Asymmetric Twin Dark Matter

Journal of Cosmology and Astroparticle Physics

OPEN ACCESS Related content

- The fraternal WIMP miracle Asymmetric twin Dark Matter Nathaniel Craig and Andrey Katz - Asymmetric dark matter models and the To cite this article: Marco Farina JCAP11(2015)017 LHC diphoton excess Mads T. Frandsen and Ian M. Shoemaker

- Sharing but not caring: dark matter and the baryon asymmetry of the universe Nicolás Bernal, Chee Sheng Fong and View the article online for updates and enhancements. Nayara Fonseca

Recent citations

- Minimal non-abelian supersymmetric Twin Higgs Marcin Badziak and Keisuke Harigaya

- Effective theory of flavor for Minimal Mirror Twin Higgs Riccardo Barbieri et al

- Simplified models for displaced dark matter signatures Oliver Buchmueller et al

This content was downloaded from IP address 131.169.4.70 on 28/11/2017 at 22:54 JCAP11(2015)017 hysics P le ic t ar doi:10.1088/1475-7516/2015/11/017 strop A . Content from this work may be used 3 osmology and and osmology C 1506.03520 dark matter theory, dark matter experiments, particle physics - cosmology con-

We study a natural implementation of Asymmetric Dark Matter in Twin Higgs rnal of rnal Article funded byunder SCOAP the terms of the Creative Commons Attribution 3.0 License .

