Literature DB >> 16907428

New cosmic microwave background constraint to primordial gravitational waves.

Tristan L Smith1, Elena Pierpaoli, Marc Kamionkowski.   

Abstract

Primordial gravitational waves (GWs) with frequencies > or approximately equal to 10(-15) Hz contribute to the radiation density of the Universe at the time of decoupling of the cosmic microwave background (CMB). This affects the CMB and matter power spectra in a manner identical to massless neutrinos, unless the initial density perturbation for the GWs is nonadiabatic, as may occur if such GWs are produced during inflation or some post-inflation phase transition. In either case, current observations provide a constraint to the GW amplitude that competes with that from big-bang nucleosynthesis (BBN), although it extends to much lower frequencies (approximately 10(-15) Hz rather than the approximately 10(-10) Hz from BBN): at 95% confidence level, omega(gw)h(2) <or approximately = 8.4 x 10(-6) for homogeneous (i.e., nonadiabatic) initial conditions. Future CMB experiments, like Planck and CMBPol, should allow sensitivities to omega(gw)h(2) <or approximately = 1.4 x 10(-6) and omega(gw)h(2) < or approximately 5 x 10(-7), respectively.

Entities:  

Year:  2006        PMID： 16907428     DOI： 10.1103/PhysRevLett.97.021301

Source DB:  PubMed          Journal:  Phys Rev Lett        ISSN： 0031-9007            Impact factor:   9.161


  2 in total

1.  An upper limit on the stochastic gravitational-wave background of cosmological origin.

Authors:  B P Abbott; R Abbott; F Acernese; R Adhikari; P Ajith; B Allen; G Allen; M Alshourbagy; R S Amin; S B Anderson; W G Anderson; F Antonucci; S Aoudia; M A Arain; M Araya; H Armandula; P Armor; K G Arun; Y Aso; S Aston; P Astone; P Aufmuth; C Aulbert; S Babak; P Baker; G Ballardin; S Ballmer; C Barker; D Barker; F Barone; B Barr; P Barriga; L Barsotti; M Barsuglia; M A Barton; I Bartos; R Bassiri; M Bastarrika; Th S Bauer; B Behnke; M Beker; M Benacquista; J Betzwieser; P T Beyersdorf; S Bigotta; I A Bilenko; G Billingsley; S Birindelli; R Biswas; M A Bizouard; E Black; J K Blackburn; L Blackburn; D Blair; B Bland; C Boccara; T P Bodiya; L Bogue; F Bondu; L Bonelli; R Bork; V Boschi; S Bose; L Bosi; S Braccini; C Bradaschia; P R Brady; V B Braginsky; J F J van den Brand; J E Brau; D O Bridges; A Brillet; M Brinkmann; V Brisson; C Van Den Broeck; A F Brooks; D A Brown; A Brummit; G Brunet; A Bullington; H J Bulten; A Buonanno; O Burmeister; D Buskulic; R L Byer; L Cadonati; G Cagnoli; 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R Weiss; L Wen; S Wen; K Wette; J T Whelan; S E Whitcomb; B F Whiting; C Wilkinson; P A Willems; H R Williams; L Williams; B Willke; I Wilmut; L Winkelmann; W Winkler; C C Wipf; A G Wiseman; G Woan; R Wooley; J Worden; W Wu; I Yakushin; H Yamamoto; Z Yan; S Yoshida; M Yvert; M Zanolin; J Zhang; L Zhang; C Zhao; N Zotov; M E Zucker; J Zweizig
Journal:  Nature       Date:  2009-08-20       Impact factor: 49.962

2.  Astrophysics: Gravity ripples chased.

Authors:  Marc Kamionkowski
Journal:  Nature       Date:  2009-08-20       Impact factor: 49.962
  2 in total

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