Non-Gaussianity of secondary anisotropies from ACTPol and Planck

被引:22
作者
Coulton, William R. [1 ]
Aiola, Simone [1 ]
Battaglia, Nicholas [2 ,3 ]
Calabrese, Erminia [4 ]
Choi, Steve K. [1 ]
Devlin, Mark J. [5 ]
Gallardo, Patricio A. [6 ]
Hill, J. Colin [3 ,7 ]
Hincks, Adam D. [8 ,9 ]
Hubmayr, Johannes [10 ]
Hughes, John P. [11 ]
Kosowsky, Arthur [12 ,13 ]
Louis, Thibaut [14 ]
Madhavacheril, Mathew S.
Maurin, Loic [15 ,16 ]
Naess, Sigurd [5 ]
Nati, Federico [5 ]
Niemack, Michael D. [6 ]
Page, Lyman A. [1 ]
Partridge, Bruce [17 ]
Sherwin, Blake D. [18 ,19 ]
Spergel, David N. [2 ,3 ]
Staggs, Suzanne T. [1 ]
Van Engelen, Alexander [20 ]
Wollack, Edward J. [21 ]
机构
[1] Princeton Univ, Joseph Henry Labs, Princeton, NJ 08544 USA
[2] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA
[3] Flatiron Inst, Ctr Computat Astrophys, 162 5th Ave, New York, NY 10010 USA
[4] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales
[5] Univ Penn, Dept Phys & Astron, 209 South 33rd St, Philadelphia, PA 19104 USA
[6] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA
[7] Inst Adv Study, Sch Nat Sci, Olden Lane, Princeton, NJ 08540 USA
[8] Univ Roma La Sapienza, Dept Phys, Piazzale Aldo Moro 5, I-00185 Rome, Italy
[9] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada
[10] NIST Quantum Devices Grp, 325 Broadway,Mailcode 817-03, Boulder, CO 80305 USA
[11] State Univ New Jersey, Rutgers, Dept Phys & Astron, Piscataway, NJ 08854 USA
[12] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA
[13] Univ Pittsburgh, Pittsburgh Particle Phys Astrophys & Cosmol Ctr, Pittsburgh, PA 15260 USA
[14] Univ Paris Sud, Univ Paris Saclay, CNRS IN2P3, Lab Accelerateur Lineaire, Orsay, France
[15] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago, Chile
[16] Pontificia Univ Catolica Chile, Fac Fis, Ctr Astroingn, Av Vicuna Mackenna 4860, Santiago 7820436, Chile
[17] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA
[18] Univ Cambridge, Dept Appl Math & Theoret Phys, Wilberforce Rd, Cambridge CB3 0WA, England
[19] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA
[20] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada
[21] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA
基金
加拿大创新基金会; 美国国家科学基金会;
关键词
non-gaussianity; Sunyaev-Zeldovich effect; INFRARED BACKGROUND ANISOTROPIES; HALO OCCUPATION DISTRIBUTION; 3-POINT CORRELATION-FUNCTION; PRIMORDIAL NON-GAUSSIANITY; ANGULAR POWER SPECTRUM; RADIO GALAXIES; FLUCTUATIONS; PROBE; TEMPERATURE; PREDICTIONS;
D O I
10.1088/1475-7516/2018/09/022
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Most secondary sources of cosmic microwave background anisotropy (radio sources, dusty galaxies, thermal Sunyaev Zel'dovich distortions from hot gas, and gravitational lensing) are highly non-Gaussian. Statistics beyond the power spectrum are therefore potentially important sources of information about the physics of these processes. We combine data from the Atacama Cosmology Telescope and with data from the Planck satellite (only using Planck data in the overlapping region) to constrain the amplitudes of a set of theoretical bispectrum templates from the thermal Sunyaev-Zeldovich (tSZ) effect, dusty star-forming galaxies (DSFGs), gravitational lensing, and radio galaxies. We make a strong detection of radio galaxies (> 5 sigma) and have hints of non-Gaussianity arising from the tSZ effect, DSFGs, from cross-correlations between the tSZ effect and DSFGs and from cross-correlations among the tSZ effect, DSFGs and radio galaxies. These results suggest that the same halos host radio sources, DSFGs, and have tSZ signal. We present a new method to calculate the non-Gaussian contributions to the template covariances. Using this method we find significant non-Gaussian contributions to the variance and covariance of our templates, with templates involving the tSZ effect most effected. Strong degeneracies exist between the various sources at the current noise levels. In light of these degeneracies, combined with theoretical uncertainty in the templates, these results are a demonstration of this technique. With these caveats, we demonstrate the utility of future bispectrum measurements by using the tSZ bispectrum measurement to constrain a combination of the amplitude of matter fluctuations and the matter density to be sigma(8)Omega(0.17)(m) = 0.65(-0.06)(+0.05). Improvements in signal to noise from upcoming Advanced ACT, SPT-3G, Simons Observatory, and CMB-S4 observations will enable the separation of bispectrum components and robust constraints on cosmological parameters.
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