Strong gravitational radiation from a simple dark matter model - PowerPoint PPT Presentation

Strong gravitational radiation from a simple dark matter model Camilo Garcia Cely, DESY Bogot´ a-Colombia CoCo (Cosmolog´ ıa en Colombia) 31 May, 2019 In collaboration with Iason Baldes Based on JHEP 1905 (2019) 190

Introduction GWs from symmetry breaking at tree level GWs from radiatively-induced symmetry breaking Gravitational Waves (GWs) Predicted by Poincar´ e (1905). This talk Camilo Garcia Cely, DESY GWs from dark matter

Introduction GWs from symmetry breaking at tree level GWs from radiatively-induced symmetry breaking Gravitational Waves (GWs) Predicted by Poincar´ e (1905). Einstein provided a firm theoretical ground for them (1916). � h µν = − 16 π GT µν This talk Camilo Garcia Cely, DESY GWs from dark matter

Introduction GWs from symmetry breaking at tree level GWs from radiatively-induced symmetry breaking Gravitational Waves (GWs) Predicted by Poincar´ e (1905). Einstein provided a firm theoretical ground for them (1916). � h µν = − 16 π GT µν First-order phase transitions in the Early Universe produce GWs. Witten (1984). This talk Camilo Garcia Cely, DESY GWs from dark matter

Introduction GWs from symmetry breaking at tree level GWs from radiatively-induced symmetry breaking Gravitational Waves (GWs) Predicted by Poincar´ e (1905). Einstein provided a firm theoretical ground for them (1916). � h µν = − 16 π GT µν First-order phase transitions in the Early Universe produce GWs. Witten (1984). This talk Hypothesis: Dark matter are massive gauge bosons. → There was a phase transition in the Early Universe: GWs. Camilo Garcia Cely, DESY GWs from dark matter

Introduction GWs from symmetry breaking at tree level GWs from radiatively-induced symmetry breaking First-order phase transition At low T: Symmetry breaking Massive DM Camilo Garcia Cely, DESY GWs from dark matter

Introduction GWs from symmetry breaking at tree level GWs from radiatively-induced symmetry breaking First-order phase transition At high T: Symmetry restoration Kirzhnits and Linde (1972) Camilo Garcia Cely, DESY GWs from dark matter

Introduction GWs from symmetry breaking at tree level GWs from radiatively-induced symmetry breaking First-order phase transition Camilo Garcia Cely, DESY GWs from dark matter

Introduction GWs from symmetry breaking at tree level GWs from radiatively-induced symmetry breaking First-order phase transition At T = T c Camilo Garcia Cely, DESY GWs from dark matter

Introduction GWs from symmetry breaking at tree level GWs from radiatively-induced symmetry breaking First-order phase transition Camilo Garcia Cely, DESY GWs from dark matter

Introduction GWs from symmetry breaking at tree level GWs from radiatively-induced symmetry breaking First-order phase transition At T = T n nucleation Camilo Garcia Cely, DESY GWs from dark matter

Introduction GWs from symmetry breaking at tree level GWs from radiatively-induced symmetry breaking First-order phase transition At T = T n nucleation This produces produces gravitational waves E. Witten (1984) Camilo Garcia Cely, DESY GWs from dark matter

Introduction GWs from symmetry breaking at tree level GWs from radiatively-induced symmetry breaking First-order phase transition At low T: Massive DM GWs redshift. Camilo Garcia Cely, DESY GWs from dark matter

Introduction GWs from symmetry breaking at tree level GWs from radiatively-induced symmetry breaking First-order phase transition m DM ∼ 1 TeV → f ∼ 10 − 2 Hz At low T: Massive DM GWs redshift. Camilo Garcia Cely, DESY GWs from dark matter

Introduction GWs from symmetry breaking at tree level GWs from radiatively-induced symmetry breaking First-order phase transition Laser Interferometer Space Antenna m DM ∼ 1 TeV → f ∼ 10 − 2 Hz At low T: Massive DM GWs redshift. Caprini et al (2015) Camilo Garcia Cely, DESY GWs from dark matter

Introduction GWs from symmetry breaking at tree level GWs from radiatively-induced symmetry breaking Focus on a scenario based on a SU (2) D group Field SU (3) SU (2) U (1) Y SU (2) D 1 H 1 2 1 2 1 1 0 2 H D V = µ 2 1 H † H + µ 2 2 H † D H D + λ 1 ( H † H ) 2 + λ 2 ( H † D H D ) 2 + λ 3 H † D H D H † H , Local SU (2) D Global SO (3) → Gauge Fields A ′ Massive Fields A µ → µ Dark doublet H D Higgs-like h D → Hambye (JHEP 2009) Camilo Garcia Cely, DESY GWs from dark matter

Introduction GWs from symmetry breaking at tree level GWs from radiatively-induced symmetry breaking Focus on a scenario based on a SU (2) D group Field SU (3) SU (2) U (1) Y SU (2) D 1 H 1 2 1 2 1 1 0 2 H D V = µ 2 1 H † H + µ 2 2 H † D H D + λ 1 ( H † H ) 2 + λ 2 ( H † D H D ) 2 + λ 3 H † D H D H † H , Local SU (2) D Global SO (3) → Gauge Fields A ′ Massive Fields A µ Stable (DM Candidate) → µ Dark doublet H D Higgs-like h D → Hambye (JHEP 2009) Camilo Garcia Cely, DESY GWs from dark matter