ou An IOP and SISSA journal An IOP and Department of Physics, LEPP, CornellIthaca, University, NY, 14853 U.S.A. E-mail: [email protected] Any further distribution ofand this the work must title maintain of attribution the to work, the author(s) journal citation and DOI. models. The mirroringwith of mass the aroundasymmetry 5 Standard GeV comparable Model is to strong a theMatter sector natural SM in suggests Dark two asymmetry different that Matter isa scenarios, a generated. candidate one complete twin with once copy We minimal baryon a of exploresuccessful content thermal twin twin the in history the baryon baryon SM, are twin Dark presented, number includingissues sector and common a in and to doing light one so many with twin wesignatures Twin address photon. at Higgs some direct models. of The detection the The essential cosmological experiments required and requirements interactions at for we the introduce LHC. Keywords: predict nection ArXiv ePrint: Marco Farina Received August 1, 2015 Accepted October 17, 2015 Published November 9, 2015 Abstract. Asymmetric twin Dark Matter J JCAP11(2015)017 , B . It (1.1) 5Ω B of the n ' f ∼ DM DM n sets the visible matter , with the second easily B N n m , for example by having only ∼ B n DM ∼ m , DM n N = 246 GeV the SM Higgs vev. DM , and m v f m B DM n n , with – 1 – v = . Motivated by this tantalizing observation we study f B few DM Ω Ω ∼ is the nucleon mass. If the two asymmetries are generated symmetry. The scalar potential has an accidental global f N 2 symmetry suggests below Z m 2 2 Z Z and the question to address is why this mass ratio is close to unity. conserved above the scale N ˜ m B 5 − ∼ in the same way the baryon number asymmetry B DM ). Approximate DM ˜ m is the DM mass and n B ( DM B m The discovery of the Higgs boson and the lack of new physics signals at the LHC made Twin Higgs is a natural environment in which to implement the ADM idea. It is 3.1 Scenario3.2 A4 Scenario B7 2.1 Twin Dark2 Matter the combination the viability of twin baryons as ADM. SU(4) symmetry which protectsis the indeed Higgs a potentialbreaking, from pseudo-Nambu-Goldstone which quadratic boson happens corrections. at and loopSU(4) The it level. breaking Higgs is is For Naturalness naturally expected reasons to light the be even order parameter after symmetry perturbed by the breaking of Naturalness and the hierarchysolutions, problem renewed a attention critical hasthat issue been solve more recently the brought than to littlethe ever Twin hierarchy SM before. Higgs problem Lagrangian In (TH) is by models search due introducing of [10–14] to a a copy of the SM. The mirroring of straightforward to draw a comparisonlatter between baryons as and DM twin baryons candidates.number and to Both consider are the stable thanks to conservation of the SM (twin) baryon follows that raising the questionpossible. of whether One answer a6] to common (for this origin recent questionasymmetry for reviews is see the the Asymmetric [7–9]), baryondensity. Dark which and In Matter assumes general DM (ADM) the the abundances abundances picture DM is are [1– related density by to be determined by an where by the same mechanism or if one is responsible of the other then we expect 1 Introduction There is overwhelming evidenceits for nature is the yet presence to of be unveiled. Dark One Matter particularly in suggestive the observation is Universe, that however Ω 3 Thermal history4 4 Experimental8 signatures 5 Conclusions9 Contents 1 Introduction1 2 Twin sector properties2 JCAP11(2015)017 Λ. and (2.1) (2.3) (2.2) (2.4) ' p γ . While t m y expected to = t b y y . 5–10 TeV, where v ∼ and ˜ t ` y πf 4 m ∼ . ˜ f , ) (Λ) (from now on all tilded symbols ¯ ˜ j f i ˜ f g h j † ¯ ˜ f . h , ' )( f N i f N N 2 , as already explained, twin proton ˜ f y m i ˜ (Λ) ˜ ¯ m m √ f B i 5 ( g j 2 − ' ˜ , or to be integrated out ˜ – 2 – ' f ˜ ` m and ˜ symmetry, naturalness does not impose any bound 2 h B B i ¯ N SU(2) weak gauge symmetries, whose couplings are ff ˜ 2 Ω Ω B m m ˜ h m Z n f y ≡ f/v m ' h B ' O L ⊃ n ` m . In particular we have in mind recent realization of TH in the πf ˜ 4 ) is the (twin) nucleon mass and thus N SU(3) QCD and twin ∼ m is still expected from for Naturalness. We will suppose that there is a copy of each SM quark ( ˜ i v y M N are stable on cosmological time scales. If in the early Universe comparable ' m i few n y is the SM-like Higgs and its interactions with twin particles are those responsible ' h f Related work17] [15– on both thermal and asymmetric DM has been recently carried Finally the twin sector respects the same accidental global symmetries as the SM: twin Naturalness constrains the twin top and bottom Yukawas, with ˜ As for the interactions between the two sectors any TH model contains Higgs interactions where for cancellation of quadratic divergences. At low energy they induce an effective operator where again out in the context of FraternalHere TH instead models we [18], in focus which on only the the third conventional generation TH is scenario2 mirrored. with a copy Twin of all sector generations. properties Our starting point is a Twin Higgs model with an effective cutoff Λ expected to be close to the SM counterparts ˜ charged under twin baryon number, lepton numbererated and by charge. highercarrying We dimensional global will operators charges. neglect and possible consider small stable breakings2.1 gen- each of Twin the DarkDue lightest Matter to particles conservation of twin baryon number again Higher dimensional operatorseffective will scale also becomposite holographic introduced Higgs in frameworkby the [19–21], the strong following, in sector which with and effective by an operators integrating expected are out heavy generated resonances. eventually ˜ asymmetries are generated then refer to twin sector quantitiesshown and in fields). [18, Hypercharge19], is and not eventually necessarily the gauged, twin as photon recently is either massless or very heavy ˜ The presence of leptonsdifferent possibilities in in the the spectrum next is section. not strictlyfall necessary respectively within and 1% we and will 10% comment of on the SM values, so from now on we fix ˜ in general ˜ on the first two generations.this Hence in large the deviations following. canwill be be Similar possible, assumed considerations but to apply we have to will mass not the consider ˜ leptons when present; either they JCAP11(2015)017 ˜ B − (2.7) (2.6) (2.8) (2.5) B , with the πf and viceversa and rescalings ˜ B f , s into δα , unless deviations of 5 is expected to avoid . B . down from 4 . This solution depends . On the other hand the QCD y ˜ s B ˜ Λ α f/v (Λ) 1 and ˜ , s and ˜ α ) f n B . This leaves , ˜ d − q ) . Then y invariant and preserving only m s 2 ˜ . d ) 2 ˜ ˜ 2 α l (Λ) 1 function. It is also possible to directly u Z √ s − α )(˜ f/v β s is typically stable and it is the main DM ( f/ QCD k α d (10%) splitting of the UV coupling constants ( j n ∼ = 1 the operator is efficient above temperatures plays a crucial role. First the different masses π 2 (Λ), for instance this can be due to threshold O 9 d 5 Λ q 2 i s s Λ 3 ∼ u α 2 t – 3 – ' α m ( π FT y g − 5 3 , it will convert any excess in lmn ijk Exp M QCD ' g ˜ 9 B (Λ) ˜ / Λ 2 h s , as in partial compositeness, would be enough to avoid 2 ≡ − α 5 GeV. The ˜ ˜ δm ... B B v f = ˜ j B ' y s , has been introduced to evade constraints on DM lifetime. A i O . Indeed for n y ' δα ) as variables. The results are presented in figure1 which shows m . lmn ijk t πf ∝ g B y 4 and all fields are right handed. The operator flavour structure, n QCD QCD . lmn ijk ∼ ˜ Λ Λ g πf T 5 is a typical result once a B 4 is determined by the QCD confinement scale n . ' ∼ f N with mass ˜ m n M QCD i Λ y / = and, because it conserves i y QCD Having successfully accounted for the DM to baryon mass ratio, how can their number We conclude, also anticipating the results in section3, that our DM candidate is a We compute the confinement scale of twin QCD by running ˜ A different possibility is the sharing of asymmetries through non-perturbative effects, ˜ M Λ ∼ function computed for 6 flavours of mass ˜ crucially on the UV completion of the modeltwin and it neutron is ˜ beyond the scope of the present work. for example leptogenesis followed by generation of both so that it enforces ˜ density be related? Followingasymmetries the in ADM the picture twoeffective [6] sectors operator some should connecting mechanism SM be connecting and efficient the twin in baryon singlets, the early Universe. First consider an initial condition is(FT) exponentially contours amplified given by by two the loop running. contribution to We the Higgs also mass show [18] the fine tuning which is of theFT same order larger of than the few standard %. The first term accountspression for explains the the difference negligible in sensitivity the to quark the mass choice thresholds of and its evident sup- As in the SMvarious order ˜ of magnitude are allowed in the Yukawas. Then satisfying eq. (2.4) requires where again any bound and to ensureat that the temperatures operator involving third generation quarks is in equilibrium embedded in the coupling structure of the form T How likely is it to happen? The running of of all Yukawas (apart thehow ˜ is introduced. Thefixing effect ˜ can be explained by a simple approximate equation obtained by introduce a small difference of the twin quarks change the thresholdseffects in in composite the TH realizations,representations in under which heavy the resonances twin are and expected the to have SM different gaugeβ groups. JCAP11(2015)017 and f few GeV, . The solid [22, ]. 23 q ' y . As such we 1 v − T g = 2 & 2 q y T 5 cm . 4 as a function of 0 > 1200 . resulting in a cross section n 3 20 ˜ ) m QCD / 1100 ˜ n Λ asymmetry is the only asymmetry / σ QCD ˜ B ˜ Λ 1000 / QCD , in orange the case ˜ ˜ Λ q 5 y L QCD > 900 = q GeV H y f 10 800 – 4 – 700

