Finite Bubble Statistics Constrain Late Cosmological Phase Transitions

被引:4
作者
Elor, Gilly [1 ]
Jinno, Ryusuke [2 ,3 ]
Kumar, Soubhik [4 ,5 ,6 ]
Mcgehee, Robert [7 ,8 ]
Tsai, Yuhsin [9 ]
机构
[1] Univ Texas Austin, Weinberg Inst, Dept Phys, Austin, TX 78712 USA
[2] Univ Tokyo, Res Ctr Early Universe RESCEU, Grad Sch Sci, Tokyo 1130033, Japan
[3] Kobe Univ, Grad Sch Sci, Dept Phys, 1-1 Rokkodai, Kobe, Hyogo 6578501, Japan
[4] NYU, Ctr Cosmol & Particle Phys, Dept Phys, New York, NY 10003 USA
[5] Univ Calif Berkeley, Berkeley Ctr Theoret Phys, Dept Phys, Berkeley, CA 94720 USA
[6] Lawrence Berkeley Natl Lab, Theoret Phys Grp, Berkeley, CA 94720 USA
[7] Univ Minnesota, William I Fine Theoret Phys Inst, Sch Phys & Astron, Minneapolis, MN 55455 USA
[8] Univ Michigan, Leinweber Ctr Theoret Phys, Dept Phys, Ann Arbor, MI 48109 USA
[9] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA
关键词
MICROWAVE BACKGROUND SPECTRUM; GRAVITATIONAL-RADIATION; PERTURBATIONS; NUCLEATION; WAVES;
D O I
10.1103/PhysRevLett.133.211003
中图分类号
O4 [物理学];
学科分类号
0702 ;
摘要
We consider first order cosmological phase transitions (PTs) happening at late times below standard model temperatures T PT GeV. The inherently stochastic nature of bubble nucleation and the finite number of bubbles associated with a late-time PT lead to superhorizon fluctuations in the PT completion time. We compute how such fluctuations eventually source curvature fluctuations with universal properties, independent of the microphysics of the PT dynamics. Using cosmic microwave background (CMB) and large scale structure measurements, we constrain the energy released in a dark-sector PT. For 0.1 eV T PT keV this constraint is stronger than both the current bound from additional neutrino species Delta N eff , and in some cases, even CMB-S4 projections. Future measurements of CMB spectral distortions and pulsar timing arrays will also provide competitive sensitivity for keV T PT GeV.
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页数:7
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