Deviant Dark Matter: Indirect Indicators of and Constraints on the Nature of Dark Matter. Kevork Abazajian University of California, Irvine

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1 Deviant Dark Matter: Indirect Indicators of and Constraints on the Nature of Dark Matter Kevork Abazajian University of California, Irvine SCIPP Seminar March 6, 2012

2 Dark Matter Today Cosmic Microwave Background: WMAP, ACBAR, CBI, Boomerang Large Scale Structure: SDSS, 2dFGRS Ω DM =0.227 ± WMAP7 + SDSS BAO + H 0 (Komatsu et al. 2010)

3 The Cosmic Microwave Background: WMAP, Planck and the Future of LSS

4 Cosmic Microwave Background: Precision Cosmology WMAP 7

5 Cosmic Microwave Background: Precision Cosmology WMAP 7 P(k) k

6 Forecast Precision Cosmology: PLANCK (Martin White)

7 P(k) k The Primordial Spectrum: Precision Determination at Large Scales P (k) =Ak n WMAP 5 + BAO + SN: (Komatsu et al. 2008) A = ± (3.4%) n = 0.96 ± (1.4%) PLANCK + SDSS LRG: (Eisenstein, Hu, Tegmark 1998) A = ± (0.35%) n = ± (0.8%) forecast!

8 P(k) Large Scale Structure and P(k) k Tegmark & Zaldarriaga 2002

9 How far into the small-scale regime can we measure?

10 How far into the small-scale regime can we measure? The nature of dark matter...

11 How far into the small-scale regime can we measure?

12 How far into the small-scale regime can we measure? WIMP CDM k c ~ 10 6 h /Mpc (Zaldarriaga & Loeb 2006)

1999) Halo Cores and Densities: (Gilmore et al 2006; Kuzio de Naray 2008) Void Galaxy

13 Problems in Cold Dark Matter? Halo Substructure: satellite galaxies and sub-halos (Klypin et al 1999; Moore et al 1999) Halo Cores and Densities: (Gilmore et al 2006; Kuzio de Naray 2008) Void Galaxy abundances (Peebles 2001) Angular Momentum Problem (Navarro & Benz 1991; Sommer-Larsen & Dolgov 2001) Disk Dominated Galaxy Formation (Governato et al 2002)

14 Problems in Cold Dark Matter? Halo Substructure: satellite galaxies and sub-halos (Klypin et al 1999; Moore et al 1999) Halo Cores and Densities: (Gilmore et al 2006; Kuzio de Naray 2008) Void Galaxy abundances (Peebles 2001) Angular Momentum Problem (Navarro & Benz 1991; Sommer-Larsen & Dolgov 2001) Disk Dominated Galaxy Formation (Governato et al 2002) Is the power spectrum different at small scales?

15 Measuring P(k) CMB SDSS Ly-α SDSS w(p)

16 Dwarf Spheroidal Density Profiles from Radial Stellar Velocity Dispersion All dwarf spheroidals studied are consistent with NFW and cored profiles, except for UMi, only consistent with cored profile [Gilmore et al.,astro-ph/ ] Constant core mass within stellar profile CDM

18 Dark Matter Vcirc / Central Concentrations are Much Too Low... Boylan-Kolchin, Bullock, Kaplinghat 2011

19 Central densities of Dwarfs are too low relative to latest high-res CDM simulations (Parry, Eke, Frenk, Okamoto 2011)

21 Weak Lensing Measures of the Nonlinear Regime Great sensitivity to the effects of WDM Markovic et al 2011

22 Modeling nonlinear clustering: The full halo model in WDM +P ss (k)+p sh (k)

23 Modeling nonlinear clustering: The full halo model in WDM +P ss (k)+p sh (k)

24 Modeling nonlinear clustering: The full halo model in WDM +P ss (k)+p sh (k)

25 Modeling nonlinear clustering: The full halo model in WDM +P ss (k)+p sh (k)

26 Modeling nonlinear clustering: The full halo model in WDM +P ss (k)+p sh (k) Substructure within 1 halo:

27 Modeling nonlinear clustering: The full halo model in WDM +P ss (k)+p sh (k) Substructure within 1 halo: Dunstan, Abazajian, Polisensky & Ricotti 2011

