Nonthermal Dark Matter from Moduli decay. Bhaskar Dutta. Texas A&M University

Transcription

1 Nontheral Dark atter ro oduli decay Bhaskar Dutta Texas A& University Hidden Dark atter Workshop, CTP, University o ichigan 1

2 Outline Theral and Non-theral Dark atter (D) oduli Decay and D Baryogenesis ro the Decay o oduli Necessary Conditions or Successul odels Exaple o a oduli odel Dark Radiation (DR) and D correlation Exaple o visible sector odel Non-Theral Scenarios at the LHC and Direct Detection Expt. Conclusion

3 Questions Iportant questions: What is the origin o dark atter? Dark Energy 68% Dark atter 7% How does it explain the dark atter content? Is there any correlation between baryon and dark atter abundance? Atos 5% S Consequences or: Particle Physics odels Theral History o the Universe 3

4 Dark atter: Theral Production o theral non-relativistic D: D D Non-relativistic Freeze-Out: Hubble expansion doinates over the interaction rate 1 Dark atter content: ~ D v reeze out v 310 v T 6 0 ~ D ~ Assuing : c 3 s /T Y becoes constant or T>T a c ~O(10 - ) with c ~ O(100) GeV leads to the correct relic abundance 4

5 Dark atter: Theral Suitable D Candidate: Weakly Interacting assive Particle (WIP) Typical in Physics beyond the S (LSP, LKP, ) ost Coon: Neutralino (SUSY odels) Neutralino: ixture o Wino, Higgsino and Bino saller annihilation cross-section Larger annihilation cross-section Larger/Saller Annihilation Proble or theral scenario 5

6 Theral D 7% Status o Theral D Experiental constraints: ann v Gaa-rays constraints: Dwar spheroidals, Galactic center Large Crosssection is constrained ann v o : saller than the theral value Geringer-Saeth, Koushiappas 11, Hooper, Kelso, Queiroz, Astropart.Phys. 13 6

7 LHC Constraints and Status o D LHC constraints on irst generation squark ass + Higgs ass: Natural SUSY and dark atter [Baer, Barger, Huang, ickelson, ustaayev and Tata 1; Gogoladze, Nasir, Shai 1, Hall, Pinner, Ruderan, 11; Papucchi, Ruderan, Weiler 11], Higgs ass 15 GeV & Cosological gravitino solution [Allahverdi, Dutta, Sinha 1] Higgsino dark atter Higgsino dark atter has larger annihilation cross-section Typically > 3 x 10-6 c 3 /sec or sub-tev ass Theral underproduction o sub-tev Higgsino Unnatural SUSY: Wino D- Larger annihilation cross-section (or saller wino ass) Arkani-Haid, Gupta, Kapla, Weiner, Zorawsky 1 7

8 LHC status Recent Higgs search results ro Atlas and CS indicate that h ~16 GeV in the tight SS window <135 GeV (1st gen.) ~ 1.7 TeV For heavy ~ q ~q, ~ g ~ t1 g ~ ~ t ~ g 1.3 TeV produced ro, 700 GeV ~ t1 produced directly, 660 GeV (special case) 1 ~e / ~ ~ t1 excluded between 110 and 80 GeV or a ass-less or or a ass dierence >100 GeV, sall D is associated with sall issing energy Can lead to over production o relic abundance ~ 1 0 ~ 1 asses between 100 and 600 GeV are excluded 0 or ass-less ~ 1 or ~ 1 or or the ass dierence >50 GeV decaying into e/ Can lead to over production o relic abundance 8

9 Status o Theral D Theral equilibriu above T is an assuption. T T Non-standard theral history at is generic in soe explicit UV copletions o the S. Acharya, Kuar, Bobkov, Kane, Shao 08 Acharya, Kane, Watson, Kuar 09 Allahverdi, Cicoli, Dutta, Sinha, 13 D content will be dierent in non-standard theral histories (i.e., i there is entropy production at ). T T Barrow 8, Kaionkowski, Turner 90 D will be a strong probe o the theral history ater it is discovered and a odel is established.

