Composite Dark Matter George T. Fleming Yale University E. Rinaldi LLNL Sakata-Hirata Hall, Nagoya University March 4, 2015 Lattice Strong Dynamics Collaboration Xiao-Yong Jin [LSD collab., Phys. Rev. D88 (2013) 014502] [LSD collab., Phys. Rev. D89 (2014) 094508] + LSD collab., in preparation (x2) Outline • Motivations for searches of composite dark matter • Features of strongly-coupled composite dark matter • Searches for a class of models interesting for phenomenology • Importance of lattice field theory simulations • Lower bounds on composite dark matter models BSM Is Out There • Discovery of SM-like Higgs boson doesn’t mean BSM physics is dead: ➡ What is the meaning of the hierarchy problem and naturalness? ➡ What solves the strong CP problem? ➡ What explains the matter-antimatter asymmetry? BSM Is Out There • Discovery of SM-like Higgs boson doesn’t mean BSM physics is dead: ➡ What is the meaning of the hierarchy problem and naturalness? ➡ What solves the strong CP problem? ➡ What explains the matter-antimatter asymmetry? ➡ What is dark matter? Can it couple to the standard model? Is the mass scale related to the EW Higgs mechanism? Is it self-interacting? The gravity of Dark Matter ?????? New We Are Here Physics!! (QCD, EM, SM, etc.) How do we know Dark Matter is there? Rotational velocity Curves of Galaxies Gravitational Lensing Cosmological Backgrounds The gravity of Dark Matter ?????? New We Are Here Physics!! (QCD, EM, SM, etc.) [Planck and ESA] How do we know Dark Matter is there? Rotational velocity Curves of Galaxies Gravitational Lensing Cosmological Backgrounds The gravity of Dark Matter ?????? New We Are Here Physics!! (QCD, EM, SM, etc.) [Planck and ESA] How do we know Dark Matter is there? Rotational velocity Curves of Galaxies Gravitational Lensing Gravitational Interactions Cosmological Backgrounds Problems? Problems? • Number of observed dwarf galaxies is inconsistent with predictions from dark matter simulations “Missing Satellites” Problems? • Number of observed dwarf galaxies is inconsistent with predictions from dark matter simulations “Missing Satellites” • Predicted dwarf galaxies are too dense “Too Big To Fail” Problems? • Number of observed dwarf galaxies is inconsistent with predictions from dark matter simulations “Missing Satellites” • Predicted dwarf galaxies are too dense “Too Big To Fail” • Density profiles of dwarf galaxies is more cored than in simulations “Cusp vs. Core” Problems? • Number of observed dwarf galaxies is inconsistent with predictions from dark matter simulations “Missing Satellites” • Predicted dwarf galaxies are too dense “Too Big To Fail” • Density profiles of dwarf galaxies is more cored than in simulations “Cusp vs. Core” ameliorated by Self-Interacting Dark Matter Self-Interacting Dark Matter • In ΛCDM, galactic sub-halos have very dense, cuspy cores. • Any dwarf galaxies residing in a cuspy sub-halo will be smaller and dimmer than in a sub-halo with more uniform density. • Larger Milky Way and Andromeda dwarf galaxies are too bright for their expected sub-halos, if those sub-halos are made of non-interacting dark matter (ΛCDM). Self-interacting dark matter (SIDM) will make sub-halo cores less dense, enabling larger dwarf galaxies. 2 1 1 σ(v )/M 0.5 – 50 cm g− ,v 10 – 100 km s− rms ⇠ rms ' O. D. Elbert et al., arXiv:1412.1477 [astro-ph.GA] Self-Interacting Dark Matter Strongly-Coupled Composite Dark Matter interactions with SM particles that can evade current experimental constraints View from Snowmass (I) R-parity NMSSM MSSM violating WIMPless DM Supersymmetry Hidden Sector DM Gravitino DM mSUGRA Self-Interacting DM pMSSM Q-balls Techni- baryons Dark Photon R-parity Conserving Dirac Asymmetric DM DM Light Extra Dimensions Dynamical Force Carriers DM Warm DM Solitonic DM UED DM Sterile Neutrinos Quark 6d Warped Extra Nuggets Dimensions 5d RS DM T-odd DM Axion DM ? Little Higgs QCD Axions Axion-like Particles T Tait Littlest Higgs Snowmass 2013: The Cosmic Frontier [arXiv:1401.6085] Where is composite dark matter? View from Snowmass (I) R-parity NMSSM MSSM violating WIMPless DM Supersymmetry Hidden Sector DM Gravitino DM mSUGRA Self-Interacting DM pMSSM Q-balls Techni- baryons Dark Photon R-parity Conserving Dirac Asymmetric DM DM Light Extra Dimensions Dynamical Force Carriers DM Warm DM Solitonic DM UED DM Sterile Neutrinos Quark 6d Warped Extra Nuggets Dimensions 5d RS DM T-odd DM Axion DM ? Little Higgs QCD Axions Axion-like Particles T Tait Littlest Higgs Snowmass 2013: The Cosmic Frontier [arXiv:1401.6085] Where is composite dark matter? View from Snowmass (II) SuperCDMS Soudan CDMS-lite SuperCDMS Soudan Low Threshold XENON 10 S2 (2013) 10!39 CDMS-II Ge Low Threshold (2011) 10!3 CoGeNT PICO250-C3F8 !40 (2012) !4 10 CDMS Si 10 (2013) # ! ! 