28 Halo and Subhalo Mass Functions log(dnw /dnc) Halo Subhalo log(m/m f ) log(m/m f )

29 Halo Profile Effects

30 Results on the Full Nonlinear Effects from the Halo Model

31 Particle Physics of Sterile Neutrinos

32 Sterile Neutrinos Beyond the Standard Model of Particle Physics ν s Phenomenological Insertion of Majorana & Dirac Mass Terms of Comparable Magnitude (atmos. & solar) (e.g. Asaka et al 2006) νmsm ν s Left-Right Symmetric Models (Pati & Salam 1974; Mohapatra & Pati 1975) ν s ν s ν s Higher Dimensional Operators in String-Inspired models (Langacker 1998) Bulk Fermions in Large Extra Dimensions (ADD; Dvali & Smirnov 2000) Axino in R-parity Violating Minimal Supersymmetric Models (Chun & Kim 1999)

33 The νmsm : a minimalist model The Neutrino Minimal Standard Model of Particle Physics [Asaka, Blanchet & Shaposhnikov 2005] Add Dirac & Majorana Neutrino Mass Terms to MSM δl = N I i µ γ µ N I fiαφ ν N I L α M I N c 2 I N I + h.c. Two heavy sterile neutrinos provide atmospheric & solar mass scales Baryogenesis via Oscillation-based Leptogenesis in 2 more massive sterile neutrinos Light sterile neutrino is the (Warm) Dark Matter More involved models generally involve similar insertions for neutrino mass generation

34 Text PDG, RPP 2004 Aguilar-Arevalo 2007 [MiniBooNE]

35 Text Aguilar-Arevalo 2010 [MiniBooNE] Akhmedov & Schwetz 2011 PDG, RPP 2004 Aguilar-Arevalo 2007 [MiniBooNE]

36 Reactor Anomaly Text Aguilar-Arevalo 2010 [MiniBooNE] Akhmedov & Schwetz 2011 PDG, RPP 2004 Aguilar-Arevalo 2007 [MiniBooNE]

37 A Phenomenelogical Model Sterile Neutrino Dark Matter ν 6 ν 1 kev α = cos θ ν a + sin θ ν b ν s = sin θ ν a + cos θ ν b sin 2 2θ 10 7 ν 5 ν ν 3 ν 2 ν 1 δm 2 LSND } } δm 2 atm δm 2 sol 1 ev 0.01 ev

39 kev Sterile Neutrinos Could be the Dark Matter (m s ~ 1 kev) (Dodelson & Widrow 1994; Shi & Fuller 1999; Abazajian, Fuller & Patel 2001) May Solve Several Potential Problems in the cold dark matter paradigm of Galaxy and Small Scale Structure Formation (e.g., Bode, Ostriker & Turok 2001) Provides pulsar kicks (Kusenko & Segre 1999) Enhances shock heating of the shock in Type II supernovae (Hidaka & Fuller 2006)

40 Sterile Neutrino Dark Matter Production Γ(ν α ν s ) Γ α (p) 2 (p) sin 2 2θ 2 (p) sin 2 2θ + D 2 (p) + [ (p) cos 2θ V L (p) V T (p)] 2

41 Sterile Neutrino Dark Matter Production Γ(ν α ν s ) Γ α (p) G 2 F pt 4 T 5 Γ α (p) 2 (p) sin 2 2θ 2 (p) sin 2 2θ + D 2 (p) + [ (p) cos 2θ V L (p) V T (p)] 2

42 Sterile Neutrino Dark Matter Production Γ(ν α ν s ) Γ α (p) G 2 F pt 4 T 5 Γ α (p) 2 (p) sin 2 2θ 2 p 2 T 2 2 (p) sin 2 2θ + D 2 (p) + [ (p) cos 2θ V L (p) V T (p)] 2

