Dark matter and entropy dilution

Transcription

1 Dark matter and entropy dilution Miha Nemevšek Goran Senjanović, Yue Zhang Dark workshop TÜM/IAS, December 2015

2 Dark Matter stability

3 Discrete symmetries MSSM & R-parity extended Higgs Inert Higgs doublet Z 2 symmetries talk by Steffen

4 Discrete symmetries MSSM & R-parity extended Higgs Inert Higgs doublet Z 2 symmetries talk by Steffen Small couplings and or large scales small couplings (Dirac Yukawa) large scales (extended gauge symmetry) i.e. small masses (e.g. axion) talk by Redondo µ / m 5 µ/m 4 W m DM

5 Neutrino mass vs. Dark Matter new physics needed for neutrino mass talk by Schwetz

6 Neutrino mass vs. Dark Matter new physics needed for neutrino mass, same for DM?

7 Neutrino mass vs. Dark Matter small couplings (Dirac Yukawa) S MSM 5 mµ m S S ' µ m S m Dodelson, Widrow 93,... can t do justice to the field m S. 20 kev talk by Drewes

8 Neutrino mass vs. Dark Matter small couplings (Dirac Yukawa) S MSM 5 mµ m S S ' µ m S m m S. 20 kev Dodelson, Widrow 93,... can t do justice to the field large scales and small masses no direct channels below m N1 ' kev M WR m & 14 TeV N i, only mixing Left-Right Bezrukov, Hettmansperger, Lindner 09 a possible window M WR 2 (4, 7) TeV MN, Senjanović, Zhang 12 DM predicts mass and flavor of N i

9 Left-Right the minimal model SU(2) L SU(2) R U(1) B L understanding the SM asymmetry......through spontaneous breaking Pati, Salam 74 Mohapatra, Pati 75 Senjanović, Mohapatra 75 W L Q L = L L = ul d L el L Q R = L R = ur d R er R W R

10 Left-Right the minimal model understanding the SM asymmetry......through spontaneous breaking Pati, Salam 74 Mohapatra, Pati 75 Senjanović, Mohapatra 75 W L Q L = L L = ul d L el L (2, 2, 0) L(3, 1, 2) R(1, 3, 2) Q R = L R = ur d R er R W R seesaw Minkowski 79 Senjanović, Mohapatra 79 rich phenomenology: LNV, LFV at colliders, 0 2

11 Left-Right 0 2 vs. LHC in ev Senjanović, Mohapatra 82 Tello, MN, Nesti, Senjanović, Vissani 10 mn ee M WR =3.5 TeV m N =.5 TeV lightest m in ev in GeV mn D0: dijets ` 3 2 e + jetêem activity L=33.2pb -1 0n2bHHML t N ~1 mm Keung, Senjanović 83 MN, Nesti, Senjanović, Zhang e + Displaced Vertex t N ~5 m CMS e + Missing Energy M W WR in GeV mass origin in Higgs decays h! N i N i Maiezza, MN, Nesti, 15

12 Left-Right 0 2 vs. LHC in ev Senjanović, Mohapatra 82 Tello, MN, Nesti, Senjanović, Vissani 10 mn ee M WR =3.5 TeV m N =.5 TeV in GeV mn lightest in ev m Dark Matter? 1000 L=33.2pb D0: dijets ` 3 2 e + jetêem activity e + Displaced Vertex 0n2bHHML t N ~1 mm t N ~5 m Keung, Senjanović 83 MN, Nesti, Senjanović, Zhang 11 CMS e + Missing Energy M W WR in GeV mass origin in Higgs decays h! N i N i Maiezza, MN, Nesti, 15

13 Dark Matter (over)production

14 Left-Right freeze-out part 1 gauge interactions keep thermal equilibrium suppressed rate compared to SM neutrinos N ' 4 MW ' G 2 F M WR MW M WR 4 T 5 thermal freeze-out MW M WR 4 T 5 ' p GT 2 around the QCD phase transition 1/6 g (T f ) MWR T f ' 400 MeV 70 5 TeV 4/3

15 Left-Right over-abundance freeze-out relativistic, no Boltzmann suppression T f >m N kev freeze-out relativistic, no Boltzmann suppression Y N n N s ' 135 (3) 4 4 g (T f ) Y N conserved, evolve to present times N1 = Y N1 m N1 s = 3.3 c mn1 kev ' 13 DM 70 g (T f ) many species, not in LRSM m N1 g < 1000 < 0.08 kev astrophysics,...