41 5 # 2 10 DAMA SIMPLE (2012) 10 COUPP (2012) pb cm ! ! !42 CRESST !6 10 ZEPLIN-III (2012) 10 SuperCDMS !43 CDMS II Ge (2009) !7 10 EDELWEISS (2011) 10 SNOLAB SuperCDMS Soudan section section N EU TR Xenon100 (2012) !44 IN DarkSide 50 !8 10 O 10 7Be C TT LUX OHE SCA ER cross cross R NT I Neutrinos E 8 N !45 B G PICO250-CF3I !9 10 Neutrinos 10 Xenon1T !46 DEAP3600 !10 10 DarkSide G2 10 LZ nucleon nucleon ! ! !47 !11 10 (Green&ovals)&Asymmetric&DM&& 10 (Violet&oval)&Magne7c&DM& RING ATTE !48 (Blue&oval)&Extra&dimensions&& NT SC !12 E WIMP HER WIMP 10 10 (Red&circle)&SUSY&MSSM& CO RINO &&&&&MSSM:&Pure&Higgsino&& NEUT !49 !13 10 &&&&&MSSM:&A&funnel& Atmospheric and DSNB Neutrinos 10 &&&&&MSSM:&BinoEstop&coannihila7on& !50 &&&&&MSSM:&BinoEsquark&coannihila7on& !14 10 & 10 1 10 100 1000 104 WIMP Mass GeV c2 Snowmass 2013: The Cosmic Frontier [arXiv:1401.6085] ! " # Partial wave unitarity? Where is composite dark matter? View from Snowmass (II) SuperCDMS Soudan CDMS-lite SuperCDMS Soudan Low Threshold XENON 10 S2 (2013) 10!39 CDMS-II Ge Low Threshold (2011) 10!3 CoGeNT PICO250-C3F8 !40 (2012) !4 10 CDMS Si 10 (2013) # ! ! 41 5 # 2 10 DAMA SIMPLE (2012) 10 COUPP (2012) pb cm ! ! !42 CRESST !6 10 ZEPLIN-III (2012) 10 SuperCDMS !43 CDMS II Ge (2009) !7 10 EDELWEISS (2011) 10 SNOLAB SuperCDMS Soudan section section N EU TR Xenon100 (2012) !44 IN DarkSide 50 !8 10 O 10 7Be C TT LUX Dark SU(3) Baryon OHE SCA ER cross cross R NT I Neutrinos E 8 N !45 B G PICO250-CF3I !9 10 Neutrinos 10 Xenon1T !46 DEAP3600 !10 10 DarkSide G2 10 LZ nucleon nucleon ! ! !47 !11 10 (Green&ovals)&Asymmetric&DM&& 10 (Violet&oval)&Magne7c&DM& RING ATTE !48 (Blue&oval)&Extra&dimensions&& NT SC !12 E WIMP HER WIMP 10 10 (Red&circle)&SUSY&MSSM& CO RINO &&&&&MSSM:&Pure&Higgsino&& NEUT !49 !13 10 &&&&&MSSM:&A&funnel& Atmospheric and DSNB Neutrinos 10 &&&&&MSSM:&BinoEstop&coannihila7on& !50 &&&&&MSSM:&BinoEsquark&coannihila7on& !14 10 & 10 1 10 100 1000 104 WIMP Mass GeV c2 Snowmass 2013: The Cosmic Frontier [arXiv:1401.6085] ! " # Partial wave unitarity? Where is composite dark matter? Strongly-coupled composite dark matter • Dark matter is a composite object • Composite object is electroweak neutral • Constituents can have electroweak charges • Dark matter is stable thanks to a global symmetry (like baryon number) Strongly-coupled composite dark matter • Dark matter is a composite object Akin to a technibaryon • Composite object is electroweak neutral • Constituents can have electroweak charges • Dark matter is stable thanks to a global symmetry (like baryon number) Strongly-coupled composite dark matter • Dark matter is a composite object Akin to a technibaryon • Composite object is electroweak neutral Suppressed interactions with SM • Constituents can have electroweak charges • Dark matter is stable thanks to a global symmetry (like baryon number) Strongly-coupled composite dark matter • Dark matter is a composite object Akin to a technibaryon • Composite object is electroweak neutral Suppressed interactions with SM • Constituents can have electroweak charges Mechanisms to provide observed relic abundance • Dark matter is stable thanks to a global symmetry (like baryon number) Strongly-coupled composite dark matter • Dark matter is a composite object Akin to a technibaryon • Composite object is electroweak neutral Suppressed interactions with SM • Constituents can have electroweak charges Mechanisms to provide observed relic abundance • Dark matter is stable thanks to a global symmetry (like baryon number) Guaranteed in many models What do we have in mind? • In general we think about a new strongly-coupled gauge sector like QCD with a plethora of composite states in the spectrum • Dark fermions have dark color and also have electroweak charges • Depending on the model, dark fermions have electroweak breaking masses (chiral), electroweak preserving masses (vector) or a mixture • A global symmetry of the theory naturally stabilizes the dark baryonic composite states (e.g. neutron) What do we have in mind? • In general we think about a new strongly-coupled gauge sector like QCD with a plethora of composite states in the spectrum • Dark fermions have dark color and also have electroweak charges • Depending on the model, dark fermions have electroweak breaking masses (chiral), electroweak preserving masses (vector) or a mixture • A global symmetry of the theory naturally stabilizes the dark baryonic composite states (e.g. neutron) we construct a minimal model with these features “How dark is Dark Matter?” Interactions of neutral object with photons + Higgs • dimension 4 ➥ Higgs exchange µ⌫ (¯χσ χ)Fµ⌫ • ➥ dimension 5 magnetic dipole ⇤dark µ⌫ (¯χχ)vµ@⌫ F • dimension 6 ➥ charge radius 2 ⇤dark µ⌫ (¯χχ)Fµ⌫ F • dimension 7 ➥ polarizability 3 ⇤dark “How dark is Dark Matter?”