600 few GeV. = 5 computed using the approximate function deﬁned in eq. (2.6). 500 '

QCD 0.10 0.05 0.00 0.30 0.25 0.20 0.15

Α DΑ Λ which is below the current bound / 1 − QCD g ˜ Λ 2 (Λ). In blue the case in which ˜ s α − 25 cm . 0 . The region of parameter space where 6 (Λ) s ' α Scenario B: a complete copy of the SM content, including a massless twin photon. Scenario A: a minimal scenario with only twin quarks. n Notice that we cannot rely on low reheating temperatures. The Higgs portal of eq. (2.2) In the following we will present the thermal history, including a possible twin nucle- = ˜ ˜ m • • / s ˜ n δα Figure 1 Dashed lines depict thefor fine FT tuning associated values ∆ with = two 5, loops 10, strong 20. contributions to the Higgs mass, component due to charge neutrality of the Universe if the will always keep the two sectors in thermal equilibrium above temperature line corresponds to generated in theus twin sector. remark that Weσ DM will self study interaction its scales experimental like signatures (Λ in4. section 3 Let Thermal history A successful thermal historyoverproduced, must relics and address the two influencefreedom. main on points: BBN and the CMB absence of of additional relativistic other, degrees possibly of while the DM (and baryon asymmetry) are expected to be generated at discard reheating as aequilibrium solution up and to from at now on least we always consider the two sectors to be in 3.1 Scenario A We start with a minimaltwin quarks. scenario with We consider only either the the necessary twin degrees photon of heavy freedom, or which the are twin the hypercharge not gauged. osynthesis phase, for two scenarios differing in content of the twin sector: JCAP11(2015)017 ), π ππ are ) = (3.1) (3.3) (3.5) (3.2) (3.4) m T ± ( π i = ˜ n is the T ( σ in the former H represents the the scattering 2 1 n ˜ T is a singlet and can ˜ Γ , 0 . 450 MeV. The ˜ ) π ± 2 . ' / n ) the decay is efficient in 1 2 π decay keep the twin pions π ± π s f n m 0 m 4 ˜ , number density will freeze-out π − = ˜ 1 2 0 ± QCD − f n π Λ . 1 respectively, and ¯ can be computed by imposing ' T ( / ( i ) ˜ r ˜ ± T 700 GeV T π H the ˜ , 2 π = σv ) 2 SM. Neglecting the twin baryons, the h m T QCD ) ˜ 2 π T