16 Dark Matter dilution

17 Decaying particles in the early universe Scherrer, Turner 85 massive late decaying particle decays heat up radiation, dilutes the rest diluter applied to sterile neutrinos Asaka, Shaposhnikov, Kusenko 06

18 Decaying particles in the early universe Scherrer, Turner 85 massive late decaying particle decays heat up radiation, dilutes the rest diluter applied to sterile neutrinos Asaka, Shaposhnikov, Kusenko 06 Left-Right candidates Higgs sector heavy & unstable next-to-lightest N 2,3 the only remaining candidates

19 Diluting with part 1 Scherrer, Turner 85 N 2 sudden decay approximation (works for m ) t apple 2 matter dominance H 2 = 2 2 = 8 3M 2 P 22 MP 2 T < =0.65 Y 2 m 2 g (Y 2 m N2 ) 2 2 g 45 T 3 < 1/3

20 Diluting with part 1 Scherrer, Turner 85 N 2 sudden decay approximation (works for m ) t apple 2 t 2 matter dominance H 2 = 2 2 = 8 3M 2 P 22 MP 2 T < =0.65 Y 2 m 2 g (Y 2 m N2 ) 2 2 g 45 T 3 < 1/3 radiation dominance H = 2 =1.66 g1/2 T> 2 M P p T > ' 0.78 g 1/4 2M P r 1 sec ' 1.22 MeV 2 needed for BBN

21 Diluting with part 1 Scherrer, Turner 85 N 2 sudden decay approximation (works for m ) t apple 2 t 2 matter dominance H 2 = 2 2 = 8 3M 2 P 22 MP 2 T < =0.65 Y 2 m 2 g (Y 2 m N2 ) 2 2 g 45 T 3 < 1/3 radiation dominance H = 2 =1.66 g1/2 T> 2 M P p T > ' 0.78 g 1/4 2M P r 1 sec ' 1.22 MeV 2 Dilution factor S = T> T < 3 ' 1.7 T ( 2) 1/4 Y 2 m 2 p 2M P S / m 2 p 2 needed for BBN

22 Diluting with part 1 N 2 how much dilution? N1 '.228 mn1 kev 1.85 GeV sec m N2 2 g (T f2 ) g (T f1 ) Boltzmann suppressed T f1 ' 400 MeV

23 Diluting with part 1 N 2 how much dilution? N1 '.228 mn1 kev 1.85 GeV sec m N2 2 g (T f2 ) g (T f1 ) Boltzmann suppressed T f1 ' 400 MeV 1sec lifetime near the m + m` threshold, disfavored MeV MWR (N 2! ` ) =sec 5 TeV m N f(x`,x ) ` = e, µ

24 Diluting with part 1 N 2 how much dilution? N1 '.228 mn1 kev 1.85 GeV sec m N2 2 g (T f2 ) g (T f1 ) Boltzmann suppressed T f1 ' 400 MeV 1sec lifetime near the m + m` threshold, disfavored MeV MWR (N 2! ` ) =sec 5 TeV m N f(x`,x ) ` = e, µ freeze-out flavor dependent m N1 kev V Re1 ' 0 SN cooling Raffelt, Seckel 88 Barbieri, Mohapatra 89 turn off W R V R 1 ' 1 T f1 >T f2

25 Mass spectrum of DM in Left-Right mass and flavor fixed DM couples to V R ' A m N1 ' kev

26 Mass spectrum of DM in Left-Right mass and flavor fixed V R ' A m N2 ' m + m µ m N3 ' m + m e Diluters couple to e and µ

27 Dark Matter freeze-out pt. 2

28 Left-Right freeze-out part II drop in g Y N2 ' g (T f1 ) Y N1 g (T f2 ) N 1 60 g* MeV 400 MeV N T@GeVD

29 Left-Right freeze-out part II pair N i N i! `+`, uu, dd single N i`! ud, N i u! `+d, N i d! `+u W g R N2 W g R N1 n N2 H g HGeV 4 L GeVêT g 5.0

30 Left-Right freeze-out part II DM-diluter separation window T QCD = 350 MeV T QCD = 150 MeV Y=nês T QCD = 400 MeV N Boltzmann suppressed N M universal freeze-out