43 Sterile Neutrino Dark Matter Production Γ(ν α ν s ) Γ α (p) G 2 F pt 4 T 5 Γ α (p) 2 (p) sin 2 2θ 2 p 2 T 2 2 (p) sin 2 2θ + D 2 (p) + [ (p) cos 2θ V L (p) V T (p)] 2 D(p) 2 T 10

44 Sterile Neutrino Dark Matter Production Γ(ν α ν s ) Γ α (p) G 2 F pt 4 T 5 Γ α (p) 2 (p) sin 2 2θ 2 p 2 T 2 2 (p) sin 2 2θ + D 2 (p) + [ (p) cos 2θ V L (p) V T (p)] 2 D(p) 2 T 10 [V T ] 2 T 10

45 Sterile Neutrino Dark Matter Production Γ(ν α ν s ) Γ α (p) G 2 F pt 4 T 5 Γ α (p) 2 (p) sin 2 2θ 2 p 2 T 2 2 (p) sin 2 2θ + D 2 (p) + [ (p) cos 2θ V L (p) V T (p)] 2 H 2 = 8π 3 Gρ T 4 D(p) 2 T 10 [V T ] 2 T 10

46 Sterile Neutrino Dark Matter Production Γ(ν α ν s ) Γ α (p) G 2 F pt 4 T 5 Γ α (p) 2 (p) sin 2 2θ 2 p 2 T 2 2 (p) sin 2 2θ + D 2 (p) + [ (p) cos 2θ V L (p) V T (p)] 2 H 2 = 8π 3 Gρ T 4 Γ H { T 9 T 3 High T Low T D(p) 2 T 10 [V T ] 2 T 10

47 Sterile Neutrino Dark Matter Production Γ(ν α ν s ) Γ α (p) G 2 F pt 4 T 5 Γ α (p) 2 (p) sin 2 2θ 2 p 2 T 2 2 (p) sin 2 2θ + D 2 (p) + [ (p) cos 2θ V L (p) V T (p)] 2 H 2 = 8π 3 Gρ T 4 Γ H { T 9 T 3 High T Low T D(p) 2 T 10 [V T ] 2 T 10 Γ/H T (MeV)

48 Sterile Neutrino Dark Matter Production Γ(ν α ν s ) Γ α (p) G 2 F pt 4 T 5 Γ α (p) 2 (p) sin 2 2θ 2 p 2 T 2 2 (p) sin 2 2θ + D 2 (p) + [ (p) cos 2θ V L (p) V T (p)] 2 H 2 = 8π 3 Gρ T 4 Γ H { T 9 T 3 High T Low T D(p) 2 T 10 [V T ] 2 T 10 Never in Equilibrium!! Γ/H T (MeV)

49 Spectral Distribution ρ() = f s() f ν () f ν () = 1 e + 1 = p/t Abazajian 2005

50 Where does the CDM ansatz fail? Abazajian 2006 SDSS 3D P(k) Main Galaxies (Tegmark et al 2003) SDSS Lyman-alpha forest (McDonald et al 2005) High-Resolution Lyman-alpha forest (Viel, Haehnelt & Springel 2004) CMB: WMAP, ACBAR, CBI, VSA, BooMERANG-2K2

51 Where does the CDM ansatz fail? SDSS galaxy P g (k) Abazajian 2006 SDSS 3D P(k) Main Galaxies (Tegmark et al 2003) SDSS Lyman-alpha forest (McDonald et al 2005) High-Resolution Lyman-alpha forest (Viel, Haehnelt & Springel 2004) CMB: WMAP, ACBAR, CBI, VSA, BooMERANG-2K2

52 Where does the CDM ansatz fail? SDSS galaxy P g (k) SDSS Ly-α forest P F (k) Abazajian 2006 SDSS 3D P(k) Main Galaxies (Tegmark et al 2003) SDSS Lyman-alpha forest (McDonald et al 2005) High-Resolution Lyman-alpha forest (Viel, Haehnelt & Springel 2004) CMB: WMAP, ACBAR, CBI, VSA, BooMERANG-2K2