2 2 0 ˜ Λ ˜ 1, and be negligible in our discussion. π ˜ = ˜ n )] m s − and ˜ ∼ ' T ) H − − ˜ → 0 Γ ( y 0 , depleting their number, while the second s π π 0 (6 S ± ¯ n ˜ ( in eq.) (3.2 drops to zero. The first term on ∗ f / π n 4 500 MeV π SM Γ − – 5 – ± ˜ /g n will become overabundant, with each degree of f 0 n − ' 1 π π ( n π i (2) with H ( π ˜ 278 Γ. Above a certain temperature 16 . i p m Γ σv Exp[ ˜ = 0 Y and the total number density will decrease as ˜ −h −h ) = yf/ s ˜ Γ being the crucial parameter. We assume it to be induced ˜ i n ˜ QCD QCD 0 Y = = = ππ σ ˜ Λ Λ n σv m 0 v h ± f → s Hn Hn ππ ' ( + 3 σ π + 3 ))]. On the other hand below 0 ˜ m T will track ± ˙ n ( ˙ n , for example ± H are the number densities of ˜ v n (6 ± / n Γ will eventually decay. A rough estimate of − in equilibrium and no relic density will be produced. For 0 and π π 0 n )Exp[ To study the cosmological history of the twin-pions we write the corresponding Boltz- This scenario does not include any (nearly) massless particle and has no impact on the fo It must be pointed out that at least one extra twin-SU(2) doublet is necessary because of the global Witten T 1 ( i ˜ scattering cross section stable as they are the lightest charged particles. On the other hand ˜ anomaly [24], which requireshave an mass even above number the of doublets. For simplicity such additional field is supposed to decay to SM states, with its width in thermal equilibrium via the processes ˜ mann equations. We assume that operators responsible for ˜ by higher dimensional operators. and similarly their decay constant scales as Upon inspection ofkeeping eq. ˜ (3.2) it is clear that if freedom having a freeze-out density CMB. Only twin pions as possible symmetric relics are left to study. Their mass is given by In the latter caseall there is charged no leptons gauge andwill anomaly neutrinos comment and on are no this leptonic taken choice field to at is be the required, end heavy of enough the to section. be integrated out. We Boltzmann equations are equilibrium distribution. Here, angle brackets represents thermal averages and equilibrium is not maintained and the ˜ where After freeze-out thethe term right proportional hand toterm side ¯ replenishes describes it the as decay long of as ˜ will be efficient, while all ˜ n JCAP11(2015)017 ) ˜ q 5 γ (3.9) (3.6) (3.7) (3.8) µ (3.10) (3.11) mixing ¯ ˜ qγ 0 )( η q –˜ mixing [26] 5 π and thus we γ γ µ f –˜ γ qγ √ is never satisfied meson, while the )(¯ ∝ 2 H X 2 π /M [27, ].28 Alternatively, m . meson and so eq. (3.8) 2 ˜ 0 Γ i 012, we obtain η − . )) 0 ˜ T –10 ( ' 1 . . 2 H − is then given by h 2 4 (6 , 10 / ± / . 3 obs DM π 4 γ 4 π X Γ . ˜ Γ . ˜ − m m decay can be obtained by introducing h θ 2 π GeV 0 2 10 Ω ˜ α / π m is in fine tuning as ˜ 25 GeV 1 sin π Exp 1 GeV 1 − π 4 < 3 π 25 3 X ) 10 − 2 ˜ c m m decays in SM via anomaly and – 6 – h 3 π × π 2 10 /ρ π π 0 ˜ 4 ˜ f ˜ 0 6 f m . π s 2 & π 6 3 M ( 5 TeV f 2 . π ˜ Γ ˜ Y ˜ & 2 α π ' 64 ˜ Γ ˜ . m ˜ Γ = 958 MeV the required scale would be too small for any M 2 ˜ Γ = 0 η ' width can be estimated by plugging the solution of eq. (3.5) in m 2 h π π lifetime is too long its decays could inject entropy during BBN. Thus . Ω 0 π π m is left and DM can be considered as solely composed of twin baryons. . The width roughly scales as 1 s, corresponding to ± 2 2 π − . 10 (or drastic changes in the Yukawas). ˜ Γ 10 TeV is the twin photon mass. However the condition / & ∼ ≈ ) is the entropy density. The final density of ˜ θ γ T ( f/v m s Moreover, if the ˜ Finally it is possible that for sufficiently long lived pions the Universe enters anIf early twin hypercharge is gauged the ˜ We are thankful to Tongyan Lin for pointing out an error in eq. (3.9) of the original version of the paper. 2 induces a decay throughisospin mixing singlets with and theangle so sin SM we mesons. include isospin Notice breaking that effects such in operators the involve form of the ˜ expect where the first factor accounts for the mixing between the pion and an It is clear that for ˜ reasonable model. The price to pay for heavy ˜ where where ˜ higher dimensional operators. In particular, an axial current term (1 mass ratio accountssuppressions for from the the phasetranslates SM space into sector difference. we consider To avoid mixing additional with isospin the breaking An upper boundeq. on (3.6). the Imposing ˜ a conservative limit Ω when compared with theand experimental in constraint of the case of hypercharge not gauged the ˜ we require 1 It is interestingcosmological to lithium notice problem that [25]. such a lateperiod decay of could matter bedilute domination linked, both with and subsequent baryon reheating and possiblyimportant point once DM solve, to the asymmetries. the address pions in While decay. any irrelevant UV This for completion. would present discussion, it is an The bound ofrelic eq. density (3.8) of automatically ˜ satisfies eq. ( 3.7) and suggests that no significant and the width is JCAP11(2015)017 (3.15) (3.14) (3.12) (3.13) binding , which 9 few GeV ˜ − D > 10 ` m . when the fusion π ˜ m , in the twin sector is , 2 . ∗ . Various experimental / problem. On the other i 4 g 1 is equal to the SM one, y T ± i π 2 ` γ ' 2 π T T i m ˜ y m 4 i , and ˜ g − stability problem would be elim- 4 ν 1 / ± 3 , . At temperatures much above the π ± 4 θ , X 0 2 ! ˜ π =fermions ˜ i could be a WIMP candidate, a possibility T T π ˜ sin D annihilate only through weak interactions ˜ ` 8 7 ˜ 2