Introduction GWs from symmetry breaking at tree level GWs from radiatively-induced symmetry breaking Focus on a scenario based on a SU (2) D group Field SU (3) SU (2) U (1) Y SU (2) D 1 H 1 2 1 2 1 1 0 2 H D V = µ 2 1 H † H + µ 2 2 H † D H D + λ 1 ( H † H ) 2 + λ 2 ( H † D H D ) 2 + λ 3 H † D H D H † H , Local SU (2) D Global SO (3) → Gauge Fields A ′ Massive Fields A µ Stable (DM Candidate) → µ Dark doublet H D Higgs-like h D It mixes with the Higgs → Hambye (JHEP 2009) Camilo Garcia Cely, DESY GWs from dark matter

Introduction GWs from symmetry breaking at tree level GWs from radiatively-induced symmetry breaking Focus on a scenario based on a SU (2) D group Field SU (3) SU (2) U (1) Y SU (2) D 1 H 1 2 1 2 1 1 0 2 H D V = µ 2 1 H † H + µ 2 2 H † D H D + λ 1 ( H † H ) 2 + λ 2 ( H † D H D ) 2 + λ 3 H † D H D H † H , Local SU (2) D Global SO (3) → Gauge Fields A ′ Massive Fields A µ Stable (DM Candidate) → µ Dark doublet H D Higgs-like h D It mixes with the Higgs → High temperatures Low temperatures Hambye (JHEP 2009) Phase transition in the Early Universe!!!!!!!!!!! Camilo Garcia Cely, DESY GWs from dark matter

Introduction GWs from symmetry breaking at tree level GWs from radiatively-induced symmetry breaking Four parameters DM mass Higgs-like mass mixing angle. Direct detection in Xenon1T: θ � 0 . 1. vev (or g D ) are set by the relic density (via freeze-out): � g D ≈ 0 . 9 × m A � 1 TeV m A � v η ≈ 2 . 2 TeV × 1 TeV . A h D A h D A A A A A h D A h D A h D A h D Camilo Garcia Cely, DESY GWs from dark matter

Introduction GWs from symmetry breaking at tree level GWs from radiatively-induced symmetry breaking GW spectrum Phase transition parameters T n = 0 . 48 TeV η n = 3 . 8 TeV α = 0 . 29 , ∼ (latent heat) β/ H = 290 ∼ (fq. scale) Simulations give Ω GW from them Caprini et al (2015) SNR SNR FGL LISA 15 1 . 8 Baldes, CGC 2018 3 . 7 × 10 5 2 . 3 × 10 3 BBO Camilo Garcia Cely, DESY GWs from dark matter

Introduction GWs from symmetry breaking at tree level GWs from radiatively-induced symmetry breaking Parameter space for SNR > 5. � � 2 � � h 2 Ω GW ( f ) SNR = t obs df h 2 Ω sens ( f ) Baldes, CGC 2018 Camilo Garcia Cely, DESY GWs from dark matter

Introduction GWs from symmetry breaking at tree level GWs from radiatively-induced symmetry breaking Dark matter as massive dark gauge bosons Field SU (3) SU (2) U (1) Y SU (2) D 1 1 2 1 H 2 H D 1 1 0 2 V = µ 2 1 H † H + µ 2 2 H † D H D + λ 1 ( H † H ) 2 + λ 2 ( H † D H D ) 2 + λ 3 H † D H D H † H , Local SU (2) D Global SO (3) → Gauge Fields A ′ Massive Fields A µ → µ Dark doublet H D Higgs-like h D → Camilo Garcia Cely, DESY GWs from dark matter

Introduction GWs from symmetry breaking at tree level GWs from radiatively-induced symmetry breaking Dark matter as massive dark gauge bosons Field SU (3) SU (2) U (1) Y SU (2) D 1 1 2 1 H 2 H D 1 1 0 2 Set them to zero (Classically scale invariant potential) Hambye,Strumia,Teresi (2013,2018) V = µ 2 1 H † H + µ 2 2 H † D H D + λ 1 ( H † H ) 2 + λ 2 ( H † D H D ) 2 + λ 3 H † D H D H † H , Local SU (2) D Global SO (3) → Gauge Fields A ′ Massive Fields A µ → µ Dark doublet H D Higgs-like h D → Camilo Garcia Cely, DESY GWs from dark matter

Introduction GWs from symmetry breaking at tree level GWs from radiatively-induced symmetry breaking Dark matter as massive dark gauge bosons Field SU (3) SU (2) U (1) Y SU (2) D 1 1 2 1 H 2 H D 1 1 0 2 Set them to zero (Classically scale invariant potential) Hambye,Strumia,Teresi (2013,2018) V = µ 2 1 H † H + µ 2 2 H † D H D + λ 1 ( H † H ) 2 + λ 2 ( H † D H D ) 2 + λ 3 H † D H D H † H , Local SU (2) D Global SO (3) → Gauge Fields A ′ Massive Fields A µ → µ Dark doublet H D Higgs-like h D → Radiative effects break the SU (2) D symmetry Coleman-Weinberg (1973) λ 2 runs to negative values. Camilo Garcia Cely, DESY GWs from dark matter

Introduction GWs from symmetry breaking at tree level GWs from radiatively-induced symmetry breaking Baldes, CGC 2018 Only one free parameter after taking the relic density into account. Scale-invariant potential → strong signal. Camilo Garcia Cely, DESY GWs from dark matter