53 Where does the CDM ansatz fail? SDSS galaxy P g (k) SDSS Ly-α forest P F (k) LUQAS (VLT) Ly-α forest P F (k) Abazajian 2006 SDSS 3D P(k) Main Galaxies (Tegmark et al 2003) SDSS Lyman-alpha forest (McDonald et al 2005) High-Resolution Lyman-alpha forest (Viel, Haehnelt & Springel 2004) CMB: WMAP, ACBAR, CBI, VSA, BooMERANG-2K2

54 Where does the CDM ansatz fail? SDSS galaxy P g (k) SDSS Ly-α forest P F (k) LUQAS (VLT) Ly-α forest P F (k) Keck Ly-α forest P F (k) Abazajian 2006 SDSS 3D P(k) Main Galaxies (Tegmark et al 2003) SDSS Lyman-alpha forest (McDonald et al 2005) High-Resolution Lyman-alpha forest (Viel, Haehnelt & Springel 2004) CMB: WMAP, ACBAR, CBI, VSA, BooMERANG-2K2

55 Lyman-α forest: Powerful & Challenging J. Shalf, Y. Zhang (UIUC) et al., GCCC

56 Lyman-α forest: Powerful & Challenging the flux power spectrum J. Shalf, Y. Zhang (UIUC) et al., λ GCCC (Å)

57 Lyman-alpha Forest Constraints on CDM m s > 14 kev Seljak et al 2006: WMAP1 + SDSS Pg(k) + Lya + HR λ FS < 54 kpc M FS < 10 7 M sun (Abazajian & Koushiappas 2006) m s > 12.1 kev (SDSS PF(k) + VLT LUQAS data; Boyarsky et al 2008) All Depend on the McDonald et al. (2006) SDSS PF(k) Measurement

58 SDSS Ly-α Constraints: Viel et al 2006 (unpublished) WDM analysis Very high T 0 ~35000 K

59 Turning an astrophysical signal into a constraint: The Dwarf galaxy count in the Milky Way Eventually, WDM is too much of a good thing, oversupression of the dwarf galaxy scale SDSS has found a large population of new dwarf galaxies in the MW local group Polisensky & Ricotti (2011)

oversupression of the dwarf galaxy scale SDSS has found a large

60 Turning an astrophysical signal into a constraint: The Dwarf galaxy count in the Milky Way Eventually, WDM is too much of a good thing, oversupression of the dwarf galaxy scale SDSS has found a large population of new dwarf galaxies in the MW local group m GWDM Polisensky & Ricotti (2011)

61 Radiative Decay in the X-ray l - l - Pal & Wolfenstein 1981 ν s ν α + γ 2 W + 1 E γ = m s 2 1 kev Γ γ = sec 1 sin 2 2θ ms 1 kev 5

62 Radiative Decay in the X-ray l - l - Pal & Wolfenstein 1981 ν s ν α + γ 2 W + 1 E γ = m s 2 1 kev Γ γ = sec 1 sin 2 2θ ms 1 kev 5

63 Radiative Decay in the X-ray l - l - Pal & Wolfenstein 1981 ν s ν α + γ 2 W + 1 E γ = m s 2 1 kev Γ γ = sec 1 sin 2 2θ ms 1 kev 5 Virgo Cluster: DM particles

64 Upper Mass Limit: X-ray observations of Virgo m s = 4 kev m s = 5 kev Abazajian, Fuller & Tucker 2001

65 Chandra Deep Field: Milky Way Halo Limits from the Unresoved X-ray Background CDF-South Source Removal Hickox & Markevitch 2006,

66 The (Unresolved) Cosmic X-ray Background Abazajian et al Hickox & Markevitch 2007 residuals Normalized counts/sec/kev Channel Energy [kev]

1 kev Milky Way in CXB: Abazajian et al. 2006 m s < 5.