10 Theral, Non-theral ann v : Large ulticoponent/non-theral; Sall Non-theral LHC: Deterine the odel, easure D D annihilation ro galaxy, extragalactic sources Annihilation into photons: Feri, HAWC, H.E.S.S. Annihilation into neutrinos: IceCube Annihilation into electron-positrons: AS 10

11 Beyond Theral D ann v 310 Obtaining correct relic density or : 6 c 3 s 1 1) (theral underproduction): ann v c 3 s 1 Baer, Box, Suy 09 ulti-coponent D (WIP + non-wip) Exaple: ixed Higgsino/axion D ann v Zurek 13 Asyetric D (D content can have large ) ) (theral overproduction): D ro WIP decay Ex: Axino D, Gravitino D ann v c 3 s 1 Covi, Ki, Roszkowski 99 Feng, Rajaraan, Takayaa 03

12 The oduli decay width: Non-Theral D Dark atter ro oduli decay: oduli are heavy scalar ields that acquire ass ater SUSY breaking and are gravitationally coupled to atter T r ~ 3 c p start oscillating when H < t doinate the Universe beore decaying and reheating it c 1/ p 1/ T r T BBN 50 3 ev TeV For T r <T : Non-theral dark atter Inlation Radiation doination oduli doination Decay o oduli radiation doination. 3T r Abundance o decay products Y. 4. e.g., oroi, Randall 99; Acharya, Kane, Watson 08,Randall; Kitano, urayaa, Ratz 08; Dutta, Leblond, Sinha 09; Allahverdi, Cicoli, Dutta, Sinha, 13 1

13 D abundance Dark atter ro oduli D in 1. First ter on the RHS is the annihilation scenario Requires: th T ann n v s ann v.[ n T r th Since T r < T, we need ann v ann v wino/higgsino D Gaa-rays constraints: Dwar spheroidals, Galactic center D > 40 GeV, T < 30 T r T r > 70 ev D s obs v v [Hooper, Kelso, Queiroz,; Geringer-Saeth, Koushiappas] Th T T r, Y Br D ]. Second ter on the RHS is the branching scenario Can accoodate large and sall annihilation cross-sections Bino/Wino/Higgsino are all ok Y is sall to prevent the Br D ro becoing too sall (actually in realistic scenarios: Br 5 x10-3 => T r < 70eV) (or ~ 5 x10 6 GeV) 13

14 Dark atter ro oduli Decays dilutes any previous relics Theral D gets diluted i T r < T ~ D /0 ~ O(10) GeV Axionic D gets diluted i T r < L QCD ~ 00 ev ( a ~10 14 is allowed or T r T BBN ) [Fox,Pierce,Thoas 04] Baryon asyetry gets diluted i produced beore decay Non-theral D Production ro decay Annihilation scenario or T r close to T D production with large cross-section: Wino/Higgsino Branching scenario or saller T r (annihilation cross-section does not atter) Baryon asyetry ro decay Cladogenesis o D and Baryogenesis [Allaverdi, Dutta, Sinha 11] 14

15 Dark atter ro oduli Branching scenario solves the coincidence proble Baryon abundance in this odel: n s B Y Br B Y appears in the D abundance as well, Y ~ BR B ~ easy to satisy or baryogenesis, e (one loop actor) ~ b D 1 D Y Br Y Br B D 1 D Br Br B D 1 5 W=r/r c ; r=n For D ~ 5 B, e BR B ~ BR D n B ~ n D The D abundance and Baryon asyetry are ostly saturated by Y, Brs contribute the reaining not uch particle physics uncertainty

16 Baryogenesis ro oduli N W extra i N u c i X X, ' ij X d c i d c j X : S singlet; : Color triplet, hypercharge 4/3 Baryogenesis ro decays o X, X X or N N ~ : can be the D candidate : Allahverdi, Dutta, ohapatra, Sinha 1 X N N nb nb B Y Br N s Br N : branching ratio o oduli decay to N Assuing that N produces Baryon Asyetry e : asyetry actor in the N decay Y ~ , <0.1, Br N ~ B = 9x

