Dark Matter: Thermal Versus Non-thermal. Bhaskar Dutta. Texas A&M University
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1 Dark Matter: Theral Versus Non-theral Bhaskar Dutta Texas A&M University IACS, Kolkata, India Deceber 19, 014 1
2 Outline Theral and Non-theral Dark Matter (DM) Moduli Decay and DM Baryogenesis ro the Decay o Moduli Necessary Conditions or Successul Models Exaple o a oduli odel Dark Radiation (DR) and DM 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 Matter 7% How does it explain the dark atter content? Is there any correlation between baryon and dark atter abundance? Atos 5% SM Consequences or: Particle Physics Models Theral History o the Universe 3
4 Dark Matter: Theral Production o theral non-relativistic DM: DM DM Y Y n s n g * T s 3 Universe cools DM DM DM DM dn dt Boltzann equation DM v 3Hn eq DM v 3 3 d p1d p ve ( ) 3 3 d p1d p e ( ) 6 eq ( E ( E 6 1 [ n 1 E E DM ) / ) / T T n DM, eq ] /T 3 d p ( p, t ) n g nos. / 3 ( ) vol
5 Dark Matter: Theral Freeze-Out: Hubble expansion doinates over the interaction rate Dark Matter content: n DM DM 1 3H 0 DM ~ c c v 8G N reeze out v T v ~ DM 6 ~ Assuing : c 3 s Y /T Y becoes constant or T>T a c ~O(10 - ) with c ~ O(100) GeV leads to the correct relic abundance 5
6 Theral Dark Matter Dark Matter content: v ~ DM ~ 1 v reeze out T 0 ~ DM WIMP Dark Energy 68% Dark Matter 7% v c 3 s Weak scale physics : Atos 5% a c ~O(10 - ) with c ~ O(100) GeV leads to the correct relic abundance
7 Dark Matter: Theral Suitable DM Candidate: Weakly Interacting Massive Particle (WIMP) Typical in Physics beyond the SM (LSP, LKP, ) Most Coon: Neutralino (SUSY Models) Neutralino: Mixture o Wino, Higgsino and Bino saller annihilation cross-section Larger annihilation cross-section Larger/Saller Annihilation Proble or theral scenario 7
8 Theral DM 7% Status o Theral DM 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 8
9 Latest result ro Planck 9
10 Dark Matter Pair Annihilation Dark atter annihilation cross-section: <sv>= a + b v a, b are constants I S wave is suppressed then the cross-section is doinated by P wave b v >>a <sv> is uch saller today copared to the reeze-out tie Theral Relic Density: At reeze-out, <sv> =3x10-6 c 3 /s High b/a lowers the cross-section at sall v (Present Epoch) For S wave doination, cross-section reains sae (constant) Annihilation cross-section can be larger today copared to the Freeze-out tie due to Soereld enhanceent 10
11 LHC Constraints and Status o DM LHC constraints on irst generation squark ass + Higgs ass: Natural SUSY and dark atter [Baer, Barger, Huang, Mickelson, Mustaayev 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 DM- Larger annihilation cross-section (or saller wino ass) Arkani-Haid, Gupta, Kapla, Weiner, Zorawsky 1 11
12 LHC status Recent Higgs search results ro Atlas and CMS indicate that h ~16 GeV in the tight MSSM 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 DM 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 1
13 Status o Theral DM Theral equilibriu above T is an assuption. T T Non-standard theral history at is generic in soe explicit UV copletions o the SM. Acharya, Kuar, Bobkov, Kane, Shao 08 Acharya, Kane, Watson, Kuar 09 Allahverdi, Cicoli, Dutta, Sinha, 13 DM content will be dierent in non-standard theral histories (i.e., i there is entropy production at ). T T Barrow 8, Kaionkowski, Turner 90 DM will be a strong probe o the theral history ater it is discovered and a odel is established. 13
14 Theral, Non-theral ann v : Large ulticoponent/non-theral; Sall Non-theral LHC: Investigate colorless particles, establish the odel DM annihilation ro galaxy, extragalactic sources Annihilation into photons: Feri, HAWC, H.E.S.S. Annihilation into neutrinos: IceCube Annihilation into electron-positrons: AMS 14
15 Beyond Theral DM 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 Multi-coponent DM (WIMP + non-wimp) Exaple: ixed Higgsino/axion DM ann v Zurek 13 Asyetric DM (DM content can have large ) ) (theral overproduction): DM ro WIMP decay Ex: Axino DM, Gravitino DM ann v c 3 s 1 Covi, Ki, Roszkowski 99 Feng, Rajaraan, Takayaa 03
16 The oduli decay width: Non-Theral DM Dark Matter ro Moduli decay: Moduli are heavy scalar ields that acquire ass ater SUSY breaking and are gravitationally coupled to atter T r ~ 3 c M p start oscillating when H < t doinate the Universe beore decaying and reheating it c 1/ M p 1/ T r T BBN 50 3 MeV 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., Moroi, Randall 99; Acharya, Kane, Watson 08,Randall; Kitano, Murayaa, Ratz 08; Dutta, Leblond, Sinha 09; Allahverdi, Cicoli, Dutta, Sinha, 13 16
17 Dark Matter ro Moduli DM abundance in 1. First ter on the RHS is the annihilation scenario Requires: th T ann Since T r < T, we need wino/higgsino DM n v DM s ann ann v v.[ n T r DM s ann obs v th v v Th T T r, Y Br DM ] Gaa-rays constraints: Dwar spheroidals, Galactic center M DM > 40 GeV, T < 30 T r T r > 70 MeV. 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 DM ro becoing too sall (actually in realistic scenarios: Br 5 x10-3 => T r < 70MeV) (or ~ 5 x10 6 GeV) 17