67 X-ray Constraint Summary XMM Newton: The Virgo Cluster Andromeda Galaxy: Watson et al m s < 2.2 kev Ursa Minor: Lowenstein et al m s < 3.1 kev Milky Way in CXB: Abazajian et al m s < 5.7 kev Coma + Virgo Clusters: Boyarsky et al m s < 6.3 kev X-Ray Background: Boyarsky et al m s < 8.9 kev

68 The Detection of a WDM Sterile Neutrino? ApJ 2010, arxiv: v1 Text significance of 1.8 σ Method of subtraction of the background could be revealing this line (Mirabel & Nieto, arxiv: )

69 Claimed νs line: unaddressed problems... One should see a line in the noise in a 0.2 kev resolution spectrum from 1-7 kev at this level of statistical significance (2.8 σ) Sulfur Kα and Kβ lines present in this region Subtraction of the background can produce a similar feature (Mirabel & Nieto, arxiv: ) Presence of feature is inconsistent at > 14σ with limits from Andromeda (M31) observations, even when maximizing Willman I DM profile and minimizing that from M31

70 International X-ray Observatory

71 Sterile Neutrino Dark Matter Parameter Space Summary Abazajian 2011

72 Sterile Neutrino Dark Matter Parameter Space Summary Abazajian 2011

73 Not-So-Deviant Dark Matter Candidates

74 CDM to γ-ray: the potential dark matter sky X DM + X DM Y + + Y (brems), X DM γ + γ Springel et al 2008

75 The Observed Fermi-LAT Gamma-Ray

76 The Observed Isotropic Diffuse γ-ray Spectrum The Fermi-LAT collaboration (A.A. Abdo et al.) JCAP, arxiv:

77 DM Annihilation: Galactic and Extragalactic Contributions Galactic: dφ γ de = σ Av 2 J Ω J 0 1 Ω obs m 2 χ dn γ de J (b,l )=J 0 xmax x min ρ 2 (r gal (b,l, x)) dx Extragalactic: dφ γ de = σ Av 2 c Ω obs H 0 (f DM Ω m ) 2 ρ 2 crit m 2 χ zup 0 f(z)(1 + z) 3 h(z) dn(e ) de e τ(z,e ) dz

78 DM Annihilation: Galactic and Extragalactic Contributions Galactic: particle dφ γ de = σ Av 2 J Ω J 0 1 Ω obs m 2 χ dn γ de J (b,l )=J 0 xmax x min ρ 2 (r gal (b,l, x)) dx Extragalactic: dφ γ de = σ Av 2 c Ω obs H 0 (f DM Ω m ) 2 ρ 2 crit m 2 χ zup 0 f(z)(1 + z) 3 h(z) dn(e ) de e τ(z,e ) dz

79 DM Annihilation: Galactic and Extragalactic Contributions Galactic: particle dφ γ de = σ Av 2 J Ω J 0 1 Ω obs m 2 χ dn γ de J (b,l )=J 0 xmax x min ρ 2 (r gal (b,l, x)) dx astro Extragalactic: dφ γ de = σ Av 2 c Ω obs H 0 (f DM Ω m ) 2 ρ 2 crit m 2 χ zup 0 f(z)(1 + z) 3 h(z) dn(e ) de e τ(z,e ) dz

80 DM Annihilation: Galactic and Extragalactic Contributions Galactic: particle dφ γ de = σ Av 2 J Ω J 0 1 Ω obs m 2 χ dn γ de J (b,l )=J 0 xmax x min ρ 2 (r gal (b,l, x)) dx astro Extragalactic: particle dφ γ de = σ Av 2 c Ω obs H 0 (f DM Ω m ) 2 ρ 2 crit m 2 χ zup 0 f(z)(1 + z) 3 h(z) dn(e ) de e τ(z,e ) dz

81 DM Annihilation: Galactic and Extragalactic Contributions Galactic: particle dφ γ de = σ Av 2 J Ω J 0 1 Ω obs m 2 χ dn γ de J (b,l )=J 0 xmax x min ρ 2 (r gal (b,l, x)) dx astro Extragalactic: particle dφ γ de = σ Av 2 c Ω obs H 0 (f DM Ω m ) 2 ρ 2 crit m 2 χ zup 0 f(z)(1 + z) 3 h(z) dn(e ) de e τ(z,e ) dz astro