17 17 Baryogenesis Fro X decay Typically, e 1, is O(10 - ) or CP violating phase O(1) and l~o(1) Baryogenesis ro oduli N N X X X d d X u N W c j c i ij c i i extra ' Siilarly, e

18 Conditions or odels Two typical probles or oduli decay Gravitino Proble: [Endo,Haaguchi,Takahashi 06][Nakaura,Yaaguchi 06] I 3/ <40 TeV Gravitino decays ater the BBN > 3/ can lead to D overproduction Large branching ratio o oduli into light Axions N e [Cicoli,Conlon,Quevedo 1][Higaki,Takahashi 1] 4/3 7 4 rad (1 N e ) 8 11 Current bound ro Planck+WAP9+ACT+SPT+BAO+HST (at 95% CL) : N e =

19 Ex: NT D in Large Volue Scenarios K 3ln( T T ), b b W W Ae at s lux Balasubraanian, Berglund, Conlon, Quevedo 05 Large volue can be obtained ater stabilization o v 3/ b 3/ np ( Tb Tb For large volue, one can have a sequestered scenario such that: 3/ vis b ) / Cicoli, Conlon, Quevedo 08 sot b ( For exaple, TeV scale SUSY can be obtained or: ~ 3/ sot 3/ b ) / ~ 10 GeV, ~ 510 GeV, b sot ~ 1 TeV [Detailed ass spectra, Aparicio, Cicoli, Kippendor, aharana, Quevedo 14 No Gravitino Proble

20 Br 3 The decay to gauge bosons arises at one-loop level: 3 S 3 gg ~ ln( b ) 4 P The decay to Higgs controlled by the Giudice-asiero ter: H NT D in Large Volue Scenarios u H d b 3 Z 4 P The decay to gauginos (and Higgsinos) is ass suppressed: sot gg ~~ Br 1 P 3/ LVS set up can successully accoodate non-theral D. Y can be quite sall ~ : branching and annhilations are ok / 0 Allahverdi, Cicoli, Dutta, Sinha 13

21 NT D in Large Volue Scenarios I the doinant decay ode is to gauge boson inal states decays into D particle via 3-body: g gg ~ ~ Since g ~ BR 10 3 D produces dark atter at the end o the decay chain The 3 body decay width larger than the -body decay width o oduli into gauginos [ g ~ g ~ is suppressed by ( gaugino / ) copared to gg ] Y ~ (using ~5 x 10 6 GeV) Y D : Y BR D ~ 10-1 D ~ O(100) GeV is allowed Solves the coincidence proble 1

22 D-DR Correlation in LVS: The axionic partner o, denoted by is not eaten up by anoalous U(1) s. a a b b acquires an exponentially suppressed ass. is produced ro a b a b 1 48 D-DR Correlation 3 P b decay: ab Cicoli, Conlon, Quevedo 13 Bulk axions are ultra-relativistic and behave as DR. a b 0 N e contribute to the eective nuber o neutrinos : 3 ( cvis ctot ) 43chid N e 48 P 7c vis ( N e N 3.04) e

23 D-DR Correlation Decay to visible sector ainly produces gauge bosons and Higgs: gg K S ~ 4 ZH u H b b d 3 P h.c. gg a b a H u H d b Z 4 P 3 tot H u H d a b a b Bound ro Planck+WAP9+ACT+SPT+BAO+HST at 95% N e N e 1 Z 3 We get a lower bound on T r

24 P r tot vis r T g C C T 4 1/ * ) ( ) ( ) ( * g TeV O T ev O r D-DR Correlation 3 3 4, 4 P vis vis P tot tot C C 1, Z C Z C tot vis Using 4 1/ 1/ 4 * )] 30 /( [ vis r g T