m π ˜ ` ˜ f + → π 45 36 500 MeV 4 . . ˜ ˜ n m 0 3 – 7 – 2 ` ˜ n i T T ' m ˜ p, ˜ 4 p eff i ˜ n, g N 1 6 TeV p πM ∆ . 32 X M =bosons i ) = ¯ ` ` ) = → T ( 0 ∗ is stable thanks to phase space. The fusion processes can proceed only π g decay is allowed. However n (if hypercharge is not gauged). ˜ Γ(˜ ˜ ν p 23. The number of relativistic degrees of freedom is defined . ± l ˜ once the temperature of the Universe is around the twin deuteron 0 n ± → ± 11 . appears because of helicity suppression and decay to muons is the dominant channel. accounts for the internal degrees of freedom. In general and ˜ π ` i p 36, rescaled to take into account the different temperatures of the two sectors decay width, cause of the mass suppression from chirality flip, and bounds from CMB g = 0 m . 0 Another possibility is a 4-fermion interaction between twin quarks and SM leptons. The What if twin leptons are added? Apparently the ˜ If the twin neutrinos are light, the contribution of ˜ Finally let us briefly comment on the possibility of twin nucleosynthesis, which could and possibly ˜ , and a modified version of the Lee-Weinberg bound [29] then requires ˜ π eff ν = 3 n N ∗ binding energy the ratiothe of abundance nucleons of to nuclei nuclei is is set negligible. by In the particular, high this entropy is of valid the at Universe and where energy. Notice that ˜ with a pion in the final state with ˜ width is where The bound from eq.) (3.8 gives which is lessjustifiable. stringent than eq. (3.11), butinated the if presence ˜ to of ˜ such operatorsto is avoid overproduction. less Ithand, easily would it is clearly an reintroduce interesting observation the that stable a heavy ˜ is not efficient thanks toof Boltzmann ˜ suppression. We conclude that DM is3.2 entirely composed Scenario B Now we consider a complete copy of the SM and again assume ˜ comparable to theis one given in by thetemperature. the SM. After larger Above decoupling the massinto the account. decoupling of different temperature twin temperature the particles, of only the which difference two becomeg sectors non must be relativistic taken at a higher involve ˜ recently explored in [15, the16]. ˜ Thecould presence be of possibly light constraining. neutrinos We does do not not significantly pursue change this direction any further. constraints [27, 28]could require be a possible smallfrom if photon-twin the mixing photon number arises∆ kinetic of at mixing effective 4-loop neutrino or species, higher the order. recent Planck A measurements second [30] constraint give comes JCAP11(2015)017 . ˜ γ n ˜ γ → (3.18) (3.17) (3.16) ˜ ` ˜ ` 7, which is 7, which is . 0 will decay to ∼ ∼ 0 π eff eff N should be involved. N e . f . So the fusion process e n ) and ∆ d is negligible, as shown in the T = ˜ ( ∗ p ± , g n π 1 GeV. How can this be achieved? ∼ 17 . 45 of one SM neutrino species. By . , . ) 0 d d 3 . T ' T / by lifting their masses, for instance by a ( 1 = 0 ) 4 ∗ 75. Thus we obtain ∆ , which is few order of magnitudes lower ν . . d g e ∗ ! the decoupling temperature is roughly given T ) ) g 10 ˜ ( m d d T T T T M H ∼ 30 TeV. We stress that the above results are ( (