18 Dark Matter ro Moduli Decays dilutes any previous relics Theral DM gets diluted i T r < T ~ DM /0 ~ O(10) GeV Axionic DM gets diluted i T r < L QCD ~ 00 MeV ( a ~10 14 GeV is allowed or T r T BBN ) [Fox,Pierce,Thoas 04] Baryon asyetry gets diluted i produced beore decay Non-theral DM Production ro decay Annihilation scenario or T r close to T DM 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 DM and Baryogenesis [Allaverdi, Dutta, Sinha 11] 18
19 Dark Matter ro Moduli Branching scenario solves the coincidence proble Baryon abundance in this odel: n s B Y Br B Y appears in the DM abundance as well, Y ~ BR B ~ easy to satisy or baryogenesis, e (one loop actor) ~ b DM 1 DM Y Br Y Br B DM 1 DM Br Br B DM 1 5 W=r/r c ; r=n For DM ~ 5 B, e BR B ~ BR DM n B ~ n DM The DM abundance and Baryon asyetry are ostly saturated by Y, Brs contribute the reaining not uch particle physics uncertainty 19
20 Baryogenesis ro Moduli N W extra i N u c i X X, ' ij X d c i d c j X : SM singlet; : Color triplet, hypercharge 4/3 Baryogenesis ro decays o X, X M X or N N ~ : can be the DM candidate : Allahverdi, Dutta, Mohapatra, Sinha 1 X M 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
21 1 Baryogenesis Fro X decay Typically, e 1, is O(10 - ) or CP violating phase O(1) and l~o(1) Baryogenesis ro Moduli N N M X X M X d d X u N W c j c i ij c i i extra ' Siilarly, e
22 Conditions or Models 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 DM 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+WMAP9+ACT+SPT+BAO+HST (at 95% CL) : N e =
23 Ex: NT DM 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 Mass spectra, Aparicio, Cicoli, Kippendor, Maharana, Quevedo 14 No Gravitino Proble 3
24 NT DM in Large Volue Scenarios Br 3 The decay to gauge bosons arises at one-loop level: b 3/ 3 SM 3 gg ~ ln( b ) 4 M P The decay to Higgs controlled by the Giudice-Masiero ter: / 0 H u H d 3 Z 4 M P The decay to gauginos (and Higgsinos) is ass suppressed: sot gg ~~ Br 1 M P LVS set up can successully accoodate non-theral DM. Y can be quite sall ~ : branching and annhilations are ok Allahverdi, Cicoli, Dutta, Sinha 13 4
25 NT DM in Large Volue Scenarios I the doinant decay ode is to gauge boson inal states decays into DM particle via 3-body: g gg ~ ~ Since g ~ BR 10 3 DM 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 DM : Y BR DM ~ 10-1 DM ~ O(100) GeV is allowed Solves the coincidence proble 5
26 DM-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 DM-DR Correlation M 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 M P 7c vis ( N e N 3.04) e 6
27 DM-DR Correlation Decay to visible sector ainly produces gauge bosons and Higgs: gg K SM ~ 4 ZH u H b b d 3 P M h.c. gg a b a H u H d b Z 4 M P 3 tot H u H d a b a b Bound ro Planck+WMAP9+ACT+SPT+BAO+HST at 95% N e N e 1 Z 3 We get a lower bound on T r 7
28 P r tot vis r M T g C C T 4 1/ * ) ( ) ( ) ( * g TeV O T MeV O r DM-DR Correlation 3 3 4, 4 P vis vis P tot tot M C M C 1, Z C Z C tot vis Using 4 1/ 1/ 4 * )] 30 /( [ vis r g T 8
29 DM-DR Correlation Abundance o DM 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 DM. 9
30 DM-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 DM, is directly constrained by Feri. For Higgsino-type DM, using the b inal state, the bound reads: T ~ 0 40 GeV 1 T r (18 GeV ) GeV Upper bound on T r gets bounded ro below v ann 30
31 DM-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
32 DM-DR Correlation T r 1 5C 88 C vis hid g * ( T r ) 1 / 4 M 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 DM ass
33 Model 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 + DM Annihilation or no annihilation works BR DM ~ 10-6 Y s =(3/4)T r / s ~ 10-4 n DM /s ~ Allahverdi, Dutta, Sinha, 13 33
34 Model 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 ~
35 Non-theral Cross Sections Scenarios via Probe the DM sector directly: One interesting way: CDM 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, M j1j > 1500 GeV; Events with loosely identiied leptons(l = e; ; t h ) and b-quark jets: rejected. Missing E T : optiized or dierent value o the LSP ass. Delannoy, Dutta, Gurrola, Kaon, Sinha et al 13 35
36 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 SM 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 M X X X N M N N 36
37 Non-Theral LHC I N is the DM candidate, i.e., N ~ p Monojet Dijet Dijet pair Dutta, Gao, Kaon 14 Dijet + Missing Energy 37
38 DM via Monojet at LHC Also, Mono-top, di-tops in this odel Monojet Cobining various observable, we can probe ann. cross-section 38
39 Direct Detection Dark Matter 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 DM particle (spin-0) For l i ~1, M x ~ 1 TeV, I N (spin ½) is DM, M N ~ p (to prevent N decay and p-decay), s N-p is c (SI) and 10-4 c (SD)
40 Conclusion The origin o DM content is a big puzzle We will be able to understand the history o the early universe Theral DM 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 DM 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
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