25 D-DR Correlation Abundance o D particles produced ro decay: Y n s 3T 4 r Br : Branching scenario Z 3, ~ GeV T r O( GeV ) Y 10 6 Br n s n s obs : Branching scenario does not work Avoiding excess o DR within LVS preers Annihilation scenario Higgsino-type D. 5

26 D-DR Correlation Obtaining the correct relic density in Annihilation scenario needs: T r T 3 10 v ann 6 ann c v 3 s 1 Assuing S-wave annihilation, which is valid or the Higgsinotype D, is directly constrained by Feri. For Higgsino-type D, using the b inal state, the bound reads: T ~ 0 40 GeV 1 T r (18 GeV ) GeV Upper bound on v ann T r gets bounded ro below

27 D-DR Correlation T r T ann c v 3 s 1 T ~ 0 Allowed by the Feri data in the annihilation scenario Over production in the branching scenario

28 D-DR Correlation T r 1 5C 88 C vis hid g * ( T r ) 1 / 4 P using N e 43 7 C C hid vis The Feri bound is translated to constraint in N e plane: ~ GeV Allahverdi., Cicoli, Dutta, Sinha N e, : set lower bound on D ass

29 odel Exaples: can be a visible sector ield S (oduli is a hidden sector ield) W s hsx X 1 s S W=W s +W N,X s ~ O(1) TeV, X ~ O(10) TeV, N ~ O(0.5) TeV S Decay + D Annihilation or no annihilation works BR D ~ 10-6 Y s =(3/4)T r / s ~ 10-4 n D /s ~ Allahverdi, Dutta, Sinha, 13 9

30 odel Exaple S Decay + Branching ratio Baryogenesis ~ 0.01 ~ 1 8 N1 X or ( N1 / X ) ~ 10-4 ~ 10 - Y s =(3/4)T r / s ~ 10-4 ~

31 Non-theral Cross Sections Scenarios via Probe the D sector directly: One interesting way: CD pp ~ ~ jj Preselection: issing E T > 50 GeV, leading jets (j 1,j ) :p T (j 1 ),p T (j ) >30 GeV Dh(j 1, j ) > 4. and h j1 h j < 0. Optiization: Tagged jets : p T > 50 GeV, j1j > 1500 GeV; Events with loosely identiied leptons(l = e; ; t h ) and b-quark jets: rejected. issing E T : optiized or dierent value o the LSP ass. Delannoy, Dutta, Gurrola, Kaon, Sinha et al 13 31

32 W extra Non-Theral LHC i N u c i X ' ij Final states at the LHC New Particles: Heavy colored states: d c i S Singlet: LHC signals: new colored states -spin 0- are pair produced high E T our jets in the inal states new colored states spin ½- are pair produced, high E T our jets +issing energy [via cascade decays into squarks etc] d c j X X, Distinguishing Feature: 4 high E T jets and 4 high E T jets + issing energy X X X N N N 3

33 Non-Theral LHC I N is the D candidate, i.e., N ~ p onojet Dijet Dijet pair Dutta, Gao, Kaon 14 Dijet + issing Energy 33

34 D via onojet at LHC Also, ono-top, di-tops in this odel onojet Cobining various observable, we can probe ann. cross-section 34

35 Direct Detection Dark atter Candidates:, Direct detection scattering cross-section: N ~ Suppose: N ~ ~ N, c i N ~ Xu i Scatters o a quark via s-channel exchange o X N ~ is the D particle (spin-0) For l i ~1, x ~ 1 TeV, I N (spin ½) is D, N ~ p (to prevent N decay and p-decay), s N-p is c (SI) and 10-4 c (SD)

36 Conclusion The origin o D content is a big puzzle We will be able to understand the history o the early universe Theral D is a very attractive scenario However, it contains certain assuptions about theral history Alternatives with a non-standard theral history are otivated Typically arise in UV copletions Can ease the tension with tightening experiental liits Non-theral D arising ro oduli decay is a viable scenario can yield the correct density or large & sall annihilation rates Successul realization in explicit constructions is nontrivial