31 Left-Right freeze-out part II coupled Boltzmann equations i =1, 2, 3 shz dy N i dz = YNi Y eq 1 N i W R N i! 2 YNi Y eq 1 WR N i N i + N i Z LR N i N i N 3 Y=nês N 2 Y N2,3 >Y N N1 M WR =5.5TeV, T QCD =350MeV z=m N2 êt

32 Left-Right freeze-out part II final yields N 3 T QCD =350MeV T QCD =400MeV T QCD =150MeV YN= n N s Boltzmann suppressed N 2 N M WR HTeVL universal freeze-out

33 Dark Matter dilution pt. 2

34 Dilution phase space 100 Non thermal history or DM over abundance MSM WR mass in TeV Boltzmann suppressed, decays to N 1 5 e Decays too fast Dilutor mass in GeV

35 Dilution phase space e m Non thermal history or DM over abundance MSM WR mass in TeV 50 LHC reach 10 5 e Excluded by direct searches & theory Decays too fast Boltzmann suppressed Dilutor mass in GeV

36 Dilution part 1I coupled energy density evolution matter radiation d dt +4H = d N1 dt d N2 dt +4H N1 =0 +4H N2 = 2 2 d N3 dt +4H N3 = 3 3

37 Dilution part 1I freeze-out coupled energy density evolution match z m = 30 T,m ' 15 MeV t m =1/(2H) matter radiation d dt +4H = d N1 dt d N2 dt d N3 dt +4H N1 =0 +4H N2 = H N3 = 3 3 N1 (t m )= 7 4 (t m )= 2 30 g (T,m )T 4,m 2 30 g (T,m )T 4 N 1,m N2 (t m )=m N2 Y N2 (z m ) g (T,m )T 3,m N3 (t m )=m N3 Y N3 (z m ) g (T,m )T 3,m

38 Dilution part 1I radiation decrease slows down r g r N1 r DM decouples M WR =5.5TeV, T QCD =350MeV r N2 +r N têt N diluters decay

39 Dilution part 1I N2 + N3 = = 2 30 g (T r )T 4 r T r & 0.7 MeV r g r N1 r r N2 +r N M WR =5.5TeV, T QCD =350MeV S = S(t f ) S(t m ) = s(t f ) s(t m ) V (t f ) V (t m ) = têt N 3/4 3/4 (tf ) N1 (t f ) (t m ) N1 (t m )

40 Left-Right low scale DM windows min W N m N1 =0.5 kev Planck 15 t N2,3 >1.5 sec disfavored by BBN M WR HTeVL T r / 1/ p N S / p N

41 Left-Right low scale DM windows min W N m N1 =0.4 kev Planck 15 t N2,3 >1.5 sec disfavored by BBN M WR HTeVL

42 Left-Right low scale DM - further constraints dsph m N1. ( ) kev diluted Ly- m N1. O(keV) CMB & N eff repopulation N 3! + e! e + e µ µ e N 2! + µ! e + e µ µ µ e e Fuller, Kishimoto, Kusenko 11 X-ray observations M D, LR & v L Merle, Niro subject to uncertainties M WR & (5 7) TeV MN, Senjanović, Zhang 12 Lopez-Pavon, Huang 13

43 Critical conclusion RH neutrino kev DM candidate pros dilution possible in the minimal model window at the LHC X-ray limits cons fairly low reheating vs. BBN and CMB light DM mass vs. Ly-

44 Thank you

45 X-ray constraints Majorana vs. Dirac in Left-Right MN, Senjanović, Tello 13 seesaw M = MDM T 1 N M D + v L M N v R parity M D = M T D M D = im N r M 1 N M v L v R M N = V T R m N V R γ γ W ξ LR A N1! = l j ν k N 1 ν i N1 l i + ν j N 1! = µ mn1 m µ 5 3 X` 4 LR`N1 f D + LR m` m N1 f LR 2

46 0 2 constraints m N 3 ee = p 2 MW M WR 4 V 2 Re3 m N3 p 2 + m 2 N 3 MN, Nesti, Senjanović, Tello 11 m N ee = including the mixing LR + M 2 W M 2 W R MN, Senjanović, Tello 12 see also Lopez-Pavon, Huang 13 Barry, Rodejohann 13 p M 1 N M D ee M Excluded by Cosmology 1.0 Excluded by 0n2b m ee V R en = 0.8 R = 0.4 V mn V R tn = 0.4 LHC reach HL=300êfbL NME uncertainties axial coupling Barea, Kotila, Iachello 12, 13, 15 Theoretical Limit m