∗ ∗ ) – 8 – ˜ = g g d . 45 are suppressed. We are left with fusion processes 2 15 GeV . T 4 . 5 d 0 ( ˜ p ∗ T ˜ M ' ν M g are stable due to phase space, while ˜ asymmetry is generated in the early Universe as well. ' ˜ . Then charge neutrality of the Universe imposes that T T ˜ n L . ↔ ˜ eff B ˜ n N + ∆ e 75 while ˜ . 61 5, and decreasing the total number of relativistic species as can be as well as ˜ . ∼ 5 ± ) , and thus our conclusions are not sensitive to ∼ π e d y T ) ( d ∗ ' T . The estimate only involves ˜ g ( e f ∗ y g are also present, and by charge neutrality ˜ e for ˜ and as in the previous section we conclude that DM is completely composed of ˜ is open and twin atoms will be formed. The ratio of different nuclei is set by the − the temperature of decoupling of the two sectors. If the decoupling happens at ˜ π and ˜ are generated after the twin QCD phase transition. Twin neutrinos are heavy and QCD ˜ d ˜ D Dγ T p n What about nucleosynthesis? First consider the case in which the only asymmetry On the other hand, suppose a In this scenario ˜ If the neutrinos are integrated out, then each leptonic species is stable due to individual The most natural solution is to decouple the ˜ through the twin chiral anomaly. The relic density of ˜ → → ˜ ˜ n γ ˜ n ˜ ˜ ˜ n generated in the twin sector is in previous section. only ˜ so weak processes of the form ˜ γ Now ˜ initial leptonic asymmetry and we leave a detailed study4 of this case Experimental for signatures future work. The experimental signatures predicteddetection by and the possible model collider fall signals. in two Both main of categories: them DM are direct crucially dependent on the higher p Then the requiredindependent scale of is 7 TeV annihilation channel is efficient enough to eliminate any symmetric component [31]. than Λ lepton number conservation and could in principle be a thermal relic. However, the where the normalizationconservation factor of corresponds entropy the to temperatures ratio is which is compatible with present constraints.between We the conclude two that the phase twoAdditional transitions sectors interactions must with between decouple 0 the two sectors must be introduced and ˜ with the freeze-out of Higgs portal interactions, then ˜ For a 4-fermion operator suppressed byby a the scale condition ruled out. The besttransitions when possibility is to have the sectors decouple between the two QCD phase readily seen by a modified version of eq. (3.15) suitable choice of theat twin decoupling, seesaw ˜ scale. The effect is two-fold: increasing the entropy ratio however still in tension with Planck measurements. JCAP11(2015)017 ' n (4.1) (4.2) (4.3) m breaking 2 Z , 2 − = 3. n cm b ˜ decay in Scenario A, and only and similarly for twin baryons. = 48 0 d is − b N π are heavy enough to decay inside b 10 N π , +2 ' . 2 u b 2 µ ) ˜ q 4 µ 2 n = µ 2 b ˜ ) n 2 N ¯ ˜ n qγ b b πM , ˜ )( m d q 4 n b ˜ µ f f ) = – 9 – ( 4 h + 2 qγ N u ) (¯ are demanded for ˜ – b q N 2 πm 5 GeV can be naturally obtained by small n b ˜ (˜ q m M M b = 2 ∼ SI N f p σ ( b 3 TeV is already probed by present experiments [32–34] as . ) = N M – n (˜ SI σ 3 is the nucleon matrix element. The predicted cross section is below the . 0 ' N f ' 1 TeV. For a more tuned scenario in which the ˜ is the reduced mass while n (1–10) TeV are expected and often necessary for a successful thermal history. Their ˜ & f µ O On the other hand, Higgs portal interactions will always contribute with Indeed, twin baryons with mass Regardless of the twin particle content, higher dimensional operators with effective scale Notice that the lowest values of The presence of effective operators will give additional collider signatures on top of the M ∼ effects which induce a higherorder twin of QCD confining magnitude scale.scenarios for It differing the is in also baryon natural spectrumDM asymmetries to candidates. and expect in interactions, the the and same two shown sectors. that twinM We neutrons have are studied typical two introduction provides experimental signaturesDark within Matter direct current detection or experiments near and future at reach, the bothAcknowledgments LHC. at We are deeply thankfuldrea Tesi to for Jack valuableiel Collins, discussions Craig, Duccio Andrey and Katz, Pappadopulo, for Simon Knapen, reading Maxim Eric the Perelstein Kuflik, manuscript. John and March-Russell and An- We Pedro also Schwaller thank Nathan- As previously explained we assume that DM is in the form of twin neutron with mass ˜ axial couplings arecross strictly section necessary. of magnitude In comparable that to eq. case (4.2) only which spin is below dependent present are bounds. induced with the detector it could be possible to have5 signatures similar to emerging Conclusions jets [38]. We have shown that TwinMatter. Higgs They models automatically provide containular a the considering natural required the framework global parallel for symmetries between Asymmetric and baryons Dark particles, and in twin partic- baryons. usual TH signatures [13].escape Twin quarks the are detector. pairfor produced Mono-jet and [35, any36] twin particle and will mono-photon typically searches [37] can be safely evaded dimensional operators thatfermion we operators have induce introduced a inan DM-nucleon section3. operator scattering of cross In the section. form general For the simplicity presence we of consider 4- 5 GeV. The spin independent cross section on a nucleon The parameter space with shown is shown in figure2 for flavour universal couplings neutrino floor. where where JCAP11(2015)017 ]. 537 (2009) SPIRE IN 1 TeV. The A 28 Phys. Rev. ]. D 79 , M > Phys. Rept. , (1990) 445 ]. SPIRE IN (1990) 387[ ][ B 329 Phys. Rev. ]. SPIRE , 4 GeV and 10.0 IN > B 241 Int. J. Mod. Phys. ][ , SPIRE DM IN ][ Nucl. Phys. > m , 7.0 hep-ph/0506256 D Phys. Lett. , for 6 ]. 1 GeV O @ hep-ph/0410114 Asymmetric sneutrino dark matter and the ]. DM 5.0 SPIRE m Asymmetric Dark Matter IN – 10 – Electroweak Fermion Number Violation and the arXiv:1203.1247 ]. (2006) 231802[ SPIRE The Twin Higgs: Natural electroweak breaking from On Relating the Genesis of Cosmic Baryons and Dark IN ]. (2005) 228[ 96 ][

