Astronomy, University of Pennsylvania , 209 South 33rd Street, Philadelphia, PA 19104 , USA

18. A. Astrophysics Research Centre, University of KwaZulu-Natal , Westville Campus, Durban 4041 , South Africa

19. B. School of Mathematics, Statistics & Computer Science, University of KwaZulu-Natal , Westville Campus, Durban 4041 , South Africa

20. Physics and Astronomy Department, Stony Brook University , Stony Brook, NY 11794 , USA

21. Instituto de Física, Pontificia Universidad Católica de Valparaíso , Casilla 4059, Valparaíso , Chile

22. Joseph Henry Laboratories of Physics, Jadwin Hall, Princeton University, , Princeton, NJ 08544 , USA

23. McWilliams Center for Cosmology and Astrophysics, Department of Physics, Carnegie Mellon University , Pittsburgh, PA 15213 , USA

24. Department of Physics, Cornell University , Ithaca, NY 14853 , USA

Abstract

ABSTRACT Patchy reionization generates kinematic Sunyaev–Zel’dovich (kSZ) anisotropies in the cosmic microwave background (CMB). Large-scale velocity perturbations along the line of sight modulate the small-scale kSZ power spectrum, leading to a trispectrum (or four-point function) in the CMB that depends on the physics of reionization. We investigate the challenges in detecting this trispectrum and use tools developed for CMB lensing, such as realization-dependent bias subtraction and cross-correlation based estimators, to counter uncertainties in the instrumental noise and assumed CMB power spectrum. We also find that both lensing and extragalactic foregrounds can impart larger trispectrum contributions than the reionization kSZ signal. We present a range of mitigation methods for both of these sources of contamination, validated on microwave-sky simulations. We use ACT DR6 and Planck data to calculate an upper limit on the reionization kSZ trispectrum from a measurement dominated by foregrounds. The upper limit is about 50 times the signal predicted from recent simulations.

Funder

National Science Foundation

Princeton University

University of Pennsylvania

Canada Foundation for Innovation

NASA

CFI

Government of Ontario

University of Toronto

European Research Council

SNSF

NSF

DOE

Simons Foundation

CIFAR

Royal Society

Publisher

Oxford University Press (OUP)

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