82 Dark Matter in the Isotropic Diffuse Spectrum Abazajian, Agrawal, Chacko & Kilic, arxiv:

83 Lessons from the Cosmic X-ray Background

84 Chandra Deep Field: Milky Way Halo Limits from the Unresoved X-ray Background CDF-South Source Removal Hickox & Markevitch 2006,

85 The Observed Fermi-LAT Gamma-Ray 15% of extragalactic flux is already found to be from resolved blazars

86 Blazars in the Unified Model of AGN Blazars

87 Allows for Forecasts for Fermi-LAT s DGRB COMPTEL Non-blazar AGN Fermi-LAT DGRB Current Blazars current Forecast minimum and maximum (95% CL) Blazars 95% CL max Blazars 95% CL min Abazajian, Blanchet & Harding,

88 Annihilation Channel Forecasts Abazajian, Blanchet & Harding 2012

89 Annihilation Channel Forecasts Abazajian, Blanchet & Harding 2012

90 Annihilation Channel Forecasts Abazajian, Blanchet & Harding 2012

91 Annihilation Channel Forecasts Abazajian, Blanchet & Harding 2012

92 Dark Matter in the Galactic Center? Average msec pulsars Hooper & Goodenough, arxiv:

93 Dark Matter in the Galactic Center? Average msec pulsars Hooper & Goodenough, arxiv:

94 Dark Matter in the Galactic Center? Gal. Center Average msec pulsars Hooper & Goodenough, arxiv:

95 Dark Matter in the Galactic Center? Gal. Center Geminga Pulsar Average msec pulsars Hooper & Goodenough, arxiv:

96 Dark Matter in the Galactic Center? Gal. Center Omega Cen Geminga Pulsar Average msec pulsars Hooper & Goodenough, arxiv:

97 Dark Matter in the Galactic Center? Gal. Center Omega Cen NGC 6388 Geminga Pulsar Average msec pulsars Hooper & Goodenough, arxiv:

98 Dark Matter in the Galactic Center? Gal. Center Omega Cen NGC 6388 M 28 Geminga Pulsar Average msec pulsars Hooper & Goodenough, arxiv:

99 Light DM: Morphological Case? Hooper & Linden 2011

100 Morphological Evidence Non- GC Point Sources GC 2FGL + Gal Diff σ-residual in prep...

101 High Energy Spectroscopic Survey (HESS) Gamma- Ray Telescope in Namibia Would detect gamma-rays from annihilation products in PAMELA Dark Matter Models

102 Residual Spectrum Toward the Galactic Center

103 HESS Galactic Center Constraints on PAMELA Dark Matter Interpretations Abazajian & Harding 2011

104 Summary Sterile Neutrino Dark Matter Warm Dark Matter has become the standard alternate cosmological structure formation scenario, as it may resolve many problems in structure formation, though stringent limits exist Sterile Neutrino Dark Matter is a natural, minimal WDM and CDM candidate Upcoming weak lensing and galaxy surveys can be sensitive to WDM effects in the mild to strongly nonlinear regime Lower-limits mass from the Lyman-alpha Forest are dependent on the thermal history of the universe, uncorrected noise in the SDSS spectrograph and uncertain Sterile Neutrino Dark Matter, in the standard production scenarios, is detectable or potentially excludable with the IXO satellite WIMP Dark Matter The diffuse gamma-ray background is the most conservative and, when including the MW Galactic contribution, a stringent constraint The DGRB constraints are dwarfed by Fermi-LAT dwarf galaxy constraints and HESS GC Constraints Claims for DM signals from the GC based on both spectral & morphological information do not survive quantitative scrutiny

Detecting Dark Matter in the X-ray

Detecting Dark Matter in the X-ray Kev Abazajian University of Maryland Quantum 2 Cosmos 3: Airlie Center, July 8, 2008 The CDM Ansatz Problems in Cold Dark Matter? Halo Substructure: satellite galaxies