Technicolor cosmology

SPIRE D @ (1985) 55[ IN SPIRE ]. Review of asymmetric dark matter ][ IN B 605 3.0 45 47 39 41 43 37 ][ ------(2012) 095011[

10 10 10 10 10 10

B 165

cm SPIRE

14 - 2 IN Phys. Rev. Lett. , Phys. Lett. arXiv:1305.4939 , A Single explanation for both the baryon and dark matter densities Asymmetric Dark Matter: Theories, Signatures and Constraints Technocosmology — could a technibaryon excess provide a “natural” missing mass Phys. Lett. arXiv:1308.0338 , puzzle ]. (1992) 741[ arXiv:0901.4117 New J. Phys. , DM 68 . DM direct detection parameter space. The shaded region corresponds to DM-nucleon spin Ω / SPIRE b IN [ candidate? Production of Stable Particles in the Early Universe Lett. 115016[ Ω Matter (2013) 1330028[ (2014) 91[ mirror symmetry [1] S. Nussinov, [2] R.S. Chivukula and T.P. Walker, [3] S.M. Barr, R.S. Chivukula and E. Farhi, [4] D.B. Kaplan, [5] D. Hooper, J. March-Russell and S.M. West, [7] H. Davoudiasl and R.N. Mohapatra, [6] D.E. Kaplan, M.A. Luty and K.M. Zurek, [9] K.M. Zurek, [8] K. Petraki and R.R. Volkas, [10] Z. Chacko, H.-S. Goh and R. Harnik, lines correspond to the(dotted upper blue), bounds SuperCDMS from [34] current (dashed DM purple), direct LUX detection33] [ experiments: (solid red). CMDSlite [32] for useful discussions. Thethrough work of grant MF PHY-1316222. is supported by the U.S. National Science Foundation References Figure 2 independent cross sections mediated by the operator JCAP11(2015)017 , 01 05 ]. , JHEP Phys. JCAP JHEP , , , , Phys. JHEP JHEP , Phys. Rev. SPIRE , , , IN , ][ (2015) 191801 ]. 114 SPIRE ]. ]. IN (2013) L20 Colorless Top Partners, a (2015) 1462 ][ ]. ]. 431 SPIRE SPIRE (2015) 055007 (2015) 054 347 IN IN arXiv:0903.3941 The non-gravitational 10 ][ SPIRE SPIRE D 91 IN IN Phys. Rev. Lett. ]. ]. ][ , ][ Science JCAP , , Twin Higgs Asymmetric Dark Matter Twin Higgs WIMP Dark Matter The Composite Twin Higgs scenario (1982) 324[ Natural little hierarchy from a partially Naturalness in the Dark at the LHC arXiv:1006.4172 SPIRE SPIRE The Number density of a charged relic IN IN Phys. Rev. (2009) 015003[ Constraining Self-Interacting Dark Matter with ][ ][ , ]. ]. hep-ph/0510273 B 117 ]. Updated bounds on millicharged particles Planck 2015 results. XIII. Cosmological parameters – 11 – D 80 Mirror world at the large hadron collider ]. ]. SPIRE SPIRE A Twin Higgs model from left-right symmetry arXiv:1311.2600 SPIRE arXiv:1505.07410 IN IN Mon. Not. Roy. Astron. Soc. IN Probing Dark Forces and Light Hidden Sectors at (2010) 103514[ ][ ][ Twin Higgs mechanism and a composite Higgs boson , ][ SPIRE SPIRE (2006) 126[ Phys. Lett. IN IN , ]. ]. 01 ]. Metastable GeV-scale particles as a solution to the cosmological ]. ]. ]. Phys. Rev. ]. ][ ][ D 82 Cosmological Lower Bound on Heavy Neutrino Masses , arXiv:1501.07890 arXiv:1505.07109 ]. Dark Radiation constraints on minicharged particles in models with a (2014) 029[ Holographic Twin Higgs Model SPIRE SPIRE The Fraternal WIMP Miracle 02 SPIRE SPIRE SPIRE SPIRE SPIRE JHEP IN IN Anomaly (2015) 121801[ IN IN IN IN IN , SPIRE [ ][ ][ ][ ][ ][ Colliders IN [ Phys. Rev. 115 − , JCAP arXiv:1501.07803 arXiv:0807.0211 arXiv:1501.05310 SU(2) e , + e hep-ph/0001179 hep-ph/0512088 (2015) 095012[ (2015)[ 055034 An collaboration, P.A.R. Ade et al., (1977) 165[ 39 D 91 D 92 GeV Higgs and the Limits on Naturalness (2015) 161[ (2008) 005[ (2015) 105[ arXiv:1411.2974 arXiv:1211.6426 arXiv:1503.07675 arXiv:1505.07113 arXiv:1411.3310 [ lithium problem 08 Rev. the Milky Way’s dwarf[ spheroidals [ Low-Energy (2000) 003[ arXiv:1502.01589 10 hidden photon 07 interactions of dark matter in colliding galaxy clusters Lett. Planck [ Phys. Rev. Lett. Rev. (2006) 108[ hep-ph/0509242 goldstone twin Higgs 125 [ [21] M. Low, A. Tesi and L.-T. Wang, [20] M. Geller and O. Telem, [22] J. Zavala, M. Vogelsberger and M.G. Walker, [24] E. Witten, [25] M. Pospelov and J. Pradler, [26] R. Essig, P. Schuster and N. Toro, [31] C.F. Berger, L. Covi, S. Kraml and F. Palorini, [23] D. Harvey, R. Massey, T. Kitching, A. Taylor and E. Tittley, [28] H. Vogel and J. Redondo, [19] R. Barbieri, D. Greco, R. Rattazzi and A. Wulzer, [27] S. Davidson, S. Hannestad and G. Raffelt, [29] B.W. Lee and S. Weinberg, [30] [17] I. Lasenby Garc´ıaGarc´ıa,R. and J. March-Russell, [18] N. Craig, A. Katz, M. Strassler and R. Sundrum, [15] I. Garc´ıaGarc´ıa,R. Lasenby and J. March-Russell, [16] N. Craig and A. Katz, [12] Z. Chacko, Y. Nomura, M. Papucci and G. Perez, [11] Z. Chacko, H.-S. Goh and R. Harnik, [13] G. Burdman, Z. Chacko, R. Harnik, L. de Lima and C.B. Verhaaren, [14] R. Barbieri, T. Gregoire and L.J. Hall, JCAP11(2015)017 ]. Eur. , SPIRE IN ][ ]. SPIRE (2015) 235 IN ][ (2015) 059 (2014) 091303 arXiv:1402.7137 C 75 05 112 TeV with the ATLAS detector JHEP ]. , ]. = 8 s SPIRE Eur. Phys. J. (2014)[ 241302 √ arXiv:1309.3259 , IN SPIRE Search for Low-Mass Weakly Interacting Massive Search for Low-Mass Weakly Interacting Massive ][ IN 112 [ TeV Phys. Rev. Lett. , – 12 – Emerging Jets = 8 First results from the LUX dark matter experiment at s √ (2014) 041302[ ]. 112 ]. ]. Phys. Rev. Lett. arXiv:1502.01518 , arXiv:1410.8812 , SPIRE Search for new phenomena in final states with an energetic jet and large SPIRE SPIRE IN IN IN Search for dark matter, extra dimensions and unparticles in monojet Search for new phenomena in monophoton final states in proton-proton TeV ][ ][ ][ = 8 (2015) 299[ collaboration, R. Agnese et al., collaboration, R. Agnese et al., s Phys. Rev. Lett. √ , collaboration, C 75 collaboration, collaboration, collaboration, D.S. Akerib et al., arXiv:1408.3583 arXiv:1502.05409 arXiv:1310.8214 CMS events in proton-proton collisions at SuperCDMS LUX Phys. J. [ collisions at [ Particles Using Voltage-Assisted CalorimetricExperiment Ionization Detection in the SuperCDMS the Sanford Underground Research Facility CMS [ SuperCDMS Particles with SuperCDMS ATLAS missing transverse momentum in pp collisions at [36] [32] [33] [37] [38] P. Schwaller, D. Stolarski and A. Weiler, [34] [35]